FN Thomson Reuters Web of Science™ VR 1.0 PT S AU Rein-Weston, D Jacoby, R Chevalley, E Globus, A Yoo, HS Parke, B Lee, P Omar, F Kraut, JM Bienert, N Borade, A Gabriel, C Gonter, K Palmer, E AF Rein-Weston, Daphne Jacoby, Richard Chevalley, Eric Globus, Albert Yoo, Hyo-Sang Parke, Bonny Lee, Paul Omar, Faisal Kraut, Joshua M. Bienert, Nancy Borade, Abhay Gabriel, Conrad Gonter, Kari Palmer, Everett GP IEEE TI DEVELOPMENT OF A ROUTE CROSSING TOOL FOR SHARED AIRSPACE ENVIRONMENTS SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press AB In current-day Terminal Radar Approach Control (TRACON) operations, departure and arrival controllers maintain separate and dedicated airspace for their respective traffic flows. Although this practice has obvious safety features, it also leads to inefficiencies; for example, departure aircraft may be routinely capped beneath arrival airspace. With the right decision-support and coordination tools, departures could continue to climb through arrival airspace when sufficient gaps exist. Previous studies of 'shared airspace' have examined pre-arranged coordination procedures, as well as tools that gave feedback to the controllers on where gaps between arrivals were located and whether the departure aircraft could be scheduled to fly through those gaps [1-4]. Since then, the Route Crossing Tool (RCT) has been developed to allow controllers to assess multiple pre-defined route options at points where the arrivals and departures cross, thereby increasing the possibility of climbing a departure through an arrival gap. The RCT aids in ensuring lateral separation between departure and arrival aircraft that pass through the same altitude. Since the RCT can be applied tactically, it can enable aircraft to fly through arrival flows even if these aircraft depart outside scheduled times. The RCT makes use of a set of predefined parallel departure routes crossing the arrival flow at equidistant intersecting points on the arrival route. The RCT uses the Estimated Time of Arrival (ETA) of the departure aircraft at each intersecting point to calculate the lateral separation with the neighboring arrivals when it crosses that point; this information is graphically displayed to the controller. Additionally, the RCT incorporates forecast winds in its ETA predictions. Multiple prototypes of the RCT have been iteratively developed with feedback from Subject Matter Experts (SMEs). This paper presents the final design, the design process, and lessons learned. Initial results from a simulation suggest that the tool was successful in helping controllers to safely climb more aircraft. Controller feedback on the tool was also positive. C1 [Rein-Weston, Daphne; Chevalley, Eric; Globus, Albert; Yoo, Hyo-Sang; Parke, Bonny; Lee, Paul; Omar, Faisal; Kraut, Joshua M.; Bienert, Nancy; Borade, Abhay; Gabriel, Conrad; Gonter, Kari] San Jose State Univ, Moffett Field, CA 94035 USA. [Rein-Weston, Daphne; Chevalley, Eric; Globus, Albert; Yoo, Hyo-Sang; Parke, Bonny; Lee, Paul; Omar, Faisal; Kraut, Joshua M.; Bienert, Nancy; Borade, Abhay; Gabriel, Conrad; Gonter, Kari; Palmer, Everett] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Jacoby, Richard] ASRC Res & Technol Solut, Moffett Field, CA USA. RP Rein-Weston, D (reprint author), San Jose State Univ, Moffett Field, CA 94035 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 14 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983004075 ER PT S AU Rios, J Hogan, P Gaskins, T Collins, D AF Rios, Joseph Hogan, Patrick Gaskins, Tom Collins, David GP IEEE TI OPEN SOURCE, 3-D TERRAIN VISUALIZATION ON A MOBILE DEVICE SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press AB With the increase in computing power available to mobile devices has come the ability to efficiently display geographic data, which includes 3-dimensional terrain, virtually anywhere. In the work presented here, we provide a high-level overview of software for fetching, viewing, and interacting with geographic data on a mobile device. The software is a re-implementation of NASA's World Wind code targeted for Apple's iOS platform. The resulting code and application programming interface are available in an open source and extensible manner, which allows other developers to build computationally efficient and more custom applications for using 3D geographic data on the iOS platform than with other popular geographic visualization software. To demonstrate the utility of the software, we describe a tool targeted for use in general aviation that is intended to increase situational awareness while en route as well as enabling improved visualization and planning capabilities during pre-flight. To accomplish this, many of the features of the World Wind iOS implementation are exercised. C1 [Rios, Joseph; Hogan, Patrick] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gaskins, Tom] Tom Gaskins Inc, Redmond, WA USA. [Collins, David] Paul Collins Software, Mill Creek, WA USA. RP Rios, J (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Joseph.L.Rios@nasa.gov; Patrick.Hogan@nasa.gov; tom@tomgaskins.com; paul@paulcollinssoftware.com NR 4 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 8 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983005010 ER PT S AU Robinson, JE AF Robinson, John E., III GP IEEE TI CALCULATION OF FLIGHT DECK INTERVAL MANAGEMENT ASSIGNED SPACING GOALS SUBJECT TO MULTIPLE SCHEDULING CONSTRAINTS SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press AB The Federal Aviation Administration's Next Generation Air Transportation System will combine advanced air traffic management technologies, performance-based procedures, and state-of-the-art avionics to maintain efficient operations throughout the entire arrival phase of flight. Flight deck Interval Management (FIM) operations are expected to use sophisticated airborne spacing capabilities to meet precise in-trail spacing from top-of-descent to touchdown. Recent human-in-the-loop simulations by the National Aeronautics and Space Administration have found that selection of the assigned spacing goal using the runway schedule can lead to premature interruptions of the FIM operation during periods of high traffic demand. This study compares three methods for calculating the assigned spacing goal for a FIM operation that is also subject to time-based metering constraints. The particular paradigms investigated include: one based upon the desired runway spacing interval, one based upon the desired meter fix spacing interval, and a composite method that combines both intervals. These three paradigms are evaluated for the primary arrival procedures to Phoenix Sky Harbor International Airport using the entire set of Rapid Update Cycle wind forecasts from 2011. For typical meter fix and runway spacing intervals, the runway-and meter fix-based paradigms exhibit moderate FIM interruption rates due to their inability to consider multiple metering constraints. The addition of larger separation buffers decreases the FIM interruption rate but also significantly reduces the achievable runway throughput. The composite paradigm causes no FIM interruptions, and maintains higher runway throughput more often than the other paradigms. A key implication of the results with respect to time-based metering is that FIM operations using a single assigned spacing goal will not allow reduction of the arrival schedule's excess spacing buffer. Alternative solutions for conducting the FIM operation in a manner more compatible with the arrival schedule are discussed in detail. C1 [Robinson, John E., III] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Robinson, JE (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 17 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983003030 ER PT S AU Robinson, JE AF Robinson, John E., III GP IEEE TI Calculation of Flight Deck Interval Management Assigned Spacing Goals Subject to Multiple Scheduling Constraints SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press C1 [Robinson, John E., III] NASA Ames Res Ctr, Mountain View, CA 94035 USA. RP Robinson, JE (reprint author), NASA Ames Res Ctr, Mountain View, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 23 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983000009 ER PT S AU Robinson, JE AF Robinson, John E., III GP IEEE TI Calculation of Flight Deck Interval Management Assigned Spacing Goals Subject to Multiple Scheduling Constraints SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press C1 [Robinson, John E., III] NASA Ames Res Ctr, Mountain View, CA 94035 USA. RP Robinson, JE (reprint author), NASA Ames Res Ctr, Mountain View, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 19 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983000008 ER PT S AU Sheth, K Gutierrez-Nolasco, S AF Sheth, Kapil Gutierrez-Nolasco, Sebastian GP IEEE TI DEVELOPMENT OF MILES-IN-TRAIL PASSBACK RESTRICTIONS FOR AIR TRAFFIC MANAGEMENT SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press AB This paper presents modeling of miles-in-trail passback restrictions for use in air traffic management. Generally, FAA managers employ miles-in-trail as a traffic management initiative when downstream traffic congestion at airports or in sectors is anticipated. In order to successfully implement the miles-in-trail at airspace fixes or navigational aids, it is desired that restriction values be computed for passing back to upstream facilities at specific boundaries. This paper presents a model which can be used for that purpose. This model improves on a previous version using traffic manager feedback resulting in significant improvement in guidance. The modeling approach is described along with lessons learned and improvements made during model development. Results for two sample traffic and one real traffic scenarios are presented. Additional operational considerations required by the traffic managers to implement the passback restrictions, namely maximum ground delay and absorbable airborne delay are incorporated in the model. A main result of this research is that absorbing small amount of ground and airborne delays are sufficient to handle the imposed constraint. Another finding is that implementing the passback restrictions provides the traffic managers ways to alleviate traffic constraints to help reduce excessive airborne delay for current traffic conditions. C1 [Sheth, Kapil] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gutierrez-Nolasco, Sebastian] UC Santa Cruz, Moffett Field, CA USA. RP Sheth, K (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Kapil.Sheth@nasa.gov; Sebastian.A.GutierrezNolasco@nasa.gov NR 9 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 11 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983003038 ER PT S AU Wang, Y AF Wang, Yao GP IEEE TI ANALYSIS AND PREDICTION OF WEATHER IMPACTED GROUND STOP OPERATIONS SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press AB When the air traffic demand is expected to exceed the available airport's capacity for a short period of time, Ground Stop (GS) operations are implemented by Federal Aviation Administration (FAA) Traffic Flow Management (TFM). The GS requires departing aircraft meeting specific criteria to remain on the ground to achieve reduced demands at the constrained destination airport until the end of the GS. This paper provides a high-level overview of the statistical distributions as well as causal factors for the GSs at the major airports in the United States. The GS's character, the weather impact on GSs, GS variations with delays, and the interaction between GSs and Ground Delay Programs (GDPs) at Newark Liberty International Airport (EWR) are investigated. The machine learning methods are used to generate classification models that map the historical airport weather forecast, schedule traffic, and other airport conditions to implemented GS/GDP operations and the models are evaluated using the cross-validations. This modeling approach produced promising results as it yielded an 85% overall classification accuracy to distinguish the implemented GS days from the normal days without GS and GDP operations and a 71% accuracy to differentiate the GS and GDP implemented days from the GDP only days. C1 [Wang, Yao] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Wang, Y (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 13 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 14 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983004070 ER PT S AU Wang, Y AF Wang, Yao GP IEEE TI Ground Stop Analysis & Prediction SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press C1 [Wang, Yao] NASA Ames Res Ctr, Mountain View, CA 94035 USA. RP Wang, Y (reprint author), NASA Ames Res Ctr, Mountain View, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 34 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983002021 ER PT S AU Witzberger, K Swenson, H Martin, L Lin, M Cheng, JH AF Witzberger, Kevin Swenson, Harry Martin, Lynne Lin, Melody Cheng, Jinn-Hwei GP IEEE TI NEXTGEN TECHNOLOGIES ON THE FAA'S STANDARD TERMINAL AUTOMATION REPLACEMENT SYSTEM SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press AB This paper describes the integration, evaluation, and results from a high-fidelity human-in-the-loop (HITL) simulation of key NASA Air Traffic Management Technology Demonstration - 1 (ATD-1) technologies implemented in an enhanced version of the FAA's Standard Terminal Automation Replacement System (STARS) platform. These ATD-1 technologies include: (1) a NASA enhanced version of the FAA's Time-Based Flow Management, (2) a NASA ground-based automation technology known as controller-managed spacing (CMS), and (3) a NASA advanced avionics airborne technology known as flight-deck interval-management (FIM). These ATD-1 technologies have been extensively tested in large-scale HITL simulations using general-purpose workstations to study air transportation technologies. These general-purpose workstations perform multiple functions and are collectively referred to as the Multi-Aircraft Control System (MACS). Researchers at NASA Ames Research Center and Raytheon collaborated to augment the STARS platform by including CMS and FIM advisory tools to validate the feasibility of integrating these automation enhancements into the current FAA automation infrastructure. NASA Ames acquired three STARS terminal controller workstations, and then integrated the ATD-1 technologies. HITL simulations were conducted to evaluate the ATD-1 technologies when using the STARS platform. These results were compared with the results obtained when the ATD-1 technologies were tested in the MACS environment. Results collected from the numerical data show acceptably minor differences, and, together with the subjective controller questionnaires showing a trend towards preferring STARS, validate the ATD-1/STARS integration. C1 [Witzberger, Kevin; Swenson, Harry] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Martin, Lynne] San Jose State Univ, San Jose, CA 95192 USA. [Lin, Melody] Optimal Synth, Los Altos, CA USA. [Cheng, Jinn-Hwei] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. RP Witzberger, K (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 38 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 15 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983003031 ER PT S AU Xue, M Zelinski, S AF Xue, Min Zelinski, Shannon GP IEEE TI DYNAMIC STOCHASTIC SCHEDULER FOR INTEGRATED ARRIVALS AND DEPARTURES SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press AB In terminal airspace, inefficient operations occur frequently due to constrained airspace and uncertainty. Choke points can easily form in the terminal area and therefore reduce the efficiency of the entire National Airspace System. Based on previous work on scheduling of aircraft arrivals and departures with shared fixes in terminal airspace and uncertainty in departure and arrival times, this work extends the previous stochastic scheduler with dynamic capability such that the scheduler can be sequentially applied to air traffic in terminal airspace with a much larger time frame through sliding windows instead of a static 30-minute traffic scenario. Results show that great delay savings can be achieved by using the dynamic stochastic scheduler relative to current air traffic control procedures. With a 30-minute time window, if an aggressive solution is chosen, on average 5.2 hours can be saved in a day in Los Angeles out of the 30% arrivals and 10% departures that are covered in the experiment. The expected value of annual fuel saving would be more than 10 million dollars. However, the cost of potential controller intervention, which results from the uncertainty of estimated departure and arrival times, will increase by 50% on average. If a moderate solution is chosen instead, with the same expected controller intervention as using current procedure, more than four hours delay saving can still be expected. When uncertainty of departure time increases with look-ahead time, experiments show that optimizations with large windows still find better solutions than the ones with small windows when delay saving is moderate. However, when delay saving is high, time-varied uncertainty plays a more important role than window size, where a small window is preferred for finding good solutions. C1 [Xue, Min] Univ Calif Santa Cruz, Moffett Field, CA 94035 USA. [Zelinski, Shannon] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Xue, M (reprint author), Univ Calif Santa Cruz, Moffett Field, CA 94035 USA. NR 25 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 9 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983003023 ER PT S AU Xue, M Zelinski, SJ AF Xue, Min Zelinski, Shannon J. GP IEEE TI Dynamic Stochastic Scheduler for Integrated Arrivals and Departures SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press C1 [Xue, Min] Univ Calif Santa Cruz, Moffett Field, CA 94035 USA. [Zelinski, Shannon J.] NASA Ames Res Ctr, Moffett Field, CA USA. RP Xue, M (reprint author), Univ Calif Santa Cruz, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 21 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983000002 ER PT S AU Yoo, HS Lee, P Palmer, E AF Yoo, Hyo-sang Lee, Paul Palmer, Everett GP IEEE TI IMPROVING DEPARTURE THROUGHPUT BY DYNAMICALLY ADJUSTING INTER-ARRIVAL SPACING SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press AB LaGuardia airport (LGA) in New York has many unique challenges that create excess taxi-out delays. The purpose of this paper is to investigate the potential benefit that could be gained by tactically adjusting the Terminal Sequencing and Spacing (TSS) schedule to precisely manage inter-arrival spacing to maximize the number of departures per arrival pair. Three strategies for dynamically adjusting arrival schedules are proposed in this paper: Delay Control, Delay and Advance, and No Slack Capacity. The benefits of these strategies were examined on actual traffic data at LGA. The results showed that by applying these strategies, a 10 to 60% increase in departures and a reduction in unutilized departure capacity (gaps) could be achieved during the airport's busiest six-hour period. Significant increases in departure throughput would improve air traffic operations. Furthermore, the concept could be used to resolve temporal mismatches between departure capacity and demand which also cause excessive departure delays. C1 [Yoo, Hyo-sang; Lee, Paul] San Jose State Univ, Res Fdn, Moffett Field, CA 94035 USA. [Yoo, Hyo-sang; Lee, Paul; Palmer, Everett] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Yoo, HS (reprint author), San Jose State Univ, Res Fdn, Moffett Field, CA 94035 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 11 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983003025 ER PT S AU Yoo, HS Lee, P Palmer, E AF Yoo, Hyo-Sang Lee, Paul Palmer, Everett GP IEEE TI IMPROVING DEPARTURE THROUGHPUT BY DYNAMICALLY ADJUSTING INTER-ARRIVAL SPACING SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press C1 [Yoo, Hyo-Sang; Lee, Paul] San Jose State Univ, Res Fdn, NASA Ames Res Ctr, San Jose, CA 95192 USA. [Palmer, Everett] NASA Ames Res Ctr, Moffett Field, CA USA. RP Yoo, HS (reprint author), San Jose State Univ, Res Fdn, NASA Ames Res Ctr, San Jose, CA 95192 USA. EM hyo-sang.yoo@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 15 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983000004 ER PT S AU Zelinski, S AF Zelinski, Shannon GP IEEE TI A FRAMEWORK FOR INTEGRATING ARRIVAL, DEPARTURE, AND SURFACE OPERATIONS SCHEDULING SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press AB This paper proposes a framework for integrating scheduling between arrival, departure, and surface operations to address the drawbacks of domain segregated scheduling. The framework organizes scheduling tasks by time horizon rather than domain. The four-level framework hierarchy includes the configuration schedule, flight schedule, flight schedule update, and schedule conformance. Current NASA research gaps within this framework are discussed and key areas are proposed where future research should focus to facilitate scheduler integration. C1 [Zelinski, Shannon] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Zelinski, S (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Shannon.j.zelinski@nasa.gov NR 60 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 17 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983003022 ER PT S AU Zelinski, S AF Zelinski, Shannon GP IEEE TI A Framework for Integrating Arrival, Departure, and Surface Operations Scheduling SO 2014 IEEE/AIAA 33RD DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC) SE IEEE-AIAA Digital Avionics Systems Conference LA English DT Proceedings Paper CT IEEE/AIAA 33rd Digital Avionics Systems Conference (DASC) CY OCT 05-09, 2014 CL Colorado Springs, CO SP IEEE, AIAA, AIAA Digital Avion Tech Comm, AESS, AdaCore, Great River Technol, Avionics Magazine, Taylor & Francis Grp, CRC Press C1 [Zelinski, Shannon] NASA Ames Res Ctr, Mountain View, CA 94035 USA. RP Zelinski, S (reprint author), NASA Ames Res Ctr, Mountain View, CA 94035 USA. EM Shannon.J.Zelinski@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2155-7195 BN 978-1-4799-5002-7 J9 IEEEAAIA DIGIT AVION PY 2014 PG 42 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE0UA UT WOS:000366983000001 ER PT S AU Margomenos, A Kurdoghlian, A Micovic, M Shinohara, K Brown, DF Corrion, AL Moyer, HP Burnham, S Regan, DC Grabar, RM McGuire, C Wetzel, MD Bowen, R Chen, PS Tai, HY Schmitz, A Fung, H Fung, A Chow, DH AF Margomenos, A. Kurdoghlian, A. Micovic, M. Shinohara, K. Brown, D. F. Corrion, A. L. Moyer, H. P. Burnham, S. Regan, D. C. Grabar, R. M. McGuire, C. Wetzel, M. D. Bowen, R. Chen, P. S. Tai, H. Y. Schmitz, A. Fung, H. Fung, A. Chow, D. H. GP IEEE TI GaN Technology for E, W and G-band Applications SO 2014 IEEE COMPOUND SEMICONDUCTOR INTEGRATED CIRCUIT SYMPOSIUM (CSICS): INTEGRATED CIRCUITS IN GAAS, INP, SIGE, GAN AND OTHER COMPOUND SEMICONDUCTORS SE IEEE Compound Semiconductor Integrated Circuits Symposium LA English DT Proceedings Paper CT IEEE Compound Semiconductor Integrated Circuit Symposium (CSICS) - Integrated Circuits in GaAs, InP, SiGe, GaN and other Compound Semiconductors CY OCT 19-22, 2014 CL La Jolla, CA SP IEEE, IEEE Electron Devices Soc, IEEE Solid State Circuits Soc, IEEE Microwave Theory & Tech Soc DE Gallium nitride; low-noise amplifiers; millimeter wave integrated circuits; millimeter wave transistors; power amplifiers AB Highly scaled GaN T-gate technology offers devices with high f(t)/f(MAX), and low minimum noise figure while still maintaining high breakdown voltage and high linearity typical for GaN technology. In this paper we report an E-band GaN power amplifier (PA) with output power (P-out) of 1.3 W at power added efficiency (PAE) of 27% and a 65-110 GHz ultra-wideband low noise amplifier (LNA). We also report the first G-band GaN amplifier capable of producing output power density of 296mW/mm at 180 GHz. All these components were realized with a 40 nm T-gate process (f(t)= 200 GHz, f(MAX)= 400 GHz, V-brk > 40V) which can enable the next generation of transmitter and receiver components that meet or exceed performance reported by competing device technologies while maintaining > 5x higher breakdown voltage, higher linearity, dynamic range and RF survivability. C1 [Margomenos, A.; Kurdoghlian, A.; Micovic, M.; Shinohara, K.; Brown, D. F.; Corrion, A. L.; Moyer, H. P.; Burnham, S.; Regan, D. C.; Grabar, R. M.; McGuire, C.; Wetzel, M. D.; Bowen, R.; Chen, P. S.; Tai, H. Y.; Schmitz, A.; Fung, H.; Chow, D. H.] HRL Labs LLC, 3011 Malibu Canyon Rd, Malibu, CA 90265 USA. [Fung, A.] CALTECH, Jet Prop Labs, Pasadena, CA 91109 USA. RP Margomenos, A (reprint author), HRL Labs LLC, 3011 Malibu Canyon Rd, Malibu, CA 90265 USA. NR 17 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2162-7940 BN 978-1-4799-3622-9 J9 IEEE COMP SEMICON PY 2014 PG 4 WC Computer Science, Theory & Methods; Engineering, Electrical & Electronic; Physics, Applied SC Computer Science; Engineering; Physics GA BE2PA UT WOS:000369763800037 ER PT J AU Donalek, C Djorgovski, SG Cioc, A Wang, A Zhang, J Lawler, E Yeh, S Mahabal, A Graham, M Drake, A Davidoff, S Norris, JS Longo, G AF Donalek, Ciro Djorgovski, S. G. Cioc, Alex Wang, Anwell Zhang, Jerry Lawler, Elizabeth Yeh, Stacy Mahabal, Ashish Graham, Matthew Drake, Andrew Davidoff, Scott Norris, Jeffrey S. Longo, Giuseppe GP IEEE BE Lin, J Hu, XH Chang, W Nambiar, R Aggarwal, C Cercone, N Honavar, V Huan, J Mobasher, B Pyne, S TI Immersive and Collaborative Data Visualization Using Virtual Reality Platforms SO 2014 IEEE INTERNATIONAL CONFERENCE ON BIG DATA (BIG DATA) LA English DT Proceedings Paper CT IEEE International Conference on Big Data CY OCT 27-30, 2014 CL Washington, DC SP IEEE, IEEE Comp Soc, ELSEVIER, Natl Sci Fdn, CISCO, CCF DE astroinformatics; visualization; virtual reality; data analysis; big data; pattern recognition ID TIME TRANSIENT SURVEY; SYSTEMS AB Effective data visualization is a key part of the discovery process in the era of "big data". It is the bridge between the quantitative content of the data and human intuition, and thus an essential component of the scientific path from data into knowledge and understanding. Visualization is also essential in the data mining process, directing the choice of the applicable algorithms, and in helping to identify and remove bad data from the analysis. However, a high complexity or a high dimensionality of modern data sets represents a critical obstacle. How do we visualize interesting structures and patterns that may exist in hyper-dimensional data spaces? A better understanding of how we can perceive and interact with multidimensional information poses some deep questions in the field of cognition technology and human-computer interaction. To this effect, we are exploring the use of immersive virtual reality platforms for scientific data visualization, both as software and inexpensive commodity hardware. These potentially powerful and innovative tools for multi-dimensional data visualization can also provide an easy and natural path to a collaborative data visualization and exploration, where scientists can interact with their data and their colleagues in the same visual space. Immersion provides benefits beyond the traditional "desktop" visualization tools: it leads to a demonstrably better perception of a datascape geometry, more intuitive data understanding, and a better retention of the perceived relationships in the data. C1 [Donalek, Ciro; Djorgovski, S. G.; Cioc, Alex; Wang, Anwell; Zhang, Jerry; Lawler, Elizabeth; Yeh, Stacy; Mahabal, Ashish; Graham, Matthew; Drake, Andrew] CALTECH, Pasadena, CA 91125 USA. [Davidoff, Scott; Norris, Jeffrey S.] Jet Prop Lab, Pasadena, CA 91109 USA. [Longo, Giuseppe] Univ Naples Federico II, Naples, Italy. RP Donalek, C (reprint author), CALTECH, Pasadena, CA 91125 USA. EM donalek@astro.caltech.edu; Scott.Davidoff@jpl.nasa.gov; jeffrey.s.norris@jpl.nasa.gov; longo@na.infn.it NR 27 TC 9 Z9 9 U1 1 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4799-5666-1 PY 2014 BP 609 EP 614 PG 6 WC Computer Science, Information Systems; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BF2FK UT WOS:000380462900080 ER PT S AU Oktem, FS Kamalabadi, F Davila, JM AF Oktem, Figen S. Kamalabadi, Farzad Davila, Joseph M. GP IEEE TI HIGH-RESOLUTION COMPUTATIONAL SPECTRAL IMAGING WITH PHOTON SIEVES SO 2014 IEEE INTERNATIONAL CONFERENCE ON IMAGE PROCESSING (ICIP) SE IEEE International Conference on Image Processing ICIP LA English DT Proceedings Paper CT IEEE International Conference on Image Processing (ICIP) CY OCT 27-30, 2014 CL Paris, FRANCE SP IEEE ID IMAGES AB Photon sieves, modifications of Fresnel zone plates, are a new class of diffractive image forming devices that open up new possibilities for high resolution imaging and spectroscopy, especially at UV and x-ray regime. In this paper, we develop a novel computational photon sieve imaging modality that enables high-resolution spectral imaging. For the spatially incoherent illumination, we study the problem of recovering the individual spectral images from the superimposed and blurred measurements of the proposed photon sieve system. This inverse problem, which can be viewed as a multi frame deconvolution problem involving multiple objects, is formulated as a maximum posterior estimation problem, and solved using a fixed-point algorithm. The performance of the proposed technique is illustrated for EUV spectral imaging through numerical simulations. The results suggest that higher spatial and spectral resolution can be achieved as compared to conventional spectral imagers. C1 [Oktem, Figen S.; Kamalabadi, Farzad] Univ Illinois, Dept Elect & Comp Engn, Urbana, IL 61801 USA. [Oktem, Figen S.; Kamalabadi, Farzad] Univ Illinois, Coordinated Sci Lab, Urbana, IL 61801 USA. [Davila, Joseph M.] NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD 20771 USA. RP Oktem, FS (reprint author), Univ Illinois, Dept Elect & Comp Engn, Urbana, IL 61801 USA. NR 17 TC 2 Z9 2 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1522-4880 BN 978-1-4799-5751-4 J9 IEEE IMAGE PROC PY 2014 BP 5122 EP 5126 PG 5 WC Computer Science, Theory & Methods; Engineering, Electrical & Electronic; Imaging Science & Photographic Technology SC Computer Science; Engineering; Imaging Science & Photographic Technology GA BE2TU UT WOS:000370063605058 ER PT S AU Burkhardt, MR Davoodi, F Burdick, JW Davoudi, F AF Burkhardt, Matthew R. Davoodi, Faranak Burdick, Joel W. Davoudi, Farhooman GP IEEE TI Energy Harvesting Analysis for Moball, A Self-Propelled Mobile Sensor Platform Capable of Long Duration Operation in Harsh Terrains SO 2014 IEEE INTERNATIONAL CONFERENCE ON ROBOTICS AND AUTOMATION (ICRA) SE IEEE International Conference on Robotics and Automation ICRA LA English DT Proceedings Paper CT IEEE International Conference on Robotics and Automation (ICRA) CY MAY 31-JUN 07, 2014 CL Hong Kong, PEOPLES R CHINA SP IEEE AB This paper considers the design and optimization of an autonomous electromechanical control and energy scavenging system for the wind-propelled Moball, a spherical mobile sensor platform concept [1, 2]. This mechanism converts mechanical motion to electrical energy, and the same mechanism can function as an actuator to self-generate motion. Simulations of a simplified model on flat ground show that a diameter Moball operating in typical Arctic conditions can generate W of power continuously while being wind-propelled. We also demonstrate a simple motion control algorithm, showing that self-propulsion in windless conditions requires. Hence, using this mechanism, a Moball can self-generate sufficient energy for long duration missions involving self-propulsion, sensing, and communication in harsh, cold, windy climates (e.g., Polar regions on Earth, or the surface of Titan or Mars) where solar energy may be limited. Simulations with key design parameters are also used to draw general conclusions regarding optimal design for energy recovery. The addition of springs inside the generating mechanism greatly increases the range of wind speeds over which Moball can harvest energy. C1 [Burkhardt, Matthew R.; Burdick, Joel W.] CALTECH, Dept Mech Engn, Pasadena, CA 91125 USA. [Davoodi, Faranak] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Burkhardt, MR (reprint author), CALTECH, Dept Mech Engn, Pasadena, CA 91125 USA. EM mburkhar@caltech.edu; faranak.davoodi@jpl.nasa.gov NR 22 TC 1 Z9 1 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1050-4729 BN 978-1-4799-3685-4 J9 IEEE INT CONF ROBOT PY 2014 BP 2665 EP 2672 PG 8 WC Automation & Control Systems; Robotics SC Automation & Control Systems; Robotics GA BE9BP UT WOS:000377221102119 ER PT S AU Matthies, L Brockers, R Kuwata, Y Weiss, S AF Matthies, Larry Brockers, Roland Kuwata, Yoshiaki Weiss, Stephan GP IEEE TI Stereo vision-based obstacle avoidance for micro air vehicles using disparity space SO 2014 IEEE INTERNATIONAL CONFERENCE ON ROBOTICS AND AUTOMATION (ICRA) SE IEEE International Conference on Robotics and Automation ICRA LA English DT Proceedings Paper CT IEEE International Conference on Robotics and Automation (ICRA) CY MAY 31-JUN 07, 2014 CL Hong Kong, PEOPLES R CHINA SP IEEE AB We address obstacle avoidance for outdoor flight of micro air vehicles. The highly textured nature of outdoor scenes enables camera-based perception, which will scale to very small size, weight, and power with very wide, two-axis field of regard. In this paper, we use forward-looking stereo cameras for obstacle detection and a downward-looking camera as an input to state estimation. For obstacle representation, we use image space with the stereo disparity map itself. We show that a C-space-like obstacle expansion can be done with this representation and that collision checking can be done by projecting candidate 3-D trajectories into image space and performing a z-buffer-like operation with the disparity map. This approach is very efficient in memory and computing time. We do motion planning and trajectory generation with an adaptation of a closed-loop RRT planner to quadrotor dynamics and full 3D search. We validate the performance of the system with Monte Carlo simulations in virtual worlds and flight tests of a real quadrotor through a grove of trees. The approach is designed to support scalability to high speed flight and has numerous possible generalizations to use other polar or hybrid polar/Cartesian representations and to fuse data from additional sensors, such as peripheral optical fiow or radar. C1 [Matthies, Larry; Brockers, Roland; Weiss, Stephan] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Matthies, L (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM lhm@jpl.nasa.gov; brockers@jpl.nasa.gov; kuwata@alum.mit.edu; stephan.weiss@ieee.org NR 24 TC 6 Z9 6 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1050-4729 BN 978-1-4799-3685-4 J9 IEEE INT CONF ROBOT PY 2014 BP 3242 EP 3249 PG 8 WC Automation & Control Systems; Robotics SC Automation & Control Systems; Robotics GA BE9BP UT WOS:000377221103037 ER PT S AU Bruce, J Caluwaerts, K Iscen, A Sabelhaus, AP SunSpiral, V AF Bruce, Jonathan Caluwaerts, Ken Iscen, Atil Sabelhaus, Andrew P. SunSpiral, Vytas GP IEEE TI Design and Evolution of a Modular Tensegrity Robot Platform SO 2014 IEEE INTERNATIONAL CONFERENCE ON ROBOTICS AND AUTOMATION (ICRA) SE IEEE International Conference on Robotics and Automation ICRA LA English DT Proceedings Paper CT IEEE International Conference on Robotics and Automation (ICRA) CY MAY 31-JUN 07, 2014 CL Hong Kong, PEOPLES R CHINA SP IEEE ID FRAMEWORKS; LOCOMOTION AB NASA Ames Research Center is developing a compliant modular tensegrity robotic platform for planetary exploration. In this paper we present the design and evolution of the platform's main hardware component, an untethered, robust tensegrity strut, with rich sensor feedback and cable actuation. Each strut is a complete robot, and multiple struts can be combined together to form a wide range of complex tensegrity robots. Our current goal for the tensegrity robotic platform is the development of SUPERball, a 6-strut icosahedron underactuated tensegrity robot aimed at dynamic locomotion for planetary exploration rovers and landers, but the aim is for the modular strut to enable a wide range of tensegrity morphologies. SUPERball is a second generation prototype, evolving from the tensegrity robot ReCTeR, which is also a modular, lightweight, highly compliant 6-strut tensegrity robot that was used to validate our physics based NASA Tensegrity Robot Toolkit (NTRT) simulator. Many hardware design parameters of the SUPERball were driven by locomotion results obtained in our validated simulator. These evolutionary explorations helped constrain motor torque and speed parameters, along with strut and string stress. As construction of the hardware has finalized, we have also used the same evolutionary framework to evolve controllers that respect the built hardware parameters. C1 [Bruce, Jonathan] Univ Calif Santa Cruz, Autonomous Syst Lab, Santa Cruz, CA 95064 USA. [Caluwaerts, Ken] Univ Ghent, Elect & Informat Syst Dept, B-9000 Ghent, Belgium. [Iscen, Atil] Oregon State Univ, Corvallis, OR 97331 USA. [Sabelhaus, Andrew P.] Univ Calif Berkeley, Berkeley Inst Design, Berkeley, CA 94720 USA. [SunSpiral, Vytas] SGT Inc, Greenbelt, MD 20770 USA. [SunSpiral, Vytas] NASA, Ames Intelligent Robot Grp, Moffett Field, CA 94035 USA. RP Bruce, J (reprint author), Univ Calif Santa Cruz, Autonomous Syst Lab, Santa Cruz, CA 95064 USA. EM jbruce@soe.ucsc.edu; ken.caluwaerts@ugent.be; iscena@onid.orst.edu; apsabelhaus@berkeley.edu; vytas.sunspiral@nasa.gov NR 29 TC 7 Z9 7 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1050-4729 BN 978-1-4799-3685-4 J9 IEEE INT CONF ROBOT PY 2014 BP 3483 EP 3489 PG 7 WC Automation & Control Systems; Robotics SC Automation & Control Systems; Robotics GA BE9BP UT WOS:000377221103073 ER PT S AU Rao, D De Deuge, M Nourani-Vatani, N Douillard, B Williams, SB Pizarro, O AF Rao, Dushyant De Deuge, Mark Nourani-Vatani, Navid Douillard, Bertrand Williams, Stefan B. Pizarro, Oscar GP IEEE TI Multimodal Learning for Autonomous Underwater Vehicles from Visual and Bathymetric Data SO 2014 IEEE INTERNATIONAL CONFERENCE ON ROBOTICS AND AUTOMATION (ICRA) SE IEEE International Conference on Robotics and Automation ICRA LA English DT Proceedings Paper CT IEEE International Conference on Robotics and Automation (ICRA) CY MAY 31-JUN 07, 2014 CL Hong Kong, PEOPLES R CHINA SP IEEE ID DENOISING AUTOENCODERS; CLASSIFICATION AB Autonomous Underwater Vehicles (AUVs) gather large volumes of visual imagery, which can help monitor marine ecosystems and plan future surveys. One key task in marine ecology is benthic habitat mapping, the classification of large regions of the ocean floor into broad habitat categories. Since visual data only covers a small fraction of the ocean floor, traditional habitat mapping is performed using shipborne acoustic multi-beam data, with visual data as ground truth. However, given the high resolution and rich textural cues in visual data, an ideal approach should explicitly utilise visual features in the classification process. To this end, we propose a multimodal model which utilises visual data and shipborne multi-beam bathymetry to perform both classification and sampling tasks. Our algorithm learns the relationship between both modalities, but is also effective when visual data is missing. Our results suggest that by performing multimodal learning, classification performance is improved in scenarios where visual data is unavailable, such as the habitat mapping scenario. We also demonstrate empirically that the model is able to perform generative tasks, producing plausible samples from the underlying data-generating distribution. C1 [Douillard, Bertrand] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA. [Rao, Dushyant; De Deuge, Mark; Nourani-Vatani, Navid; Williams, Stefan B.; Pizarro, Oscar] Univ Sydney, Australian Ctr Field Robot, Sydney, NSW 2006, Australia. RP Rao, D (reprint author), Univ Sydney, Australian Ctr Field Robot, Sydney, NSW 2006, Australia. EM dushyant.rao@acfr.usyd.edu.au; mark.dedeuge@acfr.usyd.edu.au; navid.nourani-vatani@acfr.usyd.edu.au; Bertrand.Douillard@jpl.nasa.gov; stefan.williams@acfr.usyd.edu.au; oscar.pizarro@acfr.usyd.edu.au RI Nourani, Vahid/F-4051-2017; OI Williams, Stefan/0000-0001-9416-5639 NR 21 TC 4 Z9 4 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1050-4729 BN 978-1-4799-3685-4 J9 IEEE INT CONF ROBOT PY 2014 BP 3819 EP 3825 PG 7 WC Automation & Control Systems; Robotics SC Automation & Control Systems; Robotics GA BE9BP UT WOS:000377221103125 ER PT S AU Friesen, J Pogue, A Bewley, T de Oliveira, M Skelton, R Sunspiral, V AF Friesen, Jeffrey Pogue, Alexandra Bewley, Thomas de Oliveira, Mauricio Skelton, Robert Sunspiral, Vytas GP IEEE TI DuCTT: a Tensegrity Robot for Exploring Duct Systems SO 2014 IEEE INTERNATIONAL CONFERENCE ON ROBOTICS AND AUTOMATION (ICRA) SE IEEE International Conference on Robotics and Automation ICRA LA English DT Proceedings Paper CT IEEE International Conference on Robotics and Automation (ICRA) CY MAY 31-JUN 07, 2014 CL Hong Kong, PEOPLES R CHINA SP IEEE ID LOCOMOTION AB A robot with the ability to traverse complex duct systems requires a large range of controllable motions as well as the ability to grip the duct walls in vertical shafts. We present a tensegrity robot with two linked tetrahedral frames, each containing a linear actuator, connected by a system of eight actuated cables. The robot climbs by alternately wedging each tetrahedron within the duct and moving one tetrahedron relative to the other. We first introduce our physical prototype, called DuCTT (Duct Climbing Tetrahedral Tensegrity). We next discuss the inverse kinematic control strategy used to actuate the robot and analyze the controller's capabilities within a physics simulation. Finally, we discuss the hardware prototype and compare its performance with simulation. C1 [Friesen, Jeffrey; Pogue, Alexandra; Bewley, Thomas] Univ Calif San Diego, Coordinated Robot Lab, MC 0411, La Jolla, CA 92093 USA. [de Oliveira, Mauricio; Skelton, Robert] Univ Calif San Diego, Dept MAE, La Jolla, CA 92093 USA. [Sunspiral, Vytas] NASA, Ames Res Ctr, SGT Inc, Intelligent Robot Grp, Moffett Field, CA 94035 USA. RP Friesen, J (reprint author), Univ Calif San Diego, Coordinated Robot Lab, MC 0411, La Jolla, CA 92093 USA. EM jfriesen@ucsd.edu; alexie.pogue@gmail.com; bewley@ucsd.edu; mauricio@ucsd.edu; bobskelton@ucsd.edu; vytas.sunspiral@nasa.gov OI de Oliveira, Mauricio/0000-0002-1482-2123 NR 12 TC 6 Z9 6 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1050-4729 BN 978-1-4799-3685-4 J9 IEEE INT CONF ROBOT PY 2014 BP 4222 EP 4228 PG 7 WC Automation & Control Systems; Robotics SC Automation & Control Systems; Robotics GA BE9BP UT WOS:000377221104038 ER PT S AU Johnson-Roberson, M Bryson, M Douillard, B Pizarro, O Williams, SB AF Johnson-Roberson, Matthew Bryson, Mitch Douillard, Bertrand Pizarro, Oscar Williams, Stefan B. GP IEEE TI Crowdsourced Saliency for Mining Robotically Gathered 3D Maps Using Multitouch Interaction on Smartphones and Tablets SO 2014 IEEE INTERNATIONAL CONFERENCE ON ROBOTICS AND AUTOMATION (ICRA) SE IEEE International Conference on Robotics and Automation ICRA LA English DT Proceedings Paper CT IEEE International Conference on Robotics and Automation (ICRA) CY MAY 31-JUN 07, 2014 CL Hong Kong, PEOPLES R CHINA SP IEEE ID RECOGNITION; ATTENTION AB This paper presents a system for crowdsourcing saliency interest points for robotically gathered 3D maps rendered on smartphones and tablets. An app was created that is capable of interactively rendering 3D reconstructions gathered with an Autonomous Underwater Vehicle. Through hundreds of thousands of logged user interactions with the models we attempt to data-mine salient interest points. To this end we propose two models for calculating saliency from human interaction with the data. The first uses the view frustum of the camera to track the amount of time points are on screen. The second treats the camera's path as a time series and uses a Hidden Markov model to learn the classification of salient and non-salient points. To provide a comparison to existing techniques, several traditional visual saliency approaches are applied to orthographic views of the models' photo-texturing. The results of all approaches are validated with human attention ground truth gathered using a remote gaze-tracking system that recorded the locations of the person's attention while exploring the models. C1 [Johnson-Roberson, Matthew] Univ Michigan, Dept Naval Architecture & Marine Engn, Ann Arbor, MI 48109 USA. [Bryson, Mitch; Pizarro, Oscar; Williams, Stefan B.] Univ Sydney, Australian Ctr Field Robot, Sydney, NSW 2006, Australia. [Douillard, Bertrand] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. RP Johnson-Roberson, M (reprint author), Univ Michigan, Dept Naval Architecture & Marine Engn, Ann Arbor, MI 48109 USA. EM mattjr@umich.edu; m.bryson@acfr.usyd.edu.au; Bertrand.Douillard@jpl.nasa.gov; o.pizarro@acfr.usyd.edu.au; stefanw@acfr.usyd.edu.au OI Williams, Stefan/0000-0001-9416-5639 NR 25 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1050-4729 BN 978-1-4799-3685-4 J9 IEEE INT CONF ROBOT PY 2014 BP 6032 EP 6039 PG 8 WC Automation & Control Systems; Robotics SC Automation & Control Systems; Robotics GA BE9BP UT WOS:000377221106011 ER PT S AU Ruffatto, D Beganovic, D Parness, A Spenko, M AF Ruffatto, Donald, III Beganovic, Dzenis Parness, Aaron Spenko, Matthew GP IEEE TI Experimental Evaluation of Adhesive Technologies for Robotic Grippers on Micro-Rough Surfaces SO 2014 IEEE INTERNATIONAL CONFERENCE ON ROBOTICS AND AUTOMATION (ICRA) SE IEEE International Conference on Robotics and Automation ICRA LA English DT Proceedings Paper CT IEEE International Conference on Robotics and Automation (ICRA) CY MAY 31-JUN 07, 2014 CL Hong Kong, PEOPLES R CHINA SP IEEE AB This paper presents the performance of a newly developed adhesive that combines an electrostatic adhesive with a directional dry (gecko-like) adhesive. The focus is on the adhesive's performance on micro-rough surfaces, which has a large number of applications in robotic mobility and manipulation such as climbing, perching, and grasping. Performance was characterized using shear/normal adhesion pressure limit curves and comparing the new hybrid adhesive to each individual adhesive mechanism and a control. Results show that the electrostatic directional dry adhesive generally performs better than a directional dry adhesive, but that on several surfaces, an electrostatic adhesive with no fibrillar mechanism performs the best. Additionally, the paper introduces a new mechanism that maintains an adhesive's compliance on micro-rough surfaces while transmitting shear and normal forces to a rigid structure. The mechanism is experimentally compared to a rigid backing and a gecko-like hierarchical suspension layer. Results show that the mechanism performs the best when subjected to mainly normal loads, but a hierarchical suspension handles shear loads better. C1 [Ruffatto, Donald, III; Beganovic, Dzenis; Spenko, Matthew] IIT, Mech Mat & Aerosp Dept, Chicago, IL 60616 USA. [Parness, Aaron] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Ruffatto, D (reprint author), IIT, Mech Mat & Aerosp Dept, Chicago, IL 60616 USA. EM druffatto@hawk.iit.edu; dbeganov@hawk.iit.edu; aaron.parness@jpl.nasa.gov; mspenko@iit.edu NR 13 TC 1 Z9 1 U1 2 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1050-4729 BN 978-1-4799-3685-4 J9 IEEE INT CONF ROBOT PY 2014 BP 6150 EP 6155 PG 6 WC Automation & Control Systems; Robotics SC Automation & Control Systems; Robotics GA BE9BP UT WOS:000377221106028 ER PT S AU Koenig, AW Pavone, M Castillo-Rogez, JC Nesnas, IAD AF Koenig, Adam W. Pavone, Marco Castillo-Rogez, Julie C. Nesnas, Issa A. D. GP IEEE TI A Dynamical Characterization of Internally-Actuated Microgravity Mobility Systems SO 2014 IEEE INTERNATIONAL CONFERENCE ON ROBOTICS AND AUTOMATION (ICRA) SE IEEE International Conference on Robotics and Automation ICRA LA English DT Proceedings Paper CT IEEE International Conference on Robotics and Automation (ICRA) CY MAY 31-JUN 07, 2014 CL Hong Kong, PEOPLES R CHINA SP IEEE ID ASTEROIDS AB The in-situ exploration of small Solar System bodies (such as asteroids or comets) is becoming a central objective for future planetary exploration. Such bodies are characterized by very weak gravitational fields, which make hopping mobility platforms one of the preferred mobility strategies for microgravity surface exploration, as recognized by space agencies worldwide. However, little is known about the dynamical behavior of hopping platforms in low gravity environments, where small bodies' rotational dynamics can have a critical effect. Accordingly, the objective of this paper is to study in detail the "dynamic envelope" of hopping microgravity rovers, with a focus on internal actuation. Specifically, we first perform a static analysis with the goal of determining regions of a small body where an internally-actuated hopping rover can stably remain at rest. Then, we perform a dynamic analysis and discuss the actuation and instrument pointing performance of hopping microgravity platforms as a function of a number of system and environmental parameters (e.g., rover shape, body rotation rate). Finally, we tailor our analysis to a potential mission to Mars' moon Phobos. Collectively, our results show that internally-actuated rovers, from an actuation standpoint, are a viable mobility solution for a vast class of small Solar System bodies. Also, our analysis represents a key first step to develop path planning algorithms for microgravity explorers to safely explore dynamically feasible regions. C1 [Koenig, Adam W.; Pavone, Marco] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA. [Castillo-Rogez, Julie C.; Nesnas, Issa A. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Koenig, AW (reprint author), Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA. EM awkoenig@stanford.edu; pavone@stanford.edu; julie.c.castillo@jpl.nasa.gov; issa.a.nesnas@jpl.nasa.gov NR 19 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1050-4729 BN 978-1-4799-3685-4 J9 IEEE INT CONF ROBOT PY 2014 BP 6618 EP 6624 PG 7 WC Automation & Control Systems; Robotics SC Automation & Control Systems; Robotics GA BE9BP UT WOS:000377221106099 ER PT S AU Niehues, T Badger, J Diftler, M Deshpande, AD AF Niehues, Taylor Badger, Julia Diftler, Myron Deshpande, Ashish D. GP IEEE TI Cartesian-Space Control and Dextrous Manipulation for Multi-Fingered Tendon-Driven Hand SO 2014 IEEE INTERNATIONAL CONFERENCE ON ROBOTICS AND AUTOMATION (ICRA) SE IEEE International Conference on Robotics and Automation ICRA LA English DT Proceedings Paper CT IEEE International Conference on Robotics and Automation (ICRA) CY MAY 31-JUN 07, 2014 CL Hong Kong, PEOPLES R CHINA SP IEEE ID IMPEDANCE CONTROL; OBJECT; GRASP AB Dextrous object manipulation is a crucial task for the hands of the space humanoid Robonaut 2 (R2), and requires accurate control of fingertip positions and forces. We present a novel Cartesian control for the fingers and thumb of the R2 hand. The controller is designed such that the singularities in the fingers are avoided, and distal joint stiffness is added in the thumb for full controllability. We then present a higher-level object stiffness control law for explicit control of object position, orientation, and grasp forces. The complete algorithm is tested experimentally on the R2 hand, with results demonstrating tracking performance and robustness against disturbances. C1 [Niehues, Taylor; Deshpande, Ashish D.] Univ Texas Austin, Dept Mech Engn, Austin, TX 78712 USA. [Badger, Julia; Diftler, Myron] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Niehues, T (reprint author), Univ Texas Austin, Dept Mech Engn, Austin, TX 78712 USA. EM taylor.niehues@utexas.edu; julia.m.badger@nasa.gov; myron.a.diftler@nasa.gov; ashish@austin.utexas.edu NR 18 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1050-4729 BN 978-1-4799-3685-4 J9 IEEE INT CONF ROBOT PY 2014 BP 6777 EP 6783 PG 7 WC Automation & Control Systems; Robotics SC Automation & Control Systems; Robotics GA BE9BP UT WOS:000377221106123 ER PT J AU Kim, K Agogino, AK Moon, D Taneja, L Toghyan, A Dehghani, B SunSpiral, V Agogino, AM AF Kim, Kyunam Agogino, Adrian K. Moon, Deaho Taneja, Laqshya Toghyan, Aliakbar Dehghani, Borna SunSpiral, Vytas Agogino, Alice M. GP IEEE TI Rapid Prototyping Design and Control of Tensegrity Soft Robot for Locomotion SO 2014 IEEE INTERNATIONAL CONFERENCE ON ROBOTICS AND BIOMIMETICS IEEE-ROBIO 2014 LA English DT Proceedings Paper CT 2014 IEEE International Conference on Robotics and Biomimetics (ROBIO) CY DEC 05-10, 2014 CL Bali, INDONESIA SP IEEE Robot & Automat Soc, State Key Lab Robot & Syst, Harbin Inst Technol, Natl Univ Def Technol, Shenzhen Inst Adv Technol AB Co-robots that can effectively move with and operate alongside humans in a variety of conditions could revolutionize the utility of robots for a wide range of applications. Unfortunately, most current robotic systems have difficulty operating in human environments that people easily traverse, much less interact with people. Wheeled robots have difficulty climbing stairs or going over rough terrain. Heavy and powerful legged robots pose safety risks when interacting with humans. Compliant, lightweight tensegrity robots built from interconnected tensile (cables) and compressive (rods) elements are promising structures for co-robotic applications. This paper describes design and control of a rapidly prototyped tensegrity robot for locomotion. The software and hardware of this robot can be extended to build a wide range of tensegrity robotic configurations and control strategies. This rapid prototyping approach will greatly lower the barrier-of-entry in time and cost for research groups studying tensegrity robots suitable for co-robot applications. C1 [Kim, Kyunam; Moon, Deaho; Taneja, Laqshya; Toghyan, Aliakbar; Dehghani, Borna; Agogino, Alice M.] Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA. [Agogino, Adrian K.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Agogino, Adrian K.; SunSpiral, Vytas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [SunSpiral, Vytas] Stinger Ghaffarian Technol Inc, Greenbelt, MD 20770 USA. RP Kim, K (reprint author), Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA. EM knkim@berkeley.edu; adrian.k.agogino@nasa.gov; dmoon@berkeley.edu; laqshya_taneja@berkeley.edu; aliakbar_toghyan@ber-keley.edu; borna2467@berkeley.edu; vytas.sunspiral@nasa.gov; agogino@berkeley.edu NR 35 TC 4 Z9 4 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4799-7397-2 PY 2014 BP 7 EP 14 PG 8 WC Automation & Control Systems; Engineering, Biomedical; Engineering, Electrical & Electronic; Robotics SC Automation & Control Systems; Engineering; Robotics GA BF1IH UT WOS:000380399500002 ER PT S AU Sievers, M Madni, AM AF Sievers, Michael Madni, Azad M. GP IEEE TI A Flexible Contracts Approach to System Resiliency SO 2014 IEEE INTERNATIONAL CONFERENCE ON SYSTEMS, MAN AND CYBERNETICS (SMC) SE IEEE International Conference on Systems Man and Cybernetics Conference Proceedings LA English DT Proceedings Paper CT IEEE International Conference on Systems, Man, and Cybernetics (SMC) CY OCT 05-08, 2014 CL San Diego, CA SP IEEE DE MBSE; system resiliency; contract-based design ID DESIGN AB Contract-based design (CBD) employs formalisms that explicitly define system requirements, constraints, and interfaces. This paper explores a contract-based design paradigm for expressing system resiliency features. Specifically, resilience formalisms are defined in terms of invariant and flexible assertions. A flexible assertion is one that is learned during system operation and can accommodate unpredicted system behaviors. Invariant assertions are fixed system constraints that are known a priori. A general model structure comprising four key features that contribute to system resilience is presented. In particular, the concept of flexible contracts is operationalized using the Hidden Markov Model (HMM) construct. A system architecture based on flexible contracts and lightweight error monitoring and resiliency response mechanisms is also presented. The proposed framework can serve as a testbed to experiment with different systems resiliency approaches. C1 [Sievers, Michael] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Madni, Azad M.] Univ So Calif, Viterbi Sch Engn, Los Angeles, CA USA. RP Sievers, M (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA. EM msievers@jpl.nasa.gov; azad.madni@usc.edu NR 19 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1062-922X BN 978-1-4799-3840-7 J9 IEEE SYS MAN CYBERN PY 2014 BP 1002 EP 1007 PG 6 WC Computer Science, Artificial Intelligence; Computer Science, Cybernetics; Computer Science, Information Systems SC Computer Science GA BE3MJ UT WOS:000370963701021 ER PT S AU Zaal, PMT Sweet, BT AF Zaal, Peter M. T. Sweet, Barbara T. GP IEEE TI The Challenges of Measuring Transfer of Stall Recovery Training SO 2014 IEEE INTERNATIONAL CONFERENCE ON SYSTEMS, MAN AND CYBERNETICS (SMC) SE IEEE International Conference on Systems Man and Cybernetics Conference Proceedings LA English DT Proceedings Paper CT IEEE International Conference on Systems, Man, and Cybernetics (SMC) CY OCT 05-08, 2014 CL San Diego, CA SP IEEE ID MOTION; MODELS; FLIGHT; PITCH AB Airline pilots will soon be required to perform full stall recovery training in simulators. However, flight simulators currently used for pilot training do not represent aircraft behavior in upset situations that take the aircraft out of its normal flight envelope. Post-stall aircraft models need to be implemented to correctly simulate the aircraft response after the stall point. In addition, motion cues need to adequately represent this response to ensure the skills learned in simulator training are directly usable in real flight. This paper will discuss stall recognition and recovery training and why motion is important. Next, we discuss why subjective and traditional outcome-based measures are less effective to measure transfer of stall recovery training and propose to use a measure based on a cybernetic approach that captures how pilots' use of visual and motion cues develops during training. C1 [Zaal, Peter M. T.] San Jose State Univ, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sweet, Barbara T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Zaal, PMT (reprint author), San Jose State Univ, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM peter.m.t.zaal@nasa.gov; barbara.t.sweet@nasa.gov NR 31 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1062-922X BN 978-1-4799-3840-7 J9 IEEE SYS MAN CYBERN PY 2014 BP 3138 EP 3143 PG 6 WC Computer Science, Artificial Intelligence; Computer Science, Cybernetics; Computer Science, Information Systems SC Computer Science GA BE3MJ UT WOS:000370963703044 ER PT S AU Frye, MT Provence, RS AF Frye, Michael T. Provence, Robert S. GP IEEE TI Direct Inverse Control using an Artificial Neural Network for the Autonomous Hover of a Helicopter SO 2014 IEEE INTERNATIONAL CONFERENCE ON SYSTEMS, MAN AND CYBERNETICS (SMC) SE IEEE International Conference on Systems Man and Cybernetics Conference Proceedings LA English DT Proceedings Paper CT IEEE International Conference on Systems, Man, and Cybernetics (SMC) CY OCT 05-08, 2014 CL San Diego, CA SP IEEE DE Direct Inverse Control; Neural Network; Flight Control; UAV helicopter AB This paper presents the initial results of a research project which investigates the application of the Direct Inverse Control technique to the problem of the Autonomous Hover of a quadrotor UAV Helicopter. The goal of the project is to investigate the effectiveness of the Direct Inverse Control technique using an Artificial Neural Network to learn and then cancel out the Hover dynamics of the quadrotor UAV Helicopter under various environmental conditions during a hover mode. The project is to evaluate how robust the control technique is to uncertainty and change in nonlinear dynamics. C1 [Frye, Michael T.] Univ Incarnate Word, Dept Engn, San Antonio, TX USA. [Provence, Robert S.] NASA, Lyndon B Johnson Space Ctr, Aerosci & Flight Mech Div, Houston, TX 77058 USA. RP Frye, MT (reprint author), Univ Incarnate Word, Dept Engn, San Antonio, TX USA. NR 11 TC 2 Z9 2 U1 1 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1062-922X BN 978-1-4799-3840-7 J9 IEEE SYS MAN CYBERN PY 2014 BP 4121 EP 4122 PG 2 WC Computer Science, Artificial Intelligence; Computer Science, Cybernetics; Computer Science, Information Systems SC Computer Science GA BE3MJ UT WOS:000370963704046 ER PT J AU Choi, JM Han, JW Choi, YK AF Choi, Ji-Min Han, Jin-Woo Choi, Yang-Kyu GP IEEE TI Flexible High-performance Nonvolatile Memory by Transferring GAA Silicon Nanowire SONOS onto a Plastic Substrate SO 2014 IEEE INTERNATIONAL ELECTRON DEVICES MEETING (IEDM) SE International Electron Devices Meeting LA English DT Proceedings Paper CT 60th Annual IEEE International Electron Devices Meeting (IEDM) CY DEC 15-17, 2014 CL San Francisco, CA SP IEEE, IEEE Electron Devices Soc AB Flexible nonvolatile memory is demonstrated with excellent memory properties comparable to the traditional wafer-based rigid type of memory. This achievement is realized through the transfer of an ultrathin film consisting of single crystalline silicon nanowire (SiNW) gate-all-around (GAA) SONOS memory devices onto a plastic substrate from a host silicon wafer. C1 [Choi, Ji-Min; Choi, Yang-Kyu] Korea Adv Inst Sci & Technol, Dept Elect Engn, Daejeon, South Korea. [Han, Jin-Woo] NASA, Ctr Nanotech, San Francisco, CA USA. RP Choi, JM (reprint author), Korea Adv Inst Sci & Technol, Dept Elect Engn, Daejeon, South Korea. EM ykchoi@ee.kaist.ac.kr NR 7 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4799-8000-0 J9 INT EL DEVICES MEET PY 2014 PG 4 WC Computer Science, Theory & Methods; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BE3AI UT WOS:000370384800160 ER PT J AU Nikzad, S Hoenk, ME Hennessy, J Jewell, AD Carver, AG Jones, TJ Cheng, SL Goodsall, T Shapiro, C AF Nikzad, Shouleh Hoenk, Michael E. Hennessy, John Jewell, April D. Carver, Alexander G. Jones, Todd J. Cheng, Samuel L. Goodsall, Timothy Shapiro, Charles GP IEEE TI High Performance Silicon Imaging Arrays for Cosmology, Planetary Sciences, & Other Applications SO 2014 IEEE INTERNATIONAL ELECTRON DEVICES MEETING (IEDM) SE International Electron Devices Meeting LA English DT Proceedings Paper CT 60th Annual IEEE International Electron Devices Meeting (IEDM) CY DEC 15-17, 2014 CL San Francisco, CA SP IEEE, IEEE Electron Devices Soc ID INTENSIFIER AB High performance back-illuminated silicon arrays processed with precision atomic control of surface and interfaces are described. Precision atomic control of surface and interfaces parameters dictates quantum efficiency (QE), surface generated dark current, and cosmetic characteristics. Molecular Beam Epitaxy is used to grow delta layers and superlattice structures on the back surface of Si arrays. Photoelectron loss is greatly reduced and near 100% internal QE achieved. Photon losses are reduced by interface engineering using atomic layer deposition. Using these surface and interface treatments in different readout structures and formats creates a suite of devices with many applications. Si detectors spanning planetary science, astrophysics, medical diagnostics, machine vision, and commercial applications will be described. C1 [Nikzad, Shouleh; Hoenk, Michael E.; Hennessy, John; Jewell, April D.; Carver, Alexander G.; Jones, Todd J.; Cheng, Samuel L.; Goodsall, Timothy; Shapiro, Charles] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Nikzad, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM shouleh.nikzad@jpl.nasa.gov NR 21 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4799-8000-0 J9 INT EL DEVICES MEET PY 2014 PG 4 WC Computer Science, Theory & Methods; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BE3AI UT WOS:000370384800065 ER PT J AU Seol, ML Han, JW Woo, JH Moon, DI Kim, JY Choi, YK AF Seol, Myeong-Lok Han, Jin-Woo Woo, Jong-Ho Moon, Dong-Il Kim, Jee-Yeon Choi, Yang-Kyu GP IEEE TI Comprehensive Analysis of Deformation of Interfacial Micro-Nano Structure by Applied Force in Triboelectric Energy Harvester SO 2014 IEEE INTERNATIONAL ELECTRON DEVICES MEETING (IEDM) SE International Electron Devices Meeting LA English DT Proceedings Paper CT 60th Annual IEEE International Electron Devices Meeting (IEDM) CY DEC 15-17, 2014 CL San Francisco, CA SP IEEE, IEEE Electron Devices Soc AB The correlation between the deformation of an interfacial micro-nano structure and the applied pressure in a triboelectric energy harvester (TEH) is analyzed for the first time. The modeling, simulation, visualization experiment, and electrical measurements are conducted in order to clarify the effects of the structural deformation, which governs the triboelectric charge density. The results imply that a small-sized structure is advantageous in output power, while a large-sized structure is advantageous in the pressure sensing range. C1 [Seol, Myeong-Lok; Woo, Jong-Ho; Moon, Dong-Il; Kim, Jee-Yeon; Choi, Yang-Kyu] Korea Adv Inst Sci & Technol, Dept Elect Engn, 291 Daehak Ro, Taejon 305701, South Korea. [Han, Jin-Woo] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Seol, ML (reprint author), Korea Adv Inst Sci & Technol, Dept Elect Engn, 291 Daehak Ro, Taejon 305701, South Korea. EM ykchoi@ee.kaist.ac.kr NR 6 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4799-8000-0 J9 INT EL DEVICES MEET PY 2014 PG 4 WC Computer Science, Theory & Methods; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BE3AI UT WOS:000370384800048 ER PT S AU Kim, J Lee, J Oh, H Rim, T Baek, CK Meyyappan, M Lee, JS AF Kim, Jungsik Lee, Junyoung Oh, Hyeongwan Rim, Taiuk Baek, Chang-Ki Meyyappan, M. Lee, Jeong-Soo BE Takahashi, Y Samukawa, S Tanemura, M Okano, K Endo, K Ono, T Murayama, A Usami, N Saitoh, E Sakamoto, T Nagao, M Shiraishi, K TI The Variability due to Random Discrete Dopant and Grain Boundary in 3D NAND Unit Cell SO 2014 IEEE INTERNATIONAL NANOELECTRONICS CONFERENCE (INEC) SE International Nanoelectronics Conference LA English DT Proceedings Paper CT 6th IEEE International Nanoelectronics Conference (INEC) CY JUL 28-31, 2014 CL Hokkaido Univ, Sapporo, JAPAN SP IEEE Singapore Sect, IEEE Nanotechnol Chapter Singapore Sect HO Hokkaido Univ DE Grain boundary; discrete dopant; threshold voltage; variation; subthreshold swing variation; 3D NAND ID THIN-FILM TRANSISTORS AB We investigate the electrical variability of polysilicon (poly-Si) channels with the single discrete dopant (SDD) and single grain boundary (SGB) for 3D NAND applications. A 3D simulation is used to investigate the effect of the SGB and the SDD on the threshold voltage (Vth) and subthreshold swing (S/S) variation where the SDD and SGB are randomly located in poly-Si channels. The SGB affects the entire channel potential and causes the Vth and S/S variations. On the other hand, the SDD can cause only small fluctuation in the S/S characteristics. C1 [Kim, Jungsik; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang 790784, South Korea. [Lee, Junyoung; Oh, Hyeongwan] Pohang Univ Sci & Technol POSTECH, Dept Elect Engn, Pohang 790784, South Korea. [Rim, Taiuk; Baek, Chang-Ki] Pohang Univ Sci & Technol POSTECH, Dept Creat IT Engn, Pohang 790784, South Korea. [Rim, Taiuk; Baek, Chang-Ki] Pohang Univ Sci & Technol POSTECH, Future IT Innovat Lab, Pohang 790784, South Korea. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lee, JS (reprint author), Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang 790784, South Korea. EM ljs6951@postech.ac.kr NR 7 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2159-3523 BN 978-1-4799-5038-6 J9 INT NANOELECTR CONF PY 2014 PG 3 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology SC Engineering; Science & Technology - Other Topics GA BF6ED UT WOS:000383011300020 ER PT S AU Brat, G AF Brat, Guillaume GP IEEE TI Compositional Verification Using Formal Analysis for a Flight Critical System SO 2014 IEEE INTERNATIONAL TEST CONFERENCE (ITC) SE International Test Conference Proceedings LA English DT Proceedings Paper CT 45th IEEE International Test Conference (ITC) CY OCT 21-23, 2014 CL Seattle, DC SP IEEE Comp Soc, Test Technol Tech Council, IEEE, IEEE Philadelphia Sect C1 [Brat, Guillaume] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. RP Brat, G (reprint author), NASA Ames Res Ctr, Moffett Field, CA 94035 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1089-3539 BN 978-1-4799-4722-5 J9 INT TEST CONF P PY 2014 PG 1 WC Computer Science, Hardware & Architecture; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BE3GX UT WOS:000370703300034 ER PT B AU Zhadobov, M Guraliuc, A Chahat, N Sauleau, R AF Zhadobov, Maxim Guraliuc, Anda Chahat, Nacer Sauleau, Ronan GP IEEE TI Tissue-Equivalent Phantoms in the 60-GHz Band and Their Application to the Body-Centric Propagation Studies SO 2014 IEEE MTT-S INTERNATIONAL MICROWAVE WORKSHOP SERIES ON RF AND WIRELESS TECHNOLOGIES FOR BIOMEDICAL AND HEALTHCARE APPLICATIONS (IMWS-BIO) LA English DT Proceedings Paper CT IEEE MTT-S International Microwave Workshop Series on: RF and Wireless Technologies for Biomedical and Healthcare Applications (IMWS-Bio 2014) CY DEC 08-10, 2014 CL London, UNITED KINGDOM SP Queen Mary Univ London, IEEE, MTT S, APS, Inst Eng Technol, Gold Sponsor CST DE Body-centric communications; millimeter waves; water-based phantoms; polymer-based phantoms ID 60 GHZ AB Experimental tissue-equivalent phantoms represent an essential element for accurate evaluation of antenna / human body interactions as well as for body-centric propagation measurements. The paper is focused on recent advances in design of tissue-equivalent phantoms in the 60-GHz band, in particular on semi-solid and solid phantoms. Recently developed prototypes are presented and compared. Some application examples for propagation measurements are provided, demonstrating that these phantoms can be successfully used for such applications. C1 [Zhadobov, Maxim; Guraliuc, Anda; Sauleau, Ronan] Univ Rennes 1, UMR CNRS 6164, IETR, F-35042 Rennes, France. [Chahat, Nacer] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA. RP Zhadobov, M (reprint author), Univ Rennes 1, UMR CNRS 6164, IETR, F-35042 Rennes, France. EM maxim.zhadobov@univ-rennes1.fr; Nacer.E.Chahat@jpl.nasa.gov NR 14 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4799-5447-6 PY 2014 PG 3 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA BF2EQ UT WOS:000380461000040 ER PT J AU Kislat, F Beilicke, M Zajczyk, A Guo, QZ Endsley, R Cowsik, R Dowkontt, P Barthelmy, S Hams, T Okajima, T Sasaki, M De Geronimo, G Haba, Y Saji, S Krawczynski, H AF Kislat, Fabian Beilicke, Matthias Zajczyk, Anna Guo, Qingzhen Endsley, Ryan Cowsik, Ramanath Dowkontt, Paul Barthelmy, Scott Hams, Thomas Okajima, Takashi Sasaki, Makoto De Geronimo, Gianluigi Haba, Yoshito Saji, Shigetaka Krawczynski, Henric GP IEEE TI The X-Ray Scattering Polarimeter X-Calibur SO 2014 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE (NSS/MIC) LA English DT Proceedings Paper CT IEEE Nuclear Science Symposium / Medical Imaging Conference (NSS/MIC) CY NOV 08-15, 2014 CL Seattle, WA SP IEEE ID ACCRETING BLACK-HOLES; CYGNUS X-1; POLARIZATION; EMISSION; CRAB; TELESCOPE; NEBULA; SPI AB X-ray polarimetry holds the promise to resolve the inner regions of compact systems like mass accreting black holes in X-ray binaries and X-ray bright neutron stars. For example, spectropolarimetric observations of pulsars and pulsar wind nebulae can constrain the geometry and locale of particle acceleration in these sources. We designed and built X-Calibur, a hard x-ray polarimeter which was flown in the focal plane of the InFOC mu S grazing incidence mirror in the fall of 2014 from Fort Sumner (NM). Additional flights are planned for the fall of 2016 from Fort Sumner, as well as for the 2018/19 Antarctic season from McMurdo (Antarctica). X-Calibur exploits the fact that polarized photons scatter preferentially in a direction orthogonal to the orientation of their electric field vector. By combining a low-Z scattering slab with high-Z Cadmium Zinc Telluride detectors to photo-absorb the scattered X-rays, X-Calibur achieves a high detection efficiency of almost unity and a large modulation factor. We have calibrated and tested X-Calibur extensively in the laboratory at Washington University and at the Cornell High-Energy Synchrotron Source (CHESS). Measurements using the highly polarized synchrotron beam at CHESS confirm the polarization sensitivity of the instrument. In this paper we report on the design of X-Calibur, results of laboratory calibration measurements characterizing the performance of the instrument, as well as background measurements taken during the first flight. C1 [Kislat, Fabian; Beilicke, Matthias; Zajczyk, Anna; Guo, Qingzhen; Endsley, Ryan; Cowsik, Ramanath; Dowkontt, Paul; Krawczynski, Henric] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Kislat, Fabian; Beilicke, Matthias; Zajczyk, Anna; Guo, Qingzhen; Endsley, Ryan; Cowsik, Ramanath; Dowkontt, Paul; Krawczynski, Henric] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Barthelmy, Scott; Hams, Thomas; Okajima, Takashi; Sasaki, Makoto] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [De Geronimo, Gianluigi] Brookhaven Natl Lab, Upton, NY 11973 USA. [Haba, Yoshito] Aichi Univ Educ, Kariya, Aichi, Japan. [Saji, Shigetaka] Nagoya Univ, Nagoya, Aichi, Japan. RP Kislat, F (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA. EM fk-islat@physics.wustl.edu FU NASA [NNX10AJ56G, NNX12AD51G]; McDonnell Center; National Science Foundation; National Institutes of Health/National Institute of General Medical Sciences under NSF [DMR-0936384] FX We are grateful for NASA funding from grant NNX10AJ56G & NNX12AD51G and discretionary funding from the McDonnell Center for the Space Sciences to build the X-Calibur polarimeter. Polarization measurements: This work is based upon research conducted at the Cornell High Energy Synchrotron Source (CHESS) which is supported by the National Science Foundation and the National Institutes of Health/National Institute of General Medical Sciences under NSF award DMR-0936384. NR 27 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4799-6097-2 PY 2014 PG 8 WC Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA BG9AN UT WOS:000392917500462 ER PT J AU Terada, Y Yamaguchi, S Sugimoto, S Inoue, T Nakaya, S Ogawa, M Dotani, T Ishisaki, Y Mizushima, K Kominato, T Mine, H Hihara, H Iwase, K Kouzu, T Tashiro, MS Natsukari, C Ozaki, M Kokubun, M Takahashi, T Kawakami, S Kasahara, M Kumagai, S Angelini, L Witthoeft, M AF Terada, Yukikatsu Yamaguchi, Sunao Sugimoto, Shigenobu Inoue, Taku Nakaya, Souhei Ogawa, Mina Dotani, Tadayasu Ishisaki, Yoshitaka Mizushima, Kazuyo Kominato, Takashi Mine, Hiroaki Hihara, Hiroki Iwase, Kaori Kouzu, Tomomi Tashiro, Makoto S. Natsukari, Chikara Ozaki, Masanobu Kokubun, Motohide Takahashi, Tadayuki Kawakami, Satoko Kasahara, Masan. Kumagai, Susumu Angelini, Lorella Witthoeft, Michael GP IEEE TI Design of the Time assignment System for ASTRO-H and Its Performance before Launch SO 2014 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE (NSS/MIC) LA English DT Proceedings Paper CT IEEE Nuclear Science Symposium / Medical Imaging Conference (NSS/MIC) CY NOV 08-15, 2014 CL Seattle, WA SP IEEE DE Astrophysics and Space Instrumentation; X-ray satellite; ASTRO-H mission; Time Assignment; SpaceWire C1 [Terada, Yukikatsu; Yamaguchi, Sunao; Sugimoto, Shigenobu; Inoue, Taku; Nakaya, Souhei; Tashiro, Makoto S.] Saitama Univ, Grad Sch Sci & Engn, Saitama, Saitama, Japan. [Ogawa, Mina; Dotani, Tadayasu; Natsukari, Chikara; Ozaki, Masanobu; Kokubun, Motohide; Takahashi, Tadayuki] ISAS JAXA, Chofu, Tokyo, Japan. [Ishisaki, Yoshitaka] Tokyo Metropolitan Univ, Hachioji, Tokyo, Japan. [Mizushima, Kazuyo; Kominato, Takashi; Mine, Hiroaki] NEC Corp Ltd, Tokyo, Japan. [Hihara, Hiroki; Iwase, Kaori; Kouzu, Tomomi; Kawakami, Satoko; Kasahara, Masan.; Kumagai, Susumu] NEC TOSHIBA Space Syst, Tokyo, Japan. [Angelini, Lorella; Witthoeft, Michael] NASA GSFC, Greenbelt, MD USA. RP Terada, Y (reprint author), Saitama Univ, Grad Sch Sci & Engn, Saitama, Saitama, Japan. EM terada@phy.saitama-u.ac.jp NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4799-6097-2 PY 2014 PG 1 WC Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA BG9AN UT WOS:000392917500464 ER PT J AU Vogel, JK Bhandari, HB Gaskin, JA Miller, SR Nagarkar, VV Pivovaroff, MJ Ramsey, BD Singh, B AF Vogel, Julia K. Bhandari, Harish B. Gaskin, Jessica A. Miller, Stuart R. Nagarkar, Vivek V. Pivovaroff, Michael J. Ramsey, Brian D. Singh, Bipin GP IEEE TI Development of a High Spatial Resolution Detector for at-Wavelength Metrology of X-Ray Optics SO 2014 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE (NSS/MIC) LA English DT Proceedings Paper CT IEEE Nuclear Science Symposium / Medical Imaging Conference (NSS/MIC) CY NOV 08-15, 2014 CL Seattle, WA SP IEEE AB Recent advancements in the field of x-ray astronomy have relied significantly on innovations in grazing-incidence x-ray optics technology, especially for the hard x-ray range for energies above 10 keV. The behavior of these x-ray telescopes for current and planned astrophysical and solar imaging missions needs to be well understood, and fully characterizing the optics includes measurements of the point spread function and effective area for flight optics as a function of energy and off-axis position as well as understanding the scattering and reflectivity properties of substrate coatings. This requires unique detectors with large areas, very high spatial resolution, high sensitivity, photon counting capability and energy discrimination. We report on the development of a detector that is well suited to meet these requirements. The key piece of the instrument is a high spatial-resolution, electron-multiplying charge-coupled device. The detector is back-thinned and optically bonded via a fiberoptic taper to a purpose-fabricated high resolution, high brightness CsI:Tl scintillator with a microcolumnar structure. A prototype version of this camera was used to calibrate the x-ray focusing optics for the Nuclear Spectroscopic Telescope Array (NuSTAR) mission successfully operating in space since its launch in June 2012. Here we present our recent work on the design of the EMCCD detector and scintillators, fabrication, assembly and testing of the full detector system as well as our software development efforts for single photon detection and energy discrimination. Also included are first results from our recent measurement campaign at the x-ray stray light calibration facility of NASA's Marshall Space Flight Center. C1 [Vogel, Julia K.; Pivovaroff, Michael J.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. [Bhandari, Harish B.; Miller, Stuart R.; Nagarkar, Vivek V.; Singh, Bipin] Radiat Monitoring Devices RMD Inc, Watertown, MA 02472 USA. [Gaskin, Jessica A.; Ramsey, Brian D.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA. RP Vogel, JK (reprint author), Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. EM vogel@llnl.gov FU U.S. Department of Energy; Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; NASA [NNX12CA83C] FX Part of this work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. We thank NASA for funding this research under grant number NNX12CA83C. NR 14 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4799-6097-2 PY 2014 PG 9 WC Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA BG9AN UT WOS:000392917500463 ER PT S AU Gunapala, SD Rafol, SB Ting, DZ Soibel, A Hoeglund, L Hill, CJ Khoshakhlagh, A Liu, JK Mumolo, JM Keo, SA AF Gunapala, S. D. Rafol, S. B. Ting, D. Z. Soibel, A. Hoeglund, L. Hill, C. J. Khoshakhlagh, A. Liu, J. K. Mumolo, J. M. Keo, S. A. GP IEEE TI 1/f Noise QWIP Infrared Focal Plane Arrays SO 2014 IEEE PHOTONICS CONFERENCE (IPC) SE IEEE Photonics Conference LA English DT Proceedings Paper CT 27th IEEE Photonics Conference (IPC) CY OCT 12-16, 2014 CL San Diego, CA SP IEEE DE infrared detector; focal plane arrays; quantum wells; QWIP; long-wavelength infrared; noise C1 [Gunapala, S. D.; Rafol, S. B.; Ting, D. Z.; Soibel, A.; Hoeglund, L.; Hill, C. J.; Khoshakhlagh, A.; Liu, J. K.; Mumolo, J. M.; Keo, S. A.] CALTECH, Jet Prop Lab, Ctr Infrared Photodetectors, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Gunapala, SD (reprint author), CALTECH, Jet Prop Lab, Ctr Infrared Photodetectors, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 4 TC 0 Z9 0 U1 5 U2 5 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2374-0140 BN 978-1-4577-1504-4 J9 IEEE PHOTON CONF PY 2014 BP 344 EP 345 PG 2 WC Engineering, Electrical & Electronic; Optics SC Engineering; Optics GA BE4YN UT WOS:000372323200166 ER PT J AU Breneman, AW Cattell, CA Kersten, K Paradise, A Schreiner, S Kellogg, PJ Goetz, K Wilson, LB AF Breneman, A. W. Cattell, C. A. Kersten, K. Paradise, A. Schreiner, S. Kellogg, P. J. Goetz, K. Wilson, L. B., III GP IEEE TI STEREO and Wind Observations of Intense Electron Cyclotron Harmonic Waves at the Earth's Bow Shock and Inside the Magnetosheath SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI C1 [Breneman, A. W.; Cattell, C. A.; Kersten, K.; Paradise, A.; Schreiner, S.; Kellogg, P. J.; Goetz, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Wilson, L. B., III] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Breneman, AW (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. RI Wilson III, Lynn/D-4425-2012 OI Wilson III, Lynn/0000-0002-4313-1970 NR 0 TC 0 Z9 0 U1 1 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 1 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628703091 ER PT J AU Chi, PJ Le, G AF Chi, P. J. Le, G. GP IEEE TI Estimation of Wave Frequency and Azimuthal Wavenumber of High-m ULF Waves by ST-5 Satellite Observations at Low Altitudes SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI C1 [Chi, P. J.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. [Le, G.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. RP Chi, PJ (reprint author), Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. EM pchi@igpp.ucla.edu; guan.le@nasa.gov RI Le, Guan/C-9524-2012 OI Le, Guan/0000-0002-9504-5214 NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 1 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628703119 ER PT J AU de Matthaeis, P Le Vine, D AF de Matthaeis, Paolo Le Vine, David GP IEEE TI RFI Detection and Mitigation for Aquarius: Status and Ongoing Improvements SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI ID SALINITY AB Aquarius is an L-band active/passive sensor designed to globally map sea surface salinity from space [1,2]. Two instruments, a radar scatterometer and a radiometer, observe the same surface footprint almost simultaneously. The radiometer is the primary instrument for sensing sea surface salinity (SSS), while the scatterometer is included to provide a correction for sea surface roughness, which is a primary source of error in the salinity retrieval. Although the primary objective is the measurement of SSS, the instrument combination operates continuously, acquiring data over land and sea ice as well. An important feature of the data processing includes detection and mitigation of Radio Frequency Interference (RFI), which is done separately for both active and passive instruments. Correcting for RFI is particularly critical over ocean because of the high accuracy required in the brightness temperature measurements for SSS retrieval. It is also necessary for applications of the Aquarius data over land, where man-made interference is widespread, even though less accuracy is required in this case. This paper will provide an overview of the current status of the Aquarius RFI processing and an update on the ongoing work on the improvement of the RFI detection and mitigation performance. C1 [de Matthaeis, Paolo] GESTAR, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Le Vine, David] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP de Matthaeis, P (reprint author), GESTAR, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM paolo.dematthaeis@nasa.gov; david.m.levine@nasa.gov NR 7 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 3 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628702147 ER PT J AU Dinnat, EP Boutin, J Yin, X Le Vine, DM Waldteufel, P Vergely, JL AF Dinnat, E. P. Boutin, J. Yin, X. Le Vine, D. M. Waldteufel, P. Vergely, J. -L. GP IEEE TI Comparison of SMOS and Aquarius Sea Surface Salinity and analysis of possible causes for the differences SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI ID MODEL C1 [Dinnat, E. P.; Le Vine, D. M.] NASA GSFC, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Dinnat, E. P.] Chapman Univ, Greenbelt, MD USA. [Boutin, J.; Yin, X.] UPMC, Lab Oceanog & Climat Experimentat & Approches Num, CNRS, IRD,MN, Paris, France. [Waldteufel, P.] UPMC, Lab Atmospheres, CNRS, Milieux,Observat Spatiales,UVSQ, Paris, France. [Vergely, J. -L.] ACRI ST, Sophia Antipolis, France. RP Dinnat, EP (reprint author), NASA GSFC, Cryospher Sci Lab, Greenbelt, MD 20771 USA. NR 11 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628702182 ER PT J AU Horiuchi, S Clark, JE Garcia-Miro, C Goodhart, CE Jacobs, CS Madde, R Mercolino, M Snedeker, L Sotuela, I White, LA AF Horiuchi, S. Clark, J. E. Garcia-Miro, C. Goodhart, C. E. Jacobs, C. S. Madde, R. Mercolino, M. Snedeker, L. Sotuela, I. White, L. A. GP IEEE TI The All Sky Celestial Reference Frame at X/Ka-band (8.4/32 GHz) SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI C1 [Horiuchi, S.] CSIRO, Canberra Deep Space Commun Complex NASA, Canberra, ACT, Australia. [Clark, J. E.; Goodhart, C. E.; Jacobs, C. S.; White, L. A.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. [Garcia-Miro, C.; Sotuela, I.] INSA, Madrid Deep Space Commun Complex NASA, Madrid, Spain. [Madde, R.; Mercolino, M.] ESA, ESOC, Darmstadt, Germany. [Snedeker, L.] NASA, ITT Exelis, Goldstone, CA USA. RP Horiuchi, S (reprint author), CSIRO, Canberra Deep Space Commun Complex NASA, Canberra, ACT, Australia. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 1 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628703239 ER PT J AU Jorgensen, AM Wise, J Lichtenberger, J Heilig, B Vellante, M Reda, J Fridel, RHW Henderson, MG Ober, DM Boudouridis, A Zesta, E Chi, PJ AF Jorgensen, Anders M. Wise, John Lichtenberger, Janos Heilig, Balazs Vellante, Massimo Reda, Jan Fridel, Reiner H. W. Henderson, Michael G. Ober, Daniel M. Boudouridis, Athanasios Zesta, Eftyhia Chi, Peter J. GP IEEE TI Data Assimilation of Space-Based and Ground-Based Observations, and Empirical Models Into a Plasmasphere Model SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI C1 [Jorgensen, Anders M.; Wise, John] New Mexico Inst Min & Technol, Socorro, NM 87801 USA. [Lichtenberger, Janos] Eotvos Lorand Univ, Budapest, Hungary. [Heilig, Balazs] MFGI, Budapest, Hungary. [Vellante, Massimo] Univ Aquila, I-67100 Laquila, Italy. [Reda, Jan] Polish Acad Sci, Inst Geophys, Warsaw 42, Poland. [Fridel, Reiner H. W.; Henderson, Michael G.] Los Alamos Natl Lab, Los Alamos, NM USA. [Ober, Daniel M.] Air Force Res Lab, Albuquerque, NM USA. [Boudouridis, Athanasios] Space Sci Inst, Boulder, CO USA. [Zesta, Eftyhia] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chi, Peter J.] Univ Calif Los Angeles, Los Angeles, CA USA. RP Jorgensen, AM (reprint author), New Mexico Inst Min & Technol, Socorro, NM 87801 USA. EM anders@nmt.edu NR 0 TC 0 Z9 0 U1 1 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 1 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628703134 ER PT J AU Kempf, Y Gutynska, O Pokhotelov, D Wilson, LB Walsh, B von Alfthan, S Sibeck, D Palmroth, M AF Kempf, Y. Gutynska, O. Pokhotelov, D. Wilson, L. B., III Walsh, B. von Alfthan, S. Sibeck, D. Palmroth, M. GP IEEE TI Ion distributions in the Earth's foreshock region: hybrid-Vlasov simulations and spacecraft observations SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI C1 [Kempf, Y.; Pokhotelov, D.] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland. [Kempf, Y.; von Alfthan, S.; Palmroth, M.] Finnish Meteorol Inst, Earth Observat Unit, FIN-00101 Helsinki, Finland. [Gutynska, O.; Wilson, L. B., III; Walsh, B.; Sibeck, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kempf, Y (reprint author), Univ Helsinki, Dept Phys, POB 64, FIN-00014 Helsinki, Finland. EM yann.kempf@fmi.fi; olga.gutynska@nasa.gov; dimitry.pokhotelov@fmi.fi; lynn.b.wilson@nasa.gov; brian.m.walsh-1@nasa.gov; sebastian.von.alfthan@fmi.fi; david.g.sibeck@nasa.gov; minna.palmroth@fmi.fi RI Wilson III, Lynn/D-4425-2012 OI Wilson III, Lynn/0000-0002-4313-1970 NR 0 TC 0 Z9 0 U1 2 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 1 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628703110 ER PT J AU Lang, R Seker, S Yuan, Y Kurum, M Ogut, M O'Neill, P Cosh, M AF Lang, R. Seker, S. Yuan, Y. Kurum, M. Ogut, M. O'Neill, P. Cosh, M. GP IEEE TI Use of Periodic Stalks to Model L Band Returns from Corn SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI C1 [Lang, R.; Yuan, Y.; Ogut, M.] George Washington Univ, Dept Elect & Comp Engn, Washington, DC 20037 USA. [Seker, S.] Bogazici Univ, Dept Elect Elect Engn, Istanbul, Turkey. [Kurum, M.] TUBITAK BILGEM, Informat Technol Inst, Kocaeli, Turkey. [O'Neill, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cosh, M.] USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. RP Lang, R (reprint author), George Washington Univ, Dept Elect & Comp Engn, Washington, DC 20037 USA. EM lang@gwu.edu; sseker@gwu.edu; gwyuan@gwmail.gwu.edu; seker@boun.edu.tr; ogutmehmet@yahoo.com; peggy.e.oneill@nasa.gov; mehmet.kurum@tubitak.gov.tr NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 1 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628702138 ER PT J AU Law, CJ Bower, GC Burke-Spolaor, S Butler, B Lawrence, E Lazio, TJW Mattmann, C Rupen, M Siemion, A VanderWiel, S AF Law, C. J. Bower, G. C. Burke-Spolaor, S. Butler, B. Lawrence, E. Lazio, T. J. W. Mattmann, C. Rupen, M. Siemion, A. VanderWiel, S. GP IEEE TI Interferometric Imaging of Millisecond Transients at 1 TB/hour SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI C1 [Law, C. J.; Bower, G. C.; Siemion, A.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Bower, G. C.] ASIAA, Taipei, Taiwan. [Burke-Spolaor, S.] CALTECH, Pasadena, CA 91125 USA. [Burke-Spolaor, S.; Lazio, T. J. W.; Mattmann, C.] JPL, Pasadena, CA USA. [Butler, B.; Rupen, M.] NRAO, Iowa City, IA USA. [Lawrence, E.; VanderWiel, S.] LANL, Los Alamos, NM USA. RP Law, CJ (reprint author), Univ Calif Berkeley, Berkeley, CA 94720 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 1 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628703235 ER PT J AU Le, G Chi, PJ Blanco-Cano, X Boardsen, S Slavin, JA Anderson, BJ Korth, H AF Le, Guan Chi, Peter J. Blanco-Cano, Xochitl Boardsen, Scott Slavin, James A. Anderson, Brian J. Korth, Haje GP IEEE TI Observations of Upstream Ultra-Low-Frequency Waves in the Mercury's Foreshock SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI C1 [Le, Guan; Chi, Peter J.; Boardsen, Scott] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20546 USA. [Chi, Peter J.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA. [Blanco-Cano, Xochitl] Univ Nacl Autonoma Mexico, Inst Geofis, Ciencias Espaciales, Mexico City, DF, Mexico. [Slavin, James A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Le, G (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20546 USA. EM guan.le@nasa.gov RI Le, Guan/C-9524-2012; Slavin, James/H-3170-2012 OI Le, Guan/0000-0002-9504-5214; Slavin, James/0000-0002-9206-724X NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 1 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628703127 ER PT J AU Le, G Burke, WJ Pfaff, RF Freudenreich, H Maus, S Luhr, H AF Le, Guan Burke, William J. Pfaff, Robert F. Freudenreich, Henry Maus, Stefan Luehr, Hermann GP IEEE TI C/NOFS Measurements of Ring Current Magnetic Field in Low-latitude Ionosphere SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI AB The Vector Electric Field Instrument (VEFI) suite onboard the C/NOFS spacecraft includes a sensitive fluxgate magnetometer to measure DC and ULF magnetic fields in the low latitude ionosphere. The instrument includes a DC vector measurement at 1 sample/sec with a range of +/- 45,000 nT whose primary objective is to enable both V x B and E x B measurements that are more accurate than those provided when a simple magnetic field model is used instead. The magnetic field data can also be used for scientific research to provide information of large-scale ionospheric and magnetospheric current systems. At low latitudes the magnetic field residuals (data with the internal magnetic field model subtracted) are predominately produced by the stormtime ring current. Since C/NOFS provides a complete coverage of all local times every 97 minutes, magnetic field data allow studies of the temporal evolution and local-time variations of stormtime ring current. The analysis demonstrates the feasibility of using instrumented spacecraft in low-inclination orbits to specify the ring current's evolution and local time asymmetry. We will present the results of a statistical study of the stormtime ring current. C1 [Le, Guan; Pfaff, Robert F.; Freudenreich, Henry] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20546 USA. [Burke, William J.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02167 USA. [Maus, Stefan] NOAA, Natl Geophys Data Ctr, Boulder, CO 80303 USA. [Luehr, Hermann] GFZ German Res Ctr Geosci, Potsdam, Germany. RP Le, G (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20546 USA. EM guan.le@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 3 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 1 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628703019 ER PT J AU Le Vine, DM Lagerloef, GSE de Matthaeis, P Dinnat, EP Abraham, S AF Le Vine, D. M. Lagerloef, G. S. E. de Matthaeis, P. Dinnat, E. P. Abraham, S. GP IEEE TI Aquarius Overview and Up Date SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI AB Aquarius is an L-band instrument designed to map the surface salinity field of the global oceans. It consists of three L-band (1.41 GHz) radiometers and an L-band (1.26 GHz) scatterometer. The radiometers are the primary instruments for measuring salinity and the scatterometer provides a correction for surface roughness. Aquarius was launched in June 2011 and has been mapping the surface salinity field since it was turned on in August. In addition, Aquarius is now producing maps of radio frequency interference (RFI), Faraday rotation and soil moisture. C1 [Le Vine, D. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lagerloef, G. S. E.] Earth & Space Res, Seattle, WA 98121 USA. [de Matthaeis, P.] NASA, Goddard Space Flight Ctr, USRA GESTAR, Greenbelt, MD 20771 USA. [Dinnat, E. P.] Chapman Univ, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Abraham, S.] NASA, Goddard Space Flight Ctr, Wyle Informat Syst, Greenbelt, MD 20771 USA. RP Le Vine, DM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM david.m.levine@nasa.gov; lager@esr.org; paolo.dematthaeis@nasa.gov; emmanuel.dinnat@nasa.gov; saji.abraham@nasa.gov NR 7 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628702180 ER PT J AU Nghiem, SV Hall, DK Rigor, IG Li, P Neumann, G AF Nghiem, S. V. Hall, D. K. Rigor, I. G. Li, P. Neumann, G. GP IEEE TI Observations of Arctic Sea Ice and River Discharge with Multiple Satellite Sensors SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI C1 [Nghiem, S. V.; Li, P.; Neumann, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nghiem, S. V.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. [Hall, D. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rigor, I. G.] Univ Washington, Seattle, WA 98195 USA. RP Nghiem, SV (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 1 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628702076 ER PT J AU Pfaff, R AF Pfaff, Robert GP IEEE TI ELECTRIC FIELD AND PLASMA DENSITY OBSERVATIONS OF LARGE SCALE (100'S OF KM) WAVES BELOW THE EQUATORIAL F-PEAK AS SEEDS OF SPREAD-F SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI C1 [Pfaff, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20546 USA. RP Pfaff, R (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20546 USA. EM Robert.F.Pfaff@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 1 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628703038 ER PT J AU Pfaff, R Freudenreich, H Simoes, F Liebrecht, C AF Pfaff, Robert Freudenreich, Henry Simoes, Fernando Liebrecht, Carmen GP IEEE TI OBSERVATIONS OF 50/60 HZ POWER LINE RADIATION IN THE LOW LATITUDE IONOSPHERE DETECTED BY THE ELECTRIC FIELD INSTRUMENT ON THE C/NOFS SATELLITE SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI AB Competing demand for spectrum as a result of increasing mobile penetration and demand for high bandwidth services has placed various science services under pressure. In many instances, commercial demands have outweighed the need for spectrum by passive services, which routinely rely on natural radio emissions from earth as well as space. Science services, too, have increasing demands for spectrum as experiments become more sophisticated and complex. In the case of astronomy, technology changes have seen massive growth in discovery potential over the years, with a number of facilities increasingly relying on local and national protection mechanisms. This paper will look at some aspects of the current demands of the scientific services and how countries may resolve this, using South Africa as an example. C1 [Pfaff, Robert; Freudenreich, Henry; Simoes, Fernando; Liebrecht, Carmen] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Pfaff, R (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Robert.F.Pfaff@nasa.gov; Henry.T.Freudenreich@nasa.gov; Fernando.Simoes.nasa@gmail.com; Maria.C.Liebrecht@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 2 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628702067 ER PT J AU Tan, SR Tsang, L Kim, SB AF Tan, Shurun Tsang, Leung Kim, Seung-Bum GP IEEE TI Multiple Scattering Effects with Inclusion of Cyclical Terms in Radar Scattering of Vegetated Surfaces Using Vector Radiative Transfer Theory SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI ID BACKSCATTERING ENHANCEMENT C1 [Tan, Shurun; Tsang, Leung] Univ Washington, Dept Elect Engn, Seattle, WA 98195 USA. [Kim, Seung-Bum] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tan, SR (reprint author), Univ Washington, Dept Elect Engn, Seattle, WA 98195 USA. EM srtan@uw.edu; tsang@ee.washington.edu; seungbum.kim@jpl.nasa.gov NR 7 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628702178 ER PT J AU Tang, WQ Yueh, S Fore, A Hayashi, A AF Tang, Wenqing Yueh, Simon Fore, Alexander Hayashi, Akiko GP IEEE TI AQUARIUS' COMBINED ACTIVE PASSIVE ALGORITHM FOR OCEAN SURFACE SALINITY AND WIND RETRIEVAL SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI C1 [Tang, Wenqing; Yueh, Simon; Fore, Alexander; Hayashi, Akiko] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Tang, WQ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628702181 ER PT J AU Xu, XL Tsang, L Chang, WM Yueh, S AF Xu, Xiaolan Tsang, Leung Chang, Wenmo Yueh, Simon GP IEEE TI Bicontinuous DMRT Model Extracted from Multi-size QCA with Application to Terrestrial Snowpack SO 2014 XXXITH URSI GENERAL ASSEMBLY AND SCIENTIFIC SYMPOSIUM (URSI GASS) LA English DT Proceedings Paper CT 29th URSI General Assembly and Scientific Symposium (URSI GASS) CY AUG 16-23, 2014 CL Beijing, PEOPLES R CHINA SP URSI ID SURFACE AB In terrestrial snow, the ice particles are irregular and densely packed together. At microwave frequencies (X-band to Ka-band), there are thousands of ice grains packed within one-wavelength cube. The interaction of the propagation wave and ice particles is coherent. The bicontinuous model is using computer-generated samples to construct the snow microstructures and numerically solve the Maxwell equations to include coherent wave and incoherent wave. There are two input parameters in the model, the scale parameter zeta and the size distribution parameter b. We related those two inputs with the ground measurement by comparing scattering coefficient of the bicontinuous model and multiple size spheres model. In the multi-size sphere model, the modified gamma distribution is used to describe size distribution of the different spheres. The scattering properties of the multi-size models are calculated by quasi-crystalline approximation (QCA). The incoherent wave is calculated with the distorted Born approximation in terms of the T-matrix and Fourier transform of the Percus-Yevick (PY) cross-pair distribution function. The scale parameter is related to the mean size of the ice particles. Therefore we can extract the size distribution parameter b of the bicontinuous model from the multi-size QCA by comparing the scattering coefficients. C1 [Xu, Xiaolan; Yueh, Simon] Jet Prop Lab, Pasadena, CA 91109 USA. [Tsang, Leung; Chang, Wenmo] Univ Washington, Dept Elect Engn, Seattle, WA 98195 USA. RP Xu, XL (reprint author), Jet Prop Lab, M-S 300-233, Pasadena, CA 91109 USA. EM xiaolan.xu@jpl.nasa.gov; tsang1@uw.edu; wmchang@uw.edu; simon.yueh@jpl.nasa.gov NR 8 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-4673-5225-3 PY 2014 PG 3 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA BE0QU UT WOS:000366628702143 ER PT J AU Yang, GW Khurshid, S Person, S Rungta, N AF Yang, Guowei Khurshid, Sarfraz Person, Suzette Rungta, Neha BE Jalote, P Briand, L VanderHoek, A TI Property Differencing for Incremental Checking SO 36TH INTERNATIONAL CONFERENCE ON SOFTWARE ENGINEERING (ICSE 2014) LA English DT Proceedings Paper CT 36th International Conference on Software Engineering (ICSE) CY MAY 31-JUN 07, 2014-2015 CL Hyderabad, INDIA SP Accenture, HCL, SAP, Google, IBM, Fonds Natl Rech Luxembourg, Bosch, Progress, Talent Sprint, CA Technologies, S&P Capital IQ, McGraw Hill Financial, Broadridge, Assoc Comp Machinery, SIGSOFT, iSoft, IEEE Comp Soc, Tech Council Software Engn, SIGSE, IIID DE Incremental symbolic execution; assertions; change -impact analysis; Symbolic PathFinder; Daikon ID MODEL CHECKING; VERIFICATION AB This paper introduces iProperty, a novel approach that facilitates incremental checking of programs based on a property differencing technique. Specifically, iProperty aims to reduce the cost of checking properties as they are initially developed and as they co-evolve with the program. The key novelty of iProperty is to compute the differences between the new and old versions of expected properties to reduce the number and size of the properties that need to be checked during the initial development of the properties. Furthermore, property differencing is used in synergy with program behavior differencing techniques to optimize common regression scenarios, such as detecting regression errors or checking feature additions for conformance to new expected properties. Experimental results in the context of symbolic execution of Java programs annotated with properties written as assertions show the effectiveness of iProperty in utilizing change information to enable more efficient checking. C1 [Yang, Guowei] Texas State Univ, Dept Comp Sci, San Marcos, TX 78666 USA. [Khurshid, Sarfraz] Univ Texas Austin, Dept Elect & Comp Engn, Austin, TX 78712 USA. [Person, Suzette] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Rungta, Neha] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Yang, GW (reprint author), Texas State Univ, Dept Comp Sci, San Marcos, TX 78666 USA. EM gyang@txstate.edu; khurshid@utexas.edu; suzette.person@nasa.gov; neha.s.rungta@nasa.gov NR 60 TC 3 Z9 3 U1 0 U2 0 PU ASSOC COMPUTING MACHINERY PI NEW YORK PA 1515 BROADWAY, NEW YORK, NY 10036-9998 USA BN 978-1-4503-2756-5 PY 2014 BP 1059 EP 1070 DI 10.1145/2568225.2568319 PG 12 WC Computer Science, Software Engineering SC Computer Science GA BG3AP UT WOS:000387829200093 ER PT J AU Sarma, A Branchaud, J Dwyer, MB Person, S Rungta, N AF Sarma, Anita Branchaud, Josh Dwyer, Matthew B. Person, Suzette Rungta, Neha BE Jalote, P Briand, L VanDerHoek, A TI Development Context Driven Change Awareness and Analysis Framework SO 36TH INTERNATIONAL CONFERENCE ON SOFTWARE ENGINEERING (ICSE COMPANION 2014) LA English DT Proceedings Paper CT 36th International Conference on Software Engineering ((ICSE Companion) CY MAY 31-JUN 07, 2014-2015 CL Hyderabad, INDIA SP TATA Consultency Services, Infosys, Microsoft Res, Accenture, HCL, SAP, Google, IBM, Fonds Natl Rech Luxembourg, Bosch, Progress, Talent Sprint, CA Technologies, S&P Capital IQ, McGraw Hill Financial, Broadridge, Assoc Comp Machinery, SIGSOFT, iSoft, IEEE Comp Soc, Tech Council Software Engn, SIGSE, IIID DE Verification; Algorithms; Change impact analysis; distributed software development; change awareness; conflict prediction AB Recent work on workspace monitoring allows conflict prediction early in the development process, however, these approaches mostly use syntactic differencing techniques to compare different program versions. In contrast, traditional change-impact analysis techniques analyze related versions of the program only after the code has been checked into the master repository. We propose a novel approach, DeCAF (Development Context Analysis Framework), that leverages the development context to scope a change impact analysis technique. The goal is to characterize the impact of each developer on other developers in the team. There are various client applications such as task prioritization, early conflict detection, and providing advice on testing that can bene fit from such a characterization. The DeCAF framework leverages information from the development context to bound the iDiSE change impact analysis technique to analyze only the parts of the code base that are of interest. Bounding the analysis can enable DeCAF to efficiently compute the impact of changes using a combination of program dependence and symbolic execution based approaches. C1 [Sarma, Anita; Branchaud, Josh; Dwyer, Matthew B.] Univ Nebraska, Lincoln, NE 68588 USA. [Person, Suzette] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Rungta, Neha] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Sarma, A (reprint author), Univ Nebraska, Lincoln, NE 68588 USA. EM asarma@cse.unl.edu; jbrancha@cse.unl.edu; dwyer@cse.unl.edu; suzette.person@nasa.gov; neha.s.rungta@nasa.gov NR 10 TC 0 Z9 0 U1 0 U2 0 PU ASSOC COMPUTING MACHINERY PI NEW YORK PA 1515 BROADWAY, NEW YORK, NY 10036-9998 USA BN 978-1-4503-2768-8 PY 2014 BP 404 EP 407 DI 10.1145/2591062.2591100 PG 4 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BF4GR UT WOS:000380902900049 ER PT J AU Wang, YR Person, S Elbaum, S Dwyer, MB AF Wang, Yurong Person, Suzette Elbaum, Sebastian Dwyer, Matthew B. BE Jalote, P Briand, L VanDerHoek, A TI A Framework to Advise Tests using Tests SO 36TH INTERNATIONAL CONFERENCE ON SOFTWARE ENGINEERING (ICSE COMPANION 2014) LA English DT Proceedings Paper CT 36th International Conference on Software Engineering ((ICSE Companion) CY MAY 31-JUN 07, 2014-2015 CL Hyderabad, INDIA SP TATA Consultency Services, Infosys, Microsoft Res, Accenture, HCL, SAP, Google, IBM, Fonds Natl Rech Luxembourg, Bosch, Progress, Talent Sprint, CA Technologies, S&P Capital IQ, McGraw Hill Financial, Broadridge, Assoc Comp Machinery, SIGSOFT, iSoft, IEEE Comp Soc, Tech Council Software Engn, SIGSE, IIID DE Automated test generation; regression testing AB Tests generated by different approaches can form a rich body of information about the system under test (SUT), which can then he used to amplify the power of test suites. Diversity in test representations, however, creates;to obstacle to extracting and using this information. In this work, we introduce a test advice framework which enables extraction and application of information contained in existing tests to help improve other tests or test generation techniques. Our framework aims to 1) define a simple., yet expressive test case language so that different types of tests can be represented using a unified language, and 2) define an advice extraction function that enables the elicitation and application of the information encoded in a set of test cases. Preliminary results show how test advice can be used to generate amplified test suites with higher code coverage and improved mutants killed scores over the original test suite. C1 [Wang, Yurong; Elbaum, Sebastian; Dwyer, Matthew B.] Univ Nebraska, Lincoln, NE 68588 USA. [Person, Suzette] NASA LaRC, Hampton, VA 23681 USA. RP Wang, YR (reprint author), Univ Nebraska, Lincoln, NE 68588 USA. EM ywang@cse.unl.edu; suzette.person@nasa.gov; elbaum@cse.unl.edu; dwyer@cse.unl.edu NR 10 TC 0 Z9 0 U1 0 U2 0 PU ASSOC COMPUTING MACHINERY PI NEW YORK PA 1515 BROADWAY, NEW YORK, NY 10036-9998 USA BN 978-1-4503-2768-8 PY 2014 BP 440 EP 443 DI 10.1145/2591062.2591106 PG 4 WC Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BF4GR UT WOS:000380902900058 ER PT B AU Gabb, TP Telesman, J Banik, A McDevitt, E AF Gabb, Tim P. Telesman, Jack Banik, Anthony McDevitt, Erin BE Ott, E Banik, A Andersson, J Dempster, I Gabb, T Groh, J Heck, K Helmink, R Liu, X WusatowskaSarnek, A TI USE OF SLOW STRAIN RATE TENSILE TESTING TO ASSESS THE ABILITY OF SEVERAL SUPERALLOYS TO RESIST ENVIRONMENTALLY-ASSISTED INTERGRANULAR CRACKING SO 8TH INTERNATIONAL SYMPOSIUM ON SUPERALLOY 718 AND DERIVATIVES LA English DT Proceedings Paper CT 8th International Symposium on Superalloy 718 and Derivatives CY SEP 28-OCT 01, 2014 CL Pittsburgh, PA SP Minerals, Met & Mat Soc DE Disk; environment; intergranular; tensile; fatigue AB Intergranular fatigue crack initiation and growth due to environmental degradation, especially at notched features, can often limit the fatigue life of disk superalloys at high temperatures. For clear comparisons, the effects of alloy composition on cracking in air needs to be understood and compared separately from variables associated with notches and cracks such as effective stress concentration, plastic flow, stress relaxation, and stress redistribution. The objective of this study was to attempt using simple tensile tests of specimens with uniform gage sections to compare the effects of varied alloy composition on environment-assisted cracking of several powder metal and cast and wrought superalloys including ME3, LSHR, Udimet 720 (TM), ATI 718Plus (R) alloy, Haynes 282 (TM), and Inconel 740 (TM). Slow and fast strain-rate tensile tests were found to be a useful tool to compare propensities for intergranular surface crack initiation and growth. The effects of composition and heat treatment on tensile fracture strain and associated failure modes were compared. Environment interactions were determined to often limit ductility, by promoting intergranular surface cracking. The response of various superalloys and heat treatments to slow strain rate tensile testing varied substantially, showing that composition and microstructure can significantly influence environmental resistance to cracking. C1 [Gabb, Tim P.; Telesman, Jack] NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA. [Banik, Anthony; McDevitt, Erin] ATI Allvac, Monroe, NC 28110 USA. RP Gabb, TP (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA. NR 16 TC 1 Z9 1 U1 3 U2 3 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA BN 978-1-119-01685-4; 978-1-119-01680-9 PY 2014 BP 697 EP 712 PG 16 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA BE6PQ UT WOS:000374558400054 ER PT B AU Tuccella, P Curci, G Crumeyrolle, S Visconti, G AF Tuccella, Paolo Curci, Gabriele Crumeyrolle, Suzanne Visconti, Guido BE Steyn, D Mathur, R TI Modeling of Aerosol Indirect Effects with WRF/Chem over Europe SO AIR POLLUTION MODELING AND ITS APPLICATION XXIII SE Springer Proceedings in Complexity LA English DT Proceedings Paper CT 33rd International Technical Meeting (ITM) on Air Pollution Modelling and Its Application CY AUG 27-31, 2013 CL US Environm Protect Agcy, Miami, FL SP Univ British Columbia, Environm Canada HO US Environm Protect Agcy AB WRF/Chem has been updated in order to simulate the aerosol indirect effects using a new parameterization for production of secondary organic aerosol. The model has been evaluated over North Sea among the ATR-42 aircraft measurements of aerosol and cloud issued in frame European Integrated project on Aerosol Cloud Climate and Air Quality Interactions (EUCAARI). WRF/Chem tends to overpredict the number of condensation nuclei. Simulated liquid water content shows a bias of +15 %. Predicted cloud droplet number concentration is overestimated and radius effective droplet is underestimated. C1 [Tuccella, Paolo; Curci, Gabriele; Visconti, Guido] Univ Aquila, CETEMPS Dip Sci Fis & Chim, Laquila, Italy. [Crumeyrolle, Suzanne] Univ Blaise Pascal, Lab Meteorol Phys, UMR 6016, Clermont Ferrand, France. [Crumeyrolle, Suzanne] NASA, Langley Res Ctr, Hampton, VA 23666 USA. RP Tuccella, P (reprint author), Univ Aquila, CETEMPS Dip Sci Fis & Chim, Laquila, Italy. EM paolo.tuccella@aquila.infn.it; gabriele.curci@aquila.infn.it FU Italian Space Agency in the frame of the PRIMES [I/017/11/0] FX The work was founded by Italian Space Agency in the frame of the PRIMES (contract I/017/11/0) projects. The authors gratefully acknowledge Denier van der Gon and TNO to make available the anthropogenic emissions. The authors are grateful to NOAA for availability of the supercomputer to run the model. They also thank Fred Burnet, Bruno Piguet and Vincent Puygrenier to provide EUCAARI- IMPACT data. NR 11 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-319-04379-1; 978-3-319-04378-4 J9 SPRINGER PR COMPLEX PY 2014 BP 91 EP 95 DI 10.1007/978-3-319-04379-1_15 PG 5 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA BG8LE UT WOS:000392403800015 ER PT B AU Neu, JL Osterman, G Eldering, A Pinder, R McQueen, J Tang, YH AF Neu, Jessica L. Osterman, Gregory Eldering, Annmarie Pinder, Rob McQueen, Jeff Tang, Youhua BE Steyn, D Mathur, R TI Evaluating the Vertical Distribution of Ozone and Its Relationship to Pollution Events in Air Quality Models Using Satellite Data SO AIR POLLUTION MODELING AND ITS APPLICATION XXIII SE Springer Proceedings in Complexity LA English DT Proceedings Paper CT 33rd International Technical Meeting (ITM) on Air Pollution Modelling and Its Application CY AUG 27-31, 2013 CL US Environm Protect Agcy, Miami, FL SP Univ British Columbia, Environm Canada HO US Environm Protect Agcy AB Most regional scale models that are used for air quality forecasts and ozone source attribution do not adequately capture the distribution of ozone in the mid-and upper troposphere, but it is unclear how this shortcoming relates to their ability to simulate surface ozone. We combine ozone profile data from the NASA Earth Observing System (EOS) Tropospheric Emission Spectrometer (TES) and a new joint product from TES and the Ozone Monitoring Instrument along with ozonesonde measurements and EPA AirNow ground station ozone data to examine air quality events during August 2006 in the Community Multi-Scale Air Quality (CMAQ) and National Air Quality Forecast Capability (NAQFC) models. We present both aggregated statistics and case-study analyses with the goal of assessing the relationship between the models' ability to reproduce surface air quality events and their ability to capture the vertical distribution of ozone. We find that the models lack the mid-tropospheric ozone variability seen in TES and the ozonesonde data, and discuss future work to determine the conditions under which this variability appears to be important for surface air quality. C1 [Neu, Jessica L.; Osterman, Gregory; Eldering, Annmarie] CALTECH, NASA, Jet Prop Lab, Earth Atmospher Sci Div, Pasadena, CA 91109 USA. [Pinder, Rob] US EPA, Atmospher Modeling & Anal Div, Res Triangle Pk, NC 27711 USA. [McQueen, Jeff; Tang, Youhua] Natl Weather Service, NOAA, Ctr Weather & Climate Predict, Natl Ctr Environm Predict, Camp Springs, MD 20748 USA. RP Neu, JL (reprint author), CALTECH, NASA, Jet Prop Lab, Earth Atmospher Sci Div, Pasadena, CA 91109 USA. EM jessica.l.neu@jpl.nasa.gov; gregory.b.osterman@jpl.nasa.gov; annmarie.eldering@jpl.nasa.gov; pinder.rob@epa.gov; jeff.mcqueen@noaa.gov; youhua.tang@noaa.gov NR 8 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-319-04379-1; 978-3-319-04378-4 J9 SPRINGER PR COMPLEX PY 2014 BP 575 EP 580 DI 10.1007/978-3-319-04379-1__95 PG 6 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA BG8LE UT WOS:000392403800095 ER PT B AU Kishcha, P da Silva, AM Starobinets, B Alpert, P AF Kishcha, Pavel da Silva, Arlindo M. Starobinets, Boris Alpert, Pinhas BE Steyn, D Mathur, R TI Modeling of Air Pollution over the Ganges Basin and North-West Bay of Bengal in the Early Post-monsoon Season Using the NASA GEOS-5 Model SO AIR POLLUTION MODELING AND ITS APPLICATION XXIII SE Springer Proceedings in Complexity LA English DT Proceedings Paper CT 33rd International Technical Meeting (ITM) on Air Pollution Modelling and Its Application CY AUG 27-31, 2013 CL US Environm Protect Agcy, Miami, FL SP Univ British Columbia, Environm Canada HO US Environm Protect Agcy AB The NASA GEOS-5 model was used to extend the MERRA reanalysis with five atmospheric aerosol components (sulfates, organic carbon, black carbon, desert dust, and sea-salt). The obtained eight-year (2002-2009) MERRA-driven aerosol reanalysis (MERRAero) dataset was applied to the study of aerosol optical thickness (AOT) trends over the Ganges basin and north-west Bay of Bengal (BoB) in the early post-monsoon season. In October, in the absence of aerosol sources in north-west Bay of Bengal (BoB), MERRAero showed increasing AOT trends over north-west BoB exceeding those over the east of the Ganges basin. Various aerosol components showed strong increasing AOT trends over north-west BoB. Our analysis showed that the AOT trends over north-west BoB were reproduced by GEOS-5, not because of MODIS AOT assimilation, but because of the model capability of reproducing meteorological factors contributing to AOT trends. The following factors contributed to the increasing AOT trend over the area in question in October: an increasing number of days when prevailing winds blew from land to sea, resulting in a drier environment and an increase in air pollution over north-west BoB; wind convergence was observed over north-west BoB causing the accumulation of aerosol particles over that region, when prevailing winds blew from land to sea. C1 [Kishcha, Pavel; Starobinets, Boris; Alpert, Pinhas] Tel Aviv Univ, Dept Geophys Atmospher & Planetary Sci, Tel Aviv, Israel. [da Silva, Arlindo M.] NASA, Global Modeling & Assimilat Off, GSFC, Greenbelt, MD USA. RP Kishcha, P (reprint author), Tel Aviv Univ, Dept Geophys Atmospher & Planetary Sci, Tel Aviv, Israel. EM pavel@cyclone.tau.ac.il FU German Helmholtz Association FX This study was made with support from and in cooperation with the international Virtual Institute DESERVE (Dead Sea Research Venue), funded by the German Helmholtz Association. NR 4 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-319-04379-1; 978-3-319-04378-4 J9 SPRINGER PR COMPLEX PY 2014 BP 593 EP 598 DI 10.1007/978-3-319-04379-1__98 PG 6 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA BG8LE UT WOS:000392403800098 ER PT S AU Goodson, TD Antreasian, PG Bhat, RS Chung, MK Criddle, KE Hatch, SJ Jefferson, DC Lau, EL Roncoli, RB Ryne, MS Sweetser, TH You, TH Young, BT Wong, MC Kangas, JA Wen, HY AF Goodson, Troy D. Antreasian, Peter G. Bhat, Ram S. Chung, Min-Kun Criddle, Kevin E. Hatch, Sara J. Jefferson, David C. Lau, Eunice L. Roncoli, Ralph B. Ryne, Mark S. Sweetser, Theodore H. You, Tung-Han Young, Brian T. Wong, Mau C. Kangas, Julie A. Wen, Hui Ying BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI NAVIGATION OF THE GRAIL SPACECRAFT PAIR THROUGH THE EXTENDED MISSION AT THE MOON SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB The GRAIL extended mission (XM) dramatically expands the scope of GRAIL's gravity science investigation by flying the pair of spacecraft at the lowest orbit the flight team can safely support. From the perspective of the Navigation team, the low orbit altitude introduces new challenges. At this lower altitude, navigation is more sensitive to higher-order terms of the gravity field so that orbit determination solutions are more difficult and there is less certainty of achieving maneuver targets. This paper reports on the strategy and performance of the Navigation system for GRAIL's XM. On a weekly basis, the Navigation team provided reference trajectory updates, designed three maneuvers, and reconstructed the execution of those maneuvers. In all, the XM involved 55 planned maneuvers; five were canceled. The results of the Navigation team's efforts, in terms of maintaining the reference-trajectory targets, satisfying requirements, and achieving desired separation distances, are assessed. C1 [Goodson, Troy D.; Antreasian, Peter G.; Bhat, Ram S.; Chung, Min-Kun; Criddle, Kevin E.; Hatch, Sara J.; Jefferson, David C.; Lau, Eunice L.; Roncoli, Ralph B.; Ryne, Mark S.; Sweetser, Theodore H.; You, Tung-Han; Young, Brian T.; Wong, Mau C.; Kangas, Julie A.; Wen, Hui Ying] CALTECH, Jet Prop Lab, Sect 343, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Goodson, TD (reprint author), CALTECH, Jet Prop Lab, Sect 343, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 135 EP 159 PN I-III PG 25 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600008 ER PT S AU Chung, MKJ AF Chung, Min-Kun J. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI GRAIL TCM-5 GO/NO-GO: DEVELOPING LUNAR ORBIT INSERTION CRITERIA SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB The Gravity Recovery and Interior Laboratory (GRAIL) mission successfully completed mapping the Moon's gravity field to an unprecedented level. The mission success was critically dependent on the success of the Lunar Orbit Insertion (LOI). It was somewhat unfamiliar as it involved an elliptical approach from a low-energy trans-lunar cruise trajectory via Sun-Earth three-body region rather than a more conventional hyperbolic approach from a direct Earth-to Moon transfer. In addition, how its delivery dispersion affected the science formation of the two spacecraft was not well understood. In this paper we establish a set of LOI criteria to meet all the requirements and we use these criteria to establish Go/No-Go boundaries of the last, statistical Trajectory Correction Maneuvers (TCM-5s) for operations. In the end both spacecraft were found to be within the established boundaries and TCM-5s of both spacecraft were cancelled. C1 [Chung, Min-Kun J.] CALTECH, Jet Prop Lab, M-S 301-121,4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Chung, MKJ (reprint author), CALTECH, Jet Prop Lab, M-S 301-121,4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 161 EP 179 PN I-III PG 19 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600009 ER PT S AU Wawrzyniak, GG Carpenter, JR Mattern, DJ Williams, TW Ottenstein, NA Jones, BA AF Wawrzyniak, Geoffrey G. Carpenter, J. Russell Mattern, Daniel J. Williams, Trevor W. Ottenstein, Neil A. Jones, Brandon A. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI CONJUNCTION ASSESSMENT CONCEPT OF OPERATIONS FOR THE MAGNETOSPHERIC MULTISCALE (MMS) MISSION SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB While collisions between the four MMS spacecraft are unlikely, the consequence of a collision between two spacecraft is mission failure. The MMS mission design requirements state that no more than 1 in 1000 unsafe close approaches may remain undetected. However, mission operators and the science team require that collision risk mitigation maneuvers are not excessively frequent and hence that no more than 1 in 20 collision alarms may occur when the conjunction is safe. These competing requirements-collision avoidance conservatism vs. unnecessary interruption of science activities and inconvenience to the ground system-induce the conjunction assessment Operations Concept for the MMS mission. C1 [Wawrzyniak, Geoffrey G.; Mattern, Daniel J.; Ottenstein, Neil A.] Ai Solut Inc, Mission Serv Div, Lanham, MD 20706 USA. [Carpenter, J. Russell; Williams, Trevor W.] NASA, Goddard Space Flight Ctr, Nav & Mission Design Branch, Greenbelt, MD 20771 USA. [Jones, Brandon A.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA. RP Wawrzyniak, GG (reprint author), Ai Solut Inc, Mission Serv Div, Lanham, MD 20706 USA. NR 25 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 181 EP 200 PN I-III PG 20 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600010 ER PT S AU Wagner, SV Arrieta, J Hahn, Y Stumpf, PW Valerino, PN Wong, MC AF Wagner, Sean V. Arrieta, Juan Hahn, Yungsun Stumpf, Paul W. Valerino, Powtawche N. Wong, Mau C. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI CASSINI SOLSTICE MISSION MANEUVER EXPERIENCE: YEAR THREE SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB The Solstice Mission is the final extension of the Cassini spacecraft's tour of Saturn and its moons. To accommodate an end of mission in 2017, the maneuver decision process continues to be refined. This process includes determining whether a maneuver is performed or cancelled, choosing the engine to use for execution, and deciding the maneuver design strategy. Additionally, the Cassini Project now prioritizes saving propellant over minimizing maneuver cycles. This paper highlights 30 maneuvers planned from June 2012 through July 2013, targeted to nine Titan flybys and the final Rhea encounter in the mission. To maintain the prescribed trajectory or to preserve downstream Delta V, 27 of the 30 maneuvers were performed. Through execution-error modeling and analysis, the majority of the observed magnitude biases in maneuver executions were removed either through a flight parameter change or within the maneuver design process starting in August 2012. These execution error model updates are discussed and assessments of maneuver performance following the model and maneuver execution changes are also presented. C1 [Wagner, Sean V.] CALTECH, Jet Prop Lab, Mail Stop 230-205,4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Wong, Mau C.] CALTECH, Jet Prop Lab, Flight Path Control Grp & Cassini Nav Team, Pasadena, CA 91109 USA. RP Wagner, SV (reprint author), CALTECH, Jet Prop Lab, Mail Stop 230-205,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Sean.V.Wagner@jpl.nasa.gov NR 20 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 223 EP + PN I-III PG 2 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600013 ER PT S AU Cianciolo, AD Maddock, RW Prince, JL Bowes, A Powell, RW White, JP Tolson, R O'Shaughnessy, D Curelli, D AF Cianciolo, Alicia D. Maddock, Robert W. Prince, Jill L. Bowes, Angela Powell, Richard W. White, Joseph P. Tolson, Robert O'Shaughnessy, Daniel Curelli, David BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI AUTONOMOUS AEROBRAKING DEVELOPMENT SOFTWARE: PHASE 2 SUMMARY SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB NASA has used aerobraking at Mars and Venus to reduce the fuel required to deliver a spacecraft into a desired orbit compared to an all-propulsive solution. Although aerobraking reduces the propellant, it does so at the expense of mission duration, large staff, and DSN coverage. These factors make aerobraking a significant cost element in the mission design. By moving on-board the current ground-based tasks of ephemeris determination, atmospheric density estimation, and maneuver sizing and execution, a flight project would realize significant cost savings. The NASA Engineering and Safety Center (NESC) sponsored Phase 1 and 2 of the Autonomous Aerobraking Development Software (AADS) study, which demonstrated the initial feasibility of moving these current ground-based functions to the spacecraft. This paper highlights key state-of-the-art advancements made in the Phase 2 effort to verify that the AADS algorithms are accurate, robust and ready to be considered for application on future missions that utilize aerobraking. The advancements discussed herein include both model updates and simulation and benchmark testing. Rigorous testing using observed flight atmospheres, operational environments and statistical analysis characterized the AADS operability in a perturbed environment. C1 [Cianciolo, Alicia D.; Maddock, Robert W.; Prince, Jill L.; Bowes, Angela] NASA LaRC, AFESB, Hampton, VA 23681 USA. [Powell, Richard W.; White, Joseph P.] Analyt Mech & Associates, AFESB, Hampton, VA 23681 USA. [Tolson, Robert] Natl Inst Aerosp, Hampton, VA 23666 USA. [O'Shaughnessy, Daniel; Curelli, David] Johns Hopkins Appl Phys Lab, Dept Space, Laurel, MD 20723 USA. RP Cianciolo, AD (reprint author), NASA LaRC, AFESB, Hampton, VA 23681 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 521 EP 536 PN I-III PG 16 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600031 ER PT S AU Guerrant, D Lawrence, D Heaton, A AF Guerrant, Daniel Lawrence, Dale Heaton, Andrew BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI EARTH ESCAPE CAPABILITIES OF THE HELIOGYRO SOLAR SAIL SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB The heliogyro is a spinning solar sail architecture with the sail membrane partitioned into extremely high aspect ratio "blades". It can pitch these blades to generate attitude control moments (similar to a helicopter) or change the direction of thrust. The heliogyro's performance for various Earth escape trajectories is evaluated, accounting for reasonable slew rates and thrust variation during attitude maneuvers. Additionally, several strategies are proposed that improve upon those in the literature. In most cases, the heliogyro's angular momentum is found to be too high to follow Earth escape trajectories that precess its spin axis. Fortunately, an improved escape strategy is found that is 87% as good at the best ideal trajectory, and it does not precess the spin axis. This strategy would escape from geostationary orbit in approximately 150 days. C1 [Guerrant, Daniel; Lawrence, Dale] Univ Colorado, Aerosp Engn Sci, ECOT 634, 429 UCB, Boulder, CO 80309 USA. [Heaton, Andrew] NASA, Marshall Space Flight Ctr, Guidance Nav & Control Grp, EV 42, Huntsville, AL 35812 USA. RP Guerrant, D (reprint author), Univ Colorado, Aerosp Engn Sci, ECOT 634, 429 UCB, Boulder, CO 80309 USA. NR 18 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 639 EP 658 PN I-III PG 20 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600038 ER PT S AU Parker, JS Leonard, JM Anderson, RL Born, GH AF Parker, Jeffrey S. Leonard, Jason M. Anderson, Rodney L. Born, George H. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI LIAISON-SUPPLEMENTED NAVIGATION OF A CREWED VEHICLE IN A LUNAR HALO ORBIT SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB This paper offers an early examination of the challenges of navigating a crewed vehicle, with all of the associated unmodeled accelerations that arise from the crew's activities, in an orbit about the Earth-Moon L2 point. The combination of the unstable nature of libration orbits with the lack of acceleration knowledge makes the station keeping strategy challenging. It is found that a combination of ground tracking and satellite-to-satellite tracking produces the most favorable navigation accuracy. This paper examines the costs and benefits of applying LiAISON (Linked Autonomous Interplanetary Satellite Orbit Navigation) to a crewed mission in an unstable L2 orbit. C1 [Parker, Jeffrey S.; Leonard, Jason M.; Born, George H.] Univ Colorado, Colorado Ctr Astrodynam Res, 431 UCB, Boulder, CO 80309 USA. [Anderson, Rodney L.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Parker, JS (reprint author), Univ Colorado, Colorado Ctr Astrodynam Res, 431 UCB, Boulder, CO 80309 USA. OI Anderson, Rodney/0000-0001-5336-2775 FU National Aeronautics and Space Administration FX .The research presented in this paper has been partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 27 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 1113 EP + PN I-III PG 4 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600066 ER PT S AU Haapala, AF Vaquero, M Pavlak, TA Howell, KC Folta, DC AF Haapala, Amanda F. Vaquero, Mar Pavlak, Thomas A. Howell, Kathleen C. Folta, David C. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI TRAJECTORY SELECTION STRATEGY FOR TOURS IN THE EARTH-MOON SYSTEM SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA ID RESTRICTED 3-BODY PROBLEM; PERIODIC-ORBITS AB As mission requirements become increasingly complex, improved flexibility in mission design tools is vital. Strategies that offer interactive access to a variety of solutions supply an enhanced perspective of the design space. In this investigation, interactive and automated trajectory design tools are examined for applications in the Earth-Moon system. Operating within a graphical user interface, these tools offer a composite view of multi-body orbits possessing a variety of characteristics, and facilitate the assembly of end-to-end mission designs via interactive selection of trajectory arcs with desirable characteristics. Final designs are imported into NASA's General Mission Analysis Tool for validation and further access in a mission setting. C1 [Haapala, Amanda F.; Vaquero, Mar; Pavlak, Thomas A.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. [Howell, Kathleen C.] Purdue Univ, Sch Aeronaut & Astronaut, Aeronaut & Astronaut, W Lafayette, IN 47907 USA. [Folta, David C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Haapala, AF (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. NR 25 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 1151 EP 1170 PN I-III PG 20 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600068 ER PT S AU Llanos, PJ Hintz, GR Lo, MW Miller, JK AF Llanos, Pedro J. Hintz, Gerald R. Lo, Martin W. Miller, James K. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI POWERED HETEROCLINIC, HOMOCLINIC CONNECTIONS BETWEEN THE SUN-EARTH TRIANGULAR POINTS AND QUASI-SATELLITE ORBITS FOR SOLAR OBSERVATIONS SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB Investigation of new orbit geometries exhibits a very attractive behavior for a spacecraft to monitor space weather coming from the Sun. Several orbit transfer mechanisms are analyzed as potential alternatives to monitor solar activity such as a sub-solar orbit or quasi-satellite orbit and short and long heteroclinic and homoclinic connections between the triangular points L-4 and L-5 and the collinear point L-3 of the Circular Restricted Three-Body Problem (CRTBP) in the Sun-Earth system. C1 [Llanos, Pedro J.] GMV Space & Def SA, Flight Mech Grp, Madrid 28760, Spain. [Hintz, Gerald R.] Univ So Calif, Astronaut Engn Dept, Los Angeles, CA 90089 USA. [Lo, Martin W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Llanos, PJ (reprint author), GMV Space & Def SA, Flight Mech Grp, Madrid 28760, Spain. NR 14 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 1215 EP 1229 PN I-III PG 15 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600071 ER PT S AU Anderson, RL Campagnola, S Lantoine, G AF Anderson, Rodney L. Campagnola, Stefano Lantoine, Gregory BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI BROAD SEARCH FOR UNSTABLE RESONANT ORBITS IN THE PLANAR CIRCULAR RESTRICTED THREE-BODY PROBLEM SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA ID DYNAMICAL-SYSTEMS ANALYSIS; 2ND SPECIES SOLUTIONS; CAPTURE; FLYBYS; DESIGN; COMETS; GRAPH AB Unstable resonant orbits in the circular restricted three-body problem have increasingly been used for trajectory design using optimization and invariant manifold techniques. In this study, several methods for computing these unstable resonant orbits are explored including flyby maps, continuation from two-body models, and grid searches. Families of orbits are computed focusing on the Jupiter-Europa system, and their characteristics are explored. Different parameters such as period and stability are examined for each set of resonant orbits, and the continuation of several specific orbits is explored in more detail. C1 [Campagnola, Stefano] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Tokyo, Japan. [Anderson, Rodney L.; Lantoine, Gregory] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Anderson, RL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Anderson, Rodney/0000-0001-5336-2775 NR 49 TC 0 Z9 0 U1 1 U2 2 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 1231 EP + PN I-III PG 3 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600072 ER PT S AU Strange, NJ Landau, DF Longuski, JM AF Strange, Nathan J. Landau, Damon F. Longuski, James M. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI DESIGN OF INITIAL INCLINATION REDUCTION SEQUENCE FOR URANIAN GRAVITY-ASSIST TOURS SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA ID MISSIONS AB Although a gravity-assist tour of the Uranian moons would be desirable component of a Uranus mission, such tours are especially challenging due to its distance from the Sun and the planet's very high obliquity (97.77). The high obliquity means that the initial orbits at Uranus tend to be very highly inclined (60 80), except in the rare case of arrival during the Uranian equinox (the equinoxes occur every 42 years, with the next one in 2049). The long flight time to Uranus means that there may be precious little time left in a mission for inclination reduction flybys to reach the Equatorial plane. This paper presents a method for the design of the initial capture orbit maneuvers to target a satellite v(infinity) that allows for an efficient gravity assist inclination reduction sequence. We also provide an example case for a 2025 mission with a 13-year trajectory to Uranus, a 1-year inclination reduction sequence, and a 2.5 km/s total mission Delta V. C1 [Strange, Nathan J.; Landau, Damon F.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. [Strange, Nathan J.; Longuski, James M.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. RP Strange, NJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. NR 14 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 1469 EP 1485 PN I-III PG 17 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600085 ER PT S AU Folta, D Barbee, BW Englander, J Vaughn, F Lin, TY AF Folta, David Barbee, Brent W. Englander, Jacob Vaughn, Frank Lin, Tzu Yu BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI OPTIMAL ROUND-TRIP TRAJECTORIES FOR SHORT DURATION MARS MISSIONS SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB We describe techniques and results for computing optimal (minimum Initial Mass in Low Earth Orbit (IMLEO)) round-trip trajectories to Mars with total mission duration no greater than one year. The trajectory options surveyed include direct trajectories between Earth and Mars, as well as trajectories that include a Venus gravity assist flyby on the way to Mars, on the way back to Earth, or both. The method of embedded trajectory grids is used to identify the optimal round-trip trajectory solutions without Venus flybys, while a genetic algorithm is employed to identify the optimal solutions that include Venus. The IMLEO required for the mission is further reduced by modeling a pre-positioning of Earth return propellant at Mars via lower energy trajectories in advance of the human portion of the mission, as well as assuming the use of On-Orbit Staging (OOS) in the propulsion system design. Optimal trajectory design results are presented for an array of cases that span ranges of values for various key design parameters including thruster specific impulses, human spacecraft dry mass, and maximum permissible Earth atmospheric entry speed. C1 [Folta, David; Barbee, Brent W.; Englander, Jacob; Vaughn, Frank] NASA, Goddard Space Flight Ctr, Code 595,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Lin, Tzu Yu] Univ Florida, Dept Mech & Aerosp Engn, Gainesville, FL 32611 USA. RP Folta, D (reprint author), NASA, Goddard Space Flight Ctr, Code 595,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM david.c.foita@nasa.gov; brent.w.barbee@nasa.gov; jacob.a.englander@nasa.gov; frank.j.vaughn@nasa.gov; tyl.j.lin@gmail.com NR 15 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 1565 EP 1584 PN I-III PG 20 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600091 ER PT S AU Lantoine, G Broschart, SB Grebow, DJ AF Lantoine, Gregory Broschart, Stephen B. Grebow, Daniel J. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI DESIGN OF QUASI-TERMINATOR ORBITS NEAR PRIMITIVE BODIES SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA ID SATELLITE DYNAMICS; RADIATION PRESSURE; ASTEROIDS AB Quasi-terminator orbits are a class of quasi-periodic orbits around a primitive body that exist in the vicinity of the well-known terminator orbits. The inherent stability of quasi-terminator trajectories and their wide variety of viewing geometries make them a very compelling option for primitive body mapping missions. In this paper, we discuss orbit design methodologies for selection of an appropriate quasi-terminator orbit that would meet the needs of a specific mission. Convergence of these orbits in an eccentric, higher-fidelity model is also discussed with an example mapping orbit design presented for NASA's upcoming OSIRIS-REx mission. C1 [Lantoine, Gregory; Broschart, Stephen B.; Grebow, Daniel J.] CALTECH, Jet Prop Lab, Mission Design & Nav Sect, M-S 301-121,4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Lantoine, G (reprint author), CALTECH, Jet Prop Lab, Mission Design & Nav Sect, M-S 301-121,4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 21 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 1657 EP 1673 PN I-III PG 17 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600096 ER PT S AU Wallace, MS Broschart, S AF Wallace, Mark S. Broschart, Stephen BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI CIRCULAR-ORBIT MAINTENANCE STRATEGIES FOR PRIMITIVE BODY ORBITERS SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB For missions to smaller primitive bodies, solar radiation pressure (SRP) is a significant perturbation to Keplerian dynamics. For most orbits, SRP drives large oscillations in orbit eccentricity, which leads to large perturbations from the irregular gravity field at periapsis. Ultimately, chaotic motion results that often escapes or impacts that body. This paper presents an orbit maintenance strategy to keep the orbit eccentricity small, thus avoiding the destabilizing secondary interaction with the gravity field. An estimate of the frequency and magnitude of the required maneuvers as a function of the orbit and body parameters is derived from the analytic perturbation equations. C1 [Wallace, Mark S.; Broschart, Stephen] CALTECH, Jet Prop Lab, Mission Design & Nav Sect, 4800 Oak Grove Dr,M-S 301-121, Pasadena, CA 91109 USA. RP Wallace, MS (reprint author), CALTECH, Jet Prop Lab, Mission Design & Nav Sect, 4800 Oak Grove Dr,M-S 301-121, Pasadena, CA 91109 USA. NR 3 TC 0 Z9 0 U1 0 U2 2 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 1675 EP 1687 PN I-III PG 13 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600097 ER PT S AU Mortari, D de Dilectis, F D'Souza, C AF Mortari, Daniele de Dilectis, Francesco D'Souza, Christopher BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI IMAGE PROCESSING OF ILLUMINATED ELLIPSOID SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB This paper presents the image processing algorithms (and associated mathematics) of Moon or Earth pictures taken by a visible camera to accurately measure the vector to an observed illuminated body (Moon or Earth). Using a sequence of these vectors it is then possible to perform initial trajectory estimation in cis lunar trajectories. Even though Moon can be considered a sphere and Earth an axial-symmetric ellipsoid, the theory presented is developed for the general case of three-axis ellipsoid. It is proved that, using a pin-hole camera model, the observed image is a projected ellipse that is obtained by the intersection of an elliptical cone with a unit-radius sphere. This paper proves that the observed ellipse center and the body center are displaced by an offset. The paper show how to quantify this offset and how to take it into account in the image processing. The equation of the terminator of a three-axis ellipsoid is also derived. High accuracy estimation of body center and radius is obtained by least-squares using circular and elliptical sigmoid functions. A numerical example and a flowchart is provided to clarify the image processing steps. C1 [Mortari, Daniele; de Dilectis, Francesco] Texas A&M Univ, Aerosp Engn, 746C HR Bright Bldg, College Stn, TX 77843 USA. [D'Souza, Christopher] NASA, GN&C Autonomous Flight Syst Branch, Spacecraft Nav Team, Johnson Space Ctr, Houston, TX 77058 USA. RP Mortari, D (reprint author), Texas A&M Univ, Aerosp Engn, 746C HR Bright Bldg, College Stn, TX 77843 USA. EM MORTARI@TAMU.EDU; F.DE.DILECTIS@NEO.TAMU.EDU; CHRIS.DSOUZA-I@NASA.GOV NR 5 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 2245 EP 2262 PN I-III PG 18 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600132 ER PT S AU Carson, JM Bailey, ES Trawny, N Johnson, AE Roback, VE Amzajerdian, F Werner, RA AF Carson, John M. Bailey, Erik S. Trawny, Nikolas Johnson, Andrew E. Roback, Vincent E. Amzajerdian, Farzin Werner, Robert A. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI OPERATIONS CONCEPT, HARDWARE IMPLEMENTATION AND GROUND-TEST VERIFICATION OF A HAZARD DETECTION SYSTEM FOR AUTONOMOUS AND SAFE PRECISION LUNAR LANDING SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB The Autonomous precision Landing and Hazard detection and Avoidance Technology (ALHAT) project has developed a Hazard Detection System (HDS) for real-time determination of safe landing sites and site-relative navigation during precision landing of a robotic or crewed vehicle. The HDS design was driven by real-time landing-operations requirements to detect 30-cm terrain hazards, locate safe landing sites, and track terrain features under any surface lighting conditions within a 1-hectare region of the Lunar surface starting from a 1-kilometer slant range with a 30 approach angle and a 30-100 m/s descent rate. To achieve the requirements, the FIDS constructs in real time a 10-cm resolution Digital Elevation Model (DEM) and processes it through a Hazard Detection (HD) algorithm to determine safe landing sites. Subsequently, the HDS provides Hazard Relative Navigation (HRN) updates that are correlated with the DEM to provide site-relative position measurements. The current-generation HDS hardware implementation consists of a two-axis gimbaled flash Lidar (Light Detection and Ranging) sensor with a 1 Field of View (FOV) lens and a 128 x 128 pixel detector array, a dedicated Inertial Measurement Unit (IMU) and a custom Compute Element (CE). The Lidar narrow-FOV lens is necessary for providing the DEM resolution from images with the current-generation detector, but it also imposes precision control and knowledge requirements on the HDS and vehicle Navigation during HD and HRN. This paper gives an overview of the HDS design implementation and operations concept to meet these challenging operations objectives, as well as details on the rigorous development and ground-testing campaign to calibrate and align the HDS to achieve the necessary precision pointing. This work has been in preparation for flight tests onboard a helicopter and the NASA Morpheus rocket-propelled, terrestrial flight-test vehicle. C1 [Carson, John M.; Bailey, Erik S.; Trawny, Nikolas; Johnson, Andrew E.] CALTECH, Jet Prop Lab, GN&C Hardware & Testbed Dev Grp, Pasadena, CA 91109 USA. [Roback, Vincent E.] NASA, Langley Res Ctr, Remote Sensing Flight Syst Branch, Hampton, VA 23665 USA. [Amzajerdian, Farzin] NASA, Langley Res Ctr, Laser Remote Sensing Branch, Hampton, VA 23665 USA. [Werner, Robert A.] CALTECH, Jet Prop Lab, Opt Nav Grp, Pasadena, CA USA. RP Carson, JM (reprint author), CALTECH, Jet Prop Lab, GN&C Hardware & Testbed Dev Grp, Pasadena, CA 91109 USA. NR 19 TC 0 Z9 0 U1 0 U2 2 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 2275 EP 2292 PN I-III PG 18 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600134 ER PT S AU Sweetser, TH Vincent, MA AF Sweetser, Theodore H. Vincent, Mark A. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI THE ECCENTRIC BEHAVIOR OF NEARLY FROZEN ORBITS SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB Frozen orbits are orbits which have only short-period changes in their mean eccentricity and argument of periapse, so that they basically keep a fixed orientation within their plane of motion. Nearly frozen orbits are those whose eccentricity and argument of periapse have values close to those of a frozen orbit. We call them "nearly" frozen because their eccentricity vector (a vector whose polar coordinates are eccentricity and argument of periapse) will stay within a bounded distance from the frozen orbit eccentricity vector, circulating around it over time. For highly inclined orbits around the Earth, this distance is effectively constant over time. Furthermore, frozen orbit eccentricity values are low enough that these orbits are essentially eccentric (i.e., off center) circles, so that nearly frozen orbits around Earth are bounded above and below by frozen orbits. C1 [Sweetser, Theodore H.] CALTECH, Jet Prop Lab, Mission Design & Nav Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Vincent, Mark A.] Raytheon, Nav & Mission Design, 299 N Euclid Ave,Suite 500, Pasadena, CA 91101 USA. RP Sweetser, TH (reprint author), CALTECH, Jet Prop Lab, Mission Design & Nav Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 2443 EP 2455 PN I-III PG 13 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600144 ER PT S AU Cianciolo, AD Cantor, B Barnes, J Tyler, D Rafkin, S Chen, A Kass, D Mischna, M Vasavada, AR AF Cianciolo, Alicia D. Cantor, Bruce Barnes, Jeff Tyler, Daniel, Jr. Rafkin, Scot Chen, Allen Kass, David Mischna, Michael Vasavada, Ashwin R. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI ATMOSPHERE ASSESSMENT FOR MARS SCIENCE LABORATORY ENTRY, DESCENT AND LANDING OPERATIONS SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB On August 6, 2012, the Mars Science Laboratory rover, Curiosity, successfully landed on the surface of Mars. The Entry, Descent and Landing (EDL) sequence was designed using atmospheric conditions estimated from mesoscale numerical models. The models, developed by two independent organizations (Oregon State University and the Southwest Research Institute), were validated against observations at Mars from three prior years. In the weeks and days before entry, the MSL "Council of Atmospheres" (CoA), a group of atmospheric scientists and modelers, instrument experts and EDL simulation engineers, evaluated the latest Mars data from orbiting assets including the Mars Reconnaissance Orbiter's Mars Color Imager (MARCI) and Mars Climate Sounder (MCS), as well as Mars Odyssey's Thermal Emission Imaging System (THEMIS). The observations were compared to the mesoscale models developed for EDL performance simulation to determine if a spacecraft parameter update was necessary prior to entry. This paper summarizes the daily atmosphere observations and comparison to the performance simulation atmosphere models. Options to modify the atmosphere model in the simulation to compensate for atmosphere effects are also presented. Finally, a summary of the CoA decisions and recommendations to the MSL project in the days leading up to EDL is provided. C1 [Cianciolo, Alicia D.] NASA, Atmospher Flight & Entry Syst Branch, LaRC, Hampton, VA 23681 USA. [Cantor, Bruce] Malin Space Sci Syst, San Diego, CA 92121 USA. [Barnes, Jeff; Tyler, Daniel, Jr.] Oregon State Univ, CEOAS, Corvallis, OR 97331 USA. [Rafkin, Scot] SW Res Inst, Planetary Atmospheres & Surfaces Dept Space Studi, Boulder, CO 80302 USA. [Chen, Allen] CALTECH, Jet Prop Lab, EDL & Adv Technol Grp, Pasadena, CA 91109 USA. [Kass, David] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA. [Mischna, Michael] CALTECH, Jet Prop Lab, Div Sci, Earth & Planetary Atm Grp, Pasadena, CA 91109 USA. [Vasavada, Ashwin R.] CALTECH, Jet Prop Lab, MSL, Pasadena, CA 91109 USA. RP Cianciolo, AD (reprint author), NASA, Atmospher Flight & Entry Syst Branch, LaRC, MS 489, Hampton, VA 23681 USA. NR 9 TC 0 Z9 0 U1 0 U2 2 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 2525 EP 2536 PN I-III PG 12 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600149 ER PT S AU Parker, JS McElrath, TP Anderson, RL Sweetser, TH AF Parker, Jeffrey S. McElrath, Timothy P. Anderson, Rodney L. Sweetser, Theodore H. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI TRAJECTORY DESIGN FOR MOONRISE: A PROPOSED LUNAR SOUTH POLE AITKEN BASIN SAMPLE RETURN MISSION SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB This paper presents the mission design for the proposed MoonRise New Frontiers mission: a lunar far side lander and return vehicle, with an accompanying communication satellite. Both vehicles are launched together, but fly separate low-energy transfers to the Moon. The communication satellite enters lunar orbit immediately upon arrival at the Moon, whereas the lander enters a staging orbit about the lunar Lagrange points. The lander descends and touches down on the surface 17 days after the communication satellite enters orbit. The lander remains on the surface for nearly two weeks before lifting off and returning to Earth via a low-energy return. C1 [Parker, Jeffrey S.] Univ Colorado, Colorado Ctr Astrodynam Res, 431 UCB, Boulder, CO 80309 USA. [McElrath, Timothy P.; Anderson, Rodney L.; Sweetser, Theodore H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Parker, JS (reprint author), Univ Colorado, Colorado Ctr Astrodynam Res, 431 UCB, Boulder, CO 80309 USA. OI Anderson, Rodney/0000-0001-5336-2775 NR 23 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 2677 EP 2696 PN I-III PG 20 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600158 ER PT S AU Mueterthies, MJ Longuski, JM Vaughn, JA AF Mueterthies, Michael J. Longuski, James M. Vaughn, Jason A. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI APPLICATIONS OF THE ELECTRODYNAMIC TETHER SLING SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA ID AEROBRAKING TETHERS; EXPLORATION; MASS AB The electrodynamic tether sling is a novel method for propellantless spacecraft propulsion which combines a tether sling with an electrodynamic tether. The electrodynamic force allows the tether to be spun up and a payload thrown with all momentum (ultimately) coming from the rotation of the Earth. The performance of the electrodynamic tether sling is assessed for various tether parameters and various tether orbits. The mass of the tether and the time to reset between launches is calculated. The performance of the electrodynamic tether sling will be compared to conventional propellants. Under ideal conditions the electrodynamic tether sling can outperform the use of conventional rocket propulsion after fewer than ten payload throws. A list of caveats (the trouble with tethers) provides a host of challenges that must be addressed before the potential advantages of the electrodynamic tether sling can be realized. C1 [Mueterthies, Michael J.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Longuski, James M.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. [Vaughn, Jason A.] NASA, Marshall Space Flight Ctr, Space Environm & Effects, Huntsville, AL 35812 USA. RP Mueterthies, MJ (reprint author), Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. NR 25 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 2829 EP 2848 PN I-III PG 20 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600169 ER PT S AU Bokelmann, K Russell, RP Lantoine, G AF Bokelmann, Kevin Russell, Ryan P. Lantoine, Gregory BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI LYAPUNOV ORBITS IN THE JUPITER SYSTEM USING ELECTRODYNAMIC TETHERS SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA ID PERIODIC-ORBITS; STABILITY; POWER AB Various researchers have proposed the use of electrodynamic tethers for power generation and capture from interplanetary transfers. In this paper the effect of tether forces on periodic orbits in Jupiter-satellite systems are investigated. The restricted three body problem model is perturbed and a series of simplifications allows development of a conservative system that retains the Jacobi integral. The modified equations of motion lead to new locations of equilibrium positions as tether length is changed. Modified families of Lyapunov orbits are generated as functions of tether size and Jacobi integral, leading to new resonant-like orbits atypical of unperturbed families. Zero velocity curves and stability analyses are used to evaluate the dynamical properties of tether-modified orbits and several stable orbits are identified. C1 [Bokelmann, Kevin; Russell, Ryan P.] Univ Texas Austin, Aerosp & Engn Mech, Austin, TX 78712 USA. [Lantoine, Gregory] CALTECH, Jet Prop Lab, Mission Design & Nav Sect, Pasadena, CA 91109 USA. RP Bokelmann, K (reprint author), Univ Texas Austin, Aerosp & Engn Mech, Austin, TX 78712 USA. EM kbokelmann@utexas.edu; ryan.russell@utexas.edu NR 27 TC 0 Z9 0 U1 0 U2 1 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 2859 EP 2878 PN I-III PG 20 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600171 ER PT S AU Hejduk, MD Plakalovic, D Newman, LK Ollivierre, JC Hametz, ME Beaver, BA Thompson, RC AF Hejduk, M. D. Plakalovic, D. Newman, L. K. Ollivierre, J. C. Hametz, M. E. Beaver, B. A. Thompson, R. C. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI RECOMMENDED RISK ASSESSMENT TECHNIQUES AND THRESHOLDS FOR LAUNCH COLA OPERATIONS SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB This paper describes the second phase of a study to develop uniform launch collision avoidance and risk assessment (LCOLA) guidance and practices among the various NASA launch organizations and ranges. The first phase established the accuracy levels and covariance realism of predicted launch trajectories. This second phase used these trajectory data in a large screening experiment to examine the differences in results between general perturbations and special perturbations screenings. In addition, the trade space among probability of collision (Pc) screening threshold, required duration of the launch window, and average percent of the launch window remaining open was examined; the miss distance offset values that can be used as proxies for LCOLA screenings at different Pc values, and the difficulties that this approach presents, were explored; and the degree to which the risk posture is improved by having a LCOLA program in place, as compared to launching under a "big sky" assumption in which no conjunction prediction and mitigation are performed, was assessed. C1 [Hejduk, M. D.; Plakalovic, D.] Ai Solut Inc, Mission Serv Div, Colorado Springs, CO 80915 USA. [Newman, L. K.] NASA, Robot Syst Protect Program, Greenbelt, MD 20771 USA. [Hametz, M. E.] Ai Solut Inc, Cape Canaveral, FL 32920 USA. [Thompson, R. C.] Aerosp Corp, Chantilly, VA 20151 USA. RP Hejduk, MD (reprint author), Ai Solut Inc, Mission Serv Div, Colorado Springs, CO 80915 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 3061 EP 3080 PN I-III PG 20 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600182 ER PT S AU Ellison, DH Englander, JA Conway, BA AF Ellison, Donald H. Englander, Jacob A. Conway, Bruce A. BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI ROBUST GLOBAL OPTIMIZATION OF LOW-THRUST, MULTIPLE-FLYBY TRAJECTORIES SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA ID ALGORITHMS AB There are many challenging aspects of the design of multiple flyby, low-thrust trajectories. One of the most significant, from the point of view of a numerical optimizer, can be the characteristic time scale of the dynamical system. Trajectories in a setting with a short characteristic time scale (i.e. those occurring in the vicinity of Mercury or the Jovian moons) are more challenging to optimize than those with a longer time scale (i.e. trajectories to the outer solar system) because the spacecraft must often perform many revolutions about the central body as well as several flyby maneuvers. This paper introduces modifications that can be made to a multiple flyby trajectory optimizer employing the Sims-Flanagan transcription to improve its performance on challenging problems. These improvements include full specification of the problem Jacobian sparsity pattern and analytical expressions for many of its entries as well as refinements to how the problem constraints are scaled. The improvements are then quantified by solving two challenging problems: a Jovian moon rendezvous and a notional solar electric mission to Mercury. C1 [Ellison, Donald H.; Conway, Bruce A.] Univ Illinois, Dept Aerosp Engn, 104 South Wright St,Mail Code 236, Champaign, IL USA. [Englander, Jacob A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Ellison, DH (reprint author), Univ Illinois, Dept Aerosp Engn, 104 South Wright St,Mail Code 236, Champaign, IL USA. NR 18 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 3213 EP 3232 PN I-III PG 20 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600191 ER PT S AU Barbee, BW Landau, D AF Barbee, Brent W. Landau, Damon BE Broschart, SB Turner, JD Howell, KC Hoots, FR TI TRAJECTORY DESIGN FOR THE EXPLORATION OF PHOBOS AND DEIMOS SO ASTRODYNAMICS 2013, PTS I-III SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT AAS/AIAA Astrodynamics Specialist Conference CY AUG 11-15, 2013 CL Hilton Head, SC SP AAS, AIAA AB The two moons of Mars, Phobos and Deimos, are among the potential destinations for future human explorers. In this paper we present results from recent NASA working group studies in the areas of orbit analysis and trajectory design for human space flight missions to explore Phobos and Deimos. The evolution of the moons' orbits under natural perturbations are analyzed, which informs the design and optimization of trajectories to rendezvous with each moon in turn after arriving and inserting into a highly elliptical parking orbit. The abilities of the moons to support captured orbits during proximity operations are also considered. The results for optimal rendezvous trajectories between the moons, terminal rendezvous profile designs, and analysis of the Delta v and time required for reorientation of a highly elliptical parking orbit at Mars, to align with incoming and outgoing asymptotes for Mars arrival and departure, are synthesized to assess the required total Delta v at Mars, not including Earth departure Delta v or Earth return entry speed management Delta v. We find that the total Delta v performed in the vicinity of Mars for human space flight missions to explore Phobos and Deimos will range between 4.5 and 10.5 km/s, depending on the mission's Earth departure date and the type of round-trip trajectory flown. C1 [Barbee, Brent W.] NASA, Goddard Space Flight Ctr, Code 595,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Landau, Damon] CALTECH, Jet Prop Lab, Mission Design & Nav Sect, Pasadena, CA 91109 USA. RP Barbee, BW (reprint author), NASA, Goddard Space Flight Ctr, Code 595,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM brent.w.barbee@nasa.gov; damon.landau@jpl.nasa.gov NR 6 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-605-0 J9 ADV ASTRONAUT SCI PY 2014 VL 150 BP 3333 EP 3352 PN I-III PG 20 WC Engineering, Aerospace SC Engineering GA BE9EE UT WOS:000377326600199 ER PT B AU Krzaczek, R Shuping, R Lin, L Sun, L Charcos-Llorens, M Alles, R Perez, R AF Krzaczek, Robert Shuping, Ralph Lin, Lan Sun, Li Charcos-Llorens, Miguel Alles, Rosemary Perez, Robert BE Manset, N Forshay, P TI The SOFIA DCS Persistent Store: Maintaining Science and Mission Data in the Long Term SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XXIII SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 23rd Annual Conference on Astronomical Data Analysis Software and Systems CY SEP 29-OCT 03, 2013 CL Canada France Hawaii Telescope Corp, Waikoloa Beach, HI SP Canada France Hawaii Telescope Corp, Anglo Australian Observ, Elsevier, European Space Agcy, European So Observ, Infrared Process & Anal Ctr, Joint Astron Ctr, Large Binocular Telescope Observ, Natl Opt Astron Observ, Natl Radio Astron Observ, Smithsonian Astrophys Observ, Space Telescope Sci Inst HO Canada France Hawaii Telescope Corp AB The Stratospheric Observatory for Infrared Astronomy (SOFIA) is an airborne astronomical observatory comprised of a 2.5 meter infrared telescope mounted in the aft section of a Boeing 747SP aircraft that flies at operational altitudes between 37 000 and 45 000 feet, above 99% of atmospheric water vapor. SOFIA is projected to collect data over a 20 year lifetime, using a growing variety of instruments and observational modes. This in turn poses significant challenges for the long term maintenance and storage of science and mission data, as well as the delivery of that data to the astronomical community. Herein we present some aspects from the design of the SOFIA Data Cycle System (DCS) Persistent Store, which collects, maintains, and ultimately delivers all mission, science, and processed data to our end users. Features such as DCS Data Integrity, ensuring that all files are uncorrupted during their entire lifetime, from collection and generation through delivery to a user's desktop, are efficiently enabled by the Persistent Store. Key techniques in its implementation, such as the adoption of content addressable storage and inode indexing, are presented as well. Finally, both planned and unplanned benefits from our adoption of the Persistent Store are briefly detailed. C1 [Krzaczek, Robert] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, 1 Lomb Mem Dr, Rochester, NY 14623 USA. [Shuping, Ralph] Space Sci Inst, Boulder, CO 80301 USA. [Lin, Lan; Sun, Li; Charcos-Llorens, Miguel; Alles, Rosemary; Perez, Robert] NASA, Ames Res Ctr, Univ Space Res Assoc, Moffett Field, CA 94035 USA. RP Krzaczek, R (reprint author), Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, 1 Lomb Mem Dr, Rochester, NY 14623 USA. NR 2 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-854-1 J9 ASTR SOC P PY 2014 VL 485 BP 171 EP 174 PG 4 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BE7YW UT WOS:000376047600039 ER PT B AU Coulais, A Schellens, M Duvert, G Park, J Arabas, S Erard, S Roudier, G Hivon, E Mottet, S Laurent, B Pinter, M Kasradze, N Ayad, M AF Coulais, A. Schellens, M. Duvert, G. Park, J. Arabas, S. Erard, S. Roudier, G. Hivon, E. Mottet, S. Laurent, B. Pinter, M. Kasradze, N. Ayad, M. BE Manset, N Forshay, P TI Scaling GDL for Multi-cores to Process Planck HFI Beams Monte Carlo on HPC SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XXIII SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 23rd Annual Conference on Astronomical Data Analysis Software and Systems CY SEP 29-OCT 03, 2013 CL Canada France Hawaii Telescope Corp, Waikoloa Beach, HI SP Canada France Hawaii Telescope Corp, Anglo Australian Observ, Elsevier, European Space Agcy, European So Observ, Infrared Process & Anal Ctr, Joint Astron Ctr, Large Binocular Telescope Observ, Natl Opt Astron Observ, Natl Radio Astron Observ, Smithsonian Astrophys Observ, Space Telescope Sci Inst HO Canada France Hawaii Telescope Corp ID IDL AB After reviewing the majors progress done in GDL -now in 0.9.4- on performance and plotting capabilities since ADASS XXI paper (Coulais et al. 2012), we detail how a large code for Planck HFI beams Monte Carlo was successfully transposed from IDL to GDL on HPC. C1 [Coulais, A.; Laurent, B.; Pinter, M.; Kasradze, N.; Ayad, M.] LERMA CNRS, Paris, France. [Coulais, A.; Laurent, B.; Pinter, M.; Kasradze, N.; Ayad, M.] Observ Paris, F-75014 Paris, France. [Duvert, G.] UJF Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France. [Park, J.] Seoul Natl Univ, Dept Phys & Astron, Seoul 151747, South Korea. [Arabas, S.] Univ Warwick, Fac Phys, Coventry CV4 7AL, W Midlands, England. [Erard, S.] LESIA CNRS, Meudon, France. [Erard, S.] Observ Paris, Meudon, France. [Roudier, G.] JPL, Pasadena, CA USA. [Roudier, G.] CALTECH, Pasadena, CA 91125 USA. [Hivon, E.; Mottet, S.] CNRS, IAP, Paris, France. RP Coulais, A (reprint author), LERMA CNRS, Paris, France. EM alain.coulais@obspm.fr NR 6 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-854-1 J9 ASTR SOC P PY 2014 VL 485 BP 331 EP 334 PG 4 WC Astronomy & Astrophysics; Computer Science, Information Systems; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BE7YW UT WOS:000376047600076 ER PT J AU Chaplin, WJ Basu, S Huber, D Serenelli, A Casagrande, L Aguirre, VS Ball, WH Creevey, OL Gizon, L Handberg, R Karoff, C Lutz, R Marques, JP Miglio, A Stello, D Suran, MD Pricopi, D Metcalfe, TS Monteiro, MJPFG Molenda-Zakowicz, J Appourchaux, T Christensen-Dalsgaard, J Elsworth, Y Garcia, RA Houdek, G Kjeldsen, H Bonanno, A Campante, TL Corsaro, E Gaulme, P Hekker, S Mathur, S Mosser, B Regulo, C Salabert, D AF Chaplin, W. J. Basu, S. Huber, D. Serenelli, A. Casagrande, L. Aguirre, V. Silva Ball, W. H. Creevey, O. L. Gizon, L. Handberg, R. Karoff, C. Lutz, R. Marques, J. P. Miglio, A. Stello, D. Suran, M. D. Pricopi, D. Metcalfe, T. S. Monteiro, M. J. P. F. G. Molenda-Zakowicz, J. Appourchaux, T. Christensen-Dalsgaard, J. Elsworth, Y. Garcia, R. A. Houdek, G. Kjeldsen, H. Bonanno, A. Campante, T. L. Corsaro, E. Gaulme, P. Hekker, S. Mathur, S. Mosser, B. Regulo, C. Salabert, D. TI ASTEROSEISMIC FUNDAMENTAL PROPERTIES OF SOLAR-TYPE STARS OBSERVED BY THE NASA KEPLER MISSION SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE asteroseismology; methods: data analysis; stars: fundamental parameters; stars: interiors ID STELLAR EVOLUTION CODE; MAIN-SEQUENCE STARS; EQUATION-OF-STATE; RED-GIANT BRANCH; CHEMICAL-COMPOSITION; HELIUM CONTENT; REACTION-RATES; NGC 6791; OSCILLATIONS; SUN AB We use asteroseismic data obtained by the NASA Kepler mission to estimate the fundamental properties of more than 500 main-sequence and sub-giant stars. Data obtained during the first 10 months of Kepler science operations were used for this work, when these solar-type targets were observed for one month each in survey mode. Stellar properties have been estimated using two global asteroseismic parameters and complementary photometric and spectroscopic data. Homogeneous sets of effective temperatures, T-eff, were available for the entire ensemble from complementary photometry; spectroscopic estimates of T-eff and [Fe/H] were available from a homogeneous analysis of ground-based data on a subset of 87 stars. We adopt a grid-based analysis, coupling six pipeline codes to 11 stellar evolutionary grids. Through use of these different grid-pipeline combinations we allow implicitly for the impact on the results of stellar model dependencies from commonly used grids, and differences in adopted pipeline methodologies. By using just two global parameters as the seismic inputs we are able to perform a homogenous analysis of all solar-type stars in the asteroseismic cohort, including many targets for which it would not be possible to provide robust estimates of individual oscillation frequencies (due to a combination of low signal-to-noise ratio and short dataset lengths). The median final quoted uncertainties from consolidation of the grid-based analyses are for the full ensemble (spectroscopic subset) approximately 10.8% (5.4%) in mass, 4.4% (2.2%) in radius, 0.017 dex (0.010 dex) in log g, and 4.3% (2.8%) in mean density. Around 36% (57%) of the stars have final age uncertainties smaller than 1 Gyr. These ages will be useful for ensemble studies, but should be treated carefully on a star-by-star basis. Future analyses using individual oscillation frequencies will offer significant improvements on up to 150 stars, in particular for estimates of the ages, where having the individual frequency data is most important. C1 [Chaplin, W. J.; Handberg, R.; Miglio, A.; Elsworth, Y.; Campante, T. L.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Chaplin, W. J.; Aguirre, V. Silva; Handberg, R.; Karoff, C.; Miglio, A.; Stello, D.; Metcalfe, T. S.; Christensen-Dalsgaard, J.; Elsworth, Y.; Houdek, G.; Kjeldsen, H.; Campante, T. L.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Basu, S.] Yale Univ, Dept Phys & Astron, New Haven, CT 06520 USA. [Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Serenelli, A.] Inst Ciencias Espacio CSIC IEEC, Fac Ciencies, E-08193 Bellaterra, Spain. [Casagrande, L.] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Ball, W. H.; Gizon, L.; Lutz, R.; Marques, J. P.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Ball, W. H.; Gizon, L.; Lutz, R.; Marques, J. P.; Hekker, S.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Creevey, O. L.; Salabert, D.] Univ Nice Sophia Antipolis, Lab Lagrange, UMR 7293, Observ Cote Azur,CNRS, F-06304 Nice, France. [Creevey, O. L.; Appourchaux, T.] Univ Paris 11, CNRS UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France. [Stello, D.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Suran, M. D.; Pricopi, D.] Romanian Acad, Astron Inst, RO-40557 Bucharest, Romania. [Metcalfe, T. S.; Mathur, S.] Space Sci Inst, Boulder, CO 80301 USA. [Monteiro, M. J. P. F. G.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Molenda-Zakowicz, J.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Garcia, R. A.] Univ Paris Diderot, Lab AIM, CEA DSM, IRFU SAp, F-91191 Gif Sur Yvette, France. [Bonanno, A.; Corsaro, E.] INAF Astrophys Observ Catania, I-95123 Catania, Italy. [Corsaro, E.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Gaulme, P.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Mathur, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Mosser, B.] Univ Paris 06, Univ Denis Diderot, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Regulo, C.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Regulo, C.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. RP Chaplin, WJ (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RI Monteiro, Mario J.P.F.G./B-4715-2008; OI Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Bonanno, Alfio/0000-0003-3175-9776; Metcalfe, Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965; Basu, Sarbani/0000-0002-6163-3472; Garcia, Rafael/0000-0002-8854-3776; Serenelli, Aldo/0000-0001-6359-2769; Ball, Warrick/0000-0002-4773-1017; Handberg, Rasmus/0000-0001-8725-4502 FU Danish National Research Foundation [DNRF106]; ASTERISK project; European Research Council [267864]; European Community [312844] FX Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant agreement No.: DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement No.: 267864). The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312844 (SPACEINN). NR 99 TC 113 Z9 113 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JAN PY 2014 VL 210 IS 1 AR 1 DI 10.1088/0067-0049/210/1/1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 269TP UT WOS:000328265100001 ER PT J AU Evans, PA Osborne, JP Beardmore, AP Page, KL Willingale, R Mountford, CJ Pagani, C Burrows, DN Kennea, JA Perri, M Tagliaferri, G Gehrels, N AF Evans, P. A. Osborne, J. P. Beardmore, A. P. Page, K. L. Willingale, R. Mountford, C. J. Pagani, C. Burrows, D. N. Kennea, J. A. Perri, M. Tagliaferri, G. Gehrels, N. TI 1SXPS: A DEEP SWIFT X-RAY TELESCOPE POINT SOURCE CATALOG WITH LIGHT CURVES AND SPECTRA SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; methods: data analysis; surveys; X-rays: general ID SERENDIPITOUS SOURCE CATALOG; MEDIUM-SENSITIVITY SURVEY; NEWTON SLEW SURVEY; XMM-NEWTON; CONFIDENCE-LIMITS; LIKELIHOOD RATIO; REPRESENTATIONS; POPULATION; STATISTICS; ABSORPTION AB We present the 1SXPS (Swift-XRT point source) catalog of 151,524 X-ray point sources detected by the Swift-XRT in 8 yr of operation. The catalog covers 1905 deg(2) distributed approximately uniformly on the sky. We analyze the data in two ways. First we consider all observations individually, for which we have a typical sensitivity of similar to 3 x 10(-13) erg cm(-2) s(-1) (0.3-10 keV). Then we co-add all data covering the same location on the sky: these images have a typical sensitivity of similar to 9 x 10(-14) erg cm(-2) s(-1) (0.3-10 keV). Our sky coverage is nearly 2.5 times that of 3XMM-DR4, although the catalog is a factor of similar to 1.5 less sensitive. The median position error is 5.'' 5 (90% confidence), including systematics. Our source detection method improves on that used in previous X-ray Telescope (XRT) catalogs and we report >68,000 new X-ray sources. The goals and observing strategy of the Swift satellite allow us to probe source variability on multiple timescales, and we find similar to 30,000 variable objects in our catalog. For every source we give positions, fluxes, time series (in four energy bands and two hardness ratios), estimates of the spectral properties, spectra and spectral fits for the brightest sources, and variability probabilities in multiple energy bands and timescales. C1 [Evans, P. A.; Osborne, J. P.; Beardmore, A. P.; Page, K. L.; Willingale, R.; Mountford, C. J.; Pagani, C.] Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England. [Burrows, D. N.; Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Perri, M.] ASI Sci Data Ctr, I-00133 Rome, Italy. [Perri, M.] INAF Osservatorio Astron Roma, I-000040 Monte Porzio Catone, Italy. [Tagliaferri, G.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Evans, PA (reprint author), Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Univ Rd, Leicester LE1 7RH, Leics, England. EM pae9@leicester.ac.uk OI Perri, Matteo/0000-0003-3613-4409; Tagliaferri, Gianpiero/0000-0003-0121-0723 FU UK Space Agency; NASA [NAS5-00136]; ASI-INAF grant [I/004/11/0] FX P.A.E., J.P.O., A. P. B., K. L. P., C. P. and C.J.M. acknowledge support from the UK Space Agency. D.N.B. and J.A.K. acknowledge support from NASA contract NAS5-00136. G. T. acknowledges support from ASI-INAF grant I/004/11/0. We thank Simon Vaughan for helpful discussions during the preparation of this paper and Paul O'Brien for feedback on the manuscript. We also thank the anonymous referee and the Scientific Editor for insightful and helpful comments. This work made use of data supplied by the UK Swift Science Data Center at the University of Leicester. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 42 TC 41 Z9 42 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JAN PY 2014 VL 210 IS 1 AR 8 DI 10.1088/0067-0049/210/1/8 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 269TP UT WOS:000328265100008 ER PT B AU Montes, C Allgood, D Allouche, E Islam, R Tham, I AF Montes, C. Allgood, D. Allouche, E. Islam, R. Tham, I. BE Grantham, M Basheer, PAM Magee, B Soutsos, M TI Evaluation of geopolymer concrete for repair of rocket test facility flame deflectors SO CONCRETE SOLUTIONS: PROCEEDINGS OF CONCRETE SOLUTIONS, 5TH INTERNATIONAL CONFERENCE ON CONCRETE REPAIR LA English DT Proceedings Paper CT 5th International Conference on Concrete Repair CY SEP 01-03, 2014 CL Belfast, IRELAND ID METAKAOLIN AB A joint research effort by Louisiana Tech University (LTU) and NASA Stennis Space Center (SSC) was established to develop refractory geopolymer concrete. In preliminary tests, geopolymer was used to complete small repairs of the floors and walls of the refractory-lined flame trench at the SSC E-1 Cell 3 rocket engine testing facility. These repairs were then exposed to high temperature exhaust plumes of a 1780 kN class LOX/RP-1 engine. Subsequently, a controlled study was conducted of the geopolymer's performance under direct rocket plume impingement conditions. The NASA-SSC Diagnostic Test Facility (DTF) thruster, which is a 5.78 kN LOX/GH2 rocket engine, was used to generate the necessary supersonic plume environments to produce direct impingement on refractory test panels 30 cm wide x 60 cm x 15 cm deep. Various geopolymer and commercial grade formulations were tested. Data collected included surface profiles of the test panels giving localized erosion rates during the test. C1 [Montes, C.; Allouche, E.; Islam, R.] Louisiana Tech Univ, Ruston, LA 71270 USA. [Allgood, D.] NASA, Stennis Space Ctr, Pearlington, MS USA. [Tham, I.] ML Smith, Ruston, LA USA. RP Montes, C (reprint author), Louisiana Tech Univ, Ruston, LA 71270 USA. NR 9 TC 0 Z9 0 U1 1 U2 1 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-315-73731-7; 978-1-138-02708-4 PY 2014 BP 499 EP 506 PG 8 WC Construction & Building Technology; Materials Science, Multidisciplinary SC Construction & Building Technology; Materials Science GA BE0SJ UT WOS:000366827300070 ER PT B AU Davis, H Scalice, D AF Davis, Hilarie Scalice, Daniella BE Manning, JG Hemenway, MK Jensen, JB Gibbs, MG TI Defining and Measuring Impact for Ourselves SO ENSURING STEM LITERACY: A NATIONAL CONFERENCE ON STEM EDUCATION AND PUBLIC OUTREACH SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 125th ASP Annual Conference on Ensuring STEM Literacy: A National Conference on STEM Education and Public Outreach CY JUL 20-24, 2013 CL San Jose State Univ, San Jose, CA SP EXOPLANET EXPLORAT PROGRAM, JPL, Stratospher Observ Infrared Astron, NRAO, E&S, Sky Skan, LOCKHEED MARTIN, sapl learn, Bell Aerosp & Technol Corp, AAS, EXPLORE SCI, SEILER INSTRUMENT, Astron Soc Pacif, San Jose State Univ HO San Jose State Univ AB This paper describes a practical method to flexibly and robustly measure the impact of EPO programs. C1 [Davis, Hilarie] Technol Learning Consortium Inc, 75 Sauga Ave, North Kingstown, RI 02852 USA. NASA, Astrobiol Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Davis, H (reprint author), Technol Learning Consortium Inc, 75 Sauga Ave, North Kingstown, RI 02852 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-850-3 J9 ASTR SOC P PY 2014 VL 483 BP 163 EP 172 PG 10 WC Astronomy & Astrophysics; Education & Educational Research; Education, Scientific Disciplines SC Astronomy & Astrophysics; Education & Educational Research GA BE7YU UT WOS:000376047500022 ER PT B AU Martin, AM Chambers, LH Pippin, MR AF Martin, Ann M. Chambers, Lin H. Pippin, Margaret R. BE Manning, JG Hemenway, MK Jensen, JB Gibbs, MG TI What and How Are We Evaluating? Meta-Evaluation of Climate Education Projects Funded by NASA SO ENSURING STEM LITERACY: A NATIONAL CONFERENCE ON STEM EDUCATION AND PUBLIC OUTREACH SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 125th ASP Annual Conference on Ensuring STEM Literacy: A National Conference on STEM Education and Public Outreach CY JUL 20-24, 2013 CL San Jose State Univ, San Jose, CA SP EXOPLANET EXPLORAT PROGRAM, JPL, Stratospher Observ Infrared Astron, NRAO, E&S, Sky Skan, LOCKHEED MARTIN, sapl learn, Bell Aerosp & Technol Corp, AAS, EXPLORE SCI, SEILER INSTRUMENT, Astron Soc Pacif, San Jose State Univ HO San Jose State Univ AB NASA Innovations in Climate Education (NICE) at Langley Research Center has funded 71 climate education initiatives over four years, each evaluated separately by external evaluators. NICE has undertaken a systematic meta-evaluation, seeking to understand the range of evaluations, approaches, and methods represented in this portfolio. When NASA asks for evaluation of funded projects, what happens? Which questions are asked and answered, using which tools? To what extent do the evaluations meet the needs of projects and program officers? How do they contribute to best practices in (climate) science education? These questions are important to ask about general STEM education work; the NICE portfolio provides a broad test case for thinking strategically, critically, and progressively about evaluation in our community. Our findings can inform the NASA, ASP, and STEM EPO communities and prompt us to consider a broad range of informative evaluation options. C1 [Martin, Ann M.; Chambers, Lin H.; Pippin, Margaret R.] NASA, Langley Res Ctr, 21 Langley Blvd, Hampton, VA 23681 USA. RP Martin, AM (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd, Hampton, VA 23681 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-850-3 J9 ASTR SOC P PY 2014 VL 483 BP 241 EP 247 PG 7 WC Astronomy & Astrophysics; Education & Educational Research; Education, Scientific Disciplines SC Astronomy & Astrophysics; Education & Educational Research GA BE7YU UT WOS:000376047500034 ER PT B AU Hasan, H Smith, D AF Hasan, Hashima Smith, Denise BE Manning, JG Hemenway, MK Jensen, JB Gibbs, MG TI Innovation in NASA's Astrophysics Education and Public Outreach SO ENSURING STEM LITERACY: A NATIONAL CONFERENCE ON STEM EDUCATION AND PUBLIC OUTREACH SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 125th ASP Annual Conference on Ensuring STEM Literacy: A National Conference on STEM Education and Public Outreach CY JUL 20-24, 2013 CL San Jose State Univ, San Jose, CA SP EXOPLANET EXPLORAT PROGRAM, JPL, Stratospher Observ Infrared Astron, NRAO, E&S, Sky Skan, LOCKHEED MARTIN, sapl learn, Bell Aerosp & Technol Corp, AAS, EXPLORE SCI, SEILER INSTRUMENT, Astron Soc Pacif, San Jose State Univ HO San Jose State Univ AB New technology and media are being rapidly incorporated in NASA's Astrophysics Education and Public Outreach (EPO) portfolio. In addition to web pages that provide basic information on missions and links to educational sites, missions have developed Facebook and Twitter followers. Recent highlights are presented about the innovative techniques used in presenting NASA science to the public, educators and students, together with representative examples. The immense treasure trove of electronic NASA EPO material is available to the public. C1 [Hasan, Hashima] NASA Headquarters, 300 E St SW, Washington, DC 20546 USA. [Smith, Denise] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Hasan, H (reprint author), NASA Headquarters, 300 E St SW, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-850-3 J9 ASTR SOC P PY 2014 VL 483 BP 267 EP 272 PG 6 WC Astronomy & Astrophysics; Education & Educational Research; Education, Scientific Disciplines SC Astronomy & Astrophysics; Education & Educational Research GA BE7YU UT WOS:000376047500038 ER PT B AU Bartolone, L Nichols-Yehling, M Brinkworth, C Hurt, RL Llamas, J Squires, GK Wenger, M Martin, A AF Bartolone, Lindsay Nichols-Yehling, Michelle Brinkworth, Carolyn Hurt, Robert L. Llamas, Jacob Squires, Gordon K. Wenger, Matthew Martin, Ann BE Manning, JG Hemenway, MK Jensen, JB Gibbs, MG TI STEMdex: CliffsNotes for Education and Public Outreach SO ENSURING STEM LITERACY: A NATIONAL CONFERENCE ON STEM EDUCATION AND PUBLIC OUTREACH SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 125th ASP Annual Conference on Ensuring STEM Literacy: A National Conference on STEM Education and Public Outreach CY JUL 20-24, 2013 CL San Jose State Univ, San Jose, CA SP EXOPLANET EXPLORAT PROGRAM, JPL, Stratospher Observ Infrared Astron, NRAO, E&S, Sky Skan, LOCKHEED MARTIN, sapl learn, Bell Aerosp & Technol Corp, AAS, EXPLORE SCI, SEILER INSTRUMENT, Astron Soc Pacif, San Jose State Univ HO San Jose State Univ AB We present a new resource for the astronomy education community, with the goal of improving our community's knowledge and understanding of the educational research pertinent to our work. STEMdex will be a searchable database of summaries of peer-reviewed education papers, written by educators and researchers, and posted for the entire community to use. While we know we should base our EPO work on a solid research foundation, many people have limited time when it comes to staying on top of the literature. STEMdex aims to reduce that workload. Our database will summarize papers across the astronomy education spectrum, including formal and informal education, outreach, pedagogy, evaluation, and other topics.(1) C1 [Bartolone, Lindsay; Nichols-Yehling, Michelle] Adler Planetarium, 1300 S Lake Shore Dr, Chicago, IL 60605 USA. [Brinkworth, Carolyn; Hurt, Robert L.; Llamas, Jacob; Squires, Gordon K.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Wenger, Matthew] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA. [Martin, Ann] NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Bartolone, L (reprint author), Adler Planetarium, 1300 S Lake Shore Dr, Chicago, IL 60605 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-850-3 J9 ASTR SOC P PY 2014 VL 483 BP 411 EP 413 PG 3 WC Astronomy & Astrophysics; Education & Educational Research; Education, Scientific Disciplines SC Astronomy & Astrophysics; Education & Educational Research GA BE7YU UT WOS:000376047500065 ER PT B AU Meinke, B Smith, D Bleacher, L Hauck, K Soeffing, C AF Meinke, Bonnie Smith, Denise Bleacher, Lora Hauck, Karin Soeffing, Cassie CA NASA SMD EPO Community BE Manning, JG Hemenway, MK Jensen, JB Gibbs, MG TI NASA Science4Girls: Engaging Girls in STEM at Their Local Library SO ENSURING STEM LITERACY: A NATIONAL CONFERENCE ON STEM EDUCATION AND PUBLIC OUTREACH SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 125th ASP Annual Conference on Ensuring STEM Literacy: A National Conference on STEM Education and Public Outreach CY JUL 20-24, 2013 CL San Jose State Univ, San Jose, CA SP EXOPLANET EXPLORAT PROGRAM, JPL, Stratospher Observ Infrared Astron, NRAO, E&S, Sky Skan, LOCKHEED MARTIN, sapl learn, Bell Aerosp & Technol Corp, AAS, EXPLORE SCI, SEILER INSTRUMENT, Astron Soc Pacif, San Jose State Univ HO San Jose State Univ AB The NASA Science Mission Directorate (SMD) Science Education and Public Outreach Forums coordinate the participation of SMD education and public out-reach (EPO) programs in Women's History Month through the NASA Science4Girls and Their Families initiative. The initiative partners NASA science education programs with public libraries to provide NASA-themed hands-on education activities for girls and their families. The initiative has expanded from the successful 2012 Astro4Girls pilot to engage girls in all four NASA science discipline areas, which broadens the impact of the pilot by enabling audiences to experience the full range of NASA science topics and the different career skills each requires. The events focus on engaging underserved and underrepresented audiences in Science, Technology, Engineering, and Mathematics (STEM) via use of research-based best practices, collaborations with libraries, partnerships with local and national organizations, and remote engagement of audiences. C1 [Meinke, Bonnie; Smith, Denise] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Bleacher, Lora] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hauck, Karin] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Soeffing, Cassie] Inst Global Environm Strategies, Arlington, VA 22209 USA. RP Meinke, B (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-850-3 J9 ASTR SOC P PY 2014 VL 483 BP 429 EP 432 PG 4 WC Astronomy & Astrophysics; Education & Educational Research; Education, Scientific Disciplines SC Astronomy & Astrophysics; Education & Educational Research GA BE7YU UT WOS:000376047500068 ER PT S AU Orr, JS Wall, JH VanZwieten, TS Hall, CE AF Orr, Jeb S. Wall, John H. VanZwieten, Tannen S. Hall, Charles E. BE May, AJ TI SPACE LAUNCH SYSTEM ASCENT FLIGHT CONTROL DESIGN SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect ID CONSTRAINED CONTROL ALLOCATION AB A robust and flexible autopilot architecture for NASA's Space Launch System (SLS) family of launch vehicles is presented. The SLS configurations represent a potentially significant increase in complexity and performance capability when compared with other manned launch vehicles. It was recognized early in the program that a new, generalized autopilot design should be formulated to fulfill the needs of this new space launch architecture. The present design concept is intended to leverage existing NASA and industry launch vehicle design experience and maintain the extensibility and modularity necessary to accommodate multiple vehicle configurations while relying on proven and flight tested control design principles for large boost vehicles. The SLS flight control architecture combines a digital three-axis autopilot with traditional bending filters to support robust active or passive stabilization of the vehicle's bending and sloshing dynamics using optimally blended measurements from multiple rate gyros on the vehicle structure. The algorithm also relies on a pseudo-optimal control allocation scheme to maximize the performance capability of multiple vectored engines while accommodating throttling and engine failure contingencies in real time with negligible impact to stability characteristics. The architecture supports active in-flight disturbance compensation through the use of nonlinear observers driven by acceleration measurements. Envelope expansion and robustness enhancement is obtained through the use of a multiplicative forward gain modulation law based upon a simple model reference adaptive control scheme. C1 [Orr, Jeb S.] Charles Stark Draper Lab Inc, Dynam & Control, Jacobs ESSSA Grp, Huntsville, AL 35806 USA. [Wall, John H.] Dynamic Concepts Inc, Guidance Nav & Control Grp, Jacobs ESSSA Grp, Huntsville, AL 35806 USA. [VanZwieten, Tannen S.; Hall, Charles E.] NASA Marshall Space Flight Ctr, Control Syst Design & Anal Branch, Huntsville, AL 35812 USA. RP Orr, JS (reprint author), Charles Stark Draper Lab Inc, Dynam & Control, Jacobs ESSSA Grp, Huntsville, AL 35806 USA. NR 22 TC 0 Z9 0 U1 1 U2 1 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 141 EP 154 PG 14 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300012 ER PT S AU Wall, JH Orr, JS VanZwieten, TS AF Wall, John H. Orr, Jeb S. VanZwieten, Tannen S. BE May, AJ TI SPACE LAUNCH SYSTEM IMPLEMENTATION OF ADAPTIVE AUGMENTING CONTROL SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB Given the complex structural dynamics, challenging ascent performance requirements, and rigorous flight certification constraints owing to its manned capability, the NASA Space Launch System (SLS) launch vehicle requires a proven thrust vector control algorithm design with highly optimized parameters to provide stable and high-performance flight. On its development path to Preliminary Design Review (PDR), the SLS flight control system has been challenged by significant vehicle flexibility, aerodynamics, and sloshing propellant. While the design has been able to meet all robust stability criteria, it has done so with little excess margin. Through significant development work, an Adaptive Augmenting Control (AAC) algorithm has been shown to extend the envelope of failures and flight anomalies the SLS control system can accommodate while maintaining a direct link to flight control stability criteria such as classical gain and phase margin. In this paper, the work performed to mature the AAC algorithm as a baseline component of the SLS flight control system is presented. The progress to date has brought the algorithm design to the PDR level of maturity. The algorithm has been extended to augment the full SLS digital 3-axis autopilot, including existing load-relief elements, and the necessary steps for integration with the production flight software prototype have been implemented. Several updates which have been made to the adaptive algorithm to increase its performance, decrease its sensitivity to expected external commands, and safeguard against limitations in the digital implementation are discussed with illustrating results. Monte Carlo simulations and selected stressing case results are also shown to demonstrate the algorithm's ability to increase the robustness of the integrated SLS flight control system. C1 [Wall, John H.] Dynam Concepts Inc, Guidance Nav & Control Grp, Jacobs ESSSA Grp, Huntsville, AL 35806 USA. [Orr, Jeb S.] Charles Stark Draper Lab Inc, Dynam & Control, Jacobs ESSSA Grp, Huntsville, AL 35806 USA. [VanZwieten, Tannen S.] NASA Marshall Space Flight Ctr, Control Syst Design & Anal Branch, Huntsville, AL 35812 USA. RP Wall, JH (reprint author), Dynam Concepts Inc, Guidance Nav & Control Grp, Jacobs ESSSA Grp, Huntsville, AL 35806 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 225 EP 239 PG 15 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300018 ER PT S AU VanZwieten, TS Gilligan, ET Wall, JH Orr, JS Miller, CJ Hanson, CE AF VanZwieten, Tannen S. Gilligan, Eric T. Wall, John H. Orr, Jeb S. Miller, Christopher J. Hanson, Curtis E. BE May, AJ TI ADAPTIVE AUGMENTING CONTROL FLIGHT CHARACTERIZATION EXPERIMENT ON AN F/A-18 SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB The NASA Marshall Space Flight Center (MSFC) Flight Mechanics and Analysis Division developed an Adaptive Augmenting Control (AAC) algorithm for launch vehicles that improves robustness and performance by adapting an otherwise well tuned classical control algorithm to unexpected environments or variations in vehicle dynamics. This AAC algorithm is currently part of the baseline design for the SLS Flight Control System (FCS), but prior to this series of research flights it was the only component of the autopilot design that had not been flight tested. The Space Launch System (SLS) flight software prototype, including the adaptive component, was recently tested on a piloted aircraft at Dryden Flight Research Center (DFRC) which has the capability to achieve a high level of dynamic similarity to a launch vehicle. Scenarios for the flight test campaign were designed specifically to evaluate the AAC algorithm to ensure that it is able to achieve the expected performance improvements with no adverse impacts in nominal or near nominal scenarios. Having completed the recent series of flight characterization experiments on DFRC's F/A-18, the AAC algorithm's capability, robustness, and reproducibility, have been successfully demonstrated. Thus, the entire SLS control architecture has been successfully flight tested in a relevant environment. This has increased NASA's confidence that the autopilot design is ready to fly on the SLS Block I vehicle and will exceed the performance of previous architectures. C1 [VanZwieten, Tannen S.; Gilligan, Eric T.] NASA Marshall Space Flight Ctr, Control Syst Design & Anal Branch, Huntsville, AL 35812 USA. [Wall, John H.] Dynam Concepts Inc, Guidance Nav & Control Grp, Jacobs ESSSA Grp, Huntsville, AL 35806 USA. [Orr, Jeb S.] Charles Stark Draper Lab Inc, Dynam & Control, Jacobs ESSSA Grp, Huntsville, AL 35806 USA. [Miller, Christopher J.; Hanson, Curtis E.] NASA Dryden Flight Res Cente, Flight Controls & Dynam Branch, Edwards AFB, CA 93523 USA. RP VanZwieten, TS (reprint author), NASA Marshall Space Flight Ctr, Control Syst Design & Anal Branch, Huntsville, AL 35812 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 241 EP 257 PG 17 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300019 ER PT S AU Sorgenfrei, M Nehrenz, M Edwards, R Joshi, S AF Sorgenfrei, Matt Nehrenz, Matt Edwards, Robert Joshi, Sanjay BE May, AJ TI FORMULATION OF A SMALL SPACECRAFT AVIONICS TESTBED SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB Small spacecraft are increasingly being considered for scientific missions in low Earth orbit and beyond, however these small platforms suffer from less flight heritage than their larger counterparts. In particular, new missions will require advanced guidance, navigation, and control (GNC) capabilities, an area of active research and development for small spacecraft. Successful implementation of advanced GNC technologies in smaller spacecraft requires additional testing, verification, and validation, which in turn places greater pressure on the mission schedule. In an effort to reduce both system-level risk and schedule pressure, a new facility is under development at NASA Ames Research Center. This lab, known as the Generalized Nanosatellite Avionics Testbed (G-NAT), accelerates the development of avionics subsystems for small spacecraft through hardware characterization, software development, and testing of GNC components. This paper will present an overview of the sensors, actuators, and processors that are currently being tested in the G-NAT lab, and will present a case study of a simple single-axis hardware characterization problem. C1 [Sorgenfrei, Matt] NASA Ames Res Ctr, Stinger Ghaffarian Technol, Moffett Field, CA 94035 USA. [Nehrenz, Matt] NASA Ames Res Ctr, Emergent Space Technol, Moffett Field, CA 94035 USA. [Edwards, Robert; Joshi, Sanjay] Univ Calif Davis, Dept Mech & Aerosp Engn, Davis, CA 95616 USA. RP Sorgenfrei, M (reprint author), NASA Ames Res Ctr, Stinger Ghaffarian Technol, Moffett Field, CA 94035 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 309 EP 320 PG 12 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300023 ER PT S AU Abbott, FB Thompson, W Ely, TA AF Abbott, F. Brent Thompson, William Ely, Todd A. BE May, AJ TI HOSTING THE DEEP SPACE ATOMIC CLOCK (DSAC) ON THE ORBITAL TEST BED (OTB-1) SATELLITE SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB This paper will share the experiences, ongoing work and lessons learned in hosting the DSAC instrument on a relatively standard satellite bus, OTB-1. As DSAC is a great advancement in navigation, this hosting will confirm the on-orbit performance to enable DSAC to be used for future operational systems. Payload performance and operational requirements will be discussed. The process in which JPL and Surrey US work together with requirements and bus design to optimize maximum return on on-orbit testing will be presented with focus on GN&C systems. C1 [Abbott, F. Brent; Thompson, William] Surrey Satellite Technol US LLC, 345 Inverness Dr South,Suite 100, Englewood, CO 80112 USA. [Ely, Todd A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Abbott, FB (reprint author), Surrey Satellite Technol US LLC, 345 Inverness Dr South,Suite 100, Englewood, CO 80112 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 431 EP 440 PG 10 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300032 ER PT S AU Johnson, AE Mandalia, AB AF Johnson, Andrew E. Mandalia, Amit B. BE May, AJ TI SIMPLE SAFE SITE SELECTION: HAZARD AVOIDANCE ALGORITHM PERFORMANCE AT MARS SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB Many scientifically interesting sites at Mars have small-scale hazards that can pose a threat to landers and rovers. Hazard Detection and Avoidance (HDA) can be used during the terminal phase of flight to find and divert to a safe site. An algorithm has been developed that operates directly on a single flash lidar range image and is able to rapidly select a safe site in a computationally efficient manner. A flash lidar simulator is used to analyze the performance of the algorithm relative to the terrain and vehicle. The algorithm is able to select a safe site with confidence for terrains with rock abundances up to 35% and slopes up to the capability of the selected rover (22). Variation in altitude, attitude, and lidar noise do not significantly affect the performance of the safe site selection. This hazard avoidance algorithm can decrease landing failures at all the landing sites listed in the Mars 2020 Science Definition Report, and has the potential to operate at far more difficult sites. C1 [Johnson, Andrew E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Mandalia, Amit B.] Georgia Inst Technol, Guggenheim Sch Aerosp Engn, Atlanta, GA 30332 USA. RP Johnson, AE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 443 EP 456 PG 14 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300033 ER PT S AU Aubuchon, VV AF Aubuchon, Vanessa V. BE May, AJ TI FULL-ENVELOPE LAUNCH ABORT SYSTEM PERFORMANCE ANALYSIS METHODOLOGY SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB The implementation of a new dispersion methodology is described, which disperses abort initiation altitude or time along with all other Launch Abort System (LAS) parameters during Monte Carlo simulations. In contrast, the standard methodology assumes that an abort initiation condition is held constant (e.g., aborts initiated at altitude for Mach 1, altitude for maximum dynamic pressure, etc.) while dispersing other LAS parameters. The standard method results in large gaps in performance information due to the discrete nature of initiation conditions, while the full-envelope dispersion method provides a significantly more comprehensive assessment of LAS abort performance for the full launch vehicle ascent flight envelope and identifies performance "pinch-points" that may occur at flight conditions outside of those contained in the discrete set. The new method has significantly increased the fidelity of LAS abort simulations and confidence in the results. C1 [Aubuchon, Vanessa V.] NASA Langley Res Ctr, Flight Dynam Branch, MS 308, Hampton, VA 23681 USA. RP Aubuchon, VV (reprint author), NASA Langley Res Ctr, Flight Dynam Branch, MS 308, Hampton, VA 23681 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 487 EP 498 PG 12 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300036 ER PT S AU Sud, J Gay, R Holt, G Zanetti, R AF Sud, Jastesh Gay, Robert Holt, Greg Zanetti, Renato BE May, AJ TI ORION EXPLORATION FLIGHT TEST-1 (EFT-1) ABSOLUTE NAVIGATION DESIGN SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB Scheduled to launch in September 2014 atop a Delta IV Heavy from the Kennedy Space Center, the Orion Multi-Purpose-Crew-Vehicle (MPCV's) maiden flight dubbed "Exploration Flight Test-1" (EFT-1) intends to stress the system by placing the uncrewed vehicle on a high-energy parabolic trajectory replicating conditions similar to those that would be experienced when returning from an asteroid or a lunar mission. Unique challenges associated with designing the navigation system for EFT-1 are presented in the narrative with an emphasis on how redundancy and robustness influenced the architecture. Two Inertial Measurement Units (IMUs), one GPS receiver and three barometric altimeters (BALTs) comprise the navigation sensor suite. The sensor data is multiplexed using conventional integration techniques and the state estimate is refined by the GPS pseudorange and deltarange measurements in an Extended Kalman Filter (EKF) that employs the UDUT decomposition approach. The design is substantiated by simulation results to show the expected performance. C1 [Sud, Jastesh] Lockheed Martin Space Syst Co, M-S B3003,POB 179, Denver, CO 80201 USA. [Gay, Robert; Zanetti, Renato] NASA Johnson Space Ctr, Aerosci & Flight Mech Div, Houston, TX 77058 USA. [Holt, Greg] NASA Johnson Space Ctr, Flight Dynam Div, Houston, TX 77058 USA. RP Sud, J (reprint author), Lockheed Martin Space Syst Co, M-S B3003,POB 179, Denver, CO 80201 USA. EM jastesh.sud@lmco.com; robert.gay-l@nasa.gov; greg.n.holt@nasa.gov; renato.zanetti@nasa.gov NR 0 TC 1 Z9 1 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 499 EP 509 PG 11 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300037 ER PT S AU McNamara, LW Rea, JR AF McNamara, Luke W. Rea, Jeremy R. BE May, AJ TI DEFINITION OF THE DESIGN ENTRY TRAJECTORY AND ENTRY FLIGHT CORRIDOR FOR THE NASA ORION EXPLORATION MISSION 1 USING AN INTEGRATED APPROACH AND OPTIMIZATION SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB For NASA's Orion Exploration Mission 1 (EM-1) the Orion spacecraft is being designed to execute a guided skip-entry trajectory. In order to determine the design trajectory, an assessment of the entry flight corridor must first be completed. Defining the flyable entry flight corridor requires taking into account multiple subsystem constraints such as those on guided landing accuracy, service module debris disposal, Human System Interface Requirements, contingency entry modes, and structural loads in addition to flight test objectives. During the EM-1 Design Analysis Cycle 2 design changes occurred, due to mass reduction efforts, that made defining the flyable entry corridor for the EM-1 mission challenging. Approaches to characterize the domain space using discretized independent variables along with polynomial curve fitting of the resulting dependent variables are discussed. This paper describes the techniques, such as grid searches and iterative numerical optimization searches, that were explored to characterize the EM-1 entry flight corridor and define the design entry interface state with respect to key flight test constraints and objectives. C1 [McNamara, Luke W.] NASA Johnson Space Ctr, Flight Mech & Trajectory Design Branch, Houston, TX 77058 USA. [Rea, Jeremy R.] NASA Johnson Space Ctr, Flight Mech & Trajectory Design Branch, Houston, TX 77058 USA. RP McNamara, LW (reprint author), NASA Johnson Space Ctr, Flight Mech & Trajectory Design Branch, Houston, TX 77058 USA. EM luke.w.mcnamara@nasa.gov NR 20 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 529 EP 542 PG 14 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300039 ER PT S AU D'Souza, C Holt, G Gay, R Zanetti, R AF D'Souza, Christopher Holt, Greg Gay, Robert Zanetti, Renato BE May, AJ TI NAVIGATION DESIGN AND ANALYSIS FOR THE ORION CISLUNAR EXPLORATION MISSIONS SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB This paper details the design and analysis of the cislunar optical navigation system being proposed for the Orion Earth-Moon (EM) missions. In particular, it presents the mathematics of the navigation filter. It also presents the sensitivity analysis that has been performed to understand the performance of the proposed system, with particular attention paid to entry flight path angle constraints and the DV performance. C1 [D'Souza, Christopher; Gay, Robert; Zanetti, Renato] NASA Johnson Space Ctr, Aerosci & Flight Mech Div, 2101 NASA Pkwy, Houston, TX 77058 USA. [Holt, Greg] NASA Johnson Space Ctr, Missoin Operat Directorate, Houston, TX 77058 USA. RP D'Souza, C (reprint author), NASA Johnson Space Ctr, Aerosci & Flight Mech Div, 2101 NASA Pkwy, Houston, TX 77058 USA. EM chris.dsouza@nasa.gov; greg.n.holt@nasa.gov; robert.gay-1@nasa.gov; renato.zanetti@nasa.gov NR 7 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 543 EP 556 PG 14 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300040 ER PT S AU Gutkowski, JP Dawn, TF Jedrey, RM AF Gutkowski, Jeffrey P. Dawn, Timothy F. Jedrey, Richard M. BE May, AJ TI TRAJECTORY DESIGN ANALYSIS OVER THE LUNAR NODAL CYCLE FOR THE MULTI-PURPOSE CREW VEHICLE (MPCV) EXPLORATION MISSION 2 (EM-2) SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB The first crewed mission, Exploration Mission 2 (EM-2), for the MPCV Orion spacecraft is scheduled for August 2021, and its current mission is to orbit the Moon in a highly elliptical lunar orbit for three days. A 21-year scan was performed to identify feasible missions that satisfy the propulsive capabilities of the Interim Cryogenic Propulsion Stage (ICPS) and MPCV Service Module (SM). The mission is divided into 4 phases: (1) a lunar free return trajectory, (2) a hybrid maneuver, during the trans-lunar coast, to lower the approach perilune altitude to 100 km, (3) lunar orbit insertion into a 100 x 10,000 km orbit, and (4) lunar orbit loiter and Earth return to a splashdown off the coast of Southern California. Trajectory data was collected for all feasible missions and converted to information that influence different subsystems including propulsion, power, thermal, communications, and mission operations. The complete 21-year scan data shows seasonal effects that are due to the Earth-Moon geometry and the initial Earth parking orbit. The data and information is also useful to identify mission opportunities around the current planned launch date for EM-2. C1 [Gutkowski, Jeffrey P.; Dawn, Timothy F.; Jedrey, Richard M.] NASA, EG Aerosci & Flight Mech, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. RP Gutkowski, JP (reprint author), NASA, EG Aerosci & Flight Mech, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 557 EP 569 PG 13 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300041 ER PT S AU Dennehy, N AF Dennehy, Neil BE May, AJ TI SPACECRAFT HYBRID CONTROL AT NASA: A HISTORICAL LOOK BACK, CURRENT INITIATIVES, AND SOME FUTURE CONSIDERATIONS SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB There is a heightened interest within NASA for the design, development, and flight implementation of mixed-actuator hybrid attitude-control systems for science spacecraft that have less than three functional reaction wheel actuators. This interest is driven by a number of recent reaction wheels failures on aging, but still scientifically productive, NASA spacecraft. This paper describes the highlights of the first NASA Cross-Center Hybrid Control Workshop that was held in Greenbelt, Maryland in April of 2013 under the sponsorship of the NASA Engineering and Safety Center (NESC). A brief historical summary of NASA's past experiences with spacecraft mixed-actuator hybrid attitude control approaches, some of which were implemented inflight, will be provided. This paper will also convey some of the lessons learned and best practices captured at that workshop. Some relevant recent and current hybrid control activities will be described with an emphasis on work in support of a repurposed Kepler spacecraft. Specific technical areas for future considerations regarding spacecraft hybrid control will also be identified. C1 [Dennehy, Neil] NASA, Goddard Space Flight Ctr, GN&C, NESC, Mail Code 590, Greenbelt, MD 20771 USA. RP Dennehy, N (reprint author), NASA, Goddard Space Flight Ctr, GN&C, NESC, Mail Code 590, Greenbelt, MD 20771 USA. EM cornelius.j.dennehy@nasa.gov NR 18 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 583 EP 603 PG 21 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300043 ER PT S AU Stoneking, E Lebsock, K AF Stoneking, Eric Lebsock, Ken BE May, AJ TI POINTING AND MANEUVERING A SPACECRAFT WITH A RANK-DEFICIENT REACTION WHEEL COMPLEMENT SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB The Kepler spacecraft has suffered two reaction wheel failures, leaving two wheels remaining to perform attitude control. While Kepler may enlist thrusters and solar radiation pressure as control actuators, we investigate two complementary algorithms for controlling a Kepler-like spacecraft using the wheels only. First, we consider the problem of holding an inertial attitude. Some attitude drift in the uncontrolled axis is unavoidable, but a series of two-axis wheel maneuvers may be used to re-center the attitude. We present the performance and limitations of this technique. Second, we consider periodically performing a 180 degrees maneuver to enable passive momentum unloading as a fuel conservation measure. We show that an attitude control law feeding back attitude, attitude rate, and wheel momentum errors may be employed to perform this maneuver while keeping the telescope boresight a safe angle away from the direction of the Sun. C1 [Stoneking, Eric] NASA, Goddard Space Flight Ctr, Code 591, Greenbelt, MD 20771 USA. [Lebsock, Ken] Orbital Sci Tech Serv Div, Greenbelt, MD 20770 USA. RP Stoneking, E (reprint author), NASA, Goddard Space Flight Ctr, Code 591, Greenbelt, MD 20771 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 617 EP 626 PG 10 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300045 ER PT S AU Smith, BA Lim, RS Fieseler, PD AF Smith, Brett A. Lim, Ryan S. Fieseler, Paul D. BE May, AJ TI DAWN SPACECRAFT OPERATIONS WITH HYBRID CONTROL: IN-FLIGHT PERFORMANCE AND CERES APPLICATIONS SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB Dawn is a low-thrust interplanetary spacecraft currently en-route to the asteroid Ceres following a successful 14-month visit to Vesta, to better understand the early creation of the solar system. The Dawn spacecraft uses both reaction wheel assemblies (RWA) and a reaction control system (RCS) to provide 3-axis attitude control for the spacecraft. Reaction wheels were designed to be the primary system for attitude control, however two of the wheels have shown high friction anomalies and have been removed from service. The project has implemented a hybrid control algorithm using two healthy reaction wheels and RCS thrusters to provide the most science return at Ceres. With only two remaining healthy RWAs, hybrid control became part of the baseline plan for Ceres science operations. There are a number of operational complexities and changes that must be accommodated to make this new control method function effectively in coordination with the desired science observations. Using two RWAs in a hybrid configuration to control two of the three spacecraft axes increases operational complexity. The benefit of the increased complexity is reduced hydrazine use as well as more accurate pointing, when compared to all-RCS control. Hydrazine propellant for the RCS thrusters is the major constraining resource for the Dawn mission, making the hybrid controller very desirable for science acquisition. This paper discusses Dawn's attitude control flight experiences with hybrid control and planned hybrid control use in Ceres orbit operations. Actual Flight data under hybrid control are presented and compared with simulation predictions. Operational considerations for preparing Dawn to use a hybrid actuator configuration are outlined as well. The discussion also includes the science operational plan for using hybrid control in Ceres orbit. Lastly, some considerations that should be of interest to similar reduced-actuator missions are presented. C1 [Smith, Brett A.; Lim, Ryan S.] CALTECH, Jet Prop Lab, Guidance & Control Sect, M-S 264-854,4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Fieseler, Paul D.] CALTECH, Jet Prop Lab, Flight Operat Sect, Pasadena, CA 91109 USA. RP Smith, BA (reprint author), CALTECH, Jet Prop Lab, Guidance & Control Sect, M-S 264-854,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Brett.A.Smith@jpl.nasa.gov; Ryan.S.Lim@jpl.nasa.gov; Paul.D.Fieseler@jpl.nasa.gov NR 6 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 671 EP 683 PG 13 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300049 ER PT S AU San Martin, M Mendeck, GF Brugarolas, PB Singh, G Serricchio, F AF San Martin, Miguel Mendeck, Gavin F. Brugarolas, Paul B. Singh, Gurkirpal Serricchio, Frederick BE May, AJ TI RECONSTRUCTED FLIGHT PERFORMANCE OF THE MARS SCIENCE LABORATORY GUIDANCE, NAVIGATION, AND CONTROL SYSTEM FOR ENTRY, DESCENT, AND LANDING SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB The Mars Science Laboratory (MSL) project landed successfully the rover Curiosity in Gale crater in August 5, 2012, after going through a complex and risky Entry, Descent, and Landing (EDL) sequence that demonstrated a series of innovations and advances in the area of Guidance, Navigation, and Control (GN&C) that resulted in a quantum leap in Mars EDL performance. Among those were the first use at Mars of Entry Guidance to reduce the size of the landing ellipse and the first use of the SkyCrane landing architecture to place a one-ton class rover on the surface of the red planet. Given the first time nature and the associated risks of the new and bold EDL/GN&C design, the project was committed from the start to implement a comprehensive telemetry system for post landing reconstruction of its performance. This paper will give a high level description of the design of the MSL EDL/GN&C system and its performance requirements, the areas of highest uncertainty and risk as understood prior to the arrival to Mars, and its resulting flight performance as reconstructed after landing. C1 [San Martin, Miguel] CALTECH, Jet Prop Lab, Guidance & Control Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Mendeck, Gavin F.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Brugarolas, Paul B.] CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, Guidance & Control Sect, Pasadena, CA 91109 USA. [Singh, Gurkirpal; Serricchio, Frederick] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP San Martin, M (reprint author), CALTECH, Jet Prop Lab, Guidance & Control Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 771 EP 800 PG 30 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300056 ER PT S AU Wallace, MS Roncoli, RB Young, BT Hatch, SJ AF Wallace, Mark S. Roncoli, Ralph B. Young, Brian T. Hatch, Sara J. BE May, AJ TI THE LAST DAYS OF GRAIL SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB The Gravity Recovery and Interior Laboratory (GRAIL) extended mission ended on December 17th, 2012 after both spacecraft impacted the side of a small unnamed lunar "mountain" at approximately 75.6 degrees N latitude, 333.2 degrees E longitude. This end was the culmination of a deliberate choice on the part of the Project to eke out every possible gram of scientific and engineering value from the propellant remaining on board. This paper details the design processes and choices made for the last six weeks of the extended mission, from the initial discussions for the Orientale Campaign in June 2012 and concluding with mission's dramatic end six months later. C1 [Wallace, Mark S.; Roncoli, Ralph B.; Young, Brian T.; Hatch, Sara J.] CALTECH, Jet Prop Lab, Mission Design & Nav Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Wallace, MS (reprint author), CALTECH, Jet Prop Lab, Mission Design & Nav Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 859 EP 870 PG 12 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300062 ER PT S AU Anzalone, EJ AF Anzalone, Evan J. BE May, AJ TI UNIFIED SIMULATION AND ANALYSIS FRAMEWORK FOR DEEP SPACE NAVIGATION DESIGN SO GUIDANCE, NAVIGATION, AND CONTROL 2014 SE Advances in the Astronautical Sciences LA English DT Proceedings Paper CT 37th Annual AAS Rocky Mountain Section Guidance and Control Conference CY JAN 31-FEB 05, 2014 CL Rocky Mt Sect, Breckenridge, CO HO Rocky Mt Sect AB Due to the complex nature of deep space navigation, design, analysis, and validation heavily rely on software tools. These are used to support all phases of design from initial phase A-type studies up to flight validation and post-flight analysis. These tools are typically problem- and method-dependent. In order to allow for a common simulation environment for navigation analysis and design, this paper presents a unified framework developed using Model-Based Systems Engineering techniques to describe the notional navigation problem, as well as the analytical framework and its implementation. The functions, processes, and composition of the navigation system and the analysis framework are described using the Systems Model Language (SysML). The utilization of SysML and Model-Based Systems Engineering enables the designer to capture the requirements of the navigation system as well as its implementation and analysis. This model development feeds directly into the development of analytical elements and provides for ease of implementation as well as application to additional navigation problems. This paper describes the development and implementation of a unified simulation and analysis framework for deep space navigation design. C1 [Anzalone, Evan J.] NASA, Marshall Space Flight Ctr, EV42, Huntsville, AL 35812 USA. RP Anzalone, EJ (reprint author), NASA, Marshall Space Flight Ctr, EV42, Huntsville, AL 35812 USA. NR 33 TC 0 Z9 0 U1 0 U2 0 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 1081-6003 BN 978-0-87703-609-8 J9 ADV ASTRONAUT SCI PY 2014 VL 151 BP 873 EP 884 PG 12 WC Automation & Control Systems; Engineering, Aerospace SC Automation & Control Systems; Engineering GA BE4FS UT WOS:000371654300063 ER PT J AU Kotov, D Yee, HC Sjogreen, B AF Kotov, Dmitry Yee, H. C. Sjogreen, Bjorn BE Ancona, F Bressan, A Marcati, P Marson, A TI COMPARATIVE STUDY OF HIGH-ORDER POSITIVITY-PRESERVING WENO SCHEMES SO HYPERBOLIC PROBLEMS: THEORY, NUMERICS, APPLICATIONS SE AIMS Series on Applied Mathematics LA English DT Proceedings Paper CT 14th International Conference devoted to Theory, Numerics and Applications of Hyperbolic Problems (HYP) CY JUN 24-29, 2012 CL Padova, ITALY SP Univ Padova, Dipartimento Matematica, Univ Studi Aquila, Dipartimento Matematica Pura Applicata, Univ Padova, Univ Zurich, Univ Basel DE Positivity-preserving algorithms; WENO; Noh problem ID SHOCK-CAPTURING SCHEMES; STIFF SOURCE TERMS; EFFICIENT IMPLEMENTATION; EQUATIONS; RESOLUTION AB The objective of this study is to compare the results obtained by different non-positivity-preserving methods with the two recently developed high-order positivity-preserving schemes. Several test cases are considered, including classical Noh and Sedov 3D cases and also shock tube calculations related to NASA experiments. Studies indicate that the positivity preserving schemes produce more stable results than regular methods for the considered test cases. However some of the regular methods may obtain slightly more accurate results then the new methods for the certain problems. C1 [Kotov, Dmitry] Stanford Univ, Ctr Turbulence Res, 488 Escondido Mall Bldg 500, Stanford, CA 94305 USA. [Yee, H. C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sjogreen, Bjorn] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. RP Kotov, D (reprint author), Stanford Univ, Ctr Turbulence Res, 488 Escondido Mall Bldg 500, Stanford, CA 94305 USA. EM dkotov@stanford.edu; Helen.M.Yee@nasa.gov; sjogreen2@llnl.gov NR 17 TC 0 Z9 0 U1 0 U2 0 PU AMER INST MATHEMATICAL SCIENCES-AIMS PI SPRINGFIELD PA PO BOX 2604, SPRINGFIELD, MO 65801-2604 USA BN 978-1-60133-017-8 J9 AIMS SER APPL MATH PY 2014 VL 8 BP 1047 EP 1058 PG 12 WC Mathematics, Applied; Physics, Mathematical SC Mathematics; Physics GA BF6WY UT WOS:000383745000115 ER PT S AU Baker, S Baru, C Bryson, G Buechler, B Crosby, C Fielding, E Meertens, C Nicoll, J Youn, C AF Baker, S. Baru, C. Bryson, G. Buechler, B. Crosby, C. Fielding, E. Meertens, C. Nicoll, J. Youn, C. BE Toth, C Holm, T Jutzi, B TI Seamless Synthetic Aperture Radar Archive for Interferometry Analysis SO ISPRS TECHNICAL COMMISSION I SYMPOSIUM SE International Archives of the Photogrammetry Remote Sensing and Spatial Information Sciences LA English DT Proceedings Paper CT ISPRS Technical Commission I Symposium CY NOV 17-20, 2014 CL Denver, CO SP Int Soc Photogrammetry & Remote Sensing Tech Commiss, ASPRS Pecora Fall Meeting DE Radar; SAR; DEM; Data Mining; Processing; Archiving; Change Detection AB The NASA Advancing Collaborative Connections for Earth System Science (ACCESS) seamless synthetic aperture radar (SAR) archive (SSARA) project is a collaboration between UNAVCO, the Alaska Satellite Facility (ASF), the Jet Propulsion Laboratory (JPL), and OpenTopography at the San Diego Supercomputer Center (SDSC) to design and implement a seamless distributed access system for SAR data and derived interferometric SAR (InSAR) data products. A unified application programming interface (API) has been created to search the SAR archives at ASF and UNAVCO, 30 and 90-m SRTM DEM data available through OpenTopography, and tropospheric data from the NASA OSCAR project at JPL. The federated query service provides users a single access point to search for SAR granules, InSAR pairs, and corresponding DEM and tropospheric data products from the four archives, as well as the ability to search and download pre-processed InSAR products from ASF and UNAVCO. [GRAPHICS] . C1 [Baker, S.; Crosby, C.; Meertens, C.] UNAVCO, Boulder, CO USA. [Bryson, G.; Buechler, B.; Nicoll, J.] Univ Alaska Fairbanks, Inst Geophys, Alaska Satellite Facil, Fairbanks, AK 99775 USA. [Fielding, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Baru, C.; Youn, C.] Univ Calif San Diego, San Diego Supercomp Ctr, La Jolla, CA 92093 USA. RP Buechler, B (reprint author), Univ Alaska Fairbanks, Inst Geophys, Alaska Satellite Facil, Fairbanks, AK 99775 USA. EM baker@unavco.org; baru@sdsc.edu; gbryson@alaska.edu; btbuechler@alaska.edu; crosby@unavco.org; eric.j.fielding@jpl.nasa.gov; meertens@unavco.org; jbnicoll@alaska.edu; cyoun@sdsc.edu OI Baker, Scott/0000-0003-4802-8371 NR 8 TC 0 Z9 0 U1 1 U2 2 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLE 1E, GOTTINGEN, 37081, GERMANY SN 2194-9034 J9 INT ARCH PHOTOGRAMM PY 2014 VL 40-1 BP 65 EP 72 DI 10.5194/isprsarchives-XL-1-65-2014 PG 8 WC Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA BE1RQ UT WOS:000368435600010 ER PT S AU Schnase, JL Carroll, ML Weber, KT Brown, ME Gill, RL Wooten, M May, J Serr, K Smith, E Goldsby, R Newtoff, K Bradford, K Doyle, C Volker, E Weber, S AF Schnase, J. L. Carroll, M. L. Weber, K. T. Brown, M. E. Gill, R. L. Wooten, M. May, J. Serr, K. Smith, E. Goldsby, R. Newtoff, K. Bradford, K. Doyle, C. Volker, E. Weber, S. BE Toth, C Holm, T Jutzi, B TI AN AUTOMATED CLOUD-BASED DECISION SUPPORT SYSTEM FOR POST-FIRE REHABILITATION PLANNING SO ISPRS TECHNICAL COMMISSION I SYMPOSIUM SE International Archives of the Photogrammetry Remote Sensing and Spatial Information Sciences LA English DT Proceedings Paper CT ISPRS Technical Commission I Symposium CY NOV 17-20, 2014 CL Denver, CO SP Int Soc Photogrammetry & Remote Sensing Tech Commiss, ASPRS Pecora Fall Meeting DE Decision support systems; DSS; burned area emergency response; BAER; emergency stabilization and rehabilitation; ESR; cloud computing; rapid response ID FIRE; EROSION; RANGELANDS; KNAPWEED; WILDFIRE; IMPACTS; IDAHO AB RECOVER is a site-specific decision support system that automatically brings together in a single analysis environment the information necessary for post-fire rehabilitation decision-making. After a major wildfire, law requires that the federal land management agencies certify a comprehensive plan for public safety, burned area stabilization, resource protection, and site recovery. These burned area emergency response (BAER) plans are a crucial part of our national response to wildfire disasters and depend heavily on data acquired from a variety of sources. Final plans are due within 21 days of control of a major wildfire and become the guiding document for managing the activities and budgets for all subsequent remediation efforts. There are few instances in the federal government where plans of such wide-ranging scope and importance are assembled on such short notice and translated into action more quickly. RECOVER has been designed in close collaboration with our agency partners and directly addresses their high-priority decision-making requirements. In response to a fire detection event, RECOVER uses the rapid resource allocation capabilities of cloud computing to automatically collect Earth observational data, derived decision products, and historic biophysical data so that when the fire is contained, BAER teams will have a complete and ready-to-use RECOVER dataset and GIS analysis environment customized for the target wildfire. Initial studies suggest that RECOVER can transform this information-intensive process by reducing from days to a matter of minutes the time required to assemble and deliver crucial wildfire-related data. C1 [Schnase, J. L.; Gill, R. L.] NASA Goddard Space Flight Ctr, Off Computat & Informat Sci & Technol, Greenbelt, MD 20771 USA. [Carroll, M. L.; Brown, M. E.; Wooten, M.] NASA Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD USA. [Newtoff, K.; Bradford, K.; Doyle, C.; Volker, E.; Weber, S.] NASA Goddard Space Flight Ctr, DEVELOP Program Off, Greenbelt, MD USA. [Weber, K. T.; May, J.; Serr, K.; Smith, E.; Goldsby, R.] Idaho State Univ, GIS Training & Res Ctr, Pocatello, ID 83209 USA. RP Schnase, JL (reprint author), NASA Goddard Space Flight Ctr, Off Computat & Informat Sci & Technol, Greenbelt, MD 20771 USA. EM john.l.schnase@nasa.gov; mark.carroll@nasa.gov; webekeit@isu.edu; molly.e.brown@nasa.gov; roger.l.gill@nasa.gov; margaret.wooten@nasa.gov; mayjeff2@isu.edu; serrkind@isu.edu; smiteri6@isu.edu; goldrya2@isu.edu; kiersten.newtoff@nasa.gov; kathryn.bradford@nasa.gov; colin.s.doyle@nasa.gov; emily.volker@nasa.gov; samuel.j.weber@nasa.gov RI Brown, Molly/E-2724-2010 OI Brown, Molly/0000-0001-7384-3314 NR 23 TC 1 Z9 1 U1 2 U2 3 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLE 1E, GOTTINGEN, 37081, GERMANY SN 2194-9034 J9 INT ARCH PHOTOGRAMM PY 2014 VL 40-1 BP 363 EP 370 DI 10.5194/isprsarchives-XL-1-363-2014 PG 8 WC Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA BE1RQ UT WOS:000368435600054 ER PT J AU Marinova, MM Meckler, AN McKay, CP AF Marinova, Margarita M. Meckler, A. Nele McKay, Christopher P. TI Holocene freshwater carbonate structures in the hyper-arid Gebel Uweinat region of the Sahara Desert (Southwestern Egypt) SO JOURNAL OF AFRICAN EARTH SCIENCES LA English DT Article DE Carbonate structures; Gebel Uweinat; Sahara Desert; Holocene climate ID EASTERN SAHARA; ARABIAN PENINSULA; LATE PLEISTOCENE; NORTHERN SUDAN; PAVILION LAKE; HUMID PERIOD; AFRICA; EVOLUTION; STROMATOLITES; GEOCHRONOLOGY AB The eastern part of the Sahara is at present the driest region of the desert. Yet the extensive animal rock art in the area, presumed to depict real activities in the lives of the painters, suggests that environmental conditions were significantly different when the rock art was produced. Here we report on exploration of the area, which led to the discovery of morphologically-distinct carbonate structures that line the walls of two valleys in Gebel Uweinat, and were likely formed in standing water. The carbonate structures comprise what appear to be shoreline carbonate formations, and date back to 8100 and 9400 years BP. The chemical and morphological similarity of these formations to carbonate structures from modern lakes suggests that these lakes contained fresh, standing water suitable for human and animal use. However, the significant quartz content suggests that windblown sand was pervasive, and thus the vegetation cover may have been sparse. This discovery supports the possibility of grasslands in the area, which may have been able to support human habitation, and adds to the evidence for a wetter climate in the area in the early Holocene. (C) 2013 The Authors. Published by Elsevier Ltd. All rights reserved. C1 [Marinova, Margarita M.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Marinova, Margarita M.; McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Meckler, A. Nele] ETH, Inst Geol, CH-8092 Zurich, Switzerland. RP McKay, CP (reprint author), NASA, Ames Res Ctr, Div Space Sci, MS 245-3, Moffett Field, CA 94035 USA. EM nele.meckler@erdw.ethz.ch; chris.mckay@nasa.gov FU NASA Astrobiology program; NSERC postgraduate fellowship; Canadian Space Agency supplement; German Research Foundation FX We thank George Rossman, Jess Adkins, Sebastian Breitenbach, Rich Chomko, Fliegel Jezerniczky Expeditions, the members of the field party, and the field leader and guide Andras Zboray. Funding was provided by the NASA Astrobiology program, an NSERC postgraduate fellowship, a Canadian Space Agency supplement, and a research scholarship from the German Research Foundation. NR 40 TC 1 Z9 1 U1 1 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1464-343X EI 1879-1956 J9 J AFR EARTH SCI JI J. Afr. Earth Sci. PD JAN PY 2014 VL 89 BP 50 EP 55 DI 10.1016/j.jafrearsci.2013.10.003 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 268NV UT WOS:000328178500005 ER PT S AU Petit, V Cohen, DH Naze, Y Gagne, M Townsend, RHD Leutenegger, MA Ud-Doula, A Owocki, SP Wade, GA AF Petit, V. Cohen, D. H. Naze, Y. Gagne, M. Townsend, R. H. D. Leutenegger, M. A. ud-Doula, A. Owocki, S. P. Wade, G. A. BE Petit, P Jardine, M Spruit, HC TI X-rays from magnetic massive OB stars SO MAGNETIC FIELDS THROUGHOUT STELLAR EVOLUTION SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 302nd Symposium of the International-Astronomical-Union (IAU) CY AUG 25-30, 2013 CL Biarritz, FRANCE SP Int Astronom Union DE Stars; early-type; Stars; magnetic fields ID DRIVEN STELLAR WINDS; EMISSION; VARIABILITY; EVOLUTION; MODELS AB The magnetic activity of solar-type and low-mass stars is a well known source of coronal X-ray emission. At the other end of the main sequence, X-rays emission is instead associated with the powerful, radiatively driven winds of massive stars. Indeed, the intrinsically unstable line-driving mechanism of OB star winds gives rise to shock-heated, soft emission (similar to 0.5keV) distributed throughout the wind. Recently, the latest generation of spectropolarimetric instrumentation has uncovered a population of massive OB-stars hosting strong, organized magnetic fields. The magnetic characteristics of these stars are similar to the apparently fossil magnetic fields of the chemically peculiar ApBp stars. Magnetic channeling of these OB stars' strong winds leads to the formation of large-scale shock-heated magnetospheres, which can modify UV resonance lines, create complex distributions of cooled Halpha emitting material, and radiate hard (similar to 2-5 keV) X-rays. This presentation summarizes our coordinated observational and modelling efforts to characterize the manifestation of these magnetospheres in the X-ray domain, providing an important contrast between the emission originating in shocks associated with the large-scale fossil fields of massive stars, and the X-rays associated with the activity of complex, dynamo-generated fields in lower-mass stars. C1 [Petit, V.; Owocki, S. P.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Cohen, D. H.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Naze, Y.] Univ Liege, GAPHE Dept, AGO, Liege, Belgium. [Gagne, M.] West Chester Univ, Dept Geol & Astron, W Chester, PA USA. [Townsend, R. H. D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Leutenegger, M. A.] NASA, GSFC, High Energy Astrophys Lab, Greenbelt, MD USA. [ud-Doula, A.] Penn State Worthington Scranton, Dunmore, PA USA. [Wade, G. A.] Royal Mil Coll Canada, Dept Phys, Kingston, ON, Canada. RP Petit, V (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. EM vpetit@udel.edu OI Naze, Yael/0000-0003-4071-9346 NR 19 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-1-107-04498-2 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2014 VL 302 BP 330 EP 333 DI 10.1017/S1743921314002427 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BG3DM UT WOS:000387896800081 ER PT B AU Kotov, DV Yee, HC Sjogreen, B AF Kotov, D. V. Yee, H. C. Sjogreen, B. BE Pogorelov, NV Audit, E Zank, GP TI Performance of Improved High-order Filter Schemes for Turbulent Flows with Shocks SO NUMERICAL MODELING OF SPACE PLASMA FLOWS: ASTRONUM-2013 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 8th International Conference on Numerical Modeling of Space Plasma Flows: ASTRONUM-2013 CY JUL 01-05, 2013 CL Biarritz, FRANCE SP Univ Alabama Huntsville, Ctr Space Plasma & Aeronom Res, Maison Simulat AB We demonstrate the performance of the improved filter schemes of Yee & Sjogreen (2009) on a set of test cases involving different flow types. The idea behind the scheme improvement is to obtain high accuracy of the results and at the same time to avoid additional tuning of the scheme parameters depending on flow conditions. We show that using a local treatment of the dissipation control parameter kappa one can obtain more accurate results than in case of using constant or global parameter with no additinal tuning implied. C1 [Kotov, D. V.] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA. [Yee, H. C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sjogreen, B.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. RP Kotov, DV (reprint author), Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA. NR 8 TC 0 Z9 0 U1 1 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-860-2 J9 ASTR SOC P PY 2014 VL 488 BP 237 EP 242 PG 6 WC Astronomy & Astrophysics; Mathematics, Applied SC Astronomy & Astrophysics; Mathematics GA BE7YY UT WOS:000376047800033 ER PT B AU Feynman, J Ruzmaikin, A AF Feynman, Joan Ruzmaikin, Alexander BE Hu, Q Zank, GP TI Minima of the Centennial Gleissberg Cycle and the Heliospheric Boundary SO OUTSTANDING PROBLEMS IN HELIOPHYSICS: FROM CORONAL HEATING TO THE EDGE OF THE HELIOSPHERE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 12th Annual International Astrophysics Conference CY APR 14-19, 2013 CL Myrtle Beach, SC SP Univ Alabama Huntsville, Ctr Space Plasma & Aeron Res ID SOLAR-WIND; GEOMAGNETIC-ACTIVITY; CENTURIES; FIELDS AB The Centennial Gleissberg Cycle (CGC) is a 90-100 year variation observed on the Sun, in the solar wind, at Earth and throughout the Heliosphere. The CGC is expressed as a systematic variation of the amplitude of the 11-year sunspot cycle. The reality of the CGC was a matter of some debate, but the very weak solar wind that occurred during the recent transition from solar cycle 23 to 24 followed by a low cycle 24 maximum sunspot number, strongly supports the concept. In this paper we demonstrate the strong similarities among the CGC minima observed at the beginnings of the 18th, 19th, 20th, and 21st century. These similarities support the notion that we are now experiencing a typical CGC minimum solar wind that is significantly different from the solar wind observed earlier in the space age. We suggest that the current CGC minimum may be implicated in producing some aspects of the unexpected observations at the heliosphere boundary reported at this conference. C1 [Feynman, Joan; Ruzmaikin, Alexander] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Feynman, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 19 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-853-4; 978-1-58381-852-7 J9 ASTR SOC P PY 2014 VL 484 BP 36 EP 41 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE6KY UT WOS:000374279900006 ER PT B AU Gopalswamyl, N Makela, P AF Gopalswamyl, N. Makela, P. BE Hu, Q Zank, GP TI Latitudinal Connectivity of Ground Level Enhancement Events SO OUTSTANDING PROBLEMS IN HELIOPHYSICS: FROM CORONAL HEATING TO THE EDGE OF THE HELIOSPHERE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 12th Annual International Astrophysics Conference CY APR 14-19, 2013 CL Myrtle Beach, SC SP Univ Alabama Huntsville, Ctr Space Plasma & Aeron Res ID CORONAL MASS EJECTIONS; MICROWAVE OBSERVATIONS; SOLAR SOURCES AB We examined the source regions and coronal environment of the historical ground level enhancement (GLE) events in search of evidence for non-radial motion of the associated coronal mass ejection (CME). For the 13 GLE events that had source latitudes >30 degrees we found evidence for possible non-radial CME motion due to deflection by large-scale magnetic structures in nearby coronal holes, streamers, or pseudo streamers. Polar coronal holes are the main source of deflection in, the rise and declining phases of solar cycles. In the maximum phase, deflection by large-scale streamers or pseudo streamers overlying high-latitude filaments seems to be important. The BO angle reduced the ecliptic distance of some GLE source regions and increased in others with the net result that the average latitude of GLE events did not change significantly. The non-radial CME motion is the dominant factor that reduces the ecliptic distance of GLE source regions, thereby improving the latitudinal connectivity to Earth. We further infer that the GLE particles must be accelerated at the nose part of the CME-driven shocks, where the shock is likely to be quasi-parallel. C1 [Gopalswamyl, N.; Makela, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Makela, P.] Catholic Univ Amer, Washington, DC 20064 USA. RP Gopalswamyl, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 20 TC 6 Z9 6 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-853-4; 978-1-58381-852-7 J9 ASTR SOC P PY 2014 VL 484 BP 63 EP 71 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE6KY UT WOS:000374279900010 ER PT B AU Leske, RA Cummings, AC Cohen, CMS Mewaldt, RA Labrador, AW Stone, EC Wiedenbeck, ME Christian, ER von Rosenvinge, TT AF Leske, R. A. Cummings, A. C. Cohen, C. M. S. Mewaldt, R. A. Labrador, A. W. Stone, E. C. Wiedenbeck, M. E. Christian, E. R. von Rosenvinge, T. T. BE Hu, Q Zank, GP TI Observations of Loss-Cone Pitch Angle Distributions of Solar Energetic Particles SO OUTSTANDING PROBLEMS IN HELIOPHYSICS: FROM CORONAL HEATING TO THE EDGE OF THE HELIOSPHERE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 12th Annual International Astrophysics Conference CY APR 14-19, 2013 CL Myrtle Beach, SC SP Univ Alabama Huntsville, Ctr Space Plasma & Aeron Res ID STEREO MISSION; PROPAGATION; EVENT AB Pitch angle distributions of solar energetic particles (SEPs) in interplanetary space sometimes exhibit a loss cone in which an incident beam of particles is partially mirrored; particles with large pitch angles are reflected while those with smaller pitch angles are not. Mirroring requires a magnetic field enhancement, but if the field strength is not large enough to turn around particles with the smallest pitch angles or if these particles scatter before reaching their more distant mirror points, a loss cone forms. Such distributions therefore provide information on the interplanetary environment far from the spacecraft. The Low Energy Telescopes onboard the twin STEREO spacecraft have detected loss-cone distributions in several SEP events. We present some of these and other interesting anisotropy observations, and discuss their implications for SEP transport. In particular, we find that the shapes of the pitch angle distributions generally vary with energy and species, with lower energy particles usually more anisotropic than higher energy particles. Comparison with theory may be used to determine the energy and rigidity dependences of the pitch angle diffusion coefficient. C1 [Leske, R. A.; Cummings, A. C.; Cohen, C. M. S.; Mewaldt, R. A.; Labrador, A. W.; Stone, E. C.] CALTECH, Pasadena, CA 91125 USA. [Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Christian, E. R.; von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Leske, RA (reprint author), CALTECH, Pasadena, CA 91125 USA. NR 18 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-853-4; 978-1-58381-852-7 J9 ASTR SOC P PY 2014 VL 484 BP 117 EP 122 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE6KY UT WOS:000374279900018 ER PT B AU Ruzmaikin, A Feynman, J AF Ruzmaikin, Alexander Feynman, Joan BE Hu, Q Zank, GP TI The Centennial Gleissberg Cycle: Origin and Forcing of Climate SO OUTSTANDING PROBLEMS IN HELIOPHYSICS: FROM CORONAL HEATING TO THE EDGE OF THE HELIOSPHERE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 12th Annual International Astrophysics Conference CY APR 14-19, 2013 CL Myrtle Beach, SC SP Univ Alabama Huntsville, Ctr Space Plasma & Aeron Res ID MEAN-FIELD DYNAMO; IRRADIANCE VARIATIONS; SOLAR-ACTIVITY; GRAND MINIMA AB We discuss the origin of the Centennial Gleissberg Cycle (CGC) of solar activity and its forcing of the Earth's climate. The solar dynamo models, which explain the process of generating the 11-year cycle via the differential rotation and mean helicity, need to be extended to a non-linear regime that includes feedback processes. The strongest feedback on the centennial time scale is expected from the mean helicity. We advocate that the best way to see the response of the Earth's climate to the CGC forcing is to investigate the climate patterns, not the global temperature. There is anecdotal evidence of extreme low temperatures in the climate patterns at the GCC minima. Numerical modeling indicates a patterned response of the ocean to the CGC forcing. C1 [Ruzmaikin, Alexander; Feynman, Joan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ruzmaikin, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NR 28 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-853-4; 978-1-58381-852-7 J9 ASTR SOC P PY 2014 VL 484 BP 189 EP 194 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE6KY UT WOS:000374279900029 ER PT B AU Thejappa, G MacDowall, RJ AF Thejappa, G. MacDowall, R. J. BE Hu, Q Zank, GP TI Non-linear Effects Associated with Solar Type III Radio Bursts SO OUTSTANDING PROBLEMS IN HELIOPHYSICS: FROM CORONAL HEATING TO THE EDGE OF THE HELIOSPHERE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 12th Annual International Astrophysics Conference CY APR 14-19, 2013 CL Myrtle Beach, SC SP Univ Alabama Huntsville, Ctr Space Plasma & Aeron Res AB Some of the Langmuir wave packets and associated density cavities observed by the STEREO spacecraft in the source regions of solar type In radio bursts indicate that they probably correspond to collapsing envelope soliton-caviton pairs. We present the observations of one of such wave packets, whose spectrum contains harmonic peaks at f(pe), 2f(pe), and 3f(pe) (f(pe) is the electron plasma frequency). We show that frequencies, wave numbers and phases of the waves corresponding to these spectral peaks satisfy the resonance conditions of three wave interactions: L-1 + L-2 -> T-2fpe and L + T-2fpe -> T-3fpe, where L-1, L-2 and L correspond to Langmuir waves, and T-2fpe and T-3fpe correspond to second and third harmonic electromagnetic waves, respectively. C1 [Thejappa, G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [MacDowall, R. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Thejappa, G (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-853-4; 978-1-58381-852-7 J9 ASTR SOC P PY 2014 VL 484 BP 210 EP 215 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE6KY UT WOS:000374279900032 ER PT B AU Verkhoglyadova, OP Wang, SH AF Verkhoglyadova, Olga P. Wang, Shuhui BE Hu, Q Zank, GP TI Middle Atmosphere Response to Large SEP Events: September 2005 Event SO OUTSTANDING PROBLEMS IN HELIOPHYSICS: FROM CORONAL HEATING TO THE EDGE OF THE HELIOSPHERE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 12th Annual International Astrophysics Conference CY APR 14-19, 2013 CL Myrtle Beach, SC SP Univ Alabama Huntsville, Ctr Space Plasma & Aeron Res ID SOLAR PROTON EVENTS; ENERGETIC PARTICLE EVENTS; NORTHERN-HEMISPHERE; ACCELERATION; MLS AB Solar proton events (SPEs) have been shown to affect chemical balance of the middle atmosphere (from 60 to 90 km in altitude). Solar protons of energies above 10 MeV penetrate deep into the atmosphere temporarily inducing production of chemically active odd hydrogen species (HOx, primarily OH and HO2) which in turn causes ozone (O-3) destruction. Latitudinal extend of HO signature is dependent on the geomagnetic cut-off latitude and changes due to geomagnetic conditions, especially during geomagnetic storms. The Microwave Limb Sounder (MLS) launched onboard Aura satellite in 2004 provides daily simultaneous measurements of HOx, O-3 and related parameters such as H2O and temperature on a global scale during both day and night. This is the first time that global measurements of odd hydrogen species are made on a daily basis. We will present an example of a large solar energetic particle (SEP) event of September 2005 and corresponding middle atmospheric signatures. We will demonstrate enhancements in nighttime odd hydrogen density (up to 500%) and decreases in nighttime ozone density (similar to 50%) concomitant with the SEP event. We advocate a study of how different types of SEP events affect composition and dynamics of the middle atmosphere in different latitude and altitude ranges. C1 [Verkhoglyadova, Olga P.] UAH, Ctr Space Plasma & Aeron Res, Huntsville, AL USA. [Verkhoglyadova, Olga P.; Wang, Shuhui] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Verkhoglyadova, OP (reprint author), UAH, Ctr Space Plasma & Aeron Res, Huntsville, AL USA. NR 19 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-853-4; 978-1-58381-852-7 J9 ASTR SOC P PY 2014 VL 484 BP 216 EP 221 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE6KY UT WOS:000374279900033 ER PT B AU Wiedenbeck, ME Mason, GM AF Wiedenbeck, M. E. Mason, G. M. BE Hu, Q Zank, GP TI The Interplanetary Population of Suprathermal Ions from Impulsive Solar Energetic Particle Events: Solar Cycle Variations SO OUTSTANDING PROBLEMS IN HELIOPHYSICS: FROM CORONAL HEATING TO THE EDGE OF THE HELIOSPHERE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 12th Annual International Astrophysics Conference CY APR 14-19, 2013 CL Myrtle Beach, SC SP Univ Alabama Huntsville, Ctr Space Plasma & Aeron Res ID HE-3-RICH EVENTS; SEED POPULATION; 1 AU; HELIOSPHERE; HE-3; SUN AB Suprathermal ions in the solar corona or interplanetary medium play an important role in the determining the accelerated particle population produced by CME-driven shocks. Impulsive solar energetic particle events provide one of the sources of interplanetary suprathermals, and the presence of this material is detectable based on its unique composition in which the ion He-3 is normally enhanced by several orders of magnitude over its typical solar wind abundance. Using composition measurements made with instruments on NASA's Advanced Composition Explorer between 1997 and 2013 we have investigated the solar cycle variation of suprathermals from impulsive events over more than a full solar cycle. We find that the fraction of time with energetic 3He detectable in the interplanetary medium near 1 AU dropped by more than a factor of 100 between the cycle 23 solar maximum and the following minimum. Comparison between the rising portions of cycles 23 and 24 shows that the fraction of time with 3He present is significantly lower in the present solar cycle. C1 [Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Mason, G. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Wiedenbeck, ME (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 14 TC 0 Z9 0 U1 1 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-853-4; 978-1-58381-852-7 J9 ASTR SOC P PY 2014 VL 484 BP 234 EP 240 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE6KY UT WOS:000374279900036 ER PT B AU Bringsjord, S Clark, MH Taylor, J AF Bringsjord, Selmer Clark, Micah H. Taylor, Joshua BE Hagengruber, R Riss, UV TI SOPHISTICATED KNOWLEDGE REPRESENTATION AND REASONING REQUIRES PHILOSOPHY SO PHILOSOPHY, COMPUTING AND INFORMATION SCIENCE SE History and Philosophy of Technoscience LA English DT Article; Book Chapter C1 [Bringsjord, Selmer] Rensselaer Polytech Inst, Dept Cognit Sci, Troy, NY 12181 USA. [Bringsjord, Selmer] Lally Sch Management, Troy, NY USA. [Clark, Micah H.] Florida Inst Human & Machine Cognit IHMC, Pensacola, FL USA. [Clark, Micah H.] CALTECH, Pasadena, CA 91125 USA. [Clark, Micah H.] NASA, Jet Prop Lab, New York, NY USA. [Taylor, Joshua] Assured Informat Secur Inc, Rome, NY USA. [Taylor, Joshua] Rensselaer Polytech Inst, Troy, NY 12181 USA. RP Bringsjord, S (reprint author), Rensselaer Polytech Inst, Dept Cognit Sci, Troy, NY 12181 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE PI ABINGDON PA 2 PARK SQ, MILTON PARK, ABINGDON OX14 4RN, OXFORD, ENGLAND BN 978-1-317-31756-2; 978-1-84893-508-2 J9 HIST PHILOS TECHNOSC PY 2014 VL 3 BP 99 EP 119 PG 21 WC Computer Science, Information Systems; History & Philosophy Of Science; Information Science & Library Science SC Computer Science; History & Philosophy of Science; Information Science & Library Science GA BD7XA UT WOS:000363665100011 ER PT J AU Breed, M Venter, C Harding, AK Johnson, TJ AF Breed, M. Venter, C. Harding, A. K. Johnson, T. J. BE Engelbrecht, C Karataglidis, S TI The effect of an offset-dipole magnetic field on the Vela pulsar's gamma-ray light curves SO PROCEEDINGS OF SAIP2014: THE 59TH ANNUAL CONFERENCE OF THE SOUTH AFRICAN INSTITUTE OF PHYSICS LA English DT Proceedings Paper CT 59th Annual Conference of the South-African-Institute-of-Physics (SAIP) CY JUL 07-11, 2014 CL Univ Johannesburg, Johannesburg, SOUTH AFRICA SP South African Inst Phys HO Univ Johannesburg ID LARGE-AREA TELESCOPE; HIGH-ENERGY EMISSION; OUTER MAGNETOSPHERE; MILLISECOND PULSARS; POLAR CAPS; SLOT GAPS; RADIATION; ACCELERATION; CASCADES AB Over the past six years, the Fermi Large Area Telescope has detected more than 150 gamma-ray pulsars, discovering a variety of light curve trends and classes. Such diversity hints at distinct underlying magnetospheric and/or emission geometries. We implemented an offset-dipole magnetic field, with an offset characterised by parameters epsilon and magnetic azimuthal angle, in an existing geometric pulsar modelling code which already includes static and retarded vacuum dipole fields. We use these different B-field solutions in conjunction with standard emission geometries, namely the two-pole caustic and outer gap models (the latter only for non-offset dipoles), and construct intensity maps and light curves for several pulsar parameters. We compare our model light curves to the Vela data from the second pulsar catalogue of Fermi. We use a refined chi-square grid search method for finding best-fit light curves for each of the different models. Our best fit is for the retarded vacuum dipole field and the outer gap model. C1 [Breed, M.; Venter, C.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Harding, A. K.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Johnson, T. J.] Natl Acad Sci, Washington, DC 20001 USA. [Johnson, T. J.] Naval Res Lab, Washington, DC 20375 USA. RP Breed, M (reprint author), North West Univ, Ctr Space Res, Potchefstroom Campus,Private Bag X6001, ZA-2520 Potchefstroom, South Africa. EM 20574266@nwu.ac.za NR 25 TC 0 Z9 0 U1 0 U2 0 PU SOUTH AFRICAN INST PHYSICS PI LYNNWOOD RIDGE PA POSTNET STE 165, PRIVATE BAG X025, LYNNWOOD RIDGE, 0040, SOUTH AFRICA BN 978-0-620-65391-6 PY 2014 BP 311 EP 316 PG 6 WC Physics, Applied; Physics, Multidisciplinary SC Physics GA BE1GJ UT WOS:000367881700053 ER PT S AU Li, W Leusenkamp, M Ellis, D AF Li, W. Leusenkamp, M. Ellis, D. GP IEEE TI Testing A Cu-8Cr-4Nb Contact Material in Vacuum Interrupters SO PROCEEDINGS OF THE 2014 26TH INTERNATIONAL SYMPOSIUM ON DISCHARGES AND ELECTRICAL INSULATION IN VACUUM (ISDEIV-2014) SE International Symposium on Discharges and Electrical Insulation in a Vacuum LA English DT Proceedings Paper CT 26th International Symposium on Discharges and Electrical Insulation in Vacuum (ISDEIV) CY SEP 28-OCT 03, 2014 CL Bhabha Atom Res Ctr, Mumbai, INDIA SP Indian Vacuum Soc, Plansee, IEEE DEIS, Toshiba, Schneider Elect, DAE, IEEE, BRNS HO Bhabha Atom Res Ctr AB GRCop-84 is a Cu-8 at.% Cr-4 at.% Nb alloy developed at NASA Glenn Research Center for use in rocket engine liners. Its high thermal and electrical conductivities make it a possible candidate for the electrical contact of a vacuum interrupter (VI). In this work, contacts were made from a warm rolled Cu-8Cr-4Nb plate and tested in a VI of the Axial Magnetic Field (AMF) type as well as a VI of the Transverse Magnetic Field (TMF) type. The material showed comparable performance in dielectric strength as well as current interruption to those of typical powder-metallurgically made or vacuum cast Cu-Cr contact materials. Contact resistance values are also in the same range as those of typical commercial Cu-Cr. Postmortem examinations of the VIs saw appearance of a significant melt depth, and rather fluid molten metal flow on the contact surface, and splashing on to the surrounding shields. The results of the testing are discussed in terms of the microstructure and properties of the GRCop-84 material. Future work to examine the addition of a fourth element and increased Cr2Nb content is proposed. C1 [Li, W.; Leusenkamp, M.] Eaton Co, Vacuum Interrupter Plant, Horseheads, NY 14845 USA. [Ellis, D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. RP Li, W (reprint author), Eaton Co, Vacuum Interrupter Plant, Horseheads, NY 14845 USA. EM Wangpeili@Eaton.Com; David.L.Ellis@Nasa.Gov NR 8 TC 1 Z9 1 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1093-2941 BN 978-1-4799-6750-6 J9 INT SYM DISCH ELECTR PY 2014 BP 409 EP 412 PG 4 WC Engineering, Electrical & Electronic SC Engineering GA BE2QM UT WOS:000369858100104 ER PT S AU Leonard, D Parsons, J Cates, G AF Leonard, Daniel Parsons, Jeremy Cates, Grant BE Tolk, A Yilmaz, L Diallo, SY Ryzhov, IO TI USING DISCRETE EVENT SIMULATION TO MODEL FLUID COMMODITY USE BY THE SPACE LAUNCH SYSTEM SO PROCEEDINGS OF THE 2014 WINTER SIMULATION CONFERENCE (WSC) SE Winter Simulation Conference Proceedings LA English DT Proceedings Paper CT Winter Simulation Conference CY DEC 07-10, 2014 CL Savannah, GA AB In May 2013, NASA requested a study to develop a discrete event simulation (DES) model that analyzes the launch campaign process of the Space Launch System (SLS) from an integrated commodities perspective. The scope of the study includes launch countdown and scrub turnaround and focuses on four core launch commodities: hydrogen, oxygen, nitrogen, and helium. Previously, the commodities were only analyzed individually and deterministically for their launch support capability, but this study was the first to integrate them to examine the impact of their interactions on a launch campaign as well as the effects of process variability on commodity availability. The model utilized the flow process modules in Rockwell Arena to simulate the commodity flows and calculate total use. The study produced a validated DES model that showed that Kennedy Space Center's ground systems were capable of supporting a 48-hour scrub turnaround for the SLS. C1 [Leonard, Daniel] Prod Apex Inc, DES Modeling & Anal Ctr, 3505 Lake Lynda Dr,Suite 206, Orlando, FL 32817 USA. [Parsons, Jeremy] NASA Kennedy Space Ctr, Ground Syst Dev & Operat Program, Operat Integrat Div, Kennedy Space Ctr, FL 32899 USA. [Cates, Grant] Aerosp Corp, DES Modeling & Anal Ctr, Kennedy Space Ctr, FL 32815 USA. RP Leonard, D (reprint author), Prod Apex Inc, DES Modeling & Anal Ctr, 3505 Lake Lynda Dr,Suite 206, Orlando, FL 32817 USA. EM dan@productivityapex.com; jeremy.w.parsons@nasa.gov; grant.r.cates@nasa.gov NR 8 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0891-7736 BN 978-1-4799-7486-3 J9 WINT SIMUL C PROC PY 2014 BP 2954 EP 2965 PG 12 WC Computer Science, Information Systems; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA BG4XP UT WOS:000389248203061 ER PT B AU Mehrpouyan, H Giannakopoulou, D Tumer, IY Hoyle, C Brat, G AF Mehrpouyan, Hoda Giannakopoulou, Dimitra Tumer, Irem Y. Hoyle, Chris Brat, Guillaume GP ASME TI COMBINATION OF COMPOSITIONAL VERIFICATION AND MODEL CHECKING FOR SAFETY ASSESSMENT OF COMPLEX ENGINEERED SYSTEMS SO PROCEEDINGS OF THE ASME INTERNATIONAL DESIGN ENGINEERING TECHNICAL CONFERENCES AND COMPUTERS AND INFORMATION IN ENGINEERING CONFERENCE, 2014, VOL 1B LA English DT Proceedings Paper CT ASME Design Engineering Technical Conferences and Computers and Information in Engineering Conference (DETC) CY AUG 17-20, 2014 CL Buffalo, NY SP ASME ID FUNCTIONAL BASIS; DESIGN METHOD AB This paper presents a novel safety specification and verification approach based on the compositional reasoning and model checking algorithms. The behavioral specification of each component and subsystem is modeled to describe the overall structure of the design. Then, these specifications are analyzed to determine the least number of component redundancies that are required to tolerate and prevent catastrophic system failure. The framework utilizes Labelled Transition Systems (LTS) formalism to model the behavior of components and subsystems. Furthermore, compositional analysis is used to reason about the components' constraints (or assumptions) on their environments and the properties (or guarantees) of their output. This identification of local safety properties of components and subsystems leads to satisfaction of the desired safety requirements for the global system. A model of quad-redundant Electro-Mechanical Actuator (EMA) is constructed and, in an iterative approach, its safety properties are analyzed. Experimental results confirm the feasibility of the proposed approach for verifying the safety issues associated with complex systems in the early stages of the design process. C1 [Mehrpouyan, Hoda; Tumer, Irem Y.; Hoyle, Chris] Oregon State Univ, Sch Mech Ind & Mfg Engn, Corvallis, OR 97331 USA. [Giannakopoulou, Dimitra; Brat, Guillaume] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Brat, Guillaume] Carnegie Mellon Univ, Moffett Field, CA 94035 USA. RP Mehrpouyan, H (reprint author), Oregon State Univ, Sch Mech Ind & Mfg Engn, Corvallis, OR 97331 USA. NR 36 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4629-2 PY 2014 AR V01BT02A021 PG 12 WC Engineering, Electrical & Electronic; Engineering, Mechanical SC Engineering GA BF0ZM UT WOS:000379987100021 ER PT B AU Guo, R Nguyen, V Niu, L Bridgwater, L AF Guo, Raymond Nguyen, Vienny Niu, Lei Bridgwater, Lyndon GP ASME TI DESIGN AND ANALYSIS OF A TENDON-DRIVEN, UNDER-ACTUATED ROBOTIC HAND SO PROCEEDINGS OF THE ASME INTERNATIONAL DESIGN ENGINEERING TECHNICAL CONFERENCES AND COMPUTERS AND INFORMATION IN ENGINEERING CONFERENCE, 2014, VOL 5A LA English DT Proceedings Paper CT ASME Design Engineering Technical Conferences and Computers and Information in Engineering Conference (DETC) CY AUG 17-20, 2014 CL Buffalo, NY SP ASME DE hand; tendon; under-actuated; robotic AB There has been continuous research and development to add more actuators into robotic hands to increase their dexterity. However, dexterous hands require complex control and are more costly to build. Therefore, many researchers and commercial enterprises have begun developing under-actuated robotic hands with fewer actuators and passive mechanical adaptation to not only reduce complexity and cost, but to also achieve better grasp performance in unstructured settings. This paper presents the design and analysis of the Valkyrie hand a four fingered, tendon-driven, and under-actuated robotic hand that balances dexterity and simplicity with total 14 joints, and six degrees of actuated freedom. A derivation is provided of general dynamic and static equations for the analysis of a tendon driven mechanism, based on Euler-Lagrange formulation. The equations were used to evaluate the design parameters' impact on the hand grasp shape and closing effort, and also validated against a design case study. C1 [Guo, Raymond] Gen Motors R&D, Mfg Syst Res Lab, Warren, MI USA. [Nguyen, Vienny; Bridgwater, Lyndon] NASA, Software Robot & Simulat, Johnson Space Ctr, Houston, TX 77058 USA. [Niu, Lei] Jacobs Technol, Houston, TX USA. RP Bridgwater, L (reprint author), NASA, Software Robot & Simulat, Johnson Space Ctr, Houston, TX 77058 USA. EM raymond.guo@gm.com; vienny.n.nguyen@nasa.gov; lei.niu@nasa.dov; lyndon.bridgwater-1@nasa.gov NR 16 TC 0 Z9 0 U1 1 U2 1 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4636-0 PY 2014 AR V05AT08A095 PG 10 WC Engineering, Electrical & Electronic; Engineering, Mechanical SC Engineering GA BF0ZR UT WOS:000379987600095 ER PT B AU Reher, J Yule, J Fritz, E Wheeler, M Nelson, CA Dungan, LK AF Reher, Jake Yule, Joan Fritz, Eric Wheeler, Max Nelson, Carl A. Dungan, Larry K. GP ASME TI CLOSED-LOOP CONTROL AND RELEASE MECHANISM DEVELOPMENT FOR MICROGRAVITY FREE FLYER SO PROCEEDINGS OF THE ASME INTERNATIONAL DESIGN ENGINEERING TECHNICAL CONFERENCES AND COMPUTERS AND INFORMATION IN ENGINEERING CONFERENCE, 2014, VOL 5B LA English DT Proceedings Paper CT ASME Design Engineering Technical Conferences and Computers and Information in Engineering Conference (DETC) CY AUG 17-20, 2014 CL Buffalo, NY SP ASME AB As human exploration into our solar system expands, the necessity for robotic assistance increases. A free-flying robotic apparatus would be beneficial for space exploration missions to aid humans in small programmed tasks as well as remote planetary or asteroid exploration. The design of these drones would need to account for the fact that much of their time would be spent in a microgravity environment. As this complicates the design, a method for simulating exposure to microgravity was developed by NASA Johnson Space Center: the Active Response Gravity Offload System (ARGOS). ARGOS has been confirmed as accurate for gravity compensation of large payloads, but its reliability is less certain for small-scale loads. To test the accuracy of ARGOS on small-scale devices, a free-flying octocopter was developed and flown both on ARGOS and in a reduced-gravity aircraft to compare the reduced gravity effects. This testing helped identify the need for an improved control system and a release mechanism to provide consistent initial conditions, which were subsequently added to the system. This paper describes the robotic flyer design, control, and release mechanism, along with results of reduced-gravity testing. C1 [Reher, Jake; Yule, Joan; Fritz, Eric; Wheeler, Max; Nelson, Carl A.] Univ Nebraska, Dept Mech & Mat Engn, Lincoln, NE USA. [Dungan, Larry K.] NASA Johnson Space Ctr, Houston, TX USA. RP Reher, J (reprint author), Univ Nebraska, Dept Mech & Mat Engn, Lincoln, NE USA. NR 10 TC 0 Z9 0 U1 1 U2 1 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4637-7 PY 2014 AR V05BT08A020 PG 5 WC Engineering, Electrical & Electronic; Engineering, Mechanical SC Engineering GA BF0ZQ UT WOS:000379987500020 ER PT B AU Sigel, D Trease, BP Thomson, MW Webb, DR Willis, P Lisman, PD AF Sigel, Deborah Trease, Brian P. Thomson, Mark W. Webb, David R. Willis, Paul Lisman, P. Doug GP ASME TI APPLICATION OF ORIGAMI IN STARSHADE SPACECRAFT BLANKET DESIGN SO PROCEEDINGS OF THE ASME INTERNATIONAL DESIGN ENGINEERING TECHNICAL CONFERENCES AND COMPUTERS AND INFORMATION IN ENGINEERING CONFERENCE, 2014, VOL 5B LA English DT Proceedings Paper CT ASME Design Engineering Technical Conferences and Computers and Information in Engineering Conference (DETC) CY AUG 17-20, 2014 CL Buffalo, NY SP ASME AB A Starshade is a large deployable structure and sole payload of an external occulter. At 34m in diameter or more, starshades are designed to block most of the light from a nearby star so that a small orbiting space telescope can image and characterize the Earth-like exoplanets in orbit around it. The starshade resembles a sunflower with a circular central disk supporting petals that are arrayed around its periphery. The petal edges are precisely shaped to match an optical profile that prevents diffraction. The area circumscribed by the edges must be completely opaque, black, and non-reflective. The petals and ring structure are covered by specially designed deployable blankets that must remain completely opaque even if they become perforated by micrometeorites. The blankets must also not cause any significant on-orbit thermoelastic loads on the lightweight supporting ring and petal structures despite very large differential thermal strains that are developed between these Kapton blankets and the thermally stable composite ring and petal structures. There are two types of blankets: one for the deployable petals and one for the central support disc that is formed by a lightweight deployable ring truss structure. The starshade blankets cover such a large area that they must be unusually lightweight compared to conventional multi-layer insulated (MU) spacecraft blankets. The blankets must also stow around the central hub of the spacecraft with the deployable ring and petal structures in a highly repeatable fashion. This makes them ideal candidates for origami folding schemes. Based on prior studies of large deployable rigid arrays, we began with variants on the origami flasher to fold the central ring blanket, which is a minimum of 20m in diameter. We looked at the simplest methods for integrating this large blanket with a mechanical ring truss while providing ample optical baffling and little to no thermally induced loads on the structure. Petal blankets were also developed using deployable softgoods with pseudo-mechanical and shingled designs with optically blocking folds for deployment. The design was developed iteratively utilizing a variety of prototypes to explore and demonstrate the interaction between the softgoods and rigid elements. C1 [Sigel, Deborah; Trease, Brian P.; Thomson, Mark W.; Webb, David R.; Willis, Paul; Lisman, P. Doug] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. RP Sigel, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4637-7 PY 2014 AR V05BT08A033 PG 8 WC Engineering, Electrical & Electronic; Engineering, Mechanical SC Engineering GA BF0ZQ UT WOS:000379987500033 ER PT B AU Mukherjee, R Howard, T Myint, S Chang, J Craft, J AF Mukherjee, Rudranarayan Howard, Thomas Myint, Steven Chang, Johnny Craft, Jack GP ASME TI VEHICLE DYNAMICS MODELS FOR ONBOARD MOTION PLANNING SO PROCEEDINGS OF THE ASME INTERNATIONAL DESIGN ENGINEERING TECHNICAL CONFERENCES AND COMPUTERS AND INFORMATION IN ENGINEERING CONFERENCE, 2014, VOL 6 LA English DT Proceedings Paper CT ASME Design Engineering Technical Conferences and Computers and Information in Engineering Conference (DETC) CY AUG 17-20, 2014 CL Buffalo, NY SP ASME ID ENVIRONMENTS AB Offline multibody dynamics based modeling and simulation of vehicle dynamics has been pursued with varying levels of success for more than two decades. This has been used in design, controls, training, and other technical and programmatic objectives. Over the last decade, autonomous vehicle dynamics has become an important area of research. This has resulted in a growing need for onboard vehicle model that works with the vehicle controller and path planner. Typically, kinematic models have largely been used for these objectives. Use of dynamics models for onboard motion planning is a relatively new topic of research with only a handful of prior work. In this paper we report our attempts at addressing the need for onboard vehicle dynamics models for motion planning in relatively fast autonomous mobility scenarios. We present the idea of using adaptive motion models that trade fidelity and cost of simulation to enable a motion planner to select an adequate model. Towards this, we present representative simulation results that demonstrate the need for adaptivity. We then present some technical challenges with onboard vehicle models and our attempts at addressing these challenges. Finally, we present some results that compare raw vehicle data with model predictive results. C1 [Mukherjee, Rudranarayan; Howard, Thomas; Myint, Steven; Chang, Johnny; Craft, Jack] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Howard, Thomas] MIT, Comp Sci & Artificial Intelligence Lab, Cambridge, MA USA. RP Mukherjee, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Rudranarayan.M.Mukherjee@jpl.nasa.gov NR 5 TC 0 Z9 0 U1 1 U2 1 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4639-1 PY 2014 AR V006T10A047 PG 8 WC Engineering, Electrical & Electronic; Engineering, Mechanical SC Engineering GA BF0ZP UT WOS:000379987400047 ER PT B AU Mukherjee, R Moreland, S Kim, I Lele, N Goodwin, S Houlihan, R Parness, A Wu, A Cutkosky, M AF Mukherjee, Rudranarayan Moreland, Scott Kim, Isaac Lele, Nikhil Goodwin, Stephen Houlihan, Ryan Parness, Aaron Wu, Alice Cutkosky, Mark GP ASME TI COMPUTATIONAL AND EXPERIMENTAL APPROACH TO UNDERSTANDING LEGGED MOBILITY IN MICRO GROUND VEHICLES SO PROCEEDINGS OF THE ASME INTERNATIONAL DESIGN ENGINEERING TECHNICAL CONFERENCES AND COMPUTERS AND INFORMATION IN ENGINEERING CONFERENCE, 2014, VOL 6 LA English DT Proceedings Paper CT ASME Design Engineering Technical Conferences and Computers and Information in Engineering Conference (DETC) CY AUG 17-20, 2014 CL Buffalo, NY SP ASME AB The army has a vision for using autonomous micro ground vehicles (MGV) for soldier support in the last 100 meters of operations in urban and natural environments. These MGVs are expected to typically fit in a human palm and weigh in the order of 30-50 grains. Robust mobility is a necessary condition to ensure operations. Given the severe challenge of size, weight and power (SWAP) of the MGVs, significant uncertainties currently remain in quantifying micro ground vehicle mobility. In this paper we describe a research methodology and representative results for understanding legged MGV mobility in different types of terrain. Our methodology is based on a synergy of novel experimental setup and high-fidelity computational methods. We report the use of a novel "single-leg" test rig that uses tactile sensors to measure ground interaction loads. We also report the use of high speed imaging and use of particle image velocimetry to understand soil deformation during legged interactions with terrain. Finally, we report on the use of multibody dynamics and High Performance Computing (HPC) based granular media simulations. This conference paper emphases more on the overall approach based on synergistic use of high fidelity modeling and experimental methods supported by representative results rather than presenting a detailed analyses of the results. C1 [Mukherjee, Rudranarayan; Moreland, Scott; Kim, Isaac; Lele, Nikhil; Goodwin, Stephen; Houlihan, Ryan; Parness, Aaron] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wu, Alice; Cutkosky, Mark] Stanford Univ, Dept Mech Engn, Paolo Alto, VA USA. RP Mukherjee, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Rudranarayan.M.Mukherjee@jpl.nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4639-1 PY 2014 AR V006T10A005 PG 6 WC Engineering, Electrical & Electronic; Engineering, Mechanical SC Engineering GA BF0ZP UT WOS:000379987400005 ER PT B AU Mylapilli, H Jain, A AF Mylapilli, Harshavardhan Jain, Abhinandan GP ASME TI EVALUATION OF COMPLEMENTARITY TECHNIQUES FOR MINIMAL COORDINATE CONTACT DYNAMICS SO PROCEEDINGS OF THE ASME INTERNATIONAL DESIGN ENGINEERING TECHNICAL CONFERENCES AND COMPUTERS AND INFORMATION IN ENGINEERING CONFERENCE, 2014, VOL 6 LA English DT Proceedings Paper CT ASME Design Engineering Technical Conferences and Computers and Information in Engineering Conference (DETC) CY AUG 17-20, 2014 CL Buffalo, NY SP ASME AB In this article, the non-smooth contact dynamics of multi body systems is formulated as a complementarily problem. Minimal coordinates operational space formulation is used to derive the dynamics equations of motion. Depending on the approach used for modeling Coulomb's friction, the complementarity problem can be posed either as a linear or a nonlinear problem. Both formulations are studied in this paper An exact modeling of the friction cone leads to a nonlinear complementarity problem (NCP) formulation whereas a polyhedral approximation of the friction cone results in a linear complementarity problem (LCP) formulation. These complementarity problems are further recast as non-smooth unconstrained optimization problems, which are solved by employing a class of Levenberg-Marquardt algorithms. The necessary theory detailing these techniques is discussed and five schemes are implemented to solve contact dynamics problems. A simple test case of a sphere moving on a plane surface is used to validate these schemes, while a twelve link pendulum example is chosen to compare the speed and accuracy of the schemes presented in this paper. C1 [Mylapilli, Harshavardhan] Univ Southern Calif, Dept Aerosp & Mech Engn, Los Angeles, CA 90089 USA. [Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jain, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM mylapill@usc.edu; Abhinandan.Jain@jpl.nasa.gov NR 22 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4639-1 PY 2014 AR V006T10A010 PG 13 WC Engineering, Electrical & Electronic; Engineering, Mechanical SC Engineering GA BF0ZP UT WOS:000379987400010 ER PT B AU Mukherjee, R Myint, S Chang, J Kim, I Craft, J Pomerantz, M Kim, J Peterson, L AF Mukherjee, Rudranarayan Myint, Steven Chang, Johnny Kim, Isaac Craft, Jack Pomerantz, Marc Kim, Junggon Peterson, Lee GP ASME TI M3TK: A ROBOT MOBILITY AND MANIPULATION MODELING TOOLKIT SO PROCEEDINGS OF THE ASME INTERNATIONAL DESIGN ENGINEERING TECHNICAL CONFERENCES AND COMPUTERS AND INFORMATION IN ENGINEERING CONFERENCE, 2014, VOL 7 LA English DT Proceedings Paper CT ASME Design Engineering Technical Conferences and Computers and Information in Engineering Conference (DETC) CY AUG 17-20, 2014 CL Buffalo, NY SP ASME AB In this brief paper, we present an overview of the M3tk software for modeling robotic systems. M3tk contains basic kinematics, inverse kinematics, dynamics and inverse dynamics capabilities for articulated multi-rigid body systems. Written in C++, the software features a core kinematics and dynamics library, a linear algebra library specialized for use with the algorithms in M3tk, and a Graphical User Interface with full 3D visualization. It contains implementations of multiple contact mechanics models and the ability to model terrain through heightfields. M3tk also features an ability to model terrains with spatially distributed properties. There is also an ability to manipulate objects using a joystick. This paper summarizes M3tk without delving into the details of the code. C1 [Mukherjee, Rudranarayan; Myint, Steven; Chang, Johnny; Kim, Isaac; Craft, Jack; Pomerantz, Marc; Kim, Junggon; Peterson, Lee] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mukherjee, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Rudranarayan.M.Mukherjee@jpl.nasa.gov NR 2 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 978-0-7918-4640-7 PY 2014 AR V007T05A003 PG 4 WC Engineering, Electrical & Electronic; Engineering, Mechanical SC Engineering GA BF0ZZ UT WOS:000380080200003 ER PT S AU Reed, MK AF Reed, Monty K. GP IEEE TI LIFESUIT Exoskeleton Gives the Gift of Walking so They Shall Walk SO PROCEEDINGS OF THE FOURTH IEEE GLOBAL HUMANITARIAN TECHNOLOGY CONFERENCE (GHTC 2014) SE IEEE Global Humanitarian Technology Conference Proceedings LA English DT Proceedings Paper CT 4th annual IEEE Global Humanitarian Technology Conference (GHTC) CY OCT 10-13, 2014 CL San Jose, CA SP IEEE, IEEE Reg 6, IEEE Santa Clara Valley Sect, IEEE Seattle Sect, IEEE Humanitarian Ad Hoc Comm, Natl Aeronaut & Space Adm, IEEE Special Grp Humanitarian Technol, Joe Decuir, Coughlin Associates, IEEE Tech Activities Board DE LIFESUIT; passive therapy; exoskeleton; reciprocating gate orthosis; robothon; robogames; hardiman; arduino AB LIFESUIT Exoskeleton Gives the Gift of Walking so They Shall Walk. Recent studies have shown the majority of paralyzed people who participate in passive exercise therapy will regain mobility and learn to walk(i).(ii iii) The current medical system only pays for one session per week or month.(iv) The LIFE SUIT therapy system will allow a full therapy session to be recorded(v). By outfitting the therapist with a telemetry suit, the patient in the LIFESUIT can be moved through the entire exercise routine. The recordings are stored in a patient profile(vi), for future use. The recorded session could be "played back" allowing the paralyzed person to exercise daily and get the exercise they need to fully recover. Collaboration between the They Shall Walk.org clinic in Seattle and other physical therapy clinics in India, Nepal, Kenya and other parts of the world will facilitate faster development of exercise and therapy recordings that can then be shared. The LIFE SUIT Exoskeleton prototype allows actual recovery from paralysis using the existing funded therapy and exercise sessions. C1 [Reed, Monty K.] They Shall Walk, Seattle, WA 98108 USA. [Reed, Monty K.] Univ Washington, NASA, Space Grant Consortium, Seattle, WA 98195 USA. RP Reed, MK (reprint author), They Shall Walk, Seattle, WA 98108 USA. EM monty@theyshallwalk.org NR 1 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 2377-6919 BN 978-1-4799-7193-0 J9 IEEE GLOB HUMANIT C PY 2014 BP 382 EP 385 PG 4 WC Engineering, Multidisciplinary SC Engineering GA BG9BD UT WOS:000392950900058 ER PT B AU Guzik, JA Houdek, G Chaplin, WJ Kurtz, D Gilliland, RL Mullally, F Rowe, JF Haas, MR Bryson, ST Still, MD Boyajian, T AF Guzik, J. A. Houdek, G. Chaplin, W. J. Kurtz, D. Gilliland, R. L. Mullally, F. Rowe, J. F. Haas, M. R. Bryson, S. T. Still, M. D. Boyajian, T. BE CreechEakman, MJ Guzik, JA Stencel, RE TI Observational Constraints, Stellar Models, and Kepler Data for 0 Cyg, the Brightest Star Observable by Kepler SO RESOLVING THE FUTURE OF ASTRONOMY WITH LONG-BASELINE INTERFEROMETRY SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Resolving the Future of Astronomy with Long-Baseline Interferometry CY MAR 28-31, 2011 CL Socorro, NM SP New Mexico Tech, Magdalena Ridge Observ ID OSCILLATIONS; ABUNDANCES; PULSATIONS AB The V = 4.48 F4 main-sequence star 8 Cyg is the brightest star observable in the Kepler spacecraft field of view. Short-cadence (58.8 s) photometric data were obtained by Kepler during June September 2010. Preliminary analysis shows solar like oscillations in the frequency range 1200 2500,uHz. To interpret these data and to motivate further observations, we use observational constraints from the literature to construct stellar evolution and pulsation models for this star. We compare the observed large frequency separation of the solar-like oscillations with the model predictions and discuss the prospects for y Doradus-like g-mode pulsations, given the observational constraints. We discuss the value of angular diameter measurements from optical interferometry for constraining stellar properties and the implications for asteroseismology. C1 [Guzik, J. A.] Los Alamos Natl Lab, XTD 2,MS T-086, Los Alamos, NM 87545 USA. [Houdek, G.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Chaplin, W. J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Kurtz, D.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Mullally, F.; Rowe, J. F.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Haas, M. R.; Bryson, S. T.; Still, M. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Still, M. D.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Boyajian, T.] Georgia State Univ, Ctr High Angular Resolut Astron, Dept Phys & Astron, Atlanta, GA 30302 USA. RP Guzik, JA (reprint author), Los Alamos Natl Lab, XTD 2,MS T-086, Los Alamos, NM 87545 USA. NR 22 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-858-9 J9 ASTR SOC P PY 2014 VL 487 BP 105 EP 114 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE7YX UT WOS:000376047700009 ER PT B AU Monnier, JD Che, X Zhao, M ten Brummelaar, T AF Monnier, John D. Che, Xiao Zhao, Ming ten Brummelaar, Theo BE CreechEakman, MJ Guzik, JA Stencel, RE TI Imaging Rapid Rotators SO RESOLVING THE FUTURE OF ASTRONOMY WITH LONG-BASELINE INTERFEROMETRY SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Resolving the Future of Astronomy with Long-Baseline Interferometry CY MAR 28-31, 2011 CL Socorro, NM SP New Mexico Tech, Magdalena Ridge Observ ID BASE-LINE INTERFEROMETRY; CHARA ARRAY; ROTATIONAL VELOCITIES; STELLAR ROTATION; ALPHA OPHIUCHI; POLE-ON; STARS; VEGA; INSTRUMENT; LEONIS AB The combination of the long-baseline CHARA Array and the four-beam "imaging" combiner MIRC has revolutionized the study of rapidly rotating stars. Here we give an overview of our group's results from the past five years. In this time, we have verified the basic "gravity darkening" paradigm for rapidly rotating stars, originally outlined by von Zeipel nearly 90 years ago. We have found that the original gravity darkening parameter derived by von Zeipel (1924) is far too high to match observations, and recommend a value of 0.19 (instead of 0.25). Our modeling of beta Cas led to unexpected constraints on core-envelope coupling, and we conclude that effective coupling persists even on the fast-evolving subgiant branch. Lastly, we outline a new method ("oblateness method") for measuring the mass of a single star based on interferometric imaging and spectral measurements of vs in i. We end this brief review with a look towards the future and the exciting potential for visible light imaging and spectro-interferometry all with existing instrumentation and demonstrated capabilities. C1 [Monnier, John D.; Che, Xiao] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Zhao, Ming] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [ten Brummelaar, Theo] Georgia State Univ, CHARA Array, Atlanta, GA 30303 USA. RP Monnier, JD (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. NR 31 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-858-9 J9 ASTR SOC P PY 2014 VL 487 BP 137 EP 147 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE7YX UT WOS:000376047700012 ER PT B AU Cotton, WD Perrin, G Mennesson, B AF Cotton, W. D. Perrin, G. Mennesson, B. BE CreechEakman, MJ Guzik, JA Stencel, RE TI Radio and IR Observations of the Envelopes of AGB Stars SO RESOLVING THE FUTURE OF ASTRONOMY WITH LONG-BASELINE INTERFEROMETRY SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Resolving the Future of Astronomy with Long-Baseline Interferometry CY MAR 28-31, 2011 CL Socorro, NM SP New Mexico Tech, Magdalena Ridge Observ ID MIRA VARIABLE-STARS; VLBA OBSERVATIONS; SIO MASERS AB Asymptotic Giant Branch stars (AGB) are evolved red giants with tenuous molecular envelopes that have been the subject of much recent study using infrared and radio interferometers. In oxygen-rich stars, radio SiO masers form in the outer regions of the molecular envelopes and are powerful probes of the extent and dynamics of these envelopes. We discuss recent IR and radio measurements that are providing a wealth of information on these systems. C1 [Cotton, W. D.] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22902 USA. [Perrin, G.] Observ Paris, LESIA, UMR 8109, F-92190 Meudon, France. [Mennesson, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cotton, WD (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22902 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-858-9 J9 ASTR SOC P PY 2014 VL 487 BP 163 EP 170 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE7YX UT WOS:000376047700014 ER PT B AU Zhao, M Monnier, JD Che, X Pedretti, E Thureau, N AF Zhao, Ming Monnier, John D. Che, Xiao Pedretti, Ettore Thureau, Nathalie BE CreechEakman, MJ Guzik, JA Stencel, RE TI Toward Direct Detection of Hot Jupiters with Precision Closure Phase SO RESOLVING THE FUTURE OF ASTRONOMY WITH LONG-BASELINE INTERFEROMETRY SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Resolving the Future of Astronomy with Long-Baseline Interferometry CY MAR 28-31, 2011 CL Socorro, NM SP New Mexico Tech, Magdalena Ridge Observ ID EXTRASOLAR GIANT PLANETS; UPSILON ANDROMEDAE B; CHARA ARRAY; THEORETICAL SPECTRA; LIGHT CURVES; INTERFEROMETRY; ATMOSPHERES; STARS AB Direct detection of thermal emission from nearby hot Jupiters has greatly advanced our knowledge of extrasolar planets in recent years. Since hot Jupiter systems can be regarded as analogs of high-contrast binaries, ground-based infrared long baseline interferometers have the potential to resolve them and detect their thermal emission with precision closure phase a method that is immune to the systematic errors induced by the Earth's atmosphere. Here we present closure phase studies toward direct detection of nearby hot Jupiters using the CHARA interferometer array outfitted with the MIRC instrument. We find much larger systematic errors than expected in our observations, most likely caused by dispersion across different wavelengths. We also find that using higher spectral resolution modes (e.g., R=150) can significantly reduce the systematics. By combining all calibrators in an observing run together, we are able to roughly re-calibrate the lower spectral resolution data, allowing us to obtain upper limits of the star-planet contrast ratios of v And b across the H band. The data also allow us to get a refined stellar radius of 1.625 +/- 0.011R(circle dot). Our best upper limit corresponds to a contrast ratio of 2.1x10(3):1 with 90% confidence level at 1.52 mu m, suggesting that we are starting to have the capability of constraining atmospheric models of hot Jupiters with interferometry. C1 [Zhao, Ming] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-327, Pasadena, CA 91109 USA. [Monnier, John D.; Che, Xiao] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Pedretti, Ettore; Thureau, Nathalie] Univ St Andrews, SUPA, St Andrews KY16 9AJ, Fife, Scotland. RP Zhao, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-327, Pasadena, CA 91109 USA. NR 29 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-858-9 J9 ASTR SOC P PY 2014 VL 487 BP 185 EP 195 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE7YX UT WOS:000376047700016 ER PT J AU Zeng, XZ Peng, SQ Li, ZJ Qi, YQ Chen, RY AF Zeng, Xuezhi Peng, Shiqiu Li, Zhijin Qi, Yiquan Chen, Rongyu TI A reanalysis dataset of the South China Sea SO SCIENTIFIC DATA LA English DT Article AB Ocean reanalysis provides a temporally continuous and spatially gridded four-dimensional estimate of the ocean state for a better understanding of the ocean dynamics and its spatial/temporal variability. Here we present a 19-year (1992-2010) high-resolution ocean reanalysis dataset of the upper ocean in the South China Sea (SCS) produced from an ocean data assimilation system. A wide variety of observations, including in-situ temperature/salinity profiles, ship-measured and satellite-derived sea surface temperatures, and sea surface height anomalies from satellite altimetry, are assimilated into the outputs of an ocean general circulation model using a multi-scale incremental three-dimensional variational data assimilation scheme, yielding a daily high-resolution reanalysis dataset of the SCS. Comparisons between the reanalysis and independent observations support the reliability of the dataset. The presented dataset provides the research community of the SCS an important data source for studying the thermodynamic processes of the ocean circulation and meso-scale features in the SCS, including their spatial and temporal variability. C1 [Zeng, Xuezhi; Peng, Shiqiu; Qi, Yiquan; Chen, Rongyu] Chinese Acad Sci, South China Sea Inst Oceanol, State Key Lab Trop Oceanog, Guangzhou 510301, Guangdong, Peoples R China. [Zeng, Xuezhi] Univ Chinese Acad Sci, Beijing 100049, Peoples R China. [Li, Zhijin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Peng, SQ (reprint author), Chinese Acad Sci, South China Sea Inst Oceanol, State Key Lab Trop Oceanog, Guangzhou 510301, Guangdong, Peoples R China. EM speng@scsio.ac.cn FU Strategic Priority Research Program of the Chinese Academy of Sciences [XDA11010304]; Ministry of Science and Technology of the People's Republic of China (MOST) [2011CB403505, 2014CB953904]; Innovation Key Program of the Chinese Academy of Sciences [KZCX2-EW-208]; National Natural Science Foundation of China [41376021, 41306013]; National Project of Fundamental Work for Science and Technology of China [2008FY110100]; Integrated Project of State Key Laboratory of Tropical Oceanography (LTO) FX Great thanks are given to the scientists and crews of cruises organized by the SCSIO for providing the valuable in-situ observations. The construction of the reanalysis was jointly supported by the Strategic Priority Research Program of the Chinese Academy of Sciences with Grant No. XDA11010304, the Ministry of Science and Technology of the People's Republic of China (MOST) (2011CB403505 & 2014CB953904), the Innovation Key Program of the Chinese Academy of Sciences (KZCX2-EW-208), the National Natural Science Foundation of China (41376021, 41306013), the National Project of Fundamental Work for Science and Technology of China (2008FY110100), and the Integrated Project (2013) of State Key Laboratory of Tropical Oceanography (LTO). All numerical experiments were carried out at the High Performance Computing Center (HPCC) of the SCSIO. NR 33 TC 1 Z9 2 U1 1 U2 1 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2052-4463 J9 SCI DATA JI Sci. Data PY 2014 VL 1 AR 140052 DI 10.1038/sdata.2014.52 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA V45VG UT WOS:000209843500049 ER PT B AU Kubo, M Kano, R Kobayashi, K Bando, T Narukage, N Ishikawa, R Tsuneta, S Katsukawa, Y Ishikawa, S Suematsu, Y Hara, H Shimizu, T Sakao, T Ichimoto, K Goto, M Holloway, T Winebarger, A Cirtain, J De Pontieu, B Casini, R Auchere, F Bueno, JT Sainz, RM Belluzzi, L Ramos, AA Stepan, J Carlsson, M AF Kubo, M. Kano, R. Kobayashi, K. Bando, T. Narukage, N. Ishikawa, R. Tsuneta, S. Katsukawa, Y. Ishikawa, S. Suematsu, Y. Hara, H. Shimizu, T. Sakao, T. Ichimoto, K. Goto, M. Holloway, T. Winebarger, A. Cirtain, J. De Pontieu, B. Casini, R. Auchere, F. Trujillo Bueno, J. Manso Sainz, R. Belluzzi, L. Asensio Ramos, A. Stepan, J. Carlsson, M. BE Nagendra, KN Stenflo, JO Qu, ZQ Sampoorna, M TI A Sounding Rocket Experiment for the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) SO SOLAR POLARIZATION 7 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 7th Solar Polarization Workshop (SPW7) CY SEP 09-13, 2013 CL Kunming, PEOPLES R CHINA SP Natl Sci Fdn China, Chinese Acad Sci ID QUIET-SUN; HE II; SOLAR; POLARIZATION; ULTRAVIOLET; MISSION; REGION; WAVES; LINES AB A sounding-rocket experiment called the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is presently under development to measure the linear polarization profiles in the hydrogen Lyman-alpha (Ly alpha) line at 121.567 nm. CLASP is a vacuum-UV (VUV) spectropolarimeter to aim for first detection of the linear polarizations caused by scattering processes and the Hanle effect in the Lya line with high accuracy (0.1%). This is a fist step for exploration of magnetic fields in the upper chromosphere and transition region of the Sun. Accurate measurements of the linear polarization signals caused by scattering processes and the Hanle effect in strong UV lines like Lya are essential to explore with future solar telescopes the strength and structures of the magnetic field in the upper chromosphere and transition region of the Sun. The CLASP proposal has been accepted by NASA in 2012, and the flight is planned in 2015. C1 [Kubo, M.; Kano, R.; Bando, T.; Narukage, N.; Ishikawa, R.; Katsukawa, Y.; Ishikawa, S.; Suematsu, Y.; Hara, H.] Natl Astron Observ Japan, Tokyo, Japan. [Kobayashi, K.; Holloway, T.; Winebarger, A.; Cirtain, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Tsuneta, S.; Shimizu, T.; Sakao, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Yokohama, Kanagawa, Japan. [Ichimoto, K.] Kyoto Univ, Kyoto, Japan. [Goto, M.] Natl Inst Fus Sci, Gifu, Japan. [De Pontieu, B.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA USA. [Casini, R.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Auchere, F.] Inst Astrophys Spatiale, Orsay, France. [Trujillo Bueno, J.; Manso Sainz, R.; Belluzzi, L.; Asensio Ramos, A.] Inst Astrofis Canarias, Tenerife, Spain. [Stepan, J.] ASCR, Astron Inst, Ondrejov, Czech Republic. [Carlsson, M.] Univ Oslo, Oslo, Norway. RP Kubo, M (reprint author), Natl Astron Observ Japan, Tokyo, Japan. NR 25 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-863-3; 978-1-58381-862-6 J9 ASTR SOC P PY 2014 VL 489 BP 307 EP 318 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2YL UT WOS:000370308600030 ER PT B AU Ishikawa, R Bando, T Hara, H Ishikawa, S Kano, R Kubo, M Katsukawa, Y Kobiki, T Narukage, N Suematsu, Y Tsuneta, S Aoki, K Miyagawa, K Ichimoto, K Kobayashi, K Auchere, F AF Ishikawa, R. Bando, T. Hara, H. Ishikawa, S. Kano, R. Kubo, M. Katsukawa, Y. Kobiki, T. Narukage, N. Suematsu, Y. Tsuneta, S. Aoki, K. Miyagawa, K. Ichimoto, K. Kobayashi, K. Auchere, F. CA CLASP Team BE Nagendra, KN Stenflo, JO Qu, ZQ Sampoorna, M TI Precision VUV Spectro-Polarimetry for Solar Chromospheric Magnetic Field Measurements SO SOLAR POLARIZATION 7 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 7th Solar Polarization Workshop (SPW7) CY SEP 09-13, 2013 CL Kunming, PEOPLES R CHINA SP Natl Sci Fdn China, Chinese Acad Sci ID CLASP AB The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a VUV spectro-polarimeter optimized for measuring the linear polarization of the Lyman a line (121.6 nm) to be launched in 2015 with NASA's sounding rocket (Ishikawa et al. 2011; Narukage et al. 2011; Kano et al. 2012; Kobayashi et al. 2012). With this experiment, we aim to (1) observe the scattering polarization in the Lyman-a line, (2) detect the Hanle effect, and (3) assess the magnetic fields in the upper chromosphere and transition region for the first time. The polarization measurement error consists of scale error delta alpha (error in amplitude of linear polarization), azimuth error Delta phi (error in the direction of linear polarization), and spurious polarization epsilon (false linear polarization signals). The error e should be suppressed below 0.1% in the Lyman-alpha core (121.567 nm +/- 0.02 nm), and 0.5% in the Lyman-a wing (121.567 nm 0.05 nm), based on our scientific requirements shown in Table 2 of Kubo et al. (2014). From scientific justification, we adopt Delta phi < 2 degrees and Sa < 10% as the instrument requirements. The spectro-polarimeter features a continuously rotating MgF2 waveplate (Ishikawa et al. 2013), a dual-beam spectrograph with a spherical grating working also as a beam split ter, and two polarization analyzers (Bridou et al. 2011), which are mounted at 90 degree from each other to measure two orthogonal polarization simultaneously. For the optical layout of the CLASP instrument, see Figure 3 in Kubo et al. (2014). Considering the continuous rotation of the half-waveplate, the modulation efficiency is 0.64 both for Stokes Q and U. All the raw data are returned and demodulation (successive addition or subtraction of images) is done on the ground. We control the CLASP polarization performance in the following three steps. First, we evaluate the throughput and polarization properties of each optical component in the Lyman-a line, using the Ultraviolet Synchrotron ORbital Radiation Facility (UVSOR) at the Institute for Molecular Science. The second step is polarization calibration of the spectro-polarimeter after alignment. Since the spurious polarization caused by the axisymmetric telescope is estimated to be negligibly small because of the symmetry (Ishikawa et al. 2014), we do not perform end-to-end polarization calibration. As the final step, before the scientific observation near the limb, we make a short observation at the Sun center and verify the polarization sensitivity, because the scattering polarization is expected to be close to zero at the Sun center due to symmetric geometry. In order to clarify whether we will be able to achieve the required polarization sensitivity and accuracy via these steps, we exercise polarization error budget, by investigating all the possible causes and their magnitudes of polarization errors, all of which are not necessarily verified by the polarization calibration. Based on these error budgets, we conclude that a polarization sensitivity of 0.1% in the line core, delta a < 10% and Delta phi < 2 degrees can be achieved combined with the polarization calibration of the spectropolarimeter and the onboard calibration at the Sun center (refer to Ishikawa et al. 2014, for the detail). We are currently conducting verification tests of the flight components and development of the UV light source for the polarization calibration. From 2014 spring, we will begin the integration, alignment, and calibration. We will update the error budgets throughout the course of these tests. C1 [Ishikawa, R.; Bando, T.; Hara, H.; Ishikawa, S.; Kano, R.; Kubo, M.; Katsukawa, Y.; Kobiki, T.; Narukage, N.; Suematsu, Y.] Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo, Japan. [Tsuneta, S.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Aoki, K.; Miyagawa, K.] Univ Tokyo, Dept Astron, Sch Sci, Bunkyo Ku, Tokyo 113, Japan. [Ichimoto, K.] Kyoto Univ, Kwasan Observ, Takayama, Gifu, Japan. [Ichimoto, K.] Kyoto Univ, Hida Observ, Takayama, Gifu, Japan. [Kobayashi, K.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Auchere, F.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France. RP Ishikawa, R (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo, Japan. NR 8 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-863-3; 978-1-58381-862-6 J9 ASTR SOC P PY 2014 VL 489 BP 319 EP 322 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE2YL UT WOS:000370308600031 ER PT B AU Mason, E Bianchini, A Orio, M Williams, RE Mukai, K de Marino, D Abbot, TMC di Mille, F AF Mason, Elena Bianchini, Antonio Orio, Marina Williams, Robert E. Mukai, Koji de Marino, Domitilla Abbot, Timothy M. C. di Mille, Francesco BE Woudt, PA Ribeiro, VARM TI The Multiple Periods and the Magnetic Nature of CP Puppis SO STELLA NOVAE: PAST AND FUTURE DECADES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 4th International Conference on Classical and Recurrent Novae - Stella Novae: Past and Future Decades CY FEB 04-08, 2013 CL Pavilion Clock Tower, Cape Town, SOUTH AFRICA SP Univ Cape Town, Natl Res Fdn, S African Astron Observ, Univ Cape Town, Astrophys Cosmol & Grav Ctr, Royal Astron Soc, Square Kilometre Array S Africa Project Off HO Pavilion Clock Tower ID OLD NOVA; DQ AB Fast cadence time resolved spectra taken at the CTIO-4 m telescope with the RC-spectrograph during 2 consecutive nights revealed a long term modulation of the binary radial velocity. Chandra hard X-ray spectra taken with the HETGS instrument showed features typically observed in magnetic white dwarfs. Here, we present the new data and suggest that CP Pup is possibly a long orbital period intermediate polar. C1 [Mason, Elena; Williams, Robert E.] STScI, Baltimore, MD 21218 USA. [Bianchini, Antonio; di Mille, Francesco] Univ Padua, I-35122 Padua, Italy. [Orio, Marina] INAF Padova, I-35122 Padua, Italy. [Mukai, Koji] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [de Marino, Domitilla] INAF Capodimonte, I-80131 Naples, Italy. [Abbot, Timothy M. C.] CTIO, La Serena, Chile. [Orio, Marina] Univ Wisconsin, Madison, WI 53704 USA. RP Mason, E (reprint author), STScI, Baltimore, MD 21218 USA. NR 17 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-864-0 J9 ASTR SOC P PY 2014 VL 490 BP 63 EP 66 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE1ZC UT WOS:000368750100007 ER PT B AU Evans, A Gehrz, RD Woodward, CE Helton, LA AF Evans, A. Gehrz, R. D. Woodward, C. E. Helton, L. A. BE Woudt, PA Ribeiro, VARM TI A WISE View of Novae SO STELLA NOVAE: PAST AND FUTURE DECADES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 4th International Conference on Classical and Recurrent Novae - Stella Novae: Past and Future Decades CY FEB 04-08, 2013 CL Pavilion Clock Tower, Cape Town, SOUTH AFRICA SP Univ Cape Town, Natl Res Fdn, S African Astron Observ, Univ Cape Town, Astrophys Cosmol & Grav Ctr, Royal Astron Soc, Square Kilometre Array S Africa Project Off HO Pavilion Clock Tower ID RS OPHIUCHI; CLASSICAL NOVAE; 2006 ERUPTION; DUST; ENVIRONMENT; SPECTRA; MISSION; EJECTA AB We present the result of trawling through the WISE archive for data on classical and recurrent novae. The data show a variety of spectral energy distributions, including stellar photospheres, dust and probable line emission. During the mission WISE also detected some novae which erupted subsequent to the survey, providing information about the progenitor systems. C1 [Evans, A.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Gehrz, R. D.; Woodward, C. E.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Helton, L. A.] NASA, SOFIA Sci Ctr, USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Evans, A (reprint author), Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. NR 21 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-864-0 J9 ASTR SOC P PY 2014 VL 490 BP 237 EP 242 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE1ZC UT WOS:000368750100032 ER PT B AU Rushton, MT Woodward, CE Helton, LA Gehrz, RD Evans, A Kaminsky, B Pavlenko, YV Eyres, SPS Maxwell, M AF Rushton, M. T. Woodward, C. E. Helton, L. A. Gehrz, R. D. Evans, A. Kaminsky, B. Pavlenko, Ya V. Eyres, S. P. S. Maxwell, M. BE Woudt, PA Ribeiro, VARM TI Silicate Dust in RS Ophiuchi SO STELLA NOVAE: PAST AND FUTURE DECADES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 4th International Conference on Classical and Recurrent Novae - Stella Novae: Past and Future Decades CY FEB 04-08, 2013 CL Pavilion Clock Tower, Cape Town, SOUTH AFRICA SP Univ Cape Town, Natl Res Fdn, S African Astron Observ, Univ Cape Town, Astrophys Cosmol & Grav Ctr, Royal Astron Soc, Square Kilometre Array S Africa Project Off HO Pavilion Clock Tower ID SPITZER-SPACE-TELESCOPE; SYMBIOTIC STARS; 1985 OUTBURST; RECURRENT NOVAE; 2006 ERUPTION; INFRARED OBSERVATIONS; GIANT; ENVIRONMENT; SYSTEMS AB We present Spitzer IRS spectra of the recurrent nova RS Ophiuchi obtained between 2006 and 2009. The data show emission lines due to H i, [Ne II], [Ne v], [Ne VI] and [0 IV] and the well known silicate features at 10 mu m and 18 mu m, whose behaviour are reported here. The silicate features are variable in the period covered by the observations, appearing strongest in our 2007 data. Interestingly, the central wavelength of the 18 m band is shorter than observed in other symbiotic systems and other circumstellar environments, suggesting unusual grain properties in RS Oph. We report changes that have taken place in the dusty environment in RS Oph and investigate the properties of the dust grains. C1 [Rushton, M. T.; Eyres, S. P. S.; Maxwell, M.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Woodward, C. E.; Gehrz, R. D.] Univ Minnesota, Minneapolis, MN 55455 USA. [Helton, L. A.] NASA, Ames Res Ctr, SOFIA, Moffat Field, CA 94035 USA. [Evans, A.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Kaminsky, B.; Pavlenko, Ya V.] Natl Acad Sci Ukraine, Main Observ, UA-03680 Kiev, Ukraine. RP Rushton, MT (reprint author), Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. NR 29 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-864-0 J9 ASTR SOC P PY 2014 VL 490 BP 249 EP 254 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE1ZC UT WOS:000368750100034 ER PT B AU Williams, SC Bode, MF Darnley, MJ Zubko, V Evans, A Shafter, AW AF Williams, S. C. Bode, M. F. Darnley, M. J. Zubko, V. Evans, A. Shafter, A. W. BE Woudt, PA Ribeiro, VARM TI Rapid Dust Formation in Novae: Speed Class and Grain Formation Timescale SO STELLA NOVAE: PAST AND FUTURE DECADES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 4th International Conference on Classical and Recurrent Novae - Stella Novae: Past and Future Decades CY FEB 04-08, 2013 CL Pavilion Clock Tower, Cape Town, SOUTH AFRICA SP Univ Cape Town, Natl Res Fdn, S African Astron Observ, Univ Cape Town, Astrophys Cosmol & Grav Ctr, Royal Astron Soc, Square Kilometre Array S Africa Project Off HO Pavilion Clock Tower AB Observations show that the time of onset of dust formation in classical novae depends strongly on their speed class, with dust typically taking longer to form in slower novae. Using empirical relationships of speed class, luminosity and ejection velocity, it can be shown that dust formation timescale is expected to be essentially independent of speed class. However, following a nova outburst the spectrum of the central hot source evolves, with an increasing proportion of the radiation being emitted blue-wards of the Lyman limit. The rate at which the spectrum evolves depends on the speed class. We have therefore refined the simple model by assuming photons at wavelengths shorter than the Lyman limit are absorbed by neutral hydrogen gas internal to the dust formation sites. We find that the dust formation timescale is then dependent on speed class and the predicted relationship agrees well with the observations. C1 [Williams, S. C.; Bode, M. F.; Darnley, M. J.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Zubko, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Evans, A.] Keele Univ, Lennard Jones Lab, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Shafter, A. W.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Williams, SC (reprint author), Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. NR 12 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-864-0 J9 ASTR SOC P PY 2014 VL 490 BP 255 EP 260 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE1ZC UT WOS:000368750100035 ER PT B AU Helton, LA Evans, A Woodward, CE Gehrz, RD Vacca, W AF Helton, L. Andrew Evans, A. Woodward, C. E. Gehrz, R. D. Vacca, W. BE Woudt, PA Ribeiro, VARM TI The Dusty Nova: An Examination of Dust Production and Processing in the Ejecta of Classical Novae SO STELLA NOVAE: PAST AND FUTURE DECADES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 4th International Conference on Classical and Recurrent Novae - Stella Novae: Past and Future Decades CY FEB 04-08, 2013 CL Pavilion Clock Tower, Cape Town, SOUTH AFRICA SP Univ Cape Town, Natl Res Fdn, S African Astron Observ, Univ Cape Town, Astrophys Cosmol & Grav Ctr, Royal Astron Soc, Square Kilometre Array S Africa Project Off HO Pavilion Clock Tower ID SPITZER-SPACE-TELESCOPE; EMISSION; SPECTROSCOPY AB Classical novae (CNe) are known to frequently produce dust in their ejecta. Infrared observations have revealed that the dust produced can be of a variety of different species, including silicates, amorphous carbon, hydrocarbons, and silicon carbide. Due to their relatively rapid evolution, CNe provide unique laboratories for the examination of the processes of dust condensation, grain growth, and destruction. Here we present analysis of the near- to mid-IR spectra of a number of recent dust forming novae, including V2361 Cyg, V2362 Cyg, and V1280 Sco. We discuss the implications for our understanding of dust formation and processing with particular emphasis on the role of hydrocarbon species. C1 [Helton, L. Andrew; Vacca, W.] NASA Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Evans, A.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Woodward, C. E.; Gehrz, R. D.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. RP Helton, LA (reprint author), NASA Ames Res Ctr, SOFIA Sci Ctr, Mail Stop 232-12, Moffett Field, CA 94035 USA. NR 24 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-864-0 J9 ASTR SOC P PY 2014 VL 490 BP 261 EP 266 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE1ZC UT WOS:000368750100036 ER PT B AU Mukai, K Nelson, T Chomiuk, L Mioduszewski, A Rupen, MP Sokoloski, JL Weston, JHS Bode, MF Eyres, SPS O'Brien, TJ AF Mukai, K. Nelson, T. Chomiuk, L. Mioduszewski, A. Rupen, M. P. Sokoloski, J. L. Weston, J. H. S. Bode, M. F. Eyres, S. P. S. O'Brien, T. J. BE Woudt, PA Ribeiro, VARM TI X-ray Observations of Shocked Nova Ejecta SO STELLA NOVAE: PAST AND FUTURE DECADES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 4th International Conference on Classical and Recurrent Novae - Stella Novae: Past and Future Decades CY FEB 04-08, 2013 CL Pavilion Clock Tower, Cape Town, SOUTH AFRICA SP Univ Cape Town, Natl Res Fdn, S African Astron Observ, Univ Cape Town, Astrophys Cosmol & Grav Ctr, Royal Astron Soc, Square Kilometre Array S Africa Project Off HO Pavilion Clock Tower ID HERCULIS 1991; RS-OPHIUCHI; EMISSION; OUTBURST; MODEL AB We present X-ray observations of novae, obtained in conjunction with radio observations. The 1-10 keV X-rays are optically thin thermal emission from the ejecta shock-heated to >10 million degrees, while the radio emission is often dominated by Bremsstrahlung emission from similar to 10,000 K gas, perhaps with additional contributions from shocks. The very presence of hard X-ray emission requires faster ejecta to catch up with a slower material ejected earlier. The X-ray temperatures allow us to estimate the velocity differential between the two systems. Non-ionization-equilibrium signatures, when present, allow us to constrain the density of the shocked plasma. The absorbing columns, usually observed to decrease as the ejecta expand, constrain the amount of the slower, earlier ejecta that still remain unshocked. Specifically, we will present our analysis of the Swift and Suzaku observations of T Pyx and Nova Mon 2012 and discuss implications. C1 [Mukai, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Mukai, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Mukai, K.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Chomiuk, L.; Mioduszewski, A.; Rupen, M. P.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Chomiuk, L.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Sokoloski, J. L.; Weston, J. H. S.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Bode, M. F.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Eyres, S. P. S.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [O'Brien, T. J.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Mukai, K (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. NR 18 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-864-0 J9 ASTR SOC P PY 2014 VL 490 BP 327 EP 332 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE1ZC UT WOS:000368750100044 ER PT B AU Weston, JHS Sokoloski, JL Zheng, Y Chomiuk, L Mioduszewsld, A Mukai, K Rupen, MP Krauss, MI Roy, N Nelson, T AF Weston, Jennifer H. S. Sokoloski, Jennifer L. Zheng, Yong Chomiuk, Laura Mioduszewsld, Amy Mukai, Koji Rupen, Michael P. Krauss, Miriam I. Roy, Nirupam Nelson, Thomas BE Woudt, PA Ribeiro, VARM TI Shocks and Ejecta Mass: Radio Observations of Nova V1723 Aql SO STELLA NOVAE: PAST AND FUTURE DECADES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 4th International Conference on Classical and Recurrent Novae - Stella Novae: Past and Future Decades CY FEB 04-08, 2013 CL Pavilion Clock Tower, Cape Town, SOUTH AFRICA SP Univ Cape Town, Natl Res Fdn, S African Astron Observ, Univ Cape Town, Astrophys Cosmol & Grav Ctr, Royal Astron Soc, Square Kilometre Array S Africa Project Off HO Pavilion Clock Tower ID RS OPHIUCHI; CLASSICAL NOVAE; EMISSION; OUTBURST; IMAGES AB The radio light curves of novae rise and fall over the course of months to years, allowing for detailed observations of the evolution of the nova shell. However, the main parameter determined by radio models of nova explosions the mass of the ejecta often seems to exceed theoretical expectations by an order of magnitude. With the recent technological improvements on the Karl G. Jansky Very Large Array (VLA), new observations can test the assumptions upon which ejecta mass estimates are based. Early observations of the classical nova V1723 Aql showed an unexpectedly rapid rise in radio flux density and a distinct bump in the radio light curve on the rise to radio maximum, which is inconsistent with the simple model of spherical ejecta expelled in a single discrete event. This initial bump appears to indicate the presence of shocked material in the outer region of the ejected shell, with the emission from the shocks fading over time. We explore possible origins for this emission and its relation to the mass loss history of the nova. The evolution of the radio spectrum also reveals the density profile, the mass of the ejected shell, and other properties of the ejecta. These observations comprise one of the most complete, longterm set of multi wavelength radio observations for any classical nova to date. C1 [Weston, Jennifer H. S.; Sokoloski, Jennifer L.; Zheng, Yong] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Chomiuk, Laura] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Chomiuk, Laura; Mioduszewsld, Amy; Rupen, Michael P.; Krauss, Miriam I.; Roy, Nirupam] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Mukai, Koji] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Mukai, Koji] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Mukai, Koji] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Nelson, Thomas] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. RP Weston, JHS (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. NR 16 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-864-0 J9 ASTR SOC P PY 2014 VL 490 BP 339 EP 344 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE1ZC UT WOS:000368750100046 ER PT B AU Helton, LA AF Helton, L. Andrew CA SOFIA Sci Team BE Woudt, PA Ribeiro, VARM TI SOFIA: A Promising Resource for Future Nova Studies SO STELLA NOVAE: PAST AND FUTURE DECADES SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 4th International Conference on Classical and Recurrent Novae - Stella Novae: Past and Future Decades CY FEB 04-08, 2013 CL Pavilion Clock Tower, Cape Town, SOUTH AFRICA SP Univ Cape Town, Natl Res Fdn, S African Astron Observ, Univ Cape Town, Astrophys Cosmol & Grav Ctr, Royal Astron Soc, Square Kilometre Array S Africa Project Off HO Pavilion Clock Tower ID NO. 2 AB The Stratospheric Observatory for Infrared Astronomy (SOFIA) is a 2.5-m telescope carried on board a Boeing 747-SP aircraft. Optimized for observations from infrared through sub-nun wavelengths, SOFIA observes from an altitude of 37,000 - 45,000 feet, above 99% of the atmospheric water vapor. The Observatory's complement of instruments possesses a broad range of capabilities, many of which are especially well suited for observations of classical novae, recurrent novae, and other cataclysmic variables. Here we present a selection of the instruments available on board SOFIA that may prove to be very useful for future novae studies. C1 [Helton, L. Andrew; SOFIA Sci Team] NASA, Ames Res Ctr, SOFIA Sci Ctr, Mail Stop 232-12, Moffett Field, CA 94035 USA. RP Helton, LA (reprint author), NASA, Ames Res Ctr, SOFIA Sci Ctr, Mail Stop 232-12, Moffett Field, CA 94035 USA. NR 6 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-864-0 J9 ASTR SOC P PY 2014 VL 490 BP 401 EP 404 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE1ZC UT WOS:000368750100057 ER PT B AU Borrego, E AF Borrego, Espiridion Al BE Klingner, DE Espinosa, RM TI How Cartel Violence Is Affecting Cross-Border Collaboration SO USING THE NARCOTRAFICO THREAT TO BUILD PUBLIC ADMINISTRATION CAPACITY BETWEEN THE US AND MEXICO SE American Society for Public Administration Series on Public Administration and Public Policy LA English DT Article; Book Chapter C1 [Borrego, Espiridion Al] Univ Texas Pan Amer, Dept Secur Studies & Publ Affairs, Edinburg, TX 78541 USA. [Borrego, Espiridion Al] President Obamas Transit Team, Washington, DC USA. [Borrego, Espiridion Al] Alignment Strategies Inc ALS, Washington, DC USA. [Borrego, Espiridion Al] US Dept Labor, Vet Employment & Training, Washington, DC 20210 USA. [Borrego, Espiridion Al] Univ Alaska Southeast, Sch Business & Publ Adm, Juneau, AK USA. [Borrego, Espiridion Al] NASA, Off Comptroller, Washington, DC 20546 USA. [Borrego, Espiridion Al] Ford Fdn, New York, NY USA. RP Borrego, E (reprint author), Univ Texas Pan Amer, Dept Secur Studies & Publ Affairs, Edinburg, TX 78541 USA. EM alborrego@utpa.edu NR 19 TC 0 Z9 0 U1 0 U2 0 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-1-4665-7110-5; 978-1-4665-7109-9 J9 AM SOC PUBLIC ADMIN PY 2014 BP 163 EP 178 D2 10.1201/b16582 PG 16 WC Criminology & Penology; Public Administration SC Criminology & Penology; Public Administration GA BF9YK UT WOS:000386053800011 ER PT J AU Solomon, J Chung, P Srivastava, D Darve, E AF Solomon, Jose Chung, Peter Srivastava, Deepak Darve, Eric TI Method and advantages of genetic algorithms in parameterization of interatomic potentials: Metal oxides SO COMPUTATIONAL MATERIALS SCIENCE LA English DT Article DE Genetic algorithms; Shell model potential; Molecular dynamics; Perovskite metal oxide; Barium titanate ID ATOMIC-LEVEL SIMULATION; BARIUM-TITANATE; SILICON; BATIO3; FERROELECTRICITY; TEMPERATURE; CRYSTALS; DESIGN; PHASES; ENERGY AB The method and the advantages of an evolutionary computing based approach using a steady state genetic algorithm (GA) for the parameterization of interatomic potentials for metal oxides within the shell model framework are developed and described. We show that the GA based methodology for the parameterization of interatomic force field functions is capable of (a) simultaneous optimization of the multiple phases or properties of a material in a single run, (b) facilitates the incremental re-optimization of the whole system as more data is made available for either additional phases or material properties not included in previous runs, and (c) successful global optimization in the presence of multiple local minima in the parameter space. As an example, we apply the method towards simultaneous optimization of four distinct crystalline phases of Barium Titanate (BaTiO3 or BTO) using an ab initio density functional theory (DFT) based reference dataset. We find that the optimized force field function is capable of the prediction of the two phases not used in the optimization procedure, and that many derived physical properties such as the equilibrium lattice constants, unit cell volume, elastic properties, coefficient of thermal expansion, and average electronic polarization are in good agreement with the experimental results available from the literature. (C) 2013 Elsevier B.V. All rights reserved. C1 [Solomon, Jose; Darve, Eric] Stanford Univ, Dept Mech Engn, Stanford, CA 94305 USA. [Chung, Peter] US Army Res Lab, Aberdeen Proving Ground, MD USA. [Srivastava, Deepak] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Solomon, J (reprint author), Durand Bldg,Room 229, Stanford, CA 94305 USA. EM jose.e.solomon@gmail.com FU US Army Research Laboratory (ARL), through the Army High Performance Computing Research Center [W911NF-07-0027]; Alfred P. Sloan Foundation; National Science Foundation Graduate Research Fellowship FX This research was performed at Stanford University and supported in part by the US Army Research Laboratory (ARL), through the Army High Performance Computing Research Center, Cooperative Agreement W911NF-07-0027. Additional funding for J.E. Solomon came from the Alfred P. Sloan Foundation and the National Science Foundation Graduate Research Fellowship. Special acknowledgement goes to L. Munday of ARL for his insightful talks with J.E. Solomon with regards to the use of DL_POLY. NR 53 TC 2 Z9 2 U1 4 U2 28 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-0256 EI 1879-0801 J9 COMP MATER SCI JI Comput. Mater. Sci. PD JAN PY 2014 VL 81 BP 453 EP 465 DI 10.1016/j.commatsci.2013.08.054 PG 13 WC Materials Science, Multidisciplinary SC Materials Science GA 251OU UT WOS:000326940300064 ER PT J AU Bux, SK Zevalkink, A Janka, O Uhl, D Kauzlarich, S Snyder, JG Fleurial, JP AF Bux, Sabah K. Zevalkink, Alexandra Janka, Oliver Uhl, David Kauzlarich, Susan Snyder, Jeffrey G. Fleurial, Jean-Pierre TI Glass-like lattice thermal conductivity and high thermoelectric efficiency in Yb9Mn4.2Sb9 SO JOURNAL OF MATERIALS CHEMISTRY A LA English DT Article ID POWER-GENERATION; ZINTL COMPOUND; RARE-EARTH; YB14MNSB11; CHEMISTRY; ALLOYS; PHASES AB Motivated by excellent thermoelectric performance in the well-known Yb-based Zintl compounds Yb14MnSb11 and YbZn2-xMnxSb2, this study investigates the thermoelectric properties of Yb9Mn4.2Sb9. Unlike most transition metal containing Zintl phases, Yb9Mn4.2Sb9 contains a partially occupied Mn site and thus does not have a valence-precise stoichiometry. Samples were synthesized by direct ball milling of the elements, followed by hot pressing. Consistent with previous reports, X-ray diffraction and wavelength dispersive spectroscopy confirmed a narrow composition range near Yb9Mn4.2Sb9. High temperature measurements of the electronic properties of Yb9Mn4.2Sb9 indicate that it is a degenerate p-type semiconductor with a band gap sufficiently large for high temperature thermoelectric applications. Hall measurements reveal that Yb9Mn4.2Sb9 has a high extrinsic carrier concentration (similar to 10(20) h(+) cm(-3)), which is due to the deviation from the theoretical "Zintl composition" of Yb9Mn4.5Sb9. The measured carrier concentration coincides with the optimum concentration predicted using a single parabolic band model. Measurements of the thermal diffusivity and heat capacity reveal an extremely low, temperature-independent lattice thermal conductivity in this compound (k(L) < 0.4 W mK(-1)), which is due to both the large unit cell size (44 atoms per primitive cell) and substantial disorder on the Mn site. This favorable combination of optimized electronic properties and low lattice thermal conductivity leads to a promising figure of merit at high temperature (zT = 0.7 at 950 K). C1 [Bux, Sabah K.; Uhl, David; Fleurial, Jean-Pierre] CALTECH, Jet Prop Lab, Thermal Energy Convers Technol Grp, Pasadena, CA 91109 USA. [Zevalkink, Alexandra; Snyder, Jeffrey G.] CALTECH, Dept Mat Sci, Pasadena, CA 91125 USA. [Janka, Oliver; Kauzlarich, Susan] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA. RP Bux, SK (reprint author), CALTECH, Jet Prop Lab, Thermal Energy Convers Technol Grp, 4800 Oak Grove Dr,MS 277-207, Pasadena, CA 91109 USA. EM sabah.k.bux@jpl.nasa.gov RI Janka, Oliver/B-3233-2011 OI Janka, Oliver/0000-0002-9480-3888 FU National Aeronautics and Space Administration; NASA Science Missions Directorate's Radioisotope Power Systems Technology Advancement Program FX The authors would like to thank Dr Thierry Caillat for his helpful discussions. They would also like to thank Leslie D. Zoltan, George Nakatsukasa and Dr Pawan Gogna for their assistance in sample characterization and measurement. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. This work was supported by the NASA Science Missions Directorate's Radioisotope Power Systems Technology Advancement Program. NR 29 TC 41 Z9 42 U1 8 U2 64 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 2050-7488 EI 2050-7496 J9 J MATER CHEM A JI J. Mater. Chem. A PY 2014 VL 2 IS 1 BP 215 EP 220 DI 10.1039/c3ta14021k PG 6 WC Chemistry, Physical; Energy & Fuels; Materials Science, Multidisciplinary SC Chemistry; Energy & Fuels; Materials Science GA 260TZ UT WOS:000327618600025 ER PT J AU Plotnikov, EY Mao, ZG Noebe, RD Seidman, DN AF Plotnikov, Elizaveta Y. Mao, Zugang Noebe, Ronald D. Seidman, David N. TI Temporal evolution of the gamma(fcc)/gamma '(L1(2)) interfacial width in binary Ni-Al alloys SO SCRIPTA MATERIALIA LA English DT Article DE Atom-probe tomography; Nickel aluminum alloys; Interfacial width; Vacancy-mediated lattice kinetic Monte Carlo simulations ID 3-DIMENSIONAL ATOM-PROBE; CR-AL; PHASE-SEPARATION; COARSENING BEHAVIOR; KINETIC PATHWAYS; SOLID-SOLUTION; GAMMA'-PHASE; MODEL; SUPERALLOY; PRECIPITATION AB The temporal evolution of gamma'(L1(2) structure) precipitates is studied in Ni-12.5 at.% A1 and Ni-13.4 at.% A1 alloys, aged at 823 and 873 K, utilizing three-dimensional atom-probe tomography. The values of the interfacial widths, delta(t)s, between the gamma(face-centered cubic) and gamma' phases are calculated utilizing proximity histograms. It is demonstrated that delta(t) decreases continuously with increasing aging time for both Ni-Al alloys: that is, the delta(t)s decrease with increasing mean precipitate radius, (R(t)). The ratio delta(t)/(R(t)) decreases, to first order, as (C) 2013 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Plotnikov, Elizaveta Y.; Mao, Zugang; Seidman, David N.] Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA. [Noebe, Ronald D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Seidman, David N.] Northwestern Univ, Ctr Atom Probe Tomog, Evanston, IL 60208 USA. RP Seidman, DN (reprint author), Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA. EM d-seidman@northwestern.edu RI Seidman, David/B-6697-2009 FU National Science Foundation; Division of Materials Research (DMR) [1207539]; NSF-MRI [DMR-0420532]; ONR-DURIP [N00014-0400798, N00014-0610539, N00014-0910781]; National Science Foundation [DMR-1121262] FX This research was supported by the National Science Foundation, Division of Materials Research (DMR) Grant No. 1207539, Prof. Eric Taleff, grant officer. Atom-probe tomography was performed at the Northwestern University Center for Atom-Probe Tomography (NUCAPT), whose LEAP tomograph was purchased and upgraded with funding from NSF-MRI (DMR-0420532) and ONR-DURIP (N00014-0400798, N00014-0610539, N00014-0910781) grants. Instrumentation at NUCAPT was further upgraded by the Initiative for Sustainability and Energy at Northwestern (ISEN). NUCAPT is a Shared Facility at the Materials Research Center of Northwestern University, partially supported by the National Science Foundation's MRSEC program (DMR-1121262). The authors thank Dr. Georges Martin for his insightful comments and a critical reading of the manuscript. NR 49 TC 9 Z9 10 U1 1 U2 35 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6462 J9 SCRIPTA MATER JI Scr. Mater. PD JAN 1 PY 2014 VL 70 BP 51 EP 54 DI 10.1016/j.scriptamat.2013.09.016 PG 4 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 255HV UT WOS:000327230900012 ER PT J AU Williams, PE Pesnell, WD Beck, JG Lee, S AF Williams, Peter E. Pesnell, W. Dean Beck, John G. Lee, Shannon TI Analysis of Supergranule Sizes and Velocities Using Solar Dynamics Observatory (SDO)/Helioseismic Magnetic Imager (HMI) and Solar and Heliospheric Observatory (SOHO)/Michelson Doppler Imager (MDI) Dopplergrams SO SOLAR PHYSICS LA English DT Article DE Sun: convection; Dopplergrams; Helioseismology; Sun: photosphere; SDO/HMI; SOHO/MDI; Sun: supergranulation ID STEADY PHOTOSPHERIC FLOWS; SPHERICAL HARMONIC-ANALYSIS; CHROMOSPHERIC NETWORK; MAGNETIC-FIELDS; SUPERROTATION; ATMOSPHERE; EVOLUTION; SPECTRUM; IMAGER; SDO AB Co-temporal Doppler images from Solar and Heliospheric Observatory (SOHO)/Michelson Doppler Imager (MDI) and Solar Dynamics Observatory (SDO)/Helioseismic Magnetic Imager (HMI) have been analyzed to extract quantitative information about global properties of the spatial and temporal characteristics of solar supergranulation. Preliminary comparisons show that supergranules appear to be smaller and have stronger horizontal velocity flows within HMI data than was measured with MDI. There appears to be no difference in their evolutionary timescales. Supergranule sizes and velocities were analyzed over a ten-day time period at a 15-minute cadence. While the averages of the time-series retain the aforementioned differences, fluctuations of these parameters first observed in MDI data were seen in both MDI and HMI time-series, exhibiting a strong cross-correlation. This verifies that these fluctuations are not instrumental, but are solar in origin. The observed discrepancies between the averaged values from the two sets of data are a consequence of instrument resolution. The lower spatial resolution of MDI results in larger observed structures with lower velocities than is seen in HMI. While these results offer a further constraint on the physical nature of supergranules, they also provide a level of calibration between the two instruments. C1 [Williams, Peter E.] No Virginia Community Coll, Dept Phys, Annandale, VA 22003 USA. [Williams, Peter E.] Catholic Univ Amer, Washington, DC 20064 USA. [Williams, Peter E.; Pesnell, W. Dean] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Beck, John G.] Stanford Univ, Stanford, CA 94305 USA. [Lee, Shannon] San Francisco State Univ, San Francisco, CA 94132 USA. RP Williams, PE (reprint author), No Virginia Community Coll, Dept Phys, Annandale, VA 22003 USA. EM pewilliams@nvcc.edu; william.d.pesnell@nasa.gov; jbeck@solar.stanford.edu; shannonl@sfsu.edu RI Pesnell, William/D-1062-2012 OI Pesnell, William/0000-0002-8306-2500 FU NASA Postdoctoral Program at NASA Goddard Space Flight Center FX This research was supported by an appointment to the NASA Postdoctoral Program at NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA via the Solar Dynamics Observatory. SDO is part of NASA's Living With a Star (LWS) program. HMI was designed and assembled at Stanford University and Lockheed Martin Solar and Astrophysics Laboratory. SOHO is a project of international cooperation between ESA and NASA. The authors wish to thank the referee for the comments that further enhanced the contents of this article. NR 38 TC 3 Z9 3 U1 1 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD JAN PY 2014 VL 289 IS 1 BP 11 EP 25 DI 10.1007/s11207-013-0330-8 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 253NL UT WOS:000327094700002 ER PT J AU Didkovsky, L Gurman, JB AF Didkovsky, L. Gurman, J. B. TI A Change in the Solar He II EUV Global Network Structure as an Indicator of the Geo-Effectiveness of Solar Minima SO SOLAR PHYSICS LA English DT Article DE Solar extreme ultraviolet irradiance; Solar cycle; Solar minimum ID UPPER-ATMOSPHERE; THERMOSPHERE; IONOSPHERE; FLUX AB Solar activity during 2007 -aEuro parts per thousand 2009 was very low, causing anomalously low thermospheric density. A comparison of solar extreme ultraviolet (EUV) irradiance in the He ii spectral band (26 to 34 nm) from the Solar Extreme ultraviolet Monitor (SEM), one of instruments on the Charge Element and Isotope Analysis System (CELIAS) on board the Solar and Heliospheric Observatory (SOHO) for the two latest solar minima showed a decrease of the absolute irradiance of about 15 +/- 6 % during the solar minimum between Cycles 23 and 24 compared with the Cycle 22/23 minimum when a yearly running-mean filter was used. We found that some local, shorter-term minima including those with the same absolute EUV flux in the SEM spectral band show a higher concentration of spatial power in the global network structure from the 30.4 nm SOHO/Extreme ultraviolet Imaging Telescope (EIT) images for the local minimum of 1996 compared with the minima of 2008 -aEuro parts per thousand 2011. We interpret this higher concentration of spatial power in the transition region's global network structure as a larger number of larger-area features on the solar disk. These changes in the global network structure during solar minima may characterize, in part, the geo-effectiveness of the solar He ii EUV irradiance in addition to the estimations based on its absolute levels. C1 [Didkovsky, L.] Univ So Calif, Ctr Space Sci, Los Angeles, CA 90089 USA. [Gurman, J. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Didkovsky, L (reprint author), Univ So Calif, Ctr Space Sci, Los Angeles, CA 90089 USA. EM leonid@usc.edu; Joseph.B.Gurman@nasa.gov FU University of Colorado [153-5979] FX This work was partially supported by the University of Colorado award 153-5979. SOHO is a project of international cooperation between NASA and ESA. NR 23 TC 1 Z9 1 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD JAN PY 2014 VL 289 IS 1 BP 153 EP 166 DI 10.1007/s11207-013-0329-1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 253NL UT WOS:000327094700010 ER PT J AU Love, SG Harvey, RP AF Love, Stanley G. Harvey, Ralph P. TI Crew autonomy for deep space exploration: Lessons from the Antarctic Search for Meteorites SO ACTA ASTRONAUTICA LA English DT Article DE Human space flight; Crew autonomy; Human exploration; Deep space exploration; Space flight analog; Antarctica AB Future piloted missions to explore asteroids, Mars, and other targets beyond the Moon will experience strict limitations on communication between vehicles in space and control centers on Earth. These limitations will require crews to operate with greater autonomy than any past space mission has demonstrated. The Antarctic Search for Meteorites (ANSMET) project, which regularly sends small teams of researchers to remote parts of the southern continent, resembles a space mission in many ways but does not rely upon a control center. It provides a useful crew autonomy model for planners of future deep space exploration missions. In contrast to current space missions, ANSMET gives the crew the authority to adjust competing work priorities, task assignments, and daily schedules; allows the crew to be the primary monitor of mission progress; demands greater crew accountability for operational errors; requires the crew to make the most of limited communication bandwidth; adopts systems designed for simple operation and failure recovery; and grants the crew a leading role in the selection and stowage of their equipment. Published by Elsevier Ltd. on behalf of IAA. C1 [Love, Stanley G.] NASA Johnson Space Ctr, Houston, TX 77058 USA. [Harvey, Ralph P.] Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA. RP Love, SG (reprint author), NASA Johnson Space Ctr, Mail Code CB,2101 NASA Pkwy, Houston, TX 77058 USA. EM stanley.g.love@nasa.gov; rph@case.edu FU NASA; NSF FX NASA and NSF funding supported this work. The authors thank Jeff Hanley and Lee Morin for their valuable feedback on an early draft of this paper, and two anonymous reviewers for suggestions that improved the final version. NR 12 TC 1 Z9 1 U1 1 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JAN-FEB PY 2014 VL 94 IS 1 BP 83 EP 92 DI 10.1016/j.actaastro.2013.08.001 PG 10 WC Engineering, Aerospace SC Engineering GA 245SJ UT WOS:000326483800008 ER PT J AU Youngquist, RC Nurge, MA Starr, SO Koontz, SL AF Youngquist, Robert C. Nurge, Mark A. Starr, Stanley O. Koontz, Steven L. TI Thick galactic cosmic radiation shielding using atmospheric data SO ACTA ASTRONAUTICA LA English DT Article DE Galactic cosmic radiation; Radiation protection; Radiation shielding; Inverse problem; Atmospheric radiation ID EXPOSURE; TRAVEL AB NASA is concerned with protecting astronauts from the effects of galactic cosmic radiation and has expended substantial effort in the development of computer models to predict the shielding obtained from various materials. However, these models were only developed for shields up to about 120 g/cm(2) in mass thickness and have predicted that shields of this mass thickness are insufficient to provide adequate protection for extended deep space flights. Consequently, effort is underway to extend the range of these models to thicker shields and experimental data is required to help confirm the resulting code. In this paper empirically obtained effective dose measurements from aircraft flights in the atmosphere are used to obtain the radiation shielding function of the Earth's atmosphere, a very thick, i.e. high mass, shield. Obtaining this result required solving an inverse problem and the method for solving it is presented. The results are shown to be in agreement with current code in the ranges where they overlap. These results are then checked and used to predict the radiation dosage under thick shields such as planetary regolith and the atmosphere of Venus. Published by Elsevier Ltd. on behalf of IAA. C1 [Youngquist, Robert C.; Nurge, Mark A.; Starr, Stanley O.] NASA, Kennedy Space Ctr, FL 32899 USA. [Koontz, Steven L.] NASA, Johnson Space Ctr, TX 77058 USA. RP Youngquist, RC (reprint author), NASA, Mail Stop NE-L5, Kennedy Space Ctr, FL 32899 USA. EM Robert.C.Youngquist@nasa.gov NR 16 TC 0 Z9 0 U1 2 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JAN-FEB PY 2014 VL 94 IS 1 BP 132 EP 138 DI 10.1016/j.actaastro.2013.08.010 PG 7 WC Engineering, Aerospace SC Engineering GA 245SJ UT WOS:000326483800012 ER PT J AU Rayman, MD Mase, RA AF Rayman, Marc D. Mase, Robert A. TI Dawn's exploration of Vesta SO ACTA ASTRONAUTICA LA English DT Article DE Dawn; Ion propulsion; Solar electric propulsion; Asteroid; Vesta; Operations ID MISSION; CERES AB On 16 July 2011, after completing nearly four years of interplanetary flight, Dawn entered orbit around (4) Vesta, the second most massive body in the main asteroid belt. Dawn used solar electric propulsion to spiral to six different orbits to accomplish its science campaign. Although the transfers to progressively lower orbits presented significant challenges, all were executed smoothly. During its nearly 14 months in orbit, Dawn spiraled down to 210 km above the surface and back up before initiating the gradual departure to travel to dwarf planet (1) Ceres for a 2015 rendezvous. Dawn's exploration of Vesta has shown it to be geologically complex and fascinating, resembling terrestrial planets more than typical asteroids. Among the principal features is a 500-km-diameter impact basin within which is the second tallest mountain known in the solar system. This paper presents Dawn's operations at Vesta and summarizes the principal findings. (C) 2013 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Rayman, Marc D.; Mase, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rayman, MD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mrayman@jpl.nasa.gov NR 8 TC 4 Z9 4 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JAN-FEB PY 2014 VL 94 IS 1 BP 159 EP 167 DI 10.1016/j.actaastro.2013.08.003 PG 9 WC Engineering, Aerospace SC Engineering GA 245SJ UT WOS:000326483800015 ER PT J AU Folta, DC Pavlak, TA Haapala, AF Howell, KC Woodard, MA AF Folta, David C. Pavlak, Thomas A. Haapala, Amanda F. Howell, Kathleen C. Woodard, Mark A. TI Earth-Moon libration point orbit stationkeeping: Theory, modeling, and operations SO ACTA ASTRONAUTICA LA English DT Article; Proceedings Paper CT 1st International-Academy-of-Astronautics Conference on Dynamics and Control of Space Systems (DyCoSS) CY MAR 19-21, 2012 CL Porto, PORTUGAL SP Int Acad Astronaut DE Stationkeeping; ARTEMIS; Circular restricted three-body problem; Poincare maps ID RESTRICTED 3-BODY PROBLEM; PERIODIC-ORBITS; TRAJECTORIES; ENVIRONMENTS; TRANSITIONS; DESIGN AB Collinear Earth-Moon libration points have emerged as locations with immediate applications. These libration point orbits are inherently unstable and must be maintained regularly which constrains operations and maneuver locations. Stationkeeping is challenging due to relatively short time scales for divergence, effects of large orbital eccentricity of the secondary body, and third-body perturbations. Using the Acceleration Reconnection and Turbulence and Electrodynamics of the Moon's Interaction with the Sun (ARTEMIS) mission orbit as a platform, the fundamental behavior of the trajectories is explored using Poincare maps in the circular restricted three-body problem. Operational stationkeeping results obtained using the Optimal Continuation Strategy are presented and compared to orbit stability information generated from mode analysis based in dynamical systems theory. Published by Elsevier Ltd. on behalf of IAA. C1 [Folta, David C.; Woodard, Mark A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pavlak, Thomas A.; Haapala, Amanda F.; Howell, Kathleen C.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA. RP Folta, DC (reprint author), 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM david.c.folta@nasa.gov; tpavlak@purdue.edu; ahaapala@purdue.edu; howell@purdue.edu; mark.a.woodard@nasa.gov NR 29 TC 16 Z9 17 U1 2 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JAN-FEB PY 2014 VL 94 IS 1 BP 421 EP 433 DI 10.1016/j.actaastro.2013.01.022 PG 13 WC Engineering, Aerospace SC Engineering GA 245SJ UT WOS:000326483800038 ER PT B AU Hurst, J AF Hurst, Janet BE Schulz, MJ Shanov, VN Yin, Z TI Boron Nitride Nanotubes, Silicon Carbide Nanotubes, and Carbon Nanotubesd-A Comparison of Properties and Applications SO NANOTUBE SUPERFIBER MATERIALS: CHANGING ENGINEERING DESIGN LA English DT Article; Book Chapter ID CHEMICAL-VAPOR-DEPOSITION; IN-SITU; THERMAL-CONDUCTIVITY; SIC NANOTUBES; BN NANOTUBES; COMPOSITES; NANOWIRES; IMPROVEMENTS; ELECTRONICS; OXIDATION C1 NASA, Glenn Res Ctr, Cleveland, OH USA. RP Hurst, J (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. NR 82 TC 1 Z9 1 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS BN 978-1-4557-7864-5; 978-1-4557-7863-8 PY 2014 BP 267 EP 287 DI 10.1016/B978-1-4557-7863-8.00009-8 PG 21 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA BHP25 UT WOS:000326233300010 ER PT J AU Wal, RLV Bryg, VM Huang, CH AF Wal, Randy L. Vander Bryg, Victoria M. Huang, Chung-Hsuan TI Insights into the combustion chemistry within a gas-turbine driven auxiliary power unit as a function of fuel type and power level using soot nanostructure as a tracer SO FUEL LA English DT Article DE HRTEM; Soot; Nanostructure; Fullerenic; Curvature ID DIFFUSION FLAMES; AROMATIC-HYDROCARBONS; ETHYLENE FLAMES; GENERATED SOOT; FULLERENES; PYROLYSIS; EVOLUTION; PRESSURE; METHANE; IMPACT AB Particulate emissions were collected from an Auxiliary power unit (APU) directly upon TEM grids for particle characterization by HRTEM. Carbonaceous emissions from two fuels, a coal-based Fischer-Tropsch and standard JP-8 were compared, each at three power levels. Differences in soot nanostructure, specifically fullerenic content reveal changes in the combustion chemistry with engine power level, as do differences in aggregate size between the two fuels. As inferred from the soot nanostructure, comparison between fuels demonstrates the impact of fuel structure upon soot formation chemistry. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Wal, Randy L. Vander; Huang, Chung-Hsuan] Penn State Univ, John & Willie Leone Family Dept Energy & Mineral, University Pk, PA 16802 USA. [Wal, Randy L. Vander; Huang, Chung-Hsuan] Penn State Univ, EMS Energy Inst, University Pk, PA 16802 USA. [Bryg, Victoria M.] USRA, NCSER, NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Wal, RLV (reprint author), Penn State Univ, John & Willie Leone Family Dept Energy & Mineral, University Pk, PA 16802 USA. EM ruv12@psu.edu FU NASA Aeronautics Subsonic Fixed Wing (SSFW) Program, NASA [NNX09AD42A]; Pennsylvania State University, at University Park PA FX The authors gratefully acknowledge sample collection during the weeks of field campaign testing by Dr. Kathleen Tacina (NASA-Glenn) and overall project coordination and steadfast experimental aid and technical input by Dr. Bruce Anderson (NASA-Langley). Support for this work was through the NASA Aeronautics Subsonic Fixed Wing (SSFW) Program, NASA Cooperative Agreement NNX09AD42A with The Pennsylvania State University, at University Park PA. NR 36 TC 0 Z9 0 U1 3 U2 24 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0016-2361 EI 1873-7153 J9 FUEL JI Fuel PD JAN PY 2014 VL 115 BP 282 EP 287 DI 10.1016/j.fuel.2013.07.011 PG 6 WC Energy & Fuels; Engineering, Chemical SC Energy & Fuels; Engineering GA 234LY UT WOS:000325647000032 ER PT J AU Willson, D Rask, JC George, SC de Leon, P Bonaccorsi, R Blank, J Slocombe, J Silburn, K Steele, H Gargarno, M Mckay, CP AF Willson, D. Rask, J. C. George, S. C. de Leon, P. Bonaccorsi, R. Blank, J. Slocombe, J. Silburn, K. Steele, H. Gargarno, M. McKay, C. P. TI The performance of field scientists undertaking observations of early life fossils while in simulated space suit SO ACTA ASTRONAUTICA LA English DT Article DE Space suit; Off-world; Field science; Pilbara; Stromatolites; Scientist astronauts ID WESTERN-AUSTRALIA; STROMATOLITE REEF; PILBARA CRATON; MARS; OLD AB We conducted simulated Apollo Extravehicular Activity's (EVA) at the 3.45 Ga Australian 'Pilbara Dawn of life' (Western Australia) trail with field and non-field scientists using the University of North Dakota's NDX-1 pressurizable space suit to overview the effectiveness of scientist astronauts employing their field observation skills while looking for stromatolite fossil evidence. Off-world scientist astronauts will be faced with space suit limitations in vision, human sense perception, mobility, dexterity, the space suit fit, time limitations, and the psychological fear of death from accidents, causing physical fatigue reducing field science performance. Finding evidence of visible biosignatures for past life such as stromatolite fossils, on Mars, is a very significant discovery. Our preliminary overview trials showed that when in simulated EVAs, 25% stromatolite fossil evidence is missed with more incorrect identifications compared to ground truth surveys but providing quality characterization descriptions becomes less affected by simulated EVA limitations as the science importance of the features increases. Field scientists focused more on capturing high value characterization detail from the rock features whereas non-field scientists focused more on finding many features. We identified technologies and training to improve off-world field science performance. The data collected is also useful for NASA's "EVA performance and crew health" research program requirements but further work will be required to confirm the conclusions. (C) 2013 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Willson, D.] NASA Ames Res Ctr, KISS Inst Pract Robot, Moffett Field, CA 94035 USA. [Rask, J. C.] NASA Ames Res Ctr, Dynamac Corp, Space Biosci Div, Moffett Field, CA 94035 USA. [George, S. C.] Macquarie Univ, Dept Earth & Planetary Sci, N Ryde, NSW 2109, Australia. [de Leon, P.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. [Bonaccorsi, R.; Blank, J.] SETI Inst, Mountain View, CA 94043 USA. [Slocombe, J.] Creators Orb Educ & Training Consultants, Redwood Pk, SA 5097, Australia. [Silburn, K.] Casula High Sch, Casula, NSW 2170, Australia. [Steele, H.] Univ Sydney, Wesley Coll, Sydney, NSW 2006, Australia. [Gargarno, M.] Curtin Univ, Dept Imaging & Appl Phys, Bentley, WA 6102, Australia. [McKay, C. P.] NASA Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP Willson, D (reprint author), NASA Ames Res Ctr, KISS Inst Pract Robot, Bldg 245, Moffett Field, CA 94035 USA. EM david.willson@nasa.gov RI George, Simon/G-7134-2015 OI George, Simon/0000-0001-6534-3846 NR 28 TC 3 Z9 3 U1 0 U2 20 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JAN PY 2014 VL 93 BP 193 EP 206 DI 10.1016/j.actaastro.2013.07.012 PG 14 WC Engineering, Aerospace SC Engineering GA 234TS UT WOS:000325667800022 ER PT J AU Stansbery, EK Draper, DS AF Stansbery, Eileen K. Draper, David S. TI Role of sample return and sample science in low cost missions SO ACTA ASTRONAUTICA LA English DT Article DE Sample return; Sample science; Curation; Low-cost missions; Planetary exploration ID OXYGEN ISOTOPIC COMPOSITION; GENESIS DISCOVERY MISSION; SOLAR-WIND; LUNAR DUST; ITOKAWA; HAYABUSA; WATER; ASTROMATERIALS; EXTRACTION; TOXICITY AB Sample return is an essential component of solar system exploration. Samples provide a unique data set that is critical for understanding formation and evolution of our solar system. This uniqueness is based on the scale of observations, precision of measurements, the ability to modify experiments as logic and technology dictate, and the ability to use instruments free of the constraints on mass, power, reliability, and data rate of flight instruments. Advances in analytical capabilities in recent years enable fundamental measurements to be made on extremely small samples, greatly reducing mass constraints on robotic sample return spacecraft. Sample studies provide irreplaceable ground truth for remotely-sensed data on planetary surfaces and fit within a variety of architectures for human exploration of the solar system. Published by Elsevier Ltd. on behalf of IAA. C1 [Stansbery, Eileen K.; Draper, David S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Stansbery, EK (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code KA,2101 NASA Pkwy, Houston, TX 77058 USA. EM eileen.k.stansbery@nasa.gov; david.s.draper@nasa.gov NR 42 TC 1 Z9 1 U1 1 U2 16 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JAN PY 2014 VL 93 BP 453 EP 459 DI 10.1016/j.actaastro.2013.03.018 PG 7 WC Engineering, Aerospace SC Engineering GA 234TS UT WOS:000325667800045 ER PT J AU Murchie, S Eng, D Chabot, N Guo, Y Arvidson, R Yen, A Trebi-Ollennu, A Seelos, F Adams, E Fountain, G AF Murchie, S. Eng, D. Chabot, N. Guo, Y. Arvidson, R. Yen, A. Trebi-Ollennu, A. Seelos, F. Adams, E. Fountain, G. TI MERLIN: Mars-Moon Exploration, Reconnaissance and Landed Investigation SO ACTA ASTRONAUTICA LA English DT Article DE Deimos; Mars; Phobos; Volatiles; Organics ID TAGISH LAKE METEORITE; MARTIAN SATELLITES; CARBONACEOUS CHONDRITE; SURFACE-COMPOSITION; TROJAN ASTEROIDS; PHOBOS; DEIMOS; FEATURES; IDENTIFICATION; SPECTROSCOPY AB Mars' moons Phobos and Deimos are low-albedo, D-type bodies that may preserve samples of outer solar system material that contributed organics and volatiles to the accreting terrestrial planets. A Discovery-class mission concept described in this paper, the Mars-Moon Exploration, Reconnaissance and Landed Investigation (MERLIN), will obtain in situ measurements from Deimos to test models for the moon's origin. The measurement objectives of MERLIN are to determine Deimos' elemental and mineralogical composition, to investigate its volatile and organic content, and to characterize processes that have modified its surface. To achieve these objectives, a landed payload will provide stereo imaging and measurements of elemental and mineralogical composition and interior structure. An orbital payload will acquire global high-resolution and color imaging, putting the landing site in context by characterizing Deimos' geology. Following MOI the spacecraft flies in formation with Deimos, and uses small changes in its orbit around Mars to investigate Deimos from a range of altitudes and illuminations over 4 months. Data taken during 1- to 2-km altitude flyovers will certify a landing site. The spacecraft will be delivered to a point several kilometers above Deimos, and will navigate to landing on a fresh exposure of regolith using onboard imaging. 90 days of baseline landed operations will provide a complete set of measurements, with schedule reserve, and there is sufficient propellant to repeat the measurements at a second site. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Murchie, S.; Eng, D.; Chabot, N.; Guo, Y.; Seelos, F.; Adams, E.; Fountain, G.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Arvidson, R.] Washington Univ, St Louis, MO USA. [Yen, A.; Trebi-Ollennu, A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Murchie, S (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. EM Scott.Murchie@jhuapl.edu RI Murchie, Scott/E-8030-2015; Chabot, Nancy/F-5384-2015; Seelos, Frank/C-7875-2016 OI Murchie, Scott/0000-0002-1616-8751; Chabot, Nancy/0000-0001-8628-3176; Seelos, Frank/0000-0001-9721-941X NR 43 TC 2 Z9 2 U1 2 U2 35 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JAN PY 2014 VL 93 BP 475 EP 482 DI 10.1016/j.actaastro.2012.10.014 PG 8 WC Engineering, Aerospace SC Engineering GA 234TS UT WOS:000325667800048 ER PT J AU Ehrenfreund, P Ricco, AJ Squires, D Kitts, C Agasid, E Bramall, N Bryson, K Chittenden, J Conley, C Cook, A Mancinelli, R Mattioda, A Nicholson, W Quinn, R Santos, O Tahu, G Voytek, M Beasley, C Bica, L Diaz-Aguado, M Friedericks, C Henschke, M Landis, D Luzzi, E Ly, D Mai, N Minelli, G McIntyre, M Neumann, M Parra, M Piccini, M Rasay, R Ricks, R Schooley, A Stackpole, E Timucin, L Yost, B Young, A AF Ehrenfreund, P. Ricco, A. J. Squires, D. Kitts, C. Agasid, E. Bramall, N. Bryson, K. Chittenden, J. Conley, C. Cook, A. Mancinelli, R. Mattioda, A. Nicholson, W. Quinn, R. Santos, O. Tahu, G. Voytek, M. Beasley, C. Bica, L. Diaz-Aguado, M. Friedericks, C. Henschke, M. Landis, D. Luzzi, E. Ly, D. Mai, N. Minelli, G. McIntyre, M. Neumann, M. Parra, M. Piccini, M. Rasay, R. Ricks, R. Schooley, A. Stackpole, E. Timucin, L. Yost, B. Young, A. TI The O/OREOS mission-Astrobiology in low Earth orbit SO ACTA ASTRONAUTICA LA English DT Article DE Astrobiology; Cubesats; Low cost mission; Spectroscopy; Space biology; O/OREOS; SEVO; SESLO AB The O/OREOS (Organism/Organic Exposure to Orbital Stresses) nanosatellite is the first science demonstration spacecraft and flight mission of the NASA Astrobiology Small Payloads Program (ASP). O/OREOS was launched successfully on November 19, 2010, to a high-inclination (72), 650-km Earth orbit aboard a US Air Force Minotaur IV rocket from Kodiak, Alaska. O/OREOS consists of 3 conjoined cubesat (each 1000 cm(3)) modules: (i) a control bus; (ii) the Space Environment Survivability of Living Organisms (SESLO) experiment; and (iii) the Space Environment Viability of Organics (SEVO) experiment. Among the innovative aspects of the O/OREOS mission are a real-time analysis of the photostability of organics and biomarkers and the collection of data on the survival and metabolic activity for microorganisms at 3 times during the 6-month mission. We report on the spacecraft characteristics, payload capabilities, and present operational phase and flight data from the O/OREOS mission. The science and technology rationale of O/OREOS supports NASA's scientific exploration program by investigating the local space environment as well as space biology relevant to Moon and Mars missions. It also serves as a precursor for experiments on small satellites, the International Space Station (ISS), future free-flyers and lunar surface exposure facilities. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Ehrenfreund, P.] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA. [Ricco, A. J.; Squires, D.; Agasid, E.; Bramall, N.; Chittenden, J.; Cook, A.; Mattioda, A.; Santos, O.; Beasley, C.; Diaz-Aguado, M.; Friedericks, C.; Henschke, M.; Luzzi, E.; Ly, D.; Mai, N.; Minelli, G.; McIntyre, M.; Parra, M.; Piccini, M.; Ricks, R.; Schooley, A.; Stackpole, E.; Timucin, L.; Yost, B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kitts, C.; Bica, L.; Neumann, M.; Rasay, R.; Young, A.] Santa Clara Univ, Robot Syst Lab, Santa Clara, CA 95053 USA. [Bryson, K.; Mancinelli, R.] Bay Area Environm Res Inst, Sonoma, CA USA. [Conley, C.; Tahu, G.; Voytek, M.] NASA Headquarters, Washington, DC USA. [Nicholson, W.] Univ Florida, Gainesville, FL USA. [Quinn, R.] SETI Inst, Mountain View, CA USA. [Landis, D.] Charles Stark Draper Lab Inc, Cambridge, MA 02139 USA. RP Ehrenfreund, P (reprint author), George Washington Univ, Inst Space Policy, Washington, DC 20052 USA. EM pehren@gwu.edu RI Bryson, Kathryn/I-6914-2012; OI Ricco, Antonio/0000-0002-2355-4984 NR 7 TC 8 Z9 8 U1 3 U2 32 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JAN PY 2014 VL 93 BP 501 EP 508 DI 10.1016/j.actaastro.2012.09.009 PG 8 WC Engineering, Aerospace SC Engineering GA 234TS UT WOS:000325667800052 ER PT J AU McNutt, RL Solomon, SC Bedini, PD Anderson, BJ Blewett, DT Evans, LG Gold, RE Krimigis, SM Murchie, SL Nittler, LR Phillips, RJ Prockter, LM Slavin, JA Zuber, MT Finnegan, EJ Grant, DG AF McNutt, Ralph L., Jr. Solomon, Sean C. Bedini, Peter D. Anderson, Brian J. Blewett, David T. Evans, Larry G. Gold, Robert E. Krimigis, Stamatios M. Murchie, Scott L. Nittler, Larry R. Phillips, Roger J. Prockter, Louise M. Slavin, James A. Zuber, Maria T. Finnegan, Eric J. Grant, David G. CA MESSENGER Team TI MESSENGER at Mercury: Early orbital operations SO ACTA ASTRONAUTICA LA English DT Article DE Mercury; MESSENGER; Planetary science; Orbital missions; NASA; Surface composition; Exosphere; Impact basins; Gravity field ID MAGNETIC-FIELD; 1ST FLYBY; GLOBAL PERSPECTIVE; IMPACT BASIN; MISSION; SPECTROMETER; EXOSPHERE; INSTRUMENT; SPACECRAFT; SURFACE AB The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft, launched in August 2004 under NASA's Discovery Program, was inserted into orbit about the planet Mercury in March 2011. MESSENGER's three flybys of Mercury in 2008-2009 marked the first spacecraft visits to the innermost planet since the Mariner 10 flybys in 1974-1975. The unprecedented orbital operations are yielding new insights into the nature and evolution of Mercury. The scientific questions that frame the MESSENGER mission led to the mission measurement objectives to be achieved by the seven payload instruments and the radio science experiment. Interweaving the full set of required orbital observations in a manner that maximizes the opportunity to satisfy all mission objectives and yet meet stringent spacecraft pointing and thermal constraints was a complex optimization problem that was solved with a software tool that simulates science observations and tracks progress toward meeting each objective. The final orbital observation plan, the outcome of that optimization process, meets all mission objectives. MESSENGER's Mercury Dual Imaging System is acquiring a global monochromatic image mosaic at better than 90% coverage and at least 250 m average resolution, a global color image mosaic at better than 90% coverage and at least I km average resolution, and global stereo imaging at better than 80% coverage and at least 250 m average resolution. Higher-resolution images are also being acquired of targeted areas. The elemental remote sensing instruments, including the Gamma-Ray and Neutron Spectrometer and the X-Ray Spectrometer, are being operated nearly continuously and will establish the average surface abundances of most major elements. The Visible and Infrared Spectrograph channel of MESSENGER's Mercury Atmospheric and Surface Composition Spectrometer is acquiring a global map of spectral reflectance from 300 to 1450 nm wavelength at a range of incidence and emission angles. Targeted areas have been selected for spectral coverage into the ultraviolet with the Ultraviolet and Visible Spectrometer (UVVS). MESSENGER's Mercury Laser Altimeter is acquiring topographic profiles when the slant range to Mercury's surface is less than 1800 km, encompassing latitudes from 20 S to the north pole. Topography over the remainder of the southern hemisphere will be derived from stereo imaging, radio occultations, and limb profiles. MESSENGER's radio science experiment is determining Mercury's gravity field from Doppler signals acquired during frequent downlinks. MESSENGER's Magnetometer is measuring the vector magnetic field both within Mercury's magnetosphere and in Mercury's solar wind environment at an instrument sampling rate of up to 20 samples/s. The UVVS is determining the three-dimensional, time-dependent distribution of Mercury's exospheric neutral and ionic species via their emission lines. During each spacecraft orbit, the Energetic Particle Spectrometer measures energetic electrons and ions, and the Fast Imaging Plasma Spectrometer measures the energies and mass per charge of thermal plasma components, both within Mercury's magnetosphere and in Mercury's solar-wind environment. The primary mission observation sequence will continue for one Earth year, until March 2012. An extended mission, currently under discussion with NASA, would add a second year of orbital observations targeting a set of focused follow-on questions that build on observations to date and take advantage of the more active Sun expected during 2012-2013. MESSENGER's total primary mission cost, projected at $446 M in real-year dollars, is comparable to that of Mariner 10 after adjustment for inflation. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved. C1 [McNutt, Ralph L., Jr.; Bedini, Peter D.; Anderson, Brian J.; Blewett, David T.; Gold, Robert E.; Krimigis, Stamatios M.; Murchie, Scott L.; Prockter, Louise M.; Finnegan, Eric J.; Grant, David G.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Solomon, Sean C.; Nittler, Larry R.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Evans, Larry G.] Comp Sci Corp, Lanham, MD 20706 USA. [Krimigis, Stamatios M.] Acad Athens, Athens 11527, Greece. [Phillips, Roger J.] SW Res Inst, Boulder, CO 80302 USA. [Slavin, James A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02129 USA. RP McNutt, RL (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM ralph.mcnutt@jhuapl.edu RI Slavin, James/H-3170-2012; McNutt, Ralph/E-8006-2010; Blewett, David/I-4904-2012; Murchie, Scott/E-8030-2015 OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166; Blewett, David/0000-0002-9241-6358; Murchie, Scott/0000-0002-1616-8751 FU NASA Discovery Program [NAS5-97271]; MESSENGER mission to Mercury FX The NASA Discovery Program under contract NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington supports the MESSENGER mission to Mercury. NR 47 TC 0 Z9 1 U1 0 U2 34 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JAN PY 2014 VL 93 BP 509 EP 515 DI 10.1016/j.actaastro.2012.08.012 PG 7 WC Engineering, Aerospace SC Engineering GA 234TS UT WOS:000325667800053 ER PT J AU Anderson, DJ Pencil, E Vento, D Peterson, T Dankanich, J Hahne, D Munk, MM AF Anderson, David J. Pencil, Eric Vento, Daniel Peterson, Todd Dankanich, John Hahne, David Munk, Michelle M. TI Products from NASA's in-space propulsion technology program applicable to low-cost planetary missions SO ACTA ASTRONAUTICA LA English DT Article DE Electric propulsion; Chemical propulsion; Aerocapture; Entry vehicles; Trajectory tools AB Since September 2001, NASA's In-Space Propulsion Technology (ISPT) program has been developing technologies for lowering the cost of planetary science missions. Recently completed is the high-temperature Advanced Material Bipropellant Rocket (AMBR) engine providing higher performance for lower cost. Two other cost saving technologies nearing completion are the NEXT ion thruster and the Aerocapture technology project. Under development are several technologies for low-cost sample return missions. These include a low-cost Hall-effect thruster (HIVHAC) which will be completed in 2011, light-weight propellant tanks, and a Multi-Mission Earth Entry Vehicle (MMEEV). This paper will discuss the status of the technology development, the cost savings or performance benefits, and applicability of these in-space propulsion technologies to NASA's future Discovery, and New Frontiers missions, as well as their relevance for sample return missions. Published by Elsevier Ltd. on behalf of IAA. C1 [Anderson, David J.; Pencil, Eric; Vento, Daniel; Peterson, Todd] NASA, Glenn Res Ctr, S Cleveland, OH 44135 USA. [Dankanich, John] Gray Res Inc, Cleveland, OH 44135 USA. [Hahne, David; Munk, Michelle M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Anderson, DJ (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM David.J.Anderson@nasa.gov; Eric.J.Pencil@nasa.gov; Daniel.M.Vento@nasa.gov; Todd.T.Peterson@nasa.gov; John.Dankanich@nasa.gov; David.E.Hahne@nasa.gov; Michelle.M.Munk@nasa.gov FU NASA's Science Mission Directorate (SMD) FX The results and findings presented here are based on work funded by NASA's Science Mission Directorate (SMD). The ISPT program is managed out of the Glenn Research Center for SMD's Planetary Sciences Division (PSD). NR 9 TC 0 Z9 0 U1 2 U2 39 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JAN PY 2014 VL 93 BP 516 EP 523 DI 10.1016/j.actaastro.2012.07.006 PG 8 WC Engineering, Aerospace SC Engineering GA 234TS UT WOS:000325667800054 ER PT J AU Youngquist, RC Ihlefeld, CM Starr, SO AF Youngquist, Robert C. Ihlefeld, Curtis M. Starr, Stanley O. TI A DC Transformer SO IEEE TRANSACTIONS ON POWER ELECTRONICS LA English DT Article DE DC power; DC transformer; homopolar generator; homopolar machine; homopolar motor ID FLYWHEEL ENERGY; SYSTEMS AB A component level dc transformer is described in which no alternating currents or voltages are present. It operates by combining features of a homopolar motor and a homopolar generator, both dc devices, such that the output voltage of a dc power supply can be stepped up (or down) with a corresponding step down (or up) in the current. The basic theory for this device is developed, performance predictions are made, and the results from a small prototype are presented. Based on demonstrated technology in the literature, this dc transformer should be scalable to low megawatt levels, but it is more suited to high current than high voltage applications. Significant development would be required before it could achieve the kilovolt levels needed for dc power transmission. C1 [Youngquist, Robert C.; Ihlefeld, Curtis M.; Starr, Stanley O.] NASA, Kennedy Space Ctr, FL 32899 USA. RP Youngquist, RC (reprint author), NASA, Kennedy Space Ctr, FL 32899 USA. EM Robert.C.Youngquist@nasa.gov; Curtis.M.Ihlefeld@nasa.gov; Stanley.O.Starr@nasa.gov FU National Aeronautics and Space Administration office of the Chief Technologist FX Manuscript received March 1, 2013; revised May 15, 2013; accepted May 24, 2013. Date of current version July 18, 2013. This work was supported by the National Aeronautics and Space Administration office of the Chief Technologist. Recommended for publication by Associate Editor R. Ayyanar NR 11 TC 2 Z9 2 U1 0 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0885-8993 J9 IEEE T POWER ELECTR JI IEEE Trans. Power Electron. PD JAN PY 2014 VL 29 IS 1 BP 42 EP 44 DI 10.1109/TPEL.2013.2266198 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 212YY UT WOS:000324020500008 ER PT J AU Leckey, CAC Rogge, MD Parker, FR AF Leckey, Cara A. C. Rogge, Matthew D. Parker, F. Raymond TI Guided waves in anisotropic and quasi-isotropic aerospace composites: Three-dimensional simulation and experiment SO ULTRASONICS LA English DT Article DE Guided wave; Finite integration; Simulation; Composite; Delamination ID FINITE INTEGRATION TECHNIQUE; FIBER-REINFORCED POLYMER; IMPACT DAMAGE; PROPAGATION; PREDICTION; SCATTERING; GEOMETRIES AB Three-dimensional (3D) elastic wave simulations can be used to investigate and optimize nondestructive evaluation (NDE) and structural health monitoring (SHM) ultrasonic damage detection techniques for aerospace materials. 3D anisotropic elastodynamic finite integration technique (EFIT) has been implemented for ultrasonic waves in carbon fiber reinforced polymer (CFRP) composite laminates. This paper describes 3D EFIT simulations of guided wave propagation in undamaged and damaged anisotropic and quasi-isotropic composite plates. Comparisons are made between simulations of guided waves in undamaged anisotropic composite plates and both experimental laser Doppler vibrometer (LDV) wavefield data and dispersion curves. Time domain and wavenumber domain comparisons are described. Wave interaction with complex geometry delamination damage is then simulated to investigate how simulation tools incorporating realistic damage geometries can aid in the understanding of wave interaction with CFRP damage. In order to move beyond simplistic assumptions of damage geometry, volumetric delamination data acquired via X-ray microfocus computed tomography is directly incorporated into the simulation. Simulated guided wave interaction with the complex geometry delamination is compared to experimental LDV time domain data and 3D wave interaction with the volumetric damage is discussed. Published by Elsevier B.V. C1 [Leckey, Cara A. C.; Rogge, Matthew D.; Parker, F. Raymond] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Leckey, CAC (reprint author), NASA, Langley Res Ctr, MS 231, Hampton, VA 23681 USA. EM cara.ac.leckey@nasa.gov NR 35 TC 19 Z9 19 U1 2 U2 112 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0041-624X J9 ULTRASONICS JI Ultrasonics PD JAN PY 2014 VL 54 IS 1 BP 385 EP 394 DI 10.1016/j.ultras.2013.05.007 PG 10 WC Acoustics; Radiology, Nuclear Medicine & Medical Imaging SC Acoustics; Radiology, Nuclear Medicine & Medical Imaging GA 215XJ UT WOS:000324244100045 PM 23769180 ER PT J AU Monahan, WB Cook, T Melton, F Connor, J Bobowski, B AF Monahan, William B. Cook, Tammy Melton, Forrest Connor, Jeff Bobowski, Ben TI Forecasting Distributional Responses of Limber Pine to Climate Change at Management-Relevant Scales in Rocky Mountain National Park SO PLOS ONE LA English DT Article ID COLORADO FRONT RANGE; SPECIES DISTRIBUTIONS; UNITED-STATES; FLEXILIS; FOREST; ALPINE; USA; CONSERVATION; MECHANISMS; SUCCESSION AB Resource managers at parks and other protected areas are increasingly expected to factor climate change explicitly into their decision making frameworks. However, most protected areas are small relative to the geographic ranges of species being managed, so forecasts need to consider local adaptation and community dynamics that are correlated with climate and affect distributions inside protected area boundaries. Additionally, niche theory suggests that species' physiological capacities to respond to climate change may be underestimated when forecasts fail to consider the full breadth of climates occupied by the species rangewide. Here, using correlative species distribution models that contrast estimates of climatic sensitivity inferred from the two spatial extents, we quantify the response of limber pine (Pinus flexilis) to climate change in Rocky Mountain National Park (Colorado, USA). Models are trained locally within the park where limber pine is the community dominant tree species, a distinct structural-compositional vegetation class of interest to managers, and also rangewide, as suggested by niche theory. Model forecasts through 2100 under two representative concentration pathways (RCP 4.5 and 8.5 W/m(2)) show that the distribution of limber pine in the park is expected to move upslope in elevation, but changes in total and core patch area remain highly uncertain. Most of this uncertainty is biological, as magnitudes of projected change are considerably more variable between the two spatial extents used in model training than they are between RCPs, and novel future climates only affect local model predictions associated with RCP 8.5 after 2091. Combined, these results illustrate the importance of accounting for unknowns in species' climatic sensitivities when forecasting distributional scenarios that are used to inform management decisions. We discuss how our results for limber pine may be interpreted in the context of climate change vulnerability and used to help guide adaptive management. C1 [Monahan, William B.] Natl Pk Serv, Inventory & Monitoring Div, Ft Collins, CO 80525 USA. [Cook, Tammy] Natl Pk Serv, Biol Resource Management Div, Ft Collins, CO USA. [Melton, Forrest] Calif State Univ Monterey Bay, Seaside, CA USA. [Melton, Forrest] NASA, Ames Res Ctr, Cooperat Res Earth Sci & Technol, Moffett Field, CA 94035 USA. [Connor, Jeff; Bobowski, Ben] Rocky Mt Natl Pk, Estes Pk, CO USA. RP Monahan, WB (reprint author), Natl Pk Serv, Inventory & Monitoring Div, Ft Collins, CO 80525 USA. EM Bill_Monahan@nps.gov OI Cook, Timothee/0000-0003-2354-824X FU National Park Service; NASA Applied Sciences program [10-BIOCLIM10-0034] FX Support for this study was provided by the National Park Service, and by the NASA Applied Sciences program through award number 10-BIOCLIM10-0034. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 70 TC 8 Z9 8 U1 2 U2 35 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD DEC 31 PY 2013 VL 8 IS 12 AR e83163 DI 10.1371/journal.pone.0083163 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 284NF UT WOS:000329325200039 PM 24391742 ER PT J AU Siddon, EC Kristiansen, T Mueter, FJ Holsman, KK Heintz, RA Farley, EV AF Siddon, Elizabeth Calvert Kristiansen, Trond Mueter, Franz J. Holsman, Kirstin K. Heintz, Ron A. Farley, Edward V. TI Spatial Match-Mismatch between Juvenile Fish and Prey Provides a Mechanism for Recruitment Variability across Contrasting Climate Conditions in the Eastern Bering Sea SO PLOS ONE LA English DT Article ID POLLOCK THERAGRA-CHALCOGRAMMA; OSCILLATING CONTROL HYPOTHESIS; AGE-0 WALLEYE POLLOCK; COD GADUS-MORHUA; BIOENERGETICS MODEL; MALLOTUS-VILLOSUS; HABITAT SELECTION; BODY-SIZE; LARVAL; ECOSYSTEM AB Understanding mechanisms behind variability in early life survival of marine fishes through modeling efforts can improve predictive capabilities for recruitment success under changing climate conditions. Walleye pollock (Theragra chalcogramma) support the largest single-species commercial fishery in the United States and represent an ecologically important component of the Bering Sea ecosystem. Variability in walleye pollock growth and survival is structured in part by climate-driven bottom-up control of zooplankton composition. We used two modeling approaches, informed by observations, to understand the roles of prey quality, prey composition, and water temperature on juvenile walleye pollock growth: (1) a bioenergetics model that included local predator and prey energy densities, and (2) an individual-based model that included a mechanistic feeding component dependent on larval development and behavior, local prey densities and size, and physical oceanographic conditions. Prey composition in late-summer shifted from predominantly smaller copepod species in the warmer 2005 season to larger species in the cooler 2010 season, reflecting differences in zooplankton composition between years. In 2010, the main prey of juvenile walleye pollock were more abundant, had greater biomass, and higher mean energy density, resulting in better growth conditions. Moreover, spatial patterns in prey composition and water temperature lead to areas of enhanced growth, or growth 'hot spots', for juvenile walleye pollock and survival may be enhanced when fish overlap with these areas. This study provides evidence that a spatial mismatch between juvenile walleye pollock and growth 'hot spots' in 2005 contributed to poor recruitment while a higher degree of overlap in 2010 resulted in improved recruitment. Our results indicate that climate-driven changes in prey quality and composition can impact growth of juvenile walleye pollock, potentially severely affecting recruitment variability. C1 [Siddon, Elizabeth Calvert; Mueter, Franz J.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK USA. [Kristiansen, Trond] Inst Marine Res, N-5024 Bergen, Norway. [Holsman, Kirstin K.] Univ Washington, Joint Inst Study Atmosphere & Ocean, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv,Natl Ocean & Atmospher, Seattle, WA 98195 USA. [Heintz, Ron A.; Farley, Edward V.] Natl Ocean & Atmospher Adm, Ted Stevens Marine Res Inst, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK USA. RP Siddon, EC (reprint author), Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK USA. EM ecsiddon@alaska.edu FU North Pacific Anadromous Fish Commission; North Pacific Research Board; Norwegian Research Council FX This work was supported by the North Pacific Anadromous Fish Commission; North Pacific Research Board; and Norwegian Research Council. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 37 TC 16 Z9 16 U1 11 U2 68 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD DEC 31 PY 2013 VL 8 IS 12 AR e84526 DI 10.1371/journal.pone.0084526 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 284MV UT WOS:000329323900106 PM 24391963 ER PT J AU Wu, PF Tang, SN Raible, DE AF Wu, Pengfei Tang, Suning Raible, Daniel E. TI A prototype high-speed optically-steered X-band phased array antenna SO OPTICS EXPRESS LA English DT Article ID TRUE-TIME-DELAY; STIMULATED BRILLOUIN-SCATTERING; FIBER GRATING PRISM; SLOW LIGHT; BEAMFORMER; LINE AB We develop a prototype of optically-steered X-band phased array antenna with capabilities of multi-band and multi-beam operations. It exploits high-speed wavelength tunable lasers for optical true-time delays over a dispersive optical fiber link, enabling agile, broadband and vibration-free RF beam steering with large angle. (C) 2013 Optical Society of America C1 [Wu, Pengfei; Tang, Suning] Crystal Res Inc, Fremont, CA 95469 USA. [Raible, Daniel E.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Wu, PF (reprint author), Crystal Res Inc, 48501 Warm Springs Blvd 103, Fremont, CA 95469 USA. EM pengfeiwu@eocrystal.com FU NASA SBIR research program [NNX11CA52C] FX This research work was partially supported by NASA SBIR research program (contract number: NNX11CA52C). NR 26 TC 8 Z9 9 U1 2 U2 23 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD DEC 30 PY 2013 VL 21 IS 26 BP 32599 EP 32604 DI 10.1364/OE.21.032599 PG 6 WC Optics SC Optics GA 282WP UT WOS:000329205200085 PM 24514853 ER PT J AU Werdell, PJ Franz, BA Lefler, JT Robinson, WD Boss, E AF Werdell, P. Jeremy Franz, Bryan A. Lefler, Jason T. Robinson, Wayne D. Boss, Emmanuel TI Retrieving marine inherent optical properties from satellites using temperature and salinity-dependent backscattering by seawater SO OPTICS EXPRESS LA English DT Article ID CLEAREST NATURAL-WATERS; IMPROVED IN-SITU; OCEAN-COLOR; PURE WATER; ABSORPTION; REFLECTANCE; ALGORITHM; SEAWIFS; NM; VALIDATION AB Time-series of marine inherent optical properties (IOPs) from ocean color satellite instruments provide valuable data records for studying long-term time changes in ocean ecosystems. Semi-analytical algorithms (SAAs) provide a common method for estimating IOPs from radiometric measurements of the marine light field. Most SAAs assign constant spectral values for seawater absorption and backscattering, assume spectral shape functions of the remaining constituent absorption and scattering components (e. g., phytoplankton, non-algal particles, and colored dissolved organic matter), and retrieve the magnitudes of each remaining constituent required to match the spectral distribution of measured radiances. Here, we explore the use of temperature-and salinity-dependent values for seawater backscattering in lieu of the constant spectrum currently employed by most SAAs. Our results suggest that use of temperature-and salinity-dependent seawater spectra elevate the SAA-derived particle backscattering, reduce the non-algal particles plus colored dissolved organic matter absorption, and leave the derived absorption by phytoplankton unchanged. (C) 2013 Optical Society of America C1 [Werdell, P. Jeremy; Franz, Bryan A.; Lefler, Jason T.; Robinson, Wayne D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Werdell, P. Jeremy; Boss, Emmanuel] Univ Maine, Sch Marine Sci, Orono, ME 04401 USA. [Lefler, Jason T.] JHT Inc, Orlando, FL 32826 USA. [Robinson, Wayne D.] Sci Applicat Int Corp, Mclean, VA 22102 USA. RP Werdell, PJ (reprint author), NASA, Goddard Space Flight Ctr, Code 616, Greenbelt, MD 20771 USA. EM jeremy.werdell@nasa.gov RI Boss, Emmanuel/C-5765-2009; Franz, Bryan/D-6284-2012 OI Boss, Emmanuel/0000-0002-8334-9595; Franz, Bryan/0000-0003-0293-2082 FU NASA Ocean Biology and Biogeochemistry Program FX We thank S.W. Bailey, C.S. Roesler, M.J. Perry, J. Goes, A. Thomas, H. Xue, Z. Ahmad, and other members of the NASA Ocean Biology Processing Group for their valuable comments. The NASA Ocean Biology and Biogeochemistry Program provided funding for this activity. NR 31 TC 7 Z9 7 U1 1 U2 11 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD DEC 30 PY 2013 VL 21 IS 26 BP 32611 EP 32622 DI 10.1364/OE.21.032611 PG 12 WC Optics SC Optics GA 282WP UT WOS:000329205200087 PM 24514855 ER PT J AU Jain, A Kandel, S Wagner, J Larsen, A Vaidehi, N AF Jain, Abhinandan Kandel, Saugat Wagner, Jeffrey Larsen, Adrien Vaidehi, Nagarajan TI Fixman compensating potential for general branched molecules SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CLASSICAL STATISTICAL-MECHANICS; LINKED RIGID BODIES; DYNAMICS SIMULATIONS; POLYMER-CHAIN; FREE-ENERGY; CONSTRAINED DYNAMICS; BROWNIAN DYNAMICS; ALGORITHM; MACROMOLECULES; CONFORMATIONS AB The technique of constraining high frequency modes of molecular motion is an effective way to increase simulation time scale and improve conformational sampling in molecular dynamics simulations. However, it has been shown that constraints on higher frequency modes such as bond lengths and bond angles stiffen the molecular model, thereby introducing systematic biases in the statistical behavior of the simulations. Fixman proposed a compensating potential to remove such biases in the thermodynamic and kinetic properties calculated from dynamics simulations. Previous implementations of the Fixman potential have been limited to only short serial chain systems. In this paper, we present a spatial operator algebra based algorithm to calculate the Fixman potential and its gradient within constrained dynamics simulations for branched topology molecules of any size. Our numerical studies on molecules of increasing complexity validate our algorithm by demonstrating recovery of the dihedral angle probability distribution function for systems that range in complexity from serial chains to protein molecules. We observe that the Fixman compensating potential recovers the free energy surface of a serial chain polymer, thus annulling the biases caused by constraining the bond lengths and bond angles. The inclusion of Fixman potential entails only a modest increase in the computational cost in these simulations. We believe that this work represents the first instance where the Fixman potential has been used for general branched systems, and establishes the viability for its use in constrained dynamics simulations of proteins and other macromolecules. (C) 2013 AIP Publishing LLC. C1 [Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kandel, Saugat; Wagner, Jeffrey; Larsen, Adrien; Vaidehi, Nagarajan] City Hope Natl Med Ctr, Beckman Res Inst, Div Immunol, Duarte, CA 91010 USA. RP Jain, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Abhi.Jain@jpl.nasa.gov; nvaidehi@coh.org FU NIH Grant [RO1GM082896]; National Aeronautics and Space Administration FX This work was supported by funding from NIH Grant No. RO1GM082896. Part of the research described in this paper was performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 43 TC 4 Z9 4 U1 2 U2 14 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 28 PY 2013 VL 139 IS 24 AR 244103 DI 10.1063/1.4851315 PG 11 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 282RZ UT WOS:000329191800004 PM 24387353 ER PT J AU Santee, ML Livesey, NJ Manney, GL Lambert, A Read, WG AF Santee, M. L. Livesey, N. J. Manney, G. L. Lambert, A. Read, W. G. TI Methyl chloride from the Aura Microwave Limb Sounder: First global climatology and assessment of variability in the upper troposphere and stratosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Review ID QUASI-BIENNIAL OSCILLATION; BIOMASS BURNING EMISSIONS; PEM-WEST-B; TROPICAL TROPOPAUSE; REACTIVE CHLORINE; TRACE GASES; ATMOSPHERIC CHEMISTRY; PACIFIC-OCEAN; POLAR VORTEX; FIRN AIR C1 [Santee, M. L.; Livesey, N. J.; Lambert, A.; Read, W. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Manney, G. L.] NorthWest Res Associates, Socorro, NM USA. [Manney, G. L.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. RP Santee, ML (reprint author), CALTECH, Jet Prop Lab, Mail Stop 233-200,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Michelle.L.Santee@jpl.nasa.gov FU National Aeronautics and Space Administration FX We thank Ryan Fuller, William Daffer, Bob Thurstans, Brian Knosp, and Brian Mills for programming, system administration, and data management support. We gratefully acknowledge provision of MkIV data by Geoffrey Toon and the MkIV Team, ACE-FTS data by Kaley Walker and the ACE-FTS Team, and Singapore winds by the Institute of Meteorology of the Freie Universitat Berlin. Comments from three anonymous reviewers substantially improved the manuscript. Work at the Jet Propulsion Laboratory, California Institute of Technology, was done under contract with the National Aeronautics and Space Administration. NR 173 TC 8 Z9 8 U1 0 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 27 PY 2013 VL 118 IS 24 BP 13532 EP 13560 DI 10.1002/2013JD020235 PG 29 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 293KX UT WOS:000329971100012 ER PT J AU Hurwitz, MM Garfinkel, CI Newman, PA Oman, LD AF Hurwitz, Margaret M. Garfinkel, Chaim I. Newman, Paul A. Oman, Luke D. TI Sensitivity of the atmospheric response to warm pool El Nino events to modeled SSTs and future climate forcings SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SEA-SURFACE TEMPERATURE; SOUTHERN OSCILLATION; CHANGE PROJECTIONS; STRATOSPHERE; HEMISPHERE; ANOMALIES; LAYER C1 [Hurwitz, Margaret M.] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 20771 USA. [Hurwitz, Margaret M.; Newman, Paul A.; Oman, Luke D.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Garfinkel, Chaim I.] Johns Hopkins Univ, Baltimore, MD USA. RP Hurwitz, MM (reprint author), Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 20771 USA. EM margaret.m.hurwitz@nasa.gov RI Newman, Paul/D-6208-2012; Oman, Luke/C-2778-2009; garfinkel, chaim/H-6215-2012 OI Newman, Paul/0000-0003-1139-2508; Oman, Luke/0000-0002-5487-2598; garfinkel, chaim/0000-0001-7258-666X FU NASA's MAP; ACMAP FX The authors thank NASA's MAP and ACMAP programs for funding, and three anonymous reviewers for their helpful feedback. NR 42 TC 4 Z9 4 U1 0 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 27 PY 2013 VL 118 IS 24 BP 13371 EP 13382 DI 10.1002/2013JD021051 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 293KX UT WOS:000329971100001 ER PT J AU Nalli, NR Barnet, CD Reale, A Tobin, D Gambacorta, A Maddy, ES Joseph, E Sun, BM Borg, L Mollner, AK Morris, VR Liu, X Divakarla, M Minnett, PJ Knuteson, RO King, TS Wolf, WW AF Nalli, Nicholas R. Barnet, Christopher D. Reale, Anthony Tobin, David Gambacorta, Antonia Maddy, Eric S. Joseph, Everette Sun, Bomin Borg, Lori Mollner, Andrew K. Morris, Vernon R. Liu, Xu Divakarla, Murty Minnett, Peter J. Knuteson, Robert O. King, Thomas S. Wolf, Walter W. TI Validation of satellite sounder environmental data records: Application to the Cross-track Infrared Microwave Sounder Suite SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID NUMERICAL WEATHER PREDICTION; RADIATIVE-TRANSFER MODEL; WATER-VAPOR MEASUREMENTS; SEA-SURFACE TEMPERATURE; RADIOSONDE MEASUREMENTS; VERTICAL RESOLUTION; DATA PRODUCTS; RAMAN LIDAR; AWEX-G; OCEAN C1 [Nalli, Nicholas R.; Gambacorta, Antonia; Sun, Bomin; Divakarla, Murty; King, Thomas S.] IMSG Inc, Rockville, MD USA. [Nalli, Nicholas R.; Gambacorta, Antonia; Maddy, Eric S.; Divakarla, Murty; King, Thomas S.; Wolf, Walter W.] NOAA, NESDIS, STAR, College Pk, MD 20740 USA. [Barnet, Christopher D.; Maddy, Eric S.] STC, Columbia, MD USA. [Reale, Anthony; Sun, Bomin] NOAA, NESDIS, STAR, Suitland, MD USA. [Tobin, David; Borg, Lori; Knuteson, Robert O.] Univ Wisconsin, Madison, WI USA. [Joseph, Everette; Morris, Vernon R.] Howard Univ, Washington, DC 20059 USA. [Mollner, Andrew K.] Aerosp Corp, El Segundo, CA 90245 USA. [Liu, Xu] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Minnett, Peter J.] Univ Miami, RSMAS, Miami, FL USA. RP Nalli, NR (reprint author), NOAA, Ctr Weather & Climate Predict, IMSG Inc, 5830 Univ Res Court, College Pk, MD 20740 USA. EM Nick.Nalli@noaa.gov RI Nalli, Nicholas/F-6731-2010; Divakarla, Murty/E-7936-2011; Maddy, Eric/G-3683-2010; Reale, Tony/F-5621-2010; Wolf, Walter/E-7935-2011; Gambacorta, Antonia/E-7937-2011; Sun, Bomin/P-8742-2014; Richards, Amber/K-8203-2015 OI Nalli, Nicholas/0000-0002-6914-5537; Divakarla, Murty/0000-0002-0399-3381; Maddy, Eric/0000-0003-1151-339X; Reale, Tony/0000-0003-2150-5246; Wolf, Walter/0000-0002-2102-8833; Gambacorta, Antonia/0000-0002-2446-9132; Sun, Bomin/0000-0002-4872-9349; FU NOAA Joint Polar Satellite System Office; Integrated Program Office (IPO); STAR Satellite Meteorology and Climatology Division; NOAA [NA17AE1625, NA17AE1623]; JPSS; NOAA/NESDIS/STAR; NASA [NNG11VH00B] FX This research was supported by the NOAA Joint Polar Satellite System Office (M. D. Goldberg) and the former Integrated Program Office (IPO), along with the STAR Satellite Meteorology and Climatology Division (F. Weng and I. Csiszar). AEROSE works in collaboration with the NOAA PIRATA Northeast Extension (PNE) project and is supported by the NOAA Educational Partnership Program grant NA17AE1625, NOAA grant NA17AE1623, JPSS and NOAA/NESDIS/STAR. We are grateful to several contributors to the S-NPP CrIMSS EDR validation effort, especially L. Zhou, M. Wilson, F. Iturbide-Sanchez, C. Tan, X. Xiong, H. Xie, J. Wei, F. Tilley, C. Brown, M. Petty (NOAA/NESDIS/STAR), and M. Feltz (UW/CIMSS). We also acknowledge the following collaborators for their contributions to the S-NPP validation data collection effort: B. Demoz and M. Oyola (Howard University, BCCSO and AEROSE); D. Wolfe (NOAA Earth System Research Laboratory, AEROSE); J. E. Wessel (Aerospace PMRF). We thank D. Holdridge and J. Mather and the U.S. DOE ARM Climate Research Facility for its support of the satellite overpass radiosonde efforts. Data collection by The Aerospace Corporation was supported by NASA contract NNG11VH00B. We also thank two anonymous reviewers who provided many expert suggestions that we used to improve the overall quality of the paper. The views, opinions, and findings contained in this paper are those of the authors and should not be construed as an official NOAA or U.S. Government position, policy, or decision. NR 73 TC 12 Z9 12 U1 1 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 27 PY 2013 VL 118 IS 24 BP 13628 EP 13643 DI 10.1002/2013JD020436 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 293KX UT WOS:000329971100018 ER PT J AU Ahlborg, NL Zhu, DM AF Ahlborg, Nadia L. Zhu, Dongming TI Calcium-magnesium aluminosilicate (CMAS) reactions and degradation mechanisms of advanced environmental barrier coatings SO SURFACE & COATINGS TECHNOLOGY LA English DT Article; Proceedings Paper CT 40th International Conference on Metallurgical Coatings and Thin Films (ICMCTF) CY APR 29-MAY 03, 2013 CL San Diego, CA SP Amer Vacuum Soc, Adv Surface Engn Div DE Environmental barrier coatings; Calcium-magnesium aluminosilicate; Ytterbium silicate; Yttrium silicate; Hafnia; Zirconia ID DEPOSITS AB The thermochemical reactions between calcium-magnesium-aluminosilicate (CMAS) based road sand and several advanced turbine engine environmental barrier coating (EEC) materials were studied. The phase stability, reaction kinetics and degradation mechanisms of rare earth (RE)-silicates Yb2SiO5 and Y2Si2O7 and RE-oxide doped HfO2 and ZrO2 under the CMAS infiltration condition at 1500 degrees C were investigated, and the microstructure and phase characteristics of CMAS-EBC specimens were examined using Scanning Electron Microscopy (SEM) and X-ray Diffraction (XRD). Experimental results showed that the CMAS dissolved RE-silicates to form crystalline, highly non-stoichiometric apatite phases, and in particular attacking the silicate grain boundaries. Cross-section images show that the CMAS reacted with specimens and deeply penetrated into the EBC grain boundaries and formed extensive low-melting eutectic phases, causing grain boundary recession with increasing testing time in the silicate materials. The preliminary results also showed that CMAS reactions also formed low melting grain boundary phases in the higher concentration RE-oxide doped HfO2 systems. The effect of the test temperature on CMAS reactions of the EBC materials will also be discussed. The faster diffusion exhibited by apatite and RE-doped oxide phases and the formation of extensive grain boundary low-melting phases may limit the CMAS resistance of some of the environmental barrier coatings at high temperatures. Published by Elsevier B.V. C1 [Ahlborg, Nadia L.] Ohio State Univ, NASA, Glenn Res Ctr, Columbus, OH 43210 USA. [Zhu, Dongming] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Zhu, DM (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Dongming.Zhu@nasa.gov NR 15 TC 9 Z9 10 U1 9 U2 51 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0257-8972 J9 SURF COAT TECH JI Surf. Coat. Technol. PD DEC 25 PY 2013 VL 237 BP 79 EP 87 DI 10.1016/j.surfcoat.2013.08.036 PG 9 WC Materials Science, Coatings & Films; Physics, Applied SC Materials Science; Physics GA 300TX UT WOS:000330488000012 ER PT J AU Stedman, K AF Stedman, Ken TI The forgotten extraterrestrials SO NEW SCIENTIST LA English DT Editorial Material C1 [Stedman, Ken] Portland State Univ, Ctr Life Extreme Environm, Portland, OR 97207 USA. [Stedman, Ken] NASA, Virus Focus Grp, Washington, DC USA. RP Stedman, K (reprint author), Portland State Univ, Ctr Life Extreme Environm, Portland, OR 97207 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU REED BUSINESS INFORMATION LTD PI SUTTON PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND SN 0262-4079 J9 NEW SCI JI New Sci. PD DEC 21 PY 2013 VL 220 IS 2948 BP 42 EP 43 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 278WC UT WOS:000328919600029 ER PT J AU Schnittman, JD AF Schnittman, Jeremy D. TI Astrophysics of super-massive black hole mergers SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article ID ACTIVE GALACTIC NUCLEI; PULSAR TIMING ARRAYS; LONG-TERM EVOLUTION; COALESCING BINARY-SYSTEMS; DOUBLE-PEAKED EMITTER; MONTE-CARLO CODE; GAS PILE-UP; GRAVITATIONAL-WAVE; SUPERMASSIVE BINARY; ACCRETION DISKS AB We present here an overview of recent work in the subject of astrophysical manifestations of super-massive black hole (SMBH) mergers. This is a field that has been traditionally driven by theoretical work, but in recent years has also generated a great deal of interest and excitement in the observational astronomy community. In particular, the electromagnetic (EM) counterparts to SMBH mergers provide the means to detect and characterize these highly energetic events at cosmological distances, even in the absence of a space-based gravitational-wave observatory. In addition to providing a mechanism for observing SMBH mergers, EM counterparts also give important information about the environments in which these remarkable events take place, thus teaching us about the mechanisms through which galaxies form and evolve symbiotically with their central black holes. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Schnittman, JD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM jeremy.schnittman@nasa.gov NR 248 TC 14 Z9 14 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD DEC 21 PY 2013 VL 30 IS 24 AR 244007 DI 10.1088/0264-9381/30/24/244007 PG 21 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 259RG UT WOS:000327543400008 ER PT J AU Preston, A Merkowitz, S AF Preston, Alix Merkowitz, Stephen TI Next-generation hollow retroreflectors for lunar laser ranging SO APPLIED OPTICS LA English DT Article ID SPACE AB The three retroreflector arrays put on the Moon 40 years ago by the Apollo astronauts and the French-built arrays on the Soviet Lunokhod rovers continue to be useful targets, and have provided the most stringent tests of the Strong Equivalence Principle and the time variation of Newton's gravitational constant, as well as valuable insight into the Moon's interior. However, the precision of the ranging measurements are now being limited by the physical size of the arrays and a new generation of retroreflectors is required to make significant advances over current capabilities. Large single-cube retroreflectors represent the most promising approach to overcoming current limitations, and hollow retroreflectors in particular have the potential to maintain their good optical performance over the nearly 300 K temperature swing that occurs during the lunar cycle. Typically, epoxies are used for aligning and bonding hollow retroreflectors, but their thermal stability will predominantly be limited by the difference of the coefficient of thermal expansion (CTE) between the epoxy and the glass. A relatively new bonding method known as hydroxide catalysis bonding (HCB) has been used to adhere complex optical components for space-based missions. HCB has an extremely thin bond, a low CTE, and a high breaking strength that makes it an ideal candidate for bonding hollow retroreflectors for lunar laser ranging (LLR). In this work, we present results of a feasibility study of bonded Pyrex and fused silica hollow retroreflectors using both epoxy and HCB methods, including the results of thermally cycling the hollow retroreflectors from 295 to 185 K. Finally, we discuss the potential for using these retroreflectors for future LLR. (C) 2013 Optical Society of America C1 [Preston, Alix; Merkowitz, Stephen] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Merkowitz, S (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM stephen.m.merkowitz@nasa.gov RI Merkowitz, Stephen/D-6680-2012 OI Merkowitz, Stephen/0000-0002-0412-4209 FU NASA; NASA Lunar Science Institute [NNA09DB30A] FX This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The authors would like to thank Thomas Zagwodski and Michael Perry for their contributions in setting up the fabrication and testing facility at the Goddard Geophysical and Astronomical Observatory. S. M. M. is a member of the LUNAR consortium (http://lunar.colorado.edu), headquartered at the University of Colorado, and funded by the NASA Lunar Science Institute (via Cooperative Agreement NNA09DB30A) to investigate concepts for astrophysical observatories on the Moon. NR 19 TC 2 Z9 2 U1 0 U2 14 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD DEC 20 PY 2013 VL 52 IS 36 BP 8676 EP 8684 DI 10.1364/AO.52.008676 PG 9 WC Optics SC Optics GA 279GL UT WOS:000328948300007 PM 24513933 ER PT J AU Datta, R Munson, CD Niemack, MD McMahon, JJ Britton, J Wollack, EJ Beall, J Devlin, MJ Fowler, J Gallardo, P Hubmayr, J Irwin, K Newburgh, L Nibarger, JP Page, L Quijada, MA Schmitt, BL Staggs, ST Thornton, R Zhang, L AF Datta, R. Munson, C. D. Niemack, M. D. McMahon, J. J. Britton, J. Wollack, E. J. Beall, J. Devlin, M. J. Fowler, J. Gallardo, P. Hubmayr, J. Irwin, K. Newburgh, L. Nibarger, J. P. Page, L. Quijada, M. A. Schmitt, B. L. Staggs, S. T. Thornton, R. Zhang, L. TI Large-aperture wide-bandwidth antireflection-coated silicon lenses for millimeter wavelengths SO APPLIED OPTICS LA English DT Article ID SURFACE-RELIEF GRATINGS; EYE PRINCIPLE; LOSS TANGENT; PERMITTIVITY; FREQUENCIES; TELESCOPE; DESIGN; OPTICS; WINDOW; ARRAY AB The increasing scale of cryogenic detector arrays for submillimeter and millimeter wavelength astrophysics has led to the need for large aperture, high index of refraction, low loss, cryogenic refracting optics. Silicon with n = 3.4, low loss, and high thermal conductivity is a nearly optimal material for these purposes but requires an antireflection (AR) coating with broad bandwidth, low loss, low reflectance, and a matched coefficient of thermal expansion. We present an AR coating for curved silicon optics comprised of subwavelength features cut into the lens surface with a custom three-axis silicon dicing saw. These features constitute a metamaterial that behaves as a simple dielectric coating. We have fabricated silicon lenses as large as 33.4 cm in diameter with micromachined layers optimized for use between 125 and 165 GHz. Our design reduces average reflections to a few tenths of a percent for angles of incidence up to 30 degrees with low cross polarization. We describe the design, tolerance, manufacture, and measurements of these coatings and present measurements of the optical properties of silicon at millimeter wavelengths at cryogenic and room temperatures. This coating and lens fabrication approach is applicable from centimeter to submillimeter wavelengths and can be used to fabricate coatings with greater than octave bandwidth. (C) 2013 Optical Society of America C1 [Datta, R.; Munson, C. D.; McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Niemack, M. D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Niemack, M. D.; Britton, J.; Beall, J.; Fowler, J.; Hubmayr, J.; Irwin, K.] Natl Inst Stand & Technol, Boulder, CO 80305 USA. [Wollack, E. J.; Quijada, M. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Devlin, M. J.; Schmitt, B. L.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Gallardo, P.] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Newburgh, L.; Page, L.; Staggs, S. T.; Zhang, L.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Nibarger, J. P.] Natl Inst Stand & Technol, Boulder Microfabricat Facil, Boulder, CO 80305 USA. [Thornton, R.] West Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA. RP Datta, R (reprint author), Univ Michigan, Dept Phys, 450 Church St, Ann Arbor, MI 48109 USA. EM dattar@umich.edu RI Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Britton, Joe/0000-0001-8103-7347 FU U.S. National Science Foundation [AST-0965625, PHY-1214379]; NASA through the NASA Space Technology Research Fellowship training grant [NNX12AM32H] FX This work was supported by the U.S. National Science Foundation through awards AST-0965625 and PHY-1214379 and by NASA through the NASA Space Technology Research Fellowship training grant NNX12AM32H. The authors would like to thank Ki Won Yoon and Molly Dee for useful discussions. NR 43 TC 26 Z9 26 U1 2 U2 10 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD DEC 20 PY 2013 VL 52 IS 36 BP 8747 EP 8758 DI 10.1364/AO.52.008747 PG 12 WC Optics SC Optics GA 279GL UT WOS:000328948300013 PM 24513939 ER PT J AU Aartsen, MG Abbasi, R Abdou, Y Ackermann, M Adams, J Aguilar, JA Ahlers, M Altmann, D Auffenberg, J Bai, X Baker, M Barwick, SW Baum, V Bay, R Beatty, JJ Bechet, S Tjus, JB Becker, KH Benabderrahmane, ML BenZvi, S Berghaus, P Berley, D Bernardini, E Bernhard, A Besson, DZ Binder, G Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohaichuk, S Bohm, C Bose, D Boser, S Botner, O Brayeur, L Bretz, HP Brown, AM Bruijn, R Brunner, J Carson, M Casey, J Casier, M Chirkin, D Christov, A Christy, B Clark, K Clevermann, F Coenders, S Cohen, S Cowen, DF Silva, AHC Danninger, M Daughhetee, J Davis, JC Day, M De Clercq, C De Ridder, S Desiati, P de Vries, KD de With, M DeYoung, T Diaz-Velez, JC Dunkman, M Eagan, R Eberhardt, B Eisch, J Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feintzeig, J Feusels, T Filimonov, K Finley, C Fischer-Wasels, T Flis, S Franckowiak, A Frantzen, K Fuchs, T Gaisser, TK Gallagher, J Gerhardt, L Gladstone, L Glusenkamp, T Goldschmidt, A Golup, G Gonzalez, JG Goodman, JA Gora, D Grandmont, DT Grant, D Gross, A Ha, C Ismail, AH Hallen, P Hallgren, A Halzen, F Hanson, K Heereman, D Heinen, D Helbing, K Hellauer, R Hickford, S Hill, GC Hoffman, KD Hoffmann, R Homeier, A Hoshina, K Huelsnitz, W Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobi, E Jacobsen, J Jagielski, K Japaridze, GS Jero, K Jlelati, O Kaminsky, B Kappes, A Karg, T Karle, A Kelley, JL Kiryluk, J Klas, J Klein, SR Kohne, JH Kohnen, G Kolanoski, H Kopke, L Kopper, C Kopper, S Koskinen, DJ Kowalski, M Krasberg, M Krings, K Kroll, G Kunnen, J Kurahashi, N Kuwabara, T Labare, M Landsman, H Larson, MJ Lesiak-Bzdak, M Leuermann, M Leute, J Lunemann, J Macias, O Madsen, J Maggi, G Maruyama, R Mase, K Matis, HS McNally, F Meagher, K Merck, M Meures, T Miarecki, S Middell, E Milke, N Miller, J Mohrmann, L Montaruli, T Morse, R Nahnhauer, R Naumann, U Niederhausen, H Nowicki, SC Nygren, DR Obertacke, A Odrowski, S Olivas, A Omairat, A O'Murchadha, A Paul, L Pepper, JA de los Heros, CP Pfendner, C Pieloth, D Pinat, E Posselt, J Price, PB Przybylski, GT Radel, L Rameez, M Rawlins, K Redl, P Reimann, R Resconi, E Rhode, W Ribordy, M Richman, M Riedel, B Rodrigues, JP Rott, C Ruhe, T Ruzybayev, B Ryckbosch, D Saba, SM Salameh, T Sander, HG Santander, M Sarkar, S Schatto, K Scheriau, F Schmidt, T Schmitz, M Schoenen, S Schoneberg, S Schonwald, A Schukraft, A Schulte, L Schulz, O Seckel, D Sestayo, Y Seunarine, S Shanidze, R Sheremata, C Smith, MWE Soldin, D Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stasik, A Stezelberger, T Stokstad, RG Stossl, A Strahler, EA Strom, R Sullivan, GW Taavola, H Taboada, I Tamburro, A Tepe, A Ter-Antonyan, S Tesic, G Tilav, S Toale, PA Toscano, S Unger, E Usner, M Vallecorsa, S van Eijndhoven, N Van Overloop, A van Santen, J Vehring, M Voge, M Vraeghe, M Walck, C Waldenmaier, T Wallraff, M Weaver, C Wellons, M Wendt, C Westerhoff, S Whitehorn, N Wiebe, K Wiebusch, CH Williams, DR Wissing, H Wolf, M Wood, TR Woschnagg, K Xu, DL Xu, XW Yanez, JP Yodh, G Yoshida, S Zarzhitsky, P Ziemann, J Zierke, S Zoll, M AF Aartsen, M. G. Abbasi, R. Abdou, Y. Ackermann, M. Adams, J. Aguilar, J. A. Ahlers, M. Altmann, D. Auffenberg, J. Bai, X. Baker, M. Barwick, S. W. Baum, V. Bay, R. Beatty, J. J. Bechet, S. Tjus, J. Becker Becker, K. -H. Benabderrahmane, M. L. BenZvi, S. Berghaus, P. Berley, D. Bernardini, E. Bernhard, A. Besson, D. Z. Binder, G. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohaichuk, S. Bohm, C. Bose, D. Boeser, S. Botner, O. Brayeur, L. Bretz, H. -P. Brown, A. M. Bruijn, R. Brunner, J. Carson, M. Casey, J. Casier, M. Chirkin, D. Christov, A. Christy, B. Clark, K. Clevermann, F. Coenders, S. Cohen, S. Cowen, D. F. Silva, A. H. Cruz Danninger, M. Daughhetee, J. Davis, J. C. Day, M. De Clercq, C. De Ridder, S. Desiati, P. de Vries, K. D. de With, M. DeYoung, T. Diaz-Velez, J. C. Dunkman, M. Eagan, R. Eberhardt, B. Eisch, J. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feintzeig, J. Feusels, T. Filimonov, K. Finley, C. Fischer-Wasels, T. Flis, S. Franckowiak, A. Frantzen, K. Fuchs, T. Gaisser, T. K. Gallagher, J. Gerhardt, L. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Golup, G. Gonzalez, J. G. Goodman, J. A. Gora, D. Grandmont, D. T. Grant, D. Gross, A. Ha, C. Ismail, A. Haj Hallen, P. Hallgren, A. Halzen, F. Hanson, K. Heereman, D. Heinen, D. Helbing, K. Hellauer, R. Hickford, S. Hill, G. C. Hoffman, K. D. Hoffmann, R. Homeier, A. Hoshina, K. Huelsnitz, W. Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jacobi, E. Jacobsen, J. Jagielski, K. Japaridze, G. S. Jero, K. Jlelati, O. Kaminsky, B. Kappes, A. Karg, T. Karle, A. Kelley, J. L. Kiryluk, J. Klaes, J. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koepke, L. Kopper, C. Kopper, S. Koskinen, D. J. Kowalski, M. Krasberg, M. Krings, K. Kroll, G. Kunnen, J. Kurahashi, N. Kuwabara, T. Labare, M. Landsman, H. Larson, M. J. Lesiak-Bzdak, M. Leuermann, M. Leute, J. Luenemann, J. Macias, O. Madsen, J. Maggi, G. Maruyama, R. Mase, K. Matis, H. S. McNally, F. Meagher, K. Merck, M. Meures, T. Miarecki, S. Middell, E. Milke, N. Miller, J. Mohrmann, L. Montaruli, T. Morse, R. Nahnhauer, R. Naumann, U. Niederhausen, H. Nowicki, S. C. Nygren, D. R. Obertacke, A. Odrowski, S. Olivas, A. Omairat, A. O'Murchadha, A. Paul, L. Pepper, J. A. de los Heros, C. Perez Pfendner, C. Pieloth, D. Pinat, E. Posselt, J. Price, P. B. Przybylski, G. T. Raedel, L. Rameez, M. Rawlins, K. Redl, P. Reimann, R. Resconi, E. Rhode, W. Ribordy, M. Richman, M. Riedel, B. Rodrigues, J. P. Rott, C. Ruhe, T. Ruzybayev, B. Ryckbosch, D. Saba, S. M. Salameh, T. Sander, H. -G. Santander, M. Sarkar, S. Schatto, K. Scheriau, F. Schmidt, T. Schmitz, M. Schoenen, S. Schoeneberg, S. Schoenwald, A. Schukraft, A. Schulte, L. Schulz, O. Seckel, D. Sestayo, Y. Seunarine, S. Shanidze, R. Sheremata, C. Smith, M. W. E. Soldin, D. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stasik, A. Stezelberger, T. Stokstad, R. G. Stoessl, A. Strahler, E. A. Strom, R. Sullivan, G. W. Taavola, H. Taboada, I. Tamburro, A. Tepe, A. Ter-Antonyan, S. Tesic, G. Tilav, S. Toale, P. A. Toscano, S. Unger, E. Usner, M. Vallecorsa, S. van Eijndhoven, N. Van Overloop, A. van Santen, J. Vehring, M. Voge, M. Vraeghe, M. Walck, C. Waldenmaier, T. Wallraff, M. Weaver, Ch Wellons, M. Wendt, C. Westerhoff, S. Whitehorn, N. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wissing, H. Wolf, M. Wood, T. R. Woschnagg, K. Xu, D. L. Xu, X. W. Yanez, J. P. Yodh, G. Yoshida, S. Zarzhitsky, P. Ziemann, J. Zierke, S. Zoll, M. TI SEARCH FOR TIME-INDEPENDENT NEUTRINO EMISSION FROM ASTROPHYSICAL SOURCES WITH 3 yr OF IceCube DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE astroparticle physics; cosmic rays; neutrinos; telescopes ID GAMMA-RAY EMISSION; HIGH-ENERGY NEUTRINOS; BRIGHT GALAXY SAMPLE; FERMI-LAT DISCOVERY; SUPERNOVA-REMNANTS; COSMIC-RAYS; CRAB-NEBULA; STARBURST GALAXIES; MOLECULAR CLOUDS; GALACTIC SOURCES AB We present the results of a search for neutrino point sources using the IceCube data collected between 2008 April and 2011 May with three partially completed configurations of the detector: the 40-, 59-, and 79-string configurations. The live-time of this data set is 1040 days. An unbinned maximum likelihood ratio test was used to search for an excess of neutrinos above the atmospheric background at any given direction in the sky. By adding two more years of data with improved event selection and reconstruction techniques, the sensitivity was improved by a factor of 3.5 or more with respect to the previously published results obtained with the 40-string configuration of IceCube. We performed an all-sky survey and a dedicated search using a catalog of a priori selected objects observed by other telescopes. In both searches, the data are compatible with the background-only hypothesis. In the absence of evidence for a signal, we set upper limits on the flux of muon neutrinos. For an E-2 neutrino spectrum, the observed limits are (0.9-5) x 10(-12) TeV-1 cm(-2) s(-1) for energies between 1 TeV and 1 PeV in the northern sky and (0.9-23.2) x 10(-12) TeV-1 cm(-2) s(-1) for energies between 10(2) TeV and 10(2) PeV in the southern sky. We also report upper limits for neutrino emission from groups of sources that were selected according to theoretical models or observational parameters and analyzed with a stacking approach. Some of the limits presented already reach the level necessary to quantitatively test current models of neutrino emission. C1 [Aartsen, M. G.; Hill, G. C.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Abbasi, R.; Ahlers, M.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kelley, J. L.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Abbasi, R.; Ahlers, M.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kelley, J. L.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA. [Abdou, Y.; Carson, M.; De Ridder, S.; Feusels, T.; Ismail, A. Haj; Jlelati, O.; Labare, M.; Ryckbosch, D.; Van Overloop, A.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium. [Ackermann, M.; Benabderrahmane, M. L.; Berghaus, P.; Bernardini, E.; Bretz, H. -P.; Brunner, J.; Silva, A. H. Cruz; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Kaminsky, B.; Karg, T.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Shanidze, R.; Spiering, C.; Stoessl, A.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany. [Adams, J.; Brown, A. M.; Hickford, S.; Macias, O.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Aguilar, J. A.; Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland. [Altmann, D.; de With, M.; Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Bai, X.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bai, X.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Baum, V.; Eberhardt, B.; Koepke, L.; Kroll, G.; Luenemann, J.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Bay, R.; Binder, G.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Bechet, S.; Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.; Pinat, E.] Univ Libre Brussels, Sci Fac CP230, B-1050 Brussels, Belgium. [Tjus, J. Becker; Fedynitch, A.; Saba, S. M.; Schoeneberg, S.; Unger, E.] Ruhr Univ Bochum, Fac Phys & Astron, D-44780 Bochum, Germany. [Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Helbing, K.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Omairat, A.; Posselt, J.; Soldin, D.; Tepe, A.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Berley, D.; Blaufuss, E.; Christy, B.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Bernhard, A.; Gross, A.; Leute, J.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany. [Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Binder, G.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Bissok, M.; Blumenthal, J.; Coenders, S.; Euler, S.; Hallen, P.; Heinen, D.; Jagielski, K.; Krings, K.; Leuermann, M.; Paul, L.; Raedel, L.; Reimann, R.; Schoenen, S.; Schukraft, A.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.; Zierke, S.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Boersma, D. J.; Botner, O.; Hallgren, A.; de los Heros, C. Perez; Strom, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden. [Bohaichuk, S.; Grandmont, D. T.; Grant, D.; Nowicki, S. C.; Sheremata, C.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Bose, D.; Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; Golup, G.; Kunnen, J.; Maggi, G.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Schulte, L.; Stasik, A.; Usner, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Bruijn, R.; Cohen, S.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Clark, K.; Cowen, D. F.; DeYoung, T.; Dunkman, M.; Eagan, R.; Koskinen, D. J.; Salameh, T.; Smith, M. W. E.; Tesic, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Clevermann, F.; Frantzen, K.; Fuchs, T.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.; Scheriau, F.; Schmitz, M.; Ziemann, J.] TU Dortmund Univ, Dept Phys, Dortmund, Germany. [Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Larson, M. J.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea. [Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA. [Huelsnitz, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Montaruli, T.] Sezione Ist Nazl Fis Nucl, Dipartimento Fis, I-70126 Bari, Italy. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Aartsen, MG (reprint author), Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. RI Taavola, Henric/B-4497-2011; Aguilar Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011; Tjus, Julia/G-8145-2012; Wiebusch, Christopher/G-6490-2012; Auffenberg, Jan/D-3954-2014; Koskinen, David/G-3236-2014; Brunner, Juergen/G-3540-2015 OI Taavola, Henric/0000-0002-2604-2810; Carson, Michael/0000-0003-0400-7819; Perez de los Heros, Carlos/0000-0002-2084-5866; Benabderrahmane, Mohamed Lotfi/0000-0003-4410-5886; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Rott, Carsten/0000-0002-6958-6033; Ter-Antonyan, Samvel/0000-0002-5788-1369; Schukraft, Anne/0000-0002-9112-5479; Wiebusch, Christopher/0000-0002-6418-3008; Auffenberg, Jan/0000-0002-1185-9094; Koskinen, David/0000-0002-0514-5917; Brunner, Juergen/0000-0002-5052-7236 FU US National Science Foundation's Office of Polar Programs; US National Science Foundation's Physics Division; University of Wisconsin Alumni Research Foundation; Grid Laboratory of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison; Open Science Grid (OSG) grid infrastructure; US Department of Energy; National Energy Research Scientific Computing Center; Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada; West-Grid; Swedish Research Council; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Helmholtz Alliance for Astroparticle Physics (HAP); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus program; Flanders Institute to encourage scientific and technological research in industry (IWT); Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF) FX We acknowledge support from the following agencies: US National Science Foundation's Office of Polar Programs, US National Science Foundation's Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid infrastructure; US Department of Energy and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada, West-Grid and Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus program, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; and National Research Foundation of Korea (NRF). NR 88 TC 43 Z9 43 U1 0 U2 18 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 132 DI 10.1088/0004-637X/779/2/132 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200042 ER PT J AU Acero, F Donato, D Ojha, R Stevens, J Edwards, PG Ferrara, E Blanchard, J Lovell, JEJ Thompson, DJ AF Acero, F. Donato, D. Ojha, R. Stevens, J. Edwards, P. G. Ferrara, E. Blanchard, J. Lovell, J. E. J. Thompson, D. J. TI HUNTING FOR TREASURES AMONG THE FERMI UNASSOCIATED SOURCES: A MULTIWAVELENGTH APPROACH SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; gamma rays: general; pulsars: general; quasars: general; radio continuum: galaxies; ultraviolet: galaxies; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; GAMMA-RAY SOURCES; LINE SEYFERT 1; LARGE-AREA TELESCOPE; X-RAY; BLAZAR SEQUENCE; CATALOG; GALAXY; RADIO; SWIFT AB The Fermi Gamma-Ray Space Telescope has been detecting a wealth of sources where the multiwavelength counterpart is either inconclusive or missing altogether. We present a combination of factors that can be used to identify multiwavelength counterparts to these Fermi unassociated sources. This approach was used to select and investigate seven bright, high-latitude unassociated sources with radio, UV, X-ray, and gamma-ray observations. As a result, four of these sources are candidates to be active galactic nuclei, and one to be a pulsar, while two do not fit easily into these known categories of sources. The latter pair of extraordinary sources might reveal a new category subclass or a new type of gamma-ray emitter. These results altogether demonstrate the power of a multiwavelength approach to illuminate the nature of unassociated Fermi sources. C1 [Acero, F.; Ojha, R.] NASA, ORAU, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Donato, D.; Ferrara, E.] NASA, CRESST, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Ojha, R.] Catholic Univ Amer, Washington, DC 20064 USA. [Ojha, R.; Blanchard, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Stevens, J.] CSIRO Astron & Space Sci, Narrabri, NSW 2390, Australia. [Edwards, P. G.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Thompson, D. J.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Acero, F (reprint author), NASA, ORAU, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA. EM fabio.f.acero@nasa.gov FU Commonwealth of Australia; NASA [NNH09ZDA001N, NNH10ZDA001N] FX This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester (Evans et al. 2009). The Australia Telescope Compact Array is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This research was funded in part by NASA through Fermi Guest Investigator grants NNH09ZDA001N and NNH10ZDA001N. This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This research has made use of data from the NASA/IPAC Extragalactic Database (NED, operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration); and the SIMBAD database (operated at CDS, Strasbourg, France). This research has made use of NASA's Astrophysics Data System. NR 29 TC 11 Z9 11 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 133 DI 10.1088/0004-637X/779/2/133 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200043 ER PT J AU An, HJ Hascoet, R Kaspi, VM Beloborodov, AM Dufour, F Gotthelf, EV Archibald, R Bachetti, M Boggs, SE Christensen, FE Craig, WW Greffenstette, BW Hailey, CJ Harrison, FA Kitaguchi, T Kouveliotou, C Madsen, KK Markwardt, CB Stern, D Vogel, JK Zhang, WW AF An, Hongjun Hascoet, Romain Kaspi, Victoria M. Beloborodov, Andrei M. Dufour, Francois Gotthelf, Eric V. Archibald, Robert Bachetti, Matteo Boggs, Steven E. Christensen, Finn E. Craig, William W. Greffenstette, Brian W. Hailey, Charles J. Harrison, Fiona A. Kitaguchi, Takao Kouveliotou, Chryssa Madsen, Kristin K. Markwardt, Craig B. Stern, Daniel Vogel, Julia K. Zhang, William W. TI NuSTAR OBSERVATIONS OF MAGNETAR 1E 1841-045 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (1E 1841-045); stars: magnetars; stars: neutron ID X-RAY PULSAR; SOFT GAMMA-REPEATERS; HIGH-ENERGY CHARACTERISTICS; SWIFT J1822.3-1606; NEUTRON-STARS; XMM-NEWTON; 4U 0142+61; SPIN-DOWN; KES 73; EMISSION AB We report new spectral and temporal observations of the magnetar 1E 1841-045 in the Kes 73 supernova remnant obtained with the Nuclear Spectroscopic Telescope Array. Combined with new Swift and archival XMM-Newton and Chandra observations, the phase-averaged spectrum is well characterized by a blackbody plus double power law, in agreement with previous multimission X-ray results. However, we are unable to reproduce the spectral results reported based on Suzaku observations. The pulsed fraction of the source is found to increase with photon energy. The measured rms pulsed fractions are similar to 12% and similar to 17% at similar to 20 and similar to 50 keV, respectively. We detect a new feature in the 24-35 keV band pulse profile that is uniquely double peaked. This feature may be associated with a possible absorption or emission feature in the phase-resolved spectrum. We fit the X-ray data using the recently developed electron-positron outflow model by Beloborodov for the hard X-ray emission from magnetars. This produces a satisfactory fit, allowing a constraint on the angle between the rotation and magnetic axes of the neutron star of similar to 20 degrees and on the angle between the rotation axis and line of sight of similar to 50 degrees. In this model, the soft X-ray component is inconsistent with a single blackbody; adding a second blackbody or a power-law component fits the data. The two-blackbody interpretation suggests a hot spot of temperature kT approximate to 0.9 keV occupying similar to 1% of the stellar surface. C1 [An, Hongjun; Kaspi, Victoria M.; Dufour, Francois; Archibald, Robert] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Hascoet, Romain; Beloborodov, Andrei M.; Gotthelf, Eric V.; Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Bachetti, Matteo] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Bachetti, Matteo] Inst Rech Astrophys & Planetol, CNRS, F-31028 Toulouse 4, France. [Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, William W.; Vogel, Julia K.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Greffenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Kitaguchi, Takao] RIKEN, Wako, Saitama 3510198, Japan. [Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Markwardt, Craig B.; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP An, HJ (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337; Madsen, Kristin/0000-0003-1252-4891 FU NASA [NNG08FD60C, NNX10AI72G, NNX13AI34G]; NSERC Discovery Grant; FQRNT Centre de Recherche Astrophysique du Quebec; R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR); Canada Research Chairs Program; Lorne Trottier Chair in Astrophysics and Cosmology; US Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344] FX This work was supported under NASA contract NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration Teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (US). V. M. K. acknowledges support from an NSERC Discovery Grant, the FQRNT Centre de Recherche Astrophysique du Quebec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. A. M. B. acknowledges the support by NASA grants NNX10AI72G and NNX13AI34G. Part of this work was performed under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344. NR 45 TC 12 Z9 12 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 163 DI 10.1088/0004-637X/779/2/163 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200072 ER PT J AU Archambault, S Beilicke, M Benbow, W Berger, K Bird, R Bouvier, A Buckley, JH Bugaev, V Byrum, K Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Duke, C Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fortson, L Furniss, A Galante, N Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Kaaret, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Lang, MJ Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Pandel, D Park, N Perkins, JS Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Rajotte, J Reyes, LC Reynolds, PT Richards, GT Roache, E Sembroski, GH Sheidaei, F Smith, AW Staszak, D Telezhinsky, I Theiling, M Tucci, JV Tyler, J Varlotta, A Vincent, S Wakely, SP Weekes, TC Weinstein, A Williams, DA Zitzer, B McCollough, ML AF Archambault, S. Beilicke, M. Benbow, W. Berger, K. Bird, R. Bouvier, A. Buckley, J. H. Bugaev, V. Byrum, K. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Duke, C. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Lang, M. J. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Pandel, D. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Rajotte, J. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Sembroski, G. H. Sheidaei, F. Smith, A. W. Staszak, D. Telezhinsky, I. Theiling, M. Tucci, J. V. Tyler, J. Varlotta, A. Vincent, S. Wakely, S. P. Weekes, T. C. Weinstein, A. Williams, D. A. Zitzer, B. McCollough, M. L. CA VERITAS Collaboration Smithsonian Astrophys Observ TI VERITAS OBSERVATIONS OF THE MICROQUASAR CYGNUS X-3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; binaries: close; gamma rays: stars; X-rays: individual (Cygnus X-3) ID GAMMA-RAY EMISSION; LARGE-AREA TELESCOPE; X-RAY; CYG X-3; CHERENKOV TELESCOPES; RELATIVISTIC JET; SCATTERING HALO; CONSTRAINTS; MISSION; SEARCH AB We report results from TeV gamma-ray observations of the microquasar Cygnus X-3. The observations were made with the Very Energetic Radiation Imaging Telescope Array System (VERITAS) over a time period from 2007 June 11 to 2011 November 28. VERITAS is most sensitive to gamma rays at energies between 85 GeV and 30 TeV. The effective exposure time amounts to a total of about 44 hr, with the observations covering six distinct radio/X-ray states of the object. No significant TeV gamma-ray emission was detected in any of the states, nor with all observations combined. The lack of a positive signal, especially in the states where GeV gamma rays were detected, places constraints on TeV gamma-ray production in Cygnus X-3. We discuss the implications of the results. C1 [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Galante, N.; Roache, E.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Chen, X.; Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Chen, X.; Federici, S.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.] DESY, D-15738 Zeuthen, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Dumm, J.; Fortson, L.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Errando, M.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Humensky, T. B.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Kieda, D.; Sheidaei, F.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Majumdar, P.; Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Majumdar, P.] Saha Inst Nucl Phys, Kolkata 700064, India. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Pandel, D.] Grand Valley State Univ, Dept Phys, Allendale, MI 49401 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [McCollough, M. L.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Cui, W (reprint author), Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. EM cui@purdue.edu; avarlott@purdue.edu RI Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755; Cui, Wei/0000-0002-6324-5772; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563 FU NASA through a Fermi GI grant [NNX11AP90G]; Purdue University; U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K. FX This work has made use of high-level data products provided by the ASM/RXTE, MAXI, and BAT/Swift teams. The AMI-LA radio results were obtained from a public archive maintained by Guy Pooley. Paul Ray is thanked for making available the ephemeris for PSR J2032+4127. A. V. and W. C. gratefully acknowledge financial support from NASA through a Fermi GI grant (NNX11AP90G) and from Purdue University. The VERI-TAS operation is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. NR 48 TC 2 Z9 2 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR UNSP 150 DI 10.1088/0004-637X/779/2/150 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200059 ER PT J AU Brodwin, M Stanford, SA Gonzalez, AH Zeimann, GR Snyder, GF Mancone, CL Pope, A Eisenhardt, PR Stern, D Alberts, S Ashby, MLN Brown, MJI Chary, RR Dey, A Galametz, A Gettings, DP Jannuzi, BT Miller, ED Moustakas, J Moustakas, LA AF Brodwin, M. Stanford, S. A. Gonzalez, Anthony H. Zeimann, G. R. Snyder, G. F. Mancone, C. L. Pope, A. Eisenhardt, P. R. Stern, D. Alberts, S. Ashby, M. L. N. Brown, M. J. I. Chary, R-R Dey, Arjun Galametz, A. Gettings, D. P. Jannuzi, B. T. Miller, E. D. Moustakas, J. Moustakas, L. A. TI THE ERA OF STAR FORMATION IN GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: distances and redshifts; galaxies: evolution; galaxies: formation; galaxies: starburst ID ACTIVE GALACTIC NUCLEI; SIMILAR-TO 1; SUPERMASSIVE BLACK-HOLES; COLOR-MAGNITUDE RELATION; DUST-OBSCURED GALAXIES; IRAC SHALLOW SURVEY; INFRARED LUMINOUS GALAXIES; FORMATION-DENSITY RELATION; HIGH-REDSHIFT GALAXIES; INITIAL MASS FUNCTION AB We analyze the star formation properties of 16 infrared-selected, spectroscopically confirmed galaxy clusters at 1 < z < 1.5 from the Spitzer/IRAC Shallow Cluster Survey (ISCS). We present new spectroscopic confirmation for six of these high-redshift clusters, five of which are at z > 1.35. Using infrared luminosities measured with deep Spitzer/Multiband Imaging Photometer for Spitzer observations at 24 mu m, along with robust optical + IRAC photometric redshifts and spectral-energy-distribution-fitted stellar masses, we present the dust-obscured star-forming fractions, star formation rates, and specific star formation rates in these clusters as functions of redshift and projected cluster centric radius. We find that z similar to 1.4 represents a transition redshift for the ISCS sample, with clear evidence of an unquenched era of cluster star formation at earlier times. Beyond this redshift, the fraction of star-forming cluster members increases monotonically toward the cluster centers. Indeed, the specific star formation rate in the cores of these distant clusters is consistent with field values at similar redshifts, indicating that at z > 1.4 environment-dependent quenching had not yet been established in ISCS clusters. By combining these observations with complementary studies showing a rapid increase in the active galactic nucleus (AGN) fraction, a stochastic star formation history, and a major merging episode at the same epoch in this cluster sample, we suggest that the starburst activity is likely merger-driven and that the subsequent quenching is due to feedback from merger-fueled AGNs. The totality of the evidence suggests we are witnessing the final quenching period that brings an end to the era of star formation in galaxy clusters and initiates the era of passive evolution. C1 [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Stanford, S. A.] Univ Calif Davis, Davis, CA 95616 USA. [Gonzalez, Anthony H.; Mancone, C. L.; Gettings, D. P.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Zeimann, G. R.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Snyder, G. F.; Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pope, A.; Alberts, S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Eisenhardt, P. R.; Stern, D.; Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Chary, R-R] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Galametz, A.] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Jannuzi, B. T.] Univ Arizona, Steward Observ, Tucson, AZ 85121 USA. [Miller, E. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Moustakas, J.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. RP Brodwin, M (reprint author), Univ Missouri, Dept Phys & Astron, 5110 Rockhill Rd, Kansas City, MO 64110 USA. RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Moustakas, Leonidas/0000-0003-3030-2360 FU NASA [G09-0150A]; JPL/Caltech; NASA Space Telescope Science Institute [10496, 11002, 11597, 11663]; W. M. Keck Foundation; Chandra X-ray Observatory [SV4-74018, A31]; Smithsonian Astrophysical Observatory FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Support for HST programs 10496, 11002, 11597, and 11663 were provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This work is based in part on observations obtained with the Chandra X-ray Observatory, under contract SV4-74018, A31 with the Smithsonian Astrophysical Observatory which operates the Chandra X-ray Observatory for NASA. Support for this research was provided by NASA grant G09-0150A. This work is based in part on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This work makes use of image data from the NOAO Deep Wide-Field Survey (NDWFS) as distributed by the NOAO Science Archive. NOAO is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under a cooperative agreement with the National Science Foundation. NR 120 TC 74 Z9 74 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 138 DI 10.1088/0004-637X/779/2/138 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200047 ER PT J AU Coudert, LH Drouin, BJ Tercero, B Cernicharo, J Guillemin, JC Motiyenko, RA Margules, L AF Coudert, L. H. Drouin, B. J. Tercero, B. Cernicharo, J. Guillemin, J-C Motiyenko, R. A. Margules, L. TI THE FIRST ASTROPHYSICAL DETECTION, TERAHERTZ SPECTRUM, AND DATABASE FOR THE MONODEUTERATED SPECIES OF METHYL FORMATE HCOOCH2D SO ASTROPHYSICAL JOURNAL LA English DT Article DE astronomical databases: miscellaneous; ISM: individual objects (Orion KL); ISM: molecules; line: identification; methods: data analysis; methods: laboratory: molecular; submillimeter: ISM ID SUBMILLIMETER-WAVE SPECTRUM; EXCITED TORSIONAL STATES; ORION-KL; ROTATIONAL SPECTRUM; LINE SURVEY; MICROWAVE-SPECTRUM; TENTATIVE DETECTION; ETHYL CYANIDE; ISM DETECTION; MILLIMETER AB Based on new measurements carried out in the laboratory from 0.77 to 1.2 THz and on a line-frequency analysis of these new data, along with previously published data, we build a line list for HCOOCH2D that leads to its first detection in the Orion KL nebula. The observed lines, both in space and in the laboratory, involve the cis D-in-plane and trans D-out-of-plane conformations of HCOOCH2D and the two tunneling states arising from the large-amplitude motion connecting the two trans configurations. The model used in the line position calculation accounts for both cis and trans conformations, as well as the large-amplitude motion. C1 [Coudert, L. H.] Univ Paris Est Creteil, CNRS, UMR 7583, LISA, F-94010 Creteil, France. [Coudert, L. H.] Univ Paris Diderot, CNRS, UMR 7583, LISA, F-94010 Creteil, France. [Drouin, B. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tercero, B.; Cernicharo, J.] Dept Astrophys, Lab Mol Astrophys, Ctr Astrobiol CSIC INTA, E-28850 Madrid, Spain. [Guillemin, J-C] ENSCR, CNRS, UMR 6226, Inst Sci Chim Rennes, F-35708 Rennes 7, France. [Motiyenko, R. A.; Margules, L.] Univ Lille 1, UMR 8523, CNRS, Lab Phys Lasers Atomes & Mol, F-59655 Villeneuve Dascq, France. RP Coudert, LH (reprint author), Univ Paris Est Creteil, CNRS, UMR 7583, LISA, 61 Ave Gen Gaulle, F-94010 Creteil, France. EM laurent.coudert@lisa.u-pec.fr OI Guillemin, Jean-Claude/0000-0002-2929-057X FU French program Action sur Projets de l'INSU "Physique et Chimie du Milieu Interstellaire" (PCMI); Spanish MINECO [CSD2009-00038, AYA2009-07304, AYA2012-32032]; [ANR-08-BLAN-0054]; [ANR-08-BLAN-0225] FX Portions of this paper present research carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Government sponsorship is acknowledged. This work was also supported by the French program Action sur Projets de l'INSU "Physique et Chimie du Milieu Interstellaire" (PCMI) and by the contracts ANR-08-BLAN-0054 and ANR-08-BLAN-0225. J. C. and B. T. thank the Spanish MINECO for funding support from grants CSD2009-00038, AYA2009-07304, and AYA2012-32032. NR 49 TC 11 Z9 11 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 119 DI 10.1088/0004-637X/779/2/119 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200029 ER PT J AU Coustenis, A Bampasidis, G Achterberg, RK Lavvas, P Jennings, DE Nixon, CA Teanby, NA Vinatier, S Flasar, FM Carlson, RC Orton, G Romani, PN Guandique, EA Stamogiorgos, S AF Coustenis, Athena Bampasidis, G. Achterberg, R. K. Lavvas, P. Jennings, D. E. Nixon, C. A. Teanby, N. A. Vinatier, S. Flasar, F. M. Carlson, R. C. Orton, G. Romani, P. N. Guandique, E. A. Stamogiorgos, S. TI EVOLUTION OF THE STRATOSPHERIC TEMPERATURE AND CHEMICAL COMPOSITION OVER ONE TITANIAN YEAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE molecular processes; planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: individual (Titan); radiation mechanisms: thermal ID VOYAGER INFRARED OBSERVATIONS; ISOTOPIC-RATIOS; ATMOSPHERIC TEMPERATURES; HETERODYNE OBSERVATIONS; VERTICAL DISTRIBUTIONS; SPECTROSCOPIC DATABASE; ETHANE ABUNDANCE; CASSINI/CIRS; SPECTRA; HCN AB Since the Voyager 1 (V1) flyby in 1980, Titan's exploration from space and the ground has been ongoing for more than a full revolution of Saturn around the Sun (one Titanian year or 29.5 Earth years had elapsed in 2010 May). In this study, we search for temporal variations affecting Titan's atmospheric thermal and chemical structure within that year. We process Cassini/CIRS data taken during the Titan flybys from 2006-2013 and find a rather uneventful equatorial evolution. Conversely, at northern latitudes, we found enhanced abundances around the period of the northern spring equinox in mid-2009, which subsequently decreased (from 2010 to 2012), returning to values similar to those found in the V1 epoch, one Titanian year before. In the southern latitudes, since 2012, we see a trend for an increase of several trace gases (C4H2, C3H4, and HCN), indicative of a seasonal atmospheric reversal setting in. When we compare the CIRS 2010 and the 1980 V1/IRIS spectra (reanalyzed here), we find limited inter-annual variations. A return to the 1980 stratospheric temperatures and abundances is generally achieved from 50 degrees N to 50 degrees S, indicative of the solar radiation being the dominating energy source at 10 AU, as for the Earth, as predicted by general circulation and photochemical models. Exceptions concern the most complex hydrocarbons (C4H2 and C3H4). We also consider data from ground-based and Earth-orbiting observatories (such as from the Infrared Space Observatory, revisited here) and discuss possible atmospheric composition trends during a Titanian year. C1 [Coustenis, Athena; Bampasidis, G.; Vinatier, S.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Bampasidis, G.; Stamogiorgos, S.] Univ Athens, Fac Phys, GR-15783 Athens, Greece. [Achterberg, R. K.; Jennings, D. E.; Nixon, C. A.; Flasar, F. M.; Carlson, R. C.; Romani, P. N.; Guandique, E. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Achterberg, R. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Lavvas, P.] Univ Reims, GSMA, F-51687 Reims 2, France. [Teanby, N. A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. [Carlson, R. C.] Catholic Univ Amer, IACS, Washington, DC 20064 USA. [Orton, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Guandique, E. A.] Adnet Syst Inc, Rockville, MD 20852 USA. [Stamogiorgos, S.] Tech Univ Munich, D-80333 Munich, Germany. RP Coustenis, A (reprint author), Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France. EM athena.coustenis@obspm.fr RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; OI Nixon, Conor/0000-0001-9540-9121; Teanby, Nicholas/0000-0003-3108-5775 FU ESA/NASA Cassini mission funds through the CNES program; Agence Nationale de la Recherche (ANR) [11BS56002]; UK Science and Technology Facilities Council; Leverhulme Trust; NASA FX We thank Florence Henry, Marcia Segura, and Nicolas Gorius for help with the data during this project. We are grateful to Pascal Rannou and Sebastien Lebonnois for discussions on general circulation models. The authors acknowledge the support of the ESA/NASA Cassini mission funds through the CNES program. A. C. and S. V. received support from the Agence Nationale de la Recherche (ANR project "APOSTIC" #11BS56002, France). N.A.T. received support from the UK Science and Technology Facilities Council and the Leverhulme Trust. Support for G.O. was provided by NASA to the Jet Propulsion Laboratory, California Institute of Technology. NR 50 TC 11 Z9 11 U1 0 U2 18 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 177 DI 10.1088/0004-637X/779/2/177 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200086 ER PT J AU Dutka, MS Ojha, R Pottschmidt, K Finke, JD Stevens, J Edwards, PG Blanchard, J Lovell, JEJ Nesci, R Kadler, M Wilms, J Tosti, G Pursimo, T Krauss, F Muller, C Gehrels, N AF Dutka, Michael S. Ojha, Roopesh Pottschmidt, Katja Finke, Justin D. Stevens, Jamie Edwards, Philip G. Blanchard, Jay Lovell, James E. J. Nesci, Roberto Kadler, Matthias Wilms, Joern Tosti, Gino Pursimo, Tapio Krauss, Felicia Mueller, Cornelia Gehrels, Neil TI MULTI-WAVELENGTH OBSERVATIONS OF PKS 2142-75 DURING ACTIVE AND QUIESCENT GAMMA-RAY STATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; gamma rays: galaxies; quasars: individual (PKS 2142-75); radio continuum: galaxies; ultraviolet: galaxies; X-rays: individual (PKS 2142-75) ID LARGE-AREA TELESCOPE; SPECTRUM RADIO QUASARS; BL-LAC OBJECTS; RELATIVISTIC JETS; COMPTON ANALYSIS; BRIGHT BLAZARS; SOURCE CATALOG; X-RAY; RADIATION; MISSION AB PKS 2142-75 (a.k.a. 2FGL J2147.4-7534) is a flat-spectrum radio quasar that was observed quasi-simultaneously by a suite of instruments across the electromagnetic spectrum during two flaring states in 2010 April and 2011 August as well as a quiescent state from 2011 December through 2012 January. The results of these campaigns and model spectral energy distributions (SEDs) from the active and quiescent states are presented. The SED model parameters of PKS 2142-75 indicate that the two flares of the source are created by unique physical conditions. SED studies of flat-spectrum radio quasars are beginning to indicate that there might be two types of flares, those that can be described purely by changes in the electron distribution and those that require changes in other parameters, such as the magnetic field strength or the size of the emitting region. C1 [Dutka, Michael S.] Catholic Univ Amer, Washington, DC 20064 USA. [Ojha, Roopesh] NASA, ORAU, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Pottschmidt, Katja] UMBC, CRESST, Greenbelt, MD 20771 USA. [Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Finke, Justin D.] US Navy, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Stevens, Jamie] CSIRO Astron & Space Sci, Narrabri, NSW 2390, Australia. [Edwards, Philip G.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Blanchard, Jay] Univ Concepcion, Dept Astronoma, Concepcion 4089100, Chile. [Lovell, James E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Nesci, Roberto] IAPS, INAF, I-00133 Rome, Italy. [Kadler, Matthias; Mueller, Cornelia] Univ Wurzburg, Lehrstuhl Astron, D-97074 Wurzburg, Germany. [Wilms, Joern; Krauss, Felicia; Mueller, Cornelia] Remeis Observ, D-96049 Bamberg, Germany. [Wilms, Joern; Krauss, Felicia; Mueller, Cornelia] ECAP, D-96049 Bamberg, Germany. [Tosti, Gino] Univ Perugia, I-06123 Perugia, Italy. [Pursimo, Tapio] Nord Opt Telescope, E-38700 Santa Cruz Palma Santa C, Spain. [Gehrels, Neil] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Dutka, MS (reprint author), Catholic Univ Amer, 620 Michigan Ave NE, Washington, DC 20064 USA. EM ditko86@gmail.com RI Wilms, Joern/C-8116-2013; OI Wilms, Joern/0000-0003-2065-5410; Krauss, Felicia/0000-0001-6191-1244; Kadler, Matthias/0000-0001-5606-6154 FU NASA [NNH09ZDA001N, NNH10ZDA001N]; NASA Postdoctoral Program at the Goddard Space Flight Center; NASA; National Aeronautics and Space Administration; Commonwealth of Australia; SIMBAD; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX We thank the Swift team for scheduling our Target of Opportunity requests. This research was funded in part by NASA through Fermi Guest Investigator grants NNH09ZDA001N and NNH10ZDA001N. This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This publication makes use of data products from the Wide-Field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The Australia Telescope Compact Array is part of the Australia Telescope National Facility, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This research has made use of data from the NASA/IPAC Extragalactic Database (NED), operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; and the SIMBAD database (operated at CDS, Strasbourg, France). This research has made use of NASA's Astrophysics Data System. This research has made use of the United States Naval Observatory (USNO) Radio Reference Frame Image Database (RRFID). This article has made use of up-to-date SMARTS optical/near-infrared light curves that are available at www.astro.yale.edu/smarts/glast/home.php.; Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. NR 45 TC 9 Z9 9 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR UNSP 174 DI 10.1088/0004-637X/779/2/174 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200083 ER PT J AU Frederiks, DD Hurley, K Svinkin, DS Pal'shin, VD Mangano, V Oates, S Aptekar, RL Golenetskii, SV Mazets, EP Oleynik, PP Tsvetkova, AE Ulanov, MV Kokomov, AA Cline, TL Burrows, DN Krimm, HA Pagani, C Sbarufatti, B Siegel, MH Mitrofanov, IG Golovin, D Litvak, ML Sanin, AB Boynton, W Fellows, C Harshman, K Enos, H Starr, R von Kienlin, A Rau, A Zhang, X Goldstein, J AF Frederiks, D. D. Hurley, K. Svinkin, D. S. Pal'shin, V. D. Mangano, V. Oates, S. Aptekar, R. L. Golenetskii, S. V. Mazets, E. P. Oleynik, Ph. P. Tsvetkova, A. E. Ulanov, M. V. Kokomov, A. A. Cline, T. L. Burrows, D. N. Krimm, H. A. Pagani, C. Sbarufatti, B. Siegel, M. H. Mitrofanov, I. G. Golovin, D. Litvak, M. L. Sanin, A. B. Boynton, W. Fellows, C. Harshman, K. Enos, H. Starr, R. von Kienlin, A. Rau, A. Zhang, X. Goldstein, J. TI THE ULTRALUMINOUS GRB 110918A SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: individual (GRB 110918A) ID GAMMA-RAY BURST; ULTRA-VIOLET/OPTICAL TELESCOPE; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; AFTERGLOW LIGHT CURVES; X-RAY; LORENTZ-FACTOR; INTERPLANETARY NETWORK; SPECTRAL EVOLUTION; OPTICAL AFTERGLOW; ENERGY INJECTION AB GRB 110918A is the brightest long gamma-ray burst (GRB) detected by Konus-WIND during its almost 19 yr of continuous observations and the most luminous GRB ever observed since the beginning of the cosmological era in 1997. We report on the final Interplanetary Network localization of this event and its detailed multiwavelength study with a number of space-based instruments. The prompt emission is characterized by a typical duration, a moderate peak energy of the time-integrated spectrum, and strong hard-to-soft evolution. The high observed energy fluence yields, at z = 0.984, a huge isotropic-equivalent energy release E-iso = (2.1 +/- 0.1) x 10(54) erg. The record-breaking energy flux observed at the peak of the short, bright, hard initial pulse results in an unprecedented isotropic-equivalent luminosity L-iso = (4.7 +/- 0.2) x 10(54) erg s(-1). A tail of the soft gamma-ray emission was detected with temporal and spectral behavior typical of that predicted by the synchrotron forward-shock model. The Swift/X-Ray Telescope and the Swift/Ultraviolet Optical Telescope observed the bright afterglow from 1.2 to 48 days after the burst and revealed no evidence of a jet break. The post-break scenario for the afterglow is preferred from our analysis, with a hard underlying electron spectrum and interstellar-medium-like circumburst environment implied. We conclude that, among the multiple reasons investigated, the tight collimation of the jet must have been a key ingredient to produce this unusually bright burst. The inferred jet opening angle of 1.degrees 7-3.degrees 4 results in reasonable values of the collimation-corrected radiated energy and the peak luminosity, which, however, are still at the top of their distributions for such tightly collimated events. We estimate a detection horizon for a similar ultraluminous GRB of z similar to 7.5 for Konus-WIND and z similar to 12 for the Swift/Burst Alert Telescope, which stresses the importance of GRBs as probes of the early Universe. C1 [Frederiks, D. D.; Svinkin, D. S.; Pal'shin, V. D.; Aptekar, R. L.; Golenetskii, S. V.; Mazets, E. P.; Oleynik, Ph. P.; Tsvetkova, A. E.; Ulanov, M. V.; Kokomov, A. A.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Mangano, V.; Burrows, D. N.; Sbarufatti, B.; Siegel, M. H.] Penn State Univ, Dept Astron & Astrophys, College Pk, PA 16801 USA. [Mangano, V.] INAF IASFPA, I-90146 Palermo, Italy. [Oates, S.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Cline, T. L.; Krimm, H. A.; Starr, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pagani, C.] Univ Leicester, Leicester LE1 7RH, Leics, England. [Sbarufatti, B.] INAF OAB, I-23807 Merate, LC, Italy. [Mitrofanov, I. G.; Golovin, D.; Litvak, M. L.; Sanin, A. B.] Moscow Space Res Inst, Moscow 117997, Russia. [Boynton, W.; Fellows, C.; Harshman, K.; Enos, H.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [von Kienlin, A.; Rau, A.; Zhang, X.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Goldstein, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Frederiks, DD (reprint author), AF Ioffe Phys Tech Inst, Politekhnicheskaya 26, St Petersburg 194021, Russia. EM fred@mail.ioffe.ru RI Oleynik, Philipp/C-1104-2014; Svinkin, Dmitry/C-1934-2014; Frederiks, Dmitry/C-7612-2014; Pal'shin, Valentin/F-3973-2014; Ulanov, Mikhail/B-3467-2015; Aptekar, Raphail/B-3456-2015; Golenetskii, Sergey/B-3818-2015; Tsvetkova, Anastasia/B-3858-2015 OI Frederiks, Dmitry/0000-0002-1153-6340; Sbarufatti, Boris/0000-0001-6620-8347; Ulanov, Mikhail/0000-0002-0076-5228; Tsvetkova, Anastasia/0000-0003-0292-6221 FU Russian Space Agency; RFBR [12-02-00032a, 13-02-12017 ofi-m]; NASA [NNX07AR71G, NNX12AE41G]; UK Space Agency; ASI-INAF [I/009/10/0] FX We thank the anonymous referee for comments and suggestions that significantly improved the paper. The Konus-WIND experiment is supported by a Russian Space Agency contract, RFBR grants 12-02-00032a and 13-02-12017 ofi-m. K. H. acknowledges support from NASA grants NNX07AR71G (MESSENGER Participating Scientist Program) and NNX12AE41G (Astrophysics Data Analysis Program). S.R.O. acknowledges support from the UK Space Agency. V. M. and B. S. acknowledge financial contribution from the agreement ASI-INAF I/009/10/0. NR 96 TC 7 Z9 7 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR UNSP 151 DI 10.1088/0004-637X/779/2/151 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200060 ER PT J AU Guerrero, G Smolarkiewicz, PK Kosovichev, AG Mansour, NN AF Guerrero, G. Smolarkiewicz, P. K. Kosovichev, A. G. Mansour, N. N. TI DIFFERENTIAL ROTATION IN SOLAR-LIKE STARS FROM GLOBAL SIMULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: interior; Sun: rotation ID SPHERICAL-SHELL CONVECTION; LARGE-EDDY SIMULATIONS; MERIDIONAL FLOW; TURBULENT CONVECTION; DYNAMO ACTION; MAGNETIC WREATHS; ANGULAR VELOCITY; ZONAL FLOW; MODELS; CYCLES AB To explore the physics of large-scale flows in solar-like stars, we perform three-dimensional anelastic simulations of rotating convection for global models with stratification resembling the solar interior. The numerical method is based on an implicit large-eddy simulation approach designed to capture effects from non-resolved small scales. We obtain two regimes of differential rotation, with equatorial zonal flows accelerated either in the direction of rotation (solar-like) or in the opposite direction (anti-solar). While the models with the solar-like differential rotation tend to produce multiple cells of meridional circulation, the models with anti-solar differential rotation result in only one or two meridional cells. Our simulations indicate that the rotation and large-scale flow patterns critically depend on the ratio between buoyancy and Coriolis forces. By including a sub-adiabatic layer at the bottom of the domain, corresponding to the stratification of a radiative zone, we reproduce a layer of strong radial shear similar to the solar tachocline. Similarly, enhanced super-adiabaticity at the top results in a near-surface shear layer located mainly at lower latitudes. The models reveal a latitudinal entropy gradient localized at the base of the convection zone and in the stable region, which, however, does not propagate across the convection zone. In consequence, baroclinicity effects remain small, and the rotation isocontours align in cylinders along the rotation axis. Our results confirm the alignment of large convective cells along the rotation axis in the deep convection zone and suggest that such "banana-cell" pattern can be hidden beneath the supergranulation layer. C1 [Guerrero, G.; Kosovichev, A. G.] Stanford Univ, HEPL, Stanford, CA 94305 USA. [Smolarkiewicz, P. K.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. [Kosovichev, A. G.] NJIT, Big Bear Solar Observ, Big Bear City, CA 92314 USA. [Mansour, N. N.] NASA, Ames Res Ctr, Mountain View, CA 94040 USA. RP Guerrero, G (reprint author), Stanford Univ, HEPL, 452 Lomita Mall, Stanford, CA 94305 USA. EM gag@stanford.edu; smolar@ecmwf.int; sasha@sun.stanford.edu; nagi.n.mansour@nasa.gov FU NASA [NNX09AG81, NNX09AT36G] FX We thank P. Charbonneau for his valuable comments on this paper and J.-F. Cossette for his important help in the construction of the spherical model. We also thank the anonymous referee for his/her valuable comments that have improved this paper. G.G. acknowledges NSF and NORDITA for travel support. This work was supported by the NASA grants NNX09AG81 and NNX09AT36G. All the simulation here were performed in the NASA cluster Pleiades. NR 61 TC 34 Z9 35 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 176 DI 10.1088/0004-637X/779/2/176 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200085 ER PT J AU Hinkley, S Pueyo, L Faherty, JK Oppenheimer, BR Mamajek, EE Kraus, AL Rice, EL Ireland, MJ David, T Hillenbrand, LA Vasisht, G Cady, E Brenner, D Veicht, A Nilsson, R Zimmerman, N Parry, IR Beichman, C Dekany, R Roberts, JE Roberts, LC Baranec, C Crepp, JR Burruss, R Wallace, JK King, D Zhai, CX Lockhart, T Shao, M Soummer, R Sivaramakrishnan, A Wilson, LA AF Hinkley, Sasha Pueyo, Laurent Faherty, Jacqueline K. Oppenheimer, Ben R. Mamajek, Eric E. Kraus, Adam L. Rice, Emily L. Ireland, Michael J. David, Trevor Hillenbrand, Lynne A. Vasisht, Gautam Cady, Eric Brenner, Douglas Veicht, Aaron Nilsson, Ricky Zimmerman, Neil Parry, Ian R. Beichman, Charles Dekany, Richard Roberts, Jennifer E. Roberts, Lewis C., Jr. Baranec, Christoph Crepp, Justin R. Burruss, Rick Wallace, J. Kent King, David Zhai, Chengxing Lockhart, Thomas Shao, Michael Soummer, Remi Sivaramakrishnan, Anand Wilson, Louis A. TI THE kappa ANDROMEDAE SYSTEM: NEW CONSTRAINTS ON THE COMPANION MASS, SYSTEM AGE, AND FURTHER MULTIPLICITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: adaptive optics; instrumentation: interferometers; planetary systems; planets and satellites: detection; stars: individual (kappa Andromedae); techniques: high angular resolution ID A-TYPE STARS; INTEGRAL FIELD SPECTROGRAPH; L DWARF COMPANION; SOLAR-TYPE STARS; M-CIRCLE-DOT; BROWN DWARF; ADAPTIVE OPTICS; YOUNG STARS; B-STARS; ROTATIONAL VELOCITIES AB kappa Andromedae is a B9IVn star at 52 pc for which a faint substellar companion separated by 55 +/-2 AU was recently announced. In this work, we present the first spectrum of the companion, "kappa And B," using the Project 1640 high-contrast imaging platform. Comparison of our low-resolution YJH-band spectra to empirical brown dwarf spectra suggests an early-L spectral type. Fitting synthetic spectra from PHOENIX model atmospheres to our observed spectrum allows us to constrain the effective temperature to similar to 2000 K as well as place constraints on the companion surface gravity. Further, we use previously reported log(g) and T-eff measurements of the host star to argue that the kappa And system has an isochronal age of 220 +/- 100 Myr, older than the 30 Myr age reported previously. This interpretation of an older age is corroborated by the photometric properties of kappa And B, which appear to be marginally inconsistent with other 10-100 Myr low-gravity L-dwarfs for the spectral type range we derive. In addition, we use Keck aperture masking interferometry combined with published radial velocity measurements to rule out the existence of any tight stellar companions to kappa And A that might be responsible for the system's overluminosity. Further, we show that luminosity enhancements due to a nearly "pole-on" viewing angle coupled with extremely rapid rotation is unlikely. kappa And A is thus consistent with its slightly evolved luminosity class (IV), and we propose here that kappa And, with a revised age of 220 +/- 100 Myr, is an interloper to the 30 Myr Columba association with which it was previously associated. The photometric and spectroscopic evidence for kappa And B combined with our reassessment of the system age implies a substellar companion mass of 50(-13)(+16) M-Jup, consistent with a brown dwarf rather than a planetary-mass companion. C1 [Hinkley, Sasha; David, Trevor; Hillenbrand, Lynne A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Pueyo, Laurent; Soummer, Remi; Sivaramakrishnan, Anand] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Faherty, Jacqueline K.] Univ Chile Cerro Calan, Dept Astron, Las Condes, Chile. [Oppenheimer, Ben R.; Rice, Emily L.; Brenner, Douglas; Veicht, Aaron; Nilsson, Ricky] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Mamajek, Eric E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Kraus, Adam L.] Harvard Smithsonian CfA, Cambridge, MA 02140 USA. [Rice, Emily L.] CUNY Coll Staten Isl, Dept Engn Sci & Phys, Staten Isl, NY 10314 USA. [Ireland, Michael J.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Ireland, Michael J.] Australian Astron Observ, Epping, NSW 1710, Australia. [Vasisht, Gautam; Cady, Eric; Roberts, Jennifer E.; Roberts, Lewis C., Jr.; Burruss, Rick; Wallace, J. Kent; Zhai, Chengxing; Lockhart, Thomas; Shao, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zimmerman, Neil] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Parry, Ian R.; King, David] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Beichman, Charles] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Dekany, Richard; Baranec, Christoph] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Wilson, Louis A.] Washington Univ, St Louis, MO 63130 USA. RP Hinkley, S (reprint author), CALTECH, Dept Astron, 1200 East Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. OI Zimmerman, Neil/0000-0001-5484-1516 FU NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1203023]; Clay Fellowship; NSF [AST-1008908]; NASA OSS grant [NMO7110830/102190]; California Institute of Technology; NASA through the Sagan Fellowship Program; Helge Axson Johnson's foundation; NASA Origins of Solar Systems Grant [NNX13AB03G]; National Science Foundation [AST-0215793, 0334916, 0520822, 0804417, 1245018]; internal Research and Technology Development funds FX We thank the anonymous referee for numerous helpful suggestions. S. H. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1203023. ALK was supported by a Clay Fellowship. E. E. M. is supported by NSF award AST-1008908 and the generous donations of Gabriela Mistral Pisco. G. V. is supported by a NASA OSS grant NMO7110830/102190. L. P. performed this work in part under contract with the California Institute of Technology funded by NASA through the Sagan Fellowship Program. R.N. performed this work with funding through a grant from Helge Axson Johnson's foundation. J.R.C. is supported by NASA Origins of Solar Systems Grant NNX13AB03G. A portion of this work is or was supported by the National Science Foundation under Grant Numbers AST-0215793, 0334916, 0520822, 0804417, and 1245018. A portion of the research in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA and was funded by internal Research and Technology Development funds. Our team is also grateful to the Plymouth Hill Foundation, an anonymous donor, and the efforts of Mike Werner, Paul Goldsmith and Jacob van Zyl. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. Finally, the entire team expresses its sincere gratitude and appreciation for the hard work of the Palomar mountain crew, especially by Steve Kunsman, Mike Doyle, Greg van Idsinga, Bruce Baker, Jean Mueller, Kajsa Peffer, Kevin Rykowski, Carolyn Heffner, and Dan McKenna. This project would be impossible without the flexibility, responsiveness, and dedication of such an effective and motivated staff. NR 121 TC 32 Z9 32 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 153 DI 10.1088/0004-637X/779/2/153 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200062 ER PT J AU Kauffmann, J Pillai, T Goldsmith, PF AF Kauffmann, Jens Pillai, Thushara Goldsmith, Paul F. TI LOW VIRIAL PARAMETERS IN MOLECULAR CLOUDS: IMPLICATIONS FOR HIGH-MASS STAR FORMATION AND MAGNETIC FIELDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; methods: data analysis; stars: formation ID INFRARED-DARK CLOUDS; DENSE CORE POPULATION; COMPETITIVE ACCRETION; STELLAR CLUSTERS; PROTOSTELLAR CANDIDATES; GRAVITATIONAL COLLAPSE; PHYSICAL-PROPERTIES; INITIAL CONDITIONS; DUST CONTINUUM; SIZE RELATION AB Whether or not molecular clouds and embedded cloud fragments are stable against collapse is of utmost importance for the study of the star formation process. Only "supercritical" cloud fragments are able to collapse and form stars. The virial parameter alpha = M-vir/M, which compares the virial mass to the actual mass, provides one way to gauge stability against collapse. Supercritical cloud fragments are characterized by alpha less than or similar to 2, as indicated by a comprehensive stability analysis considering perturbations in pressure and density gradients. Past research has suggested that virial parameters alpha greater than or similar to 2 prevail in clouds. This would suggest that collapse toward star formation is a gradual and relatively slow process and that magnetic fields are not needed to explain the observed cloud structure. Here, we review a range of very recent observational studies that derive virial parameters << 2 and compile a catalog of 1325 virial parameter estimates. Low values of a are in particular observed for regions of high-mass star formation (HMSF). These observations may argue for a more rapid and violent evolution during collapse. This would enable "competitive accretion" in HMSF, constrain some models of "monolithic collapse," and might explain the absence of high-mass starless cores. Alternatively, the data could point at the presence of significant magnetic fields similar to 1 mG at high gas densities. We examine to what extent the derived observational properties might be biased by observational or theoretical uncertainties. For a wide range of reasonable parameters, our conclusions appear to be robust with respect to such biases. C1 [Kauffmann, Jens; Pillai, Thushara] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kauffmann, J (reprint author), CALTECH, Dept Astron, 1200 East Calif Blvd, Pasadena, CA 91125 USA. EM jens.kauffmann@astro.caltech.edu; tpillai@astro.caltech.edu RI Goldsmith, Paul/H-3159-2016 FU NASA Astrophysics Data Analysis program; National Aeronautics and Space Administration FX We are grateful to a very constructive and helpful anonymous referee with attention to detail. The reports significantly helped to improve the readability of the paper and also helped to streamline some of the quantitative arguments presented in this work. We thank Christopher F. McKee, Jonathan Tan, and Matthew Bate for reading and commenting on our manuscript in advance of publication, Marion Wienen for kindly providing data before publication, and Kostas Tassis for enlightening discussions on magnetic fields in star-forming regions. We thank additional colleagues who helped to develop this paper over several stages: Fumitaka Nakamura, Norman Murray, Fred C. Adams, and Tom Megeath. J.K. acknowledges support from the NASA Astrophysics Data Analysis program. This paper benefited from invitations of T. P. and J.K. to the 2012 ASTROWIN workshop at the University of Florida at Gainesville, organized by Jonathan Tan, the 2012 Star Formation Winter School held at the National Astronomical Observatory of Japan (NAOJ) in Tokyo, organized by Fumitaka Nakamura, and Caltech's Red Door Cafe. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. T. P. and J.K. dedicate this paper to the memory of K.S.S. NR 83 TC 45 Z9 46 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 185 DI 10.1088/0004-637X/779/2/185 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200094 ER PT J AU Mandell, AM Haynes, K Sinukoff, E Madhusudhan, N Burrows, A Deming, D AF Mandell, Avi M. Haynes, Korey Sinukoff, Evan Madhusudhan, Nikku Burrows, Adam Deming, Drake TI EXOPLANET TRANSIT SPECTROSCOPY USING WFC3: WASP-12 b, WASP-17 b, AND WASP-19 b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; techniques: photometric; techniques: spectroscopic ID HUBBLE-SPACE-TELESCOPE; EXTRASOLAR GIANT PLANETS; THERMAL PHASE VARIATIONS; HOT-JUPITER WASP-19B; HD 189733B; MU-M; TRANSMISSION SPECTRUM; LIGHT CURVES; SECONDARY ECLIPSE; RETROGRADE ORBIT AB We report an analysis of transit spectroscopy of the extrasolar planets WASP-12 b, WASP-17 b, and WASP-19 b using the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope (HST). We analyze the data for a single transit for each planet using a strategy similar, in certain aspects, to the techniques used by Berta et al., but we extend their methodology to allow us to correct for channel-or wavelength-dependent instrumental effects by utilizing the band-integrated time series and measurements of the drift of the spectrum on the detector over time. We achieve almost photon-limited results for individual spectral bins, but the uncertainties in the transit depth for the band-integrated data are exacerbated by the uneven sampling of the light curve imposed by the orbital phasing of HST's observations. Our final transit spectra for all three objects are consistent with the presence of a broad absorption feature at 1.4 mu m most likely due to water. However, the amplitude of the absorption is less than that expected based on previous observations with Spitzer, possibly due to hazes absorbing in the NIR or non-solar compositions. The degeneracy of models with different compositions and temperature structures combined with the low amplitude of any features in the data preclude our ability to place unambiguous constraints on the atmospheric composition without additional observations with WFC3 to improve the signal-to-noise ratio and/or a comprehensive multi-wavelength analysis. C1 [Mandell, Avi M.; Haynes, Korey] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Haynes, Korey] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Sinukoff, Evan] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Madhusudhan, Nikku] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Mandell, AM (reprint author), NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Avi.Mandell@nasa.gov FU HST through Space Telescope Science Institute [12181]; NASA; NASA ATP [NNX07AG80G]; HST [HST-GO-12181.04-A, HST-GO-12314.03-A]; JPL/Spitzer [1417122, 1348668, 1371432, 1377197]; Yale Center for Astronomy and Astrophysics (YCAA) at Yale university; NASA Astrobiology Institute's Virtual Planetary Laboratory FX We thank the two referees and the editor for their insightful comments and suggestions for improvements to the manuscript. Support for this work was provided as part of the HST Observing Program # 12181 through a grant from the Space Telescope Science Institute, as well as a grant from the NASA Astrophysics Data Analysis Program. A. B. acknowledges support in part under NASA ATP grant NNX07AG80G, HST grants HST-GO-12181.04-A and HST-GO-12314.03-A, and JPL/Spitzer Agreements 1417122, 1348668, 1371432, and 1377197. N. M. thanks the Yale Center for Astronomy and Astrophysics (YCAA) at Yale university for support through the YCAA postdoctoral prize fellowship. D. D. acknowledges support from the NASA Astrobiology Institute's Virtual Planetary Laboratory. NR 71 TC 43 Z9 43 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 128 DI 10.1088/0004-637X/779/2/128 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200038 ER PT J AU Morii, M Tomida, H Kimura, M Suwa, F Negoro, H Serino, M Kennea, JA Page, KL Curran, PA Walter, FM Kuin, NPM Pritchard, T Nakahira, S Hiroi, K Usui, R Kawai, N Osborne, JP Mihara, T Sugizaki, M Gehrels, N Kohama, M Kotani, T Matsuoka, M Nakajima, M Roming, PWA Sakamoto, T Sugimori, K Tsuboi, Y Tsunemi, H Ueda, Y Ueno, S Yoshida, A AF Morii, M. Tomida, H. Kimura, M. Suwa, F. Negoro, H. Serino, M. Kennea, J. A. Page, K. L. Curran, P. A. Walter, F. M. Kuin, N. P. M. Pritchard, T. Nakahira, S. Hiroi, K. Usui, R. Kawai, N. Osborne, J. P. Mihara, T. Sugizaki, M. Gehrels, N. Kohama, M. Kotani, T. Matsuoka, M. Nakajima, M. Roming, P. W. A. Sakamoto, T. Sugimori, K. Tsuboi, Y. Tsunemi, H. Ueda, Y. Ueno, S. Yoshida, A. TI EXTRAORDINARY LUMINOUS SOFT X-RAY TRANSIENT MAXI J0158-744 AS AN IGNITION OF A NOVA ON A VERY MASSIVE O-Ne WHITE DWARF SO ASTROPHYSICAL JOURNAL LA English DT Article DE Magellanic Clouds; novae, cataclysmic variables; stars: individual (MAXI J0158-744); white dwarfs; X-rays: bursts; X-rays: individual (MAXI J0158-744) ID SMALL-MAGELLANIC-CLOUD; IN-ORBIT PERFORMANCE; SLIT CAMERA GSC; CLASSICAL NOVAE; H-I; ISS; ATMOSPHERES; TELESCOPE; OUTBURST; CALIBRATION AB We present the observation of an extraordinary luminous soft X-ray transient, MAXI J0158-744, by the Monitor of All-sky X-ray Image (MAXI) on 2011 November 11. This transient is characterized by a soft X-ray spectrum, a short duration (1.3 x 10(3) s < Delta T-d < 1.10 x 10(4) s), a rapid rise (<5.5 x 10(3) s), and a huge peak luminosity of 2 x 10(40) erg s(-1) in 0.7-7.0 keV band. With Swift observations and optical spectroscopy from the Small and Moderate Aperture Research Telescope System, we confirmed that the transient is a nova explosion, on a white dwarf in a binary with a Be star, located near the Small Magellanic Cloud. An early turn-on of the super-soft X-ray source (SSS) phase (<0.44 days), the short SSS phase duration of about one month, and a 0.92 keV neon emission line found in the third MAXI scan, 1296 s after the first detection, suggest that the explosion involves a small amount of ejecta and is produced on an unusually massive O-Ne white dwarf close to, or possibly over, the Chandrasekhar limit. We propose that the huge luminosity detected with MAXI was due to the fireball phase, a direct manifestation of the ignition of the thermonuclear runaway process in a nova explosion. C1 [Morii, M.; Serino, M.; Mihara, T.; Sugizaki, M.; Matsuoka, M.] RIKEN, MAXI Team, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. [Tomida, H.; Kimura, M.; Nakahira, S.; Kohama, M.; Ueno, S.] Japan Aerosp Explorat Agcy, ISS Sci Project Off, Inst Space & Astronaut Sci, Tsukuba, Ibaraki 3058505, Japan. [Suwa, F.; Negoro, H.] Nihon Univ, Dept Phys, Chiyoda Ku, Tokyo 1018308, Japan. [Kennea, J. A.; Pritchard, T.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Page, K. L.; Osborne, J. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Curran, P. A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Walter, F. M.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Kuin, N. P. M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Hiroi, K.; Ueda, Y.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Usui, R.; Kawai, N.; Sugimori, K.] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kotani, T.] Waseda Univ, Org Univ Res Initiat, Shinjuku Ku, Tokyo 1620044, Japan. [Nakajima, M.] Nihon Univ, Sch Dent Matsudo, Matsudo, Chiba 2718587, Japan. [Roming, P. W. A.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78228 USA. [Sakamoto, T.; Yoshida, A.] Aoyama Gakuin Univ, Dept Math & Phys, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan. [Tsuboi, Y.] Chuo Univ, Dept Phys, Fac Sci & Engn, Bunkyo Ku, Tokyo 1128551, Japan. [Tsunemi, H.] Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. RP Morii, M (reprint author), RIKEN, MAXI Team, Inst Phys & Chem Res, 2-1 Hirosawa, Wako, Saitama 3510198, Japan. RI Curran, Peter/B-5293-2013; Mihara, Tatehiro/C-5536-2017 OI Curran, Peter/0000-0003-3003-4626; Mihara, Tatehiro/0000-0002-6337-7943 FU Ministry of Education, Culture, Sports, Science and Technology (MEXT); Global-COE from MEXT "The Next Generation of Physics, Spun from Universality and Emergence"; Global-COE from MEXT "Nanoscience and Quantum Physics"; UK Space Agency; NASA; Australian Research Council [DP120102393]; [23740147]; [19047001] FX We are grateful to the members of the MAXI and Swift operation teams. We thank K. Asano, I. Hachisu, D. N. Burrows, D. Takei, S. R. Kulkarni, Y. Maeda, and T. Shigeyama for discussions and comments. This research was partially supported by the Ministry of Education, Culture, Sports, Science and Technology (MEXT), Grant-in-Aid No. 23740147, 19047001, and Global-COE from MEXT "The Next Generation of Physics, Spun from Universality and Emergence" and "Nanoscience and Quantum Physics." J. P. O., K. L. P. and N. P. M. K. acknowledge financial support from the UK Space Agency. J. A. K. acknowledges support from NASA. This work was supported by the Australian Research Council Discovery Projects funding scheme (project number DP120102393). NR 61 TC 8 Z9 8 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR UNSP 118 DI 10.1088/0004-637X/779/2/118 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200028 ER PT J AU Pivato, G Hewitt, JW Tibaldo, L Acero, F Ballet, J Brandt, TJ de Palma, F Giordano, F Janssen, GH Johannesson, G Smith, DA AF Pivato, G. Hewitt, J. W. Tibaldo, L. Acero, F. Ballet, J. Brandt, T. J. de Palma, F. Giordano, F. Janssen, G. H. Johannesson, G. Smith, D. A. TI FERMI LAT AND WMAP OBSERVATIONS OF THE SUPERNOVA REMNANT HB 21 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; ISM: individual objects (HB 21); radiation mechanisms: non-thermal ID LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; SPECTRAL INDEX VARIATIONS; MOLECULAR CLOUDS; COSMIC-RAYS; SPACE-TELESCOPE; RX J1713.7-3946; SOURCE CATALOG; CYGNUS LOOP; HIGH-ENERGY AB We present the analysis of Fermi Large Area Telescope gamma-ray observations of HB 21 (G89.0+4.7). We detect significant gamma-ray emission associated with the remnant: the flux >100 MeV is 9.4 +/- 0.8 (stat) +/- 1.6 (syst) x 10(-11) erg cm(-2) s(-1). HB 21 is well modeled by a uniform disk centered at l = 88 degrees.75 +/- 0 degrees.04, b = +4 degrees.65 +/- 0 degrees.06 with a radius of 1 degrees.19 +/- 0 degrees.06. The gamma-ray spectrum shows clear evidence of curvature, suggesting a cutoff or break in the underlying particle population at an energy of a few GeV. We complement gamma-ray observations with the analysis of the WMAP 7 yr data from 23 to 93 GHz, achieving the first detection of HB 21 at these frequencies. In combination with archival radio data, the radio spectrum shows a spectral break, which helps to constrain the relativistic electron spectrum, and, in turn, parameters of simple non-thermal radiation models. In one-zone models multiwavelength data favor the origin of gamma rays from nucleon-nucleon collisions. A single population of electrons cannot produce both gamma rays through bremsstrahlung and radio emission through synchrotron radiation. Apredominantly inverse-Compton origin of the gamma-ray emission is disfavored because it requires lower interstellar densities than are inferred for HB 21. In the hadronic-dominated scenarios, accelerated nuclei contribute a total energy of similar to 3 x 10(49) erg, while, in a two-zone bremsstrahlung-dominated scenario, the total energy in accelerated particles is similar to 1 x 10(49) erg. C1 [Pivato, G.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Pivato, G.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Hewitt, J. W.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA. [Hewitt, J. W.; Acero, F.; Brandt, T. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tibaldo, L.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Tibaldo, L.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Ballet, J.] CEA IRFU CNRS Univ Paris Diderot, Lab AIM, Serv Astrophys, CEA Saclay, F-91191 Gif Sur Yvette, France. [de Palma, F.; Giordano, F.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [de Palma, F.; Giordano, F.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Janssen, G. H.] Univ Manchester, Manchester M13 9PL, Lancs, England. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Smith, D. A.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS IN2P3, F-33175 Gradignan, France. RP Pivato, G (reprint author), Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. EM giovanna.pivato@pd.infn.it; john.w.hewitt@nasa.gov; ltibaldo@slac.stanford.edu RI Johannesson, Gudlaugur/O-8741-2015; OI Johannesson, Gudlaugur/0000-0003-1458-7036; Giordano, Francesco/0000-0002-8651-2394 FU Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; Science and Technology Facilities Council of the United Kingdom FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT and scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France.; The Lovell Telescope is owned and operated by the University of Manchester as part of the Jodrell Bank Centre for Astrophysics with support from the Science and Technology Facilities Council of the United Kingdom. The Westerbork Synthesis Radio Telescope is operated by Netherlands Foundation for Radio Astronomy, ASTRON. NR 71 TC 10 Z9 10 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 179 DI 10.1088/0004-637X/779/2/179 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200088 ER PT J AU Savani, NP Vourlidas, A Shiota, D Linton, MG Kusano, K Lugaz, N Rouillard, AP AF Savani, N. P. Vourlidas, A. Shiota, D. Linton, M. G. Kusano, K. Lugaz, N. Rouillard, A. P. TI A PLASMA beta TRANSITION WITHIN A PROPAGATING FLUX ROPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar-terrestrial relations; Sun: coronal mass ejections (CMEs); Sun: heliosphere ID CORONAL MASS EJECTION; STRUCTURED SOLAR-WIND; INTERPLANETARY MAGNETIC-FIELD; CLOUDS; EARTH; RECONSTRUCTION; EVOLUTION; DISTORTION; HELICITY; MODEL AB We present a 2.5 dimensional magnetohydrodynamic simulation of a magnetic flux rope (FR) propagating in the heliosphere and investigate the cause of the observed sharp plasma beta transition. Specifically, we consider a strong internal magnetic field and an explosive fast start, such that the plasma beta is significantly lower in the FR than in the sheath region that is formed ahead. This leads to an unusual FR morphology in the first stage of propagation, while the more traditional view (e. g., from space weather simulations like Enlil) of a pancake-shaped FR is observed as it approaches 1 AU. We investigate how an equipartition line, defined by a magnetic Weber number, surrounding a core region of a propagating FR, can demarcate a boundary layer where there is a sharp transition in the plasma beta. The substructure affects the distribution of toroidal flux, with the majority of the flux remaining in a small core region that maintains a quasi-cylindrical structure. We quantitatively investigate a locus of points where the kinetic energy density of the relative inflow field is equal to the energy density of the transverse magnetic field (i.e., effective tension force). The simulation provides compelling evidence that at all heliocentric distances the distribution of toroidal magnetic flux away from the FR axis is not linear, with 80% of the toroidal flux occurring within 40% of the distance from the FR axis. Thus, our simulation displays evidence that the competing ideas of a pancaking structure observed remotely can coexist with a quasi-cylindrical magnetic structure seen in situ. C1 [Savani, N. P.] George Mason Univ, Fairfax, VA 22030 USA. [Vourlidas, A.; Linton, M. G.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Shiota, D.] RIKEN, Adv Sci Inst, Computat Astrophys Lab, Wako, Saitama 3510198, Japan. [Kusano, K.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Lugaz, N.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Lugaz, N.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Rouillard, A. P.] Univ Toulouse UPS, Inst Rech Astrophys & Plantol, Toulouse, France. [Savani, N. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kusano, K.] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa 2360001, Japan. [Rouillard, A. P.] CNRS, UMR 5277, Toulouse, France. RP Savani, NP (reprint author), George Mason Univ, Fairfax, VA 22030 USA. RI Lugaz, Noe/C-1284-2008; Savani, Neel/G-4066-2014; Vourlidas, Angelos/C-8231-2009 OI Lugaz, Noe/0000-0002-1890-6156; Savani, Neel/0000-0002-1916-7877; Vourlidas, Angelos/0000-0002-8164-5948 FU NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program; NASA; office of Naval Research FX N.P.S. was partially supported by the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program, administered by the UCAR Visiting Scientist Programs and hosted by the Naval Research Laboratory. A. V. and M. G. L. were supported by NASA and the office of Naval Research. The numerical calculations were performed using the supercomputing cluster at the Solar-Terrestrial Environment Laboratory, Nagoya University. NR 56 TC 4 Z9 4 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 142 DI 10.1088/0004-637X/779/2/142 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200051 ER PT J AU Schmit, DJ Gibson, S Luna, M Karpen, J Innes, D AF Schmit, Donald J. Gibson, S. Luna, M. Karpen, J. Innes, D. TI PROMINENCE MASS SUPPLY AND THE CAVITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; Sun: filaments, prominences ID MAGNETIC-FIELD GEOMETRY; SOLAR CORONAL LOOPS; THERMAL NONEQUILIBRIUM; QUIESCENT PROMINENCES; DYNAMICS; MODEL; CHROMOSPHERE; CONDENSATION; INSTABILITY; STABILITY AB A prevalent but untested paradigm is often used to describe the prominence-cavity system: the cavity is under-dense because it is evacuated by supplying mass to the condensed prominence. The thermal non-equilibrium (TNE) model of prominence formation offers a theoretical framework to predict the thermodynamic evolution of the prominence and the surrounding corona. We examine the evidence for a prominence-cavity connection by comparing the TNE model with diagnostics of dynamic extreme ultraviolet (EUV) emission surrounding the prominence, specifically prominence horns. Horns are correlated extensions of prominence plasma and coronal plasma which appear to connect the prominence and cavity. The TNE model predicts that large-scale brightenings will occur in the Solar Dynamics Observatory Atmospheric Imaging Assembly 171 angstrom bandpass near the prominence that are associated with the cooling phase of condensation formation. In our simulations, variations in the magnitude of footpoint heating lead to variations in the duration, spatial scale, and temporal offset between emission enhancements in the other EUV bandpasses. While these predictions match well a subset of the horn observations, the range of variations in the observed structures is not captured by the model. We discuss the implications of our one-dimensional loop simulations for the three-dimensional time-averaged equilibrium in the prominence and the cavity. Evidence suggests that horns are likely caused by condensing prominence plasma, but the larger question of whether this process produces a density-depleted cavity requires a more tightly constrained model of heating and better knowledge of the associated magnetic structure. C1 [Schmit, Donald J.; Innes, D.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Gibson, S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Luna, M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Luna, M.] Univ la Laguna, Dept Astrofis, E-38206 San Cristobal de la Laguna, Tenerife, Spain. [Karpen, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Schmit, DJ (reprint author), Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. FU Max-Planck/Princeton Center for Plasma Physics; National Science Foundation; Spanish Ministry of Economy [AYA2011-24808, CSD2007-00050]; FP7 European Research Council [277829] FX This work was partially funded by the Max-Planck/Princeton Center for Plasma Physics. The National Center for Atmospheric Research is funded by the National Science Foundation. M. L. gratefully acknowledges partial financial support by the Spanish Ministry of Economy through projects AYA2011-24808 and CSD2007-00050. This work contributes to the deliverables identified in FP7 European Research Council grant agreement 277829, "Magnetic connectivity through the Solar Partially Ionized Atmosphere", whose PI is E. Khomenko. NR 44 TC 4 Z9 4 U1 2 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR UNSP 156 DI 10.1088/0004-637X/779/2/156 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200065 ER PT J AU Walton, DJ Fuerst, F Harrison, F Stern, D Bachetti, M Barret, D Bauer, F Boggs, SE Christensen, FE Craig, WW Fabian, AC Grefenstette, BW Hailey, CJ Madsen, KK Miller, JM Ptak, A Rana, V Webb, NA Zhang, WW AF Walton, D. J. Fuerst, F. Harrison, F. Stern, D. Bachetti, M. Barret, D. Bauer, F. Boggs, S. E. Christensen, F. E. Craig, W. W. Fabian, A. C. Grefenstette, B. W. Hailey, C. J. Madsen, K. K. Miller, J. M. Ptak, A. Rana, V. Webb, N. A. Zhang, W. W. TI AN EXTREMELY LUMINOUS AND VARIABLE ULTRALUMINOUS X-RAY SOURCE IN THE OUTSKIRTS OF CIRCINUS OBSERVED WITH NuSTAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; X-rays: binaries; X-rays: individual (Circinus ULX5) ID MASS BLACK-HOLES; ACTIVE GALACTIC NUCLEI; HOLMBERG IX X-1; SPECTRAL STATE TRANSITIONS; SPITZER-SPACE-TELESCOPE; PHOTON IMAGING CAMERA; COOL ACCRETION DISKS; NGC 1313 X-1; XMM-NEWTON; ESO 243-49 AB Following a serendipitous detection with the Nuclear Spectroscopic Telescope Array (NuSTAR), we present a multi-epoch spectral and temporal analysis of an extreme ultraluminous X-ray source (ULX) located in the outskirts of the Circinus galaxy, hereafter Circinus ULX5, including coordinated XMM-Newton+NuSTAR follow-up observations. The NuSTAR data presented here represent one of the first instances of a ULX reliably detected at hard (E > 10 keV) X-rays. Circinus ULX5 is variable on long time scales by at least a factor of similar to 5 in flux, and was caught in a historically bright state during our 2013 observations (0.3-30.0 keV luminosity of 1.6 x 10(40) erg s(-1)). During this epoch, the source displayed a curved 3-10 keV spectrum, broadly similar to other bright ULXs. Although pure thermal models result in a high energy excess in the NuSTAR data, this excess is too weak to be modeled with the disk reflection interpretation previously proposed to explain the 3-10 keV curvature in other ULXs. In addition to flux variability, clear spectral variability is also observed. While in many cases the interpretation of spectral components in ULXs is uncertain, the spectral and temporal properties of all the high quality data sets currently available strongly support a simple disk-corona model reminiscent of that invoked for Galactic binaries, with the accretion disk becoming more prominent as the luminosity increases. However, although the disk temperature and luminosity are well correlated across all time scales currently probed, the observed luminosity follows L proportional to T1.70+/-0.17, flatter than expected for simple blackbody radiation. The spectral variability displayed here is highly reminiscent of that observed from known Galactic black hole binaries (BHBs) at high luminosities. This comparison implies a black hole mass of similar to 90 M-circle dot for Circinus ULX5. However, given the diverse behavior observed from Galactic BHB accretion disks, this mass estimate is still uncertain. Finally, the limits placed on any undetected iron absorption features with the 2013 data set imply that we are not viewing the central regions of Circinus ULX5 through any extreme super-Eddington outflow. C1 [Walton, D. J.; Fuerst, F.; Harrison, F.; Stern, D.; Grefenstette, B. W.; Madsen, K. K.; Rana, V.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bachetti, M.; Barret, D.; Webb, N. A.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Bachetti, M.; Barret, D.; Webb, N. A.] IRAP, CNRS, F-31028 Toulouse 4, France. [Bauer, F.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, F.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Ptak, A.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Walton, DJ (reprint author), CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337; Rana, Vikram/0000-0003-1703-8796 FU NASA; XMM-Newton; ESA Member States; Suzaku observatory; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024, Anillo ACT1101]; Centre National DEtudes Spatiales (CNES) FX The authors thank Koji Mukai for useful discussion regarding Galactic CVs, and Rubens Reis for discussion regarding Galactic BHBs. This research has made use of data obtained with the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA, XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and the Suzaku observatory, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). In addition, this research has also made use of data obtained from NASA's Swift, Chandra, and Spitzer satellites. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA). We also made use of the NASA/IPAC Extragalactic Database (NED), which is operated by JPL, Caltech, under contract with NASA. Some of the figures included in this work have been produced with the Veusz plotting package: http://home.gna.org/veusz, written and maintained by Jeremy Sanders. F. E. B. acknowledges support from Basal-CATA (PFB-06/2007) and CONICYT-Chile (under grants FONDECYT 1101024 and Anillo ACT1101). M. B. wishes to acknowledge the support from the Centre National DEtudes Spatiales (CNES). NR 126 TC 37 Z9 37 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 148 DI 10.1088/0004-637X/779/2/148 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200057 ER PT J AU Wuyts, S Schreiber, NMF Nelson, EJ van Dokkum, PG Brammer, G Chang, YY Faber, SM Ferguson, HC Franx, M Fumagalli, M Genzel, R Grogin, NA Kocevski, DD Koekemoer, AM Lundgren, B Lutz, D McGrath, EJ Momcheva, I Rosario, D Skelton, RE Tacconi, LJ van der Wel, A Whitaker, KE AF Wuyts, Stijn Schreiber, Natascha M. Foerster Nelson, Erica J. van Dokkum, Pieter G. Brammer, Gabe Chang, Yu-Yen Faber, Sandra M. Ferguson, Henry C. Franx, Marijn Fumagalli, Mattia Genzel, Reinhard Grogin, Norman A. Kocevski, Dale D. Koekemoer, Anton M. Lundgren, Britt Lutz, Dieter McGrath, Elizabeth J. Momcheva, Ivelina Rosario, David Skelton, Rosalind E. Tacconi, Linda J. van der Wel, Arjen Whitaker, Katherine E. TI A CANDELS-3D-HST SYNERGY: RESOLVED STAR FORMATION PATTERNS AT 0.7 < z < 1.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: stellar content; galaxies: structure; stars: formation ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; LOW ANGULAR-MOMENTUM; ULTRALUMINOUS INFRARED GALAXIES; SIMILAR-TO 2; HOST GALAXIES; HIGH-REDSHIFT; COSMOLOGICAL SIMULATIONS; FORMING GALAXIES; COLD FLOWS AB We analyze the resolved stellar populations of 473 massive star-forming galaxies at 0.7 < z < 1.5, with multi-wavelength broadband imaging from CANDELS and H alpha surface brightness profiles at the same kiloparsec resolution from 3D-HST. Together, this unique data set sheds light on how the assembled stellar mass is distributed within galaxies, and where new stars are being formed. We find the H alpha morphologies to resemble more closely those observed in the ACS I band than in the WFC3 H band, especially for the larger systems. We next derive a novel prescription for H alpha dust corrections, which accounts for extra extinction toward H II regions. The prescription leads to consistent star formation rate (SFR) estimates and reproduces the observed relation between the H alpha/UV luminosity ratio and visual extinction, on both a pixel-by-pixel and a galaxy-integrated level. We find the surface density of star formation to correlate with the surface density of assembled stellar mass for spatially resolved regions within galaxies, akin to the so-called "main sequence of star formation" established on a galaxy-integrated level. Deviations from this relation toward lower equivalent widths are found in the inner regions of galaxies. Clumps and spiral features, on the other hand, are associated with enhanced H alpha equivalent widths, bluer colors, and higher specific SFRs compared to the underlying disk. Their H alpha/UV luminosity ratio is lower than that of the underlying disk, suggesting that the ACS clump selection preferentially picks up those regions of elevated star formation activity that are the least obscured by dust. Our analysis emphasizes that monochromatic studies of galaxy structure can be severely limited by mass-to-light ratio variations due to dust and spatially inhomogeneous star formation histories. C1 [Wuyts, Stijn; Schreiber, Natascha M. Foerster; Genzel, Reinhard; Lutz, Dieter; Rosario, David; Tacconi, Linda J.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Nelson, Erica J.; van Dokkum, Pieter G.; Momcheva, Ivelina] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Brammer, Gabe] European So Observ, Santiago 19, Chile. [Chang, Yu-Yen; van der Wel, Arjen] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Faber, Sandra M.] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ferguson, Henry C.; Grogin, Norman A.; Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Franx, Marijn; Fumagalli, Mattia] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Kocevski, Dale D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Lundgren, Britt] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [McGrath, Elizabeth J.] Colby Coll, Dept Phys & Astron, Waterville, ME USA. [Skelton, Rosalind E.] S African Astron Observ, ZA-7925 Cape Town, South Africa. [Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Wuyts, S (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312,Giessenbachstr, D-85741 Garching, Germany. EM swuyts@mpe.mpg.de RI Skelton, Rosalind/S-1845-2016; OI Skelton, Rosalind/0000-0001-7393-3336; Koekemoer, Anton/0000-0002-6610-2048 FU NSF [AST-0847696, AST 1107675, AST-0607819]; Aspen Center for Physics; NASA [ATP NNX10AC84G, ATP NNX08AG84G, NNX07AH03G]; SAO [TM1-12007X]; Marie Curie Career Integration grant [PCIG10-GA-2011-303609]; Grainger Foundation FX Simulations were run using computer resources and technical support from NAS. J. B. acknowledges support from NSF CAREER award AST-0847696, as well as support from the Aspen Center for Physics. M. V. acknowledges funding support from NASA, through Award Number ATP NNX10AC84G; from SAO, through Award Number TM1-12007X, from NSF, through Award Number AST 1107675, and from a Marie Curie Career Integration grant (PCIG10-GA-2011-303609). F. G. acknowledges support from a NSF grant AST-0607819 and NASA ATP NNX08AG84G. J. B. and T. Q. acknowledge support from NASA Grant NNX07AH03G. A. B. acknowledges support from The Grainger Foundation. The authors thank Kelly Holley-Bockelmann, Ferah Munshi, and the anonymous referee for their helpful comments. NR 101 TC 62 Z9 63 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 135 DI 10.1088/0004-637X/779/2/135 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200045 ER PT J AU Zeimann, GR Stanford, SA Brodwin, M Gonzalez, AH Mancone, C Snyder, GF Stern, D Eisenhardt, P Dey, A Moustakas, J AF Zeimann, Gregory R. Stanford, S. A. Brodwin, Mark Gonzalez, Anthony H. Mancone, Conor Snyder, Gregory F. Stern, Daniel Eisenhardt, Peter Dey, Arjun Moustakas, John TI H alpha STAR FORMATION RATES OF z > 1 GALAXY CLUSTERS IN THE IRAC SHALLOW CLUSTER SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: evolution; galaxies: high-redshift ID FUNDAMENTAL METALLICITY RELATION; HUBBLE-SPACE-TELESCOPE; WIDE-FIELD SURVEY; X-RAY SURVEY; FORMING GALAXIES; RED SEQUENCE; STELLAR MASS; DENSITY RELATION; DUST EXTINCTION; LENSED GALAXIES AB We present Hubble Space Telescope near-IR spectroscopy for 18 galaxy clusters at 1.0 < z < 1.5 in the IRAC Shallow Cluster Survey. We use Wide Field Camera 3 grism data to spectroscopically identify H alpha emitters in both the cores of galaxy clusters as well as in field galaxies. We find a large cluster-to-cluster scatter in the star formation rates within a projected radius of 500 kpc, and many of our clusters (similar to 60%) have significant levels of star formation within a projected radius of 200 kpc. A stacking analysis reveals that dust reddening in these star-forming galaxies is positively correlated with stellar mass and may be higher in the field than the cluster at a fixed stellar mass. This may indicate a lower amount of gas in star-forming cluster galaxies than in the field population. Also, H alpha equivalent widths of star-forming galaxies in the cluster environment are still suppressed below the level of the field. This suppression is most significant for lower mass galaxies (log M-* < 10.0 M-circle dot). We therefore conclude that environmental effects are still important at 1.0 < z < 1.5 for star-forming galaxies in galaxy clusters with log M-* less than or similar to 10.0 M-circle dot. C1 [Zeimann, Gregory R.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Zeimann, Gregory R.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Brodwin, Mark] Univ Missouri, Kansas City, MO 64110 USA. [Gonzalez, Anthony H.; Mancone, Conor] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Snyder, Gregory F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stern, Daniel; Eisenhardt, Peter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. RP Zeimann, GR (reprint author), Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA. FU National Science Foundation [AST-0708490]; NASA [NAS 5-26555]; JPL/Caltech; NASA through Space Telescope Science Institute [10496, 11002, 11597, 11663]; U.S. Department of Energy [W-7405-ENG-48] FX A.H.G. acknowledges support from the National Science Foundation through grant AST-0708490. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Support for HST programs 10496, 11002, 11597, and 11663 were provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This work makes use of image data from the NOAO Deep Wide-Field Survey (NDWFS) as distributed by the NOAO Science Archive. NOAO is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under a cooperative agreement with the National Science Foundation.; We thank Matt Ashby for creating the IRAC catalogs for SDWFS, Buell Jannuzi for his work on the NDWFS, Michael Brown for combining the NDWFS with SDWFS catalogs, and Steve Murray and the XBootes team for obtaining the Chandra data in the Bootes field. This paper would not have been possible without the efforts of the support staffs of the Spitzer Space Telescope, Hubble Space Telescope, and Chandra X-ray Observatory. The work by S. A. S. at LLNL was performed under the auspices of the U.S. Department of Energy under Contract No. W-7405-ENG-48. NR 66 TC 20 Z9 20 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2013 VL 779 IS 2 AR 137 DI 10.1088/0004-637X/779/2/137 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268RC UT WOS:000328187200046 ER PT J AU Zheng, M Chen, XM Park, C Fay, CC Pugno, NM Ke, CH AF Zheng, Meng Chen, Xiaoming Park, Cheol Fay, Catharine C. Pugno, Nicola M. Ke, Changhong TI Nanomechanical cutting of boron nitride nanotubes by atomic force microscopy SO NANOTECHNOLOGY LA English DT Article ID WALLED CARBON NANOTUBES; CHEMICAL-VAPOR-DEPOSITION; LENGTH CONTROL; FRACTURE-MECHANICS; CONTACT PROBLEM; ELECTRON-BEAM; GROWTH; MANIPULATION; DEFORMATIONS AB The length of nanotubes is a critical structural parameter for the design and manufacture of nanotube-based material systems and devices. High-precision length control of nanotubes by means of mechanical cutting using a scriber has not materialized due to the lack of the knowledge of the appropriate cutting conditions and the tube failure mechanism. In this paper, we present a quantitative nanomechanical study of the cutting of individual boron nitride nanotubes (BNNTs) using atomic force microscopy (AFM) probes. In our nanotube cutting measurements, a nanotube standing still on a flat substrate was laterally scribed by an AFM tip. The tip-tube collision force deformed the tube, and eventually fractured the tube at the collision site by increasing the cutting load. The mechanical response of nanotubes during the tip-tube collision process and the roles of the scribing velocity and the frictional interaction on the tip-tube collision contact in cutting nanotubes were quantitatively investigated by cutting double-walled BNNTs of 2.26-4.28 nm in outer diameter. The fracture strength of BNNTs was also quantified based on the measured collision forces and their structural configurations using contact mechanics theories. Our analysis reports fracture strengths of 9.1-15.5 GPa for the tested BNNTs. The nanomechanical study presented in this paper demonstrates that the AFM-based nanomechanical cutting technique not only enables effective control of the length of nanotubes with high precision, but is also promising as a new nanomechanical testing technique for characterizing the mechanical properties of tubular nanostructures. C1 [Zheng, Meng; Chen, Xiaoming; Ke, Changhong] SUNY Binghamton, Dept Mech Engn, Binghamton, NY 13902 USA. [Park, Cheol] Natl Inst Aerosp, Hampton, VA 23666 USA. [Park, Cheol] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA. [Fay, Catharine C.] NASA Langley Res Ctr, Hampton, VA 23681 USA. [Pugno, Nicola M.] Univ Trento, Dept Civil Environm & Mech Engn, I-38123 Trento, Italy. RP Zheng, M (reprint author), SUNY Binghamton, Dept Mech Engn, Binghamton, NY 13902 USA. EM cke@binghamton.edu RI Pugno, Nicola/C-2289-2014; Zheng, Meng/D-3985-2011; Ke, Changhong/C-4064-2008; CHEN, XIAOMING/A-1377-2016 OI Zheng, Meng/0000-0002-6769-3054; NR 73 TC 5 Z9 5 U1 0 U2 26 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0957-4484 EI 1361-6528 J9 NANOTECHNOLOGY JI Nanotechnology PD DEC 20 PY 2013 VL 24 IS 50 AR 505719 DI 10.1088/0957-4484/24/50/505719 PG 11 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA 272RU UT WOS:000328478900034 PM 24285263 ER PT J AU Zahnle, KJ Catling, DC Claire, MW AF Zahnle, Kevin J. Catling, David C. Claire, Mark W. TI The rise of oxygen and the hydrogen hourglass SO CHEMICAL GEOLOGY LA English DT Article DE Oxygen; Hydrogen escape; Atmospheric evolution; Oxygenation; Evolution ID MULTIPLE SULFUR ISOTOPES; EARTHS EARLY ATMOSPHERE; GREAT OXIDATION EVENT; ARCHEAN ATMOSPHERE; MANTLE REDOX; TERRESTRIAL PLANETS; EVOLUTION; RECORD; STATE; ENVIRONMENTS AB Oxygenic photosynthesis appears to be necessary for an oxygen-rich atmosphere like Earth's. But available geological and geochemical evidence suggest that at least 200 Myr, and possibly more than 700 Myr, elapsed between the advent of oxygenic photosynthesis and the establishment of an oxygen atmosphere. The interregnum implies that at least one other necessary condition for O-2 needed to be met. Here we argue that the second condition was the oxidation of the surface and crust to the point where O-2 became more stable than competing reduced gases such as CH4. The cause of Earth's surface oxidation would be the same cause as it is for other planets with oxidized surfaces: hydrogen escape to space. The duration of the interregnum would have been determined by the rate of hydrogen escape and by the size of the reduced reservoir that needed to be oxidized before O-2 became favored. We suggest that continental growth has been influenced by hydrogen escape, and we speculate that, if there must be an external bias to biological evolution, hydrogen escape can be that bias. Published by Elsevier B.V. C1 [Zahnle, Kevin J.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Catling, David C.] Univ Washington, Dept Earth & Space Sci, Astrobiol Program, Seattle, WA 98195 USA. [Claire, Mark W.] Univ St Andrews, St Andrews KY16 8YH, Fife, Scotland. [Claire, Mark W.] Blue Marble Space Inst Sci, Seattle, WA USA. RP Zahnle, KJ (reprint author), NASA, Ames Res Ctr, Div Space Sci, MS 245-3, Moffett Field, CA 94035 USA. EM Kevin.J.Zahnle@NASA.gov; dcatling@uw.edu; mc229@st-andrews.ac.uk OI Catling, David/0000-0001-5646-120X FU NASA Exobiology Program; NASA National Astrobiology Institute; NASA Exobiology [NNX10AQ90G] FX The authors thank A. Bekker, R. Buick, J. Farquhar, J. Kasting, L. Kump, and E. Stuecken for insightful reviews, data, or both. The authors thank the NASA Exobiology Program and the NASA National Astrobiology Institute for support of this work. DCC acknowledges support from NASA Exobiology grant number NNX10AQ90G. NR 102 TC 7 Z9 7 U1 4 U2 50 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2541 EI 1878-5999 J9 CHEM GEOL JI Chem. Geol. PD DEC 20 PY 2013 VL 362 SI SI BP 26 EP 34 DI 10.1016/j.chemgeo.2013.08.004 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 262UV UT WOS:000327764300004 ER PT J AU Franz, HB Danielache, SO Farquhar, J Wing, BA AF Franz, Heather B. Danielache, Sebastian O. Farquhar, James Wing, Boswell A. TI Mass-independent fractionation of sulfur isotopes during broadband SO2 photolysis: Comparison between O-16- and O-18-rich SO2 SO CHEMICAL GEOLOGY LA English DT Article DE Photochemistry; Sulfur dioxide; SO2; Mass-independent fractionation; Mars; Martian ID ABSORPTION-SPECTRA; ATMOSPHERIC SULFUR; DIOXIDE; REGION; OXYGEN; MARS; PHOTODISSOCIATION; METEORITES; CHEMISTRY; SULFATE AB This paper describes a comparison of ultraviolet photolysis experiments undertaken with SO2 (oxygen with isotopes at natural abundance levels) and (SO2)-O-18 (O-18-substituted oxygen). Experiments were conducted in a closed photocell using a deuterium lamp (principally 190-235 nm) under pressure regimes (5-25 Torr) that produced optically thick conditions for (SO2)-S-32 and variable optical depths for other isotopologues. The experiments, which were designed to examine the effects of intramolecular isotopic substitution of oxygen atoms on the S-MIF produced during UV photolysis of SO2, reveal generally reduced sulfur fractionation for O-18-rich SO2 as compared to O-16-rich SO2. Model shielding calculations were undertaken using spectra that were shifted due to changes in rotational and vibrational energy levels. The model calculations suggest that processes in addition to rotational and vibrational shifts in absorption spectra play a role in the experimentally produced isotope effects. Such additional processes may include differences in primary photoexcitation arising from smaller peak-to-valley amplitudes for fine structure of O-18-rich SO2 absorption spectra or an isotopically selective process associated with transitions between excited states. (C) 2013 Elsevier B. V. All rights reserved. C1 [Franz, Heather B.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Franz, Heather B.; Farquhar, James] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Danielache, Sebastian O.] Tokyo Inst Technol, Dept Environm Sci & Technol, Yokohama, Kanagawa 227, Japan. [Farquhar, James] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Wing, Boswell A.] McGill Univ, Montreal, PQ H3A 2A7, Canada. [Wing, Boswell A.] McGill Univ, Geotop, Montreal, PQ H3A 2A7, Canada. RP Franz, HB (reprint author), NASA GSFC Code 699,Bldg 33,Room F109A, Greenbelt, MD 20771 USA. EM heather.b.franz@nasa.gov FU NASA; National Science and Engineering Research Council of Canada FX The authors thank M. Quijada and T. Madison of NASA/GSFC for measurement of the D2 lamp spectrum and J. Lyons, A. Pavlov, and R. Hudson for insightful discussions during the preparation of this manuscript. The authors also thank three reviewers and additional clarification by M. Johnson and S. Ono. J. F. acknowledges research support from the NASA Exobiology program. B.A.W. acknowledges support from the National Science and Engineering Research Council of Canada through the Discovery grants program. NR 40 TC 5 Z9 5 U1 2 U2 31 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2541 EI 1878-5999 J9 CHEM GEOL JI Chem. Geol. PD DEC 20 PY 2013 VL 362 SI SI BP 56 EP 65 DI 10.1016/j.chemgeo.2013.07.021 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 262UV UT WOS:000327764300007 ER PT J AU Saraswat, P Syed, TH Famiglietti, JS Fielding, EJ Crippen, R Gupta, N AF Saraswat, Puneet Syed, Tajdarul H. Famiglietti, James S. Fielding, Eric J. Crippen, Robert Gupta, Nishant TI Recent changes in the snout position and surface velocity of Gangotri glacier observed from space SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID ANTARCTIC ICE STREAM; SEA-LEVEL RISE; CLIMATE-CHANGE; SAR INTERFEROMETRY; HIMALAYAN GLACIERS; WATER AVAILABILITY; SATELLITE IMAGERY; NEPAL HIMALAYA; ASTER DATA; RETREAT AB Glacier mass variations have a direct impact on some of the key components of the global water cycle, including sea level rise and freshwater availability. Apart from being one of the largest Himalayan glaciers, Gangotri is one of the sources of water for the Ganges river, which has a considerable influence on the socioeconomic structure of a largely over-populated catchment area accounting for approximate to 26% of India's landmass. In this study, we present the most recent assessment of the Gangotri glacier dynamics, combining the use of interferometric techniques on synthetic aperture radar data and sub-pixel offset tracking on Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) satellite imagery. Results show that on average, the Gangotri glacier snout has receded at a rate of 21.3 +/- 3m year(-1) over a period of 6 years (2004-2010). While glacier surface velocity near the snout is estimated to be between 24.8 +/- 2.3 and 28.9 +/- 2.3m year(-1), interior portions of the glacier recorded velocities in the range of 13.9 +/- 2.3 to 70.2 +/- 2.3m year(-1). Further, the average glacier surface velocity in the northern (lower) portions (28.1 +/- 2.3 m year(-1)) is observed to be significantly lower than in the southern (higher) portions (48.1 +/- 2.3m year(-1)) of the Gangotri glacier. These values are calculated with an uncertainty of less than 5 m year(-1). Results also highlight a consistent retreat and non-uniform dynamics of the Gangotri glacier. C1 [Saraswat, Puneet] Indian Sch Mines, Dept Appl Geophys, Dhanbad 826004, Bihar, India. [Syed, Tajdarul H.; Gupta, Nishant] Indian Sch Mines, Dept Appl Geol, Dhanbad 826004, Bihar, India. [Famiglietti, James S.; Crippen, Robert] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Famiglietti, James S.] Univ Calif Irvine, UC Ctr Hydrol Modeling, Irvine, CA USA. [Fielding, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Syed, TH (reprint author), Indian Sch Mines, Dept Appl Geol, Dhanbad 826004, Bihar, India. EM tsyed.ismu@gmail.com RI Syed, Tajdarul/G-6731-2014; Fielding, Eric/A-1288-2007 OI Fielding, Eric/0000-0002-6648-8067 FU NASA FX We thank Dirk Scherler for providing some of the ASTER scenes used in this study and advice on optimal scene choice. Envisat original data is copyright the European Space Agency and was provided under the AOE 668 project. Part of the work described in this article was supported by NASA's Earth Surface and Interior focus area and performed at the Jet Propulsion Laboratory, California Institute of Technology in Pasadena, California. We are also very thankful to the anonymous reviewers who helped improve the content and presentation of this study. This support is gratefully acknowledged. NR 61 TC 7 Z9 7 U1 1 U2 30 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 EI 1366-5901 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD DEC 20 PY 2013 VL 34 IS 24 BP 8653 EP 8668 DI 10.1080/01431161.2013.845923 PG 16 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 255KE UT WOS:000327237000001 ER PT J AU Thorne, RM Li, W Ni, B Ma, Q Bortnik, J Chen, L Baker, DN Spence, HE Reeves, GD Henderson, MG Kletzing, CA Kurth, WS Hospodarsky, GB Blake, JB Fennell, JF Claudepierre, SG Kanekal, SG AF Thorne, R. M. Li, W. Ni, B. Ma, Q. Bortnik, J. Chen, L. Baker, D. N. Spence, H. E. Reeves, G. D. Henderson, M. G. Kletzing, C. A. Kurth, W. S. Hospodarsky, G. B. Blake, J. B. Fennell, J. F. Claudepierre, S. G. Kanekal, S. G. TI Rapid local acceleration of relativistic radiation-belt electrons by magnetospheric chorus SO NATURE LA English DT Article ID PC5 WAVES; ENERGIZATION; SCATTERING; DIFFUSION; STORMS; MODEL AB Recent analysis of satellite data obtained during the 9 October 2012 geomagnetic storm identified the development of peaks in electron phase space density(1), which are compelling evidence for local electron acceleration in the heart of the outer radiation belt(2,3), but are inconsistent with acceleration by inward radial diffusive transport(4,5). However, the precise physical mechanism responsible for the acceleration on 9 October was not identified. Previous modelling has indicated that a magnetospheric electromagnetic emission known as chorus could be a potential candidate for local electron acceleration(6-10), but a definitive resolution of the importance of chorus for radiation-belt acceleration was not possible because of limitations in the energy range and resolution of previous electron observations and the lack of a dynamic global wave model. Here we report high-resolution electron observations(11) obtained during the 9 October storm and demonstrate, using a two-dimensional simulation performed with a recently developed time-varying data-driven model(12), that chorus scattering explains the temporal evolution of both the energy and angular distribution of the observed relativistic electron flux increase. Our detailed modelling demonstrates the remarkable efficiency of wave acceleration in the Earth's outer radiation belt, and the results presented have potential application to Jupiter, Saturn and other magnetized astrophysical objects. C1 [Thorne, R. M.; Li, W.; Ni, B.; Ma, Q.; Bortnik, J.; Chen, L.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. [Baker, D. N.] Univ Colorado, Lab Atmospher & Space Res, Boulder, CO 80303 USA. [Spence, H. E.] Univ New Hampshire, Each Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Reeves, G. D.; Henderson, M. G.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM 87544 USA. [Kletzing, C. A.; Kurth, W. S.; Hospodarsky, G. B.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Blake, J. B.; Fennell, J. F.; Claudepierre, S. G.] Aerosp Corp, Los Angeles, CA 90245 USA. [Kanekal, S. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Thorne, RM (reprint author), Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. EM rmt@atmos.ucla.edu RI Li, Wen/F-3722-2011; Henderson, Michael/A-3948-2011; OI Reeves, Geoffrey/0000-0002-7985-8098; Henderson, Michael/0000-0003-4975-9029; Kletzing, Craig/0000-0002-4136-3348; Hospodarsky, George/0000-0001-9200-9878; Spence, Harlan/0000-0002-2526-2205; Kurth, William/0000-0002-5471-6202 FU JHU/APL under NASA [967399, 921647, NAS5-01072]; EMFISIS [1001057397:01]; ECT [13-041] FX This work was supported by JHU/APL contracts 967399 and 921647 under NASA's prime contract NAS5-01072. The analysis at UCLA was supported by the EMFISIS sub-award 1001057397:01 and by the ECT sub-award 13-041. We thank OMNIweb for providing geomagnetic indices and solar wind parameters used in this study and the NOAA POES team for providing POES electron data. NR 30 TC 162 Z9 163 U1 5 U2 35 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD DEC 19 PY 2013 VL 504 IS 7480 BP 411 EP + DI 10.1038/nature12889 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 273ZR UT WOS:000328575300046 PM 24352287 ER PT J AU Koppelmans, V Erdeniz, B De Dios, YE Wood, SJ Reuter-Lorenz, PA Kofman, I Bloomberg, JJ Mulavara, AP Seidler, RD AF Koppelmans, Vincent Erdeniz, Burak De Dios, Yiri E. Wood, Scott J. Reuter-Lorenz, Patricia A. Kofman, Igor Bloomberg, Jacob J. Mulavara, Ajitkumar P. Seidler, Rachael D. TI Study protocol to examine the effects of spaceflight and a spaceflight analog on neurocognitive performance: extent, longevity, and neural bases SO BMC NEUROLOGY LA English DT Article DE Space flight; Astronauts; Microgravity; Sensorimotor feedback; Cognition; Neuroimaging; MRI; Longitudinal studies; Bed rest ID DOWN BED REST; SPATIAL WORKING-MEMORY; NEUROMUSCULAR ACTIVATION PATTERNS; GENERAL ELDERLY POPULATION; LONG-DURATION SPACEFLIGHT; SPACE-FLIGHT; TREADMILL WALKING; SHORT-TERM; SENSORIMOTOR PERFORMANCE; MENTAL PERFORMANCE AB Background: Long duration spaceflight (i.e., 22 days or longer) has been associated with changes in sensorimotor systems, resulting in difficulties that astronauts experience with posture control, locomotion, and manual control. The microgravity environment is an important causal factor for spaceflight induced sensorimotor changes. Whether spaceflight also affects other central nervous system functions such as cognition is yet largely unknown, but of importance in consideration of the health and performance of crewmembers both in-and post-flight. We are therefore conducting a controlled prospective longitudinal study to investigate the effects of spaceflight on the extent, longevity and neural bases of sensorimotor and cognitive performance changes. Here we present the protocol of our study. Methods/design: This study includes three groups (astronauts, bed rest subjects, ground-based control subjects) for which each the design is single group with repeated measures. The effects of spaceflight on the brain will be investigated in astronauts who will be assessed at two time points pre-, at three time points during-, and at four time points following a spaceflight mission of six months. To parse out the effect of microgravity from the overall effects of spaceflight, we investigate the effects of seventy days head-down tilted bed rest. Bed rest subjects will be assessed at two time points before-, two time points during-, and three time points post-bed rest. A third group of ground based controls will be measured at four time points to assess reliability of our measures over time. For all participants and at all time points, except in flight, measures of neurocognitive performance, fine motor control, gait, balance, structural MRI (T1, DTI), task fMRI, and functional connectivity MRI will be obtained. In flight, astronauts will complete some of the tasks that they complete pre- and post flight, including tasks measuring spatial working memory, sensorimotor adaptation, and fine motor performance. Potential changes over time and associations between cognition, motor-behavior, and brain structure and function will be analyzed. Discussion: This study explores how spaceflight induced brain changes impact functional performance. This understanding could aid in the design of targeted countermeasures to mitigate the negative effects of long-duration spaceflight. C1 [Koppelmans, Vincent; Erdeniz, Burak; Seidler, Rachael D.] Univ Michigan, Sch Kinesiol, Ann Arbor, MI 48109 USA. [De Dios, Yiri E.; Kofman, Igor] Wyle Life Sci, Houston, TX USA. [Wood, Scott J.] Pacific Azusa Univ, Coll Liberal Arts & Sci, Los Angeles, CA USA. [Wood, Scott J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Reuter-Lorenz, Patricia A.; Seidler, Rachael D.] Univ Michigan, Dept Psychol, Ann Arbor, MI USA. [Bloomberg, Jacob J.; Mulavara, Ajitkumar P.] NASA, Lyndon B Johnson Space Ctr, Neurosci Lab, Houston, TX 77058 USA. [Mulavara, Ajitkumar P.] Univ Space Res Assoc, Houston, TX USA. [Seidler, Rachael D.] Univ Michigan, Neurosci Program, Ann Arbor, MI 48109 USA. [Seidler, Rachael D.] Univ Michigan, Inst Gerontol, Ann Arbor, MI 48109 USA. RP Seidler, RD (reprint author), Univ Michigan, Sch Kinesiol, Ann Arbor, MI 48109 USA. EM rseidler@umich.edu FU NASA [NNX11AR02G, NCC 9-58]; National Space Biomedical Research Institute FX This work is funded by NASA NNX11AR02G and through the NASA Cooperative Agreement NCC 9-58 with the National Space Biomedical Research Institute (awarded to RDS). NR 82 TC 15 Z9 15 U1 0 U2 6 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2377 J9 BMC NEUROL JI BMC Neurol. PD DEC 18 PY 2013 VL 13 AR 205 DI 10.1186/1471-2377-13-205 PG 15 WC Clinical Neurology SC Neurosciences & Neurology GA 280YJ UT WOS:000329066400001 PM 24350728 ER PT J AU Percak-Dennett, EM Loizeau, JL Beard, BL Johnson, CM Roden, EE AF Percak-Dennett, Elizabeth M. Loizeau, Jean-Luc Beard, Brian L. Johnson, Clark M. Roden, Eric E. TI Iron isotope geochemistry of biogenic magnetite-bearing sediments from the Bay of Vidy, Lake Geneva SO CHEMICAL GEOLOGY LA English DT Article DE Bay of Vidy; Sediment; Microbial iron reduction; Iron isotope geochemistry; Magnetite formation ID ORGANIC-CARBON OXIDATION; FE(III) OXIDE REDUCTION; SEWAGE-TREATMENT PLANT; HYDROUS FERRIC-OXIDE; DISSIMILATORY FE(III); MN(IV) REDUCTION; CORE CORRELATION; ROCK RECORD; FRACTIONATION; FE AB Dissimilatory microbial iron oxide reduction (DIR) has been hypothesized to be an important respiratory pathway on early Earth, potentially generating significant quantities of Fe(II) that have been preserved in Proterozoic and Archean sedimentary rocks. In particular, DIR has been implicated in the formation of magnetite in Precambrian marine sediments. To date, however, only one modern sedimentary environment exists where in situ magnetite formation has been linked to DIR: the Bay of Vidy in Lake Geneva, Switzerland. Previous work at this locality has characterized a magnetic susceptibility anomaly that reflects the presence of fine-grained magnetite produced via microbial reduction of amorphous Fe(III) oxides that enter the Bay of Vidy from a nearby sewage treatment plant. In this study, we report on the Fe isotope composition of aqueous and solid-phase Fe in the Bay of Vidy sediments. Extensive Fe(III) reduction has occurred, resulting in the conversion of nearly all reactive (non-silicate) Fe(III) to a variety of Fe(II)-bearing phases, with mixed Fe valence magnetite being a minor but easily detectable component (0.5-8wt.%). Very little Fe isotope variation was observed in any solid phase Fe components, including magnetite, although significant fractionation was observed between aqueous and solid-phase Fe(II). Because Fe mass-balance was dominated by the solid phase, little net change in delta Fe-56 values for Fe(II)-bearing components was produced despite clear evidence for DIR. This study provides a basis for interpreting instances in the rock record where DIR was the driving force for Fe(II) production and magnetite formation, yet no significant deviations in delta Fe-56 values were preserved. A key implication of the results is that Fe isotope homogeneity is not sufficient to rule out a biological mechanism for magnetite formation, and this should be taken into account when examining the Precambrian rock record. (C) 2013 Elsevier B. V. All rights reserved. C1 [Percak-Dennett, Elizabeth M.; Beard, Brian L.; Johnson, Clark M.; Roden, Eric E.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Percak-Dennett, Elizabeth M.; Beard, Brian L.; Johnson, Clark M.; Roden, Eric E.] Univ Wisconsin, NASA, Astrobiol Inst, Madison, WI 53706 USA. [Loizeau, Jean-Luc] Univ Geneva, Inst FA Forel, CH-1290 Versoix, Switzerland. [Loizeau, Jean-Luc] Univ Geneva, Ctr Etud Sci Nat Environm, CH-1290 Versoix, Switzerland. RP Roden, EE (reprint author), Univ Wisconsin, 1215 West Dayton St, Madison, WI 53706 USA. EM eroden@geology.wisc.edu OI Loizeau, Jean-Luc/0000-0002-0611-0388 FU NASA Astrobiology Institute FX This work was supported by the NASA Astrobiology Institute. We gratefully acknowledge the assistance of D. Ortiz and J. Fournelle for assistance with SEM imaging, and H. Konishi for TEM work. NR 72 TC 6 Z9 6 U1 4 U2 48 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2541 EI 1878-5999 J9 CHEM GEOL JI Chem. Geol. PD DEC 18 PY 2013 VL 360 BP 32 EP 40 DI 10.1016/j.chemgeo.2013.10.008 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 259MX UT WOS:000327532100004 ER PT J AU Lu, ZF Streets, DG de Foy, B Krotkov, NA AF Lu, Zifeng Streets, David G. de Foy, Benjamin Krotkov, Nickolay A. TI Ozone Monitoring Instrument Observations of Interannual Increases in SO2 Emissions from Indian Coal-Fired Power Plants during 2005-2012 SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID SULFUR-DIOXIDE EMISSIONS; NOX EMISSIONS; CHINA; RETRIEVALS; INVENTORY; AEROSOLS; TRENDS; ASIA; OMI AB Due to the rapid growth of electricity demand and the absence of regulations, sulfur dioxide (SO2) emissions from coal-fired power plants in India have increased notably in the past decade. In this study, we present the first interannual comparison of SO2 emissions and the satellite SO2 observations from the Ozone Monitoring Instrument (OMI) for Indian coal-fired power plants during the OMI era of 2005-2012. A detailed unit-based inventory is developed for the Indian coal-fired power sector, and results show that its SO2 emissions increased dramatically by 71% during 2005-2012. Using the oversampling technique, yearly high-resolution OMI maps for the whole domain of India are created, and they reveal a continuous increase in SO2 columns over India. Power plant regions with annual SO2 emissions greater than 50 Gg year(-1) produce statistically significant OMI signals, and a high correlation (R = 0.93) is found between SO2 emissions and OMI-observed SO2 burdens. Contrary to the decreasing trend of national mean SO2 concentrations reported by the Indian Government, both the total OMI-observed SO2 and annual average SO2 concentrations in coal-fired power plant regions increased by >60% during 2005-2012, implying the air quality monitoring network needs to be optimized to reflect the true SO2 situation in India. C1 [Lu, Zifeng; Streets, David G.] Argonne Natl Lab, Decis & Informat Sci Div, Argonne, IL 60439 USA. [de Foy, Benjamin] St Louis Univ, Dept Earth & Atmospher Sci, St Louis, MO 63108 USA. [Krotkov, Nickolay A.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Maryland, MD 20771 USA. RP Lu, ZF (reprint author), Argonne Natl Lab, Decis & Informat Sci Div, 9700 S Cass Ave, Argonne, IL 60439 USA. EM zlu@anl.gov RI Lu, Zifeng/F-3266-2012; de Foy, Benjamin/A-9902-2010; Krotkov, Nickolay/E-1541-2012; OI de Foy, Benjamin/0000-0003-4150-9922; Krotkov, Nickolay/0000-0001-6170-6750; Streets, David/0000-0002-0223-1350 FU National Aeronautics and Space Administration (NASA) as part of the Air Quality Applied Sciences Team (AQAST) program; Ganges Valley Aerosol Experiment (GVAX) by the Office of Biological and Environmental Research in the U.S. Department of Energy, Office of Science. Argonne National Laboratory; U.S. Department of Energy [DE-AC02-06CH11357] FX This work was sponsored by the National Aeronautics and Space Administration (NASA) as part of the Air Quality Applied Sciences Team (AQAST) program. The India emission inventory was partially funded in support of the Ganges Valley Aerosol Experiment (GVAX) by the Office of Biological and Environmental Research in the U.S. Department of Energy, Office of Science. Argonne National Laboratory is operated by UChicago Argonne, LLC, under Contract No. DE-AC02-06CH11357 with the U.S. Department of Energy. NR 42 TC 17 Z9 19 U1 0 U2 40 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD DEC 17 PY 2013 VL 47 IS 24 BP 13993 EP 14000 DI 10.1021/es4039648 PG 8 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 277CT UT WOS:000328796900013 PM 24274462 ER PT J AU d'Abzac, FX Beard, BL Czaja, AD Konishi, H Schauer, JJ Johnson, CM AF d'Abzac, Francois-Xavier Beard, Brian L. Czaja, Andrew D. Konishi, Hiromi Schauer, James J. Johnson, Clark M. TI Iron Isotope Composition of Particles Produced by UV-Femtosecond Laser Ablation of Natural Oxides, Sulfides, and Carbonates SO ANALYTICAL CHEMISTRY LA English DT Article ID INDUCTIVELY-COUPLED PLASMA; MASS-SPECTROMETRY; ICP-MS; FE ISOTOPES; AEROSOLS; FRACTIONATION; SIZE; EFFICIENCY; CONDENSATION; VAPORIZATION AB The need for femtosecond laser ablation (Is-LA) systems coupled to MC-ICP-MS to accurately perform in situ stable isotope analyses remains an open question, because of the lack of knowledge concerning ablation-related isotopic fractionation in this regime. We report the first iron isotope analysis of size-resolved, laser-induced particles of natural magnetite, siderite, pyrrhotite, and pyrite, collected through cascade impaction, followed by analysis by solution nebulization MC-ICP-MS, as well as imaging using electron microscopy. Iron mass distributions are independent of mineralogy, and particle morphology includes both spheres and agglomerates for all ablated phases. X-ray spectroscopy shows elemental fractionation in siderite (C-rich agglomerates) and pyrrhotite/pyrite (S-rich spheres). We find an increase in Fe-56/Fe-54 ratios of +2 parts per thousand, +1.2 parts per thousand, and +0.8 parts per thousand with increasing particle size for magnetite, siderite, and pyrrhotite, respectively. Fe isotope differences in size-sorted aerosols from pyrite ablation are not analytically resolvable. Experimental data are discussed using models of particles generation by Hergenroder and elemental/isotopic fractionation by Richter. We interpret the isotopic fractionation to be related to the iron condensation time scale, dependent on its saturation in the gas phase, as a function of mineral composition. Despite the isotopic variations across aerosol size fractions, total aerosol composition, as calculated from mass balance, confirms that fs-LA produces a stoichiometric sampling in terms of isotopic composition. Specifically, both elemental and isotopic fractionation are produced by particle generation processes and not by femtosecond laser-matter interactions. These results provide critical insights into the analytical requirements for laser-ablation-based stable isotope measurements of high-precision and accuracy in geological samples, including the importance of quantitative aerosol transport to the ICP. C1 [d'Abzac, Francois-Xavier; Beard, Brian L.; Czaja, Andrew D.; Konishi, Hiromi; Johnson, Clark M.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [d'Abzac, Francois-Xavier; Beard, Brian L.; Czaja, Andrew D.; Konishi, Hiromi; Johnson, Clark M.] Univ Wisconsin, NASA, Astrobiol Inst, Madison, WI 53706 USA. [Czaja, Andrew D.] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA. [Czaja, Andrew D.] Univ Cincinnati, Dept Chem, Cincinnati, OH 45221 USA. [Schauer, James J.] Univ Wisconsin, Water Sci & Engn Lab 148, Madison, WI 53706 USA. [Konishi, Hiromi] Niigata Univ, Dept Geol, Nishi Ku, Niigata 9502181, Japan. RP d'Abzac, FX (reprint author), Univ Wisconsin, Dept Geosci, 1215W Dayton St, Madison, WI 53706 USA. EM fxdabzac@gmail.com FU NASA Astrobiology Institute FX Funding was provided by the NASA Astrobiology Institute. FEG/SEM and TEM were performed at the Material Sciences and Engineering Center at UW-Madison. The authors would like to thank Alexander Kvit for his help with TEM observations. John Fournelle is thanked for his assistance with EPMA analyses. NR 48 TC 11 Z9 11 U1 1 U2 49 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0003-2700 EI 1520-6882 J9 ANAL CHEM JI Anal. Chem. PD DEC 17 PY 2013 VL 85 IS 24 BP 11885 EP 11892 DI 10.1021/ac402722t PG 8 WC Chemistry, Analytical SC Chemistry GA 277CV UT WOS:000328797200031 PM 24261311 ER PT J AU Chen, S Hong, Y Cao, Q Gourley, JJ Kirstetter, PE Yong, B Tian, YD Zhang, ZX Shen, Y Hu, JJ Hardy, J AF Chen, Sheng Hong, Yang Cao, Qing Gourley, Jonathan J. Kirstetter, Pierre-Emmanuel Yong, Bin Tian, Yudong Zhang, Zengxin Shen, Yan Hu, Junjun Hardy, Jill TI Similarity and difference of the two successive V6 and V7 TRMM multisatellite precipitation analysis performance over China SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Satellite QPE; TRMM; evaluation; China ID GLOBAL PRECIPITATION; UNITED-STATES; SATELLITE; PRODUCTS; RAINFALL; CLIMATE; RADAR; MODEL; ALGORITHM; TERRAIN AB Similarities and differences of spatial error structures of surface precipitation estimated with successive version 6 (V6) and version 7 (V7) Tropical Rainfall Measuring Mission (TRMM) Multisatellite Precipitation Analysis (TMPA) algorithms are systematically analyzed through comparison with the China Meteorological Administration's national daily precipitation analysis from June 2008 to May 2011. The TMPA products include V6 and V7 real-time products 3B42RTV6 and 3B42RTV7 and research products 3B42V6 and 3B42V7. Both versions of research products outperform their respective real-time counterparts. 3B42V7 clearly improves upon 3B42V6 over China in terms of daily mean precipitation; the correlation coefficient (CC) increases from 0.89 to 0.93, the relative bias (RB) improves from -4.91% to -0.05%, and the root-mean-square error (RMSE) improves from 0.69mm to 0.54mm. When considering 3 year mean precipitation, 3B42V7 shows similar spatial patterns and statistical performance to 3B42V6. Both 3B42RTV7 and 3B42RTV6 demonstrate similar bias patterns in most regions of China with overestimation by 20% in arid regions (i.e., the north and west of China) and slight underestimation in humid regions (e.g., -5.82% in southern China). However, 3B42RTV7 overestimates precipitation more than 3B42RTV6 in the cold Qinghai-Tibetan plateau, resulting in a much higher RB of 139.95% (128.69%, 136.09%, and 121.11%) in terms of 3 year annual (spring, summer, and autumn) daily mean precipitation and an even worse performance during winter. In this region, 3B42RTV7 shows an overall slightly degraded performance than 3B42RTV6 with CC decreasing from 0.81 to 0.73 and RB (RMSE) increasing from 21.22% (0.95mm) to 35.84% (1.27mm) in terms of daily precipitation. C1 [Chen, Sheng; Hong, Yang; Kirstetter, Pierre-Emmanuel; Hu, Junjun] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA. [Chen, Sheng; Hong, Yang; Cao, Qing; Kirstetter, Pierre-Emmanuel] Univ Oklahoma, Hydrometeorol & Remote Sensing Lab, Norman, OK 73019 USA. [Chen, Sheng; Hong, Yang; Cao, Qing; Kirstetter, Pierre-Emmanuel; Hardy, Jill] Natl Weather Ctr, Adv Radar Res Ctr, Norman, OK 73072 USA. [Gourley, Jonathan J.; Hardy, Jill] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA. [Yong, Bin] Hohai Univ, State Key Lab Hydrol Water Resources & Hydraul En, Nanjing, Jiangsu, Peoples R China. [Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Tian, Yudong] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Zhang, Zengxin] Nanjing Forestry Univ, Jiansu Key Lab Forestry Ecol Engn, Nanjing, Jiangsu, Peoples R China. [Shen, Yan] China Meteorol Adm, Natl Meteorol Informat Ctr, Beijing, Peoples R China. [Hu, Junjun] Univ Oklahoma, Sch Comp Sci, Norman, OK 73019 USA. RP Hong, Y (reprint author), Natl Weather Ctr, Adv Radar Res Ctr, Suite 4160,120 David L Boren Blvd, Norman, OK 73072 USA. EM yanghong@ou.edu RI Gourley, Jonathan/C-7929-2016; Measurement, Global/C-4698-2015; Yong, Bin/C-2257-2014; Kirstetter, Pierre/E-2305-2013; Hong, Yang/D-5132-2009 OI Gourley, Jonathan/0000-0001-7363-3755; Yong, Bin/0000-0003-1466-2091; Kirstetter, Pierre/0000-0002-7381-0229; Hong, Yang/0000-0001-8720-242X FU NOAA FX We acknowledge the TRMM mission scientists and associated NASA personnel for the production of the data used in this research effort, and are very much indebted to the team responsible for the TMPA products, especially George J. Huffman. Thanks are also given to Youcun Qi of the Cooperative Institute for Mesoscale Meteorological Studies at the University of Oklahoma. This work was financially supported by the NOAA Multifunction Phased-Array Radar project administrated by the Advanced Radar Research Center at the University of Oklahoma. NR 54 TC 40 Z9 43 U1 4 U2 35 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 16 PY 2013 VL 118 IS 23 BP 13060 EP 13074 DI 10.1002/2013JD019964 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297PD UT WOS:000330266500018 ER PT J AU Kim, MH Kim, SW Yoon, SC Omar, AH AF Kim, Man-Hae Kim, Sang-Woo Yoon, Soon-Chang Omar, Ali H. TI Comparison of aerosol optical depth between CALIOP and MODIS-Aqua for CALIOP aerosol subtypes over the ocean SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE CALIOP; aerosol optical depth; aerosol type; lidar ratio; MODIS ID GROUND-BASED LIDAR; RAMAN LIDAR; CALIPSO; EXTINCTION; CLOUD; DUST; PRODUCTS; RATIO; RETRIEVALS; VALIDATION AB The Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) aerosol optical depth (AOD) has been compared with the Moderate Resolution Imaging Spectroradiometer (MODIS)-Aqua AOD using Level 2 products of both instruments. Such comparisons have been performed for five different aerosol subtypes classified by CALIOP algorithm, namely clean marine, dust, polluted dust, polluted continental, and biomass burning, over the ocean from June 2006 to December 2010. MODIS AOD at 550nm (0.1110.079) for the collocated data pairs is about 63% higher than CALIOP AOD at 532nm (0.0680.073). For clean marine, MODIS AOD (0.1100.064) is almost twice the CALIOP AOD (0.0560.038), and the difference between the AOD values has a strong latitude dependence likely related to the surface wind speed over the ocean. The difference in AOD for dust (13%) is observed to be the lowest among the five aerosol types under consideration, but it shows a slight regional variation. The discrepancy of AOD for dust also shows strong dependency on the layer mean of the particulate depolarization ratio. CALIOP AOD is higher than MODIS AOD for both polluted dust and polluted continental by 15% and 29%, respectively, for most of the ocean. One of the possible reasons for the difference is the misclassification of clean marine (or marine+dust) as polluted dust and polluted continental in the CALIOP algorithm. For biomass burning, uncertainty in the layer base altitude is thought to be one of the main reasons for the lower value of CALIOP AOD. C1 [Kim, Man-Hae; Kim, Sang-Woo; Yoon, Soon-Chang] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul 151742, South Korea. [Omar, Ali H.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Kim, SW (reprint author), Seoul Natl Univ, Sch Earth & Environm Sci, Seoul 151742, South Korea. EM sangwookim@snu.ac.kr RI Omar, Ali/D-7102-2017 OI Omar, Ali/0000-0003-1871-9235 FU BK21 plus program of the School of Earth and Environmental Sciences, Seoul National University; Korea Meteorological Administration Research and Development Program [CATER 2012-3020] FX This research was supported by the BK21 plus program of the School of Earth and Environmental Sciences, Seoul National University, and by the Korea Meteorological Administration Research and Development Program under grant CATER 2012-3020. We gratefully acknowledge J. Campbell (NRL) and three anonymous reviewers for their valuable suggestions and comments. NR 48 TC 7 Z9 7 U1 1 U2 20 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 16 PY 2013 VL 118 IS 23 BP 13241 EP 13252 DI 10.1002/2013JD019527 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297PD UT WOS:000330266500031 ER PT J AU Yu, Y Notaro, M Liu, ZY Kalashnikova, O Alkolibi, F Fadda, E Bakhrjy, F AF Yu, Yan Notaro, Michael Liu, Zhengyu Kalashnikova, Olga Alkolibi, Fahad Fadda, Eyad Bakhrjy, Fawzieh TI Assessing temporal and spatial variations in atmospheric dust over Saudi Arabia through satellite, radiometric, and station data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE atmospheric dust; Saudi Arabia ID AEROSOL OPTICAL DEPTH; IMAGING SPECTRORADIOMETER MISR; AERONET; MODIS; PRODUCTS; NETWORK; RETRIEVALS; VALIDATION; STORMS; SITES AB Temporal and spatial variations in atmospheric dust over Saudi Arabia are studied for 2000-2010 using satellite and ground-based aerosol optical depth (AOD) and station dust storm observations. These data sets show a consistent seasonal cycle in dust activity, which peaks in spring-summer in northern-central Saudi Arabia and in early spring and summer across southern-western Saudi Arabia, associated with strong winds and westerly transport, respectively. Over the desert regions, anomalies in dust activity from satellite and station observations are highly correlated on the monthly timescale and statistically consistent on the daily timescale. However, the coastal and mountainous regions exhibit limited consistency between these data sets, likely associated with the coarse spatial resolution and short sampling time in the satellite data, as well as non-aeolian aerosol contamination. We conclude that satellite AOD is a reliable index for dust activity over desert regions but not over low dust, coastal, and topographically complex regions in Saudi Arabia. C1 [Yu, Yan; Notaro, Michael; Liu, Zhengyu] Univ Wisconsin, Nelson Inst Ctr Climat Res, Madison, WI 53706 USA. [Liu, Zhengyu] Peking Univ, Sch Phys, Lab Climate Ocean & Atmospher Studies, Beijing 100871, Peoples R China. [Kalashnikova, Olga] NASA, Jet Prop Lab, Pasadena, CA USA. [Alkolibi, Fahad; Fadda, Eyad; Bakhrjy, Fawzieh] King Saud Univ, Dept Geog, Riyadh, Saudi Arabia. RP Yu, Y (reprint author), Univ Wisconsin, Nelson Inst Ctr Climat Res, 1225 W Dayton St Room 1143, Madison, WI 53706 USA. EM yu45@wisc.edu FU King Saud University FX This study was funded by the King Saud University. The authors are thankful for helpful discussions with Sun Wong, Fujung Tsai, and Guangshan Chen and comments from three anonymous reviewers. Nelson Center for Climatic Research publication 1138. NR 32 TC 9 Z9 9 U1 0 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 16 PY 2013 VL 118 IS 23 BP 13253 EP 13264 DI 10.1002/2013JD020677 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297PD UT WOS:000330266500023 ER PT J AU Seyedi, MA Yao, M O'Brien, J Wang, SY Dapkus, PD AF Seyedi, M. A. Yao, M. O'Brien, J. Wang, S. Y. Dapkus, P. D. TI Large area, low capacitance, GaAs nanowire photodetector with a transparent Schottky collecting junction SO APPLIED PHYSICS LETTERS LA English DT Article ID GALLIUM-ARSENIDE; SPECTROSCOPY; ARRAYS AB We present experimental results on a GaAs/Indium-Tin-Oxide Schottky-like heterojunction photodetector based on a nanowire device geometry. By distributing the active detecting area over an array of nanowires, it is possible to achieve large area detection with low capacitance. Devices with bare GaAs and passivated AlGaAs/GaAs nanowires are fabricated to compare the responsivity with and without surface passivation. We are able to achieve responsivity of > 0.5A/W and Signal-Noise-Ratio in excess of 7 dB for 2V applied reverse bias with passivated nanowire devices. Capacitance-voltage measurement yields < 5 nF/cm(2), which shows a strong possibility for high-speed applications with a broad area device. (C) 2013 AIP Publishing LLC. C1 [Seyedi, M. A.; Yao, M.; O'Brien, J.; Wang, S. Y.; Dapkus, P. D.] Univ So Calif, Ctr Energy Nanosci, Los Angeles, CA 90089 USA. [Wang, S. Y.] Univ Calif Santa Cruz, Adv Studies Labs, Nanostruct Energy Convers Technol & Res NECTAR, Santa Cruz, CA 95064 USA. [Wang, S. Y.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Seyedi, MA (reprint author), Univ So Calif, Ctr Energy Nanosci, Los Angeles, CA 90089 USA. EM seyedi@usc.edu RI Yao, Maoqing/H-9697-2014 OI Yao, Maoqing/0000-0002-7674-575X FU Hewlett-Packard; University of Southern California's Center for Energy Nanoscience FX This work was funded by Hewlett-Packard and University of Southern California's Center for Energy Nanoscience for the authors M. A. S. and M.Y., respectively. M. A. S. wishes to extend appreciation to Dr. R. Sarkissian for many valuable discussions. NR 23 TC 7 Z9 7 U1 4 U2 28 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD DEC 16 PY 2013 VL 103 IS 25 AR 251109 DI 10.1063/1.4852136 PG 4 WC Physics, Applied SC Physics GA 293LU UT WOS:000329973800009 ER PT J AU Wong, MH Atreya, SK Mahaffy, PN Franz, HB Malespin, C Trainer, MG Stern, JC Conrad, PG Manning, HLK Pepin, RO Becker, RH McKay, CP Owen, TC Navarro-Gonzalez, R Jones, JH Jakosky, BM Steele, A AF Wong, Michael H. Atreya, Sushil K. Mahaffy, Paul N. Franz, Heather B. Malespin, Charles Trainer, Melissa G. Stern, Jennifer C. Conrad, Pamela G. Manning, Heidi L. K. Pepin, Robert O. Becker, Richard H. McKay, Christopher P. Owen, Tobias C. Navarro-Gonzalez, Rafael Jones, John H. Jakosky, Bruce M. Steele, Andrew TI Isotopes of nitrogen on Mars: Atmospheric measurements by Curiosity's mass spectrometer SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE planetary atmospheres; Mars; nitrogen isotopes; Mars meteorites ID MARTIAN ATMOSPHERE; CARBON-DIOXIDE; SOLAR-WIND; NOBLE-GASES; FRACTIONATION; SHERGOTTITES; ABUNDANCE; METEORITE; REGOLITH; HISTORY AB The Sample Analysis at Mars (SAM) instrument suite on the Mars Science Laboratory (MSL) measured a Mars atmospheric(14)N/N-15 ratio of 173 11 on sol 341 of the mission, agreeing with Viking's measurement of 168 17. The MSL/SAM value was based on Quadrupole Mass Spectrometer measurements of an enriched atmospheric sample, with CO2 and H2O removed. Doubly ionized nitrogen data at m/z 14 and 14.5 had the highest signal/background ratio, with results confirmed by m/z 28 and 29 data. Gases in SNC meteorite glasses have been interpreted as mixtures containing a Martian atmospheric component, based partly on distinctive(14)N/N-15 and(40)Ar/N-14 ratios. Recent MSL/SAM measurements of the(40)Ar/N-14 ratio (0.51 0.01) are incompatible with the Viking ratio (0.35 0.08). The meteorite mixing line is more consistent with the atmospheric composition measured by Viking than by MSL. C1 [Wong, Michael H.; Atreya, Sushil K.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Wong, Michael H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Mahaffy, Paul N.; Franz, Heather B.; Malespin, Charles; Trainer, Melissa G.; Stern, Jennifer C.; Conrad, Pamela G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Manning, Heidi L. K.] Concordia Coll, Dept Phys, Moorhead, MN USA. [Pepin, Robert O.; Becker, Richard H.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA USA. [Owen, Tobias C.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Navarro-Gonzalez, Rafael] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Jones, John H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Jakosky, Bruce M.] Univ Colorado Boulder, LASP, Boulder, CO USA. [Steele, Andrew] Carnegie Inst Sci, Geophys Lab, Washington, DC USA. RP Wong, MH (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Space Res Bldg,2455 Hayward St, Ann Arbor, MI 48109 USA. EM mike.wong@umich.edu RI Stern, Jennifer/E-3135-2012; Gonzalez, Rafael/D-1748-2009; Trainer, Melissa/E-1477-2012 OI Stern, Jennifer/0000-0002-0162-8807; FU NASA Mars Science Laboratory Project FX The authors thank the MSL Team for successful operation of the mission, Jane Fox and Richard Quinn for thorough and helpful reviews, and Bernard Marty and Guillaume Avice for insightful comments on the analysis of Tissint. This research was supported by the NASA Mars Science Laboratory Project. NR 45 TC 12 Z9 13 U1 1 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 16 PY 2013 VL 40 IS 23 BP 6033 EP 6037 DI 10.1002/2013GL057840 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 282AH UT WOS:000329141900004 ER PT J AU Fu, YN Argus, DF Freymueller, JT Heflin, MB AF Fu, Yuning Argus, Donald F. Freymueller, Jeffrey T. Heflin, Michael B. TI Horizontal motion in elastic response to seasonal loading of rain water in the Amazon Basin and monsoon water in Southeast Asia observed by GPS and inferred from GRACE SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE horizontal seasonal deformation; GPS; GRACE; Amazon Basin; Southeast Asia ID SURFACE AB We find seasonal horizontal crustal motions observed by GPS positioning in elastic response to heavy rainfall in the Amazon Basin and to monsoons in Southeast Asia to be consistent with those inferred from Gravity Recovery and Climate Experiment (GRACE) gravity observations of water mass loading. Solid Earth moves toward the Amazon during heavy spring rainfall and toward Southeast Asia during summer monsoons and back away from these areas 6 months later when the water load is minimum. Vertical oscillations observed by GPS and inferred from GRACE are 2 to 3 times larger than horizontal oscillation near the margins of the areas of large mass loading. Some discrepancies between GPS and GRACE are probably caused by local effects that influence GPS measurements, because the GPS sites that show significant discrepancies also do not match nearby GPS sites. However, when the load is short wavelength, the limited spatial resolution of GRACE can cause systematic misfits. C1 [Fu, Yuning; Argus, Donald F.; Heflin, Michael B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Freymueller, Jeffrey T.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. RP Fu, YN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Yuning.Fu@jpl.nasa.gov FU NASA Postdoctoral Program at Jet Propulsion Laboratory; National Aeronautics and Space Administration (NASA) FX We greatly appreciate Jean-Philippe Avouac and his group at Caltech Tectonics Observatory for maintaining continuous GPS measurements in Nepal. YF thanks Richard Gross and Susan Owen for helpful discussion. We are grateful to Paul Tregoning, Shfaqat Abbas Khan, and an anonymous reviewer for constructive criticism and comments that significantly improve the manuscript. YF was supported through the NASA Postdoctoral Program at Jet Propulsion Laboratory. This paper presents the results carried out at the Jet Propulsion Laboratory, California Institute of Technology, sponsored by the National Aeronautics and Space Administration (NASA). NR 28 TC 11 Z9 11 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 16 PY 2013 VL 40 IS 23 BP 6048 EP 6053 DI 10.1002/2013GL058093 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 282AH UT WOS:000329141900007 ER PT J AU Sigmarsson, O Haddadi, B Carn, S Moune, S Gudnason, J Yang, K Clarisse, L AF Sigmarsson, Olgeir Haddadi, Baptiste Carn, Simon Moune, Severine Gudnason, Jonas Yang, Kai Clarisse, Lieven TI The sulfur budget of the 2011 Grimsvotn eruption, Iceland SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE sulfur degassing; Grimsvotn volcano; satellite-based SO2 mass loading; sulfide globules; mineral melt inclusions ID VOLCANIC-ERUPTIONS; MAGMAS EVIDENCE; GAS; EMISSIONS AB Sulfur concentrations have been measured in 28 melt inclusions (MIs) in plagioclase, clinopyroxene, and olivine crystals extracted from tephra produced during the explosive eruption of Grimsvotn in May 2011. The results are compared to sulfur concentrations in the groundmass glass in order to estimate the mass of sulfur brought to surface during the eruption. Satellite measurements yield order of magnitude lower sulfur (0.2 Tg) in the eruption plume than estimated from the difference between MI and the groundmass glass. This sulfur deficit is readily explained by sulfur adhering to tephra grains but principally by sulfide globules caused by basalt-sulfide melt exsolution before degassing. A mass balance calculation reveals that approximately 0.8 Tg of SO2 is present as globules, representing 50% of the total sulfur budget. Most of the sulfide globules likely reside at depth due to their elevated density, for potential later remobilization by new magma or hydrothermal circulation. C1 [Sigmarsson, Olgeir; Haddadi, Baptiste; Moune, Severine] CNRS UBP IRD, LMV, F-63038 Clermont Ferrand, France. [Sigmarsson, Olgeir; Gudnason, Jonas] Univ Iceland, ISE, Reykjavik, Iceland. [Carn, Simon] Michigan Technol Univ, Dept Geol Min Engn & Sci, Houghton, MI 49931 USA. [Yang, Kai] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. [Yang, Kai] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Clarisse, Lieven] Univ Libre Brussels, Serv Chim Quant & Photophys, Brussels, Belgium. RP Sigmarsson, O (reprint author), CNRS UBP IRD, LMV, 5 Rue Kessler, F-63038 Clermont Ferrand, France. EM olgeir@opgc.univ-bpclermont.fr RI moune, severine/M-6827-2014 FU Iceland Science Fund; French ANR "DegazMag" project; French-Icelandic scientific collaboration project "Jules Verne"; EC Supersite Programme (FutureVolc); NASA through the Aura Science Team [NNX11AF42G] FX We are grateful to Gudrun Larsen, Sigrun Hreinsdottir, Thora Arnadottir, Magnus T. Gudmundsson, Thorvaldur Thordarson, Armann Hoskuldsson, and Freysteinn Sigmundsson for discussions on the 2011 eruption at Grimsvotn. Jean-Luc Devidal provided expert advices during the EMP work. Critical and constructive reviews from Marie Edmonds, Peter Kelly, and Roberto Moretti led to significant improvements. This study was partially supported by the Iceland Science Fund (Volcano Anatomy grant), the French ANR "DegazMag" project, French-Icelandic scientific collaboration project "Jules Verne," and an EC Supersite Programme (FutureVolc), all of which is gratefully acknowledged. SC and KY acknowledge support from NASA through the Aura Science Team (grant NNX11AF42G). This is the Laboratory of Excellence "ClerVolc" contribution #81. NR 25 TC 11 Z9 11 U1 0 U2 28 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 16 PY 2013 VL 40 IS 23 BP 6095 EP 6100 DI 10.1002/2013GL057760 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 282AH UT WOS:000329141900016 ER PT J AU Olascoaga, MJ Beron-Vera, FJ Haller, G Trinanes, J Iskandarani, M Coelho, EF Haus, BK Huntley, HS Jacobs, G Kirwan, AD Lipphardt, BL Ozgokmen, TM Reniers, AJHM Valle-Levinson, A AF Olascoaga, M. J. Beron-Vera, F. J. Haller, G. Trinanes, J. Iskandarani, M. Coelho, E. F. Haus, B. K. Huntley, H. S. Jacobs, G. Kirwan, A. D., Jr. Lipphardt, B. L., Jr. Oezgoekmen, T. M. Reniers, A. J. H. M. Valle-Levinson, A. TI Drifter motion in the Gulf of Mexico constrained by altimetric Lagrangian coherent structures SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE geodesic LCS; LCS cores; altimetry; Gulf of Mexico; drifters; GLAD ID TRANSPORT; FLOWS AB Application of recent geometric tools for Lagrangian coherent structures (LCS) shows that material attraction in geostrophic velocities derived from altimetry data imposed an important constraint to the motion of drifters from the Grand Lagrangian Deployment (GLAD) in the Gulf of Mexico. This material attraction is largely transparent to traditional Eulerian analysis. Attracting LCS acted as approximate centerpieces for mesoscale patterns formed by the drifters. Persistently attracting LCS cores emerged 1week before the development of a filament resembling the tiger tail of the Deepwater Horizon oil slick, thereby anticipating its formation. Our results suggest that the mesoscale circulation plays a significant role in shaping near-surface transport in the Gulf of Mexico. C1 [Olascoaga, M. J.; Beron-Vera, F. J.; Iskandarani, M.; Haus, B. K.; Oezgoekmen, T. M.; Reniers, A. J. H. M.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Haller, G.] Swiss Fed Inst Technol, Inst Mech Syst, Zurich, Switzerland. [Trinanes, J.] Univ Santiago de Compostela, Inst Invest Tecnolox, Santiago, Spain. [Coelho, E. F.] Univ New Orleans, Dept Phys, New Orleans, LA 70148 USA. [Huntley, H. S.; Kirwan, A. D., Jr.; Lipphardt, B. L., Jr.] Univ Delaware, Sch Marine Sci & Policy, Newark, DE USA. [Jacobs, G.] Stennis Space Ctr, Naval Res Lab, Stennis Space Ctr, MS USA. [Valle-Levinson, A.] Univ S Florida, Dept Civil & Coastal Engn, Gainesville, FL USA. RP Olascoaga, MJ (reprint author), Univ Miami, RSMAS AMP, 4600 Rickenbacker Cswy, Miami, FL 33149 USA. EM jolascoaga@rsmas.miami.edu RI Haller, George/A-5076-2012; Trinanes, Joaquin/B-3881-2015 OI Trinanes, Joaquin/0000-0003-1529-3371 FU BP/The Gulf of Mexico Research Initiative grant; NSF [CMG0825547]; NASA [NX10AE99G]; ONR [N00014-10-1-0522, N00014-11-10081, N00014-11-1-0087]; Mary A. S. Lighthipe endowment at the University of Delaware FX We thank A. Poje for helpful comments and S. Chinchilla for proof reading an earlier version of the manuscript. S. Schofield was responsible for drifter electronics optimization. The altimeter data set is distributed by AVISO (http://www.aviso.oceanobs.com). Support for this work was provided by a BP/The Gulf of Mexico Research Initiative grant; NSF grant CMG0825547; NASA grant NX10AE99G; ONR grants N00014-10-1-0522, N00014-11-10081, and N00014-11-1-0087; and the Mary A. S. Lighthipe endowment at the University of Delaware. NR 10 TC 28 Z9 28 U1 3 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 16 PY 2013 VL 40 IS 23 BP 6171 EP 6175 DI 10.1002/2013GL058624 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 282AH UT WOS:000329141900029 ER PT J AU Ao, CO Hajj, AJ AF Ao, Chi O. Hajj, Amanda J. TI Monitoring the width of the tropical belt with GPS radio occultation measurements SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE tropical belt; GPS; RO; occultation; Hadley circulation; tropopause ID GLOBAL POSITIONING SYSTEM; ERA-INTERIM REANALYSIS; TIME-SERIES; ASSIMILATION; ATMOSPHERE AB GPS radio occultation data collected over the period 2002-2011 were analyzed to examine the possible expansion of the tropical belt due to climate change. By the use of high vertical-resolution temperature profiles, monthly averages of the lapse rate tropopause were obtained and used to derive a decade-long time series of the tropical edge latitude (TEL) in each hemisphere and its linear trends. Two different TEL criteria were examined. Our analysis shows that a statistically significant widening trend of approximate to 1 degrees latitude/decade was found in the Northern Hemisphere (NH) by either criterion. This contrasts strongly with the Southern Hemisphere (SH), where no statistically significant trends were found. Comparison with ECMWF reanalysis shows good agreement, but the agreement is worse over SH. Substantial differences in seasonal trends were found between NH and SH, with the latter showing strong widening in the austral summer countered by contraction over the austral winter and spring. C1 [Ao, Chi O.; Hajj, Amanda J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ao, CO (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 138-308, Pasadena, CA 91109 USA. EM chi.o.ao@jpl.nasa.gov RI Richards, Amber/K-8203-2015 NR 19 TC 7 Z9 7 U1 2 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 16 PY 2013 VL 40 IS 23 BP 6236 EP 6241 DI 10.1002/2013GL058203 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 282AH UT WOS:000329141900041 ER PT J AU Li, C Joiner, J Krotkov, NA Bhartia, PK AF Li, Can Joiner, Joanna Krotkov, Nickolay A. Bhartia, Pawan K. TI A fast and sensitive new satellite SO2 retrieval algorithm based on principal component analysis: Application to the ozone monitoring instrument SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE principal component analysis; OMI; sulfur dioxide AB We describe a new algorithm to retrieve SO2 from satellite-measured hyperspectral radiances. We employ the principal component analysis technique in regions with no significant SO2 to capture radiance variability caused by both physical processes (e.g., Rayleigh and Raman scattering and ozone absorption) and measurement artifacts. We use the resulting principal components and SO2 Jacobians calculated with a radiative transfer model to directly estimate SO2 vertical column density in one step. Application to the Ozone Monitoring Instrument (OMI) radiance spectra in 310.5-340nm demonstrates that this approach can greatly reduce biases in the operational OMI product and decrease the noise by a factor of 2, providing greater sensitivity to anthropogenic emissions. The new algorithm is fast, eliminates the need for instrument-specific radiance correction schemes, and can be easily adapted to other sensors. These attributes make it a promising technique for producing long-term, consistent SO2 records for air quality and climate research. C1 [Li, Can] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Li, Can; Joiner, Joanna; Krotkov, Nickolay A.; Bhartia, Pawan K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Li, C (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM can.li@nasa.gov RI Li, Can/F-6867-2011; Joiner, Joanna/D-6264-2012; Krotkov, Nickolay/E-1541-2012; Bhartia, Pawan/A-4209-2016 OI Krotkov, Nickolay/0000-0001-6170-6750; Bhartia, Pawan/0000-0001-8307-9137 FU NASA Earth Science Division FX We acknowledge the NASA Earth Science Division for funding of OMI SO2 product development and analysis. The Dutch-Finnish-built OMI instrument is part of the NASA EOS Aura satellite payload. The OMI instrument is managed by KNMI and the Netherlands Agency for Aero-space Programs (NIVR). NR 17 TC 35 Z9 36 U1 3 U2 25 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 16 PY 2013 VL 40 IS 23 BP 6314 EP 6318 DI 10.1002/2013GL058134 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 282AH UT WOS:000329141900055 ER PT J AU Schmit, TJ Goodman, SJ Lindsey, DT Rabin, RM Bedka, KM Gunshor, MM Cintineo, JL Velden, CS Bachmeier, AS Lindstrom, SS Schmidt, CC AF Schmit, Timothy J. Goodman, Steven J. Lindsey, Daniel T. Rabin, Robert M. Bedka, Kristopher M. Gunshor, Mathew M. Cintineo, John L. Velden, Christopher S. Bachmeier, A. Scott Lindstrom, Scott S. Schmidt, Christopher C. TI Geostationary Operational Environmental Satellite (GOES)-14 super rapid scan operations to prepare for GOES-R SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE rapid scan; SRSOR; GOES-14 imager; GOES-R; ABI; hurricane; Hurricane Sandy; overshooting cloud tops ID OVERSHOOTING TOPS; TROPICAL CYCLONE; GENERATION AB Geostationary Operational Environmental Satellite (GOES)-14 imager was operated by National Oceanic and Atmospheric Administration (NOAA) in an experimental rapid scan 1-min mode that emulates the high-temporal resolution sampling of the Advanced Baseline Imager (ABI) on the next generation GOES-R series. Imagery with a refresh rate of 1 min of many phenomena were acquired, including clouds, convection, fires, smoke, and hurricanes, including 6 days of Hurricane Sandy through landfall. NOAA had never before operated a GOES in a nearly continuous 1-min mode for such an extended period of time, thereby making these unique datasets to explore the future capabilities possible with GOES-R. The next generation GOES-R imager will be able to routinely take mesoscale (1000 km x 1000 km) images every 30 s (or two separate locations every minute). These images can be acquired even while scanning continental United States and full disk images. These high time-resolution images from the GOES-14 imager are being used to prepare for the GOES-R era and its advanced imager. This includes both the imagery and quantitative derived products such as cloud-top cooling. Several animations are included to showcase the rapid change of the many phenomena observed during super rapid scan operations for GOES-R (SRSOR). (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI. C1 [Schmit, Timothy J.] NOAA Ctr Satellite Applicat & Res, Adv Satellite Prod Branch, Madison, WI 53706 USA. [Goodman, Steven J.] NOAA NESDIS GOES R Program Off, Greenbelt, MD 20771 USA. [Lindsey, Daniel T.] NOAA Ctr Satellite Applicat & Res, Ft Collins, CO 80523 USA. [Rabin, Robert M.] NOAA NSSL, Norman, OK 73072 USA. [Bedka, Kristopher M.] NASA Langley Res Ctr, Sci Syst & Applicat Inc, Climate Sci Branch, Hampton, VA 23666 USA. [Gunshor, Mathew M.; Cintineo, John L.; Velden, Christopher S.; Bachmeier, A. Scott; Lindstrom, Scott S.; Schmidt, Christopher C.] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI 53706 USA. RP Schmit, TJ (reprint author), NOAA Ctr Satellite Applicat & Res, Adv Satellite Prod Branch, 1225 West Dayton St, Madison, WI 53706 USA. EM Tim.J.Schmit@noaa.gov RI Schmit, Timothy/F-5624-2010; Lindsey, Dan/F-5607-2010 OI Lindsey, Dan/0000-0002-0967-5683 NR 18 TC 9 Z9 9 U1 1 U2 13 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD DEC 16 PY 2013 VL 7 AR 073462 DI 10.1117/1.JRS.7.073462 PG 20 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 287EH UT WOS:000329523300002 ER PT J AU Refaat, TF Ismail, S Nehrir, AR Hair, JW Crawford, JH Leifer, I Shuman, T AF Refaat, Tamer F. Ismail, Syed Nehrir, Amin R. Hair, John W. Crawford, James H. Leifer, Ira Shuman, Timothy TI Performance evaluation of a 1.6-mu m methane DIAL system from ground, aircraft and UAV platforms SO OPTICS EXPRESS LA English DT Article ID DIFFERENTIAL ABSORPTION LIDAR; SPECTRAL-RESOLUTION LIDAR; FREQUENCY STABILIZATION; SENSITIVITY-ANALYSIS; CO2; AIRBORNE; CH4; OZONE; RETRIEVAL AB Methane is an efficient absorber of infrared radiation and a potent greenhouse gas with a warming potential 72 times greater than carbon dioxide on a per molecule basis. Development of methane active remote sensing capability using the differential absorption lidar (DIAL) technique enables scientific assessments of the gas emission and impacts on the climate. A performance evaluation of a pulsed DIAL system for monitoring atmospheric methane is presented. This system leverages a robust injection-seeded pulsed Nd:YAG pumped Optical Parametric Oscillator (OPO) laser technology operating in the 1.645 mu m spectral band. The system also leverages an efficient low noise, commercially available, InGaAs avalanche photo-detector (APD). Lidar signals and error budget are analyzed for system operation on ground in the range-resolved DIAL mode and from airborne platforms in the integrated path DIAL (IPDA) mode. Results indicate system capability of measuring methane concentration profiles with < 1.0% total error up to 4.5 km range with 5 minute averaging from ground. For airborne IPDA, the total error in the column dry mixing ratio is less than 0.3% with 0.1 sec average using ground returns. This system has a unique capability of combining signals from the atmospheric scattering from layers above the surface with ground return signals, which provides methane column measurement between the atmospheric scattering layer and the ground directly. In such case 0.5% and 1.2% total errors are achieved with 10 sec average from airborne platforms at 8 km and 15.24 km altitudes, respectively. Due to the pulsed nature of the transmitter, the system is relatively insensitive to aerosol and cloud interferences. Such DIAL system would be ideal for investigating high latitude methane releases over polar ice sheets, permafrost regions, wetlands, and over ocean during day and night. This system would have commercial potential for fossil fuel leaks detection and industrial monitoring applications. (C) 2013 Optical Society of America C1 [Refaat, Tamer F.] Old Dominion Univ, Appl Res Ctr, Newport News, VA 23606 USA. [Ismail, Syed; Nehrir, Amin R.; Hair, John W.; Crawford, James H.] NASA, Langley Res Ctr, Atmospher Sci Div, Hampton, VA 23681 USA. [Leifer, Ira] Bubbleol Res Int Inc, Goleta, CA 93117 USA. [Shuman, Timothy] Fibertek Inc, Herndon, VA 20171 USA. RP Refaat, TF (reprint author), Old Dominion Univ, Appl Res Ctr, Newport News, VA 23606 USA. EM trefaat@odu.edu NR 37 TC 9 Z9 9 U1 6 U2 54 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD DEC 16 PY 2013 VL 21 IS 25 BP 30415 EP 30432 DI 10.1364/OE.21.030415 PG 18 WC Optics SC Optics GA 273ZV UT WOS:000328575700028 PM 24514619 ER PT J AU Aartsen, MG Abbasi, R Ackermann, M Adams, J Aguilar, JA Ahlers, M Altmann, D Arguelles, C Auffenberg, J Bai, X Baker, M Barwick, SW Baum, V Bay, R Beatty, JJ Tjus, JB Becker, KH BenZvi, S Berghaus, P Berley, D Bernardini, E Bernhard, A Besson, DZ Binder, G Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bose, D Boser, S Botner, O Brayeur, L Bretz, HP Brown, AM Bruijn, R Casey, J Casier, M Chirkin, D Christov, A Christy, B Clark, K Clevermann, F Coenders, S Cohen, S Cowen, DF Silva, AHC Danninger, M Daughhetee, J Davis, JC Day, M De Clercq, C De Ridder, S Desiati, P de Vries, KD de With, M DeYoung, T Diaz-Velez, JC Dunkman, M Eagan, R Eberhardt, B Eisch, J Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feintzeig, J Feusels, T Filimonov, K Finley, C Fischer-Wasels, T Flis, S Franckowiak, A Frantzen, K Fuchs, T Gaisser, TK Gallagher, J Gerhardt, L Gladstone, L Glusenkamp, T Goldschmidt, A Golup, G Gonzalez, JG Goodman, JA Gora, D Grandmont, DT Grant, D Gretskov, P Groh, JC Gross, A Ha, C Ismail, AH Hallen, P Hallgren, A Halzen, F Hanson, K Heereman, D Heinen, D Helbing, K Hellauer, R Hickford, S Hill, GC Hoffman, KD Hoffmann, R Homeier, A Hoshina, K Huelsnitz, W Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobi, E Jacobsen, J Jagielski, K Japaridze, GS Jero, K Jlelati, O Kaminsky, B Kappes, A Karg, T Karle, A Kauer, M Kelley, JL Kiryluk, J Klas, J Klein, SR Kohne, JH Kohnen, G Kolanoski, H Kopke, L Kopper, C Kopper, S Koskinen, DJ Kowalski, M Krasberg, M Kriesten, A Krings, K Kroll, G Kunnen, J Kurahashi, N Kuwabara, T Labare, M Landsman, H Larson, MJ Lesiak-Bzdak, M Leuermann, M Leute, J Lunemann, J Macias, O Madsen, J Maggi, G Maruyama, R Mase, K Matis, HS McNally, F Meagher, K Merck, M Meures, T Miarecki, S Middell, E Milke, N Miller, J Mohrmann, L Montaruli, T Morse, R Nahnhauer, R Naumann, U Niederhausen, H Nowicki, SC Nygren, DR Obertacke, A Odrowski, S Olivas, A Omairat, A O'Murchadha, A Paul, L Pepper, JA de los Heros, CP Pfendner, C Pieloth, D Pinat, E Posselt, J Price, PB Przybylski, GT Radel, L Rameez, M Rawlins, K Redl, P Reimann, R Resconi, E Rhode, W Ribordy, M Richman, M Riedel, B Rodrigues, JP Rott, C Ruhe, T Ruzybayev, B Ryckbosch, D Saba, SM Sander, HG Santander, M Sarkar, S Schatto, K Scheriau, F Schmidt, T Schmitz, M Schoenen, S Schoneberg, S Schonwald, A Schukraft, A Schulte, L Schulz, O Seckel, D Sestayo, Y Seunarine, S Shanidze, R Sheremata, C Smith, MWE Soldin, D Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stanisha, NA Stasik, A Stezelberger, T Stokstad, RG Stossl, A Strahler, EA Strom, R Sullivan, GW Taavola, H Taboada, I Tamburro, A Tepe, A Ter-Antonyan, S Tesic, G Tilav, S Toale, PA Tobin, MN Toscano, S Unger, E Usner, M Vallecorsa, S van Eijndhoven, N van Overloop, A van Santen, J Vehring, M Voge, M Vraeghe, M Walck, C Waldenmaier, T Wallraff, M Weaver, C Wellons, M Wendt, C Westerhoff, S Whitehorn, N Wiebe, K Wiebusch, CH Williams, DR Wissing, H Wolf, M Wood, TR Woschnagg, K Xu, DL Xu, XW Yanez, JP Yodh, G Yoshida, S Zarzhitsky, P Ziemann, J Zierke, S Zoll, M AF Aartsen, M. G. Abbasi, R. Ackermann, M. Adams, J. Aguilar, J. A. Ahlers, M. Altmann, D. Arguelles, C. Auffenberg, J. Bai, X. Baker, M. Barwick, S. W. Baum, V. Bay, R. Beatty, J. J. Tjus, J. Becker Becker, K. -H. BenZvi, S. Berghaus, P. Berley, D. Bernardini, E. Bernhard, A. Besson, D. Z. Binder, G. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bose, D. Boeser, S. Botner, O. Brayeur, L. Bretz, H. -P. Brown, A. M. Bruijn, R. Casey, J. Casier, M. Chirkin, D. Christov, A. Christy, B. Clark, K. Clevermann, F. Coenders, S. Cohen, S. Cowen, D. F. Silva, A. H. Cruz Danninger, M. Daughhetee, J. Davis, J. C. Day, M. De Clercq, C. De Ridder, S. Desiati, P. de Vries, K. D. de With, M. DeYoung, T. Diaz-Velez, J. C. Dunkman, M. Eagan, R. Eberhardt, B. Eisch, J. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feintzeig, J. Feusels, T. Filimonov, K. Finley, C. Fischer-Wasels, T. Flis, S. Franckowiak, A. Frantzen, K. Fuchs, T. Gaisser, T. K. Gallagher, J. Gerhardt, L. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Golup, G. Gonzalez, J. G. Goodman, J. A. Gora, D. Grandmont, D. T. Grant, D. Gretskov, P. Groh, J. C. Gross, A. Ha, C. Ismail, A. Haj Hallen, P. Hallgren, A. Halzen, F. Hanson, K. Heereman, D. Heinen, D. Helbing, K. Hellauer, R. Hickford, S. Hill, G. C. Hoffman, K. D. Hoffmann, R. Homeier, A. Hoshina, K. Huelsnitz, W. Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jacobi, E. Jacobsen, J. Jagielski, K. Japaridze, G. S. Jero, K. Jlelati, O. Kaminsky, B. Kappes, A. Karg, T. Karle, A. Kauer, M. Kelley, J. L. Kiryluk, J. Klaes, J. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koepke, L. Kopper, C. Kopper, S. Koskinen, D. J. Kowalski, M. Krasberg, M. Kriesten, A. Krings, K. Kroll, G. Kunnen, J. Kurahashi, N. Kuwabara, T. Labare, M. Landsman, H. Larson, M. J. Lesiak-Bzdak, M. Leuermann, M. Leute, J. Luenemann, J. Macias, O. Madsen, J. Maggi, G. Maruyama, R. Mase, K. Matis, H. S. McNally, F. Meagher, K. Merck, M. Meures, T. Miarecki, S. Middell, E. Milke, N. Miller, J. Mohrmann, L. Montaruli, T. Morse, R. Nahnhauer, R. Naumann, U. Niederhausen, H. Nowicki, S. C. Nygren, D. R. Obertacke, A. Odrowski, S. Olivas, A. Omairat, A. O'Murchadha, A. Paul, L. Pepper, J. A. de los Heros, C. Perez Pfendner, C. Pieloth, D. Pinat, E. Posselt, J. Price, P. B. Przybylski, G. T. Raedel, L. Rameez, M. Rawlins, K. Redl, P. Reimann, R. Resconi, E. Rhode, W. Ribordy, M. Richman, M. Riedel, B. Rodrigues, J. P. Rott, C. Ruhe, T. Ruzybayev, B. Ryckbosch, D. Saba, S. M. Sander, H. -G. Santander, M. Sarkar, S. Schatto, K. Scheriau, F. Schmidt, T. Schmitz, M. Schoenen, S. Schoeneberg, S. Schoenwald, A. Schukraft, A. Schulte, L. Schulz, O. Seckel, D. Sestayo, Y. Seunarine, S. Shanidze, R. Sheremata, C. Smith, M. W. E. Soldin, D. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stanisha, N. A. Stasik, A. Stezelberger, T. Stokstad, R. G. Stoessl, A. Strahler, E. A. Strom, R. Sullivan, G. W. Taavola, H. Taboada, I. Tamburro, A. Tepe, A. Ter-Antonyan, S. Tesic, G. Tilav, S. Toale, P. A. Tobin, M. N. Toscano, S. Unger, E. Usner, M. Vallecorsa, S. van Eijndhoven, N. van Overloop, A. van Santen, J. Vehring, M. Voge, M. Vraeghe, M. Walck, C. Waldenmaier, T. Wallraff, M. Weaver, Ch. Wellons, M. Wendt, C. Westerhoff, S. Whitehorn, N. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wissing, H. Wolf, M. Wood, T. R. Woschnagg, K. Xu, D. L. Xu, X. W. Yanez, J. P. Yodh, G. Yoshida, S. Zarzhitsky, P. Ziemann, J. Zierke, S. Zoll, M. CA IceCube Collaboration TI Probing the origin of cosmic rays with extremely high energy neutrinos using the IceCube Observatory SO PHYSICAL REVIEW D LA English DT Article ID COSMOGENIC NEUTRINOS; FERMI-LAT; SPECTRUM; LIMIT; PERFORMANCE; COMPONENT; SELECTION; SYSTEM; MODEL; FLUX AB We have searched for extremely high energy neutrinos using data taken with the IceCube detector between May 2010 and May 2012. Two neutrino-induced particle shower events with energies around 1 PeV were observed, as reported previously. In this work, we investigate whether these events could originate from cosmogenic neutrinos produced in the interactions of ultrahigh energy cosmic rays with ambient photons while propagating through intergalactic space. Exploiting IceCube's large exposure for extremely high energy neutrinos and the lack of observed events above 100 PeV, we can rule out the corresponding models at more than 90% confidence level. The model-independent quasidifferential 90% C. L. upper limit, which amounts to E-2 phi(nu e)+(nu mu)+(nu tau) = 1.2 x 10(-7) GeV cm(-2) s(-1) sr(-1) at 1 EeV, provides the most stringent constraint in the energy range from 10 PeV to 10 EeV. Our observation disfavors strong cosmological evolution of the highest energy cosmic-ray sources such as the Fanaroff-Riley type II class of radio galaxies. C1 [Bissok, M.; Blumenthal, J.; Coenders, S.; Euler, S.; Gretskov, P.; Hallen, P.; Heinen, D.; Jagielski, K.; Kriesten, A.; Krings, K.; Leuermann, M.; Paul, L.; Raedel, L.; Reimann, R.; Schoenen, S.; Schukraft, A.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.; Zierke, S.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Aartsen, M. G.; Hill, G. C.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Bay, R.; Binder, G.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Binder, G.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [de With, M.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Tjus, J. Becker; Fedynitch, A.; Saba, S. M.; Schoeneberg, S.; Unger, E.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany. [Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Schulte, L.; Stasik, A.; Usner, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.; Pinat, E.] Univ Libre Bruxelles, Fac Sci, B-1050 Brussels, Belgium. [Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; Golup, G.; Kunnen, J.; Maggi, G.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Adams, J.; Brown, A. M.; Hickford, S.; Macias, O.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Berley, D.; Blaufuss, E.; Christy, B.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Koskinen, D. J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Clevermann, F.; Frantzen, K.; Fuchs, T.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.; Scheriau, F.; Schmitz, M.; Ziemann, J.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany. [Grandmont, D. T.; Grant, D.; Nowicki, S. C.; Odrowski, S.; Sheremata, C.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Altmann, D.; Gora, D.; Kappes, A.] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Aguilar, J. A.; Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland. [De Ridder, S.; Feusels, T.; Ismail, A. Haj; Jlelati, O.; Labare, M.; Ryckbosch, D.; van Overloop, A.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium. [Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bruijn, R.; Cohen, S.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Abbasi, R.; Ahlers, M.; Arguelles, C.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Tobin, M. N.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Abbasi, R.; Ahlers, M.; Arguelles, C.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Tobin, M. N.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA. [Baum, V.; Eberhardt, B.; Koepke, L.; Kroll, G.; Luenemann, J.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany. [Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Bernhard, A.; Gross, A.; Leute, J.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany. [Bai, X.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Bartol Res Inst, Newark, DC 19716 USA. [Bai, X.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.] Univ Delaware, Dept Phys & Astron, Newark, DC 19716 USA. [Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Bose, D.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea. [Clark, K.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Larson, M. J.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Cowen, D. F.; DeYoung, T.; Dunkman, M.; Eagan, R.; Groh, J. C.; Smith, M. W. E.; Stanisha, N. A.; Tesic, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Boersma, D. J.; Botner, O.; Hallgren, A.; de los Heros, C. Perez; Strom, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Helbing, K.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Omairat, A.; Posselt, J.; Soldin, D.; Tepe, A.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany. [Ackermann, M.; Berghaus, P.; Bernardini, E.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Jacobi, E.; Kaminsky, B.; Karg, T.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Shanidze, R.; Spiering, C.; Stoessl, A.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany. [Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA. [Montaruli, T.] Dipartimento Fis, Sez INFN, I-70126 Bari, Italy. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ishihara, A (reprint author), Chiba Univ, Dept Phys, Chiba 2638522, Japan. EM aya@hepburn.s.chiba-u.ac.jp; mase@hepburn.s.chiba-u.ac.jp; syoshida@hepburn.s.chiba-u.ac.jp RI Taavola, Henric/B-4497-2011; Tjus, Julia/G-8145-2012; Wiebusch, Christopher/G-6490-2012; Auffenberg, Jan/D-3954-2014; Koskinen, David/G-3236-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011; OI Groh, John/0000-0001-9880-3634; Taavola, Henric/0000-0002-2604-2810; Perez de los Heros, Carlos/0000-0002-2084-5866; Arguelles Delgado, Carlos/0000-0003-4186-4182; Schukraft, Anne/0000-0002-9112-5479; Wiebusch, Christopher/0000-0002-6418-3008; Auffenberg, Jan/0000-0002-1185-9094; Koskinen, David/0000-0002-0514-5917; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Rott, Carsten/0000-0002-6958-6033; Ter-Antonyan, Samvel/0000-0002-5788-1369 FU U.S. National Science Foundation - Office of Polar Programs; U.S. National Science Foundation - Physics Division; University of Wisconsin Alumni Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin Madison; Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy; National Energy Research Scientific Computing Center; Louisiana Optical Network Initiative (LONI); Natural Sciences and Engineering Research Council of Canada; WestGrid and Compute/Calcul Canada; Swedish Research Council; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Helmholtz Alliance for Astroparticle Physics (HAP); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus Programme; Flanders Institute to encourage scientific and technological research in industry (IWT); Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF) FX We acknowledge the support from the following agencies: U.S. National Science Foundation - Office of Polar Programs, U.S. National Science Foundation - Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada, WestGrid and Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus Programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF). NR 63 TC 40 Z9 41 U1 0 U2 12 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD DEC 16 PY 2013 VL 88 IS 11 AR 112008 DI 10.1103/PhysRevD.88.112008 PG 15 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 275QS UT WOS:000328692900001 ER PT J AU Kharuk, VI Im, ST Oskorbin, PA Petrov, IA Ranson, KJ AF Kharuk, V. I. Im, S. T. Oskorbin, P. A. Petrov, I. A. Ranson, K. J. TI Siberian pine decline and mortality in southern siberian mountains SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Climate-induced tree mortality; Drought impact on forests; Tree die-off; Siberian pine decline ID CLIMATE-CHANGE; SEVERE DROUGHT; ASPEN FORESTS; GLOBAL-CHANGE; DIE-OFF; DYNAMICS; STANDS; CARBON; SWITZERLAND; ADAPTATION AB The causes and resulting spatial patterns of Siberian pine mortality in eastern Kuznetzky Alatau Mountains, Siberia were analyzed based on satellite (Landsat, MODIS) and dendrochronology data. Climate variables studied included temperature, precipitation and Standardized Precipitation-Evapotranspiration Index (SPEI) drought index. Landsat data analysis showed that stand mortality was first detected in the year 2006 at an elevation of 650 m, and extended up to 900 m by the year 2012. Mortality was accompanied by a decrease in MODIS-derived vegetation index (EVI). The area of dead stands and the upper mortality line were correlated with increased drought. The uphill margin of mortality was limited by elevational precipitation gradients. Dead stands (i.e., >75% tree mortality) were located mainly on southern slopes. With respect to slope, mortality was observed within a 7-20 degrees range with greatest mortality occurring on convex terrain. Tree radial increment measurements correlate and were synchronous with SPEI (r(2) = 0.37, r(s) = 80). The results also showed the primary role of drought stress on Siberian pine mortality. A secondary role may be played by bark beetles and root fungi attacks. The observed Siberian pine mortality is part of a broader phenomenon of "dark needle conifers" (DNC, i.e., Siberian pine, fir and spruce) decline and mortality in European Russia, Siberia, and the Russian Far East. All locations of DNC decline coincided with areas of observed drought increase. The results obtained are one of the first observations of drought-induced decline and mortality of DNC at the southern border of boreal forests. Meanwhile if model projections of increased aridity are correct DNC within the southern part of its areal may be replaced by drought-resistant Pinus silvestris and Larix (C) 2013 Elsevier B.V. All rights reserved. C1 [Kharuk, V. I.; Im, S. T.; Oskorbin, P. A.; Petrov, I. A.] Siberian Fed Univ, VN Sukachev Inst Forest, Krasnoyarsk, Russia. [Ranson, K. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kharuk, VI (reprint author), Siberian Fed Univ, VN Sukachev Inst Forest, Krasnoyarsk, Russia. EM kharuk@ksc.krasn.ru RI Im, Sergei/J-2736-2016 OI Im, Sergei/0000-0002-5794-7938 FU NASA's Science Mission Directorate; SB RAS Program [30.25] FX This research was supported from NASA's Science Mission Directorate and the SB RAS Program No. 30.25. NR 50 TC 16 Z9 19 U1 3 U2 34 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 EI 1872-7042 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD DEC 15 PY 2013 VL 310 BP 312 EP 320 DI 10.1016/j.foreco.2013.08.042 PG 9 WC Forestry SC Forestry GA 302JO UT WOS:000330601000032 ER PT J AU Omelon, CR Brady, AL Slater, GF Laval, B Lim, DSS Southam, G AF Omelon, Christopher R. Brady, Allyson L. Slater, Greg F. Laval, Bernard Lim, Darlene S. S. Southam, Gordon TI Microstructure variability in freshwater microbialites, Pavilion Lake, Canada SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Carbonate precipitation; Freshwater microbialite; Calcite; Bacteria; Biosignature; Electron microscopy; Synchrotron micro-X-ray fluorescence spectroscopy ID MODERN MARINE STROMATOLITES; CYANOBACTERIAL CALCIFICATION; CARBONATE PRECIPITATION; BRITISH-COLUMBIA; ENVIRONMENT; MINERALS; CALCITE; TURKEY; REEF; MATS AB Calcite microbialites in Pavilion Lake, British Columbia, exhibit a diverse range in macro-morphology, biomass abundance, porosity, and mineral content To evaluate the role of microorganisms in their formation, samples collected from a range of depths were examined by scanning electron microscopy (SEM) and synchrotron radiation-based micro-X-ray fluorescence (mu-XRF) spectroscopy to characterize both their outer surfaces as well as internal structures. Observed trends in both surface colonization as well as microbialite framework with increasing lake depth include decreasing microbial abundance on outer surfaces as well as increasing ratios of carbonate :biomass in the microbialites. Microscopic investigations of the interiors show bacteria and algae entrapped within calcite, with this calate exhibiting micropores and casts similar in size and shape to microorganisms. Based on these observations, it is hypothesized that microbialite development in Pavilion Lake initiates calcite precipitation in phototrophic microbial mats, i.e., combined phototrophy and heterotrophy, followed by heterotrophic oxidation of organic matter leading to eventual carbonate infilling of the microbial-mineral matrix. In addition, an observed shift from cyanobacteria to algae with increasing lake depth suggests variability in contemporary conditions controlling microbialite growth and diagenesis. High photosynthetic growth rates at shallower depths result in significant porosity and friability due to biomass accumulation outpacing carbonate precipitation. At intermediate depths, lower light levels and slower growth rates of phototrophs lead to a greater proportion of the microbialite matrix being in-filled by carbonate. Carbonates precipitate initially within the bacteria-EPS matrix, with abundant uncalcified algae maintaining microbialite porosity. In the deepest waters, the presence of only sparse algal colonization as well as fine-grained, laminated metal-rich sediments covering microbialites suggests that present-day insolation levels are too low to support the development of photosynthetic microbial mats. As a consequence, heterotrophic carbonate precipitation has progressively in-filled these microbialite interiors to create lithified calcite fabrics that exhibit minimal porosity but preserve the casts of microorganisms as biosignatures. While the origin of microbialites in Pavilion Lake remains unknown, current observations provide valuable information in evaluating how environmental conditions influence microbialite growth in a freshwater, lacustrine environment Published by Elsevier B.V. C1 [Omelon, Christopher R.; Southam, Gordon] Univ Western Ontario, Dept Earth Sci, London, ON N6A 5B7, Canada. [Brady, Allyson L.; Slater, Greg F.] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON L8S 4K1, Canada. [Laval, Bernard] Univ British Columbia, Dept Civil Engn, Vancouver, BC V6T 1Z4, Canada. [Lim, Darlene S. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Omelon, CR (reprint author), Univ Texas Austin, Dept Geol Sci, 2275 Speedway,Mail Stop C-9000, Austin, TX 78712 USA. EM omelon@jsg.utexas.edu RI Laval, Bernard/J-9861-2012; Southam, Gordon/D-1983-2013 OI Southam, Gordon/0000-0002-8941-1249 FU Canadian Space Agency; NASA MMAMA; NASA DIO Analogs program; Natural Sciences and Engineering Research Council of Canada FX The authors would like to thank the Pavilion Lake Research Project for logistical support and sample collection, as well as Todd Simpson and Tim Goldhawk at the Nanofabrication Facility at Western University and Robert Gordon at the Advanced Photon Source for technical expertise. We acknowledge the Canadian Space Agency for funding to D. Lim and G. Slater; a NASA MMAMA grant to D. Lim as well as additional support from the NASA DIO Analogs program, and the Natural Sciences and Engineering Research Council of Canada for support for G. Southam, C.R. Omelon and A.L. Brady. We also thank Dr. D.J. Bottjer and two anonymous reviewers for their constructive comments that greatly improved the original manuscript. This is PLRP publication #13-08. NR 37 TC 7 Z9 7 U1 3 U2 43 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD DEC 15 PY 2013 VL 392 BP 62 EP 70 DI 10.1016/j.palaeo.2013.08.017 PG 9 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 300UB UT WOS:000330488400006 ER PT J AU Chandra, R Gopalswamy, N Makela, P Xie, H Yashiro, S Akiyama, S Uddin, W Srivastava, AK Joshi, NC Jain, R Awasthi, AK Manoharan, PK Mahalakshmi, K Dwivedi, VC Choudhary, DP Nitta, NV AF Chandra, R. Gopalswamy, N. Maekelae, P. Xie, H. Yashiro, S. Akiyama, S. Uddin, W. Srivastava, A. K. Joshi, N. C. Jain, R. Awasthi, A. K. Manoharan, P. K. Mahalakshmi, K. Dwivedi, V. C. Choudhary, D. P. Nitta, N. V. TI Solar energetic particle events during the rise phases of solar cycles 23 and 24 SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Solar energetic particles; Type II radio bursts; Coronal mass ejections; Flares ID CORONAL MASS EJECTIONS; NORTH-SOUTH ASYMMETRY; FLARES; FIELD; WIND; CMES; INTENSITY; EVOLUTION; ERUPTIONS; FILAMENT AB We present a comparative study of the properties of coronal mass ejections (CMEs) and flares associated with the solar energetic particle (SEP) events in the rising phases of solar cycles (SC) 23(1996-1998) (22 events) and 24(2009-2011) (20 events), which are associated with type II radio bursts. Based on the SEP intensity, we divided the events into three categories, i.e. weak (intensity < 1 pfu), minor ( I pfu < intensity < 10 pfu) and major (intensity >= 10 pfu) events. We used the GOES data for the minor and major SEP events and SOHO/ERNE data for the weak SEP event. We examine the correlation of SEP intensity with flare size and CME properties. We find that most of the major SEP events are associated with halo or partial halo CMEs originating close to the sun center and western-hemisphere. The fraction of halo CMEs in SC 24 is larger than the SC 23. For the minor SEP events one event in SC23 and one event in SC24 have widths < 120 degrees and all other events are associated with halo or partial halo CMEs as in the case of major SEP events. In case of weak SEP events, majority (more than 60%) of events are associated with CME width < 120 degrees. For both the SC the average CMEs speeds are similar. For major SEP events, average CME speeds are higher in comparison to minor and weak events. The SEP event intensity and GOES X-ray flare size are poorly correlated. During the rise phase of solar cycle 23 and 24, we find north south asymmetry in the SEP event source locations: in cycle 23 most sources are located in the south, whereas during cycle 24 most sources are located in the north. This result is consistent with the asymmetry found with sunspot area and intense flares. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Chandra, R.] Kumaun Univ, Dept Phys, Naini Tal 263002, India. [Gopalswamy, N.; Maekelae, P.; Xie, H.; Yashiro, S.; Akiyama, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Uddin, W.; Srivastava, A. K.; Joshi, N. C.] ARIES, Naini Tal 263129, India. [Jain, R.; Awasthi, A. K.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. [Manoharan, P. K.; Mahalakshmi, K.; Dwivedi, V. C.] TIFR NCRA Radio Astron Ctr, Ooty 643001, India. [Choudhary, D. P.] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. [Nitta, N. V.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. RP Chandra, R (reprint author), Kumaun Univ, Dept Phys, DSB Campus, Naini Tal 263002, India. EM rchandra.ntl@gmail.com RI Awasthi, Arun/H-5596-2016; OI Awasthi, Arun/0000-0001-5313-1125; Manoharan, Periasamy K/0000-0003-4274-211X FU ISRO/RESPOND [ISRO/RES/2/379/12-13] FX The authors thank the anonymous referee's for their comments and suggestions, which improve the paper considerably. This study was conducted as a part of the Indo-US Science and Technology Forum's Joint Center on Solar Eruptive events. We acknowledge the open data policy of NGDC, ERNE, SOHO and SDO. RC, WU and AKS also acknowledge the partial support from ISRO/RESPOND project no. ISRO/RES/2/379/12-13. NR 33 TC 2 Z9 2 U1 0 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD DEC 15 PY 2013 VL 52 IS 12 BP 2102 EP 2111 DI 10.1016/j.asr.2013.09.006 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 280CJ UT WOS:000329006000006 ER PT J AU Schmidt, ME Schrader, CM McCoy, TJ AF Schmidt, Mariek E. Schrader, Christian M. McCoy, Timothy J. TI The primary fO(2) of basalts examined by the Spirit rover in Gusev Crater, Mars: Evidence for multiple redox states in the martian interior SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Mars; Gusev basalts; oxygen fugacity; Mossbauer spectrometer ID OXYGEN FUGACITY; OXIDATION-STATE; UPPER-MANTLE; LHERZOLITIC SHERGOTTITES; GEOCHEMICAL VARIATIONS; PETROGENETIC MODEL; MINERAL CHEMISTRY; MERIDIANI-PLANUM; EARTHS MANTLE; OLIVINE AB The primary oxygen fugacity (fO(2)) of basaltic melts reflects the mantle source oxidation state, dictates the crystallizing assemblage, and determines how the magma will evolve. Basalts examined by the Spirit Mars Exploration Rover in Gusev Crater range from the K-poor Adirondack class (0.02 wt% K2O) to K-rich Backstay class (up to 1.2 wt% K2O) and exhibit substantially more variation than observed in martian basaltic meteorites. The ratios of ferric to total iron (Fe3+/Fe-T) measured by the Mossbauer spectrometer are high (equivalent to -0.76 to +2.98 Delta QFM; quartz-fayalite-magnetite buffer as defined by Wones and Gilbert, 1969), reflecting secondary Fe3+ phases. By combining the Fe3+/FeT of the igneous minerals (olivine, pyroxene, and magnetite) determined by Mossbauer spectrometer, we estimate primary fO(2) for the Gusev basalts to be 3.6 to 0.5 QFM. Estimating the fO(2) as a function of the dependence of the CIPW normative fayalite/magnetite ratios on Fe-3_/Fe-T yields a slightly smaller range of -2.58 to +0.57 Delta QFM. General similarity between the fO(2) estimated for the Gusev basalts and ranges in fO(2) for the shergottitic meteorites (-3.8 to 0.2 Delta QFM; Herd, 2003; Goodrich et al., 2003) suggests that the overall range of fO(2) for the martian igneous rocks and mantle is relatively restricted. Like the shergottites (Herd, 2003), estimated fO(2) of three Gusev classes (Adirondack, Barnhill and Irvine) correlates with a proxy for LREE enrichment (K2O/TiO2). This suggests mixing between melts or fluids derived from reservoirs with contrasting fO(2) and REE characteristics. Oxygen fugacity estimates for the martian interior suggest that tectonic processes have not led to sufficient recycling of oxidized surface material into the martian interior to entirely affect the overall oxidation state of the mantle. (C) 2013 Published by Elsevier B.V. C1 [Schmidt, Mariek E.] Brock Univ, Dept Earth Sci, St Catharines, ON L2S 3A1, Canada. [Schrader, Christian M.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35813 USA. [McCoy, Timothy J.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. RP Schmidt, ME (reprint author), Brock Univ, Dept Earth Sci, St Catharines, ON L2S 3A1, Canada. EM mschmidt2@brocku.ca; Christian.Schrader@ColoradoCollege.edu; mccoyt@si.edu FU NSERC; NASA FX We are grateful to reviews by Chris Herd and one anonymous reviewer. This work was supported by an NSERC Discovery Grant to M. Schmidt and by a NASA Athena Participating Scientist Grant to T. McCoy. We also acknowledge the MER Science and Engineering Team for their contributions to the success of the mission. NR 66 TC 7 Z9 7 U1 2 U2 24 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD DEC 15 PY 2013 VL 384 BP 198 EP 208 DI 10.1016/j.epsl.2013.10.005 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 277FM UT WOS:000328804400019 ER PT J AU Bowman, RC Payzant, EA Wilson, PR Pearson, DP Ledovskikh, A Danilov, D Notten, PHL An, K Skorpenske, HD Wood, DL AF Bowman, R. C., Jr. Payzant, E. A. Wilson, P. R. Pearson, D. P. Ledovskikh, A. Danilov, D. Notten, P. H. L. An, K. Skorpenske, H. D. Wood, D. L. TI Characterization and analyses of degradation and recovery of LaNi4.78Sn0.22 hydrides following thermal aging SO JOURNAL OF ALLOYS AND COMPOUNDS LA English DT Article DE La-Ni-Sn alloys; Pressure-composition isotherms; Hydride degradation behavior; Statistical thermodynamics modeling; Neutron powder diffraction ID ELECTROCHEMICAL CYCLING STABILITY; PRODUCE 20 K; FORMING COMPOUNDS; HYDROGEN ABSORPTION; METAL-HYDRIDES; ALLOYS AB LaNi4.78Sn0.22Hx hydride samples were held at a hydrogen content of x>5.0 (x is H/La atomic ratio) and temperatures above 465 K to accelerate the intrinsic degradation processes. Although Sn-substituted alloys are much more resistant to disproportionation than nearly all other LaNi5 alloys, the present test conditions did produce substantial degradation. Effects observed included reduction in hydrogen storage capacity, decreases in the plateau pressures, increased slopes of the plateaus, and smaller hysteresis ratios. A regeneration process nearly completely restored the behavior of the degraded LaNi4.78Sn0.22 hydride to its initial value. First-principles chemical reaction kinetics and statistical thermodynamics simulations have replicated experimental pressure-composition hydrogen gas absorption isotherms for both initial and degraded LaNi4.75Sn0.22 hydride. Neutron diffraction characterization of phase compositions, crystal structures, and hydrogen content have been performed on undamaged, degraded, and regenerated LaNi4.78Sn0.22 deuterides. (C) 2013 Elsevier B.V. All rights reserved. C1 [Bowman, R. C., Jr.; Payzant, E. A.; An, K.; Skorpenske, H. D.; Wood, D. L.] Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA. [Wilson, P. R.; Pearson, D. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ledovskikh, A.; Danilov, D.; Notten, P. H. L.] Eindhoven Univ Technol, NL-5600 MB Eindhoven, Netherlands. RP Bowman, RC (reprint author), Oak Ridge Natl Lab, POB 2008, Oak Ridge, TN 37831 USA. EM rcbjr1967@gmail.com RI Payzant, Edward/B-5449-2009; An, Ke/G-5226-2011; OI Payzant, Edward/0000-0002-3447-2060; An, Ke/0000-0002-6093-429X; Bowman, Robert/0000-0002-2114-1713 FU U.S. Department of Energy, Office of Energy Efficiency and Renewable Energy; Scientific User Facilities Division, Office of Basic Energy Sciences, U.S. Department of Energy; National Aeronautics and Space Administration (NASA) FX We wish to thank J.W. Reiter for supporting isotope exchange processing and Dr. A.D. Stoica, R.A. Mills, and R.W. Connatser for assistance with the neutron experiments. This work was partially supported by the U.S. Department of Energy, Office of Energy Efficiency and Renewable Energy. A portion of this research at ORNL's Spallation Neutron Source was sponsored by the Scientific User Facilities Division, Office of Basic Energy Sciences, U.S. Department of Energy. The Jet Propulsion Laboratory is operated by California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). NR 26 TC 3 Z9 3 U1 1 U2 12 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-8388 EI 1873-4669 J9 J ALLOY COMPD JI J. Alloy. Compd. PD DEC 15 PY 2013 VL 580 SU 1 BP S207 EP S210 DI 10.1016/j.jallcom.2013.03.129 PG 4 WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering GA 268LO UT WOS:000328172400054 ER PT J AU de Goncalves, LGG Borak, JS Costa, MH Saleska, SR Baker, I Restrepo-Coupe, N Muza, MN Poulter, B Verbeeck, H Fisher, JB Arain, MA Arkin, P Cestaro, BP Christoffersen, B Galbraith, D Guan, XD van den Hurk, BJJM Ichii, K Imbuzeiro, HMA Jain, AK Levine, N Lu, CQ Miguez-Macho, G Roberti, DR Sahoo, A Sakaguchi, K Schaefer, K Shi, MJ Shuttleworth, WJ Tian, HQ Yang, ZL Zeng, XB AF Goncalves de Goncalves, Luis Gustavo Borak, Jordan S. Costa, Marcos Heil Saleska, Scott R. Baker, Ian Restrepo-Coupe, Natalia Muza, Michel Nobre Poulter, Benjamin Verbeeck, Hans Fisher, Joshua B. Arain, M. Altaf Arkin, Phillip Cestaro, Bruno P. Christoffersen, Bradley Galbraith, David Guan, Xiaodan van den Hurk, Bart J. J. M. Ichii, Kazuhito Imbuzeiro, Hewlley M. Acioli Jain, Atul K. Levine, Naomi Lu, Chaoqun Miguez-Macho, Gonzalo Roberti, Debora R. Sahoo, Alok Sakaguchi, Koichi Schaefer, Kevin Shi, Mingjie Shuttleworth, W. James Tian, Hanqin Yang, Zong-Liang Zeng, Xubin TI Overview of the Large-Scale Biosphere-Atmosphere Experiment in Amazonia Data Model Intercomparison Project (LBA-DMIP) SO AGRICULTURAL AND FOREST METEOROLOGY LA English DT Article DE Land surface modeling; Energy, water and carbon budget; Amazonia; Model intercomparison ID GENERAL-CIRCULATION MODEL; SURFACE PARAMETERIZATION SIB2; CARBON-CYCLE FEEDBACKS; TRANSFER SCHEME LSX; LAND-SURFACE; STOMATAL CONDUCTANCE; TERRESTRIAL CARBON; GLOBAL CLIMATE; VEGETATION DYNAMICS; ECOSYSTEM MODEL AB A fundamental question connecting terrestrial ecology and global climate change is the sensitivity of key terrestrial biomes to climatic variability and change. The Amazon region is such a key biome: it contains unparalleled biological diversity, a globally significant store of organic carbon, and it is a potent engine driving global cycles of water and energy. The importance of understanding how land surface dynamics of the Amazon region respond to climatic variability and change is widely appreciated, but despite significant recent advances, large gaps in our understanding remain. Understanding of energy and carbon exchange between terrestrial ecosystems and the atmosphere can be improved through direct observations and experiments, as well as through modeling activities. Land surface/ecosystem models have become important tools for extrapolating local observations and understanding to much larger terrestrial regions. They are also valuable tools to test hypothesis on ecosystem functioning. Funded by NASA under the auspices of the LBA (the Large-Scale Biosphere-Atmosphere Experiment in Amazonia), the LBA Data Model Intercomparison Project (LBA-DMIP) uses a comprehensive data set from an observational network of flux towers across the Amazon, and an ecosystem modeling community engaged in ongoing studies using a suite of different land surface and terrestrial ecosystem models to understand Amazon forest function. Here an overview of this project is presented accompanied by a description of the measurement sites, data, models and protocol. (C) 2013 Elsevier B.V. All rights reserved. C1 [Goncalves de Goncalves, Luis Gustavo] CPTEC, Cachoeira Paulista, SP, Brazil. [Borak, Jordan S.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, Greenbelt, MD 20740 USA. [Borak, Jordan S.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Costa, Marcos Heil] Univ Fed Vicosa, Dept Agr Engn, BR-36570000 Vicosa, MG, Brazil. [Saleska, Scott R.; Restrepo-Coupe, Natalia; Christoffersen, Bradley] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. [Baker, Ian] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Restrepo-Coupe, Natalia] Univ Technol Sydney, Plant Funct Biol & Climate Change Cluster, Sydney, NSW 2007, Australia. [Muza, Michel Nobre] Inst Fed Santa Catarina, Florianopolis, SC, Brazil. [Poulter, Benjamin] LSCE, F-91191 Gif Sur Yvette, France. [Verbeeck, Hans] Univ Ghent, Fac Biosci Engn, Plant Ecol Lab, B-9000 Ghent, Belgium. [Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Arain, M. Altaf] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON L8S 4K1, Canada. [Arkin, Phillip] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, Cooperat Inst Climate & Satellites, College Pk, MD 20740 USA. [Cestaro, Bruno P.] Univ Sao Paulo, Dept Atmospher Sci, Sao Paulo, Brazil. [Galbraith, David] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. [Guan, Xiaodan] Lanzhou Univ, Coll Atmospher Sci, MOE, Key Lab Semiarid Climate Change, Lanzhou 730000, Peoples R China. [van den Hurk, Bart J. J. M.] Royal Netherlands Meteorol Inst, KNMI, NL-3730 AE De Bilt, Netherlands. [Ichii, Kazuhito] Fukushima Univ, Fac Symbiot Syst Sci, Fukushima 9601296, Japan. [Imbuzeiro, Hewlley M. Acioli] Univ Fed Vicosa, Grp Pesquisas Interacao Atmosfera Biosfera, Vicosa, MG, Brazil. [Jain, Atul K.] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA. [Levine, Naomi] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Lu, Chaoqun] Auburn Univ, Sch Forestry & Wildlife Sci, Int Ctr Climate & Global Change Res, Auburn, AL USA. [Miguez-Macho, Gonzalo] Univ Santiago de Compostela, Nonlinear Phys Grp, Santiago De Compostela, Spain. [Roberti, Debora R.] Univ Fed Santa Maria, Dept Phys, BR-97119900 Santa Maria, RS, Brazil. [Sahoo, Alok] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. [Sakaguchi, Koichi] Univ Arizona, Dept Atmospher Sci, Tucson, AZ 85271 USA. [Schaefer, Kevin] Univ Colorado, Natl Snow & Ice Data Ctr, UCB 449, Boulder, CO 80309 USA. [Shi, Mingjie] Univ Texas Austin, Jackson Sch Geosci, Dept Geol Sci, Austin, TX 78712 USA. [Shuttleworth, W. James] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Tian, Hanqin] Auburn Univ, Sch Forestry & Wildlife Sci, Int Ctr Climate & Global Change Res, Auburn, AL 36849 USA. [Yang, Zong-Liang] Univ Texas Austin, Jackson Sch Geosci, Ctr Integrated Earth Syst Sci, Austin, TX 78712 USA. [Zeng, Xubin] Univ Arizona, Dept Atmospher Sci, Tucson, AZ 85721 USA. RP de Goncalves, LGG (reprint author), CPTEC, Cachoeira Paulista, SP, Brazil. EM gustavo.goncalves@cptec.inpe.br; Jordan.Borak@nasa.gov; mhcosta@ufv.br; saleska@arizona.edu; baker@atmos.colostate.edu; ncoupe@email.arizona.edu; micmuza@gmail.com; Benjamin.Poulter@lsce.ipsl.fr; Hans.Verbeeck@UGent.be; jbfisher@jpl.nasa.gov; arainm@mcmaster.ca; parkin@essic.umd.edu; brunocesta@gmail.com; bchristo@arizona.edu; d.r.galbraith@leeds.ac.uk; guanxd@lzu.edu.cn; hurkvd@knmi.nl; kazuhito.ichii@gmail.com; jain1@illinois.edu; nlevine@oeb.harvard.edu; CZL0003@auburn.edu; gonzalo.miguez@usc.es; debora@ufsm.br; sahoo@princeton.edu; ksa@arizona.edu; kevin.schaefer@nsidc.org; mshi.lh@utexas.edu; shuttle@arizona.edu; tianhan@auburn.edu; liang@jsg.utexas.edu; xubin@atmo.arizona.edu RI Yang, Zong-Liang/B-4916-2011; Ichii, Kazuhito/D-2392-2010; Costa, Marcos/A-5695-2009; Tian, Hanqin/A-6484-2012; Restrepo-Coupe, Natalia/C-3507-2015; Guan, Xiaodan/K-6425-2016; Jain, Atul/D-2851-2016; OI Poulter, Benjamin/0000-0002-9493-8600; Levine, Naomi/0000-0002-4963-0535; Ichii, Kazuhito/0000-0002-8696-8084; Costa, Marcos/0000-0001-6874-9315; Tian, Hanqin/0000-0002-1806-4091; Restrepo-Coupe, Natalia/0000-0003-3921-1772; Guan, Xiaodan/0000-0003-3716-4503; Jain, Atul/0000-0002-4051-3228; Zeng, Xubin/0000-0001-7352-2764; Arain, M. Altaf/0000-0002-1433-5173; Fisher, Joshua/0000-0003-4734-9085 FU NASA [NNX09AL52G] FX Financial support comes from NASA Terrestrial Ecology Program Grant NNX09AL52G. Research contributed by J.B. Fisher was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. We thank the various individuals and modeling groups from Brazil, United States, Canada, Netherlands, England, Japan, Spain among other countries that, with limited or no funding sources, kindly devoted their time and efforts to the success of this project. We also thank the LBA scientists who obtained observations in the field including the Principal Investigators for the tower sites referenced as follows. NR 165 TC 16 Z9 16 U1 3 U2 49 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1923 EI 1873-2240 J9 AGR FOREST METEOROL JI Agric. For. Meteorol. PD DEC 15 PY 2013 VL 182 SI SI BP 111 EP 127 DI 10.1016/j.agrformet.2013.04.030 PG 17 WC Agronomy; Forestry; Meteorology & Atmospheric Sciences SC Agriculture; Forestry; Meteorology & Atmospheric Sciences GA 252JE UT WOS:000327000200012 ER PT J AU von Randow, C Zeri, M Restrepo-Coupe, N Muza, MN de Goncalves, LGG Costa, MH Araujo, AC Manzi, AO da Rocha, HR Saleska, SR Arain, MA Baker, IT Cestaro, BP Christoffersen, B Ciais, P Fisher, JB Galbraith, D Guan, XD Van den Hurk, B Ichii, K Imbuzeiro, H Jain, A Levine, N Miguez-Macho, G Poulter, B Roberti, DR Sahoo, A Schaefer, K Shi, MJ Tian, HQ Verbeeck, H Yang, ZL AF von Randow, Celso Zeri, Marcelo Restrepo-Coupe, Natalia Muza, Michel N. de Goncalves, Luis Gustavo G. Costa, Marcos H. Araujo, Alessandro C. Manzi, Antonio O. da Rocha, Humberto R. Saleska, Scott R. Arain, M. Alaf Baker, Ian T. Cestaro, Bruno P. Christoffersen, Bradley Ciais, Philippe Fisher, Joshua B. Galbraith, David Guan, Xiaodan Van den Hurk, Bart Ichii, Kazuhito Imbuzeiro, Hewlley Jain, Atul Levine, Naomi Miguez-Macho, Gonzalo Poulter, Ben Roberti, Debora R. Sahoo, Alok Schaefer, Kevin Shi, Mingjie Tian, Hanqin Verbeeck, Hans Yang, Zong-Liang TI Inter-annual variability of carbon and water fluxes in Amazonian forest, Cerrado and pasture sites, as simulated by terrestrial biosphere models SO AGRICULTURAL AND FOREST METEOROLOGY LA English DT Article DE Land-surface modeling; Surface fluxes; Amazonia; Inter-annual variability ID GLOBAL VEGETATION MODEL; RAIN-FOREST; EDDY-COVARIANCE; CLIMATE-CHANGE; TROPICAL FOREST; SOUTH-AMERICA; CO2 EXCHANGE; LONG-TERM; ENERGY; DYNAMICS AB This study analyzes the inter-annual variability (IAV) of simulations of 21 different land surface model formulations, driven by meteorological conditions measured at 8 flux towers, located in rain forest, forest-savanna ecotone and pasture sites in Amazonia, and one in savanna site in Southeastern Brazil. Annual totals of net ecosystem exchange (NEE) of carbon and evapotranspiration (ET), measured and simulated by each model for each site-year, were compared in terms of year-to-year variability and possible relation to climate drivers. Results have shown that most of models simulations for annual totals of NEE and ET, and IAV of these fluxes, are frequently different from measurements. The average of the model simulations of annual fluxes tend to respond to climatic drivers similarly to the observations, but with noticeable discrepancies. Annual measurements of NEE are negatively correlated to annual rainfall in the forest sites group. Although the ensemble of all models yields a similar result, only three model formulations reproduce a significant negative correlation of simulated NEE with rainfall. For the IAV of ET, tower measurements are controlled by annual variations of radiation and this feature is captured by the ensemble of the models, both at individual sites and when all forest sites are grouped. However, simulated ET values are also significantly correlated to the amount of precipitation in many models and in the model ensemble, while there is no significant correlation in the observations. In general, the surface models are able to reproduce the responses of fluxes to climatic drivers, but improvements are still needed to better capture their inter-annual variability. (C) 2013 Elsevier B.V. All rights reserved. C1 [von Randow, Celso; Zeri, Marcelo] Inst Nacl Pesquisas Espaciais, Ctr Ciencia Sistema Terrestre, Cachoeira Paulista, SP, Brazil. [Restrepo-Coupe, Natalia] Univ Technol Sydney, Plant Funct Biol & Climate Change Cluster, Sydney, NSW 2007, Australia. [Muza, Michel N.] Inst Fed Santa Catarina, Florianopolis, SC, Brazil. [de Goncalves, Luis Gustavo G.] Inst Nacl Pesquisas Espaciais, Ctr Previsao Tempo & Estudos Climat, Cachoeira Paulista, SP, Brazil. [Costa, Marcos H.; Imbuzeiro, Hewlley] Univ Fed Vicosa, Dep Agr Engn, Vicosa, MG, Brazil. [Araujo, Alessandro C.] Embrapa Amazonia Oriental, Belem, PA, Brazil. [Manzi, Antonio O.] INPA, Manaus, Amazonas, Brazil. [da Rocha, Humberto R.; Cestaro, Bruno P.] Univ Sao Paulo, IAG, Dept Ciencias Atmosfer, Sao Paulo, Brazil. [Saleska, Scott R.; Christoffersen, Bradley] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ USA. [Arain, M. Alaf] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON, Canada. [Baker, Ian T.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Ciais, Philippe; Poulter, Ben] CEA Orme Merisiers, Lab Sci Climat & Environm, Gif Sur Yvette, France. [Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Galbraith, David] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. [Guan, Xiaodan; Shi, Mingjie; Yang, Zong-Liang] Univ Texas Austin, Dept Geol Sci, Ctr Integrated Earth Syst Sci, Austin, TX USA. [Van den Hurk, Bart] Royal Netherlands Meteorol Inst KNMI, De Bilt, Netherlands. [Ichii, Kazuhito] Fukushima Univ, Fac Symbiot Syst Sci, Fukushima, Japan. [Jain, Atul] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA. [Levine, Naomi] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Miguez-Macho, Gonzalo] Univ Santiago de Compostela, Dept Condensed Matter Phys, Santiago De Compostela, Spain. [Roberti, Debora R.] Univ Fed Santa Maria, Dept Phys, BR-97119900 Santa Maria, RS, Brazil. [Sahoo, Alok] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. [Schaefer, Kevin] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA. [Tian, Hanqin] Auburn Univ, Sch Forestry & Wildlife Sci, Auburn, AL 36849 USA. [Verbeeck, Hans] Univ Ghent, Plant Ecol Lab, B-9000 Ghent, Belgium. RP von Randow, C (reprint author), Inst Nacl Pesquisas Espaciais, Ctr Ciencia Sistema Terrestre, Cachoeira Paulista, SP, Brazil. EM celso.vonrandow@inpe.br RI Yang, Zong-Liang/B-4916-2011; Ichii, Kazuhito/D-2392-2010; Costa, Marcos/A-5695-2009; Tian, Hanqin/A-6484-2012; Restrepo-Coupe, Natalia/C-3507-2015; Jain, Atul/D-2851-2016; OI Ichii, Kazuhito/0000-0002-8696-8084; Levine, Naomi/0000-0002-4963-0535; Poulter, Benjamin/0000-0002-9493-8600; Costa, Marcos/0000-0001-6874-9315; Tian, Hanqin/0000-0002-1806-4091; Restrepo-Coupe, Natalia/0000-0003-3921-1772; Jain, Atul/0000-0002-4051-3228; Arain, M. Altaf/0000-0002-1433-5173; Fisher, Joshua/0000-0003-4734-9085 FU Brazilian Ministry of Science, Technology and Innovation; NASA; NASA's Terrestrial Ecology Program [NNX09AL52G] FX We thank innumerous scientists and field technicians who operated the flux towers under the LBA program, funded by the Brazilian Ministry of Science, Technology and Innovation, NASA and European Agencies. We also thank the LBA-Data-Model-Intercomparison project funded by NASA's Terrestrial Ecology Program (grant NNX09AL52G), which organized the datasets that made this work possible. NR 72 TC 6 Z9 6 U1 3 U2 60 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1923 EI 1873-2240 J9 AGR FOREST METEOROL JI Agric. For. Meteorol. PD DEC 15 PY 2013 VL 182 SI SI BP 145 EP 155 DI 10.1016/j.agrformet.2013.05.015 PG 11 WC Agronomy; Forestry; Meteorology & Atmospheric Sciences SC Agriculture; Forestry; Meteorology & Atmospheric Sciences GA 252JE UT WOS:000327000200014 ER PT J AU Horodysky, AZ Brill, RW Crawford, KC Seagroves, ES Johnson, AK AF Horodysky, Andrij Z. Brill, Richard W. Crawford, Kendyl C. Seagroves, Elizabeth S. Johnson, Andrea K. TI Comparative visual ecophysiology of mid-Atlantic temperate reef fishes SO BIOLOGY OPEN LA English DT Article DE Electroretinography; Fish; Flicker fusion frequency; Spectral sensitivity; Temperate reef; Visual ecology AB The absolute light sensitivities, temporal properties, and spectral sensitivities of the visual systems of three mid-Atlantic temperate reef fishes (Atlantic spadefish [Ephippidae: Chaetodipterus faber], tautog [Labridae: Tautoga onitis], and black sea bass [Serranidae: Centropristis striata]) were studied via electroretinography (ERG). Pelagic Atlantic spadefish exhibited higher temporal resolution but a narrower dynamic range than the two more demersal foragers. The higher luminous sensitivities of tautog and black sea bass were similar to other benthic and demersal coastal mid-Atlantic fishes. Flicker fusion frequency experiments revealed significant interspecific differences at maximum intensities that correlated with lifestyle and habitat. Spectral responses of the three species spanned 400-610 nm, with high likelihood of cone dichromacy providing the basis for color and contrast discrimination. Significant day-night differences in spectral responses were evident in spadefish and black sea bass but not tautog, a labrid with characteristic structure-associated nocturnal torpor. Atlantic spadefish responded to a wider range of wavelengths than did deeper-dwelling tautog or black sea bass. Collectively, these results suggest that temperate reef-associated fishes are well-adapted to their gradient of brighter to dimmer photoclimates, representative of their unique ecologies and life histories. Continuing anthropogenic degradation of water quality in coastal environments, at a pace faster than the evolution of visual systems, may however impede visual foraging and reproductive signaling in temperate reef fishes. (C) 2013. Published by The Company of Biologists Ltd. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/3.0), which permits unrestricted use, distribution and reproduction in any medium provided that the original work is properly attributed. C1 [Horodysky, Andrij Z.; Crawford, Kendyl C.] Hampton Univ, Dept Marine & Environm Sci, Hampton, VA 23664 USA. [Brill, Richard W.] Natl Marine Fisheries Serv, Northeast Fisheries Sci Ctr, James J Howard Marine Sci Lab, Highlands, NJ 07732 USA. [Brill, Richard W.] Virginia Inst Marine Sci, Coll William & Mary, Dept Fisheries Sci, Gloucester Point, VA 23062 USA. [Johnson, Andrea K.] Univ Maryland Eastern Shore, Dept Nat Resources, Princess Anne, MD 21853 USA. RP Horodysky, AZ (reprint author), Hampton Univ, Dept Marine & Environm Sci, Hampton, VA 23664 USA. EM andrij.horodysky@hamptonu.edu FU National Oceanic and Atmospheric Association's Living Marine Resources Cooperative Science Center [NA060AR4810163, NA11SEC4810002] FX This research was funded by the National Oceanic and Atmospheric Association's Living Marine Resources Cooperative Science Center [NA060AR4810163 and NA11SEC4810002]. NR 86 TC 2 Z9 2 U1 1 U2 17 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 2046-6390 J9 BIOL OPEN JI Biol. Open PD DEC 15 PY 2013 VL 2 IS 12 BP 1371 EP 1381 DI 10.1242/bio.20136825 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA V36IW UT WOS:000209206900011 PM 24285711 ER PT J AU Lakeh, RB Lavine, AS Kavehpour, HP Ganapathi, GB Wirz, RE AF Lakeh, Reza Baghaei Lavine, Adrienne S. Kavehpour, H. Pirouz Ganapathi, Gani B. Wirz, Richard E. TI Effect of Laminar and Turbulent Buoyancy-Driven Flows on Thermal Energy Storage using Supercritical Fluids SO NUMERICAL HEAT TRANSFER PART A-APPLICATIONS LA English DT Article ID PHASE-CHANGE MATERIAL; HEAT-TRANSFER; NATURAL-CONVECTION; COMPOSITE; CONDUCTION; CONTAINER; NEPCM AB Efficient heat transfer to storage fluid is required for the desirable operation of thermal energy storage systems. Most of the fluid candidates for supercritical thermal storage have poor thermal conductivity; therefore, conduction does not provide sufficient heat transfer. The current study concerns a supercritical thermal energy storage system consisting of horizontal tubes filled with a storage fluid in its supercritical state. The results of this study show that the heat transfer to the supercritical fluid is dominated by laminar and turbulent natural convection. The buoyancy-driven flow inside the storage tubes enhances the heat transfer and dramatically reduces the charge time. C1 [Lakeh, Reza Baghaei; Lavine, Adrienne S.; Kavehpour, H. Pirouz; Wirz, Richard E.] Univ Calif Los Angeles, Dept Mech & Aerosp Engn, Los Angeles, CA 90095 USA. [Ganapathi, Gani B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Lakeh, RB (reprint author), Univ Calif Los Angeles, Dept Mech & Aerosp Engn, Los Angeles, CA 90095 USA. EM rblakeh@ucla.edu RI Lavine, Adrienne/B-6074-2013 OI Lavine, Adrienne/0000-0002-5580-7608 FU U.S. Department of Energy under Advanced Research Projects Agency-Energy (ARPA-E) [DE-AR0000140]; Southern California Gas Company [5660021607] FX This study was supported by award no. DE-AR0000140 granted by the U.S. Department of Energy under Advanced Research Projects Agency-Energy (ARPA-E), and by award no. 5660021607 granted by the Southern California Gas Company. NR 36 TC 5 Z9 5 U1 0 U2 35 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1040-7782 J9 NUMER HEAT TR A-APPL JI Numer. Heat Tranf. A-Appl. PD DEC 15 PY 2013 VL 64 IS 12 BP 955 EP 973 DI 10.1080/10407782.2013.811349 PG 19 WC Thermodynamics; Mechanics SC Thermodynamics; Mechanics GA 217FY UT WOS:000324345800001 ER PT J AU Handlin, D Stein, IY de Villoria, RG Cebeci, H Parsons, EM Socrate, S Scotti, S Wardle, BL AF Handlin, Daniel Stein, Itai Y. de Villoria, Roberto Guzman Cebeci, Huelya Parsons, Ethan M. Socrate, Simona Scotti, Stephen Wardle, Brian L. TI Three-dimensional elastic constitutive relations of aligned carbon nanotube architectures SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID POLYMER COMPOSITES; FIBER WAVINESS; FILMS; NANOCOMPOSITES; CONDUCTORS; ACTUATORS; FABRICATION; ELECTRODES; MORPHOLOGY; AEROGELS AB Tailorable anisotropic intrinsic and scale-dependent properties of carbon nanotubes (CNTs) make them attractive elements in next-generation advanced materials. However, in order to model and predict the behavior of CNTs in macroscopic architectures, mechanical constitutive relations must be evaluated. This study presents the full stiffness tensor for aligned CNT-reinforced polymers as a function of the CNT packing (up to similar to 20 vol. %), revealing noticeable anisotropy. Finite element models reveal that the usually neglected CNT waviness dictates the degree of anisotropy and packing dependence of the mechanical behavior, rather than any of the usually cited aggregation or polymer interphase mechanisms. Combined with extensive morphology characterization, this work enables the evaluation of structure-property relations for such materials, enabling design of aligned CNT material architectures. (C) 2013 AIP Publishing LLC. C1 [Handlin, Daniel; de Villoria, Roberto Guzman; Cebeci, Huelya; Wardle, Brian L.] MIT, Dept Aeronaut & Astronaut, Cambridge, MA 02139 USA. [Stein, Itai Y.] MIT, Dept Mech Engn, Cambridge, MA 02139 USA. [Parsons, Ethan M.; Socrate, Simona] MIT, Inst Soldier Nanotechnol, Cambridge, MA 02139 USA. [Scotti, Stephen] NASA Langley Res Ctr, Hampton, VA 23681 USA. RP Wardle, BL (reprint author), MIT, Dept Aeronaut & Astronaut, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM wardle@mit.edu RI Cebeci, Hulya/S-4999-2016; OI Guzman de Villoria, Roberto/0000-0001-6369-5266; Stein, Itai/0000-0003-3229-7315 FU Boeing; EADS; Embraer; Lockheed Martin; Saab AB; Composite Systems Technology; Hexcel; TohoTenax through MIT's Nano-Engineered Composite aerospace STructures (NECST) Consortium; U.S. Army Research Office [W911NF-07-D-0004, W911NF-13-D-0001]; NASA Space Technology Research Fellowship [NNX11AN79H]; National Science Foundation [CMMI-1130437, DMR-0819762] FX This work was supported by Boeing, EADS, Embraer, Lockheed Martin, Saab AB, Composite Systems Technology, Hexcel, and TohoTenax through MIT's Nano-Engineered Composite aerospace STructures (NECST) Consortium and was supported (in part) by the U.S. Army Research Office under contract W911NF-07-D-0004 and W911NF-13-D-0001. D.H. was supported by NASA Space Technology Research Fellowship Grant No. NNX11AN79H. I.Y.S. was supported by the National Science Foundation under Grant No. CMMI-1130437. The authors thank Marcel Williams (MIT), Silvia Chan (MIT, Univ. of Pennsylvania), and Kosuke Takahashi (MIT, UCLA) for early experimental contributions to this work, and Sunny Wicks (MIT), Richard Li (MIT), John Kane (MIT), and the entire necstlab at MIT for technical support and advice. This work was supported (in part) by the U.S. Army Research Office under contract W911NF-13-D-0001, made use of the MIT MRSEC Shared Experimental Facilities supported by the National Science Foundation under Award No. DMR-0819762, utilized the core facilities at the Institute for Soldier Nanotechnologies at MIT, supported in part by the U.S. Army Research Office under contract W911NF-07-D-0004 and was carried out in part through the use of MIT's Microsystems Technology Laboratories. NR 41 TC 11 Z9 11 U1 2 U2 35 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD DEC 14 PY 2013 VL 114 IS 22 AR 224310 DI 10.1063/1.4842117 PG 5 WC Physics, Applied SC Physics GA 281HI UT WOS:000329090400080 ER PT J AU Wang, XH Huang, XC Bowman, JM Lee, TJ AF Wang, Xiaohong Huang, Xinchuan Bowman, Joel M. Lee, Timothy J. TI Anharmonic rovibrational calculations of singlet cyclic C-4 using a new ab initio potential and a quartic force field SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SMALL CARBON CLUSTERS; VIBRATIONAL FREQUENCIES; SPECTROSCOPIC CONSTANTS; HARMONIC FREQUENCIES; POLYATOMIC-MOLECULES; INFRARED-SPECTRA; ENERGY SURFACES; BASIS-SETS; ACCURATE; ISOTOPOLOGUES AB We report a CCSD(T)/cc-pCV5Z quartic force field (QFF) and a semi-global CCSD(T)-F12b/aug-cc-pVTZ potential energy surface (PES) for singlet, cyclic C-4. Vibrational fundamentals, combinations, and overtones are obtained using vibrational second-order perturbation theory (VPT2) and the vibrational configuration-interaction (VCI) approach. Agreement is within 10 cm(-1) between the VCI calculated fundamentals on the QFF and PES using the MULTIMODE (MM) program, and VPT2 and VCI results agree for the fundamentals. The agreement between VPT2-QFF and MM-QFF results is also good for the C-4 combinations and overtones. The J = 1 and J = 2 rovibrational energies are reported from both VCI (MM) on the PES and VPT2 on the QFF calculations. The spectroscopic constants of C-12(4) and two C-2 nu-symmetry, single C-13-substituted isotopologues are presented, which may help identification of cyclic C-4 in future experimental analyses or astronomical observations. (C) 2013 AIP Publishing LLC. C1 [Wang, Xiaohong; Bowman, Joel M.] Emory Univ, Cherry L Emerson Ctr Sci Computat, Atlanta, GA 30322 USA. [Wang, Xiaohong; Bowman, Joel M.] Emory Univ, Dept Chem, Atlanta, GA 30322 USA. [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. [Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Wang, XH (reprint author), Emory Univ, Cherry L Emerson Ctr Sci Computat, Atlanta, GA 30322 USA. EM jmbowma@emory.edu; Timothy.J.Lee@nasa.gov RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013 FU NASA; NASA Astrophysics Research and Analysis program [NNX12AF42G]; NASA/SETI Institute Cooperative Agreement [NNX12AG96A]; NASA Laboratory Astrophysics Carbon in the Galaxy Consortium [NNH10ZDA001N]; NASA [10-APRA10-0096] FX Financial support from NASA is gratefully acknowledged, Grant No. NNX12AF42G from the NASA Astrophysics Research and Analysis program (X.W. and J.M.B.). X.H. thanks the support through NASA/SETI Institute Cooperative Agreement NNX12AG96A. Support from NASA Laboratory Astrophysics Carbon in the Galaxy Consortium (Grant No. NNH10ZDA001N) is gratefully acknowledged by T.J.L., while T.J.L. and X. H. gratefully acknowledge support from NASA Grant No. 10-APRA10-0096. NR 37 TC 3 Z9 3 U1 0 U2 16 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 14 PY 2013 VL 139 IS 22 AR 224302 DI 10.1063/1.4837177 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 276DT UT WOS:000328729000017 PM 24329063 ER PT J AU Czabaj, MW Ratcliffe, JG AF Czabaj, Michael W. Ratcliffe, James G. TI Comparison of intralaminar and interlaminar mode I fracture toughnesses of a unidirectional IM7/8552 carbon/epoxy composite SO COMPOSITES SCIENCE AND TECHNOLOGY LA English DT Article DE Polymer-matrix composites (PMCs); Intralaminar fracture; Delamination; Fracture toughness ID DELAMINATION BEHAVIOR; FAILURE MECHANISMS; CFRP COMPOSITES AB The intralaminar and interlaminar mode I fracture toughnesses of a unidirectional IM7/8552 carbon/epoxy composite were measured using compact tension (CT) and double cantilever beam (DCB) test specimens, respectively. Two starter crack geometries were considered for both the CT and DCB specimen configurations. In the first case, starter cracks were produced by 12.5 mu m thick, Teflon film inserts. In the second case, considerably sharper starter cracks were produced by fatigue precracking. For each specimen configuration, use of the Teflon film starter cracks resulted in initially unstable crack growth and artificially high initiation fracture-toughness values. Conversely, specimens with fatigue precracks exhibited stable growth onset and lower initiation fracture toughnesses. For CT and DCB specimens with fatigue precracks, the intralaminar and interlaminar initiation fracture toughnesses were essentially equal. However, during propagation, the CT specimens exhibited more extensive fiber bridging and rapidly increasing R-curve behavior as compared to the DCB specimens. Observations of initiation and propagation of intralaminar and interlaminar fracture, and the measurements of fracture toughness, were consistent with fractographic analysis using scanning electron microscopy. Published by Elsevier Ltd. C1 [Czabaj, Michael W.] NASA, Langley Res Ctr, Hampton, VA 23452 USA. [Ratcliffe, James G.] Natl Inst Aerosp, Hampton, VA 23666 USA. RP Czabaj, MW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23452 USA. EM michael.w.czabaj@nasa.gov NR 36 TC 7 Z9 7 U1 1 U2 30 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0266-3538 EI 1879-1050 J9 COMPOS SCI TECHNOL JI Compos. Sci. Technol. PD DEC 13 PY 2013 VL 89 BP 15 EP 23 DI 10.1016/j.compscitech.2013.09.008 PG 9 WC Materials Science, Composites SC Materials Science GA 275YO UT WOS:000328715500003 ER PT J AU Aasi, J Abadie, J Abbott, BP Abbott, R Abbott, T Abernathy, MR Accadia, T Acernese, F Adams, C Adams, T Adhikari, RX Affeldt, C Agathos, M Aggarwal, N Aguiar, OD Ajith, P Allen, B Allocca, A Ceron, EA Amariutei, D Anderson, RA Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, C Areeda, J Ast, S Aston, SM Astone, P Aufmuth, P Aulbert, C Austin, L Aylott, BE Babak, S Baker, PT Ballardin, G Ballmer, SW Barayoga, JC Barker, D Barnum, SH Barone, F Barr, B Barsotti, L Barsuglia, M Barton, MA Bartos, I Bassiri, R Basti, A Batch, J Bauchrowitz, J Bauer, TS Bebronne, M Behnke, B Bejger, M Beker, MG Bell, AS Bell, C Belopolski, I Bergmann, G Berliner, JM Bersanetti, D Bertolini, A Bessis, D Betzwieser, J Beyersdorf, PT Bhadbhade, T Bilenko, IA Billingsley, G Birch, J Bitossi, M Bizouard, MA Black, E Blackburn, JK Blackburn, L Blair, D Blom, M Bock, O Bodiya, TP Boer, M Bogan, C Bond, C Bondu, F Bonelli, L Bonnand, R Bork, R Born, M Boschi, V Bose, S Bosi, L Bowers, J Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brannen, CA Brau, JE Breyer, J Briant, T Bridges, DO Brillet, A Brinkmann, M Brisson, V Britzger, M Brooks, AF Brown, DA Brown, DD Bruckner, F Bulik, T Bulten, HJ Buonanno, A Buskulic, D Buy, C Byer, RL Cadonati, L Cagnoli, G Bustillo, JC Calloni, E Camp, JB Campsie, P Cannon, KC Canuel, B Cao, J Capano, CD Carbognani, F Carbone, L Caride, S Castiglia, A Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Cella, G Cepeda, C Cesarini, E Chakraborty, R Chalermsongsak, T Chao, S Charlton, P Chassande-Mottin, E Chen, X Chen, Y Chincarini, A Chiummo, A Cho, HS Chow, J Christensen, N Chu, Q Chua, SSY Chung, S Ciani, G Clara, F Clark, DE Clark, JA Cleva, F Coccia, E Cohadon, PF Colla, A Colombini, M Constancio, M Conte, A Conte, R Cook, D Corbitt, TR Cordier, M Cornish, N Corsi, A Costa, CA Coughlin, MW Coulon, JP Countryman, S Couvares, P Coward, DM Cowart, M Coyne, DC Craig, K Creighton, JDE Creighton, TD Crowder, SG Cumming, A Cunningham, L Cuoco, E Dahl, K Dal Canton, T Damjanic, M Danilishin, SL D'Antonio, S Danzmann, K Dattilo, V Daudert, B Daveloza, H Davier, M Davies, GS Daw, EJ Day, R Dayanga, T De Rosa, R Debreczeni, G Degallaix, J Del Pozzo, W Deleeuw, E Deleglise, S Denker, T Dent, T Dereli, H Dergachev, V DeRosa, R DeSalvo, R Dhurandhar, S Di Fiore, L Di Lieto, A Di Palma, I Di Virgilio, A Diaz, M Dietz, A Dmitry, K Donovan, F Dooley, KL Doravari, S Drago, M Drever, RWP Driggers, JC Du, Z Dumas, JC Dwyer, S Eberle, T Edwards, M Effler, A Ehrens, P Eichholz, J Eikenberry, SS Endroczi, G Essick, R Etzel, T Evans, K Evans, M Evans, T Factourovich, M Fafone, V Fairhurst, S Fang, Q Farinon, S Farr, B Farr, W Favata, M Fazi, D Fehrmann, H Feldbaum, D Ferrante, I Ferrini, F Fidecaro, F Finn, LS Fiori, I Fisher, R Flaminio, R Foley, E Foley, S Forsi, E Fotopoulos, N Fournier, JD Franco, S Frasca, S Frasconi, F Frede, M Frei, M Frei, Z Freise, A Frey, R Fricke, TT Fritschel, P Frolov, VV Fujimoto, MK Fulda, P Fyffe, M Gair, J Gammaitoni, L Garcia, J Garufi, F Gehrels, N Gemme, G Genin, E Gennai, A Gergely, L Ghosh, S Giaime, JA Giampanis, S Giardina, KD Giazotto, A Gil-Casanova, S Gill, C Gleason, J Goetz, E Goetz, R Gondan, L Gonzalez, G Gordon, N Gorodetsky, ML Gossan, S Gossler, S Gouaty, R Graef, C Graff, PB Granata, M Grant, A Gras, S Gray, C Greenhalgh, RJS Gretarsson, AM Griffo, C Groot, P Grote, H Grover, K Grunewald, S Guidi, GM Guido, C Gushwa, KE Gustafson, EK Gustafson, R Hall, B Hall, E Hammer, D Hammond, G Hanke, M Hanks, J Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Hartman, MT Haughian, K Hayama, K Heefner, J Heidmann, A Heintze, M Heitmann, H Hello, P Hemming, G Hendry, M Heng, IS Heptonstall, AW Heurs, M Hild, S Hoak, D Hodge, KA Holt, K Holtrop, M Hong, T Hooper, S Horrom, T Hosken, DJ Hough, J Howell, EJ Hu, Y Hua, Z Huang, V Huerta, EA Hughey, B Husa, S Huttner, SH Huynh, M Huynh-Dinh, T Iafrate, J Ingram, DR Inta, R Isogai, T Ivanov, A Iyer, BR Izumi, K Jacobson, M James, E Jang, H Jang, YJ Jaranowski, P Jimenez-Forteza, F Johnson, WW Jones, D Jones, DI Jones, R Jonker, RJG Ju, L Haris, K Kalmus, P Kalogera, V Kandhasamy, S Kang, G Kanner, JB Kasprzack, M Kasturi, R Katsavounidis, E Katzman, W Kaufer, H Kaufman, K Kawabe, K Kawamura, S Kawazoe, F Kefelian, F Keitel, D Kelley, DB Kells, W Keppel, DG Khalaidovski, A Khalili, FY Khazanov, EA Kim, BK Kim, C Kim, K Kim, N Kim, W Kim, YM King, EJ King, PJ Kinzel, DL Kissel, JS Klimenko, S Kline, J Koehlenbeck, S Kokeyama, K Kondrashov, V Koranda, S Korth, WZ Kowalska, I Kozak, D Kremin, A Kringel, V Krolak, A Kucharczyk, C Kudla, S Kuehn, G Kumar, A Kumar, P Kumar, R Kurdyumov, R Kwee, P Landry, M Lantz, B Larson, S Lasky, PD Lawrie, C Lazzarini, A Le Roux, A Leaci, P Lebigot, EO Lee, CH Lee, HK Lee, HM Lee, J Lee, J Leonardi, M Leong, JR Leroy, N Letendre, N Levine, B Lewis, JB Lhuillier, V Li, TGF Lin, AC Littenberg, TB Litvine, V Liu, F Liu, H Liu, Y Liu, Z Lloyd, D Lockerbie, NA Lockett, V Lodhia, D Loew, K Logue, J Lombardi, AL Lorenzini, M Loriette, V Lormand, M Losurdo, G Lough, J Luan, J Lubinski, MJ Luck, H Lundgren, AP Macarthur, J Macdonald, E Machenschalk, B MacInnis, M Macleod, DM Magana-Sandoval, F Mageswaran, M Mailand, K Majorana, E Maksimovic, I Malvezzi, V Man, N Manca, GM Mandel, I Mandic, V Mangano, V Mantovani, M Marchesoni, F Marion, F Marka, S Marka, Z Markosyan, A Maros, E Marque, J Martelli, F Martin, IW Martin, RM Martinelli, L Martynov, D Marx, JN Mason, K Masserot, A Massinger, TJ Matichard, F Matone, L Matzner, RA Mavalvala, N May, G Mazumder, N Mazzolo, G McCarthy, R McClelland, DE McGuire, SC McIntyre, G McIver, J Meacher, D Meadors, GD Mehmet, M Meidam, J Meier, T Melatos, A Mendell, G Mercer, RA Meshkov, S Messenger, C Meyer, MS Miao, H Michel, C Mikhailov, EE Milano, L Miller, J Minenkov, Y Mingarelli, CMF Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Moe, B Mohan, M Mohapatra, RP Mokler, F Moraru, D Moreno, G Morgado, N Mori, T Morriss, SR Mossavi, K Mours, B Mow-Lowry, CM Mueller, CL Mueller, G Mukherjee, S Mullavey, A Munch, J Murphy, D Murray, PG Mytidis, A Nagy, MF Kumar, DN Nardecchia, I Nash, T Naticchioni, L Nayak, R Necula, V Nelemans, G Neri, I Neri, M Newton, G Nguyen, T Nishida, E Nishizawa, A Nitz, A Nocera, F Nolting, D Normandin, ME Nuttall, LK Ochsner, E O'Dell, J Oelker, E Ogin, GH Oh, JJ Oh, SH Ohme, F Oppermann, P O'Reilly, B Larcher, WO O'Shaughnessy, R Osthelder, C Ott, CD Ottaway, DJ Ottens, RS Ou, J Overmier, H Owen, BJ Padilla, C Pai, A Palomba, C Pan, Y Pankow, C Paoletti, F Paoletti, R Papa, MA Paris, H Pasqualetti, A Passaquieti, R Passuello, D Pedraza, M Peiris, P Penn, S Perreca, A Phelps, M Pichot, M Pickenpack, M Piergiovanni, F Pierro, V Pinard, L Pindor, B Pinto, IM Pitkin, M Poeld, J Poggiani, R Poole, V Poux, C Predoi, V Prestegard, T Price, LR Prijatelj, M Principe, M Privitera, S Prodi, GA Prokhorov, L Puncken, O Punturo, M Puppo, P Quetschke, V Quintero, E Quitzow-James, R Raab, FJ Rabeling, DS Racz, I Radkins, H Raffai, P Raja, S Rajalakshmi, G Rakhmanov, M Ramet, C Rapagnani, P Raymond, V Re, V Reed, CM Reed, T Regimbau, T Reid, S Reitze, DH Ricci, F Riesen, R Riles, K Robertson, A Robinet, F Rocchi, A Roddy, S Rodriguez, C Rodruck, M Roever, C Rolland, L Rollins, JG Romano, JD Romano, R Romanov, G Romie, JH Rosinska, D Rowan, S Rudiger, A Ruggi, P Ryan, K Salemi, F Sammut, L Sandberg, V Sanders, J Sannibale, V Santiago-Prieto, I Saracco, E Sassolas, B Sathyaprakash, BS Saulson, PR Savage, R Schilling, R Schnabel, R Schofield, RMS Schreiber, E Schuette, D Schulz, B Schutz, BF Schwinberg, P Scott, J Scott, SM Seifert, F Sellers, D Sengupta, AS Sentenac, D Sergeev, A Shaddock, D Shah, S Shahriar, MS Shaltev, M Shapiro, B Shawhan, P Shoemaker, DH Sidery, TL Siellez, K Siemens, X Sigg, D Simakov, D 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TI Search for long-lived gravitational-wave transients coincident with long gamma-ray bursts SO PHYSICAL REVIEW D LA English DT Article ID SCIENCE RUN; LIGO OBSERVATIONS; NEUTRON-STARS; BLACK-HOLES; SUPERNOVAE; ORIGIN; VIRGO; IDENTIFICATION; AFTERGLOWS; ACCRETION AB Long gamma-ray bursts (GRBs) have been linked to extreme core-collapse supernovae from massive stars. Gravitational waves (GW) offer a probe of the physics behind long GRBs. We investigate models of long-lived (similar to 10-1000 s) GW emission associated with the accretion disk of a collapsed star or with its protoneutron star remnant. Using data from LIGO's fifth science run, and GRB triggers from the Swift experiment, we perform a search for unmodeled long-lived GW transients. Finding no evidence of GW emission, we place 90% confidence-level upper limits on the GW fluence at Earth from long GRBs for three waveforms inspired by a model of GWs from accretion disk instabilities. These limits range from F < 3.5 ergs cm(-2) to F < 1200 ergs cm(-2), depending on the GRB and on the model, allowing us to probe optimistic scenarios of GW production out to distances as far as approximate to 33 Mpc. Advanced detectors are expected to achieve strain sensitivities 10X better than initial LIGO, potentially allowing us to probe the engines of the nearest long GRBs. C1 [Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Ajith, P.; Anderson, R. A.; Anderson, S. B.; Arai, K.; Araya, M. C.; Austin, L.; Barayoga, J. C.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chakraborty, R.; Chalermsongsak, T.; Coyne, D. C.; Daudert, B.; Dergachev, V.; Driggers, J. C.; Ehrens, P.; Etzel, T.; Fotopoulos, N.; Gushwa, K. E.; Gustafson, E. K.; Hall, E.; Harms, J.; Heefner, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; James, E.; Kalmus, P.; Kells, W.; King, P. J.; Kondrashov, V.; Korth, W. 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[Calderon Bustillo, J.; Gil-Casanova, S.; Husa, S.; Jimenez-Forteza, F.; Sintes, A. M.] Univ Illes Balears, E-07122 Palma De Mallorca, Spain. [Calloni, E.; De Rosa, R.; Garufi, F.; Milano, L.] Univ Naples Federico II, I-80126 Naples, Italy. [Cannon, K. C.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Cao, J.; Du, Z.; Hua, Z.; Lebigot, E. O.; Liu, Y.; Wan, Y.; Wang, X.] Tsinghua Univ, Beijing 100084, Peoples R China. [Caride, S.; Gustafson, R.; Meadors, G. D.; Riles, K.; Sanders, J.] Univ Michigan, Ann Arbor, MI 48109 USA. [Castiglia, A.; Frei, M.; Mohapatra, R. P.; Peiris, P.; Whelan, J. T.] Rochester Inst Technol, Rochester, NY 14623 USA. [Cesarini, E.; D'Antonio, S.; Fafone, V.; Lorenzini, M.; Malvezzi, V.; Minenkov, Y.; Re, V.; Rocchi, A.; Sperandio, L.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Chao, S.; Huang, V.; Ou, J.; Wang, J.] Natl Tsing Hua Univ, Hsinchu 300, Taiwan. [Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia. [Chen, Y.; Gossan, S.; Hong, T.; Kaufman, K.; Luan, J.; Miao, H.; Ott, C. D.; Thorne, K. S.; Vallisneri, M.; Yang, H.] Caltech CaRT, Pasadena, CA 91125 USA. [Cho, H. S.; Kim, Y. -M.; Lee, C. -H.] Pusan Natl Univ, Busan 609735, South Korea. [Chow, J.; Chua, S. S. Y.; Inta, R.; McClelland, D. E.; Miller, J.; Nguyen, T.; Scott, S. M.; Shaddock, D.; Slagmolen, B. J. J.; Stochino, A.; Wade, A.; Ward, R. L.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Christensen, N.] Carleton Coll, Northfield, MN 55057 USA. [Coccia, E.] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, I-67100 Laquila, Italy. [Coccia, E.; Fafone, V.; Re, V.; Sperandio, L.] Univ Roma Tor Vergata, I-00133 Rome, Italy. [Colla, A.; Conte, A.; Frasca, S.; Mangano, V.; Nardecchia, I.; Naticchioni, L.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, I-00185 Rome, Italy. [Conte, R.; DeSalvo, R.; Pierro, V.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy. [Conte, R.; DeSalvo, R.; Pierro, V.; Pinto, I. M.; Principe, M.] Ist Nazl Fis Nucl, Sez Napoli, Rome, Italy. [Corsi, A.] George Washington Univ, Washington, DC 20052 USA. [Coughlin, M. W.; Gair, J.] Univ Cambridge, Cambridge CB2 1TN, England. [Crowder, S. G.; Kandhasamy, S.; Kremin, A.; Mandic, V.; Prestegard, T.] Univ Minnesota, Minneapolis, MN 55455 USA. [Daw, E. J.; Tomlinson, C.; White, D. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England. [Debreczeni, G.; Endroczi, G.; Nagy, M. F.; Racz, I.; Vasuth, M.] RMKI, Wigner RCP, H-1121 Budapest, Hungary. [Dhurandhar, S.; Mitra, S.; Souradeep, T.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Drago, M.; Leonardi, M.; Prodi, G. A.] Ist Nazl Fis Nucl, Grp Collegato Trento, I-38050 Povo, Trento, Italy. [Drago, M.; Leonardi, M.; Prodi, G. A.] Univ Trento, I-38050 Povo, Trento, Italy. [Drever, R. W. P.; Rodriguez, C.] CALTECH, Pasadena, CA 91125 USA. [Farr, B.; Farr, W.; Fazi, D.; Jang, Y. J.; Kalogera, V.; Littenberg, T. B.; Shahriar, M. S.; Stevens, D.; Yablon, J.; Yum, H.] Northwestern Univ, Evanston, IL 60208 USA. [Favata, M.] Montclair State Univ, Montclair, NJ 07043 USA. [Finn, L. S.; Owen, B. J.; Raffai, P.; Zhu, H.] Penn State Univ, University Pk, PA 16802 USA. [Frei, Z.; Gergely, L.; Gondan, L.; Szeifert, G.] MTA Eotvos Univ, Lendulet ARG, H-1117 Budapest, Hungary. [Fujimoto, M. -K.; Hayama, K.; Kawamura, S.; Mori, T.; Nishida, E.; Nishizawa, A.] Natl Astron Observ Japan, Tokyo 1818588, Japan. [Gammaitoni, L.; Neri, I.; Travasso, F.; Vocca, H.] Univ Perugia, I-06123 Perugia, Italy. [Greenhalgh, R. J. S.; O'Dell, J.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England. [Gretarsson, A. M.; Hughey, B.; Loew, K.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. [Groot, P.; Nelemans, G.; Shah, S.; van der Sluys, M. V.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Hanna, C.] Perimeter Inst Theoret Phys, Toronto, ON N2L 2Y5, Canada. [Harry, G. M.] Amer Univ, Washington, DC 20016 USA. [Holtrop, M.] Univ New Hampshire, Durham, NH 03824 USA. [Horrom, T.; Mikhailov, E. E.; Romanov, G.] Coll William & Mary, Williamsburg, VA 23187 USA. [Hosken, D. J.; Kim, W.; King, E. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia. [Iyer, B. R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Jang, H.; Kang, G.; Kim, B. K.; Kim, C.] Korea Inst Sci & Technol Informat, Taejon 305806, South Korea. [Jaranowski, P.] Bialystok Univ, PL-15424 Bialystok, Poland. [Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Haris, K.; Mazumder, N.; Pai, A.] IISER TVM, Trivandrum 695016, Kerala, India. [Kasturi, R.; Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [Khazanov, E. A.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia. [Kim, C.; Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea. [Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea. [Krolak, A.] IM PAN, PL-00956 Warsaw, Poland. [Krolak, A.; Ny, A. Zadroz .] NCBJ, PL-05400 Otwock, Poland. [Kumar, A.] Inst Plasma Res, Bhat 382428, Gandhinagar, India. [Larson, S.] Utah State Univ, Logan, UT 84322 USA. [Lasky, P. D.; Melatos, A.; Pindor, B.; Sammut, L.] Univ Melbourne, Parkville, Vic 3010, Australia. [Liu, F.] Univ Brussels, B-1050 Brussels, Belgium. [Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland. [Allocca, A.; Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France. [Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy. [Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA. [McGuire, S. C.; Vincent-Finley, R.] Southern Univ, Baton Rouge, LA 70813 USA. [McGuire, S. C.; Vincent-Finley, R.] A&M Coll, Baton Rouge, LA 70813 USA. [Nayak, R.] IISER Kolkata, Mohanpur 741252, W Bengal, India. [Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Daejeon 305390, South Korea. [Raja, S.] RRCAT, Indore 452013, Madhya Pradesh, India. [Rajalakshmi, G.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Mumbai 400005, Maharashtra, India. [Reed, T.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA. [Reid, S.] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland. [Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland. [Sengupta, A. S.] Indian Inst Technol, Gandhinagar Ahmedabad 382424, Gujarat, India. [Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA. [Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA. [Vedovato, G.; Zendri, J. -P.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA. [Williams, T.; Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA. [Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA. RP Aasi, J (reprint author), LIGO Calif Inst Technol, Pasadena, CA 91125 USA. EM ethrane@ligo.caltech.edu RI Howell, Eric/H-5072-2014; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Ward, Robert/I-8032-2014; Frasconi, Franco/K-1068-2016; Groot, Paul/K-4391-2016; Pinto, Innocenzo/L-3520-2016; Ferrante, Isidoro/F-1017-2012; Travasso, Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Cesarini, Elisabetta/C-4507-2017; Costa, Cesar/G-7588-2012; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011; Neri, Igor/F-1482-2010; Aggarwal, Nancy/M-7203-2015; Shaddock, Daniel/A-7534-2011; Vicere, Andrea/J-1742-2012; Rocchi, Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Strain, Kenneth/D-5236-2011; Miao, Haixing/O-1300-2013; Gehring, Tobias/A-8596-2016; Heidmann, Antoine/G-4295-2016; Ott, Christian/G-2651-2011; Zhu, Xingjiang/E-1501-2016; McClelland, David/E-6765-2010; M, Manjunath/N-4000-2014; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Finn, Lee Samuel/A-3452-2009; Leonardi, Matteo/G-9694-2015; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Ottaway, David/J-5908-2015; Garufi, Fabio/K-3263-2015; Deleglise, Samuel/B-1599-2015; Bell, Angus/E-7312-2011; Nelemans, Gijs/D-3177-2012; Bilenko, Igor/D-5172-2012; Kumar, Prem/B-6691-2009; Huerta, Eliu/J-5426-2014; Losurdo, Giovanni/K-1241-2014; Steinlechner, Sebastian/D-5781-2013; Hild, Stefan/A-3864-2010; Danilishin, Stefan/K-7262-2012; Gammaitoni, Luca/B-5375-2009; Canuel, Benjamin/C-7459-2014; Lee, Chang-Hwan/B-3096-2015; Khalili, Farit/D-8113-2012; Chen, Yanbei/A-2604-2013; prodi, giovanni/B-4398-2010; Marchesoni, Fabio/A-1920-2008; Salemi, Francesco/F-6988-2014; Iyer, Bala R./E-2894-2012; Prokhorov, Leonid/I-2953-2012; Gorodetsky, Michael/C-5938-2008; Strigin, Sergey/I-8337-2012; Mitrofanov, Valery/D-8501-2012; CONTE, ANDREA/J-6667-2012; Gemme, Gianluca/C-7233-2008; Khazanov, Efim/B-6643-2014; Zhao, Chunnong/C-2403-2013; OI Sorazu, Borja/0000-0002-6178-3198; Stuver, Amber/0000-0003-0324-5735; Bondu, Francois/0000-0001-6487-5197; Zweizig, John/0000-0002-1521-3397; Del Pozzo, Walter/0000-0003-3978-2030; O'Shaughnessy, Richard/0000-0001-5832-8517; Vocca, Helios/0000-0002-1200-3917; Fairhurst, Stephen/0000-0001-8480-1961; Allen, Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Pierro, Vincenzo/0000-0002-6020-5521; Coccia, Eugenio/0000-0002-6669-5787; Vetrano, Flavio/0000-0002-7523-4296; Denker, Timo/0000-0003-1259-5315; Naticchioni, Luca/0000-0003-2918-0730; Nishizawa, Atsushi/0000-0003-3562-0990; calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Howell, Eric/0000-0001-7891-2817; Boschi, Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418; Papa, M.Alessandra/0000-0002-1007-5298; Aulbert, Carsten/0000-0002-1481-8319; Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Guidi, Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Swinkels, Bas/0000-0002-3066-3601; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Whelan, John/0000-0001-5710-6576; Vedovato, Gabriele/0000-0001-7226-1320; Frasconi, Franco/0000-0003-4204-6587; Groot, Paul/0000-0002-4488-726X; Ferrante, Isidoro/0000-0002-0083-7228; Travasso, Flavio/0000-0002-4653-6156; Punturo, Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Neri, Igor/0000-0002-9047-9822; Shaddock, Daniel/0000-0002-6885-3494; Vicere, Andrea/0000-0003-0624-6231; Rocchi, Alessio/0000-0002-1382-9016; Martelli, Filippo/0000-0003-3761-8616; Strain, Kenneth/0000-0002-2066-5355; Miao, Haixing/0000-0003-4101-9958; Gehring, Tobias/0000-0002-4311-2593; Heidmann, Antoine/0000-0002-0784-5175; Ott, Christian/0000-0003-4993-2055; Zhu, Xingjiang/0000-0001-7049-6468; McClelland, David/0000-0001-6210-5842; M, Manjunath/0000-0001-8710-0730; Vecchio, Alberto/0000-0002-6254-1617; Finn, Lee Samuel/0000-0002-3937-0688; Sigg, Daniel/0000-0003-4606-6526; Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168; Deleglise, Samuel/0000-0002-8680-5170; Bell, Angus/0000-0003-1523-0821; Nelemans, Gijs/0000-0002-0752-2974; Losurdo, Giovanni/0000-0003-0452-746X; Steinlechner, Sebastian/0000-0003-4710-8548; Danilishin, Stefan/0000-0001-7758-7493; Gammaitoni, Luca/0000-0002-4972-7062; Lee, Chang-Hwan/0000-0003-3221-1171; prodi, giovanni/0000-0001-5256-915X; Marchesoni, Fabio/0000-0001-9240-6793; Iyer, Bala R./0000-0002-4141-5179; Gorodetsky, Michael/0000-0002-5159-2742; Gemme, Gianluca/0000-0002-1127-7406; Zhao, Chunnong/0000-0001-5825-2401; Murphy, David/0000-0002-8538-815X; Pitkin, Matthew/0000-0003-4548-526X; Veitch, John/0000-0002-6508-0713; Davies, Gareth/0000-0002-4289-3439; Principe, Maria/0000-0002-6327-0628; Kanner, Jonah/0000-0001-8115-0577; Husa, Sascha/0000-0002-0445-1971; Vitale, Salvatore/0000-0003-2700-0767; Freise, Andreas/0000-0001-6586-9901; Nitz, Alexander/0000-0002-1850-4587; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669 FU Australian Research Council; International Science Linkages program of the Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Foundation for Fundamental Research on Matter; Netherlands Organisation for Scientific Research; Polish Ministry of Science and Higher Education; FOCUS Programme of Foundation for Polish Science; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; OTKA of Hungary; Lyon Institute of Origins (LIO); National Research Foundation of Korea; Industry Canada; Province of Ontario through the Ministry of Economic Development and Innovation; National Science and Engineering Research Council Canada; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P. Sloan Foundation FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, OTKA of Hungary, the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the National Science and Engineering Research Council Canada, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. NR 49 TC 17 Z9 17 U1 4 U2 66 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD DEC 13 PY 2013 VL 88 IS 12 AR UNSP 122004 DI 10.1103/PhysRevD.88.122004 PG 13 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 275QO UT WOS:000328692500004 ER PT J AU Harrivel, AR Weissman, DH Noll, DC Peltier, SJ AF Harrivel, Angela R. Weissman, Daniel H. Noll, Douglas C. Peltier, Scott J. TI Monitoring attentional state with fNIRS SO FRONTIERS IN HUMAN NEUROSCIENCE LA English DT Article DE near infra-red spectroscopy; attention; default mode network; classification; human performance ID NEAR-INFRARED SPECTROSCOPY; MULTISOURCE INTERFERENCE TASK; BRAIN ACTIVATION; DEFAULT-MODE; FUNCTIONAL CONNECTIVITY; SLEEP-DEPRIVATION; FMRI; NETWORK; SYSTEM; PERFORMANCE AB The ability to distinguish between high and low levels of task engagement in the real world is important for detecting and preventing performance decrements during safety-critical operational tasks. We therefore investigated whether functional Near Infrared Spectroscopy (fNIRS), a portable brain neuroimaging technique, can be used to distinguish between high and low levels of task engagement during the performance of a selective attention task. A group of participants performed the multi-source interference task (MSIT) while we recorded brain activity with fNIRS from two brain regions. One was a key region of the "task-positive" network, which is associated with relatively high levels of task engagement. The second was a key region of the "task-negative" network, which is associated with relatively low levels of task engagement (e.g., resting and not performing a task). Using activity in these regions as inputs to a multivariate pattern classifier, we were able to predict above chance levels whether participants were engaged in performing the MSIT or resting. We were also able to replicate prior findings from functional magnetic resonance imaging (fMRI) indicating that activity in task-positive and task-negative regions is negatively correlated during task performance. Finally, data from a companion fMRI study verified our assumptions about the sources of brain activity in the fNIRS experiment and established an upper bound on classification accuracy in our task. Together, our findings suggest that fNIRS could prove quite useful for monitoring cognitive state in real-world settings. C1 [Harrivel, Angela R.] NASA, Biosci & Technol Branch, Glenn Res Ctr, Cleveland, OH 44135 USA. [Harrivel, Angela R.; Noll, Douglas C.; Peltier, Scott J.] Univ Michigan, Dept Biomed Engn, fMRI Lab, Ann Arbor, MI 48109 USA. [Weissman, Daniel H.] Univ Michigan, Dept Psychol, Ann Arbor, MI 48109 USA. RP Harrivel, AR (reprint author), NASA, Biosci & Technol Branch, Glenn Res Ctr, Mail Stop 110-3,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM angela.r.harrivel@nasa.gov RI Noll, Douglas/D-8124-2014 OI Noll, Douglas/0000-0002-0983-3805 FU University of Michigan fMRI Laboratory; NASA's Aviation Safety Program FX This work was supported by the University of Michigan fMRI Laboratory and NASA's Aviation Safety Program. Colleagues at the NASA Glenn and Langley Research Centers are appreciated, especially Jeffrey Mackey, Daniel Gotti and Padetha Tin for head probe design and assembly, and Tristan Hearn and Alan Pope for helpful review. We are grateful for the assistance of the fMRI laboratory at the University of Michigan for the collection and pre-processing of the fMRI data, and Ted Huppert of the University of Pittsburgh for review and invaluable guidance regarding general fNIRS techniques and analyses. NR 55 TC 4 Z9 4 U1 1 U2 16 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1662-5161 J9 FRONT HUM NEUROSCI JI Front. Hum. Neurosci. PD DEC 13 PY 2013 VL 7 AR UNSP 861 DI 10.3389/fnhum.2013.00861 PG 10 WC Neurosciences; Psychology SC Neurosciences & Neurology; Psychology GA 269WQ UT WOS:000328274400001 PM 24379771 ER PT J AU Smith, M Koren, V Zhang, ZY Moreda, F Cui, ZT Cosgrove, B Mizukami, N Kitzmiller, D Ding, F Reed, S Anderson, E Schaake, J Zhang, Y Andreassian, V Perrin, C Coron, L Valery, A Khakbaz, B Sorooshian, S Behrangi, A Imam, B Hsu, KL Todini, E Coccia, G Mazzetti, C Andres, EO Frances, F Orozco, I Hartman, R Henkel, A Fickenscher, P Staggs, S AF Smith, Michael Koren, Victor Zhang, Ziya Moreda, Fekadu Cui, Zhengtao Cosgrove, Brian Mizukami, Naoki Kitzmiller, David Ding, Feng Reed, Seann Anderson, Eric Schaake, John Zhang, Yu Andreassian, Vazken Perrin, Charles Coron, Laurent Valery, Audrey Khakbaz, Behnaz Sorooshian, Soroosh Behrangi, Ali Imam, Bisher Hsu, Kuo-Lin Todini, Ezio Coccia, Gabriele Mazzetti, Cinzia Andres, Enrique Ortiz Frances, Felix Orozco, Ismael Hartman, Robert Henkel, Arthur Fickenscher, Peter Staggs, Scott TI The distributed model intercomparison project - Phase 2: Experiment design and summary results of the western basin experiments SO JOURNAL OF HYDROLOGY LA English DT Article DE Hydrologic model; Rainfall-runoff; Distributed model; Lumped model; Calibration; Simulation ID AMERICAN RIVER-BASIN; GEOGRAPHIC INFORMATION-SYSTEM; NATIONAL-WEATHER-SERVICE; NORTHERN SIERRA-NEVADA; UNITED-STATES; HYDROLOGICAL MODELS; COMPLEX TERRAIN; STREAMFLOW SIMULATION; AUTOMATIC CALIBRATION; OKLAHOMA EXPERIMENTS AB The Office of Hydrologic Development (OHD) of the U.S. National Oceanic and Atmospheric Administration's (NOAA) National Weather Service (NWS) conducted the two phases of the Distributed Model Intercomparison Project (DMIP) as cost-effective studies to guide the transition to spatially distributed hydrologic modeling for operational forecasting at NWS River Forecast Centers (RFCs). Phase 2 of the Distributed Model lntercomparison Project (DMIP 2) was formulated primarily as a mechanism to help guide the U.S. NWS as it expands its use of spatially distributed watershed models for operational river, flash flood, and water resources forecasting. The overall purpose of DMIP 2 was to test many distributed models forced by high quality operational data with a view towards meeting NWS operational forecasting needs. At the same time, DMIP 2 was formulated as an experiment that could be leveraged by the broader scientific community as a platform for the testing, evaluation, and improvement of distributed models. DMIP 2 contained experiments in two regions: in the DMIP 1 Oklahoma basins, and second, in two basins in the Sierra Nevada Mountains in the western USA. This paper presents the overview and results of the DMIP 2 experiments conducted for the two Sierra Nevada basins. Simulations from five independent groups from France, Italy, Spain and the USA were analyzed. Experiments included comparison of lumped and distributed model streamflow simulations generated with uncalibrated and calibrated parameters, and simulations of snow water equivalent (SWE) at interior locations. As in other phases of DMIP, the participant simulations were evaluated against observed hourly streamflow and SWE data and compared with simulations provided by the NWS operational lumped model. A wide range of statistical measures are used to evaluate model performance on a run-period and event basis. Differences between uncalibrated and calibrated model simulations are assessed. Results indicate that in the two study basins, no single model performed best,in all cases. In addition, no distributed model was able to consistently outperform the lumped Model benchmark. However, one or more distributed models were able to outperform the lumped model benchmark in many of the analyses. Several calibrated distributed models achieved higher correlation and lower bias than the calibrated lumped benchmark in the calibration, validation, and combined periods. Evaluating a number of specific precipitation-runoff events, one calibrated distributed model was able to perform at a level equal to or better than the calibrated lumped model benchmark in terms of event-averaged peak and runoff volume error. However, three distributed models were able to provide improved peak timing compared to the lumped benchmark. Taken together, calibrated distributed models provided specific improvements over the lumped benchmark in 24% of the model-basin pairs for peak flow, 12% of the model-basin pairs for event runoff volume, and 41% of the model-basin pairs for peak timing. Model calibration improved the performance statistics of nearly all models (lumped and distributed). Analysis of several precipitation/runoff events indicates that distributed models may more accurately model the dynamics of the rain/snow line (and resulting hydrologic conditions) compared to the lumped benchmark model. Analysis of SWE simulations shows that better results were achieved at higher elevation observation sites. Although the performance of distributed models was mixed compared to the lumped benchmark, all calibrated models performed well compared to results in the DMIP 2 Oklahoma basins in terms of run period correlation and %Bias, and event-averaged peak and runoff error. This finding is noteworthy considering that these Sierra Nevada basins have complications such as orographically-enhanced precipitation, snow accumulation and melt, rain on snow events, and highly variable topography. Looking at these findings and those from the previous DMIP experiments, it is clear that at this point in their evolution, distributed models have the potential to provide valuable information on specific flood events that could complement lumped model simulations. Published by Elsevier B.V. C1 [Smith, Michael; Koren, Victor; Zhang, Ziya; Cui, Zhengtao; Cosgrove, Brian; Mizukami, Naoki; Kitzmiller, David; Ding, Feng; Reed, Seann; Anderson, Eric; Schaake, John; Zhang, Yu] Natl Weather Serv, Off Hydrol Dev, NOAA, Silver Spring, MD 20910 USA. [Moreda, Fekadu] Res Triangle Inst Int, Res Triangle Pk, NC USA. [Mizukami, Naoki] Natl Ctr Atmospher Res, Res Applicat Lab, Boulder, CO 80307 USA. [Ding, Feng] ADNET Syst Inc, Bethesda, MD 20817 USA. [Andreassian, Vazken; Perrin, Charles; Coron, Laurent; Valery, Audrey] Irstea Cemagref UR HBAN, F-92761 Antony, France. [Khakbaz, Behnaz] URS Corp, Ontario, CA 91764 USA. [Sorooshian, Soroosh; Hsu, Kuo-Lin] Univ Calif Irvine, Dept Civil & Environm Engn, Ctr Hydrometeorol & Remote Sensing, Irvine, CA 92697 USA. [Behrangi, Ali] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Imam, Bisher] UNESCO, Div Water Sci, Int Hydrol Programme, F-75732 Paris 15, France. [Todini, Ezio; Coccia, Gabriele] Univ Bologna, Dept Earth & Geoevironm Sci, I-40126 Bologna, Italy. [Mazzetti, Cinzia] PROGEA Srl, I-40125 Bologna, Italy. [Andres, Enrique Ortiz] Idrol & Ambience Srl, I-80122 Naples, Italy. [Frances, Felix; Orozco, Ismael] Univ Politecn Valencia, Res Inst Water Engn & Environm, Valencia 46022, Spain. [Hartman, Robert; Henkel, Arthur; Fickenscher, Peter; Staggs, Scott] Univ Corp Atmospher Res, Visiting Scientist Programs, Boulder, CO 80307 USA. RP Smith, M (reprint author), Natl Weather Serv, Off Hydrol Dev, NOAA, 1325 East West Highway, Silver Spring, MD 20910 USA. EM michael.smith@noaa.gov RI sorooshian, soroosh/B-3753-2008; Perrin, Charles/J-2486-2014; Frances, Felix/H-7179-2015; Mizukami, Naoki/J-7027-2015; OI sorooshian, soroosh/0000-0001-7774-5113; Perrin, Charles/0000-0001-8552-1881; Frances, Felix/0000-0003-1173-4969; Coccia, Gabriele/0000-0003-1124-3289 NR 174 TC 10 Z9 10 U1 1 U2 27 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 EI 1879-2707 J9 J HYDROL JI J. Hydrol. PD DEC 12 PY 2013 VL 507 BP 300 EP 329 DI 10.1016/j.jhydrol.2013.08.040 PG 30 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA 300UY UT WOS:000330490700025 ER PT J AU Li, GK Schwemmer, G Prasad, C Hwang, IH Lei, J Lee, SW Prasad, NS Philbrick, R AF Li, Guangkun Schwemmer, Geary Prasad, Coorg Hwang, I. H. Lei, Jie Lee, Sangwoo Prasad, Narasimha S. Philbrick, Russell TI Eye-safe compact Raman light detection and ranging temperature profiler SO APPLIED OPTICS LA English DT Article ID ATMOSPHERIC-TEMPERATURE; LIDAR MEASUREMENTS; SCATTERING; AEROSOL AB The vertical profile of atmospheric temperature is a principal state variable to study atmospheric stability. A lidar system, constructed using a 355 nm Nd:YAG laser transmitter, measures the temperature profile using the rotational Raman technique. In comparison with traditional Raman lidar, the major innovations are the use of a low peak power and high repetition rate laser to achieve eye-safe operation in a compact reliable instrument and the use of an angle tuning filter to select operating wavelengths. We demonstrate the capability of both nighttime and daytime measurements as a step toward a future stand-alone capability for routine measurements of important meteorological properties in the lower atmosphere. (C) 2013 Optical Society of America C1 [Li, Guangkun; Schwemmer, Geary] MassTech Inc, Columbia, MD 21046 USA. [Schwemmer, Geary; Prasad, Coorg; Hwang, I. H.; Lei, Jie; Lee, Sangwoo] Sci & Engn Serv Inc, Columbia, MD 21046 USA. [Prasad, Narasimha S.] NASA, Langley Res Ctr, Hampton, VA 23692 USA. [Philbrick, Russell] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Philbrick, Russell] N Carolina State Univ, Dept Atmospher Sci MEAS, Raleigh, NC 27695 USA. RP Prasad, C (reprint author), Sci & Engn Serv Inc, 6992 Columbia Gateway Dr,Suite 200, Columbia, MD 21046 USA. EM prasad@sesi-md.com FU NASA SBIR Phase I program entitled Raman Lidar Temperature Profiler [NNX12CF29P] FX The authors gratefully acknowledge funding under a NASA SBIR Phase I program entitled Raman Lidar Temperature Profiler, contract no. NNX12CF29P. NR 22 TC 0 Z9 0 U1 0 U2 3 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD DEC 10 PY 2013 VL 52 IS 35 BP 8540 EP 8548 DI 10.1364/AO.52.008540 PG 9 WC Optics SC Optics GA 273XN UT WOS:000328569700016 PM 24513899 ER PT J AU Aliu, E Archambault, S Behera, B Berger, K Beilicke, M Benbow, W Bird, R Bouvier, A Bugaev, V Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Dumm, J Falcone, A Federici, S Feng, Q Finley, JP Fortin, P Fortson, L Furniss, A Galante, N Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Kaaret, P Kertzman, M Khassen, Y Kieda, D Krennrich, F Lang, MJ Maier, G Majumdar, P McArthur, S McCann, A Moriarty, P Mukherjee, R de Bhroithe, AO Ong, RA Otte, AN Park, N Perkins, JS Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Rajotte, J Ratliff, G Reynolds, PT Richards, GT Roache, E Sembroski, GH Sheidaei, F Skole, C Smith, AW Staszak, D Telezhinsky, I Tyler, J Varlotta, A Vincent, S Wakely, SP Weekes, TC Weinstein, A Welsing, R Zajczyk, A Zitzer, B AF Aliu, E. Archambault, S. Behera, B. Berger, K. Beilicke, M. Benbow, W. Bird, R. Bouvier, A. Bugaev, V. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Dumm, J. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krennrich, F. Lang, M. J. Maier, G. Majumdar, P. McArthur, S. McCann, A. Moriarty, P. Mukherjee, R. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Rajotte, J. Ratliff, G. Reynolds, P. T. Richards, G. T. Roache, E. Sembroski, G. H. Sheidaei, F. Skole, C. Smith, A. W. Staszak, D. Telezhinsky, I. Tyler, J. Varlotta, A. Vincent, S. Wakely, S. P. Weekes, T. C. Weinstein, A. Welsing, R. Zajczyk, A. Zitzer, B. TI MULTIWAVELENGTH OBSERVATIONS OF THE TeV BINARY LS I+61 degrees 303 WITH VERITAS, Fermi-LAT, AND Swift/XRT DURING A TeV OUTBURST SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; binaries: general; gamma rays: stars; relativistic processes; X-rays: binaries ID GAMMA-RAY BINARY; X-RAY; EMISSION; +61-DEGREES-303; TELESCOPE; SPECTRUM; STAR AB We present the results of a multiwavelength observational campaign on the TeV binary system LS I +61 degrees 303 with the VERITAS telescope array (>200 GeV), Fermi-LAT (0.3-300 GeV), and Swift/XRT (2-10 keV). The data were taken from 2011 December through 2012 January and show a strong detection in all three wavebands. During this period VERITAS obtained 24.9 hr of quality selected livetime data in which LS I +61 degrees 303 was detected at a statistical significance of 11.9 sigma. These TeV observations show evidence for nightly variability in the TeV regime at a post-trial significance of 3.6 sigma. The combination of the simultaneously obtained TeV and X-ray fluxes do not demonstrate any evidence for a correlation between emission in the two bands. For the first time since the launch of the Fermi satellite in 2008, this TeV detection allows the construction of a detailed MeV-TeV spectral energy distribution from LS I +61 degrees 303. This spectrum shows a distinct cutoff in emission near 4 GeV, with emission seen by the VERITAS observations following a simple power-law above 200 GeV. This feature in the spectrum of LS I +61 degrees 303, obtained from overlapping observations with Fermi-LAT and VERITAS, may indicate that there are two distinct populations of accelerated particles producing the GeV and TeV emission. C1 [Aliu, E.; Humensky, T. B.; Mukherjee, R.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Behera, B.; Chen, X.; Federici, S.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Skole, C.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Berger, K.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Beilicke, M.; Bugaev, V.; Zajczyk, A.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Roache, E.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bird, R.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Bouvier, A.; Furniss, A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Furniss, A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Chen, X.; Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.; Ratliff, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Kieda, D.; Sheidaei, F.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Krennrich, F.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Majumdar, P.; Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Majumdar, P.] Saha Inst Nucl Phys, Kolkata 700064, W Bengal, India. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. RP Aliu, E (reprint author), Columbia Univ, Dept Phys, 538 W 120th St, New York, NY 10027 USA. EM sheidaei@physics.utah.edu; aw.smith@utah.edu RI Khassen, Yerbol/I-3806-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Cui, Wei/0000-0002-6324-5772 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K. FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. We thank the Swift Team for scheduling contemporaneous observations and providing data and analysis tools. The authors would also like to thank Jeremy Perkins for his tireless assistance with Fermi-LAT data analysis. NR 40 TC 5 Z9 5 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR UNSP 88 DI 10.1088/0004-637X/779/1/88 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100088 ER PT J AU Bothwell, MS Aguirre, JE Chapman, SC Marrone, DP Vieira, JD Ashby, MLN Aravena, M Benson, BA Bock, JJ Bradford, CM Brodwin, M Carlstrom, JE Crawford, TM De Breuck, C Downes, TP Fassnacht, CD Gonzalez, AH Greve, TR Gullberg, B Hezaveh, Y Holder, GP Holzapfel, WL Ibar, E Ivison, R Kamenetzky, J Keisler, R Lupu, RE Ma, J Malkan, M McIntyre, V Murphy, EJ Nguyen, HT Reichardt, CL Rosenman, M Spilker, JS Stalder, B Stark, AA Strandet, M Vernet, J Weiss, A Welikala, N AF Bothwell, M. S. Aguirre, J. E. Chapman, S. C. Marrone, D. P. Vieira, J. D. Ashby, M. L. N. Aravena, M. Benson, B. A. Bock, J. J. Bradford, C. M. Brodwin, M. Carlstrom, J. E. Crawford, T. M. De Breuck, C. Downes, T. P. Fassnacht, C. D. Gonzalez, A. H. Greve, T. R. Gullberg, B. Hezaveh, Y. Holder, G. P. Holzapfel, W. L. Ibar, E. Ivison, R. Kamenetzky, J. Keisler, R. Lupu, R. E. Ma, J. Malkan, M. McIntyre, V. Murphy, E. J. Nguyen, H. T. Reichardt, C. L. Rosenman, M. Spilker, J. S. Stalder, B. Stark, A. A. Strandet, M. Vernet, J. Weiss, A. Welikala, N. TI SPT 0538-50: PHYSICAL CONDITIONS IN THE INTERSTELLAR MEDIUM OF A STRONGLY LENSED DUSTY STAR-FORMING GALAXY AT z=2.8 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: individual; gravitational lensing: strong; submillimeter: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; SOUTH-POLE TELESCOPE; LUMINOUS SUBMILLIMETER GALAXIES; HERSCHEL-SPIRE SPECTROSCOPY; SCIENCE DEMONSTRATION PHASE; SPITZER-SPACE-TELESCOPE; INITIAL MASS FUNCTION; MOLECULAR GAS; HIGH-REDSHIFT; FORMATION HISTORY AB We present observations of SPT-S J053816-5030.8, a gravitationally lensed dusty star-forming galaxy (DSFG) at z = 2.7817 that was first discovered at millimeter wavelengths by the South Pole Telescope. SPT 0538-50 is typical of the brightest sources found by wide-field millimeter-wavelength surveys, being lensed by an intervening galaxy at moderate redshift (in this instance, at z = 0.441). We present a wide array of multi-wavelength spectroscopic and photometric data on SPT 0538-50, including data from ALMA, Herschel PACS and SPIRE, Hubble, Spitzer, the Very Large Telescope, ATCA, APEX, and the Submillimeter Array. We use high-resolution imaging from the Hubble Space Telescope to de-blend SPT 0538-50, separating DSFG emission from that of the foreground lens. Combined with a source model derived from ALMA imaging (which suggests a magnification factor of 21+/-4), we derive the intrinsic properties of SPT 0538-50, including the stellar mass, far-IR luminosity, star formation rate, molecular gas mass, and-using molecular line fluxes-the excitation conditions within the interstellar medium. The derived physical properties argue that we arewitnessing compact, merger-driven star formation in SPT 0538-50 similar to local starburst galaxies and unlike that seen in some other DSFGs at this epoch. C1 [Bothwell, M. S.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HA, England. [Bothwell, M. S.; Marrone, D. P.; Spilker, J. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Aguirre, J. E.; Lupu, R. E.; Rosenman, M.] Univ Penn, Philadelphia, PA 19104 USA. [Chapman, S. C.] Dalhousie Univ, Halifax, NS, Canada. [Vieira, J. D.; Bock, J. J.; Downes, T. P.] CALTECH, Pasadena, CA 91125 USA. [Ashby, M. L. N.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Aravena, M.; De Breuck, C.; Gullberg, B.; Vernet, J.] European So Observ, Casilla 19001, Vitacura Santia, Chile. [Aravena, M.] Univ Diego Portales, Fac Ingn, Santiago, Chile. [Benson, B. A.; Carlstrom, J. E.; Keisler, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bock, J. J.; Bradford, C. M.; Nguyen, H. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Keisler, R.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.] Argonne Natl Lab, Argonne, IL 60439 USA. [Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Gonzalez, A. H.; Ma, J.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Hezaveh, Y.; Holder, G. P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Holzapfel, W. L.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Ibar, E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Ivison, R.] Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Kamenetzky, J.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [McIntyre, V.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Murphy, E. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Strandet, M.; Weiss, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Welikala, N.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France. RP Bothwell, MS (reprint author), Univ Cambridge, Cavendish Lab, JJ Thompson Ave, Cambridge CB3 0HA, England. RI Aravena, Manuel/O-2361-2014; Lupu, Roxana/P-9060-2014; Holzapfel, William/I-4836-2015; Ivison, R./G-4450-2011 OI Lupu, Roxana/0000-0003-3444-5908; Marrone, Daniel/0000-0002-2367-1080; Reichardt, Christian/0000-0003-2226-9169; Vernet, Joel/0000-0002-8639-8560; De Breuck, Carlos/0000-0002-6637-3315; Stark, Antony/0000-0002-2718-9996; Ivison, R./0000-0001-5118-1313 FU Smithsonian Institution; Academia Sinica; National Science Foundation [AST-1009649, ANT-0638937, PHY-1125897, PHYS-1066293]; NASA from the Space Telescope Science Institute [HST-GO-12659]; JPL/Caltech [OT1_dmarrone_1, OT1_jvieira_4, OT2_jvieira_5] FX We thank the anonymous referee who provided comments that helped improve the clarity of this manuscript. The authors would like to thank N. Rangwala for sharing the M82 CO flux densities. M. S. B. would like to acknowledge the hospitality of the Aspen Center for Physics, where some of this manuscript was written. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Support is provided by National Science Foundation grants AST-1009649, ANT-0638937, PHY-1125897, and PHYS-1066293. This paper makes use of the following ALMA data: ADS/JAO. ALMA #2011.0.00957.S and #2011.0.00958.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under a cooperative agreement by Associated Universities, Inc. Partial support for this work was provided by NASA through grant HST-GO-12659 from the Space Telescope Science Institute and awards for Herschel analysis issued by JPL/Caltech for OT1_dmarrone_1, OT1_jvieira_4, and OT2_jvieira_5. NR 86 TC 17 Z9 17 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR 67 DI 10.1088/0004-637X/779/1/67 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100067 ER PT J AU Bussmann, RS Perez-Fournon, I Amber, S Calanog, J Gurwell, MA Dannerbauer, H De Bernardis, F Fu, H Harris, AI Krips, M Lapi, A Maiolino, R Omont, A Riechers, D Wardlow, J Baker, AJ Birkinshaw, M Bock, J Bourne, N Clements, DL Cooray, A De Zotti, G Dunne, L Dye, S Eales, S Farrah, D Gavazzi, R Nuevo, JG Hopwood, R Ibar, E Ivison, RJ Laporte, N Maddox, S Martinez-Navajas, P Michalowski, M Negrello, M Oliver, SJ Roseboom, IG Scott, D Serjeant, S Smith, AJ Smith, M Streblyanska, A Valiante, E van der Werf, P Verma, A Vieira, JD Wang, L Wilner, D AF Bussmann, R. S. Perez-Fournon, I. Amber, S. Calanog, J. Gurwell, M. A. Dannerbauer, H. De Bernardis, F. Fu, Hai Harris, A. I. Krips, M. Lapi, A. Maiolino, R. Omont, A. Riechers, D. Wardlow, J. Baker, A. J. Birkinshaw, M. Bock, J. Bourne, N. Clements, D. L. Cooray, A. De Zotti, G. Dunne, L. Dye, S. Eales, S. Farrah, D. Gavazzi, R. Nuevo, J. Gonzalez Hopwood, R. Ibar, E. Ivison, R. J. Laporte, N. Maddox, S. Martinez-Navajas, P. Michalowski, M. Negrello, M. Oliver, S. J. Roseboom, I. G. Scott, Douglas Serjeant, S. Smith, A. J. Smith, Matthew Streblyanska, A. Valiante, E. van der Werf, P. Verma, A. Vieira, J. D. Wang, L. Wilner, D. TI GRAVITATIONAL LENS MODELS BASED ON SUBMILLIMETER ARRAY IMAGING OF HERSCHEL-SELECTED STRONGLY LENSED SUB-MILLIMETER GALAXIES AT z > 1.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: fundamental parameters; galaxies: halos; galaxies: high-redshift; gravitational lensing: strong ID STAR-FORMING GALAXIES; SOUTH-POLE TELESCOPE; DEEP-FIELD-SOUTH; ULTRALUMINOUS INFRARED GALAXIES; MOLECULAR INTERSTELLAR-MEDIUM; ALL-SKY SURVEY; HIGH-REDSHIFT; HIGH-RESOLUTION; NUMBER COUNTS; EXTRAGALACTIC SURVEY AB Strong gravitational lenses are now being routinely discovered in wide-field surveys at (sub-)millimeter wavelengths. We present Submillimeter Array (SMA) high-spatial resolution imaging and Gemini-South and Multiple Mirror Telescope optical spectroscopy of strong lens candidates discovered in the two widest extragalactic surveys conducted by the Herschel Space Observatory: the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS) and the Herschel Multi-tiered Extragalactic Survey (HerMES). From a sample of 30 Herschel sources with S-500 > 100 mJy, 21 are strongly lensed (i.e., multiply imaged), 4 are moderately lensed (i.e., singly imaged), and the remainder require additional data to determine their lensing status. We apply a visibility-plane lens modeling technique to the SMA data to recover information about the masses of the lenses as well as the intrinsic (i.e., unlensed) sizes (r(half)) and far-infrared luminosities (L-FIR) of the lensed submillimeter galaxies (SMGs). The sample of lenses comprises primarily isolated massive galaxies, but includes some groups and clusters as well. Several of the lenses are located at z(lens) > 0.7, a redshift regime that is inaccessible to lens searches based on Sloan Digital Sky Survey spectroscopy. The lensed SMGs are amplified by factors that are significantly below statistical model predictions given the 500 mu m flux densities of our sample. We speculate that this may reflect a deficiency in our understanding of the intrinsic sizes and luminosities of the brightest SMGs. The lensed SMGs span nearly one decade in L-FIR (median L-FIR = 7.9 x 10(12) L-circle dot) and two decades in FIR luminosity surface density (median Sigma(FIR) = 6.0 x 10(11) L-circle dot kpc(-2)). The strong lenses in this sample and others identified via (sub-) mm surveys will provide a wealth of information regarding the astrophysics of galaxy formation and evolution over a wide range in redshift. C1 [Bussmann, R. S.; Gurwell, M. A.; Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Perez-Fournon, I.; Laporte, N.; Martinez-Navajas, P.; Streblyanska, A.] IAC, E-38200 Tenerife, Spain. [Perez-Fournon, I.; Laporte, N.; Martinez-Navajas, P.; Streblyanska, A.] ULL, Dept Astrofis, E-38205 Tenerife, Spain. [Amber, S.; Serjeant, S.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Calanog, J.; De Bernardis, F.; Wardlow, J.; Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dannerbauer, H.] CEA DSM Irfu CNRS Univ Paris Diderot, Lab AIM Paris Saclay, CE Saclay, F-91191 Gif Sur Yvette, France. [Fu, Hai] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Harris, A. I.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Krips, M.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Lapi, A.] Univ Tor Vergata, Dept Fis, I-00133 Rome, Italy. [Lapi, A.] SISSA, I-34136 Trieste, Italy. [Maiolino, R.] Univ Cambridge, Cavendish Lab, Cambridge CB3 OHF, England. [Maiolino, R.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 OHA, England. [Omont, A.; Gavazzi, R.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Riechers, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Birkinshaw, M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Bock, J.; Cooray, A.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bourne, N.; Dye, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Clements, D. L.; Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [De Zotti, G.; Negrello, M.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Dunne, L.; Maddox, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand. [Eales, S.; Smith, Matthew] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Nuevo, J. Gonzalez] Inst Fis Cantabria CSIC UC, Santander 39005, Spain. [Ibar, E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.; Michalowski, M.; Roseboom, I. G.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Oliver, S. J.; Roseboom, I. G.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Scott, Douglas; Valiante, E.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [van der Werf, P.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Verma, A.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. RP Bussmann, RS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Wardlow, Julie/C-9903-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Ivison, R./G-4450-2011; OI Wardlow, Julie/0000-0003-2376-8971; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Ivison, R./0000-0001-5118-1313; Scott, Douglas/0000-0002-6878-9840 FU NASA through JPL; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA); SMA Fellowship program; NSF [AST-0645427]; National Science Foundation [PHY-1066293]; Science and Technology Facilities Council [ST/I000976/1]; PRIN INAF; Programme National Cosmologie et Galaxies (PNCG); Spanish CSIC for a JAE-DOC; Spanish Ministerio de Ciencia e Innovacion [AYA2010-21766-C03-01]; Spanish grant [AYA2010-21697-C05-04] FX The results described in this paper are based on observations obtained with Herschel, an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The Herschel-ATLAS is a project with Herschel. The H-ATLAS Web site is http://www.h-atlas.org/. US participants in H-ATLAS acknowledge support from NASA through a contract from JPL.; SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).; R. S. B. acknowledges support from the SMA Fellowship program. H. F, A. C., and J.L.W. acknowledge support from NSF CAREER AST-0645427. A portion of this work was completed at the Aspen Center for Physics during a 2013 summer workshop on dusty galaxies at high redshift. R. S. B. acknowledges the hospitality of the Aspen Center for Physics, which is supported by the National Science Foundation Grant No. PHY-1066293. S.J.O., L. W., and A. S. acknowledge support from the Science and Technology Facilities Council (grant No. ST/I000976/1). M.N. acknowledges financial support from PRIN INAF 2012 project "Looking into the dust-obscured phase of galaxy formation through cosmic zoom lenses in the Herschel Astrophysical Large Area Survey." A.O. and R. G. acknowledge support from the Programme National Cosmologie et Galaxies (PNCG). J.G.N. acknowledges financial support from Spanish CSIC for a JAE-DOC fellowship and partial financial support from the Spanish Ministerio de Ciencia e Innovacion project AYA2010-21766-C03-01. I.P.-F., P.M.-N., N.L. and A.S. acknowledge support from the Spanish grant AYA2010-21697-C05-04. We thank K. Rosenfeld for assistance in implementing the visibility-plane aspect of the lens modeling software used in this paper. We thank the anonymous referee for a timely review that provided useful comments and helped improved the clarity of the manuscript. NR 126 TC 59 Z9 59 U1 0 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR 25 DI 10.1088/0004-637X/779/1/25 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100025 ER PT J AU Castro, D Lopez, LA Slane, PO Yamaguchi, H Ramirez-Ruiz, E Figueroa-Feliciano, E AF Castro, Daniel Lopez, Laura A. Slane, Patrick O. Yamaguchi, Hiroya Ramirez-Ruiz, Enrico Figueroa-Feliciano, Enectali TI A CHANDRA VIEW OF NON-THERMAL EMISSION IN THE NORTHWESTERN REGION OF SUPERNOVA REMNANT RCW 86: PARTICLE ACCELERATION AND MAGNETIC FIELDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; ISM: individual objects (RCW 86); ISM: supernova remnants; magnetic fields; X-rays: ISM ID DIFFUSIVE SHOCK ACCELERATION; RAY SYNCHROTRON EMISSION; X-RAY; HIGH-RESOLUTION; COSMIC-RAYS; SHELL; DISCOVERY; AMPLIFICATION; FILAMENTS; SN-1006 AB The shocks of supernova remnants are believed to accelerate particles to cosmic ray (CR) energies. The amplification of the magnetic field due to CRs propagating in the shock region is expected to have an impact on both the emission from the accelerated particle population as well as the acceleration process itself. Using a 95 ks observation with the Advanced CCD Imaging Spectrometer on board the Chandra X-Ray Observatory, we map and characterize the synchrotron emitting material in the northwest region of RCW 86. We model spectra from several different regions, both filamentary and diffuse, where emission appears to be dominated by synchrotron radiation. The fine spatial resolution of Chandra allows us to obtain accurate emission profiles across three different non-thermal rims in this region. The narrow width (l approximate to 10 ''-30 '') of these filaments constrains the minimum magnetic field strength at the post-shock region to approximately 80 mu G. C1 [Castro, Daniel; Lopez, Laura A.; Figueroa-Feliciano, Enectali] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. [Slane, Patrick O.; Yamaguchi, Hiroya] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yamaguchi, Hiroya] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yamaguchi, Hiroya] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Ramirez-Ruiz, Enrico] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95060 USA. RP Castro, D (reprint author), MIT, Kavli Ctr Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. FU Chandra GO grant [GO3-14080]; National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory [SV3-73016]; National Aeronautics Space Administration [NAS8-03060]; National Aeronautics and Space Administration [NAS8-03060] FX The authors thank Parviz Ghavamian for some important discussions and insight. Also, they thank John Dickel for providing ATCA data. D.C. acknowledges support for this work provided by the Chandra GO grant GO3-14080 as well as the National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory contract SV3-73016 to MIT for Support of the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. P.C. acknowledges support from the National Aeronautics and Space Administration under contract NAS8-03060. NR 50 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR 49 DI 10.1088/0004-637X/779/1/49 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100049 ER PT J AU Colbert, JW Teplitz, H Atek, H Bunker, A Rafelski, M Ross, N Scarlata, C Bedregal, AG Dominguez, A Dressler, A Henry, A Malkan, M Martin, CL Masters, D McCarthy, P Siana, B AF Colbert, James W. Teplitz, Harry Atek, Hakim Bunker, Andrew Rafelski, Marc Ross, Nathaniel Scarlata, Claudia Bedregal, Alejandro G. Dominguez, Alberto Dressler, Alan Henry, Alaina Malkan, Matt Martin, Crystal L. Masters, Dan McCarthy, Patrick Siana, Brian TI PREDICTING FUTURE SPACE NEAR-IR GRISM SURVEYS USING THE WFC3 INFRARED SPECTROSCOPIC PARALLELS SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: luminosity function, mass function ID STAR-FORMATION RATE; ALPHA LUMINOSITY FUNCTION; EMISSION-LINE GALAXIES; HIGH-REDSHIFT SURVEY; H-ALPHA; FORMING GALAXIES; DARK ENERGY; DUST EXTINCTION; TELESCOPE; HIZELS AB We present near-infrared emission line counts and luminosity functions from the Hubble Space Telescope Wide Field Camera 3 Infrared Spectroscopic Parallels (WISP) program for 29 fields (0.037 deg(2)) observed using both the G102 and G141 grism. Altogether we identify 1048 emission line galaxies with observed equivalent widths greater than 40 angstrom, 467 of which have multiple detected emission lines. We use simulations to correct for significant (>20%) incompleteness introduced in part by the non-dithered, non-rotated nature of the grism parallels. The WISP survey is sensitive to fainter flux levels ((3-5) x 10(-17) erg s(-1) cm(-2)) than the future space near-infrared grism missions aimed at baryonic acoustic oscillation cosmology ((1-4) x 10(-16) erg s(-1) cm(-2)), allowing us to probe the fainter emission line galaxies that the shallower future surveys may miss. Cumulative number counts of 0.7 < z < 1.5 galaxies reach 10,000 deg(-2) above an H alpha flux of 2 x 10(-16) erg s(-1) cm(-2). H alpha-emitting galaxies with comparable [O III] flux are roughly five times less common than galaxies with just H alpha emission at those flux levels. Galaxies with low H alpha/[O III] ratios are very rare at the brighter fluxes that future near-infrared grism surveys will probe; our survey finds no galaxies with H alpha/[O III] < 0.95 that have H alpha flux greater than 3 x 10(-16) erg s(-1) cm(-2). Our H alpha luminosity function contains a comparable number density of faint line emitters to that found by the Near IR Camera and Multi-Object Spectrometer near-infrared grism surveys, but significantly fewer (factors of 3-4 less) high-luminosity emitters. We also find that our high-redshift (z = 0.9-1.5) counts are in agreement with the high-redshift (z = 1.47) narrowband H alpha survey of HiZELS (Sobral et al.), while our lower redshift luminosity function (z = 0.3-0.9) falls slightly below their z = 0.84 result. The evolution in both the H alpha luminosity function from z = 0.3-1.5 and the [O III] luminosity function from z = 0.7-2.3 is almost entirely in the L-star parameter, which steadily increases with redshift over those ranges. C1 [Colbert, James W.; Atek, Hakim] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Teplitz, Harry; Rafelski, Marc] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Atek, Hakim] Ecole Polytech Fed Lausanne, Astrophys Lab, Observ Sauverny, CH-1290 Versoix, Switzerland. [Bunker, Andrew] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Ross, Nathaniel; Malkan, Matt] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. [Scarlata, Claudia; Bedregal, Alejandro G.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Bedregal, Alejandro G.] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. [Dominguez, Alberto; Masters, Dan; Siana, Brian] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Dressler, Alan; Masters, Dan; McCarthy, Patrick] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Henry, Alaina] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Martin, Crystal L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. RP Colbert, JW (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. OI Dominguez, Alberto/0000-0002-3433-4610 FU grants for HST programs [GO-10226, GO-11696, GO-12283] FX We would like to acknowledge the assistance of Chun Ly for his helpful advice during the production of this paper. The authors would also like to acknowledge financial support from the grants for HST programs GO-10226, GO-11696, and GO-12283. NR 55 TC 28 Z9 28 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR UNSP 34 DI 10.1088/0004-637X/779/1/34 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100034 ER PT J AU Furst, F Grefenstette, BW Staubert, R Tomsick, JA Bachetti, M Barret, D Bellm, EC Boggs, SE Chenevez, J Christensen, FE Craig, WW Hailey, CJ Harrison, F Klochkov, D Madsen, KK Pottschmidt, K Stern, D Walton, DJ Wilms, J Zhang, W AF Fuerst, Felix Grefenstette, Brian W. Staubert, Ruediger Tomsick, John A. Bachetti, Matteo Barret, Didier Bellm, Eric C. Boggs, Steven E. Chenevez, Jerome Christensen, Finn E. Craig, William W. Hailey, Charles J. Harrison, Fiona Klochkov, Dmitry Madsen, Kristin K. Pottschmidt, Katja Stern, Daniel Walton, Dominic J. Wilms, Joern Zhang, William TI THE SMOOTH CYCLOTRON LINE IN HER X-1 AS SEEN WITH NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; pulsars: individual (Her X-1); stars: neutron; X-rays: binaries ID X-RAY PULSARS; PHASE-RESOLVED SPECTROSCOPY; 35 DAY EVOLUTION; ACCRETION DISK; MAGNETIC-FIELDS; NEUTRON-STAR; HERCULES X-1; LIGHT-CURVE; MAIN-ON; RXTE AB Her X-1, one of the brightest and best studied X-ray binaries, shows a cyclotron resonant scattering feature (CRSF) near 37 keV. This makes it an ideal target for a detailed study with the Nuclear Spectroscopic Telescope Array (NuSTAR), taking advantage of its excellent hard X-ray spectral resolution. We observed Her X-1 three times, coordinated with Suzaku, during one of the high flux intervals of its 35 day superorbital period. This paper focuses on the shape and evolution of the hard X-ray spectrum. The broadband spectra can be fitted with a power law with a high-energy cutoff, an iron line, and a CRSF. We find that the CRSF has a very smooth and symmetric shape in all observations and at all pulse phases. We compare the residuals of a line with a Gaussian optical-depth profile to a Lorentzian optical-depth profile and find no significant differences, strongly constraining the very smooth shape of the line. Even though the line energy changes dramatically with pulse phase, we find that its smooth shape does not. Additionally, our data show that the continuum only changes marginally between the three observations. These changes can be explained with varying amounts of Thomson scattering in the hot corona of the accretion disk. The average, luminosity-corrected CRSF energy is lower than in past observations and follows a secular decline. The excellent data quality of NuSTAR provides the best constraint on the CRSF energy to date. C1 [Fuerst, Felix; Grefenstette, Brian W.; Bellm, Eric C.; Harrison, Fiona; Madsen, Kristin K.; Walton, Dominic J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Staubert, Ruediger; Klochkov, Dmitry] Univ Tubingen IAAT, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Tomsick, John A.; Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bachetti, Matteo; Barret, Didier] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France. [Bachetti, Matteo; Barret, Didier] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Chenevez, Jerome; Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Pottschmidt, Katja] UMBC, CRESST, Greenbelt, MD 20771 USA. [Pottschmidt, Katja; Zhang, William] NASA GSFC, Greenbelt, MD 20771 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wilms, Joern] Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany. [Wilms, Joern] ECAP, D-96049 Bamberg, Germany. RP Furst, F (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RI Wilms, Joern/C-8116-2013; Boggs, Steven/E-4170-2015; XRAY, SUZAKU/A-1808-2009; OI Wilms, Joern/0000-0003-2065-5410; Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337; Madsen, Kristin/0000-0003-1252-4891 FU NASA [NNG08FD60C]; NASA Astrophysics Data Analysis Program [NNX13AE98G]; Centre National d'Etudes Spatiales (CNES) FX This work was supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We would like to thank John E. Davis for the slxfig module, which was used to produce all figures in this work. F. F. would also like to thank the Remeis-Observatory Bamberg for their hospitality. J.A.T. acknowledges partial support from NASA Astrophysics Data Analysis Program grant NNX13AE98G. M. B. was supported by the Centre National d'Etudes Spatiales (CNES). NR 55 TC 18 Z9 18 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR UNSP 69 DI 10.1088/0004-637X/779/1/69 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100069 ER PT J AU Gorczyca, TW Bautista, MA Hasoglu, MF Garcia, J Gatuzz, E Kaastra, JS Kallman, TR Manson, ST Mendoza, C Raassen, AJJ de Vries, CP Zatsarinny, O AF Gorczyca, T. W. Bautista, M. A. Hasoglu, M. F. Garcia, J. Gatuzz, E. Kaastra, J. S. Kallman, T. R. Manson, S. T. Mendoza, C. Raassen, A. J. J. de Vries, C. P. Zatsarinny, O. TI A COMPREHENSIVE X-RAY ABSORPTION MODEL FOR ATOMIC OXYGEN SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; ISM: atoms; line: formation; line: profiles; X-rays: ISM ID PHOTOIONIZATION CROSS-SECTIONS; K-SHELL PHOTOABSORPTION; INTERSTELLAR-MEDIUM; XMM-NEWTON; R-MATRIX; WAVELENGTH MEASUREMENTS; OSCILLATOR-STRENGTHS; ANALYTIC FITS; CHANDRA; IONS AB An analytical formula is developed to accurately represent the photoabsorption cross section of O I for all energies of interest in X-ray spectral modeling. In the vicinity of the K edge, a Rydberg series expression is used to fit R-matrix results, including important orbital relaxation effects, that accurately predict the absorption oscillator strengths below threshold and merge consistently and continuously to the above-threshold cross section. Further, minor adjustments are made to the threshold energies in order to reliably align the atomic Rydberg resonances after consideration of both experimental and observed line positions. At energies far below or above the K-edge region, the formulation is based on both outer-and inner-shell direct photoionization, including significant shake-up and shake-off processes that result in photoionization-excitation and double-photoionization contributions to the total cross section. The ultimate purpose for developing a definitive model for oxygen absorption is to resolve standing discrepancies between the astronomically observed and laboratory-measured line positions, and between the inferred atomic and molecular oxygen abundances in the interstellar medium from XSTAR and SPEX spectral models. C1 [Gorczyca, T. W.; Bautista, M. A.; Mendoza, C.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Hasoglu, M. F.] Hasan Kalyoncu Univ, TR-27100 Sahinbey, Gaziantep, Turkey. [Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gatuzz, E.; Mendoza, C.] Inst Venezolano Invest Cient, Ctr Fis, Caracas 1020, Venezuela. [Kaastra, J. S.; Raassen, A. J. J.; de Vries, C. P.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Kaastra, J. S.] Univ Utrecht, Sterrenkundig Inst, NL-3508 TA Utrecht, Netherlands. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Manson, S. T.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Raassen, A. J. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Zatsarinny, O.] Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA. RP Gorczyca, TW (reprint author), Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. FU NASA [NNX11AF32G]; DOE, Office of Chemical Sciences, Atomic, Molecular and Optical Sciences Program [DE-FG02-03ER15428] FX T.W.G. acknowledges support by NASA (NNX11AF32G). S. T. M. acknowledges support by DOE, Office of Chemical Sciences, Atomic, Molecular and Optical Sciences Program (DE-FG02-03ER15428). NR 52 TC 11 Z9 11 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR 78 DI 10.1088/0004-637X/779/1/78 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100078 ER PT J AU Gressel, O Nelson, RP Turner, NJ Ziegler, U AF Gressel, O. Nelson, R. P. Turner, N. J. Ziegler, U. TI GLOBAL HYDROMAGNETIC SIMULATIONS OF A PLANET EMBEDDED IN A DEAD ZONE: GAP OPENING, GAS ACCRETION, AND FORMATION OF A PROTOPLANETARY JET SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); methods: numerical; planets and satellites: formation; protoplanetary disks ID TAURUS MOLECULAR CLOUD; HIGH-MASS PLANETS; GIANT PLANETS; MAGNETOROTATIONAL INSTABILITY; IDEAL MAGNETOHYDRODYNAMICS; CONSTRAINED TRANSPORT; PROTOSTELLAR DISKS; ANGULAR-MOMENTUM; CIRCUMPLANETARY DISKS; IONIZATION STATE AB We present global hydrodynamic (HD) and magnetohydrodynamic (MHD) simulations with mesh refinement of accreting planets embedded in protoplanetary disks (PPDs). The magnetized disk includes Ohmic resistivity that depends on the overlying mass column, leading to turbulent surface layers and a dead zone near the midplane. The main results are: (1) the accretion flow in the Hill sphere is intrinsically three-dimensional for HD and MHD models. Net inflow toward the planet is dominated by high-latitude flows. A circumplanetary disk (CPD) forms. Its midplane flows outward in a pattern whose details differ between models. (2) The opening of a gap magnetically couples and ignites the dead zone near the planet, leading to stochastic accretion, a quasi-turbulent flow in the Hill sphere, and a CPD whose structure displays high levels of variability. (3) Advection of magnetized gas onto the rotating CPD generates helical fields that launch magnetocentrifugally driven outflows. During one specific epoch, a highly collimated, one-sided jet is observed. (4) The CPD's surface density is similar to 30 g cm(-2), small enough for significant ionization and turbulence to develop. (5) The accretion rate onto the planet in the MHD simulation reaches a steady value 8 x 10(-3) M-circle plus yr(-1) and is similar in the viscous HD runs. Our results suggest that gas accretion onto a forming giant planet within a magnetized PPD with a dead zone allows rapid growth from Saturnian to Jovian masses. As well as being relevant for giant planet formation, these results have important implications for the formation of regular satellites around gas giant planets. C1 [Gressel, O.] KTH Royal Inst Technol, NORDITA, SE-10691 Stockholm, Sweden. [Gressel, O.] Stockholm Univ, SE-10691 Stockholm, Sweden. [Gressel, O.; Nelson, R. P.] Queen Mary Univ London, Astron Unit, London E1 4NS, England. [Turner, N. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ziegler, U.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. RP Gressel, O (reprint author), KTH Royal Inst Technol, NORDITA, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden. EM oliver.gressel@nordita.org; r.p.nelson@qmul.ac.uk; neal.j.turner@jpl.nasa.gov; uziegler@aip.de RI Gressel, Oliver/D-3683-2014 OI Gressel, Oliver/0000-0002-5398-9225 FU National Aeronautics and Space Administration FX We thank the anonymous referee for useful comments that led to an improvement of this paper. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The simulations presented in this paper were run on the QMUL HPC facility. Three-dimensional imagery produced by vapor (Clyne et al. 2007; www.vapor.ucar.edu), a product of the Computational Information Systems Laboratory at the National Center for Atmospheric Research. NR 80 TC 32 Z9 32 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR 59 DI 10.1088/0004-637X/779/1/59 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100059 ER PT J AU Kennedy, MB Milligan, RO Mathioudakis, M Keenan, FP AF Kennedy, Michael B. Milligan, Ryan O. Mathioudakis, Mihalis Keenan, Francis P. TI SOLAR FLARE IMPULSIVE PHASE EMISSION OBSERVED WITH SDO/EVE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: chromosphere; Sun: corona; Sun: flares ID HARD X-RAY; EXTREME-ULTRAVIOLET; ATOMIC DATABASE; SPECTRA; EUV; BRIGHTENINGS; TEMPERATURE; CONNECTION; FOOTPOINTS; DYNAMICS AB Differential emission measures (DEMs) during the impulsive phase of solar flares were constructed using observations from the EUV Variability Experiment (EVE) and the Markov-Chain Monte Carlo method. Emission lines from ions formed over the temperature range log T-e = 5.8-7.2 allow the evolution of the DEM to be studied over a wide temperature range at 10 s cadence. The technique was applied to several M-and X-class flares, where impulsive phase EUV emission is observable in the disk-integrated EVE spectra from emission lines formed up to 3-4 MK and we use spatially unresolved EVE observations to infer the thermal structure of the emitting region. For the nine events studied, the DEMs exhibited a two-component distribution during the impulsive phase, a low-temperature component with peak temperature of 1-2 MK, and a broad high-temperature component from 7 to 30 MK. A bimodal high-temperature component is also found for several events, with peaks at 8 and 25 MK during the impulsive phase. The origin of the emission was verified using Atmospheric Imaging Assembly images to be the flare ribbons and footpoints, indicating that the constructed DEMs represent the spatially average thermal structure of the chromospheric flare emission during the impulsive phase. C1 [Kennedy, Michael B.; Milligan, Ryan O.; Mathioudakis, Mihalis; Keenan, Francis P.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Milligan, Ryan O.] NASA, Solar Phys Lab, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Milligan, Ryan O.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Kennedy, MB (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland. EM mkennedy29@qub.ac.uk FU Northern Ireland Department of Employment and Learning; Leverhulme Trust [F/00203/X]; NASA [NNX11AQ53G]; Air Force Office of Scientific Research, Air Force Material Command, USAF [FA8655-09-13085] FX M.B.K. thanks the Northern Ireland Department of Employment and Learning for the award of a PhD studentship. R.O.M. is grateful to the Leverhulme Trust for financial support from grant F/00203/X, and to NASA for LWS/TR&T grant NNX11AQ53G. We thank the Air Force Office of Scientific Research, Air Force Material Command, USAF for sponsorship under grant No. FA8655-09-13085. The authors would like to thank Philip Chamberlin for providing the EVE temperature light curve routine and Harry Warren for providing the NRL-EVE DEM routines. CHIANTI is a collaborative project involving George Mason University, the University of Michigan (USA) and the University of Cambridge (UK). This research has made use of NASA's Astrophysics Data System. NR 31 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR UNSP 84 DI 10.1088/0004-637X/779/1/84 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100084 ER PT J AU Milne, PA Brown, PJ Roming, PWA Bufano, F Gehrels, N AF Milne, Peter A. Brown, Peter J. Roming, Peter W. A. Bufano, Filomena Gehrels, Neil TI GROUPING NORMAL TYPE Ia SUPERNOVAE BY UV TO OPTICAL COLOR DIFFERENCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: distances and redshifts; supernovae: general; ultraviolet: general ID SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; ULTRA-VIOLET/OPTICAL TELESCOPE; HUBBLE-SPACE-TELESCOPE; LIGHT-CURVE SHAPES; LOW-REDSHIFT; SN 2011FE; ABSOLUTE MAGNITUDES; K-CORRECTIONS; SPECTRA; DIVERSITY AB Observations of many Type Ia supernovae (SNe Ia) for multiple epochs per object with the Swift Ultraviolet Optical Telescope instrument have revealed that there exists order to the differences in the UV-optical colors of optically normal supernovae (SNe). We examine UV-optical color curves for 23 SNe Ia, dividing the SNe into four groups, and find that roughly one-third of "NUV-blue" SNe Ia have bluer UV-optical colors than the larger "NUV-red" group. Two minor groups are recognized, "MUV-blue" and "irregular" SNe Ia. While we conclude that the latter group is a subset of the NUV-red group, containing the SNe with the broadest optical peaks, we conclude that the "MUV-blue" group is a distinct group. Separating into the groups and accounting for the time evolution of the UV-optical colors lowers the scatter in two NUV-optical colors (e. g., u-v and uvw1-v) to the level of the scatter in b-v. This finding is promising for extending the cosmological utilization of SNe Ia into the NUV. We generate spectrophotometry of 33 SNe Ia and determine the correct grouping for each. We argue that there is a fundamental spectral difference in the 2900-3500 angstrom wavelength range, a region suggested to be dominated by absorption from iron-peak elements. The NUV-blue SNe Ia feature less absorption than the NUV-red SNe Ia. We show that all NUV-blue SNe Ia in this sample also show evidence of unburned carbon in optical spectra, whereas only one NUV-red SN Ia features that absorption line. Every NUV-blue event also exhibits a low gradient of the Si II lambda 6355 absorption feature. Many NUV-red events also exhibit a low gradient, perhaps suggestive that NUV-blue events are a subset of the larger low-velocity gradient group. C1 [Milne, Peter A.] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA. [Brown, Peter J.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Roming, Peter W. A.] Southwest Res Corp, Space Sci & Engn Div, San Antonio, TX 78228 USA. [Bufano, Filomena] Univ Andres Bello, Dept Cincias Fis, Santiago, Chile. [Gehrels, Neil] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Milne, PA (reprint author), Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85719 USA. EM pbrown@physics.tamu.edu FU NASA ADAP [NNX10AD58G]; FONDECYT [2130227] FX P. A. M. acknowledges support from NASA ADAP grant NNX10AD58G. F. B. acknowledges support from FONDECYT through Postdoctoral grant 2130227. P. A. M thanks R. Foley, K. Maguire, J. Cooke, X, Wang, J. Silverman, M. Ganeshlingham, R. C. Thomas, J. Parrent, and H. Marion for assistance accessing spectral and photometric datasets critical for characterizing each supernova. P. A. M. thanks P. Mazzali for text relating to line-blocking and line-blanketing effects, and R. Foley and J. Silverman for discussions of interpretation of non-UVOT datasets. All supernova observers thank the mission operations team at Penn State for scheduling the thousands of individual UVOT target-of-opportunity observations that comprise this dataset. The NASA/IPAC Extragalactic Database (NED) was utilized in this work. NED is operated by the Jet Propulsion Laboratory of the California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 72 TC 20 Z9 20 U1 2 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR 23 DI 10.1088/0004-637X/779/1/23 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100023 ER PT J AU Nieves-Chinchilla, T Vourlidas, A Stenborg, G Savani, NP Koval, A Szabo, A Jian, LK AF Nieves-Chinchilla, T. Vourlidas, A. Stenborg, G. Savani, N. P. Koval, A. Szabo, A. Jian, L. K. TI INNER HELIOSPHERIC EVOLUTION OF A "STEALTH" CME DERIVED FROM MULTI-VIEW IMAGING AND MULTIPOINT IN SITU OBSERVATIONS. I. PROPAGATION TO 1 AU SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar-terrestrial relations; solar wind; Sun: coronal mass ejections (CMEs) ID CORONAL MASS EJECTION; RANKINE-HUGONIOT PROBLEM; SOLAR-WIND; MAGNETIC CLOUD; STEREO; EARTH; SHOCK; MORPHOLOGY; MISSION; INSTRUMENT AB Coronal mass ejections (CMEs) are the main driver of space weather. Therefore, a precise forecasting of their likely geo-effectiveness relies on an accurate tracking of their morphological and kinematical evolution throughout the interplanetary medium. However, single viewpoint observations require many assumptions to model the development of the features of CMEs. The most common hypotheses were those of radial propagation and self-similar expansion. The use of different viewpoints shows that, at least for some cases, those assumptions are no longer valid. From radial propagation, typical attributes that can now be confirmed to exist are over-expansion and/or rotation along the propagation axis. Understanding the 3D development and evolution of the CME features will help to establish the connection between remote and in situ observations, and hence help forecast space weather. We present an analysis of the morphological and kinematical evolution of a STEREO-B-directed CME on 2009 August 25-27. By means of a comprehensive analysis of remote imaging observations provided by the SOHO, STEREO, and SDO missions, and in situ measurements recorded by Wind, ACE, and MESSENGER, we prove in this paper that the event exhibits signatures of deflection, which are usually associated with changes in the direction of propagation and/or also with rotation. The interaction with other magnetic obstacles could act as a catalyst of deflection or rotation effects. We also propose a method to investigate the change of the CME tilt from the analysis of height-time direct measurements. If this method is validated in further work, it may have important implications for space weather studies because it will allow for inference of the interplanetary counterpart of the CME's orientation. C1 [Nieves-Chinchilla, T.] Catholic Univ Amer, Washington, DC 20064 USA. [Nieves-Chinchilla, T.; Savani, N. P.; Koval, A.; Szabo, A.; Jian, L. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Vourlidas, A.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Stenborg, G.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Savani, N. P.] UCAR, Boulder, CO 80307 USA. [Koval, A.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. [Jian, L. K.] Univ Maryland, College Pk, MD 20742 USA. RP Nieves-Chinchilla, T (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. EM Teresa.Nieves@nasa.gov RI Savani, Neel/G-4066-2014; Vourlidas, Angelos/C-8231-2009; Jian, Lan/B-4053-2010; Nieves-Chinchilla, Teresa/F-3482-2016 OI Savani, Neel/0000-0002-1916-7877; Vourlidas, Angelos/0000-0002-8164-5948; Jian, Lan/0000-0002-6849-5527; Nieves-Chinchilla, Teresa/0000-0003-0565-4890 FU NASA SECCHI; NASA [NNX11AD40G]; NASA's Science Directorate as part of the STEREO project, including the IMPACT investigation FX Drs. Nieves-Chinchilla, Vourlidas, and Stenborg are supported by the NASA SECCHI contract to NRL. The work of G. S. was also partly funded by NASA contract NNX11AD40G. The STEREO/SECCHI data used for this study are prepared by an international consortium of NASA Goddard Space Flight Center (USA), Lockheed Martin Solar and Astrophysics Lab (USA), Naval Research Laboratory USA), Rutherford Appleton Laboratory (UK), University of Birmingham (UK), Max-Planck-Institut fur Sonnensystemforschung (Germany), Institut d'Optique Theorique et Appliquee (France), Institut d'Astrophysique Spatiale (France), and Centre Spatiale de Liege (Belgium). Dr. L. K. Jian's work is funded by NASA's Science Directorate as part of the STEREO project, including the IMPACT investigation. NR 52 TC 10 Z9 10 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR 55 DI 10.1088/0004-637X/779/1/55 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100055 ER PT J AU Phillips, MM Simon, JD Morrell, N Burns, CR Cox, NLJ Foley, RJ Karakas, AI Patat, F Sternberg, A Williams, RE Gal-Yam, A Hsiao, EY Leonard, DC Persson, SE Stritzinger, M Thompson, IB Campillay, A Contreras, C Folatelli, G Freedman, WL Hamuy, M Roth, M Shields, GA Suntzeff, NB Chomiuk, L Ivans, II Madore, BF Penprase, BE Perley, D Pignata, G Preston, G Soderberg, AM AF Phillips, M. M. Simon, Joshua D. Morrell, Nidia Burns, Christopher R. Cox, Nick L. J. Foley, Ryan J. Karakas, Amanda I. Patat, F. Sternberg, A. Williams, R. E. Gal-Yam, A. Hsiao, E. Y. Leonard, D. C. Persson, Sven E. Stritzinger, Maximilian Thompson, I. B. Campillay, Abdo Contreras, Carlos Folatelli, Gaston Freedman, Wendy L. Hamuy, Mario Roth, Miguel Shields, Gregory A. Suntzeff, Nicholas B. Chomiuk, Laura Ivans, Inese I. Madore, Barry F. Penprase, B. E. Perley, Daniel Pignata, G. Preston, G. Soderberg, Alicia M. TI ON THE SOURCE OF THE DUST EXTINCTION IN TYPE Ia SUPERNOVAE AND THE DISCOVERY OF ANOMALOUSLY STRONG Na I ABSORPTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; dust, extinction; galaxies: ISM; supernovae: general ID DIFFUSE INTERSTELLAR BANDS; GIANT BRANCH STARS; PHOTOMETRY DATA RELEASE; SMALL-MAGELLANIC-CLOUD; CIRCUMSTELLAR MATERIAL; CA-II; INFRARED PHOTOMETRY; SODIUM-ABSORPTION; LIGHT CURVES; SN 2011FE AB High-dispersion observations of the Na I D lambda lambda 5890, 5896 and K I lambda lambda 7665, 7699 interstellar lines, and the diffuse interstellar band at 5780 angstrom in the spectra of 32 Type Ia supernovae are used as an independent means of probing dust extinction. We show that the dust extinction of the objects where the diffuse interstellar band at 5780 angstrom is detected is consistent with the visual extinction derived from the supernova colors. This strongly suggests that the dust producing the extinction is predominantly located in the interstellar medium of the host galaxies and not in circumstellar material associated with the progenitor system. One quarter of the supernovae display anomalously large Na I column densities in comparison to the amount of dust extinction derived from their colors. Remarkably, all of the cases of unusually strong Na I D absorption correspond to "Blueshifted" profiles in the classification scheme of Sternberg et al. This coincidence suggests that outflowing circumstellar gas is responsible for at least some of the cases of anomalously large Na I column densities. Two supernovae with unusually strong Na I D absorption showed essentially normal K I column densities for the dust extinction implied by their colors, but this does not appear to be a universal characteristic. Overall, we find the most accurate predictor of individual supernova extinction to be the equivalent width of the diffuse interstellar band at 5780 angstrom, and provide an empirical relation for its use. Finally, we identify ways of producing significant enhancements of the Na abundance of circumstellar material in both the single-degenerate and double-degenerate scenarios for the progenitor system. C1 [Phillips, M. M.; Morrell, Nidia; Hsiao, E. Y.; Campillay, Abdo; Contreras, Carlos; Roth, Miguel] Carnegie Observ, Campanas Observ, La Serena, Chile. [Simon, Joshua D.; Burns, Christopher R.; Persson, Sven E.; Thompson, I. B.; Freedman, Wendy L.; Madore, Barry F.; Preston, G.] Carnegie Inst Sci, Observ, Pasadena, CA 91101 USA. [Cox, Nick L. J.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Foley, Ryan J.; Chomiuk, Laura; Soderberg, Alicia M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Karakas, Amanda I.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Patat, F.] ESO, D-85748 Garching, Germany. [Sternberg, A.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Williams, R. E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gal-Yam, A.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, Fac Phys, IL-76100 Rehovot, Israel. [Leonard, D. C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Stritzinger, Maximilian] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus, Denmark. [Folatelli, Gaston] Univ Tokyo, Kavli Inst Phys & Math Univ, Todai Inst Adv Study, Kashiwa, Chiba 2778583, Japan. [Hamuy, Mario] Univ Chile, Dept Astron, Santiago, Chile. [Shields, Gregory A.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Suntzeff, Nicholas B.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA. [Ivans, Inese I.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Madore, Barry F.] CALTECH, Jet Prop Lab, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Penprase, B. E.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA. [Perley, Daniel] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Pignata, G.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. RP Phillips, MM (reprint author), Carnegie Observ, Campanas Observ, Casilla 601, La Serena, Chile. EM mmp@lco.cl RI Hamuy, Mario/G-7541-2016; OI Patat, Ferdinando/0000-0002-0537-3573; stritzinger, maximilian/0000-0002-5571-1833 FU National Science Foundation [AST0306969, AST0607438, AST1008343]; NSF [1066293]; Australian Research Council [FT110100475]; EU/FP7 via an ERC grant; Kimmel Award for innovative Investigation; Danish Agency for Science and Technology and Innovation; Millennium Center for Supernova Science [P10-064-F]; Ahmanson Foundation FX The work of the CSP has been supported by the National Science Foundation under grants AST0306969, AST0607438, and AST1008343. M.M.P. gratefully acknowledges the Aspen Center for Physics and NSF grant 1066293 for hospitality during the conception of this work. M.M.P. also thanks Brandon Lawton, Andy McWilliam, and Sebastian Lopez for helpful discussions, and the Australian Astronomical Observatory and the ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) for hosting and supporting a three month research leave during which this paper was completed. A.I.K. is grateful for support from the Australian Research Council for a Future Fellowship (FT110100475). A.G. was supported by the EU/FP7 via an ERC grant, a Minerva ARCHES prize, and the Kimmel Award for innovative Investigation. M.S. acknowledges generous support provided by the Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant. M.H. and G.P. are grateful for support from Millennium Center for Supernova Science (P10-064-F), with input from Fondo de Innovacion para la Competitividad, del Ministerio de Economia, Fomento y Turismo de Chile. Computing resources used for this work were made possible by a grant from the Ahmanson Foundation. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 132 TC 59 Z9 60 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR 38 DI 10.1088/0004-637X/779/1/38 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100038 ER PT J AU Story, KT Reichardt, CL Hou, Z Keisler, R Aird, KA Benson, BA Bleem, LE Carlstrom, JE Chang, CL Cho, HM Crawford, TM Crites, AT de Haan, T Dobbs, MA Dudley, J Follin, B George, EM Halverson, NW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Joy, M Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D McMahon, JJ Mehl, J Meyer, SS Millea, M Mohr, JJ Montroy, TE Padin, S Plagge, T Pryke, C Ruhl, JE Sayre, JT Schaffer, KK Shaw, L Shirokoff, E Spieler, HG Staniszewski, Z Stark, AA van Engelen, A Vanderlinde, K Vieira, JD Williamson, R Zahn, O AF Story, K. T. Reichardt, C. L. Hou, Z. Keisler, R. Aird, K. A. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Cho, H. -M. Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. Dudley, J. Follin, B. George, E. M. Halverson, N. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Joy, M. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. McMahon, J. J. Mehl, J. Meyer, S. S. Millea, M. Mohr, J. J. Montroy, T. E. Padin, S. Plagge, T. Pryke, C. Ruhl, J. E. Sayre, J. T. Schaffer, K. K. Shaw, L. Shirokoff, E. Spieler, H. G. Staniszewski, Z. Stark, A. A. van Engelen, A. Vanderlinde, K. Vieira, J. D. Williamson, R. Zahn, O. TI MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND DAMPING TAIL FROM THE 2500-SQUARE-DEGREE SPT-SZ SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; large-scale structure of universe ID SOUTH-POLE TELESCOPE; ATACAMA COSMOLOGY TELESCOPE; BARYON ACOUSTIC-OSCILLATIONS; INFLATIONARY UNIVERSE SCENARIO; DIGITAL SKY SURVEY; POWER SPECTRUM; GALAXY CLUSTERS; SYMMETRY-BREAKING; DARK ENERGY; 148 GHZ AB We present a measurement of the cosmic microwave background (CMB) temperature power spectrum using data from the recently completed South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) survey. This measurement is made from observations of 2540 deg(2) of sky with arcminute resolution at 150 GHz, and improves upon previous measurements using the SPT by tripling the sky area. We report CMB temperature anisotropy power over the multipole range 650 < l < 3000. We fit the SPT bandpowers, combined with the 7 yr Wilkinson Microwave Anisotropy Probe (WMAP7) data, with a six-parameter Lambda CDM cosmological model and find that the two datasets are consistent and well fit by the model. Adding SPT measurements significantly improves Lambda CDM parameter constraints; in particular, the constraint on theta(s) tightens by a factor of 2.7. The impact of gravitational lensing is detected at 8.1 sigma, the most significant detection to date. This sensitivity of the SPT+WMAP7 data to lensing by large-scale structure at low redshifts allows us to constrain the mean curvature of the observable universe with CMB data alone to be Omega(k) = -0.003(-0.018)(+0.014). Using the SPT+ WMAP7 data, we measure the spectral index of scalar fluctuations to be n(s) = 0.9623 +/- 0.0097 in the Lambda CDM model, a 3.9 sigma preference for a scale-dependent spectrum with n(s) < 1. The SPT measurement of the CMB damping tail helps break the degeneracy that exists between the tensor-to-scalar ratio r and ns in large-scale CMB measurements, leading to an upper limit of r < 0.18 (95% C. L.) in the Lambda CDM+r model. Adding low-redshift measurements of the Hubble constant (H-0) and the baryon acoustic oscillation (BAO) feature to the SPT+ WMAP7 data leads to further improvements. The combination of SPT+WMAP7+H-0+BAO constrains n(s) = 0.9538 +/- 0.0081 in the Lambda CDM model, a 5.7 sigma detection of n(s) < 1, and places an upper limit of r < 0.11 (95% C. L.) in the Lambda CDM+r model. These new constraints on ns and r have significant implications for our understanding of inflation, which we discuss in the context of selected single-field inflation models. C1 [Story, K. T.; Keisler, R.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Hoover, S.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Schaffer, K. K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Story, K. T.; Keisler, R.; Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Meyer, S. S.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Reichardt, C. L.; George, E. M.; Holzapfel, W. L.; Lee, A. T.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Hou, Z.; Follin, B.; Knox, L.; Millea, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.; Mehl, J.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H. -M.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [de Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P.; Shaw, L.; van Engelen, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP Story, KT (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM kstory@uchicago.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937]; NSF [PHY-1125897, 0709498]; Kavli Foundation; Gordon and Betty Moore Foundation; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; NASA Hubble Fellowship [HF-51275.01]; KICP Fellowship; Alfred P. Sloan Research Fellowship; BCCP fellowship; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; Open Science Grid, NSF [NSF PHY 1148698]; NASA Office of Space Science; [AST-1009012] FX We thank Scott Dodelson, John Peacock, David Baumann, and Antonio Riotto for useful conversations. The SPT is supported by the National Science Foundation through grant ANT-0638937, with partial support provided by NSF grant PHY-1125897, the Kavli Foundation, and the Gordon and Betty Moore Foundation. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. Work at Harvard is supported by grant AST-1009012. R. Keisler acknowledges support from NASA Hubble Fellowship grant HF-51275.01, B. A. Benson a KICP Fellowship, M. Dobbs an Alfred P. Sloan Research Fellowship, O. Zahn a BCCP fellowship, M. Millea and L. Knox a NSF grant 0709498. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under contract No. DE-AC02-05CH11231, and the resources of the University of Chicago Computing Cooperative (UC3), supported in part by the Open Science Grid, NSF grant NSF PHY 1148698. Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) package. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. NR 79 TC 133 Z9 133 U1 2 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR 86 DI 10.1088/0004-637X/779/1/86 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100086 ER PT J AU Sultana, J Kazanas, D Mastichiadis, A AF Sultana, J. Kazanas, D. Mastichiadis, A. TI THE SUPERCRITICAL PILE GAMMA-RAY BURST MODEL: THE GRB AFTERGLOW STEEP DECLINE AND PLATEAU PHASE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; gamma-ray burst: general ID 28 FEBRUARY 1997; SWIFT XRT DATA; F-NU PEAK; FERMI OBSERVATIONS; LIGHT CURVES; SPECTRAL CATALOG; MAGNETIC-FIELD; EMISSION; COMPONENT; PROMPT AB We present a process that accounts for the steep decline and plateau phase of the Swift X-Ray Telescope (XRT) light curves, vexing features of gamma-ray burst (GRB) phenomenology. This process is an integral part of the "supercritical pile" GRB model, proposed a few years ago to account for the conversion of the GRB kinetic energy into radiation with a spectral peak at E-pk similar to m(e)c(2). We compute the evolution of the relativistic blast wave (RBW) Lorentz factor G to show that the radiation-reaction force due to the GRB emission can produce an abrupt, small (similar to 25%) decrease in G at a radius that is smaller (depending on conditions) than the deceleration radius R-D. Because of this reduction, the kinematic criticality criterion of the "supercritical pile" is no longer fulfilled. Transfer of the proton energy into electrons ceases and the GRB enters abruptly the afterglow phase at a luminosity smaller by similar to m(p)/m(e) than that of the prompt emission. If the radius at which this slow-down occurs is significantly smaller than R-D, the RBW internal energy continues to drive the RBW expansion at a constant (new) G and its X-ray luminosity remains constant until R-D is reached, at which point it resumes its more conventional decay, thereby completing the "unexpected" XRT light curve phase. If this transition occurs at R similar or equal to R-D, the steep decline is followed by a flux decrease instead of a "plateau," consistent with the conventional afterglow declines. Besides providing an account of these peculiarities, the model suggests that the afterglow phase may in fact begin before the RBW reaches R similar or equal to R-D, thus providing novel insights into GRB phenomenology. C1 [Sultana, J.] Univ Malta, Fac Sci, Dept Math, MSD-2080 Msida, Malta. [Kazanas, D.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mastichiadis, A.] Univ Athens, Dept Phys, GR-15783 Zografos, Greece. RP Sultana, J (reprint author), Univ Malta, Fac Sci, Dept Math, MSD-2080 Msida, Malta. EM joseph.sultana@um.edu.mt FU University of Malta; Swift grant; Fermi GO grant FX We thank the anonymous referee for incisive, constructive comments that have added to the completeness of this work. J.S. gratefully acknowledges financial support from the University of Malta during his visit at the NASA-GSFC and the hospitality of the Astrophysics Science Division of the GSFC. D. K. acknowledges support from Swift and Fermi GO grants. NR 52 TC 5 Z9 5 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR UNSP 16 DI 10.1088/0004-637X/779/1/16 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100016 ER PT J AU Tripathi, D Klimchuk, JA AF Tripathi, Durgesh Klimchuk, James A. TI ASYMMETRIES IN CORONAL SPECTRAL LINES AND EMISSION MEASURE DISTRIBUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: atmosphere; Sun: corona; Sun: transition region; Sun: UV radiation ID EUV IMAGING SPECTROMETER; SOLAR ACTIVE-REGION; SPECTROSCOPIC OBSERVATIONS; TRANSITION REGION; PROFILE ASYMMETRIES; OUTFLOWS; HINODE; PLASMA; LOOPS; WIND AB It has previously been argued that (1) spicules do not provide enough pre-heated plasma to fill the corona, and (2) even if they did, additional heating would be required to keep the plasma hot as it expands upward. Here we address whether spicules play an important role by injecting plasma at cooler temperatures (<2 MK), which then gets heated to coronal values at higher altitudes. We measure red-blue asymmetries in line profiles formed over a wide range of temperatures in the bright moss areas of two active regions. We derive emission measure distributions from the excess wing emission. We find that the asymmetries and emission measures are small and conclude that spicules do not inject an important (dominant) mass flux into the cores of active regions at temperatures >0.6 MK (logT > 5.8). These conclusions apply not only to spicules but also to any process that suddenly heats and accelerates chromospheric plasma (e. g., a chromospheric nanoflare). The traditional picture of coronal heating and chromospheric evaporation appears to remain the most likely explanation of the active region corona. C1 [Tripathi, Durgesh] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Klimchuk, James A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tripathi, D (reprint author), Interuniv Ctr Astron & Astrophys, Post Bag 4, Pune 411007, Maharashtra, India. RI Tripathi, Durgesh/D-9390-2012; Klimchuk, James/D-1041-2012 OI Tripathi, Durgesh/0000-0003-1689-6254; Klimchuk, James/0000-0003-2255-0305 FU NASA FX Hinode is a Japanese mission developed and launched by ISAS/JAXA, collaborating with NAOJ as a domestic partner, and NASA and STFC (UK) as international partners. The scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/JAXA. This team mainly consists of scientists from institutes in the partner countries. Support for the post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK), NASA, ESA, and NSC (Norway). CHIANTI is a collaborative project involving researchers at NRL (USA) RAL (UK), and the Universities of Cambridge (UK), George Mason (USA), and Florence (Italy). The work of J.A.K. was supported by the NASA Supporting Research and Technology Program. The authors benefited from participation in the International Space Science Institute team led by S. Bradshaw and H. Mason. The authors also thank H. Mason, P. R. Young, and Srividya Subramanian for various discussions. NR 26 TC 12 Z9 12 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR 779 DI 10.1088/0004-637X/779/1/1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100001 ER PT J AU Tsai, CW Jarrett, TH Stern, D Emonts, B Barrows, RS Assef, RJ Norris, RP Eisenhardt, PRM Lonsdale, C Blain, AW Benford, DJ Wu, JW Stalder, B Stubbs, CW High, FW Li, KL Kong, AKH AF Tsai, Chao-Wei Jarrett, T. H. Stern, Daniel Emonts, Bjorn Barrows, R. Scott Assef, Roberto J. Norris, Ray P. Eisenhardt, Peter R. M. Lonsdale, Carol Blain, Andrew W. Benford, Dominic J. Wu, Jingwen Stalder, Brian Stubbs, Christopher W. High, F. William Li, K. L. Kong, Albert K. H. TI WISE J233237.05-505643.5: A DOUBLE-PEAKED, BROAD-LINED ACTIVE GALACTIC NUCLEUS WITH A SPIRAL-SHAPED RADIO MORPHOLOGY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual: WISE J233237.05-505643.5; galaxies: interactions; galaxies: jets; galaxies: nuclei; radio continuum: galaxies ID BINARY BLACK-HOLE; SOUTH-POLE TELESCOPE; INFRARED EXTRAGALACTIC FIELD; SURVEY SPECTROSCOPIC SAMPLE; ELLIPTIC ACCRETION DISKS; TERM PROFILE VARIABILITY; GALAXY 3C 66B; EMISSION-LINES; SKY SURVEY; SUPERMASSIVE BINARY AB We present radio continuum mapping, optical imaging, and spectroscopy of the newly discovered double-peaked, broad-lined active galactic nucleus (AGN) WISE J233237.05-505643.5 at redshift z = 0.3447. This source exhibits an FR-I and FR-II hybrid morphology, characterized by a bright core, jet, and Doppler-boosted lobe structures in Australian Telescope Compact Array continuum maps at 1.5, 5.6, and 9 GHz. Unlike most FR-II objects, W2332-5056 is hosted by a disk-like galaxy. The core has a projected 5 '' linear radio feature that is perpendicular to the curved primary jet, hinting at unusual and complex activity within the inner 25 kpc. The multi-epoch, optical-near-IR photometric measurements indicate significant variability over a 3-20 yr baseline from the AGN component. Gemini South optical data show unusual double-peaked emission-line features: the centroids of the broad-lined components of H alpha and H beta are blueshifted with respect to the narrow lines and host galaxy by similar to 3800 km s(-1). We examine possible cases that involve single or double supermassive black holes in the system and discuss the required future investigations to disentangle the mysterious nature of this system. C1 [Tsai, Chao-Wei] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Tsai, Chao-Wei; Stern, Daniel; Assef, Roberto J.; Eisenhardt, Peter R. M.; Wu, Jingwen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jarrett, T. H.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Emonts, Bjorn] Ctr Astrobiol INTA CSIC, E-28850 Madrid, Spain. [Emonts, Bjorn; Norris, Ray P.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Barrows, R. Scott] Univ Arkansas, Arkansas Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA. [Assef, Roberto J.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. [Lonsdale, Carol] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Blain, Andrew W.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Benford, Dominic J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stalder, Brian; Stubbs, Christopher W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [High, F. William] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Li, K. L.; Kong, Albert K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Li, K. L.; Kong, Albert K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. RP Tsai, CW (reprint author), CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. EM Chao-Wei.Tsai@jpl.nasa.gov RI Norris, Ray/A-1316-2008; Stubbs, Christopher/C-2829-2012; Benford, Dominic/D-4760-2012 OI Norris, Ray/0000-0002-4597-1906; Stubbs, Christopher/0000-0003-0347-1724; Benford, Dominic/0000-0002-9884-4206 FU Gemini-CONICYT [32120009]; National Aeronautics and Space Administration; Commonwealth of Australia FX The authors thank the anonymous referee for the constructive comments and inspiring suggestions throughout the whole paper. We acknowledge Joaquin Vieira for verifying the W2332-5056 non-detection in the SPT survey map. We thank Roger Deane for sharing his VLBI work prior to the publication. We also appreciate the comments and suggestions by Colin Lonsdale and the discussions with Michael Eracleous and Laura Blecha in the "Binary Black Holes and Dual AGN" meeting in Tucson in 2012. R.J.A. was supported in part by Gemini-CONICYT grant number 32120009. R.J.A. was also supported in part by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. This publication makes use of data products from WISE, which is a joint project of the University of California, Los Angeles and the Jet Propulsion Laboratory, California Institute of Technology, funded by the National Aeronautics and Space Administration. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministrio da Cincia, Tecnologia e Inovao (Brazil) and Ministerio de Ciencia, Tecnologa e Innovacin Productiva (Argentina). The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 126 TC 3 Z9 3 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR 41 DI 10.1088/0004-637X/779/1/41 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100041 ER PT J AU Viero, MP Moncelsi, L Quadri, RF Arumugam, V Assef, RJ Bethermin, M Bock, J Bridge, C Casey, CM Conley, A Cooray, A Farrah, D Glenn, J Heinis, S Ibar, E Ikarashi, S Ivison, RJ Kohno, K Marsden, G Oliver, SJ Roseboom, IG Schulz, B Scott, D Serra, P Vaccari, M Vieira, JD Wang, L Wardlow, J Wilson, GW Yun, MS Zemcov, M AF Viero, M. P. Moncelsi, L. Quadri, R. F. Arumugam, V. Assef, R. J. Bethermin, M. Bock, J. Bridge, C. Casey, C. M. Conley, A. Cooray, A. Farrah, D. Glenn, J. Heinis, S. Ibar, E. Ikarashi, S. Ivison, R. J. Kohno, K. Marsden, G. Oliver, S. J. Roseboom, I. G. Schulz, B. Scott, D. Serra, P. Vaccari, M. Vieira, J. D. Wang, L. Wardlow, J. Wilson, G. W. Yun, M. S. Zemcov, M. TI HerMES: THE CONTRIBUTION TO THE COSMIC INFRARED BACKGROUND FROM GALAXIES SELECTED BY MASS AND REDSHIFT SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; infrared: galaxies; large-scale structure of universe; submillimeter: galaxies ID STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; SIMILAR-TO 2; SPECTRAL ENERGY-DISTRIBUTIONS; MULTIBAND IMAGING PHOTOMETER; DEEP-FIELD-SOUTH; HUBBLE-SPACE-TELESCOPE; GOODS NICMOS SURVEY; 160 MU-M; APERTURE-SUBMILLIMETER-TELESCOPE AB We quantify the fraction of the cosmic infrared background (CIB) that originates from galaxies identified in the UV/optical/near-infrared by stacking 81,250 (similar to 35.7 arcmin(-2)) K-selected sources (K-AB < 24.0) split according to their rest-frame U-V versus V-J colors into 72,216 star-forming and 9034 quiescent galaxies, on maps from Spitzer/MIPS (24 mu m), Herschel/PACS (100, 160 mu m), Herschel/SPIRE (250, 350, 500 mu m), and AzTEC (1100 mu m). The fraction of the CIB resolved by our catalog is (69% +/- 15%) at 24 mu m, (78% +/- 17%) at 70 mu m, (58% +/- 13%) at 100 mu m, (78% +/- 18%) at 160 mu m, (80% +/- 17%) at 250 mu m, (69% +/- 14%) at 350 mu m, (65% +/- 12%) at 500 mu m, and (45% +/- 8%) at 1100 mu m. Of that total, about 95% originates from star-forming galaxies, while the remaining 5% is from apparently quiescent galaxies. The CIB at lambda less than or similar to 200 mu m appears to be sourced predominantly from galaxies at z less than or similar to 1, while at. greater than or similar to 200 mu m the bulk originates from 1 less than or similar to z less than or similar to 2. Galaxies with stellar masses log(M/M-circle dot) = 9.5-11 are responsible for the majority of the CIB, with those in the log(M/M-circle dot) = 9.5-10 bin contributing mostly at lambda < 250 mu m, and those in the log(M/M circle dot) = 10-11 bin dominating at lambda > 350 mu m. The contribution from galaxies in the log(M/M-circle dot) = 9.0-9.5 (lowest) and log(M/M-circle dot) = 11.0-12.0 (highest) stellar-mass bins contribute the least-both of order 5%-although the highest stellar-mass bin is a significant contributor to the luminosity density at z greater than or similar to 2. The luminosities of the galaxies responsible for the CIB shifts from combinations of "normal" and luminous infrared galaxies (LIRGs) at lambda less than or similar to 160 mu m, to LIRGs at 160 less than or similar to lambda less than or similar to 500 mu m, to finally LIRGs and ultra-luminous infrared galaxies at lambda greater than or similar to 500 mu m. Stacking analyses were performed using SIMSTACK, a novel algorithm designed to account for possible biases in the stacked flux density due to clustering. It is made available to the public at www.astro.caltech.edu/similar to viero/viero_homepage/toolbox.html. C1 [Viero, M. P.; Moncelsi, L.; Bridge, C.; Cooray, A.; Schulz, B.; Vieira, J. D.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Quadri, R. F.] Carnegie Observ, Pasadena, CA 91101 USA. [Arumugam, V.; Ivison, R. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Bock, J.; Zemcov, M.] Jet Prop Lab, Pasadena, CA 91109 USA. [Bethermin, M.] Univ Paris Diderot, CEA DSM Irfu CNRS, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Bethermin, M.; Serra, P.] Univ Paris 11, Inst dAstrophys Spatiale IAS, F-91405 Orsay, France. [Bethermin, M.; Serra, P.] CNRS, UMR 8617, Inst dAstrophys Spatiale IAS, F-91405 Orsay, France. [Casey, C. M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Conley, A.; Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Cooray, A.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Heinis, S.] Univ dAix Marseille, Lab dAstrophys Marseille LAM, F-13388 Marseille, France. [Heinis, S.] CNRS, Lab dAstrophys Marseille LAM, F-13388 Marseille, France. [Ibar, E.] Pontificia Univ Catolica Chile, Dept Astron & Astrophys, Santiago 22, Chile. [Ibar, E.; Ivison, R. J.] UK Astron Technol Ctr, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ikarashi, S.; Kohno, K.] Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Kohno, K.] Univ Tokyo, Res Ctr Early Univ, Tokyo 1130033, Japan. [Marsden, G.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T IZ1, Canada. [Oliver, S. J.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Schulz, B.] CALTECH, Infrared Proc & Anal Ctr, JPL, Pasadena, CA 91125 USA. [Vaccari, M.] Univ Western Cape, Astrophys Grp, Dept Phys, ZA-7535 Bellville, Cape Town, South Africa. [Wang, L.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Wilson, G. W.; Yun, M. S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Univ Diego Port, Nucl Astron Fac Ingenieria, Santiago 441, Chile. RP Viero, MP (reprint author), CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA. EM marco.viero@caltech.edu RI Serra, Paolo/G-9678-2014; Wardlow, Julie/C-9903-2015; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; OI Serra, Paolo/0000-0002-7609-3931; Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Casey, Caitlin/0000-0002-0930-6466; Scott, Douglas/0000-0002-6878-9840; Bethermin, Matthieu/0000-0002-3915-2015 FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA) FX The authors warmly thank Duncan Hanson, Phil Korngut, Zak Staniszewski, and Yoshihiro Ueda. We also thank the anonymous referee, whose careful comments greatly improved this paper. Much credit belongs to C. Barth Netterfield and Enzo Pascale for inspiring the simultaneous stacking algorithm, and to whom we are thankful. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). NR 188 TC 41 Z9 41 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR UNSP 32 DI 10.1088/0004-637X/779/1/32 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100032 ER PT J AU Zhu, L Zhao, JH Wright, MCH Sandell, G Shi, H Wu, YF Brogan, C Corder, S AF Zhu, Lei Zhao, Jun-Hui Wright, M. C. H. Sandell, Goeran Shi, Hui Wu, Yue-Fang Brogan, Crystal Corder, Stuartt TI SUBARCSECOND OBSERVATIONS OF NGC 7538 IRS 1: CONTINUUM DISTRIBUTION AND DYNAMICS OF MOLECULAR GAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II regions; ISM: jets and outflows; ISM: kinematics and dynamics; ISM: molecules; radio lines: ISM; stars: formation ID STAR-FORMING REGIONS; NGC-7538 IRS-1; RECOMBINATION LINE; CIRCUMSTELLAR DISK; STELLAR PARAMETERS; METHANOL MASERS; HII-REGIONS; RESOLUTION; OUTFLOWS; GHZ AB We report new results based on the analysis of the Submillimeter Array (SMA) and Combined Array for Research in Millimeter-wave Astronomy (CARMA) observations of NGC 7538 IRS 1 at 1.3 and 3.4 mm with subarcsecond resolutions. With angular resolutions similar to 0.'' 7, the SMA and CARMA observations show that the continuum emission at 1.3 and 3.4 mm from the hyper-compact H II region IRS 1 is dominated by a compact source with a tail-like extended structure to the southwest of IRS 1. With a CARMA B-array image at 1.3 mm convolved to 0.'' 1, we resolve the hyper-compact H II region into two components: an unresolved hyper-compact core, and a north-south extension with linear sizes of <270 AU and similar to 2000 AU, respectively. The fine structure observed with CARMA is in good agreement with the previous Very Large Array results at centimeter wavelengths, suggesting that the hyper-compact H II region at the center of IRS 1 is associated with an ionized bipolar outflow. We image the molecular lines OCS(19-18) and CH3CN(12-11) as well as (CO)-C-13(2-1) surrounding IRS 1, showing a velocity gradient along the southwest-northeast direction. The spectral line profiles in (CO)-C-13(2-1), CO(2-1), and HCN(1-0) observed toward IRS 1 show broad redshifted absorption, providing evidence for gas infall with rates in the range of 3-10 x 10(-3) M-circle dot yr(-1) inferred from our observations. C1 [Zhu, Lei; Shi, Hui] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Zhu, Lei; Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zhu, Lei; Wu, Yue-Fang] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Wright, M. C. H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Sandell, Goeran] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Shi, Hui] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Brogan, Crystal; Corder, Stuartt] NRAO, Charlottesville, VA 22903 USA. RP Zhu, L (reprint author), Chinese Acad Sci, Natl Astron Observ, A20 Datun Rd, Beijing 100012, Peoples R China. EM lzhu@nao.cas.cn FU National Basic Research Program of China (973 program) [2012CB821802] FX L.Z. is supported by National Basic Research Program of China (973 program) No. 2012CB821802. He was a SAO predoctoral fellow, and a part of the work in this paper was carried out during the course of his PhD research. J.H.Z. is grateful to the National Astronomical Observatories of China for hosting his visit during the course of writing this research paper. We are grateful to Miller Goss for his helpful comments and suggestions. Support for CARMA construction was derived from the states of California, Illinois, and Maryland, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the Associates of the California Institute of Technology, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. The Very Large Array (VLA) is operated by the National Radio Astronomy Observatory (NRAO). The NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 41 TC 6 Z9 6 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2013 VL 779 IS 1 AR 51 DI 10.1088/0004-637X/779/1/51 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 268HD UT WOS:000328160100051 ER PT J AU Kouveliotou, C Granot, J Racusin, JL Bellm, E Vianello, G Oates, S Fryer, CL Boggs, SE Christensen, FE Craig, WW Dermer, CD Gehrels, N Hailey, CJ Harrison, FA Melandri, A McEnery, JE Mundell, CG Stern, DK Tagliaferri, G Zhang, WW AF Kouveliotou, C. Granot, J. Racusin, J. L. Bellm, E. Vianello, G. Oates, S. Fryer, C. L. Boggs, S. E. Christensen, F. E. Craig, W. W. Dermer, C. D. Gehrels, N. Hailey, C. J. Harrison, F. A. Melandri, A. McEnery, J. E. Mundell, C. G. Stern, D. K. Tagliaferri, G. Zhang, W. W. TI NuSTAR OBSERVATIONS OF GRB 130427A ESTABLISH A SINGLE COMPONENT SYNCHROTRON AFTERGLOW ORIGIN FOR THE LATE OPTICAL TO MULTI-GEV EMISSION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE acceleration of particles; gamma-ray burst: individual (GRB 130427A); magnetic fields; radiation mechanisms: non-thermal; shock waves ID GAMMA-RAY BURSTS; INTERGALACTIC MAGNETIC-FIELDS; HIGH-ENERGY EMISSION; CRAB-NEBULA; PARTICLE-ACCELERATION; RELATIVISTIC SHOCKS; RECONNECTION; FLARES; FERMI; SPECTRUM AB GRB 130427A occurred in a relatively nearby galaxy; its prompt emission had the largest GRB fluence ever recorded. The afterglow of GRB 130427A was bright enough for the Nuclear Spectroscopic Telescope ARray (NuSTAR) to observe it in the 3-79 keV energy range long after its prompt emission (similar to 1.5 and 5 days). This range, where afterglow observations were previously not possible, bridges an important spectral gap. Combined with Swift, Fermi, and ground-based optical data, NuSTAR observations unambiguously establish a single afterglow spectral component from optical to multi-GeV energies a day after the event, which is almost certainly synchrotron radiation. Such an origin of the late-time Fermi/Large Area Telescope >10 GeV photons requires revisions in our understanding of collisionless relativistic shock physics. C1 [Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Astrophys Off ZP12, Huntsville, AL 35812 USA. [Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel. [Racusin, J. L.; Gehrels, N.; McEnery, J. E.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bellm, E.; Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Vianello, G.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, W Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Oates, S.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Fryer, C. L.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Dermer, C. D.] Natl Res Lab, Washington, DC 20375 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Melandri, A.; Tagliaferri, G.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Mundell, C. G.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Stern, D. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kouveliotou, C (reprint author), NASA, George C Marshall Space Flight Ctr, Astrophys Off ZP12, Huntsville, AL 35812 USA. EM chryssa.kouveliotou@nasa.gov; granot@openu.ac.il; judith.racusin@nasa.gov RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Bellm, Eric/0000-0001-8018-5348; Tagliaferri, Gianpiero/0000-0003-0121-0723 FU NASA [NNG08FD60C]; INAF in Italy; CNES in France for science FX This work was supported under NASA Contract NNG08FD60C, and made use of data from the NuSTAR mission, a project led by CalTech, managed by JPL, and funded by NASA. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and CalTech. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. The Fermi/LAT Collaboration acknowledges support from NASA and DOE (U. S.), CEA/Irfu and IN2P3/CNRS (France), ASI and INFN (Italy), MEXT, KEK, and JAXA (Japan), and the K. A. Wallenberg Foundation, the Swedish Research Council and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. The Liverpool Telescope is operated by Liverpool John Moores University at the Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. C. G. M. acknowledges support from the Royal Society. NR 41 TC 25 Z9 26 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 10 PY 2013 VL 779 IS 1 AR L1 DI 10.1088/2041-8205/779/1/L1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263ZA UT WOS:000327845400001 ER PT J AU Miller, JM Parker, ML Fuerst, F Bachetti, M Barret, D Grefenstette, BW Tendulkar, S Harrison, FA Boggs, SE Chakrabarty, D Christensen, FE Craig, WW Fabian, AC Hailey, CJ Natalucci, L Paerels, F Rana, V Stern, DK Tomsick, JA Zhang, WW AF Miller, J. M. Parker, M. L. Fuerst, F. Bachetti, M. Barret, D. Grefenstette, B. W. Tendulkar, S. Harrison, F. A. Boggs, S. E. Chakrabarty, D. Christensen, F. E. Craig, W. W. Fabian, A. C. Hailey, C. J. Natalucci, L. Paerels, F. Rana, V. Stern, D. K. Tomsick, J. A. Zhang, W. W. TI CONSTRAINTS ON THE NEUTRON STAR AND INNER ACCRETION FLOW IN SERPENS X-1 USING NuSTAR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; equation of state; relativistic processes; X-rays: binaries ID X-RAY BINARIES; IRON EMISSION-LINES; 4U 1705-44; MASS; SPECTROSCOPY; REFLECTION; RADIUS; CLUSTERS; SPECTRUM; BURSTS AB We report on an observation of the neutron star low-mass X-ray binary Serpens X-1, made with NuSTAR. The extraordinary sensitivity afforded by NuSTAR facilitated the detection of a clear, robust, relativistic Fe K emission line from the inner disk. A relativistic profile is required over a single Gaussian line from any charge state of Fe at the 5 sigma level of confidence, and any two Gaussians of equal width at the same confidence. The Compton back-scattering "hump" peaking in the 10-20 keV band is detected for the first time in a neutron star X-ray binary. Fits with relativistically blurred disk reflection models suggest that the disk likely extends close to the innermost stable circular orbit (ISCO) or stellar surface. The best-fit blurred reflection models constrain the gravitational redshift from the stellar surface to be z(NS) >= 0.16. The data are broadly compatible with the disk extending to the ISCO; in that case, z(NS) >= 0.22 and R-NS <= 12.6 km (assuming M-NS = 1.4 M-circle dot and a = 0, where a = cJ/GM(2)). If the star is as large or larger than its ISCO, or if the effective reflecting disk leaks across the ISCO to the surface, the redshift constraints become measurements. We discuss our results in the context of efforts to measure fundamental properties of neutron stars, and models for accretion onto compact objects. C1 [Miller, J. M.] Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. [Parker, M. L.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Fuerst, F.; Grefenstette, B. W.; Tendulkar, S.; Harrison, F. A.; Rana, V.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Bachetti, M.; Barret, D.] Univ Toulouse, UPS OMP, Toulouse, France. [Bachetti, M.; Barret, D.] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Boggs, S. E.; Craig, W. W.; Tomsick, J. A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Chakrabarty, D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Christensen, F. E.] Danish Tech Univ, Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, C. J.; Paerels, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hailey, C. J.; Paerels, F.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Natalucci, L.] Ist Astrofis & Planetol Spaziali INAF, I-00133 Rome, Italy. [Stern, D. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM jonmm@umich.edu RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337; Rana, Vikram/0000-0003-1703-8796 FU NASA [NNG08FD60C]; California Institute of Technology; NASA FX This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. NR 32 TC 25 Z9 25 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 10 PY 2013 VL 779 IS 1 AR L2 DI 10.1088/2041-8205/779/1/L2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263ZA UT WOS:000327845400002 ER PT J AU Strader, MJ Johnson, MD Mazin, BA Jaeger, GVS Gwinn, CR Meeker, SR Szypryt, P van Eyken, JC Marsden, D O'Brien, K Walter, AB Ulbricht, G Stoughton, C Bumble, B AF Strader, M. J. Johnson, M. D. Mazin, B. A. Jaeger, G. V. Spiro Gwinn, C. R. Meeker, S. R. Szypryt, P. van Eyken, J. C. Marsden, D. O'Brien, K. Walter, A. B. Ulbricht, G. Stoughton, C. Bumble, B. TI EXCESS OPTICAL ENHANCEMENT OBSERVED WITH ARCONS FOR EARLY CRAB GIANT PULSES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE pulsars: general; pulsars: individual (Crab: PSR B0531+21); stars: neutron ID RADIO PULSES; EMISSION; NEBULA AB We observe an extraordinary link in the Crab pulsar between the enhancement of an optical pulse and the timing of the corresponding giant radio pulse. At optical through infrared wavelengths, our observations use the high time resolution of ARray Camera for Optical to Near-IR Spectrophotometry, a unique superconducting energy-resolving photon-counting array at the Palomar 200 inch telescope. At radio wavelengths, we observe with the Robert C. Byrd Green Bank Telescope and the Green Bank Ultimate Pulsar Processing Instrument backend. We see an 11.3% +/- 2.5% increase in peak optical flux for pulses that have an accompanying giant radio pulse arriving near the peak of the optical main pulse, in contrast to a 3.2% +/- 0.5% increase when an accompanying giant radio pulse arrives soon after the optical peak. We also observe that the peak of the optical main pulse is 2.8% +/- 0.8% enhanced when there is a giant radio pulse accompanying the optical interpulse. We observe no statistically significant spectral differences between optical pulses accompanied by and not accompanied by giant radio pulses. Our results extend previous observations of optical-radio correlation to the time and spectral domains. Our refined temporal correlation suggests that optical and radio emission are indeed causally linked, and the lack of spectral differences suggests that the same mechanism is responsible for all optical emission. C1 [Strader, M. J.; Mazin, B. A.; Jaeger, G. V. Spiro; Gwinn, C. R.; Meeker, S. R.; Szypryt, P.; van Eyken, J. C.; Marsden, D.; Walter, A. B.; Ulbricht, G.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Johnson, M. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [O'Brien, K.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Stoughton, C.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Bumble, B.] NASA Jet Prop Lab, Pasadena, CA 91125 USA. RP Strader, MJ (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. RI Mazin, Ben/B-8704-2011; Ulbricht, Gerhard/P-7487-2016 OI Mazin, Ben/0000-0003-0526-1114; Ulbricht, Gerhard/0000-0002-6497-3763 FU NASA [NNX11AD55G] FX The MKID detectors used in this work were developed under NASA grant NNX11AD55G. The MKID digital readout was partially developed under NASA grant NNX10AF58G. S. R. M. was supported by a NASA Office of the Chief Technologist's Space Technology Research Fellowship, NASA grant NNX11AN29H. This work was partially supported by the Keck Institute for Space Studies. C. G., M.J., and G.V.S.J. thank the U. S. National Science Foundation for financial support for this work (AST-1008865). Fermilab is operated by Fermi Research Alliance, LLC under Contract No. De-AC02-07CH11359 with the United States Department of Energy. NR 22 TC 10 Z9 11 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 10 PY 2013 VL 779 IS 1 AR L12 DI 10.1088/2041-8205/779/1/L12 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263ZA UT WOS:000327845400012 ER PT J AU Popa, A Li, J Samia, ACS AF Popa, Adriana Li, Jing Samia, Anna Cristina S. TI Hybrid Platinum Nanobox/Carbon Nanotube Composites for Ultrasensitive Gas Sensing SO SMALL LA English DT Article ID FUNCTIONALIZED CARBON NANOTUBES; CHLORINE GAS; CHEMICAL SENSORS; HYDROGEN SENSOR; NANOPARTICLES; FILMS; NANOSTRUCTURES; NANOCLUSTERS; SENSITIVITY; PERFORMANCE C1 [Popa, Adriana; Samia, Anna Cristina S.] Case Western Reserve Univ, Dept Chem, Cleveland, OH 44106 USA. [Li, Jing] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Li, J (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM jing.li-1@nasa.gov; anna.samia@case.edu FU Case Western Reserve University; NASA Office of the Chief Technologist's Space Technology Research Fellowship [NNX11AN69H]; [NNX09AQ44A] FX This work was supported by start-up funds from Case Western Reserve University and by a NASA Office of the Chief Technologist's Space Technology Research Fellowship for Ms. Adriana Popa (#NNX11AN69H). The HR-TEM and SEM used were available through grant #NNX09AQ44A. NR 48 TC 9 Z9 9 U1 3 U2 45 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 1613-6810 EI 1613-6829 J9 SMALL JI Small PD DEC 9 PY 2013 VL 9 IS 23 BP 3928 EP 3933 DI 10.1002/smll.201203260 PG 6 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA AA7MV UT WOS:000331282400004 PM 23828860 ER PT J AU Khan, A Pommier, A Neumann, GA Mosegaard, K AF Khan, A. Pommier, A. Neumann, G. A. Mosegaard, K. TI The lunar moho and the internal structure of the Moon: A geophysical perspective SO TECTONOPHYSICS LA English DT Review DE Lunar seismology; Crustal thickness; Lunar structure and composition; Lunar gravity and topography; Lunar origin and evolution ID PASSIVE SEISMIC EXPERIMENT; ELECTRICAL-CONDUCTIVITY; CRUSTAL THICKNESS; BULK COMPOSITION; MARE VOLCANISM; GRAVITY-FIELD; PLAGIOCLASE-FLOTATION; CHEMICAL-COMPOSITION; TEMPERATURE PROFILE; MAGMATIC EVOLUTION AB Extraterrestrial seismology saw its advent with the deployment of seismometers during the Apollo missions that were undertaken from July 1969 to December 1972. The Apollo lunar seismic data constitute a unique resource being the only seismic data set which can be used to infer the interior structure of a planetary body besides the Earth. On-going analysis and interpretation of the seismic data continues to provide constraints that help refine lunar origin and evolution. In addition to this, lateral variations in crustal thickness (similar to 0-80 km) are being mapped out at increasing resolution from gravity and topography data that have and continue to be collected with a series of recent lunar orbiter missions. Many of these also carry onboard multi-spectral imaging equipment that is able to map out major-element concentration and surface mineralogy to high precision. These results coupled with improved laboratory-based petrological studies of lunar samples provide important constraints on models for lunar magma ocean evolution, which ultimately determines internal structure. Whereas existing constraints on initial depth of melting and differentiation from quantitative modeling suggested only partial Moon involvement (<500 km depth), more recent models tend to favor a completely molten Moon, although the former cannot be ruled out sensu stricto. Recent geophysical analysis coupled with thermodynamical computations of phase equilibria and physical properties of mantle minerals suggest that the Earth and Moon are compositionally distinct. Continued analysis of ground-based laser ranging data and recent discovery of possible core reflected phases in the Apollo lunar seismic data strengthens the case for a small dense lunar core with a radius of <400 km corresponding to 1-3% of lunar mass. (C) 2013 Elsevier B.V. All rights reserved. C1 [Khan, A.] Swiss Fed Inst Technol, Inst Geochem & Petr, Zurich, Switzerland. [Pommier, A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Neumann, G. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mosegaard, K.] Tech Univ Denmark, Dept Informat & Math Modelling, DK-2800 Lyngby, Denmark. RP Khan, A (reprint author), Swiss Fed Inst Technol, Inst Geochem & Petr, Zurich, Switzerland. EM amir.khan@erdw.ethz.ch RI Neumann, Gregory/I-5591-2013; OI Neumann, Gregory/0000-0003-0644-9944; Mosegaard, Klaus/0000-0001-5292-5249 FU Swiss National Science Foundation [200021-130411] FX We are grateful to Yosio Nakamura for his thorough comments that helped improve the manuscript. Reviews by O. Kuskov and P. Lognonne were also very helpful. This work was supported by Swiss National Science Foundation grant 200021-130411. NR 212 TC 16 Z9 16 U1 4 U2 41 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0040-1951 EI 1879-3266 J9 TECTONOPHYSICS JI Tectonophysics PD DEC 8 PY 2013 VL 609 SI SI BP 331 EP 352 DI 10.1016/j.tecto.2013.02.024 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 296QR UT WOS:000330201000017 ER PT J AU Ciufolini, I Monge, BM Paolozzi, A Koenig, R Sindoni, G Michalak, G Pavlis, EC AF Ciufolini, I. Monge, B. Moreno Paolozzi, A. Koenig, R. Sindoni, G. Michalak, G. Pavlis, E. C. TI Monte Carlo simulations of the LARES space experiment to test General Relativity and fundamental physics SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article ID GRAVITOMAGNETIC FIELD; TIME-DELAY; SATELLITES; SPIN; DRAG AB The LARES (LAser RElativity Satellite) satellite was successfully launched in February 2012. The LARES space experiment is based on the orbital determinations of the laser ranged satellites LARES, LAGEOS (LAser GEOdynamics Satellite) and LAGEOS 2 together with the determination of the Earth's gravity field by the GRACE (Gravity Recovery And Climate Experiment) mission. It will test some fundamental physics predictions and provide accurate measurements of the frame-dragging effect predicted by Einstein's theory of General Relativity. By 100 Monte Carlo simulations of the LARES experiment, with simulations of the orbits of LARES, LAGEOS and LAGEOS 2 according to the latest GRACE gravity field determinations, we found that the systematic errors in the measurement of frame-dragging amount to about 1.4% of the general relativistic effect, confirming previous error analyses. C1 [Ciufolini, I.] Univ Salento, Dipartimento Ingn Innovaz, Lecce, Italy. [Ciufolini, I.] Ctr Fermi, Rome, Italy. [Monge, B. Moreno; Koenig, R.; Michalak, G.] GFZ German Res Ctr Geosci, Potsdam, Germany. [Paolozzi, A.; Sindoni, G.] Univ Roma La Sapienza, Scuola Ingn Aerospaziale, I-00185 Rome, Italy. [Paolozzi, A.; Sindoni, G.] Univ Roma La Sapienza, DIAEE, I-00185 Rome, Italy. [Pavlis, E. C.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Ciufolini, I (reprint author), Univ Salento, Dipartimento Ingn Innovaz, Lecce, Italy. EM ignazio.ciufolini@unisalento.it FU ASI [I/034/12/0]; ESA [4000103504/2011/NL/WE]; NASA [NNX09AU86G] FX The work is performed under the ASI contract no. I/034/12/0 and ESA contract no. 4000103504/2011/NL/WE. The authors acknowledge the Italian Space Agency for its support to the LARES mission and the International Laser Ranging Service for tracking and data distribution of the LARES satellite. ECP acknowledges the support of NASA grant NNX09AU86G. We thank John Ries and the anonymous referees for useful suggestions. NR 36 TC 14 Z9 14 U1 1 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD DEC 7 PY 2013 VL 30 IS 23 AR 235009 DI 10.1088/0264-9381/30/23/235009 PG 11 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 251NN UT WOS:000326936300011 ER PT J AU Hathaway, DH Upton, L Colegrove, O AF Hathaway, David H. Upton, Lisa Colegrove, Owen TI Giant Convection Cells Found on the Sun SO SCIENCE LA English DT Article ID SOLAR CONVECTION; SUPERGRANULES; ZONE; ATMOSPHERE; DYNAMICS; ROTATION; SURFACE; PROBES AB Heat is transported through the outermost 30% of the Sun's interior by overturning convective motions. These motions are evident at the Sun's surface in the form of two characteristic cellular structures: granules and supergranules (similar to 1000 and similar to 30,000 kilometers across, respectively). The existence of much larger cells has been suggested by both theory and observation for more than 45 years. We found evidence for giant cellular flows that persist for months by tracking the motions of supergranules. As expected from the effects of the Sun's rotation, the flows in these cells are clockwise around high pressure in the north and counterclockwise in the south and transport angular momentum toward the equator, maintaining the Sun's rapid equatorial rotation. C1 [Hathaway, David H.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Upton, Lisa] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Upton, Lisa] Univ Alabama, Dept Space Sci, Huntsville, AL 35899 USA. [Colegrove, Owen] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. RP Hathaway, DH (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM david.hathaway@nasa.gov FU NASA; NASA Heliophysics Supporting Research and Technology (SRT) Program; NASA Living With a Star (LWS) Program; University of Alabama in Huntsville by funds from NSF [AGS-1157027] FX The SDO/HMI data described in this paper are archived at http://jsoc.stanford.edu. The SDO/HMI project is supported by NASA grant to Stanford University. D. H. H. was supported by a grant from the NASA Heliophysics Supporting Research and Technology (SR&T) Program to NASA/MSFC. L. U. was supported by a grant from the NASA Living With a Star (LWS) Program to NASA/MSFC. O.C. was supported as a Research Experience for Undergraduates (REU) summer student at the University of Alabama in Huntsville by funds from NSF grant AGS-1157027. NR 18 TC 30 Z9 30 U1 0 U2 13 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD DEC 6 PY 2013 VL 342 IS 6163 BP 1217 EP 1219 DI 10.1126/science.1244682 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 264DT UT WOS:000327857900043 PM 24311685 ER PT J AU Akiyama, S Gopalswamy, N Yashiro, S Makela, P AF Akiyama, Sachiko Gopalswamy, Nat Yashiro, Seiji Maekelae, Pertti TI A Study of Coronal Holes Observed by SOHO/EIT and the Nobeyama Radioheliograph SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE Sun: corona; Sun: radio radiation; Sun: solar wind ID EXTREME-ULTRAVIOLET OBSERVATIONS; COROTATING INTERACTION REGIONS; HEI 10830-A SPECTROHELIOGRAMS; SOLAR-WIND VELOCITY; HIGH-SPEED STREAMS; MULTIWAVELENGTH OBSERVATIONS; MICROWAVE ENHANCEMENT; GEOMAGNETIC STORMS; ELEPHANTS TRUNK; MAGNETIC-FIELD AB Coronal holes (CHs) are areas of reduced emission in EUV and X-ray images that show bright patches of microwave enhancements (MEs) related to magnetic network junctions inside the CHs. A clear correlation between the CH size and the solar wind (SW) speed is well known, but we have less information about the relationship between MEs and other CH and SW properties. We studied the characteristics of 21 equatorial CHs associated with corotating interaction regions (CIRs) during 1996 to 2005. Our CHs were divided into two groups according to the intensity of the associated geomagnetic storms: Dst <= -100 nT (10 events) and > -100 nT (11 events). Using EUV 284 angstrom images obtained by SOHO/EIT and 17 GHz microwave images obtained by the Nobeyama Radioheliograph (NoRH), we found a linear correlation not only between the maximum SW speed and the area of EUV CH (r = 0.62), but also between the maximum SW speed and the area of the ME (r = 0.79). We also compared the EUV CH areas with and without an overlapping ME. The area of the CHs with an ME is better correlated with the SW speed (r = 0.71) than the area of those without an ME (r = 0.36). Therefore, the radio ME may play an important role in understanding the origin of SW. C1 [Akiyama, Sachiko; Yashiro, Seiji; Maekelae, Pertti] Catholic Univ Amer, Washington, DC 20064 USA. [Akiyama, Sachiko; Gopalswamy, Nat; Yashiro, Seiji; Maekelae, Pertti] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Akiyama, S (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. EM sachiko.akiyama@nasa.gov FU NASA SRT program; NASA LWS TRT program; NASA [NNM06AA33G] FX This work was supported by NASA SR&T and LWS TR&T programs. SOHO is a project of international cooperation between ESA and NASA. This effort was supported by a NASA grant (NNM06AA33G). We thank the organizers of the "Living With a Star" CDAW meeting and the members of Working Group 1 for their event identifications. We also thank the ACE and WIND teams for the solar wind and the interplanetary magnetic field data. We further thank Dr M. Shimojo (NAOJ) for a discussion on the NoRH radio images. NR 47 TC 2 Z9 2 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD DEC 5 PY 2013 VL 65 SI 1 AR S15 DI 10.1093/pasj/65.sp1.S15 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI4GL UT WOS:000336823600015 ER PT J AU Gopalswamy, N Yashiro, S AF Gopalswamy, Nat Yashiro, Seiji TI Obscuration of Flare Emission by an Eruptive Prominence SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE Sun: coronal mass ejections; Sun: flares; Sun: microwave emission; Sun: prominences ID CORONAL MASS EJECTIONS; NOBEYAMA RADIOHELIOGRAPH; MICROWAVE OBSERVATIONS; RADIO AB We report on the eclipsing of microwave flare emission by an eruptive prominence from a neighboring region as observed by the Nobeyama Radioheliograph at 17 GHz. The obscuration of the flare emission appears as a dimming feature in the microwave flare light curve. We use the dimming feature to derive the temperature of the prominence and the distribution of heating along the length of the filament. We find that the prominence is heated to a temperature above the quiet Sun temperature at 17 GHz. The duration of the dimming is the time taken by the eruptive prominence in passing over the flaring region. We also find evidence for the obscuration in EUV images obtained by the Solar and Heliospheric Observatory (SOHO) mission. C1 [Gopalswamy, Nat; Yashiro, Seiji] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yashiro, Seiji] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA. EM nat.gopalswamy@nasa.gov; seiji.yashiro@nasa.gov NR 19 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD DEC 5 PY 2013 VL 65 SI 1 AR S11 DI 10.1093/pasj/65.sp1.S11 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI4GL UT WOS:000336823600011 ER PT J AU Ammannito, E De Sanctis, MC Palomba, E Longobardo, A Mittlefehldt, DW McSween, HY Marchi, S Capria, MT Capaccioni, F Frigeri, A Pieters, CM Ruesch, O Tosi, F Zambon, F Carraro, F Fonte, S Hiesinger, H Magni, G McFadden, LA Raymond, CA Russell, CT Sunshine, JM AF Ammannito, E. De Sanctis, M. C. Palomba, E. Longobardo, A. Mittlefehldt, D. W. McSween, H. Y. Marchi, S. Capria, M. T. Capaccioni, F. Frigeri, A. Pieters, C. M. Ruesch, O. Tosi, F. Zambon, F. Carraro, F. Fonte, S. Hiesinger, H. Magni, G. McFadden, L. A. Raymond, C. A. Russell, C. T. Sunshine, J. M. TI Olivine in an unexpected location on Vesta's surface SO NATURE LA English DT Article ID ASTEROID 4 VESTA; REFLECTANCE SPECTRA; PARENT BODY; DIOGENITES; GEOCHEMISTRY; HARZBURGITE; COLLISIONS; PYROXENES; MIXTURES; EUCRITES AB Olivine is a major component of the mantle of differentiated bodies, including Earth. Howardite, eucrite and diogenite (HED) meteorites represent regolith, basaltic-crust, lower-crust and possibly ultramafic-mantle samples of asteroid Vesta, which is the lone surviving, large, differentiated, basaltic rocky protoplanet in the Solar System(1). Only a few of these meteorites, the orthopyroxene-rich diogenites, contain olivine, typically with a concentration of less than 25 per cent by volume(2). Olivine was tentatively identified on Vesta(3,4), on the basis of spectral and colour data, but other observations did not confirm its presence(5). Here we report that olivine is indeed present locally on Vesta's surface but that, unexpectedly, it has not been found within the deep, south-pole basins, which are thought to be excavated mantle rocks(6-8). Instead, it occurs as near-surface materials in the northern hemisphere. Unlike the meteorites, the olivine-rich (more than 50 per cent by volume) material is not associated with diogenite but seems to be mixed with howardite, the most common(7,9) surface material. Olivine is exposed in crater walls and in ejecta scattered diffusely over a broad area. The size of the olivine exposures and the absence of associated diogenite favour a mantle source, but the exposures are located far from the deep impact basins. The amount and distribution of observed olivine-rich material suggest a complex evolutionary history for Vesta. C1 [Ammannito, E.; De Sanctis, M. C.; Palomba, E.; Longobardo, A.; Marchi, S.; Capria, M. T.; Capaccioni, F.; Frigeri, A.; Tosi, F.; Zambon, F.; Carraro, F.; Fonte, S.; Magni, G.] INAF, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [McSween, H. Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Marchi, S.] NASA, Lunar Sci Inst, Boulder, CO 80302 USA. [Pieters, C. M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Ruesch, O.; Hiesinger, H.] Univ Munster, Inst Planetol, D-48149 Munster, Germany. [McFadden, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Sunshine, J. M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP De Sanctis, MC (reprint author), INAF, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. EM eleonora.ammannito@iaps.inaf.it; mariacristina.desanctis@iaps.inaf.it RI De Sanctis, Maria Cristina/G-5232-2013; Frigeri, Alessandro/F-2151-2010; OI De Sanctis, Maria Cristina/0000-0002-3463-4437; Frigeri, Alessandro/0000-0002-9140-3977; capria, maria teresa/0000-0002-9814-9588; McFadden, Lucy/0000-0002-0537-9975; Capaccioni, Fabrizio/0000-0003-1631-4314; Palomba, Ernesto/0000-0002-9101-6774; Tosi, Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592 FU Dawn Instrument, Operations and Science teams; Dawn Framing Camera team; Italian Space Agency [I/004/12/0]; NASA through the Dawn mission; Dawn at Vesta Participating Scientists Program FX We gratefully acknowledge the support of the Dawn Instrument, Operations and Science teams, and, in particular, the Dawn Framing Camera team. This work was supported by Italian Space Agency grant I/004/12/0 and by NASA through the Dawn mission and the Dawn at Vesta Participating Scientists Program. NR 30 TC 50 Z9 50 U1 0 U2 21 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD DEC 5 PY 2013 VL 504 IS 7478 BP 122 EP + DI 10.1038/nature12665 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 264BK UT WOS:000327851700043 PM 24196707 ER PT J AU Crabbe, A Nielsen-Preiss, SM Woolley, CM Barrila, J Buchanan, K McCracken, J Inglis, DO Searles, SC Nelman-Gonzalez, MA Ott, CM Wilson, JW Pierson, DL Stefanyshyn-Piper, HM Hyman, LE Nickerson, CA AF Crabbe, Aurelie Nielsen-Preiss, Sheila M. Woolley, Christine M. Barrila, Jennifer Buchanan, Kent McCracken, James Inglis, Diane O. Searles, Stephen C. Nelman-Gonzalez, Mayra A. Ott, C. Mark Wilson, James W. Pierson, Duane L. Stefanyshyn-Piper, Heidemarie M. Hyman, Linda E. Nickerson, Cheryl A. TI Spaceflight Enhances Cell Aggregation and Random Budding in Candida albicans SO PLOS ONE LA English DT Article ID SHEAR MODELED MICROGRAVITY; INTERNATIONAL-SPACE-STATION; CYCLASE-ASSOCIATED PROTEIN; BACTERIAL GENE-EXPRESSION; SM-LIKE PROTEINS; SACCHAROMYCES-CEREVISIAE; BIOFILM FORMATION; ESCHERICHIA-COLI; DRUG-RESISTANCE; LSM PROTEINS AB This study presents the first global transcriptional profiling and phenotypic characterization of the major human opportunistic fungal pathogen, Candida albicans, grown in spaceflight conditions. Microarray analysis revealed that C. albicans subjected to short-term spaceflight culture differentially regulated 452 genes compared to synchronous ground controls, which represented 8.3% of the analyzed ORFs. Spaceflight-cultured C. albicans-induced genes involved in cell aggregation (similar to flocculation), which was validated by microscopic and flow cytometry analysis. We also observed enhanced random budding of spaceflight-cultured cells as opposed to bipolar budding patterns for ground samples, in accordance with the gene expression data. Furthermore, genes involved in antifungal agent and stress resistance were differentially regulated in spaceflight, including induction of ABC transporters and members of the major facilitator family, downregulation of ergosterol-encoding genes, and upregulation of genes involved in oxidative stress resistance. Finally, downregulation of genes involved in actin cytoskeleton was observed. Interestingly, the transcriptional regulator Cap1 and over 30% of the Cap1 regulon was differentially expressed in spaceflight-cultured C. albicans. A potential role for Cap1 in the spaceflight response of C. albicans is suggested, as this regulator is involved in random budding, cell aggregation, and oxidative stress resistance; all related to observed spaceflight-associated changes of C. albicans. While culture of C. albicans in microgravity potentiates a global change in gene expression that could induce a virulence-related phenotype, no increased virulence in a murine intraperitoneal (i.p.) infection model was observed under the conditions of this study. Collectively, our data represent an important basis for the assessment of the risk that commensal flora could play during human spaceflight missions. Furthermore, since the low fluid-shear environment of microgravity is relevant to physical forces encountered by pathogens during the infection process, insights gained from this study could identify novel infectious disease mechanisms, with downstream benefits for the general public. C1 [Nickerson, Cheryl A.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85069 USA. [Crabbe, Aurelie; Barrila, Jennifer; Wilson, James W.; Nickerson, Cheryl A.] Arizona State Univ, Biodesign Inst, Ctr Infect Dis & Vaccinol, Tempe, AZ USA. [Nielsen-Preiss, Sheila M.; Woolley, Christine M.; Searles, Stephen C.; Hyman, Linda E.] Montana State Univ, Dept Immunol & Infect Dis, Bozeman, MT 59717 USA. [Buchanan, Kent] Oklahoma City Univ, Dept Biol, Oklahoma City, OK USA. [Buchanan, Kent; McCracken, James; Wilson, James W.] Tulane Univ, Program Mol Pathogenesis & Immun, Dept Microbiol & Immunol, Hlth Sci Ctr, New Orleans, LA 70118 USA. [McCracken, James] Univ Louisville, Diabet & Obes Ctr, Louisville, KY 40292 USA. [Inglis, Diane O.] Stanford Univ, Sch Med, Dept Genet, Stanford, CA USA. [Nelman-Gonzalez, Mayra A.] Wyle Sci Technol & Engn Grp, Houston, TX USA. [Ott, C. Mark; Pierson, Duane L.] NASA, Biomed Res & Environm Sci Div, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Wilson, James W.] Villanova Univ, Dept Biol, Villanova, PA 19085 USA. [Stefanyshyn-Piper, Heidemarie M.] NASA, Astronaut Off, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Hyman, Linda E.] Boston Univ, Sch Med, Boston, MA 02118 USA. RP Nickerson, CA (reprint author), Arizona State Univ, Sch Life Sci, Tempe, AZ 85069 USA. EM cheryl.nickerson@asu.edu OI Inglis, Diane/0000-0003-3166-4638 FU National Aeronautics and Space Administration [NCC2-1362, NNX09AH40G, NNX10AO52G] FX This work was supported by National Aeronautics and Space Administration grants NCC2-1362, NNX09AH40G, and NNX10AO52G (to C.A.N.). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 107 TC 8 Z9 8 U1 1 U2 20 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD DEC 4 PY 2013 VL 8 IS 12 AR e80677 DI 10.1371/journal.pone.0080677 PG 24 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 265KD UT WOS:000327949300038 PM 24324620 ER PT J AU Molina, MJ Colussi, AJ Molina, LT Schindler, RN Tso, TL AF Molina, M. J. Colussi, A. J. Molina, L. T. Schindler, R. N. Tso, T-L TI Historical perspective on: Quantum yield of chlorine-atom formation in the photodissociation of chlorine peroxide (ClOOCl) at 308 nm [Volume 173, Issue 4, 12 October 1990, Pages 310-315] SO CHEMICAL PHYSICS LETTERS LA English DT Editorial Material AB The original letter concluded that chlorine peroxide (ClOOCl) photolizes in the atmosphere to yield free chlorine atoms. Some later work questioned the experimental results, but subsequent papers clearly established the validity of the original findings. (C) 2013 Elsevier B. V. All rights reserved. C1 [Molina, M. J.; Colussi, A. J.; Molina, L. T.; Schindler, R. N.; Tso, T-L] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Molina, MJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mjmolina@ucsd.edu RI Colussi, Agustin/C-6520-2008 NR 0 TC 0 Z9 0 U1 1 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 EI 1873-4448 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD DEC 3 PY 2013 VL 589 BP 51 EP 51 DI 10.1016/j.cplett.2013.08.047 PG 1 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 258WY UT WOS:000327490600022 ER PT J AU Molina, MJ Colussi, AJ Molina, LT Schindler, RN Tso, TL AF Molina, M. J. Colussi, A. J. Molina, L. T. Schindler, R. N. Tso, T-L TI Quantum yield of chlorine-atom formation in the photodissociation of chlorine peroxide (ClOOCl) at 308 nm (Reprinted from Chemical Physics Letters) SO CHEMICAL PHYSICS LETTERS LA English DT Reprint ID CL2O2; DIMER; STRATOSPHERE AB The production of Cl atoms in the laser flash photolysis of ClOOCl at 308 nm has been investigated by time-resolved atomic resonance fluorescence at 235 K. A value of phi = 1.03 +/- 0.12 has been obtained for the primary quantum yield based on an absorption cross section ratio sigma(245)/sigma(308) = 22 for ClOOCl at 245 and 308 nm. (C) 2013 Published by Elsevier B. V. C1 [Molina, M. J.; Colussi, A. J.; Molina, L. T.; Schindler, R. N.; Tso, T-L] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Molina, MJ (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RI Colussi, Agustin/C-6520-2008 NR 17 TC 1 Z9 1 U1 1 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 EI 1873-4448 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD DEC 3 PY 2013 VL 589 BP 52 EP 55 DI 10.1016/j.cplett.2013.08.067 PG 4 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 258WY UT WOS:000327490600023 ER PT J AU Kharecha, PA Hansen, JE AF Kharecha, Pushker A. Hansen, James E. TI Response to Comment by Rabilloud on "Prevented Mortality and Greenhouse Gas Emissions from Historical and Projected Nuclear Power" SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Letter C1 [Kharecha, Pushker A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Columbia Univ, Earth Inst, New York, NY 10025 USA. RP Kharecha, PA (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM pushker@giss.nasa.gov NR 7 TC 0 Z9 0 U1 2 U2 13 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD DEC 3 PY 2013 VL 47 IS 23 BP 13900 EP 13901 DI 10.1021/es404806w PG 2 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 266CH UT WOS:000327999400086 PM 24215392 ER PT J AU Hansen, J Kharecha, P Sato, M Masson-Delmotte, V Ackerman, F Beerling, DJ Hearty, PJ Hoegh-Guldberg, O Hsu, SL Parmesan, C Rockstrom, J Rohling, EJ Sachs, J Smith, P Steffen, K Van Susteren, L von Schuckmann, K Zachos, JC AF Hansen, James Kharecha, Pushker Sato, Makiko Masson-Delmotte, Valerie Ackerman, Frank Beerling, David J. Hearty, Paul J. Hoegh-Guldberg, Ove Hsu, Shi-Ling Parmesan, Camille Rockstrom, Johan Rohling, Eelco J. Sachs, Jeffrey Smith, Pete Steffen, Konrad Van Susteren, Lise von Schuckmann, Karina Zachos, James C. TI Assessing "Dangerous Climate Change": Required Reduction of Carbon Emissions to Protect Young People, Future Generations and Nature SO PLOS ONE LA English DT Review ID SEA-LEVEL RISE; LAST INTERGLACIAL HIGHSTAND; GREENHOUSE-GAS EMISSIONS; SHEET MASS-BALANCE; LAND-USE CHANGE; GLOBAL TEMPERATURE; OIL SANDS; PROBABILISTIC ASSESSMENT; INTENSE PRECIPITATION; ANTHROPOGENIC CARBON AB We assess climate impacts of global warming using ongoing observations and paleoclimate data. We use Earth's measured energy imbalance, paleoclimate data, and simple representations of the global carbon cycle and temperature to define emission reductions needed to stabilize climate and avoid potentially disastrous impacts on today's young people, future generations, and nature. A cumulative industrial-era limit of similar to 500 GtC fossil fuel emissions and 100 GtC storage in the biosphere and soil would keep climate close to the Holocene range to which humanity and other species are adapted. Cumulative emissions of similar to 1000 GtC, sometimes associated with 2 degrees C global warming, would spur "slow" feedbacks and eventual warming of 3-4 degrees C with disastrous consequences. Rapid emissions reduction is required to restore Earth's energy balance and avoid ocean heat uptake that would practically guarantee irreversible effects. Continuation of high fossil fuel emissions, given current knowledge of the consequences, would be an act of extraordinary witting intergenerational injustice. Responsible policymaking requires a rising price on carbon emissions that would preclude emissions from most remaining coal and unconventional fossil fuels and phase down emissions from conventional fossil fuels. C1 [Hansen, James; Kharecha, Pushker; Sato, Makiko; Sachs, Jeffrey] Columbia Univ, Earth Inst, New York, NY 10027 USA. [Kharecha, Pushker] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Masson-Delmotte, Valerie] CEA CNRS UVSQ, Inst Pierre Simon Laplace, Lab Sci Climat & Environm, Gif Sur Yvette, France. [Ackerman, Frank] Synapse Energy Econ, Cambridge, MA USA. [Beerling, David J.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. [Hearty, Paul J.] Univ N Carolina, Dept Environm Studies, Wilmington, NC 28401 USA. [Hoegh-Guldberg, Ove] Univ Queensland, Global Change Inst, St Lucia, Qld, Australia. [Hsu, Shi-Ling] Florida State Univ, Coll Law, Tallahassee, FL 32306 USA. [Parmesan, Camille] Univ Plymouth, Inst Marine, Plymouth PL4 8AA, Devon, England. [Parmesan, Camille] Univ Texas Austin, Austin, TX 78712 USA. [Rockstrom, Johan] Stockholm Univ, Stockholm Resilience Ctr, S-10691 Stockholm, Sweden. [Rohling, Eelco J.] Univ Southampton, Sch Ocean & Earth Sci, Southampton, Hants, England. [Rohling, Eelco J.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT, Australia. [Smith, Pete] Univ Aberdeen, Aberdeen, Scotland. [Steffen, Konrad] Swiss Fed Res Inst WSL, Swiss Fed Inst Technol, Zurich, Switzerland. [Van Susteren, Lise] Harvard Univ, Sch Publ Hlth, Advisory Board, Ctr Hlth & Global Environm, Boston, MA 02115 USA. [von Schuckmann, Karina] IFREMER, Toulon, France. [Zachos, James C.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. RP Hansen, J (reprint author), Columbia Univ, Earth Inst, New York, NY 10027 USA. EM jimehansen@gmail.com RI Masson-Delmotte, Valerie/G-1995-2011; Steffen, Konrad/C-6027-2013; Beerling, David/C-2840-2009; Rohling, Eelco/B-9736-2008; Smith, Pete/G-1041-2010; OI Rockstrom, Johan/0000-0001-8988-2983; Masson-Delmotte, Valerie/0000-0001-8296-381X; Steffen, Konrad/0000-0001-8658-1026; Beerling, David/0000-0003-1869-4314; Rohling, Eelco/0000-0001-5349-2158; Smith, Pete/0000-0002-3784-1124; Ackerman, Frank/0000-0002-7940-482X FU NASA; Flora Family Foundation; Jeremy Grantham, ClimateWorks; Energy Foundation FX Funding came from: NASA Climate Research Funding, Gifts to Columbia University from H. F. ("Gerry") Lenfest, private philanthropist (no web site, but see http://en.wikipedia.org/wiki/H._F._Lenfest), Jim Miller, Lee Wasserman (Rockefeller Family Fund) (http://www.rffund.org/), Flora Family Foundation (http://www.florafamily.org/), Jeremy Grantham, ClimateWorks and the Energy Foundation provided support for Hansen's Climate Science, Awareness and Solutions program at Columbia University to complete this research and publication. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 248 TC 105 Z9 106 U1 32 U2 245 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD DEC 3 PY 2013 VL 8 IS 12 AR e81648 DI 10.1371/journal.pone.0081648 PG 26 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 265JR UT WOS:000327947800051 PM 24312568 ER PT J AU Kang, D Rim, T Baek, CK Meyyappan, M Lee, JS AF Kang, Daegun Rim, Taiuk Baek, Chang-Ki Meyyappan, M. Lee, Jeong-Soo TI Investigation of electromigration in In2Se3 nanowire for phase change memory devices SO APPLIED PHYSICS LETTERS LA English DT Article ID GE2SB2TE5 AB The decomposition of In2Se3 nanowire phase change memory devices during current-driving operation was investigated. The devices were subjected to thermal/electrical stress with current density and electric field during the reset operation at 0.24-0.38 MA/cm(2) and 5.3-6.4 kV/cm, respectively. After multiple operation cycles, a change in morphology and composition of the In2Se3 nanowire was observed and led to the device failure. The transmission electron microscopy and energy dispersive analysis indicate that electromigration causes the catastrophic failure by void formation where In atoms migrate toward the cathode and Se atoms migrate toward the anode depending on their electronegativities. (C) 2013 AIP Publishing LLC. C1 [Kang, Daegun; Lee, Jeong-Soo] Pohang Univ Sci & Technol, Dept Elect Engn, Pohang, South Korea. [Rim, Taiuk; Baek, Chang-Ki] Pohang Univ Sci & Technol, Creat IT Engn, Pohang, South Korea. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lee, Jeong-Soo] Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang, South Korea. RP Lee, JS (reprint author), Pohang Univ Sci & Technol, Dept Elect Engn, Pohang, South Korea. EM ljs6951@postech.ac.kr FU National Research Foundation (NRF) [2012R1A2A2A02010432]; center for advanced soft electronics under the global frontier research program of the Ministry of Education, Science, and Technology (MEST) [2011-0031638]; IT Consilience Creative Program [NIPA-2013-H0203-13-1001] FX This work was in part supported by National Research Foundation (NRF) (No. 2012R1A2A2A02010432) and by a Grant (Code No. 2011-0031638) from the center for advanced soft electronics under the global frontier research program of the Ministry of Education, Science, and Technology (MEST), and by the "IT Consilience Creative Program" (NIPA-2013-H0203-13-1001) supervised by the National IT Industry Promotion Agency, Korea. NR 23 TC 3 Z9 3 U1 2 U2 32 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD DEC 2 PY 2013 VL 103 IS 23 AR 233504 DI 10.1063/1.4838755 PG 4 WC Physics, Applied SC Physics GA 274VS UT WOS:000328634900092 ER PT J AU Liu, D Hussey, DS Gubarev, MV Ramsey, BD Jacobson, D Arif, M Moncton, DE Khaykovich, B AF Liu, D. Hussey, D. S. Gubarev, M. V. Ramsey, B. D. Jacobson, D. Arif, M. Moncton, D. E. Khaykovich, B. TI Response to "Comment on 'Demonstration of achromatic cold-neutron microscope utilizing axisymmetric focusing mirrors'" [Appl. Phys. Lett. 103, 236101 (2013)] SO APPLIED PHYSICS LETTERS LA English DT Editorial Material ID RESOLUTION C1 [Liu, D.; Moncton, D. E.; Khaykovich, B.] MIT, Nucl Reactor Lab, Cambridge, MA 02139 USA. [Hussey, D. S.; Jacobson, D.; Arif, M.] NIST, Phys Measurement Lab, Gaithersburg, MD 20899 USA. [Gubarev, M. V.; Ramsey, B. D.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Moncton, D. E.] MIT, Dept Phys, Cambridge, MA 02139 USA. RP Khaykovich, B (reprint author), MIT, Nucl Reactor Lab, 138 Albany St, Cambridge, MA 02139 USA. EM bkh@mit.edu RI Khaykovich, Boris/A-7376-2012 OI Khaykovich, Boris/0000-0002-9490-2771 NR 6 TC 0 Z9 0 U1 1 U2 12 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD DEC 2 PY 2013 VL 103 IS 23 AR 236102 DI 10.1063/1.4835175 PG 1 WC Physics, Applied SC Physics GA 274VS UT WOS:000328634900110 ER PT J AU Kojima, JJ Fischer, DG AF Kojima, Jun J. Fischer, David G. TI MULTISCALAR ANALYSES OF HIGH-PRESSURE SWIRL-STABILIZED COMBUSTION VIA SINGLE-SHOT DUAL-SBG RAMAN SPECTROSCOPY SO COMBUSTION SCIENCE AND TECHNOLOGY LA English DT Article DE Combustion diagnostics; High-pressure combustion; Raman spectroscopy; Scalar analysis; Turbulent flow ID TURBINE MODEL COMBUSTOR; JET DIFFUSION FLAME; 1D RAMAN/RAYLEIGH SCATTERING; RAYLEIGH-LIF MEASUREMENTS; LARGE-EDDY SIMULATION; TURBULENT COMBUSTION; NONPREMIXED FLAMES; ELEVATED PRESSURE; LASER DIAGNOSTICS; SOOT FORMATION AB We report an experimental study and thermochemical analysis of high-pressure swirl-stabilized combustion utilizing subframe burst gating (SBG) Raman spectroscopy. SBG Raman spectroscopy is a novel diagnostic technique that provides increased accuracy of quantitative scalar measurements in a single-shot pointwise manner. A recent modification of our original system allows parallel detection of both Stokes and anti-Stokes spectral components (hence the term dual SBG). We begin by briefly describing the experimental construction of a Raman calibration matrix, which allows us to reduce spectral cross-talk in the measurements. Next we describe the application of dual-SBG Raman spectroscopy to simultaneous single-shot measurement of temperature and species mass fractions in a turbulent flame stabilized over a lean-direct-injection (LDI) burner using gaseous methane fuel at elevated pressure of 17atm. Our discussion includes the practical challenges of Raman spectroscopy in a pressurized combustion rig. Statistical analyses of the single-shot thermochemical data provide insights into the nature of the partial-premixing process and its impact on the subsequent combustion process. C1 [Kojima, Jun J.] Ohio Aerosp Inst, Cleveland, OH 44142 USA. [Fischer, David G.] NASA Glenn Res Ctr, Cleveland, OH USA. RP Kojima, JJ (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA. EM Jun.J.Kojima@nasa.gov FU Fundamental Aeronautics Program's Supersonics Project at NASA John H. Glenn Research Center FX This work was supported principally by the Fundamental Aeronautics Program's Supersonics Project at NASA John H. Glenn Research Center. The authors acknowledge Quang-Viet Nguyen for his long advisory support on the project and the manuscript of this paper; and Greg Calhoun, Derek Podboy, and Kurt Rusmisel for their assistance in the construction and operation of the facilities. The authors are very thankful to J.-Y. Chen for his laminar flame calculations. NR 42 TC 6 Z9 6 U1 0 U2 14 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0010-2202 EI 1563-521X J9 COMBUST SCI TECHNOL JI Combust. Sci. Technol. PD DEC 2 PY 2013 VL 185 IS 12 BP 1735 EP 1761 DI 10.1080/00102202.2013.832231 PG 27 WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary; Engineering, Chemical SC Thermodynamics; Energy & Fuels; Engineering GA 265DA UT WOS:000327928700002 ER PT J AU Rousselet, E Stacy, NI LaVictoire, K Higgins, BM Tocidlowski, ME Flanagan, JP Godard-Codding, CAJ AF Rousselet, Estelle Stacy, Nicole I. LaVictoire, Kara Higgins, Benjamin M. Tocidlowski, Maryanne E. Flanagan, Joseph P. Godard-Codding, Celine A. J. TI HEMATOLOGY AND PLASMA BIOCHEMISTRY ANALYTES IN FIVE AGE GROUPS OF IMMATURE, CAPTIVE- REARED LOGGERHEAD SEA TURTLES (CARETTA CARETTA) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Caretta caretta; loggerhead sea turtle; immature; captivity; hematology; plasma biochemistry ID CYTOCHEMICAL CHARACTERISTICS; REFERENCE INTERVALS; CHELONIA-MYDAS; GREEN TURTLES; BLOOD-CELLS; HEALTH PARAMETERS; NORTH-CAROLINA; JUVENILE; VALUES; LENGTH AB Blood samples of 85 immature, apparently healthy, captive-reared loggerhead sea turtles (Caretta caretta) were analyzed for 13 hematologic variables and total solids of 5 age groups (8, 20, 32, 44, and 56 mo old) and for 20 plasma biochemical analytes of 4 age groups (20 to 56 mo old). Each individual turtle was sampled under similar conditions during a blood collection period of 3 days. Hematologic analytes included packed cell volume, white blood cell (WBC) counts, WBC estimates, and leukocyte differentials. Biochemical analysis included albumin, alanine aminotransferase, alkaline phosphatase, amylase, aspartate aminotransferase, blood urea nitrogen, calcium, chloride, cholesterol, creatine kinase, creatinine, gamma glutamyltransferase, globulins, glucose, phosphorous, potassium, sodium, total bilirubin, total protein, total solids, and uric acid. In due consideration of small sample size in all five age groups, the results of hematologic and biochemical analysis were used to determine ranges for these analytes and to compare values among consecutive age groups. Several significant differences in some hematologic and biochemical variables were identified and need to be considered in the interpretation of blood work of immature, growing sea turtles in human care. C1 [Rousselet, Estelle; Godard-Codding, Celine A. J.] Texas Tech Univ, Inst Environm & Human Hlth, Dept Environm Toxicol, Lubbock, TX 79416 USA. [Stacy, Nicole I.] Univ Florida, Coll Vet Med, Dept Large Anim Clin Sci, Gainesville, FL 32610 USA. [LaVictoire, Kara; Tocidlowski, Maryanne E.; Flanagan, Joseph P.] Houston Zoo Inc, Houston, TX 77030 USA. [Higgins, Benjamin M.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Galveston, TX 77551 USA. RP Stacy, NI (reprint author), Univ Florida, Coll Vet Med, Dept Large Anim Clin Sci, 2015 SW 16th Ave, Gainesville, FL 32610 USA. EM StacyN@vetmed.ufl.edu FU Florida Fish and Wildlife Conservation Commission MTP [015]; U.S. Fish and Wildlife Service [TE676379-4]; Rotary Foundation, the Houston Zoo, Inc.; NOAA Fisheries Service Galveston Laboratory; Institute of Environmental and Human Health at Texas Tech University FX The supporting personnel at the Houston Zoo, the NOAA Fisheries Service Galveston Sea Turtle Facility (specifically Nick Shaw), and the Texas Veterinary Medical Diagnostic Laboratory are gratefully acknowledged for their technical support. Research for this project was performed under Florida Fish and Wildlife Conservation Commission MTP# 015, and U.S. Fish and Wildlife Service TE676379-4. Funding and logistic support for this project was provided by the Rotary Foundation, the Houston Zoo, Inc., the NOAA Fisheries Service Galveston Laboratory, and The Institute of Environmental and Human Health at Texas Tech University. NR 37 TC 5 Z9 5 U1 2 U2 21 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 EI 1937-2825 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD DEC PY 2013 VL 44 IS 4 BP 859 EP 874 DI 10.1638/2013-0024R.1 PG 16 WC Veterinary Sciences SC Veterinary Sciences GA AM1ZR UT WOS:000339648300005 PM 24450044 ER PT J AU Morris, R Chien, S AF Morris, Robert Chien, Steve TI The Eighth International Workshop on Planning and Scheduling for Space (IWPSS) SO AI MAGAZINE LA English DT Article AB The Eighth International Workshop on Planning and Scheduling for Space (IWPSS 2013) was held on March 25-26, 2013; at the NASA Ames Research Center, Moffett Field, California. This was the eighth in a regular series that started in 1997. C1 [Morris, Robert] NASA, Ames Res Ctr, Planning & Scheduling Grp, Washington, DC 20546 USA. [Chien, Steve] CALTECH, Artificial Intelligence Grp, Pasadena, CA 91125 USA. [Chien, Steve] CALTECH, Mission Planning & Execut Sect, Pasadena, CA 91125 USA. RP Morris, R (reprint author), NASA, Ames Res Ctr, Planning & Scheduling Grp, Washington, DC 20546 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER ASSOC ARTIFICIAL INTELL PI MENLO PK PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA SN 0738-4602 J9 AI MAG JI AI Mag. PD WIN PY 2013 VL 34 IS 4 BP 126 EP 126 PG 1 WC Computer Science, Artificial Intelligence SC Computer Science GA AI5FY UT WOS:000336892000013 ER PT J AU Strawa, AW Chatfield, RB Legg, M Scarnato, B Esswein, R AF Strawa, A. W. Chatfield, R. B. Legg, M. Scarnato, B. Esswein, R. TI Improving retrievals of regional fine particulate matter concentrations from Moderate Resolution Imaging Spectroradiometer (MODIS) and Ozone Monitoring Instrument (OMI) multisatellite observations SO JOURNAL OF THE AIR & WASTE MANAGEMENT ASSOCIATION LA English DT Article ID AEROSOL OPTICAL-THICKNESS; AIR-QUALITY ASSESSMENT; GROUND-LEVEL PM2.5; PROMISED LAND; UNITED-STATES; POLLUTION; VALIDATION; PRODUCTS; ALGORITHM; SPACE AB A combination of multiplatform satellite observations and statistical data analysis are used to improve the correlation between estimates of PM2.5 (particulate mass with aerodynamic diameter less that 2.5 mu m) retrieved from satellite observations and ground-level measured PM2.5. Accurate measurements of PM2.5 can be used to assess the impact of air pollution levels on human health and the environment and to validate air pollution models. The area under study is California's San Joaquin Valley (SJV) that has a history of poor particulate air quality. Attempts to use simple linear regressions to estimate PM2.5 from satellite-derived aerosol optical depth (AOD) have not yielded good results. The period of study for this project was from October 2004 to July 2008 for six sites in the SJV. A simple linear regression between surface-measured PM2.5 and satellite-observed AOD (from MODIS [Moderate Resolution Imaging Spectroradiometer]) yields a correlation coefficient of about 0.17 in this region. The correlation coefficient between the measured PM2.5 and that retrieved combining satellite observations in a generalized additive model (GAM) resulted in an improved correlation coefficient of 0.77. The model used combinations of MODIS AOD, OMI (Ozone Monitoring Instrument) AOD, NO2 concentration, and a seasonal variable as parameters. Particularly noteworthy is the fact that the PM2.5 retrieved using the GAM captures many of the PM2.5 exceedances that were not seen in the simple linear regression model. Particulate Mass (PM) in the air is a concern because of its effect on climate and human health. PM concentrations retrieved from satellite observations of aerosol optical depth can provide broad regional coverage that is not attained by surface sites. The techniques developed in this paper have resulted in greatly improved correlations between PM retrieved from satellite observations and PM from surface measurements in areas where the correlation is typically low. These improved retrievals can be used to fill in the gaps between surface sites and validate air quality models that are used for air quality forecasts and epidemiological studies. Supplemental Materials: Supplemental materials are available for this paper. Go to the publisher's online edition of the Journal of the Air & Waste Management Association for information on the effects of grid size and MODIS data quality flags on the GAM results. The coefficients for the GAMs used in this study are also listed. C1 [Strawa, A. W.] NASA, Ames Res Ctr, New Opportun Ctr, Moffett Field, CA 94035 USA. [Chatfield, R. B.] NASA, Div Earth Sci, Ames Res Ctr, Moffett Field, CA 94035 USA. [Legg, M.; Scarnato, B.; Esswein, R.] Bay Area Environm Res Inst, Sonoma, CA USA. RP Strawa, AW (reprint author), NASA, Ames Res Ctr, Mail Stop 211-5, Moffett Field, CA 94035 USA. EM Anthony.W.Strawa@nasa.gov NR 53 TC 9 Z9 9 U1 0 U2 17 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 1096-2247 EI 2162-2906 J9 J AIR WASTE MANAGE JI J. Air Waste Manage. Assoc. PD DEC 1 PY 2013 VL 63 IS 12 BP 1434 EP 1446 DI 10.1080/10962247.2013.822838 PG 13 WC Engineering, Environmental; Environmental Sciences; Meteorology & Atmospheric Sciences SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AC5VB UT WOS:000332588000006 PM 24558706 ER PT J AU Mehta, M Sengupta, A Renno, NO Van Norman, JW Huseman, PG Gulick, DS Pokora, M AF Mehta, Manish Sengupta, Anita Renno, Nilton O. Van Norman, John W. Huseman, Peter G. Gulick, Douglas S. Pokora, Mark TI Thruster Plume Surface Interactions: Applications for Spacecraft Landings on Planetary Bodies SO AIAA JOURNAL LA English DT Article ID FREE JET IMPINGEMENT; IMPINGING JETS; NOZZLES AB Numerical and experimental investigations of supersonic jet interactions with a flat surface at various atmospheric pressures are presented in this paper. These studies were done in assessing the landing hazards of both the NASA Mars Science Laboratory and the Phoenix Mars spacecraft. Temporal and spatial ground pressure measurements in conjunction with numerical solutions at altitudes of similar to 35 nozzle exit diameters and jet expansion ratios e between 0.02 and 100 are used. This study shows that, for typical landing spacecraft engine parameters, thruster plumes exhausting into Martian environments create the largest surface pressure loads and can occur at high spacecraft altitudes in contrast to the jet interactions, which occur in terrestrial and lunar atmospheres. These differences are dependent on the stability and dynamics of the plate shock, the length of the supersonic core, and plume decay due to shear layer instability, all of which are functions of the jet expansion ratio. Theoretical, experimental, and analytical results show that subscale supersonic cold gas jets adequately simulate the flowfield and loads due to rocket plume impingement, provided important scaling parameters are in agreement. These studies indicate the critical importance of testing and modeling plume-surface interactions for descent and ascent of spacecraft and launch vehicles. C1 [Mehta, Manish] NASA, George C Marshall Space Flight Ctr, Aerosci Branch, Huntsville, AL 35812 USA. [Sengupta, Anita] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Renno, Nilton O.] Univ Michigan, Dept Atmospher & Space Sci, Ann Arbor, MI 48109 USA. [Van Norman, John W.] Analyt Mech Associates Inc, Atmospher Flight & Entry Syst Branch, Hampton, VA 23666 USA. [Huseman, Peter G.; Gulick, Douglas S.] Lockheed Martin Space Syst, Aerosci Div, Denver, CO 80125 USA. [Pokora, Mark] Univ Michigan, Dept Mech Engn, Ann Arbor, MI 48109 USA. RP Mehta, M (reprint author), NASA, George C Marshall Space Flight Ctr, Aerosci Branch, EV33, Huntsville, AL 35812 USA. EM manish.mehta@nasa.gov FU NASA Graduate Student Researchers Program [NNX06AH56H] FX This research was supported by the NASA Graduate Student Researchers Program grant NNX06AH56H. Special thanks to Ron Greeley of Arizona State University, Ken Smith of the Planetary Aeolian Laboratory at NASA Ames Research Center and the Entry, Descent, And Landing and Advanced Technologies Division at the NASA Jet Propulsion Laboratory. NR 37 TC 4 Z9 4 U1 2 U2 6 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD DEC PY 2013 VL 51 IS 12 BP 2800 EP 2818 DI 10.2514/1.J052408 PG 19 WC Engineering, Aerospace SC Engineering GA AA8XK UT WOS:000331378100006 ER PT J AU Guo, YP Brusniak, L Czech, M Thomas, RH AF Guo, Yueping Brusniak, Leon Czech, Michael Thomas, Russell H. TI Hybrid Wing-Body Aircraft Slat Noise SO AIAA JOURNAL LA English DT Article AB This paper presents an analysis of the slat noise for hybrid wing-body aircraft. It is shown that the hybrid wing-body slat noise is characterized by its broad spectral shapes with frequencies depending on both the mean flow velocity and the aircraft angle of attack, with the former following the conventional Strouhal number scaling and the latter explainable by the dependence of the coherence length of the unsteady flows on the angle of attack. Although the overall noise levels approximately follow the fifth power law in Mach number, the Mach number effects manifest themselves spectrally in both amplitudes and spectral shapes. The noise amplitude is shown to also depend on the angle of attack, assuming a minimum in the range of 3 to 5 deg. These features are all modeled and incorporated in slat noise-prediction methodologies, extending the prediction capability from conventional to hybrid wing-body configurations. Comparisons between predictions and data show very good agreements in both various parametric trends and the absolute levels. The hybrid wing-body aircraft is designed to operate at angles of attack higher than those of conventional aircraft. This is shown to significantly increase the hybrid wing-body slat noise. To further illustrate, the test data are extrapolated to full scale and compared with the slat noise of the Boeing 777 aircraft, showing that the former is higher than the latter. C1 [Guo, Yueping] Boeing Res & Technol, Acoust Technol, Huntington Beach, CA 92647 USA. [Brusniak, Leon; Czech, Michael] Boeing Commercial Airplane Co, Acoust Technol, Seattle, WA 98124 USA. [Thomas, Russell H.] NASA, Langley Res Ctr, Aeroacoust Branch, Hampton, VA 23681 USA. RP Guo, YP (reprint author), Boeing Res & Technol, Acoust Technol, 5301 Bolsa Ave, Huntington Beach, CA 92647 USA. FU NASA Environmentally Responsible Aviation Project under NASA [NNL04AA11B, NNL10AA71T] FX The work reported here was sponsored by the NASA Environmentally Responsible Aviation Project under NASA contract NNL04AA11B, task order NNL10AA71T. Dan Vicroy, NASA Langley Research Center, is acknowledged for making available the 3% blended wing-body model for the Boeing Low Speed Aeroacoustic Facility experiment. NR 18 TC 2 Z9 2 U1 0 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD DEC PY 2013 VL 51 IS 12 BP 2935 EP 2945 DI 10.2514/1.J052540 PG 11 WC Engineering, Aerospace SC Engineering GA AA8XK UT WOS:000331378100015 ER PT J AU Lawford, R Strauch, A Toll, D Fekete, B Cripe, D AF Lawford, Richard Strauch, Adrian Toll, David Fekete, Balazs Cripe, Douglas TI Earth observations for global water security SO CURRENT OPINION IN ENVIRONMENTAL SUSTAINABILITY LA English DT Review ID SOIL-MOISTURE; SEDIMENT BUDGET; MANAGEMENT TOOL; LAND; EVAPOTRANSPIRATION; MODEL; CALIBRATION; MICROWAVE; DISCHARGE; IMPACT AB The combined effects of population growth, increasing demands for water to support agriculture, energy security, and industrial expansion, and the challenges of climate change give rise to an urgent need to carefully monitor and assess trends and variations in water resources. Doing so will ensure that sustainable access to adequate quantities of safe and useable water will serve as a foundation for water security. Both satellite and in situ observations combined with data assimilation and models are needed for effective, integrated monitoring of the water cycle's trends and variability in terms of both quantity and quality. On the basis of a review of existing observational systems, we argue that a new integrated monitoring capability for water security purposes is urgently needed. Furthermore, the components for this capability exist and could be integrated through the cooperation of national observational programmes. The Group on Earth Observations should play a central role in the design, implementation, management and analysis of this system and its products. C1 [Lawford, Richard] Morgan State Univ, Baltimore, MD 21239 USA. [Strauch, Adrian] Univ Bonn, Bonn, Germany. [Toll, David] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fekete, Balazs] CUNY City Coll, Dept Civil Engn, New York, NY 10031 USA. [Fekete, Balazs] CUNY, Environm CrossRd Initiat, New York, NY 10021 USA. [Cripe, Douglas] Grp Earth Observat GEO Secretariat, Geneva, Switzerland. RP Lawford, R (reprint author), Morgan State Univ, Baltimore, MD 21239 USA. EM richard.lawford@morgan.edu FU JAXA; NASA; German Federal Ministry of Transport, Building and Urban Development [50.0355/2012] FX The authors wish to thank the editor and reviewers for their constructive comments on the article and to Dr. Paul Houser for his revised version of Figure 5 on land data assimilation. The lead author gratefully acknowledges the support of JAXA and NASA, which allowed him to carry out work related to the applications of Earth Observations in the Water domain. The second author would like to thank the 'German Federal Ministry of Transport, Building and Urban Development' (through the research project no. 50.0355/2012) for their support for his research which contributed to this article. NR 81 TC 9 Z9 9 U1 4 U2 27 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1877-3435 EI 1877-3443 J9 CURR OPIN ENV SUST JI Curr. Opin. Environ. Sustain. PD DEC PY 2013 VL 5 IS 6 BP 633 EP 643 DI 10.1016/j.cosust.2013.11.009 PG 11 WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Environmental Sciences SC Science & Technology - Other Topics; Environmental Sciences & Ecology GA AA5ON UT WOS:000331149400013 ER PT J AU Vogt, N Chene, AN Moffat, AFJ Matthews, JM Kuschnig, R Guenther, DB Rowe, JF Rucinski, SM Sasselov, D Weiss, WW AF Vogt, N. Chene, A-N. Moffat, A. F. J. Matthews, J. M. Kuschnig, R. Guenther, D. B. Rowe, J. F. Rucinski, S. M. Sasselov, D. Weiss, W. W. TI A photometric study of the nova-like variable TT Arietis with the MOST satellite SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE accretion, accretion disks; novae, cataclysmic variables; stars: activity; stars: individual (TT Ari) ID SUPERHUMPS; BEHAVIOR; DISK AB Variability on all time scales between seconds and decades is typical for cataclysmic variables (CVs). One of the brightest and best studied CVs is TTAri, a nova-like variable which belongs to the VY Scl subclass, characterized by occasional low states in their light curves. It is also known as a permanent superhumper at high state, revealing "positive" (P-S > P-0) as well as "negative" (P-S < P-0) superhumps, where P-S is the period of the superhump and P-0 the orbital period. TT Ari was observed by the Canadian space telescope MOST for about 230 hours nearly continuously in 2007, with a time resolution of 48 seconds. Here we analyze these data, obtaining a dominant "negative" superhump signal with a period P-S = 0.1331 days and a mean amplitude of 0.09 mag. Strong flickering with amplitudes up to 0.2 mag and peak-to-peak time scales of 15-20 minutes is superimposed on the periodic variations. We found no indications for significant quasi-periodic oscillations with periods around 15 minutes, reported by other authors. We discuss the known superhump behaviour of TTAri during the last five decades and conclude that our period value is at the upper limit of all hitherto determined "negative" superhump periods of TTAri, before and after the MOST run. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Vogt, N.; Chene, A-N.] Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile. [Chene, A-N.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Chene, A-N.] Gemini Observ, Northern Operat Ctr, Hilo, HI 96720 USA. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Moffat, A. F. J.] Ctr Rech Astrophys Quebec, Quebec City, PQ, Canada. [Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Rowe, J. F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rucinski, S. M.] Univ Toronto, Dept Astron Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Vogt, N (reprint author), Univ Valparaiso, Dept Fis & Astron, Av Gran Bretana 1111, Valparaiso, Chile. EM nikolaus.vogt@uv.cl FU project Gemini-CONICYT [32090027, DIUV 38/2011]; Chilean Centro de Astrofisica FONDAP [15010003]; Chilean Centro de Excelencia en Astrofisica y Tecnologias Afines (CATA) BASAL [PFB-06/2007]; Comite Mixto ESO-Gobierno de Chile; GEMINI-CONICYT [32110005]; NSERC (Canada); Austrian Science Fonds [FWF P22691-N16] FX NV acknowledges the support by project Gemini-CONICYT 32090027 and DIUV 38/2011. ANC gratefully acknowledges support from the Chilean Centro de Astrofisica FONDAP No. 15010003, the Chilean Centro de Excelencia en Astrofisica y Tecnologias Afines (CATA) BASAL PFB-06/2007, the Comite Mixto ESO-Gobierno de Chile and GEMINI-CONICYT No. 32110005. DBG, JMM, AFJM and SMR acknowledge financial support from NSERC (Canada) and for AFJM also FQRNT (Quebec). RK and WWW acknowledge support by the Austrian Science Fonds (FWF P22691-N16). NR 18 TC 3 Z9 3 U1 0 U2 3 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD DEC PY 2013 VL 334 IS 10 BP 1101 EP 1106 DI 10.1002/asna.201311949 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 297GI UT WOS:000330243400004 ER PT J AU Rawlins, MA Nicolsky, DJ McDonald, KC Romanovsky, VE AF Rawlins, M. A. Nicolsky, D. J. McDonald, K. C. Romanovsky, V. E. TI Simulating soil freeze/thaw dynamics with an improved pan-Arctic water balance model SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS LA English DT Article ID INTERNATIONAL POLAR YEAR; ACTIVE-LAYER THICKNESS; SEASONAL SNOW COVER; THERMAL STATE; DRAINAGE-BASIN; PERMAFROST; ALASKA; CONDUCTIVITY; TEMPERATURE; REANALYSIS AB The terrestrial Arctic water cycle is strongly influenced by the presence of permafrost, which is at present degrading as a result of warming. In this study, we describe improvements to the representation of processes in the pan-Arctic Water Balance Model (PWBM) and evaluate simulated soil temperature at four sites in Alaska and active-layer thickness (ALT) across the pan-Arctic drainage basin. Model improvements include new parameterizations for thermal and hydraulic properties of organic soils; an updated snow model, which accounts for seasonal changes in density and thermal conductivity; and a new soil freezing and thawing model, which simulates heat conduction with phase change. When compared against observations across Alaska within differing landscape vegetation conditions in close proximity to one another, PWBM simulations show no systematic soil temperature bias. Simulated temperatures agree well with observations in summer. In winter, results are mixed, with both positive and negative biases noted at times. In two pan-Arctic simulations forced with atmospheric reanalysis, the model captures the mean in observed ALT, although predictability as measured by correlation is limited. The geographic pattern in northern hemisphere permafrost area is well estimated. Simulated permafrost area differs from observed extent by 7 and 17% for the two model runs. Results of two simulations for the periods 1996-1999 and 2066-2069 for a single grid cell in central Alaska illustrate the potential for a drying of soils in the presence of increases in ALT, annual total precipitation, and winter snowfall. C1 [Rawlins, M. A.] Univ Massachusetts, Dept Geosci, Amherst, MA 01003 USA. [Nicolsky, D. J.; Romanovsky, V. E.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [McDonald, K. C.] CUNY, Dept Earth & Atmospher Sci, New York, NY 10021 USA. [McDonald, K. C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Rawlins, MA (reprint author), Univ Massachusetts, Climate Syst Res Ctr, Dept Geosci, 611 North Pleasant St, Amherst, MA 01002 USA. EM rawlins@geo.umass.edu FU U.S. National Aeronautics and Space Administration NASA [NNX11AR16G]; National Science Foundation (NSF); U.S. Department of Energy (DoE); National Oceanic and Atmospheric Administration (NOAA); U.S. Environmental Protection Agency Office of Research and Development (EPA) FX This research was supported by the U.S. National Aeronautics and Space Administration NASA grant (NNX11AR16G). The authors thank two anonymous reviewers and the Associate Editor for their constructive comments. We thank the North American Regional Climate Change Assessment Program (NARCCAP) for providing data used in this paper. NARCCAP is funded by the National Science Foundation (NSF), the U.S. Department of Energy (DoE), the National Oceanic and Atmospheric Administration (NOAA), and the U.S. Environmental Protection Agency Office of Research and Development (EPA). Portions of this work were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 63 TC 7 Z9 7 U1 0 U2 19 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1942-2466 J9 J ADV MODEL EARTH SY JI J. Adv. Model. Earth Syst. PD DEC PY 2013 VL 5 IS 4 BP 659 EP 675 DI 10.1002/jame.20045 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AA1BZ UT WOS:000330832600001 ER PT J AU Kinne, S O'Donnel, D Stier, P Kloster, S Zhang, K Schmidt, H Rast, S Giorgetta, M Eck, TF Stevens, B AF Kinne, Stefan O'Donnel, Declan Stier, Philip Kloster, Silvia Zhang, Kai Schmidt, Hauke Rast, Sebastian Giorgetta, Marco Eck, Tom F. Stevens, Bjorn TI MAC-v1: A new global aerosol climatology for climate studies SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS LA English DT Article ID SKY RADIANCE MEASUREMENTS; OPTICAL-PROPERTIES; TRANSPORT MODEL; SATELLITE; NETWORK; SUN; EMISSIONS; PRODUCTS; AEROCOM; DEPTH AB The Max-Planck-Institute Aerosol Climatology version 1 (MAC-v1) is introduced. It describes the optical properties of tropospheric aerosols on monthly timescales and with global coverage at a spatial resolution of 1 degrees in latitude and longitude. By providing aerosol radiative properties for any wavelength of the solar (or shortwave) and of the terrestrial (or longwave) radiation spectrum, as needed in radiative transfer applications, this MAC-v1 data set lends itself to simplified and computationally efficient representations of tropospheric aerosol in climate studies. Estimates of aerosol radiative properties are provided for both total and anthropogenic aerosol in annual time steps from preindustrial times (i.e., starting with year 1860) well into the future (until the year 2100). Central to the aerosol climatology is the merging of monthly statistics of aerosol optical properties for current (year 2000) conditions. Hereby locally sparse but trusted high-quality data by ground-based sun-photometer networks are merged onto complete background maps defined by central data from global modeling with complex aerosol modules. This merging yields 0.13 for the global annual midvisible aerosol optical depth (AOD), with 0.07 attributed to aerosol sizes larger than 1 mu m in diameter and 0.06 of attributed to aerosol sizes smaller than 1 mm in diameter. Hereby larger particles are less absorbing with a single scattering albedo (SSA) of 0.98 compared to 0.93 for smaller sizes. Simulation results of a global model are applied to prescribe the vertical distribution and to estimate anthropogenic contributions to the smaller size AOD as a function of time, with a 0.037 value for current conditions. In a demonstration application, the associated aerosol direct radiative effects are determined. For current conditions, total aerosol is estimated to reduce the combined shortwave and longwave net-flux balance at the top of the atmosphere by about -1.6 W/m(2) from which -0.5 W/m(2) (with an uncertainty of +/- 0.2 W/m(2)) is attributed to anthropogenic activities. Based on past and projected aerosol emission data, the global anthropogenic direct aerosol impact (i.e., ToA cooling) is currently near the maximum and is projected to drop by 2100 to about -0.3 W/m(2). The reported global averages are driven by considerable spatial and temporal variability. To better convey this diversity, regional and seasonal distributions of aerosol optical properties and their radiative effects are presented. On regional scales, the anthropogenic direct aerosol forcing can be an order of magnitude stronger than the global average and it can be of either sign. It is also shown that maximum anthropogenic impacts have shifted during the last 30 years from the U.S. and Europe to eastern and southern Asia. C1 [Kinne, Stefan; Kloster, Silvia; Zhang, Kai; Schmidt, Hauke; Rast, Sebastian; Giorgetta, Marco; Stevens, Bjorn] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [O'Donnel, Declan] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Stier, Philip] Univ Oxford, Dept Phys, Oxford, England. [Zhang, Kai] Pacific North Natl Lab, Dept Climate Phys, Richland, WA USA. [Eck, Tom F.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Eck, Tom F.] Univ Space Res Assoc, GESTAR, Columbia, MD USA. RP Kinne, S (reprint author), Max Planck Inst Meteorol, Bundesstr 53, D-20146 Hamburg, Germany. EM stefan.kinne@zmaw.de RI Stevens, Bjorn/A-1757-2013; Zhang, Kai/F-8415-2010; Stier, Philip/B-2258-2008 OI Stevens, Bjorn/0000-0003-3795-0475; Zhang, Kai/0000-0003-0457-6368; Stier, Philip/0000-0002-1191-0128 FU EU FX The AeroCom global modeling effort was essential to this study, as the model median provides the starting point for the new aerosol climatology. Thus, the work of all global modeling groups that contributed to AeroCom is acknowledged. Important remote sensing data were provided by many satellite retrievals groups and by the AERONET group at NASA-GSFC with particular assistance by Dave Giles and Ilya Slutsker. Also acknowledged is the support for Stefan Kinne by several, past and current, EU-projects, including MACC, MACC-2, EUCAARI, and ACTRIS. The aerosol properties described in this contribution are available on anonymous ftp://ftp-projects.zmaw.de cd aerocom/climatology/HACv1_2013/. (Contacting the first author is strongly recommended before pulling data from that ftp-site.) NR 59 TC 36 Z9 36 U1 2 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1942-2466 J9 J ADV MODEL EARTH SY JI J. Adv. Model. Earth Syst. PD DEC PY 2013 VL 5 IS 4 BP 704 EP 740 DI 10.1002/jame.20035 PG 37 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AA1BZ UT WOS:000330832600004 ER PT J AU Zhang, MH Bretherton, CS Blossey, PN Austin, PH Bacmeister, JT Bony, S Brient, F Cheedela, SK Cheng, AN Del Genio, AD De Roode, SR Endo, S Franklin, CN Golaz, JC Hannay, C Heus, T Isotta, FA Dufresne, JL Kang, IS Kawai, H Kohler, M Larson, VE Liu, YG Lock, AP Lohmann, U Khairoutdinov, MF Molod, AM Neggers, RAJ Rasch, P Sandu, I Senkbeil, R Siebesma, AP Siegenthaler-Le Drian, C Stevens, B Suarez, MJ Xu, KM von Salzen, K Webb, MJ Wolf, A Zhao, M AF Zhang, Minghua Bretherton, Christopher S. Blossey, Peter N. Austin, Phillip H. Bacmeister, Julio T. Bony, Sandrine Brient, Florent Cheedela, Suvarchal K. Cheng, Anning Del Genio, Anthony D. De Roode, Stephan R. Endo, Satoshi Franklin, Charmaine N. Golaz, Jean-Christophe Hannay, Cecile Heus, Thijs Isotta, Francesco Alessandro Dufresne, Jean-Louis Kang, In-Sik Kawai, Hideaki Koehler, Martin Larson, Vincent E. Liu, Yangang Lock, Adrian P. Lohmann, Ulrike Khairoutdinov, Marat F. Molod, Andrea M. Neggers, Roel A. J. Rasch, Philip Sandu, Irina Senkbeil, Ryan Siebesma, A. Pier Siegenthaler-Le Drian, Colombe Stevens, Bjorn Suarez, Max J. Xu, Kuan-Man von Salzen, Knut Webb, Mark J. Wolf, Audrey Zhao, Ming TI CGILS: Results from the first phase of an international project to understand the physical mechanisms of low cloud feedbacks in single column models SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS LA English DT Article ID GENERAL-CIRCULATION MODELS; GLOBAL CLIMATE MODEL; COMMUNITY ATMOSPHERE MODEL; SHALLOW CUMULUS CLOUDS; BOUNDARY-LAYER CLOUDS; MASS FLUX FRAMEWORK; PDF-BASED MODEL; PART I; MOIST CONVECTION; PARAMETERIZATION AB CGILS-the CFMIP-GASS Intercomparison of Large Eddy Models (LESs) and single column models (SCMs)-investigates the mechanisms of cloud feedback in SCMs and LESs under idealized climate change perturbation. This paper describes the CGILS results from 15 SCMs and 8 LES models. Three cloud regimes over the subtropical oceans are studied: shallow cumulus, cumulus under stratocumulus, and well-mixed coastal stratus/stratocumulus. In the stratocumulus and coastal stratus regimes, SCMs without activated shallow convection generally simulated negative cloud feedbacks, while models with active shallow convection generally simulated positive cloud feedbacks. In the shallow cumulus alone regime, this relationship is less clear, likely due to the changes in cloud depth, lateral mixing, and precipitation or a combination of them. The majority of LES models simulated negative cloud feedback in the well-mixed coastal stratus/stratocumulus regime, and positive feedback in the shallow cumulus and stratocumulus regime. A general framework is provided to interpret SCM results: in a warmer climate, the moistening rate of the cloudy layer associated with the surface-based turbulence parameterization is enhanced; together with weaker large-scale subsidence, it causes negative cloud feedback. In contrast, in the warmer climate, the drying rate associated with the shallow convection scheme is enhanced. This causes positive cloud feedback. These mechanisms are summarized as the "NESTS" negative cloud feedback and the "SCOPE" positive cloud feedback (Negative feedback from Surface Turbulence under weaker Subsidence-Shallow Convection PositivE feedback) with the net cloud feedback depending on how the two opposing effects counteract each other. The LES results are consistent with these interpretations. C1 [Zhang, Minghua; Khairoutdinov, Marat F.] SUNY Stony Brook, Inst Terr & Planetary Atmospheres, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. [Bretherton, Christopher S.; Blossey, Peter N.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Austin, Phillip H.] Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC V5Z 1M9, Canada. [Bacmeister, Julio T.; Hannay, Cecile] Natl Ctr Atmospher Res, Earth Syst Lab, Boulder, CO 80307 USA. [Bony, Sandrine; Brient, Florent; Dufresne, Jean-Louis] IPSL, Lab Meteorol Dynam, Paris, France. [Cheedela, Suvarchal K.; Heus, Thijs; Sandu, Irina; Stevens, Bjorn] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Cheng, Anning; Xu, Kuan-Man] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [De Roode, Stephan R.] Delft Univ Technol, Dept Geosci & Remote Sensing, Delft, Netherlands. [Endo, Satoshi; Liu, Yangang] Brookhaven Natl Lab, Dept Environm Sci, Upton, NY 11973 USA. [Franklin, Charmaine N.] CSIRO, Ctr Australian Weather & Climate Res, Aspendale, Vic, Australia. [Golaz, Jean-Christophe; Zhao, Ming] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. [Isotta, Francesco Alessandro; Lohmann, Ulrike; Siegenthaler-Le Drian, Colombe] Swiss Fed Inst Technol, Zurich, Switzerland. [Kang, In-Sik] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea. [Kawai, Hideaki] Meteorol Res Inst, Tsukuba, Ibaraki 305, Japan. [Koehler, Martin; Sandu, Irina] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. [Larson, Vincent E.; Senkbeil, Ryan] Univ Wisconsin, Dept Math Sci, Milwaukee, WI 53201 USA. [Lock, Adrian P.; Webb, Mark J.] Met Off Hadley Ctr, Exeter, Devon, England. [Molod, Andrea M.; Suarez, Max J.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD USA. [Neggers, Roel A. J.; Siebesma, A. Pier] Royal Netherlands Meteorol Inst KNMI, Div Atmospher Res, De Bilt, Netherlands. [Rasch, Philip] Pacific NW Natl Lab, Richland, WA 99352 USA. [von Salzen, Knut] Canadian Ctr Climate Modelling & Anal, Victoria, BC, Canada. [Wolf, Audrey] Columbia Univ, Goddard Inst Space Studies, New York, NY USA. RP Zhang, MH (reprint author), SUNY Stony Brook, Inst Terr & Planetary Atmospheres, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. EM minghua.zhang@stonybrook.edu RI Stevens, Bjorn/A-1757-2013; Golaz, Jean-Christophe/D-5007-2014; Liu, Yangang/H-6154-2011; Dufresne, Jean-Louis/I-5616-2015; Zhao, Ming/C-6928-2014; Heus, Thijs/E-7336-2012; Lohmann, Ulrike/B-6153-2009; Xu, Kuan-Man/B-7557-2013; 안, 민섭/D-9972-2015 OI Stevens, Bjorn/0000-0003-3795-0475; Bony, Sandrine/0000-0002-4791-4438; Golaz, Jean-Christophe/0000-0003-1616-5435; Dufresne, Jean-Louis/0000-0003-4764-9600; Heus, Thijs/0000-0003-2650-2423; Lohmann, Ulrike/0000-0001-8885-3785; Xu, Kuan-Man/0000-0001-7851-2629; FU Biological and Environmental Research Division in the Office of Sciences of the US Department of Energy (DOE) through its FASTER project; NASA Modeling and Analysis Program (MAP); US National Science Foundation; NSF Center for Multiscale Modeling and Prediction; Canada's NSERC; NASA MAP program; National Science Foundation [AGS-0968640]; US Department of Energy [DE-SC0006927]; DOE ASR program; Joint DECC/Defra Met Office Hadley Centre Climate Program [GA01101]; European Union [244067]; Australian Climate Change Science Program; Department of Climate Change and Energy Efficiency; Bureau of Meteorology; CSIRO; Deutscher Wetter Dienst (DWD) through the Hans-Ertel Centre for Weather Research, as part of the EUCLIPSE project under Framework Program 7 of the European Union; National Computing Facilities Foundation (NCF); National Science Foundation FX We thank two anonymous reviewers whose comments have led to a significant improvement of this paper. Sung-bin Park of the Seoul National University (SNU) participated in the initial phase of the CGILS project. His tragic death disrupted the submission of results from the SNU model. This paper serves as an appreciation and memory of him. Zhang's CGILS research is supported by the Biological and Environmental Research Division in the Office of Sciences of the US Department of Energy (DOE) through its FASTER project, by the NASA Modeling and Analysis Program (MAP) and the US National Science Foundation to the Stony Brook University. Bretherton and Blossey acknowledge support from the NSF Center for Multiscale Modeling and Prediction, Austin is supported by Canada's NSERC. Del Genio is supported by the NASA MAP program. V. Larson gratefully acknowledges support from the National Science Foundation (grant AGS-0968640) and the US Department of Energy (grant DE-SC0006927). Wolf was supported by the DOE ASR program. Webb was supported by the Joint DECC/Defra Met Office Hadley Centre Climate Program (GA01101) and funding from the European Union, Seventh Framework Program (FP7/2007-2013) under grant agreement number 244067 via the EU CLoud Intercomparison and Process Study Evaluation Project (EUCLIPSE). Franklin was supported by the Australian Climate Change Science Program, funded jointly by the Department of Climate Change and Energy Efficiency, the Bureau of Meteorology and CSIRO. Heus was funded by the Deutscher Wetter Dienst (DWD) through the Hans-Ertel Centre for Weather Research, as part of the EUCLIPSE project under Framework Program 7 of the European Union. The simulations with the Dutch LES model were sponsored by the National Computing Facilities Foundation (NCF). The National Center for Atmospheric Research is sponsored by the National Science Foundation. NR 75 TC 37 Z9 37 U1 0 U2 39 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1942-2466 J9 J ADV MODEL EARTH SY JI J. Adv. Model. Earth Syst. PD DEC PY 2013 VL 5 IS 4 BP 826 EP 842 DI 10.1002/2013MS000246 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AA1BZ UT WOS:000330832600011 ER PT J AU Koepke, ME Walker, JJ Zimmerman, MI Farrell, WM Demidov, VI AF Koepke, Mark E. Walker, J. J. Zimmerman, M. I. Farrell, W. M. Demidov, V. I. TI Signature of gyro-phase drift SO JOURNAL OF PLASMA PHYSICS LA English DT Article ID DUST GRAINS; PLASMA; PARTICLES; RING AB Gyro-phase drift is a guiding center drift that is directly dependent on the charging rate limit of dust grains. The effect of introducing a gyro-phase-dependence on the grain charge leads to two orthogonal components of guiding-center drift. One component, referred to here as grad-q drift, results from the time-varying, gyro-phase angle dependent, in-situ-equilibrium grain charge, assuming that the grain charging is instantaneous. For this component, the grain is assumed to be always in its in-situ-equilibrium charge state and this state gyro-synchronously varies with respect to the grain's average charge state. The other component, referred to here as the gyro-phase drift, arises from any non-instantaneous-charging-induced modification of the diamagnetic drift and points in the direction of -del R-Ld (where R-Ld is the grain gyro-radius), i.e. the direction associated with increasing magnitude of in-situ-equilibrium charge state. For this component, the grain gyro-synchronously undercharges and overcharges with respect to its gyro-synchronously varying, in-situ-equilibrium charge state. These characteristics are illustrated with a single-particle code for predicting grain trajectory that demonstrates how gyro-phase drift magnitude and direction could be exploited, using an extended version of the presented model, as sensitive indicators of the charging time of dust grains because of the cumulative effect of the ever-changing charge state of a grain making repeated excursions in inhomogeneous plasma over many gyro-periods. C1 [Koepke, Mark E.; Walker, J. J.; Demidov, V. I.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Zimmerman, M. I.; Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Demidov, V. I.] Univ ITMO, St Petersburg 197101, Russia. RP Koepke, ME (reprint author), W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. EM mark.koepke@mail.wvu.edu RI Demidov, Vladimir/A-4247-2013; Farrell, William/I-4865-2013 OI Demidov, Vladimir/0000-0002-2672-7684; FU U.S. Department of Energy, Office of Fusion Energy Science [DE-SC0001939] FX Funding through the U.S. Department of Energy, Office of Fusion Energy Science grant DE-SC0001939 and useful discussions with Dr. Marlene Rosenberg are gratefully acknowledged. NR 15 TC 1 Z9 1 U1 1 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-3778 EI 1469-7807 J9 J PLASMA PHYS JI J. Plasma Phys. PD DEC PY 2013 VL 79 BP 1099 EP 1105 DI 10.1017/S0022377813001128 PN 6 PG 7 WC Physics, Fluids & Plasmas SC Physics GA 300NE UT WOS:000330469800026 ER PT J AU Repasky, KS Moen, D Spuler, S Nehrir, AR Carlsten, JL AF Repasky, Kevin S. Moen, Drew Spuler, Scott Nehrir, Amin R. Carlsten, John L. TI Progress towards an Autonomous Field Deployable Diode-Laser-Based Differential Absorption Lidar (DIAL) for Profiling Water Vapor in the Lower Troposphere SO REMOTE SENSING LA English DT Article DE DIAL; trace gas sensing; ground-based lidar ID RAMAN LIDAR; PERFORMANCE; AIRBORNE; AEROSOLS; SYSTEM AB A laser transmitter has been developed and incorporated into a micro-pulse differential absorption lidar (DIAL) for water vapor profiling in the lower troposphere as an important step towards long-term autonomous field operation. The laser transmitter utilizes two distributed Bragg reflector (DBR) diode lasers to injection seed a pulsed tapered semiconductor optical amplifier (TSOA), and is capable of producing up to 10 mu J of pulse energy with a 1 mu s pulse duration and a 10 kHz pulse repetition frequency. The on-line wavelength of the laser transmitter can operate anywhere along the water vapor absorption feature centered at 828.187 nm (in vacuum) depending on the prevailing atmospheric conditions, while the off-line wavelength operates at 828.287 nm. This laser transmitter has been incorporated into a DIAL instrument utilizing a 35.6 cm Schmidt-Cassegrain telescope and fiber coupled avalanche photodiode (APD) operating in the photon counting mode. The performance of the DIAL instrument was demonstrated over a ten-day observation period. During this observation period, data from radiosondes were used to retrieve water vapor number density profiles for comparisons with the number density profiles retrieved from the DIAL data. C1 [Repasky, Kevin S.; Moen, Drew] Montana State Univ, Bozeman, MT 59717 USA. [Spuler, Scott] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Nehrir, Amin R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Carlsten, John L.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. RP Repasky, KS (reprint author), Montana State Univ, Bozeman, MT 59717 USA. EM repasky@ece.montana.edu; drew.moen@msu.montana.edu; spuler@ucar.edu; amin.r.nehrir@nasa.gov; carlsten@physics.montana.edu FU National Science Foundation [1206166] FX This work was supported under the kind auspices of the National Science Foundation grant number 1206166. NR 29 TC 8 Z9 8 U1 3 U2 19 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD DEC PY 2013 VL 5 IS 12 BP 6241 EP 6259 DI 10.3390/rs5126241 PG 19 WC Remote Sensing SC Remote Sensing GA 298JB UT WOS:000330318900005 ER PT J AU Devred, E Turpie, KR Moses, W Klemas, VV Moisan, T Babin, M Toro-Farmer, G Forget, MH Jo, YH AF Devred, Emmanuel Turpie, Kevin R. Moses, Wesley Klemas, Victor V. Moisan, Tiffany Babin, Marcel Toro-Farmer, Gerardo Forget, Marie-Helene Jo, Young-Heon TI Future Retrievals of Water Column Bio-Optical Properties using the Hyperspectral Infrared Imager (HyspIRI) SO REMOTE SENSING LA English DT Article DE hyperspectral remote sensing; phytoplankton; absorption; ocean optics ID INHERENT OPTICAL-PROPERTIES; DIFFUSE ATTENUATION COEFFICIENTS; TURBID PRODUCTIVE WATERS; FLORIDA COASTAL WATERS; SATELLITE OCEAN COLOR; CHLOROPHYLL-A; ABSORPTION-SPECTRA; PIGMENT CONCENTRATIONS; REMOTE ESTIMATION; NEURAL-NETWORK AB Interpretation of remote sensing reflectance from coastal waters at different wavelengths of light yields valuable information about water column constituents, which in turn, gives information on a variety of processes occurring in coastal waters, such as primary production, biogeochemical cycles, sediment transport, coastal erosion, and harmful algal blooms. The Hyperspectral Infrared Imager (HyspIRI) is well suited to produce global, seasonal maps and specialized observations of coastal ecosystems and to improve our understanding of how phytoplankton communities are spatially distributed and structured, and how they function in coastal and inland waters. This paper draws from previously published studies on high-resolution, hyperspectral remote sensing of coastal and inland waters and provides an overview of how the HyspIRI mission could enable the retrieval of new aquatic biophysical products or improve the retrieval accuracy of existing satellite-derived products (e.g., inherent optical properties, phytoplankton functional types, pigment composition, chlorophyll-a concentration, etc.). The intent of this paper is to introduce the development of the HyspIRI mission to the coastal and inland remote sensing community and to provide information regarding several potential data products that were not originally part of the HyspIRI mission objectives but could be applicable to research related to coastal and inland waters. Further work toward quantitatively determining the extent and quality of these products, given the instrument and mission characteristics, is recommended. C1 [Devred, Emmanuel; Babin, Marcel; Forget, Marie-Helene] Univ Laval, CNRS & U Laval, Dept Biol, Quebec City G1V 0A6, PQ, Canada. [Turpie, Kevin R.] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Moses, Wesley] Naval Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Klemas, Victor V.; Jo, Young-Heon] Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA. [Moisan, Tiffany] NASA, Wallops Flight Facil, Wallops Isl, VA 23337 USA. [Toro-Farmer, Gerardo] Univ S Florida, Coll Marine Sci, Inst Marine Remote Sensing, St Petersburg, FL 33701 USA. [Jo, Young-Heon] Pusan Natl Univ, Pusan 609735, South Korea. RP Turpie, KR (reprint author), Univ Maryland, Joint Ctr Earth Syst Technol, 5523 Res Pk Dr, Baltimore, MD 21250 USA. EM emmanuel.devred@takuvik.ulaval.ca; kevin.r.turpie@nasa.gov; wesley.moses@nrl.navy.mil; klemas@udel.edu; tiffany.a.moisan@nasa.gov; marcel.babin@takuvik.ulaval.ca; torofarmer@mail.usf.edu; marie-helene.forget@takuvik.ulaval.ca; joyoung@udel.eduapk OI Moses, Wesley/0000-0003-3551-6093 FU HyspIRI project FX We are grateful for the input provided by members of the HyspIRI Aquatic Study Group and for the support of the HyspIRI project in the development of this paper. NR 118 TC 21 Z9 21 U1 4 U2 34 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD DEC PY 2013 VL 5 IS 12 BP 6812 EP 6837 DI 10.3390/rs5126812 PG 26 WC Remote Sensing SC Remote Sensing GA 298JB UT WOS:000330318900030 ER PT J AU Cheng, YB Middleton, EM Zhang, QY Huemmrich, KF Campbell, PKE Corp, LA Cook, BD Kustas, WP Daughtry, CS AF Cheng, Yen-Ben Middleton, Elizabeth M. Zhang, Qingyuan Huemmrich, Karl F. Campbell, Petya K. E. Corp, Lawrence A. Cook, Bruce D. Kustas, William P. Daughtry, Craig S. TI Integrating Solar Induced Fluorescence and the Photochemical Reflectance Index for Estimating Gross Primary Production in a Cornfield SO REMOTE SENSING LA English DT Article DE gross primary production; light use efficiency; photochemical reflectance index; solar induced fluorescence; cornfield ID LIGHT-USE-EFFICIENCY; INDUCED CHLOROPHYLL FLUORESCENCE; RADIATION-USE-EFFICIENCY; VEGETATION APPARENT REFLECTANCE; PHOTOSYNTHETIC DOWN-REGULATION; SUN-INDUCED FLUORESCENCE; LEAF PIGMENT CONTENT; WATER-STRESS; SPECTRAL REFLECTANCE; XANTHOPHYLL CYCLE AB The utilization of remotely sensed observations for light use efficiency (LUE) and tower-based gross primary production (GPP) estimates was studied in a USDA cornfield. Nadir hyperspectral reflectance measurements were acquired at canopy level during a collaborative field campaign conducted in four growing seasons. The Photochemical Reflectance Index (PRI) and solar induced chlorophyll fluorescence (SIF), were derived. SIF retrievals were accomplished in the two telluric atmospheric oxygen absorption features centered at 688 nm (O-2-B) and 760 nm (O-2-A). The PRI and SIF were examined in conjunction with GPP and LUE determined by flux tower-based measurements. All of these fluxes, environmental variables, and the PRI and SIF exhibited diurnal as well as day-to-day dynamics across the four growing seasons. Consistent with previous studies, the PRI was shown to be related to LUE (r(2) = 0.54 with a logarithm fit), but the relationship varied each year. By combining the PRI and SIF in a linear regression model, stronger performances for GPP estimation were obtained. The strongest relationship (r(2) = 0.80, RMSE = 0.186 mg CO2/m(2)/s) was achieved when using the PRI and SIF retrievals at 688 nm. Cross-validation approaches were utilized to demonstrate the robustness and consistency of the performance. This study highlights a GPP retrieval method based entirely on hyperspectral remote sensing observations. C1 [Cheng, Yen-Ben] Earth Resources Technol Inc, Laurel, MD 20707 USA. [Middleton, Elizabeth M.; Cook, Bruce D.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Zhang, Qingyuan] Univ Space Res Assoc, Columbia, MD 21044 USA. [Huemmrich, Karl F.; Campbell, Petya K. E.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Corp, Lawrence A.] Sigma Space Corp, Lanham, MD 20706 USA. [Kustas, William P.; Daughtry, Craig S.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. RP Cheng, YB (reprint author), Earth Resources Technol Inc, Laurel, MD 20707 USA. EM yen-ben.cheng@nasa.gov; elizabeth.m.middleton@nasa.gov; qingyuan.zhang-1@nasa.gov; karl.f.huemmrich@nasa.gov; petya.k.campbell@nasa.gov; lawrence.a.corp@nasa.gov; bruce.cook@nasa.gov; bill.kustas@ars.usda.gov; craig.daughtry@ars.usda.gov RI Kustas, William/C-2063-2015; Campbell, Petya/L-7486-2013 OI Campbell, Petya/0000-0002-0505-4951 FU NASA ROSES project; Terrestrial Ecology Program FX This study was supported by a NASA ROSES project (PI, E.M. Middleton) funded through the Terrestrial Ecology Program (Diane Wickland, Program Manager). The authors gratefully acknowledge Andrew Russ and Wayne Dulaney (USDA-ARS Hydrology and Remote Sensing Lab) for assisting field campaign and data processing. The authors thank the anonymous reviewers for their very valuable suggestions and critiques. NR 108 TC 21 Z9 21 U1 3 U2 43 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD DEC PY 2013 VL 5 IS 12 BP 6857 EP 6879 DI 10.3390/rs5126857 PG 23 WC Remote Sensing SC Remote Sensing GA 298JB UT WOS:000330318900032 ER PT J AU Ngwira, CM Pulkkinen, A Mays, ML Kuznetsova, MM Galvin, AB Simunac, K Baker, DN Li, XL Zheng, YH Glocer, A AF Ngwira, Chigomezyo M. Pulkkinen, Antti Mays, M. Leila Kuznetsova, Maria M. Galvin, A. B. Simunac, Kristin Baker, Daniel N. Li, Xinlin Zheng, Yihua Glocer, Alex TI Simulation of the 23 July 2012 extreme space weather event: What if this extremely rare CME was Earth directed? SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID CORONAL MASS EJECTION; MHD SIMULATION; SOLAR-WIND; MAGNETOSPHERE; SYSTEM; MODEL; MISSION C1 [Ngwira, Chigomezyo M.; Mays, M. Leila] Catholic Univ Amer, Dept Phys, Greenbelt, MD 20771 USA. [Ngwira, Chigomezyo M.; Pulkkinen, Antti; Mays, M. Leila; Kuznetsova, Maria M.; Zheng, Yihua; Glocer, Alex] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Galvin, A. B.; Simunac, Kristin] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Baker, Daniel N.; Li, Xinlin] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. RP Ngwira, CM (reprint author), Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Code 674,Bldg 21 Room 159, Greenbelt, MD 20771 USA. EM chigongwira@yahoo.co.uk RI Glocer, Alex/C-9512-2012; ngwira, chigomezyo/D-7310-2012 OI Glocer, Alex/0000-0001-9843-9094; FU EPRI [EPRI-18403]; NASA [NAS5-00132] FX Authors acknowledge Mei-Ching Fok and Ja Soon Shim for useful discussions. All SWMF/WSA-ENLIL simulations were performed through the runs-on-request system at the CCMC located at NASA Goddard Space Flight Center. The SMWF/BATS-R-US Model was developed at the University of Michigan. SOHO is a mission of international cooperation between the European Space Agency and NASA. C. M. Ngwira is supported by EPRI under contract EPRI-18403, while A. B. Galvin and K. Simunac are supported by NASA grant NAS5-00132. The authors also thank their EURISGIC partners (European Risk from Geomagnetically Induced Currents), an EU/FP7 Space Research project, for useful discussions on this work. NR 38 TC 26 Z9 26 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD DEC PY 2013 VL 11 IS 12 BP 671 EP 679 PG 9 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 304JQ UT WOS:000330743300001 ER PT J AU Volkov, DL Landerer, FW AF Volkov, Denis L. Landerer, Felix W. TI Nonseasonal fluctuations of the Arctic Ocean mass observed by the GRACE satellites SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE Arctic Ocean; GRACE; ocean mass; sea level; nonseasonal variability; ECCO2 ID SEA-LEVEL VARIABILITY; MEDITERRANEAN SEA; NORDIC SEAS; CIRCULATION; REANALYSIS; DYNAMICS; SYSTEM; MODEL; BASIN AB Time variable gravity observations from the GRACE satellites reveal strong nonseasonal fluctuations of bottom pressure in the Arctic Ocean on the time scales from 2 to 6 months and a record-high bottom pressure anomaly in February of 2011. Here, we examine the nature and driving forces behind those fluctuations. We find that the nonseasonal variability of the Arctic Ocean mass is strongly coupled to wind forcing. The zonal wind pattern is correlated with a dipole pattern of Arctic Ocean mass changes. Westerly wind intensification over the North Atlantic at about 60 degrees N as well as over the Russian Arctic continental shelf break cause the ocean mass to decrease in the Nordic seas and in the central Arctic, and to increase over the Russian Arctic shelf. Basin-wide Arctic Ocean mass fluctuations are correlated with northward wind anomalies over the northeastern North Atlantic and Nordic seas, and over the Bering Sea. We show that positive (negative) Arctic Ocean mass anomalies are associated with anticyclonic (cyclonic) anomalies of the large-scale ocean circulation pattern. Based on ocean model simulations, we conclude that the observed nonseasonal Arctic Ocean mass variability is mostly explained by the net horizontal wind-driven transports, and the contribution of fresh water fluxes is negligible. We demonstrate that transport anomalies across both the Atlantic and Pacific gateways were equally important for generating large Arctic Ocean mass anomalies in 2011. C1 [Volkov, Denis L.] Univ Miami, Cooperat Inst Marine & Atmospher Studies, Miami, FL 33149 USA. [Volkov, Denis L.] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA. [Landerer, Felix W.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Volkov, DL (reprint author), Univ Miami, Cooperat Inst Marine & Atmospher Studies, 4301 Rickenbacker Causeway, Miami, FL 33149 USA. EM Denis.Volkov@noaa.gov RI Volkov, Denis/A-6079-2011; OI Volkov, Denis/0000-0002-9290-0502; Landerer, Felix/0000-0003-2678-095X FU NASA Physical Oceanography program [NNX11AE27G] FX The ECCO2 model runs have been carried out at Jet Propulsion Laboratory, California Institute of Technology (http://ecco2.jpl.nasa.gov). GRACE ocean data were processed by Don P. Chambers, supported by the NASA MEASURES Program, and are available at http://grace.jpl.nasa.gov. The authors thank James Morison, Andrey Proshutinsky, Molly Baringer, Sang-Ki Lee, and an anonymous reviewer for their comments and suggestions that helped to improve the manuscript. This research was funded by the NASA Physical Oceanography program (grant NNX11AE27G) and carried out at the NOAA Atlantic Oceanographic and Meteorological Laboratory and Jet Propulsion Laboratory, California Institute of Technology. NR 34 TC 13 Z9 14 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC PY 2013 VL 118 IS 12 BP 6451 EP 6460 DI 10.1002/2013JC009341 PG 10 WC Oceanography SC Oceanography GA 292TU UT WOS:000329926200009 ER PT J AU Moon, JH Song, YT Bromirski, PD Miller, AJ AF Moon, Jae-Hong Song, Y. Tony Bromirski, Peter D. Miller, Arthur J. TI Multidecadal regional sea level shifts in the Pacific over 1958-2008 SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE regional sea level shifts; Pacific Decadal Oscillation; multidecadal wind changes; a non-Boussinesq OGCM; Pacific Ocean ID WESTERN NORTH PACIFIC; TROPICAL PACIFIC; KUROSHIO EXTENSION; CIRCULATION MODEL; OCEAN CLIMATE; GLOBAL OCEAN; VARIABILITY; BOUSSINESQ; RISE; SIMULATION AB Altimeter data have significantly improved our understanding of regional sea level variability and trends, but their relatively short records do not allow either evaluation of the ocean state prior to 1993 or multidecadal low-frequency signals in the ocean. Here we characterize and quantify the multidecadal regional sea level rise (rSLR) and related ocean heat content in the Pacific from a non-Boussinesq ocean circulation model in comparison with data sets from altimeters, two sea level reconstructions, and in situ ocean profiles from 1958 to 2008. We show that the rSLR trends have undergone two shifts, during the mid-1970s and in the early 1990s, with an east-west dipole pattern in the tropical Pacific. In each of these phases, rSLR accelerated on one side of the Pacific, but decelerated on the other side. The multidecadal sea level shifts can be explained by the dynamical (steric) upper-ocean responses to the surface wind forcing associated with the Pacific Decadal Oscillation (PDO), with negligible contributions from internal (depth-integrated) ocean mass changes. Additional model experimentation further confirms that the Pacific wind stress trend over the recent two decades has played an important role in strengthening the rSLR in the western Pacific while suppressing the rSLR in the eastern Pacific. The climate-forced large-scale rSLR variability is likely to impose a long-term and uneven impact on coastal communities. C1 [Moon, Jae-Hong; Song, Y. Tony] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Bromirski, Peter D.; Miller, Arthur J.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Moon, JH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Jae-Hong.Moon@jpl.nasa.gov FU Department of Parks and Recreation, Division of Boating and Waterways; NSF [OCE-0960770] FX This research is carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). Many thanks to B. D. Hamlington and B. Meyssignac for providing their long-term sea level reconstruction data. Support for Peter D. Bromirski and Arthur J. Miller was provided by the Department of Parks and Recreation, Division of Boating and Waterways, with additional support from NSF (OCE-0960770). We thank the three referees who provided important and insightful comments that significantly improved the presentation. NR 49 TC 11 Z9 11 U1 0 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC PY 2013 VL 118 IS 12 BP 7024 EP 7035 DI 10.1002/2013JC009297 PG 12 WC Oceanography SC Oceanography GA 292TU UT WOS:000329926200046 ER PT J AU Chen, S Hong, Y Gourley, JJ Huffman, GJ Tian, YD Cao, Q Yong, B Kirstetter, PE Hu, JJ Hardy, J Li, Z Khan, SI Xue, XW AF Chen, Sheng Hong, Yang Gourley, Jonathan J. Huffman, George J. Tian, Yudong Cao, Qing Yong, Bin Kirstetter, Pierre-Emmanuel Hu, Junjun Hardy, Jill Li, Zhe Khan, Sadiq I. Xue, Xianwu TI Evaluation of the successive V6 and V7 TRMM multisatellite precipitation analysis over the Continental United States SO WATER RESOURCES RESEARCH LA English DT Article DE evaluation; QPE; TRMM; TMPA ID GAUGE OBSERVATIONS; ANALYSIS TMPA; RAINFALL; PRODUCTS; MODEL; TERRAIN; RADAR AB The spatial error structure of surface precipitation derived from successive versions of the TRMM Multisatellite Precipitation Analysis (TMPA) algorithms are systematically studied through comparison with the Climate Prediction Center Unified Gauge daily precipitation Analysis (CPCUGA) over the Continental United States (CONUS) for 3 years from June 2008 to May 2011. The TMPA products include the version-6(V6) and version-7(V7) real-time products 3B42RT (3B42RTV6 and 3B42RTV7) and research products 3B42 (3B42V6 and 3B42V7). The evaluation shows that 3B42V7 improves upon 3B42V6 over the CONUS regarding 3 year mean daily precipitation: the correlation coefficient (CC) increases from 0.85 in 3B42V6 to 0.92 in 3B42V7; the relative bias (RB) decreases from -22.95% in 3B42V6 to -2.37% in 3B42V7; and the root mean square error (RMSE) decreases from 0.80 in 3B42V6 to 0.48 mm in 3B42V7. Distinct improvement is notable in the mountainous West especially along the coastal northwest mountainous areas, whereas 3B42V6 (also 3B42RTV6 and 3B42RTV7) largely underestimates: the CC increases from 0.86 in 3B42V6 to 0.89 in 3B42V7, and the RB decreases from -44.17% in 3B42V6 to -25.88% in 3B42V7. Over the CONUS, 3B42RTV7 gained a little improvement over 3B42RTV6 as RB varies from -4.06% in 3B42RTV6 to 0.22% in 3B42RTV7. But there is more overestimation with the RB increasing from 8.18% to 14.92% (0.16-3.22%) over the central US (eastern). C1 [Chen, Sheng; Hong, Yang; Cao, Qing; Kirstetter, Pierre-Emmanuel; Khan, Sadiq I.; Xue, Xianwu] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73072 USA. [Chen, Sheng; Hong, Yang; Cao, Qing; Kirstetter, Pierre-Emmanuel; Hu, Junjun; Hardy, Jill; Khan, Sadiq I.; Xue, Xianwu] Natl Weather Ctr, Adv Radar Res Ctr, Norman, OK USA. [Gourley, Jonathan J.; Kirstetter, Pierre-Emmanuel; Hardy, Jill] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA. [Huffman, George J.] Sci Syst & Applicat Inc, Lanham, MD USA. [Huffman, George J.; Tian, Yudong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Yong, Bin] Hohai Univ, State Key Lab Hydrol Water Resources & Hydraul En, Nanjing, Jiangsu, Peoples R China. [Hu, Junjun] Univ Oklahoma, Sch Comp Sci, Norman, OK 73019 USA. [Li, Zhe] Tsinghua Univ, Dept Hydraul Engn, Beijing 100084, Peoples R China. RP Hong, Y (reprint author), Univ Oklahoma, Sch Civil Engn & Environm Sci, 202 W Boyd St, Norman, OK 73072 USA. EM yanghong@ou.edu RI Kirstetter, Pierre/E-2305-2013; Huffman, George/F-4494-2014; Yong, Bin/C-2257-2014; Hong, Yang/D-5132-2009; Gourley, Jonathan/C-7929-2016; Xue, Xianwu/C-8006-2016; Measurement, Global/C-4698-2015 OI Kirstetter, Pierre/0000-0002-7381-0229; Huffman, George/0000-0003-3858-8308; Yong, Bin/0000-0003-1466-2091; Hong, Yang/0000-0001-8720-242X; Gourley, Jonathan/0000-0001-7363-3755; Xue, Xianwu/0000-0002-2106-6370; FU NOAA Multi-function Phased-Array Radar Project; NASA Global Precipitation Measurement Ground Validation program FX This work was financially supported both by the NOAA Multi-function Phased-Array Radar Project administrated by the Advanced Radar Research Center at the University of Oklahoma and also by a NASA Global Precipitation Measurement Ground Validation program. NR 35 TC 45 Z9 46 U1 4 U2 43 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD DEC PY 2013 VL 49 IS 12 BP 8174 EP 8186 DI 10.1002/2012WR012795 PG 13 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 292UX UT WOS:000329929100024 ER PT J AU Singels, A Jones, M Marin, F Ruane, AC Thorburn, P AF Singels, A. Jones, M. Marin, F. Ruane, A. C. Thorburn, P. TI Predicting climate change impacts on sugarcane production at sites in Australia, Brazil and South Africa using the Canegro model SO INTERNATIONAL SUGAR JOURNAL LA English DT Article; Proceedings Paper CT 28th Congress of the International-Society-of-Sugar-Cane-Technologists CY JUN 24-27, 2013 CL Sao Paulo, BRAZIL SP Int Soc Sugar Cane Technologists DE climate change; crop model; cane yield; canopy cover; global climate model; sugarcane ID BIOMASS AB Future climate change is expected to have important consequences for sugarcane production, and reliable predictions of crop response to climate change are necessary to plan adaptation strategies. The objective of this study was to assess the use of global climate models (GCMs) and a crop simulation model for predicting climate change impacts on sugarcane production. The Canegro model was used to simulate growth and development of sugarcane crops under typical management conditions at three sites (irrigated crops at Ayr, Australia; rainfed crops at Piracicaba, Brazil and La Mercy, South Africa) for current and three future climate scenarios. The baseline scenario consisted of a 30-year time series of historical daily weather records and atmospheric CO2 concentration ([CO2]) set at 360 ppm. Future climate scenarios were derived from three GCMs for the A2 greenhouse gas emission scenario and [CO2] set at 734 ppm. The three GCMs were chosen to represent the uncertainty in projected rainfall changes. Future cane yields are expected to increase at all three sites, ranging from +4% for Ayr, to +9% and +20% for Piracicaba and La Mercy. The uncertainty of these predictions correlates with the magnitude of the predicted yield increase. Canopy development was accelerated at all three sites by increased temperature, which led to increased interception of radiation, increased transpiration, and slight increases in drought stress at rainfed sites. For the high potential sites (Ayr and Piracicaba), yield increases were limited by large increases in maintenance respiration which consumed most of the daily assimilate when high biomass was achieved. A weakness of the climate data used was the assumption of no change in rainfall distribution, solar radiation and relative humidity-variables that are crucial in determining the water status of rainfed sugarcane. Crop model aspects that need refinement include improved simulation of (1) elevated [CO2] effects on crop photosynthesis and transpiration, and (2) high temperature effects on crop development, photosynthesis and respiration. C1 [Singels, A.; Jones, M.] South African Sugarcane Res Inst, Mt Edgecombe, South Africa. [Marin, F.] Embrapa Agr Informat, Campinas, SP, Brazil. [Ruane, A. C.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Thorburn, P.] CSIRO Ecosyst Sci, Brisbane, Qld, Australia. RP Singels, A (reprint author), South African Sugarcane Res Inst, Mt Edgecombe, South Africa. EM abraham.singels@sugar.org.za NR 23 TC 0 Z9 0 U1 4 U2 16 PU INT SUGAR JOURNAL LTD PI KENT PA 80 CALVERLEY, TUNBRIDGE WELLS, KENT TN1 2UN, WALES SN 0020-8841 J9 INT SUGAR J JI Int. Sugar J. PD DEC PY 2013 VL 115 IS 1380 BP 874 EP 881 PG 8 WC Agronomy; Food Science & Technology SC Agriculture; Food Science & Technology GA 292CA UT WOS:000329878300030 ER PT J AU Warren-Rhodes, KA McKay, CP Boyle, LN Wing, MR Kiekebusch, EM Cowan, DA Stomeo, F Pointing, SB Kaseke, KF Eckardt, F Henschel, JR Anisfeld, A Seely, M Rhodes, KL AF Warren-Rhodes, Kimberley A. McKay, Christopher P. Boyle, Linda Ng Wing, Michael R. Kiekebusch, Elsita M. Cowan, Don A. Stomeo, Francesca Pointing, Stephen B. Kaseke, Kudzai F. Eckardt, Frank Henschel, Joh R. Anisfeld, Ari Seely, Mary Rhodes, Kevin L. TI Physical ecology of hypolithic communities in the central Namib Desert: The role of fog, rain, rock habitat, and light SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article DE hypolith; cyanobacteria; Namib Desert; fog; rainfall; light ID NEGEV-DESERT; ENVIRONMENTAL GRADIENTS; MICROBIAL COMMUNITIES; ATACAMA DESERT; SPATIAL SCALES; POLAR DESERT; LIQUID WATER; COLD DESERTS; SOIL CRUST; CHINA HOT AB Hypolithic microbial communities are productive niches in deserts worldwide, but many facets of their basic ecology remain unknown. The Namib Desert is an important site for hypolith study because it has abundant quartz rocks suitable for colonization and extends west to east across a transition from fog- to rain-dominated moisture sources. We show that fog sustains and impacts hypolithic ecology in several ways, as follows: (1) fog effectively replaces rainfall in the western zone of the central Namib to enable high (95%) hypolithic abundance at landscape (1-10 km) and larger scales; and (2) high water availability, through fog (western zone) and/or rainfall (eastern zone), results in smaller size-class rocks being colonized (mean 6.31.2 cm) at higher proportions (e.g., 98% versus approximately 3%) than in previously studied hyperarid deserts. We measured 0.1% of incident sunlight as the lower limit for hypolithic growth on quartz rocks in the Namib and found that uncolonized ventral rock surfaces were limited by light rather than moisture. In situ monitoring showed that although rainfall supplied more liquid water (36 h) per event than fog (mean 4 h), on an equivalent annual basis, fog provided nearly twice as much liquid water as rainfall to the hypolithic zone. Hypolithic abundance reaches 100% at a mean annual precipitation (MAP) of approximately 40-60 mm, but at a much lower MAP (approximately 25 mm) when moisture from fog is available. C1 [Warren-Rhodes, Kimberley A.; McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Warren-Rhodes, Kimberley A.] SETI Inst, Mountain View, CA USA. [Boyle, Linda Ng] Univ Washington, Dept Ind & Syst Engn, Seattle, WA 98195 USA. [Boyle, Linda Ng] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA. [Wing, Michael R.] Sir Francis Drake High Sch, San Anselmo, CA USA. [Kiekebusch, Elsita M.; Anisfeld, Ari; Seely, Mary] Desert Res Fdn Namibia, Windhoek, Namibia. [Cowan, Don A.] Univ Pretoria, Dept Genet, Ctr Microbial Ecol & Genom, ZA-0002 Pretoria, South Africa. [Cowan, Don A.; Stomeo, Francesca] Univ Western Cape, Inst Microbial Biotechnol & Metagen, Cape Town, South Africa. [Stomeo, Francesca] Int Livestock Res Inst Hub, Biosci Eastern & Cent Africa, Nairobi, Kenya. [Pointing, Stephen B.] Auckland Univ Technol, Inst Appl Ecol New Zealand, Sch Appl Sci, Auckland, New Zealand. [Kaseke, Kudzai F.] Indiana Univ Purdue Univ, Dept Earth Sci, Indianapolis, IN 46202 USA. [Eckardt, Frank] Univ Cape Town, Dept Environm & Geog Sci, ZA-7700 Rondebosch, South Africa. [Henschel, Joh R.] Gobabeb Res & Training Ctr, Walvis Bay, Namibia. [Rhodes, Kevin L.] Univ Hawaii, Hilo, HI 96720 USA. RP Warren-Rhodes, KA (reprint author), NASA, Ames Res Ctr, Div Space Sci, MS 245-3, Moffett Field, CA 94035 USA. EM kwarrenrhodes@gmail.com RI Cowan, Don/E-3991-2012; Eckardt, Frank/N-3682-2015 OI Cowan, Don/0000-0001-8059-861X; Eckardt, Frank/0000-0003-0200-7110 FU NASA's ASTEP Program FX The authors offer many thanks to Nathan Pavlovic for field assistance and to all the staff at the Gobabeb Research and Training Centre for helpful support during field operations. We extend appreciation to several anonymous reviewers for their suggestions on the manuscript. This work was partially supported through NASA's ASTEP Program. We gratefully acknowledge the Ministry of Environment and Tourism for permission to conduct this study in the Namib-Naukluft Park. NR 76 TC 10 Z9 12 U1 2 U2 29 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 EI 2169-8961 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD DEC PY 2013 VL 118 IS 4 BP 1451 EP 1460 DI 10.1002/jgrg.20117 PG 10 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 291ZM UT WOS:000329871400009 ER PT J AU Li, XW Tao, WK Masunaga, H Gu, GJ Zeng, XP AF Li, Xiaowen Tao, Wei-Kuo Masunaga, Hirohiko Gu, Guojun Zeng, Xiping TI Aerosol Effects on Cumulus Congestus Population over the Tropical Pacific: A Cloud-Resolving Modeling Study SO JOURNAL OF THE METEOROLOGICAL SOCIETY OF JAPAN LA English DT Article DE aerosol; CCN; cumulus congestus ID MADDEN-JULIAN OSCILLATION; DEEP CONVECTIVE CLOUDS; LIVED SQUALL LINES; TOGA COARE; CONDENSATION NUCLEI; SURFACE FLUXES; PRECIPITATION; EVOLUTION; SIMULATIONS; SYSTEMS AB This study examines the significance of aerosol serving as cloud condensation nuclei (CCN) in modulating strengths of tropical maritime convection. Through a Tropical Ocean Global Atmosphere Couple Ocean-Atmosphere Response Experiment (TOGA COARE) case study using a cloud-resolving model (the Goddard Cumulus Ensemble Model with a horizontal mesh interval of 750 m) and a detailed spectral bin microphysical scheme, it is found that low aerosol concentration acts to reduce convection strengths. Over the tropical western Pacific where low-level water vapor is abundant and a ubiquitous weak stable level exists near 0 C, the low background maritime aerosol concentration is conducive for forming cumulus congestus. Sensitivity tests show that the main mechanism of convection damping in a clean maritime environment is through reduced condensational growth, although the freezing of supercooled water, cloud top evaporation, and rain evaporation also contribute to the simulated effects. Considering the importance of congestus in tropical dynamics and the Madden-Julian oscillation (MJO) lifecycle, we further propose a hypothesis that aerosol-cloud-precipitation interactions in an ultraclean marine environment may serve as a damping mechanism for tropical convection. C1 [Li, Xiaowen; Zeng, Xiping] Morgan State Univ, GESTAR Program, Baltimore, MD USA. [Li, Xiaowen; Tao, Wei-Kuo; Zeng, Xiping] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Masunaga, Hirohiko] Nagoya Univ, Hydrospher Atmospher Res Ctr, Nagoya, Aichi 4648601, Japan. [Gu, Guojun] Univ Maryland, ESSIC, College Pk, MD 20742 USA. RP Li, XW (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA. EM Xiaowen.Li@nasa.gov RI Masunaga, Hirohiko/C-2488-2008 OI Masunaga, Hirohiko/0000-0002-6336-5002 FU NASA headquarters; NASA PMM Mission FX This research is mainly supported by NASA headquarters and the NASA PMM Mission. We thank two anonymous reviewers for their detailed suggestions that significantly improved the clarity of this manuscript. The first author wishes to thank Professor Rob Fovell of UCLA for helpful discussions, Amy Houghton of USRA, Lisa Nalborczyk, and Stephen Palm of SSAI for editing the manuscript, and Jenny Zeng for beautifully rendering Fig. 12. This study is dedicated to Joanne Simpson, who remains an inspiration for many of us. NR 53 TC 3 Z9 3 U1 3 U2 15 PU METEOROLOGICAL SOC JAPAN PI TOKYO PA C/O JAPAN METEOROLOGICAL AGENCY 1-3-4 OTE-MACHI, CHIYODA-KU, TOKYO, 100-0004, JAPAN SN 0026-1165 EI 2186-9057 J9 J METEOROL SOC JPN JI J. Meteorol. Soc. Jpn. PD DEC PY 2013 VL 91 IS 6 BP 817 EP 833 DI 10.2151/jmsj.2013-607 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 294GM UT WOS:000330032100007 ER PT J AU Mariotti, A Schubert, S Mo, K Peters-Lidard, C Wood, A Pulwarty, R Huang, J Barrie, D AF Mariotti, Annarita Schubert, Siegfried Mo, Kingtse Peters-Lidard, Christa Wood, Andy Pulwarty, Roger Huang, Jin Barrie, Dan TI ADVANCING DROUGHT UNDERSTANDING, MONITORING, AND PREDICTION SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Editorial Material C1 [Mariotti, Annarita; Pulwarty, Roger; Barrie, Dan] NOAA, OAR, Climate Program Off, Silver Spring, MD 20910 USA. [Schubert, Siegfried] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Mo, Kingtse; Huang, Jin] NOAA, NWS, Climate Predict Ctr, College Pk, MD USA. [Peters-Lidard, Christa] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Wood, Andy] NOAA, NWS, North West River Forecast Ctr, Portland, OR USA. [Pulwarty, Roger] ESRL PSD, Boulder, CO USA. RP Mariotti, A (reprint author), NOAA, OAR, Climate Program Off, 1315 East West Highway, Silver Spring, MD 20910 USA. EM annarita.mariotti@noaa.gov RI Peters-Lidard, Christa/E-1429-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876 NR 0 TC 3 Z9 3 U1 0 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD DEC PY 2013 VL 94 IS 12 BP ES186 EP ES188 DI 10.1175/BAMS-D-12-00248.1 PG 3 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 287OH UT WOS:000329551600005 ER PT J AU Nelson, R AF Nelson, Ross TI How did we get here? An early history of forestry lidar SO CANADIAN JOURNAL OF REMOTE SENSING LA English DT Article ID WATER RAMAN BACKSCATTER; AIRBORNE LASER DATA; SIMULATION APPROACH; BIOMASS ESTIMATION; HEDMARK COUNTY; SAMPLE SURVEY; ACCURACY; CANOPY; SYSTEM; FLUORESCENCE AB Functioning lasers were first demonstrated in 1960 in the United States and in 1961 in Canada and in the Soviet Union, but research into the use of lasers as forest measurement tools did not begin for another 15 years. Initially, with respect to Earth resources, lasers were employed to measure sea ice surface roughness, to make near-shore bathymetric measurements, to penetrate forests to make detailed topographic measurements, and to fluoresce oceanic phytoplankton for surface current studies. Some of these early studies noted that forest profiles were evident but in fact added noise to topographic retrievals. As early as 1964, researchers noted vegetation returns acquired using an airborne helium-neon (He-Ne), 0.63 mm, continuous wave (CW) laser. A decade and many airborne studies later, scientists with TRANARG, a mapping and surveying company in Caracas, Venezuela, reported on flights undertaken in 1976 that utilized a He-Ne lidar to collect over 11 000 km of lidar profiles, spaced 1.5 km apart, to construct a topographic map to help site a new reservoir. Though they depended on the laser to penetrate vegetation, they noted 35-40 m median canopy heights with emergents up to 55 m in their profiles. Trees came to be regarded as a signal rather than noise in the mid-1970s. In 1976 in the Soviet Union, Russian researchers felled a birch and a spruce, aimed a He-Ne CW laser with a spot size of approximately 25 mm at the horizontal trees, produced a profilograph, compared it with tape measurements, and concluded that, with increased power, such a laser could be mounted on an aircraft to remotely measure forest canopies. In 1979, they mounted their He-Ne laser on an AN-2 biplane and acquired their first airborne profiles. These studies and others done prior to 1985, i.e., the first two decades of airborne laser research, are reviewed in this glance backwards at the history of forestry lidar. C1 NASA, Goddard Space Flight Ctr, Biospher Sci Branch 618, Greenbelt, MD 20771 USA. RP Nelson, R (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch 618, Bldg 33,Room G405, Greenbelt, MD 20771 USA. EM Ross.F.Nelson@nasa.gov RI Nelson, Ross/H-8266-2014 NR 62 TC 9 Z9 9 U1 1 U2 32 PU CANADIAN AERONAUTICS SPACE INST PI KANATA PA 350 TERRY FOX DR, STE 104, KANATA, ON K2K 2W5, CANADA SN 1712-7971 J9 CAN J REMOTE SENS JI Can. J. Remote Sens. PD DEC PY 2013 VL 39 SU 1 BP S6 EP S17 DI 10.5589/m13-011 PG 12 WC Remote Sensing SC Remote Sensing GA 285OH UT WOS:000329402800002 ER PT J AU Wulder, MA Coops, NC Hudak, AT Morsdorf, F Nelson, R Newnham, G Vastaranta, M AF Wulder, M. A. Coops, N. C. Hudak, A. T. Morsdorf, F. Nelson, R. Newnham, G. Vastaranta, M. TI Status and prospects for LiDAR remote sensing of forested ecosystems SO CANADIAN JOURNAL OF REMOTE SENSING LA English DT Article ID AIRBORNE SCANNING LASER; INVENTORY AB The science associated with the use of airborne and satellite Light Detection and Ranging (LiDAR) to remotely sense forest structure has rapidly progressed over the past decade. LiDAR has evolved from being a poorly understood, potentially useful tool to an operational technology in a little over a decade, and these instruments have become a major success story in terms of their application to the measurement, mapping, or monitoring of forests worldwide. Invented in 1960, the laser and, a short time later, LiDAR, were found in research and military laboratories. Since the early 2000s, commercial technological developments coupled with an improved understanding of how to manipulate and analyze large amounts of collected data enabled notable scientific and application developments. A diversity of rapidly developing fields especially benefit from communications offered through conferences such as SilviLaser, and LiDAR has been no different. In 2002 the SilviLaser conference series was initiated to bring together those interested in the development and application of LiDAR for forested environments. Now, a little over a decade later, commercial use of LiDAR is common. In this paper - using the deliberations of SilviLaser 2012 as a source of information - we aim to capture aspects of importance to LiDAR users in the forest ecosystems community and to also point to key emerging issues as well as some remaining challenges. C1 [Wulder, M. A.] Canadian Forest Serv, Nat Resources Canada, Victoria, BC V8Z 1M5, Canada. [Coops, N. C.] Univ British Columbia, Vancouver, BC V6T 1Z4, Canada. [Hudak, A. T.] US Forest Serv, Rocky Mt Res Stn, USDA, Moscow, ID 83843 USA. [Morsdorf, F.] Univ Zurich, Dept Geog, Remote Sensing Labs, Zurich, Switzerland. [Nelson, R.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Newnham, G.] CSIRO, Clayton, Vic 3139, Australia. [Vastaranta, M.] Univ Helsinki, Dept Forest Sci, FI-00014 Helsinki, Finland. RP Wulder, MA (reprint author), Canadian Forest Serv, Nat Resources Canada, 506 W Burnside Rd, Victoria, BC V8Z 1M5, Canada. EM mwulder@nrcan.gc.ca RI Morsdorf, Felix/D-1151-2010; Coops, Nicholas/J-1543-2012; Newnham, Glenn/G-8115-2011; Nelson, Ross/H-8266-2014; Wulder, Michael/J-5597-2016 OI Vastaranta, Mikko/0000-0001-6552-9122; Coops, Nicholas/0000-0002-0151-9037; Wulder, Michael/0000-0002-6942-1896 NR 16 TC 21 Z9 21 U1 6 U2 33 PU CANADIAN AERONAUTICS SPACE INST PI KANATA PA 350 TERRY FOX DR, STE 104, KANATA, ON K2K 2W5, CANADA SN 1712-7971 J9 CAN J REMOTE SENS JI Can. J. Remote Sens. PD DEC PY 2013 VL 39 SU 1 BP S1 EP S5 DI 10.5589/m13-051 PG 5 WC Remote Sensing SC Remote Sensing GA 285OH UT WOS:000329402800001 ER PT J AU Manizza, M Follows, MJ Dutkiewicz, S Menemenlis, D Hill, CN Key, RM AF Manizza, M. Follows, M. J. Dutkiewicz, S. Menemenlis, D. Hill, C. N. Key, R. M. TI Changes in the Arctic Ocean CO2 sink (1996-2007): A regional model analysis SO GLOBAL BIOGEOCHEMICAL CYCLES LA English Estonian DT Article DE Arctic Ocean; sea ice; ocean productivity ID CARBON-CYCLE; SEA; TEMPERATURE; COMMUNITIES AB The rapid recent decline of Arctic Ocean sea ice area increases the flux of solar radiation available for primary production and the area of open water for air-sea gas exchange. We use a regional physical-biogeochemical model of the Arctic Ocean, forced by the National Centers for Environmental Prediction/National Center for Atmospheric Research atmospheric reanalysis, to evaluate the mean present-day CO2 sink and its temporal evolution. During the 1996-2007 period, the model suggests that the Arctic average sea surface temperature warmed by 0.04 degrees Ca-1, that sea ice area decreased by approximate to 0.1 x 10(6)km(2)a(-1), and that the biological drawdown of dissolved inorganic carbon increased. The simulated 1996-2007 time-mean Arctic Ocean CO2 sink is 586TgCa(-1). The increase in ice-free ocean area and consequent carbon drawdown during this period enhances the CO2 sink by approximate to 1.4TgCa(-1), consistent with estimates based on extrapolations of sparse data. A regional analysis suggests that during the 1996-2007 period, the shelf regions of the Laptev, East Siberian, Chukchi, and Beaufort Seas experienced an increase in the efficiency of their biological pump due to decreased sea ice area, especially during the 2004-2007 period, consistent with independently published estimates of primary production. In contrast, the CO2 sink in the Barents Sea is reduced during the 2004-2007 period due to a dominant control by warming and decreasing solubility. Thus, the effect of decreasing sea ice area and increasing sea surface temperature partially cancel, though the former is dominant. C1 [Manizza, M.; Follows, M. J.; Dutkiewicz, S.; Hill, C. N.] MIT, Dept Earth Atmospher & Planetary Sci, Program Atmospheres Oceans & Climate, Cambridge, MA USA. [Menemenlis, D.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Key, R. M.] Princeton Univ, Dept Geosci, Program Atmosphere & Ocean Sci, Princeton, NJ 08544 USA. RP Manizza, M (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM mmanizza@ucsd.edu FU NASA Modeling Analysis and Prediction (MAP) program; National Science Foundation; NSF [ARC-0531119]; NOAA [NA09OAR4310069]; Scripps Institution of Oceanography FX This work is a contribution to the ECCO2 project sponsored by the NASA Modeling Analysis and Prediction (MAP) program and to the "Synthesis of the Arctic System Science" project funded by the National Science Foundation. M.M. and M.J.F. were financially supported by the NSF grant ARC-0531119 and SD by NOAA grant NA09OAR4310069. M.M. thanks the NASA AMES Research Center for computer time and technical support when carrying out numerical simulations and the Scripps Institution of Oceanography postdoctoral program for additional financial support while completing the manuscript. We also thank Nick Bates and Jeremy Mathis for helpful discussions. NR 52 TC 8 Z9 9 U1 6 U2 35 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0886-6236 EI 1944-9224 J9 GLOBAL BIOGEOCHEM CY JI Glob. Biogeochem. Cycle PD DEC PY 2013 VL 27 IS 4 BP 1108 EP 1118 DI 10.1002/2012GB004491 PG 11 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA 289MP UT WOS:000329686900011 ER PT J AU Pilorget, C Edwards, CS Ehlmann, BL Forget, F Millour, E AF Pilorget, C. Edwards, C. S. Ehlmann, B. L. Forget, F. Millour, E. TI Material ejection by the cold jets and temperature evolution of the south seasonal polar cap of Mars from THEMIS/CRISM observations and implications for surface properties SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; ice; climate; surface temperature ID SUBLIMATION-DRIVEN ACTIVITY; HIRISE OBSERVATIONS; SLAB ICE; CO2 ICE; REGIONS; TES; ALBEDO AB As the seasonal CO2 ice polar caps of Mars retreat during spring, dark spots appear on the ice in some specific regions. These features are thought to result from basal sublimation of the transparent CO2 ice followed by ejection of regolith-type material, which then covers the ice. We have used Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) reflectance data, Thermal Emission Imaging System (THEMIS) visible images, and THEMIS-derived temperature retrievals along with a thermal numerical model to constrain the physical and compositional characteristics of the seasonal cap for several areas exhibiting dark spots at both high spatial and temporal resolutions. Data analysis suggests an active period of material ejection (before solar longitude (Ls) 200), accumulation around the ejection points, and spreading of part of the ejected material over the whole area, followed by a period where no significant amount of material is ejected, followed by complete defrosting (approximate to Ls 245). Dark material thickness on top of the CO2 ice is estimated to range from a few hundreds of microns to a few millimeters in the warmest spots, based on numerical modeling combined with the observed temperature evolution. The nature of the venting process and the amount of material that is moved lead to the conclusion that it could have an important impact on the surface physical properties. C1 [Pilorget, C.; Edwards, C. S.; Ehlmann, B. L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Ehlmann, B. L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Forget, F.; Millour, E.] UPMC, CNRS, IPSL, Meteorol Dynam Lab, Paris 05, France. RP Pilorget, C (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM cpilorge@caltech.edu OI Millour, Ehouarn/0000-0003-4808-9203 NR 36 TC 4 Z9 4 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC PY 2013 VL 118 IS 12 BP 2520 EP 2536 DI 10.1002/2013JE004513 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 290EF UT WOS:000329735600005 ER PT J AU Sanchez-Lavega, A Legarreta, J Garcia-Melendo, E Hueso, R Perez-Hoyos, S Gomez-Forrellad, JM Fletcher, LN Orton, GS Simon-Miller, A Chanover, N Irwin, P Tanga, P Cecconi, M AF Sanchez-Lavega, A. Legarreta, J. Garcia-Melendo, E. Hueso, R. Perez-Hoyos, S. Gomez-Forrellad, J. M. Fletcher, L. N. Orton, G. S. Simon-Miller, A. Chanover, N. Irwin, P. Tanga, P. Cecconi, M. TI Colors of Jupiter's large anticyclones and the interaction of a Tropical Red Oval with the Great Red Spot in 2008 SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE planetary atmospheres; Jupiter; anticyclones ID VERTICAL STRUCTURE; CLOUD STRUCTURE; NONLINEAR SIMULATIONS; WHITE OVALS; ZONAL WINDS; HST IMAGES; ATMOSPHERE; DYNAMICS; GALILEO; JET AB The nature and mechanisms producing the chromophore agents that provide color to the upper clouds and hazes of the atmospheres of the giant planets are largely unknown. In recent times, the changes in red coloration that have occurred in large- and medium-scale Jovian anticyclones have been particularly interesting. In late June and early July 2008, a particularly color intense tropical red oval interacted with the Great Red Spot (GRS) leading to the destruction of the tropical red oval and cloud dispersion. We present a detailed study of the tropical vortices, usually white but sometimes red, and a characterization of their color spectral signatures and dynamics. From the spectral reflectivity in methane bands we study their vertical cloud structure compared to that of the GRS and BA. Using two spectral indices we found a near correlation between anticyclones cloud top altitudes and red color. We present detailed observations of the interaction of the red oval with the GRS and model simulations of the phenomena that allow us to constrain the relative vertical extent of the vortices. We conclude that the vertical cloud structure, vertical extent, and dynamics of Jovian anticyclones are not the causes of their coloration. We propose that the red chromophore forms when background material (a compound or particles) is entrained by the vortex, transforming into red once inside the vortex due to internal conditions, exposure to ultraviolet radiation, or to the mixing of two chemical compounds that react inside the vortex, confined by a potential vorticity ring barrier. C1 [Sanchez-Lavega, A.; Perez-Hoyos, S.] Univ Basque Country, Dept Fis Aplicada, ETS Ingn, ES-48013 Bilbao, Spain. [Sanchez-Lavega, A.; Legarreta, J.; Hueso, R.; Perez-Hoyos, S.] Univ Basque Country, CSIC, IAA, Unidad Asociada Grp Ciencias Planetarias, Bilbao, Spain. [Legarreta, J.] Univ Basque Country, EUITI, Dept Ingn Sistemas & Automat, E-48080 Bilbao, Spain. [Garcia-Melendo, E.; Gomez-Forrellad, J. M.] Fundacio Privada Observ Astron Catalunya Esteve D, Seva, Spain. [Garcia-Melendo, E.] Inst Ciencies Espai, Fac Ciencies, CSIC IEEC, Bellaterra, Spain. [Fletcher, L. N.; Irwin, P.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England. [Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Simon-Miller, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chanover, N.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Tanga, P.] Univ Sophia Antipolis, CNRS, Lab Lagrange, Observ Cote Azur,UMR 7293, Nice, France. [Cecconi, M.] Roque Muchachos Astron Observ, Garafia, Spain. RP Sanchez-Lavega, A (reprint author), Univ Basque Country, Dept Fis Aplicada, ETS Ingn, Alameda Urquijo S-N, ES-48013 Bilbao, Spain. EM agustin.sanchez@ehu.es RI Fletcher, Leigh/D-6093-2011; Perez-Hoyos, Santiago/L-7543-2014; Simon, Amy/C-8020-2012; OI Fletcher, Leigh/0000-0001-5834-9588; Perez-Hoyos, Santiago/0000-0002-2587-4682; Simon, Amy/0000-0003-4641-6186; LEGARRETA ETXAGIBEL, JON JOSU/0000-0001-6501-2705; Sanchez-Lavega, Agustin/0000-0001-7355-1522; Irwin, Patrick/0000-0002-6772-384X; Tanga, Paolo/0000-0002-2718-997X; Hueso, Ricardo/0000-0003-0169-123X FU Spanish MICIIN [AYA2009-10701, AYA2012-36666]; FEDER [Grupos Gobierno Vasco IT464-07, IT765-013, UPV/EHU UFI11/55]; University of Oxford; NASA; Association of Universities for Research in Astronomy, Inc., under NASA [NAS 5-26555]; Massimo Cecconi (INAF/Fundacion Galileo Galilei, La Palma) FX This work was supported by the Spanish MICIIN project AYA2009-10701 and AYA2012-36666 with FEDER support, Grupos Gobierno Vasco IT464-07 and IT765-013, and UPV/EHU UFI11/55. We made use of computing facilities at CESCA in Barcelona with the help of MEC. Fletcher was supported by a Glasstone Fellowship at the University of Oxford during this research. Orton was supported by NASA through an award issued to the Jet Propulsion Laboratory, California Institute of Technology. This work is partly based on observations obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA Contract NAS 5-26555. The Italian Telescopio Nazionale Galileo (TNG) is operated on the island of La Palma by the Fundacion Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. We acknowledge the support of Massimo Cecconi (INAF/Fundacion Galileo Galilei, La Palma) in the observations with TNG and AdOpt. The IOPW and ALPO-Japan contributors are from the International Outer Planet Watch Team IOPW-PVOL: http://www.pvol.ehu.es/pvol/index.jsp?action=iopw and from ALPO-Japan (Association of Lunar and Planetary Observers) in Japan: http://alpo-j.asahikawa-med.ac.jp/indexE.htm. NR 59 TC 5 Z9 5 U1 2 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC PY 2013 VL 118 IS 12 BP 2537 EP 2557 DI 10.1002/2013JE004371 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 290EF UT WOS:000329735600006 ER PT J AU Tenerani, A Velli, M AF Tenerani, A. Velli, M. TI Parametric decay of radial Alfven waves in the expanding accelerating solar wind SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE parametric decay; solar wind waves; instabilities ID HYBRID SIMULATIONS; MHD TURBULENCE; AMPLITUDE; INSTABILITY; EVOLUTION AB We study the onset and evolution of the Alfven wave parametric decay instability within the Accelerating Expanding Box model in the framework of a one-fluid description of the plasma. As we are interested in understanding wave propagation and dissipation in the inner heliosphere and solar wind, the expansion of the solar wind itself may not be neglected. In this sense, the Accelerating Expanding Box provides a useful and simple model to mimic the effects that the expansion of the underlying atmosphere has on wave propagation and plasma dynamics. In the simulations, we follow the evolution of Alfven waves along a fast solar wind stream, from the sub-Alfvenic region up to a maximum heliocentric distance of nearly 4 AU. We consider exact solutions of the compressible MHD system given by circularly polarized Alfven waves which propagate in the radial direction, along the mean magnetic field. Both monochromatic waves and a nonmonochromatic wave are considered. Monochromatic waves have periods ranging from a few minutes to a few hours, the latter being stabilized by the expansion. The nonmonochromatic wave has a central period of the order of a few minutes, with a broad spectrum containing frequencies near the threshold of the instability. In this case the Alfven wave partly decays into backward daughter Alfven waves up to the instability saturation, then giving rise to a nonlinear cascade of incompressible and compressible modes. C1 [Tenerani, A.; Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tenerani, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM anna.tenerani@jpl.nasa.gov NR 26 TC 5 Z9 5 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2013 VL 118 IS 12 BP 7507 EP 7516 DI 10.1002/2013JA019293 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286ZX UT WOS:000329508900004 ER PT J AU Breneman, AW Cattell, CA Kersten, K Paradise, A Schreiner, S Kellogg, PJ Goetz, K Wilson, LB AF Breneman, A. W. Cattell, C. A. Kersten, K. Paradise, A. Schreiner, S. Kellogg, P. J. Goetz, K. Wilson, L. B., III TI STEREO and Wind observations of intense cyclotron harmonic waves at the Earth's bow shock and inside the magnetosheath SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE cyclotron; Bernstein; bowshock; harmonics; waves ID INSTRUMENT; SPACECRAFT; TURBULENCE; UPSTREAM; RADIO AB We present the first observations of electron cyclotron harmonic waves at the Earth's bow shock from STEREO and Wind burst waveform captures. These waves are observed at magnetic field gradients at a variety of shock geometries ranging from quasi-parallel to nearly perpendicular along with whistler mode waves, ion acoustic waves, and electrostatic solitary waves. Large amplitude cyclotron harmonic waveforms are also observed in the magnetosheath in association with magnetic field gradients convected past the bow shock. Amplitudes of the cyclotron harmonic waves range from a few tens to more than 500 mV/m peak-peak. A comparison between the short (15 m) and long (100 m) Wind spin plane antennas shows a similar response at low harmonics and a stronger response on the short antenna at higher harmonics. This indicates that wavelengths are not significantly larger than 100 m, consistent with the electron cyclotron radius. Waveforms are broadband and polarizations are distinctively comma-shaped with significant power both perpendicular and parallel to the magnetic field. Harmonics tend to be more prominent in the perpendicular directions. These observations indicate that the waves consist of a combination of perpendicular Bernstein waves and field-aligned waves without harmonics. A likely source is the electron cyclotron drift instability which is a coupling between Bernstein and ion acoustic waves. These waves are the most common type of high-frequency wave seen by STEREO during bow shock crossings and magnetosheath traversals and our observations suggest that they are an important component of the high-frequency turbulent spectrum in these regions. C1 [Breneman, A. W.; Cattell, C. A.; Kersten, K.; Paradise, A.; Schreiner, S.; Kellogg, P. J.; Goetz, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Wilson, L. B., III] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Breneman, AW (reprint author), Univ Minnesota, Sch Phys & Astron, 116 Church St SE, Minneapolis, MN 55455 USA. EM awbrenem@gmail.com RI Wilson III, Lynn/D-4425-2012; OI Wilson III, Lynn/0000-0002-4313-1970; Cattell, Cynthia/0000-0002-3805-320X FU NASA [NNX12AB23G, NNX10AU82G] FX Simulation results have been provided by the Community Coordinated Modeling Center at Goddard Space Flight Center through their public Runs on Request system (http://ccmc.gsfc.nasa.gov). The CCMC is a multiagency partnership between NASA, AFMC, AFOSR, AFRL, AFWA, NOAA, NSF, and ONR. The BATS-R-US Model was developed by the Space Weather Research Center at the NASA Goddard Space Flight Center. This research was supported by NASA grants NNX12AB23G and NNX10AU82G. NR 31 TC 4 Z9 4 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2013 VL 118 IS 12 BP 7654 EP 7664 DI 10.1002/2013JA019372 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286ZX UT WOS:000329508900020 ER PT J AU Korotova, GI Sibeck, DG Angelopoulos, V Walsh, BM AF Korotova, G. I. Sibeck, D. G. Angelopoulos, V. Walsh, B. M. TI THEMIS observations of compressional poloidal pulsations in the dawnside magnetosphere: A case study SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE ULF waves ID MORNINGSIDE PLASMA SHEET; GEOMAGNETIC-PULSATIONS; GEOSTATIONARY ORBIT; PC-5 WAVES; ULF WAVES; OUTER MAGNETOSPHERE; PC5 PULSATIONS; INSTABILITY; SATELLITES; PROPAGATION AB We present results from a case study of compressional poloidal pulsations with periods ranging from 5 to 12min in the dawn magnetosphere from 1630 to 2000 UT on 27 February 2011. However, we employ THEMIS (Time History of Events and Macroscale Interactions during Substorms) magnetic field, plasma, and energetic particle observations to determine azimuthal wavelengths (7000-27,000km) and velocities (9-28km/s) consistent with previous work. We then apply a new method invoking the north to south motion of the THEMIS spacecraft and the fact that the equatorial node exhibited north-south oscillations to derive the meridional structure of the wave in great detail. We determined that the amplitude of the meridional motion of the equatorial node was similar to 0.8 R-E, and that the meridional wave length exceeded 3 R-E. C1 [Korotova, G. I.] IZMIRAN, Troitsk 142190, Moscow Region, Russia. [Korotova, G. I.] UMD, IPST, College Pk, MD USA. [Sibeck, D. G.; Walsh, B. M.] NASA GSFC, Greenbelt, MD USA. [Angelopoulos, V.] Univ Calif Los Angeles, IGPP ESS, Los Angeles, CA USA. RP Korotova, GI (reprint author), IZMIRAN, Troitsk 142190, Moscow Region, Russia. EM gkorotov@umd.edu RI Walsh, Brian/C-4899-2016 OI Walsh, Brian/0000-0001-7426-5413 FU NASA [NAS5-02099, NNX12AK09G]; THEMIS project NASA's Guest Investigator Program FX THEMIS is supported by NASA NAS5-02099. We are grateful to the ESA, FGM, and SST team and magnetometer team and SST team members for supplying the THEMIS software and plasma and magnetometer data and software. We thank D. Turner for providing the software and useful discussions. Work at GSFC was supported by the THEMIS project NASA's Guest Investigator Program, while work by G. I. K. at the University of Maryland was supported by a grant from NASA NNX12AK09G. NR 38 TC 6 Z9 6 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2013 VL 118 IS 12 BP 7665 EP 7673 DI 10.1002/2013JA019360 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286ZX UT WOS:000329508900021 ER PT J AU Verkhoglyadova, OP Tsurutani, BT Lakhina, GS AF Verkhoglyadova, O. P. Tsurutani, B. T. Lakhina, G. S. TI Theoretical analysis of Poynting flux and polarization for ELF-VLF electromagnetic waves in the Earth's magnetosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE chorus; plasmaspheric hiss; wave polarization; energy flux ID PLASMASPHERIC HISS; PROPAGATION ANALYSIS; CHORUS AB We discuss properties of extremely low-frequency (ELF) and very low-frequency (VLF) electromagnetic waves in the Earth's magnetosphere. General expressions for wave magnetic field polarization and for the angle (P) between the direction of the Poynting flux vector and the ambient magnetic field are derived for low-amplitude (linear) waves taking into account first-order finite gyroradius effects. The wave magnetic field is always in a plane perpendicular to the direction of the wave propagation, and the polarization depends on wave frequency (or wavelength), dispersion, and plasma parameters. In a warm plasma, the Poynting flux is not aligned with the group velocity and generally deviates from the wave propagation direction, except for parallel propagation. Numerical estimates for (P) and wave polarization are made for plasmaspheric hiss (at L=2, 4, and 6) for typical plasma parameters and for the case of elevated electron temperature (5 keV). The plasmaspheric hiss wave magnetic field is right-hand circularly polarized, except for highly oblique hiss waves which are elliptically polarized. We note a possible transition to the magnetosonic wave regime at short wavelengths. The maximum Poynting flux angle is approximate to 20 degrees. Estimates for daytime outer zone chorus (L=6) show two regions of oblique Poynting flux corresponding to a low-frequency band (<(ce)/2) and to a high-frequency band ((ce)/2<<(ce)) where and (ce) are the wave frequency and the electron cyclotron frequency, respectively. The wave magnetic field polarization varies from circular to elliptical at shorter wavelengths. In a hot plasma, chorus is elliptically polarized. The maximum (P) in the low-frequency band is approximate to 20 degrees. (P) can reach approximate to 60 degrees in the high-frequency band. Our results are consistent with the Poynting flux statistics of Polar measurements. C1 [Verkhoglyadova, O. P.; Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Verkhoglyadova, O. P.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Lakhina, G. S.] India Inst Geomagnetism, Navi, India. RP Verkhoglyadova, OP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Olga.Verkhoglyadova@jpl.nasa.gov OI Lakhina, Gurbax /0000-0002-8956-486X; Verkhoglyadova, Olga/0000-0002-9295-9539 FU National Academy of Sciences, India under NASI-Senior Scientist Platinum Jubilee Fellowship FX The authors greatly appreciate comments by L.R.O. Storey who read the first version of the paper. Portions of this research were done at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. G. S. L. thanks the National Academy of Sciences, India for support under the NASI-Senior Scientist Platinum Jubilee Fellowship. A Poynting Vector analysis will be part of the ROGECOWAD (ROsetta GEneralized COmet and WAve Detection) code. This effort has been undertaken to understand the implications of wave Poynting Vectors. NR 38 TC 1 Z9 1 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2013 VL 118 IS 12 BP 7695 EP 7702 DI 10.1002/2013JA019371 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286ZX UT WOS:000329508900024 ER PT J AU El-Alaoui, M Richard, RL Ashour-Abdalla, M Goldstein, ML Walker, RJ AF El-Alaoui, Mostafa Richard, Robert L. Ashour-Abdalla, Maha Goldstein, Melvyn L. Walker, Raymond J. TI Dipolarization and turbulence in the plasma sheet during a substorm: THEMIS observations and global MHD simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE turbulence; dipolarization; substorm; magnetotail; MHD ID MAGNETIC TURBULENCE; NOVEMBER 24; MAGNETOTAIL; ONSET; RECONNECTION; CHALLENGE; NORTHWARD; EVENT; MODEL AB Spacecraft in the magnetotail have observed fluctuations in velocity and magnetic field that have the characteristics of fluid turbulence. We investigated the properties of these fluctuations during a substorm on 7 February 2009. During this event several spacecraft were observing the magnetotail. By using upstream observations performed by Wind, we conducted a global magnetohydrodynamic (MHD) simulation of the substorm. The simulation results were compared to time series of Time History of Events and Macroscale Interactions during Substorms (THEMIS) observations in the magnetotail, and it performed well as the spacecraft encountered dipolarizations and strong flows. Further, the power spectral densities and probability distribution functions observed in the magnetotail by THEMIS and in the MHD simulations were similar. Notable features of the event include a large dipolarization growing by accreting smaller earthward moving dipolarization fronts. The dipolarizations were associated with a strong channel of earthward flow and a large vortex. In the MHD simulation results, which are supported by the observations, strong narrow flow channels are a clear and persistent feature of magnetotail convection which exist at the driving scales for the turbulent spectra. C1 [El-Alaoui, Mostafa; Richard, Robert L.; Ashour-Abdalla, Maha] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [El-Alaoui, Mostafa; Richard, Robert L.; Ashour-Abdalla, Maha] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Goldstein, Melvyn L.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA. [Walker, Raymond J.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP El-Alaoui, M (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, 405 Hilgard Ave, Los Angeles, CA 90095 USA. EM mostafa@igpp.ucla.edu FU NASA [NNX10AQ47G, NNX08AO48G, NAS5-02099]; Magnetospheric Multiscale project Interdisciplinary Scientist program; National Science Foundation [OCI-1053575] FX This research was supported by NASA grants NNX10AQ47G and NNX08AO48G to UCLA. It was further supported by a grant to the Goddard Space Flight Center by the Magnetospheric Multiscale project Interdisciplinary Scientist program. R.J. Walker's contribution was made as part of his Individual Research and Development while he was at the National Science Foundation. We acknowledge NASA contracts NAS5-02099 and V. Angelopoulos for use of data from the THEMIS Mission. We further acknowledge C. W. Carlson and J.P. McFadden (ESA data), and K. H. Glassmeier, U. Auster, and W. Baumjohann (FGM data) for THEMIS observations. The MHD computations were performed by using the Gordon supercomputer at San Diego, part of the Extreme Science and Engineering Discovery Environment (XSEDE). This program is supported by grant OCI-1053575 from the National Science Foundation. NR 48 TC 10 Z9 10 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2013 VL 118 IS 12 BP 7752 EP 7761 DI 10.1002/2013JA019322 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286ZX UT WOS:000329508900029 ER PT J AU Lee, WK Kil, H Paxton, LJ Zhang, YL Shim, JS AF Lee, Woo Kyoung Kil, Hyosub Paxton, Larry J. Zhang, Yongliang Shim, Ja Soon TI The effect of geomagnetic-storm-induced enhancements to ionospheric emissions on the interpretation of the TIMED/GUVI O/N-2 ratio SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE GUVI O; N2 ratio; ionospheric effect; geomagnetic storm ID ULTRAVIOLET IMAGER GUVI; SOLAR EUV; THERMOSPHERE; MISSION; DAYGLOW AB We examine the consequence of enhanced atomic oxygen (OI) 135.6 nm emissions due to the recombination of O+ with electrons on the column number density ratio of atomic oxygen to molecular nitrogen (O/N-2 ratio) provided by Global Ultraviolet Imager (GUVI) on board the Thermosphere, Ionosphere, Mesosphere Energetics and Dynamics satellite. GUVI O/N-2 ratio is derived from the measurements of OI 135.6 nm and N-2 Lyman-Birge-Hopfield airglow emissions. The OI 135.6 nm emission arises from two sources: photoelectron impact excitation of neutral atomic oxygen and the radiative recombination of O+ with electrons. We estimate the O/N-2 ratio disturbance associated with the O+ density enhancement during geomagnetic storms through the case study of the storms on 20 November 2003 and 8 November 2004. The OI 135.6 nm emission enhancement originating from the ionosphere is derived using the Utah State University Global Assimilation of Ionospheric Measurements model ionosphere. Our results show that the O/N-2 ratio increase from the equator to middle latitudes during the storm periods is primarily associated with thermospheric neutral composition disturbances. However, the contribution of the OI 135.6 nm emission originating from the ionosphere to the storm time O/N-2 ratio increase is substantial in the northern low-middle latitude regions where severe plasma density enhancements occur during the main phase of the storms. Therefore, the ionospheric contribution should be considered for an accurate assessment of the storm time O/N-2 ratio increase at low-middle latitudes during these large storm events. C1 [Lee, Woo Kyoung; Kil, Hyosub; Paxton, Larry J.; Zhang, Yongliang] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Lee, Woo Kyoung] Korea Astron & Space Sci Inst, Taejon, South Korea. [Shim, Ja Soon] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Kil, H (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM hyosub.kil@jhuapl.edu RI Paxton, Larry/D-1934-2015; Kil, Hyosub/C-2577-2016; Zhang, Yongliang/C-2180-2016 OI Paxton, Larry/0000-0002-2597-347X; Kil, Hyosub/0000-0001-8288-6236; Zhang, Yongliang/0000-0003-4851-1662 FU National Radio Research Agency [2013-3-800-02]; National Science Foundation [AGS-1024886] FX W. K. Lee acknowledges support from National Radio Research Agency (2013-3-800-02). H. Kil acknowledges support from National Science Foundation National Space Weather Program (AGS-1024886) grants. Simulation results have been provided by the Community Coordinated Modeling Center (CCMC) at Goddard Space Flight Center through their public Runs on Request system (http://ccmc.gsfc.nasa.gov). The CCMC is a multi-agency partnership between NASA, AFMC, AFOSR, AFRL, AFWA, NOAA, NSF, and ONR. The USU-GAIM Model was developed by the GAIM team (R. W. Schunk, L. Scherliess, J.J. Sojka, D. C. Thompson, and L. Zhu) at Utah State University. NR 14 TC 0 Z9 0 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2013 VL 118 IS 12 BP 7834 EP 7840 DI 10.1002/2013JA019132 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286ZX UT WOS:000329508900037 ER PT J AU Garcia-Fernandez, M Desai, SD Butala, MD Komjathy, A AF Garcia-Fernandez, M. Desai, S. D. Butala, M. D. Komjathy, A. TI Evaluation of different approaches to modeling the second-order ionospheric delay on GPS measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE GPS; reference frame; ionosphere; second order ionospheric effect AB This work evaluates various approaches to compute the second order ionospheric correction (SOIC) to Global Positioning System (GPS) measurements. When estimating the reference frame using GPS, applying this correction is known to primarily affect the realization of the origin of the Earth's reference frame along the spin axis (Z coordinate). Therefore, the Z translation relative to the International Terrestrial Reference Frame 2008 is used as the metric to evaluate various published approaches to determining the slant total electron content (TEC) for the SOIC: getting the slant TEC from GPS measurements, and using the vertical total electron content (TEC) given by a Global Ionospheric Model (GIM) to transform it to slant TEC via a mapping function. All of these approaches agree to 1 mm if the ionospheric shell height needed in GIM-based approaches is set to 600 km. The commonly used shell height of 450 km introduces an offset of 1 to 2 mm. When the SOIC is not applied, the Z axis translation can be reasonably modeled with a ratio of +0.23mm/TEC units of the daily median GIM vertical TEC. Also, precise point positioning (PPP) solutions (positions and clocks) determined with and without SOIC differ by less than 1 mm only if they are based upon GPS orbit and clock solutions that have consistently applied or not applied the correction, respectively. Otherwise, deviations of few millimeters in the north component of the PPP solutions can arise due to inconsistencies with the satellite orbit and clock products, and those deviations exhibit a dependency on solar cycle conditions. C1 [Garcia-Fernandez, M.; Desai, S. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Butala, M. D.; Komjathy, A.] CALTECH, Jet Prop Lab, Ionospher & Atmospher Remote Sensing Grp, Pasadena, CA 91109 USA. RP Garcia-Fernandez, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM miquel.garcia@jpl.nasa.gov FU National Aeronautics and Space Administration FX The work described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration ((c) 2013 California Institute of Technology. Government sponsorship is acknowledged). The authors would like to thank the reviewers for their comments, which helped to improve the manuscript. NR 23 TC 5 Z9 5 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2013 VL 118 IS 12 BP 7864 EP 7873 DI 10.1002/2013JA019356 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286ZX UT WOS:000329508900040 ER PT J AU Immel, TJ Mannucci, AJ AF Immel, T. J. Mannucci, A. J. TI Ionospheric redistribution during geomagnetic storms SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE ionosphere; GPS; TEC; geomagnetic storms; ion outflow; Dst ID TOTAL ELECTRON-CONTENT; SEMIANNUAL VARIATION; FUV DAYGLOW; MIDLATITUDE; LATITUDE; PLASMA; MODEL; PERTURBATIONS; THERMOSPHERE; DISTURBANCE AB The abundance of plasma in the daytime ionosphere is often seen to grow greatly during geomagnetic storms. Recent reports suggest that the magnitude of the plasma density enhancement depends on the UT of storm onset. This possibility is investigated over a 7year period using global maps of ionospheric total electron content (TEC) produced at the Jet Propulsion Laboratory. The analysis confirms that the American sector exhibits, on average, larger storm time enhancement in ionospheric plasma content, up to 50% in the afternoon middle-latitude region and 30% in the vicinity of the high-latitude auroral cusp, with largest effect in the Southern Hemisphere. We investigate whether this effect is related to the magnitude of the causative magnetic storms. Using the same advanced Dst index employed to sort the TEC maps into quiet and active (Dst<-100 nT) sets, we find variation in storm strength that corresponds closely to the TEC variation but follows it by 3-6h. For this and other reasons detailed in this report, we conclude that the UT-dependent peak in storm time TEC is likely not related to the magnitude of external storm time forcing but more likely attributable to phenomena such as the low magnetic field in the South American region. The large Dst variation suggests a possible system-level effect of the observed variation in ionospheric storm response on the measured strength of the terrestrial ring current, possibly connected through UT-dependent modulation of ion outflow. C1 [Immel, T. J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Mannucci, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Immel, TJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM immel@ssl.berkeley.edu FU NSF [AGS-1103333, AST-1019065] FX T.J.I. would like to acknowledge the support of NSF grants AGS-1103333 and AST-1019065 for this research. T.J.I. would also like to thank Tami Kovalek and Dieter Blitza at GSFC who provided ample assistance with accessing the TEC Common Data Format files using IDL. Research conducted at the Jet Propulsion Laboratory was performed under contract to the National Aeronautics and Space Administration. NR 62 TC 9 Z9 9 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2013 VL 118 IS 12 BP 7928 EP 7939 DI 10.1002/2013JA018919 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286ZX UT WOS:000329508900046 ER PT J AU Nogueira, PAB Abdu, MA Souza, JR Bailey, GJ Batista, IS Shume, EB Denardini, CM AF Nogueira, P. A. B. Abdu, M. A. Souza, J. R. Bailey, G. J. Batista, I. S. Shume, E. B. Denardini, C. M. TI Longitudinal variation in Global Navigation Satellite Systems TEC and topside ion density over South American sector associated with the four-peaked wave structures SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE four-peaked structure; ionospheric modeling; TEC ID PLASMASPHERE IONOSPHERE MODEL; TOTAL ELECTRON-CONTENT; EQUATORIAL F-REGION; LATITUDE IONOSPHERE; DRIFT VELOCITIES; SOLAR-ACTIVITY; IONIZATION; MINIMUM; ISSUES; RADAR AB Recent observations of the low-latitude ionospheric electron density revealed a four-peaked longitudinal structure in the equatorial ionization anomaly when plotted at a constant-local-time frame. It was proposed that neutral wind-driven E region dynamo electric fields due to nonmigrating tidal modes are responsible for this pattern. We examine the four-peaked structure in the observed topside ion density and its manifestation as longitudinal structures in total electron content (TEC) over South America. The strong longitudinal variation in TEC characterized by larger value over Brazilian eastern longitude sector as compared to that over the Peruvian western longitude is modeled using the Sheffield University plasmasphere-ionosphere model (SUPIM) aiming to identify the control factors responsible for the longitude variation. We found that the SUPIM runs using as input the existing standard models of vertical drift, and thermospheric winds do not explain the TEC longitudinal structure. Realistic values of these control parameters were generated based on the strong vertical drift longitudinal variation as determined from magnetometer and Digisonde data and appropriately adjusted winds (horizontal wind model). These realistic vertical drifts together with the modified thermospheric wind, when used as input to the SUPIM, are found to satisfactorily explain the longitudinal differences in the TEC and topside ion density (Ni) over South America. The study shows that the TEC in the whole latitude distribution is larger over the east coast than over the west coast of South America and that the vertical drift and thermospheirc winds control the longitudinal four wave structure in the TEC and Ni. C1 [Nogueira, P. A. B.; Abdu, M. A.; Souza, J. R.; Batista, I. S.; Denardini, C. M.] Inst Nacl Pesquisas Espaciais, Div Aeron, Sao Jose Dos Campos, Brazil. [Bailey, G. J.] Univ Sheffield, Dept Appl Math, Sheffield, S Yorkshire, England. [Shume, E. B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Nogueira, PAB (reprint author), Inst Nacl Pesquisas Espaciais, Div Aeron, Av Astronautas 1758, BR-12227010 Sao Paulo, Brazil. EM paulo@dae.inpe.br RI Batista, Inez/F-2899-2012; Nogueira, Paulo/N-4433-2013; Shume, Esayas/I-3354-2013; De Nardin, Clezio/C-4103-2012; OI Nogueira, Paulo/0000-0003-0810-1044; De Nardin, Clezio/0000-0002-3624-2461; Shume, Esayas/0000-0002-4696-1283 FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ) [141.526/2010-6]; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo [2013/01924-1]; CNPq/MCTI [305242/2011-3]; FAPESP [2012/08445-9]; Center for Space Sciences at the University of Texas at Dallas; NSF through Cornell University [AGS-0905448] FX P.A.B Nogueira acknowledges the support from Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ) for his Ph.D. program through process 141.526/2010-6. This work has also been supported by the Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (2013/01924-1). C. M. Denardini thanks CNPq/MCTI (grant 305242/2011-3) and FAPESP (grant 2012/08445-9). We would like to acknowledge the NOAA for the F10.7 data availability. We gratefully acknowledge the Center for Space Sciences at the University of Texas at Dallas and the U.S. Air Force for providing the DMSP thermal plasma data. The Jicamarca Radio Observatory is a facility of the Instituto Geofisico del Peru operated with support from the NSF AGS-0905448 through Cornell University. NR 63 TC 6 Z9 6 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2013 VL 118 IS 12 BP 7940 EP 7953 DI 10.1002/2013JA019266 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 286ZX UT WOS:000329508900047 ER PT J AU Farrell, WM Hurley, DM Hodges, RR Killen, RM Halekas, JS Zimmerman, MI Delory, GT AF Farrell, W. M. Hurley, D. M. Hodges, R. R. Killen, R. M. Halekas, J. S. Zimmerman, M. I. Delory, G. T. TI Redistribution of lunar polar water to mid-latitudes and its role in forming an OH veneer SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Workshop on Dust, Atmospheres, and Plasma - The Moon and Small Bodies (DAP) CY JUN 06-08, 2012 CL Boulder, CO SP NASA Lunar Sci Inst, Colorado Ctr Lunar Dust & Atmospher Studies, Moon Express, Ball Aerosp & Technologies Corp, Lockheed Martin Corp DE Moon; Lunar poles; Sputtering; Impact vaporization; Desorption; Transport ID MOON; ICE; REGIONS; ATMOSPHERE; MERCURY AB We suggest that energization processes like ion sputtering and impact vaporization can eject/release polar water molecules residing within cold trapped regions with sufficient velocity to allow their redistribution to mid-latitudes. We consider the possibility that these polar-ejected molecules can contribution to the water/OH veneer observed as a 3 mu m IR absorption feature at mid-latitudes by Chandrayaan-1, Cassini, and EPDXI. We find this source cannot fully account for the observed IR feature, but could be a low intensity additional source. Published by Elsevier Ltd. C1 [Farrell, W. M.; Killen, R. M.; Zimmerman, M. I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hurley, D. M.] Johns Hopkins Applied Phys Lab, Laurel, MD USA. [Hodges, R. R.] Univ Colorado, Boulder, CO 80309 USA. [Halekas, J. S.; Delory, G. T.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Farrell, W. M.; Hurley, D. M.; Hodges, R. R.; Killen, R. M.; Halekas, J. S.; Zimmerman, M. I.; Delory, G. T.] NASA, Lunar Sci Inst, Moffett Field, CA USA. [Zimmerman, M. I.] Oak Ridge Associated Univ, Oak Ridge, TN USA. RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM william.m.farrell@nasa.gov RI Farrell, William/I-4865-2013; Hurley, Dana/F-4488-2015; OI Hurley, Dana/0000-0003-1052-1494; Halekas, Jasper/0000-0001-5258-6128 NR 30 TC 7 Z9 7 U1 0 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD DEC PY 2013 VL 89 BP 15 EP 20 DI 10.1016/j.pss.2013.05.009 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 287QW UT WOS:000329558300003 ER PT J AU Chi, PJ Russell, CT Wei, HY Farrell, WM AF Chi, P. J. Russell, C. T. Wei, H. Y. Farrell, W. M. TI Observations of narrowband ion cyclotron waves on the surface of the Moon in the terrestrial magnetotail SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Workshop on Dust, Atmospheres, and Plasma - The Moon and Small Bodies (DAP) CY JUN 06-08, 2012 CL Boulder, CO SP NASA Lunar Sci Inst, Colorado Ctr Lunar Dust & Atmospher Studies, Moon Express, Ball Aerosp & Technologies Corp, Lockheed Martin Corp DE Moon; Apollo Lunar Surface Magnetometers; Earth's magnetotail; Ion cyclotron waves ID UPSTREAM ULF WAVES; LUNAR ATMOSPHERE; MAGNETIC-FIELD; MAGNETOMETER; PLASMA; POLARIZATION; PROPAGATION; WAKE AB By examining the data collected by the Apollo 15 and 16 Lunar Surface Magnetometers between April and July of 1972, we have found a class of narrowband waves observed at the surface of the Moon. With frequencies ranging from 0.04 to 0.17 Hz, these narrowband waves were present only when the Moon was in the terrestrial magnetotail, and the wave properties are consistent with those of ion cyclotron waves. We propose two scenarios where anisotropies of ion temperature can occur in the vicinity of the Moon to excite the ion cyclotron waves observed at the lunar surface. Simultaneous observations at the Apollo 15 and 16 sites revealed small but persistent differences in wave amplitude and phase, suggesting that the wave signals were modified by the mini-magnetosphere above the Apollo 16 site. It is also suggested that subsurface electrical conductivity may possibly be involved in the amplitude change and small phase difference between the two sites. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Chi, P. J.; Russell, C. T.; Wei, H. Y.] Univ Calif Los Angeles, Dept Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Chi, PJ (reprint author), Univ Calif Los Angeles, Dept Geophys & Planetary Phys, Los Angeles, CA 90024 USA. EM pchi@igpp.ucla.edu RI Farrell, William/I-4865-2013 NR 40 TC 1 Z9 1 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD DEC PY 2013 VL 89 BP 21 EP 28 DI 10.1016/j.pss.2013.08.020 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 287QW UT WOS:000329558300004 ER PT J AU Glaser, P Haase, I Oberst, J Neumann, GA AF Glaeser, P. Haase, I. Oberst, J. Neumann, G. A. TI Co-registration of laser altimeter tracks with digital terrain models and applications in planetary science SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Workshop on Dust, Atmospheres, and Plasma - The Moon and Small Bodies (DAP) CY JUN 06-08, 2012 CL Boulder, CO SP NASA Lunar Sci Inst, Colorado Ctr Lunar Dust & Atmospher Studies, Moon Express, Ball Aerosp & Technologies Corp, Lockheed Martin Corp DE Co-registration; LOLA; Laser; DTM; LROC ID LUNAR RECONNAISSANCE ORBITER; MARS; ADJUSTMENT; LANDER AB We have derived algorithms and techniques to precisely co-register laser altimeter profiles with gridded Digital Terrain Models (DTMs), typically derived from stereo images. The algorithm consists of an initial grid search followed by a least-squares matching and yields the translation parameters at sub-pixel level needed to align the DTM and the laser profiles in 3D space. This software tool was primarily developed and tested for co-registration of laser profiles from the Lunar Orbiter Laser Altimeter (LOLA) with DTMs derived from the Lunar Reconnaissance Orbiter (LRO) Narrow Angle Camera (NAC) stereo images. Data sets can be co-registered with positional accuracy between 0.13 m and several meters depending on the pixel resolution and amount of laser shots, where rough surfaces typically result in more accurate co-registrations. Residual heights of the data sets are as small as 0.18 m. The software can be used to identify instrument misalignment, orbit errors, pointing jitter, or problems associated with reference frames being used. Also, assessments of DTM effective resolutions can be obtained. From the correct position between the two data sets, comparisons of surface morphology and roughness can be made at laser footprint- or DTM pixel-level. The precise co-registration allows us to carry out joint analysis of the data sets and ultimately to derive merged high-quality data products. Examples of matching other planetary data sets, like LOLA with LRO Wide Angle Camera (WAC) DTMs or Mars Orbiter Laser Altimeter (MOLA) with stereo models from the High Resolution Stereo Camera (HRSC) as well as Mercury Laser Altimeter (MLA) with Mercury Dual Imaging System (MDIS) are shown to demonstrate the broad science applications of the software tool. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Glaeser, P.; Haase, I.; Oberst, J.] Tech Univ Berlin, Dept Geodesy & Geoinformat Sci, D-10623 Berlin, Germany. [Oberst, J.] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany. [Neumann, G. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Glaser, P (reprint author), Tech Univ Berlin, Dept Geodesy & Geoinformat Sci, Str 17 Juni 135, D-10623 Berlin, Germany. EM philipp.glaeser@tu-berlin.de RI Neumann, Gregory/I-5591-2013 OI Neumann, Gregory/0000-0003-0644-9944 NR 30 TC 6 Z9 6 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD DEC PY 2013 VL 89 BP 111 EP 117 DI 10.1016/j.pss.2013.09.012 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 287QW UT WOS:000329558300014 ER PT J AU Posner, A Odstrcil, D MacNeice, P Rastaetter, L Zeitlin, C Heber, B Elliott, H Frahm, RA Hayes, JJE von Rosenvinge, TT Christian, ER Andrews, JP Beaujean, R Bottcher, S Brinza, DE Bullock, MA Burmeister, S Cucinotta, FA Ehresmann, B Epperly, M Grinspoon, D Guo, J Hassler, DM Kim, MH Kohler, J Kortmann, O Garcia, CM Muller-Mellin, R Neal, K Rafkin, SCR Reitz, G Seimetz, L Smith, KD Tyler, Y Weigle, E Wimmer-Schweingruber, RF AF Posner, A. Odstrcil, D. MacNeice, P. Rastaetter, L. Zeitlin, C. Heber, B. Elliott, H. Frahm, R. A. Hayes, J. J. E. von Rosenvinge, T. T. Christian, E. R. Andrews, J. P. Beaujean, R. Boettcher, S. Brinza, D. E. Bullock, M. A. Burmeister, S. Cucinotta, F. A. Ehresmann, B. Epperly, M. Grinspoon, D. Guo, J. Hassler, D. M. Kim, M. -H. Koehler, J. Kortmann, O. Garcia, C. Martin Mueller-Mellin, R. Neal, K. Rafkin, S. C. R. Reitz, G. Seimetz, L. Smith, K. D. Tyler, Y. Weigle, E. Wimmer-Schweingruber, R. F. TI The Hohmann-Parker effect measured by the Mars Science Laboratory on the transfer from Earth to Mars: Consequences and opportunities SO PLANETARY AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Workshop on Dust, Atmospheres, and Plasma - The Moon and Small Bodies (DAP) CY JUN 06-08, 2012 CL Boulder, CO SP NASA Lunar Sci Inst, Colorado Ctr Lunar Dust & Atmospher Studies, Moon Express, Ball Aerosp & Technologies Corp, Lockheed Martin Corp DE Hohmann transit; Parker field; Magnetic connection; Cosmic rays; Solar wind; Inner heliosphere ID INTERPLANETARY MAGNETIC-FIELD; ROTATING RAREFACTION REGIONS; HIGH-ENERGY TELESCOPE; COSMIC-RAY DECREASES; SOLAR-WIND STREAM; CORONAL HOLE; MASS EJECTIONS; SUN; ULYSSES; STEREO AB We show that a spacecraft launched from Earth towards Mars following a Hohmann minimum energy transfer trajectory has a strong tendency to remain well-connected magnetically to Earth, in the early phase of the transfer, or to Mars in the late phase, via the Parker spiral magnetic field. On the return trip, the spacecraft would remain reasonably well-connected magnetically first to Mars and later to Earth. Moreover, good magnetic connectivity occurs on all Hohmann transfers between neighboring planets in the inner solar system out to Mars. We call this hitherto unnamed circumstance the Hohmann-Parker effect. We show consequences of the effect by means of simultaneous cosmic radiation proxy observations made near Earth, near Mars, and at the Mars Science Laboratory on the transfer from Earth to Mars in 2011/2012. We support the observations with simulations of the large-scale magnetic field of the inner heliosphere during this period and compare the results with our predictions. The implications of the Hohmann-Parker effect are discussed. (C) 2013 Published by Elsevier Ltd. C1 [Posner, A.; Hayes, J. J. E.] NASA Headquarters, Sci Miss Directorate, Washington, DC 20548 USA. [Odstrcil, D.; MacNeice, P.; Rastaetter, L.; Christian, E. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Odstrcil, D.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Zeitlin, C.; Andrews, J. P.; Bullock, M. A.; Ehresmann, B.; Hassler, D. M.; Neal, K.; Rafkin, S. C. R.] SW Res Inst, Space Sci & Engn Div, Boulder, CO 80302 USA. [Heber, B.; Beaujean, R.; Boettcher, S.; Burmeister, S.; Guo, J.; Koehler, J.; Garcia, C. Martin; Mueller-Mellin, R.; Seimetz, L.; Wimmer-Schweingruber, R. F.] Univ Kiel, Inst Expt & Angew Phys, D-24118 Kiel, Germany. [Elliott, H.; Frahm, R. A.; Epperly, M.; Smith, K. D.; Tyler, Y.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78228 USA. [Brinza, D. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA. [Cucinotta, F. A.] Univ Nevada, Dept Hlth Phys, Las Vegas, NV 89154 USA. [Grinspoon, D.] Denver Museum Nat & Sci, Denver, CO 80205 USA. [Kim, M. -H.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Kortmann, O.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Reitz, G.] Deutsch Zentrum Luft & Raumfahrt, D-51147 Cologne, Germany. [Weigle, E.] Big Head Endian LLC, Burden, KS 67019 USA. RP Posner, A (reprint author), NASA Headquarters, Sci Miss Directorate, 300 E St SW, Washington, DC 20548 USA. EM arik.posner@nasa.gov; dusan.odstrcil@nasa.gov; peter.j.macneice@nasa.gov; lutz.rastaetter@nasa.gov; zeitlin@boulder.swri.edu; heber@physik.uni-kiel.de; helliott@swri.edu; rfrahm@swri.edu; jhayes@nasa.gov; tycho.t.vonrosenvinge@nasa.gov; eric.r.christian@nasa.gov; andrews@boulder.swri.edu; rudolf@rbeau.de; boettcher@physik.uni-kiel.de; david.e.brinza@jpl.nasa.gov; bullock@boulder.swri.edu; burmeister@physik.uni-kiel.de; francis.cucinotta@unlv.edu; ehresmann@boulder.swri.edu; mepperly@swri.edu; dgrinspoon@dmns.org; guo@physik.uni-kiel.de; hassler@boulder.swri.edu; myung-hee.y.kim@nasa.gov; koehler@physik.uni-kiel.de; onno@ssl.berkeley.edu; martin@physik.uni-kiel.de; mueller-mellin@physik.uni-kiel.de; kneal@boulder.swri.edu; rafkin@boulder.swri.edu; guenther.reitz@dlr.de; seimetz@physik.uni-kiel.de; kdsmith@swri.edu; ytyler@swri.edu; eddie@bigheadendian.com; wimmer@physik.uni-kiel.de RI Rastaetter, Lutz/D-4715-2012; OI Rastaetter, Lutz/0000-0002-7343-4147; Posner, Arik/0000-0003-1572-8734; Kim, Myung-Hee/0000-0001-5575-6858 NR 68 TC 6 Z9 6 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD DEC PY 2013 VL 89 BP 127 EP 139 DI 10.1016/j.pss.2013.09.013 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 287QW UT WOS:000329558300016 ER PT J AU Dennison, PE Thorpe, AK Pardyjak, ER Roberts, DA Qi, Y Green, RO Bradley, ES Funk, CC AF Dennison, Philip E. Thorpe, Andrew K. Pardyjak, Eric R. Roberts, Dar A. Qi, Yi Green, Robert O. Bradley, Eliza S. Funk, Christopher C. TI High spatial resolution mapping of elevated atmospheric carbon dioxide using airborne imaging spectroscopy: Radiative transfer modeling and power plant plume detection SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE AVIRIS C; AVIRIS NG; MODTRAN; Noise equivalent delta radiance; Hyperspectral data; Imaging spectroscopy; CO2 emissions; Fossil fuel power plant ID WATER-VAPOR; SPECTROMETER AVIRIS; METHANE EMISSIONS; FIRE DETECTION; CO2 EMISSIONS; PART 1; RETRIEVALS; GASES; SPACE; VEGETATION AB Carbon dioxide is emitted from the combustion of fossil fuels and is an important contributor to anthropogenic climate change. Multiple current and planned satellite missions are designed to quantify atmospheric carbon dioxide concentrations on a global scale, but most of these sensors do not have the spatial resolution necessary to resolve point sources such as fossil fuel power plants. Airborne imaging spectrometer data, such as those from the Airborne Visible InfraRed Imaging Spectrometer (AVIRIS), can have multiple, contiguous bands covering shortwave infrared (SWIR) absorption features produced by carbon dioxide. Therefore, high spatial resolution data from AVIRIS-like sensors may offer a means for detecting plumes and retrieving carbon dioxide concentrations for point source emissions. The objectives of this study include modeling minimum carbon dioxide anomalies detectable in AVIRIS data under different conditions and applying a Cluster-Tuned Matched Filter for detection of carbon dioxide plumes in simulated data and in AVIRIS images acquired over power plants. Radiative transfer simulations were used to model the residual radiance produced by increased absorption by carbon dioxide as concentration was elevated above background levels within a 0-500 m layer. Carbon dioxide anomalies, surface reflectance, water vapor concentration, solar zenith angle, sensor height, and aerosol scattering were varied in simulation sets and the resulting residual radiance spectra were compared against noise equivalent delta radiance (NEdL) for the "classic" and "next generation" AVIRIS instruments. Sensitivity to carbon dioxide anomalies improved with increased surface reflectance and declined with increased water vapor concentration, solar zenith angle, sensor height, and aerosol scattering. Zero to 500 m concentration anomalies as low as 100 parts per milion by volume (ppm) for AVIRIS C and 25 ppm for AVIRIS NG produced residual radiance values that exceeded SWIR NEdL Carbon dioxide concentrations modeled for a generic power plant emissions scenario using a plume dispersion model were combined with randomly-generated reflectance spectra to create simulated images with varying surface reflectance and NEdL For these simulated images, true positive and false positive detection rates improved as background reflectance increased and as NEdL decreased. Apparent plumes were detected in all four AVIRIS C images acquired over power plants, although the characteristics of the plumes varied according to solar-plume-sensor geometry. Improvements in modeling may allow retrieval of plume concentration, providing a valuable means for quantifying point source emissions and a basis for comparison with column concentrations retrieved from in situ measurements and coarse resolution satellite data. (C) 2013 Elsevier Inc. All rights reserved. C1 [Dennison, Philip E.; Qi, Yi] Univ Utah, Dept Geog, Salt Lake City, UT 84112 USA. [Thorpe, Andrew K.; Roberts, Dar A.; Bradley, Eliza S.; Funk, Christopher C.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA. [Pardyjak, Eric R.] Univ Utah, Dept Mech Engn, Salt Lake City, UT 84112 USA. [Green, Robert O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dennison, PE (reprint author), Univ Utah, Dept Geog, 260 S Cent Campus Dr,Room 270, Salt Lake City, UT 84112 USA. EM dennison@geog.utah.edu RI Qi, Yi/L-8492-2013; OI Qi, Yi/0000-0001-8077-3350; Dennison, Philip/0000-0002-0241-1917 FU NASA [NNX13AK85A] FX We would like to acknowledge the assistance of Lex Berk of Spectral Science, Inc. in developing the MODTRAN simulations. Partial funding for this research was provided by NASA grant #NNX13AK85A. NR 55 TC 7 Z9 7 U1 2 U2 28 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC PY 2013 VL 139 BP 116 EP 129 DI 10.1016/j.rse.2013.08.001 PG 14 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 285TK UT WOS:000329417700010 ER PT J AU Claverie, M Vermote, EF Weiss, M Baret, F Hagolle, O Demarez, V AF Claverie, Martin Vermote, Eric F. Weiss, Marie Baret, Frederic Hagolle, Olivier Demarez, Valerie TI Validation of coarse spatial resolution LAI and FAPAR time series over cropland in southwest France SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE LAI; GAI; FAPAR; Essential Climate Variables; Green Area Index; Radiative transfer model; PROSAIL; MODIS; Formosat-2; Crop; Validation; Surface reflectance; BRDF ID LEAF-AREA INDEX; ESSENTIAL CLIMATE VARIABLES; CANOPY REFLECTANCE MODELS; CYCLOPES GLOBAL PRODUCTS; SATELLITE IMAGERY; MODIS DATA; GEOV1 LAI; IN-SITU; PART 2; VEGETATION AB This study aims at validating Leaf Area Index (LAI) and Fraction of Absorbed Photosynthetically Active Radiation (FAPAR) products derived from MODIS surface reflectance (MOD09CMG) at coarse resolution (0.05) over crops. These Essential Climate Variables (ECVs) are estimated by using the inversion of the PROSAIL radiative transfer (BV-NNET tool) applied on MODIS BRDF (Bidirectional Reflectance Distribution Function) corrected surface reflectances and non-corrected. ECV estimates and the corresponding MCD15A3 Collection 5 and GEOLAND-2 (GE0v1) products are compared with ECV reference maps derived from BV-NNET applied on 105 high spatial resolution images (Formosat-2, 8 m) which were acquired from 2006 to 2010 in Southwest France. These latter are compared with local scale in situ measurements. The validation shows an uncertainty of 035 and 0.07 for LAI and FAPAR, respectively. The comparison shows that the ECV estimates from the three products properly capture the crops phenology in agreement with reference maps. Results indicate that MCD15A3 uncertainties (023 and 0.07 for LAI and FAPAR, respectively) are similar to previous intercomparison studies. GE0v1 shows a systemic positive bias for both LAI and FAPAR. The best agreement with the reference maps is found for MODIS BV-NNET products with r2 higher than 0.9 and relative uncertainties lower than 17%. The use of BRDF-corrected surface reflectances as input of BV-NNET tool improves the uncertainty of LAI estimates (0.11, compared to 0.17 when directional surface reflectances are used as input) but not the uncertainty of FAPAR estimates. The deviation between FAPAR products which mostly.affects low winter FAPAR, is related to the discrepancy of the soil directional assumption in PROSAIL model and BRDF correction method. The temporal stability of the daily MODIS BV-NNET products is better than the 4-day composite MCD15A3 products. Finally, BV-NNET tool applied at finer resolutions demonstrates that the increase of the resolution results in a decrease of the LAI and FAPAR uncertainties and a conservation of the biases. (C) 2013 Elsevier Inc. All rights reserved. C1 [Claverie, Martin] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Claverie, Martin; Vermote, Eric F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Weiss, Marie; Baret, Frederic] EMMAH, INRA UMR 1114, F-84914 Avignon, France. [Hagolle, Olivier; Demarez, Valerie] CESBIO, UMR CNES CNRS IRD UPS, F-31401 Toulouse 4, France. RP Claverie, M (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. EM martin.claverie@nasa.gov RI Baret, Fred/C-4135-2011; OI Baret, Fred/0000-0002-7655-8997; Claverie, Martin/0000-0001-9479-3205; Weiss, Marie/0000-0002-2341-667X NR 54 TC 39 Z9 40 U1 3 U2 33 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC PY 2013 VL 139 BP 216 EP 230 DI 10.1016/j.rse.2013.07.027 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 285TK UT WOS:000329417700018 ER PT J AU Hayashida, S Ono, A Yoshizaki, S Frankenberg, C Takeuchi, W Yan, X AF Hayashida, S. Ono, A. Yoshizaki, S. Frankenberg, C. Takeuchi, W. Yan, X. TI Methane concentrations over Monsoon Asia as observed by SCIAMACHY: Signals of methane emission from rice cultivation SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Methane; SCIAMACHY; Monsoon Asia; Rice paddies; Atmosphere ID ATMOSPHERIC METHANE; VEGETATION; PADDIES AB We have analyzed the column-averaged CH4 concentration (xCH(4)) using scanning imaging absorption spectrometer for atmospheric chartography (SCIAMACHY) and compared the data with the bottom-up emission inventory data sets and other satellite-derived indices such as the land-surface water coverge (LSWC) and the normalized difference vegetation index (NDVI). The geographical distribution of high CH4 values corresponds to strong emissions from regions where rice is cultivated, as indicated in the inventory maps. The Pearson's correlation coefficients (r) between xCH(4) and the rice emission inventory data are observed to be greater than similar to 0.6 over typical rice fields, with outstanding r-values of similar to 0.8 in the Ganges Basin, Myanmar, and Thailand. This suggests that the emission of CH4 from rice cultivation mainly controls the seasonality of the CH4 concentration over such regions. The correlation between xCH(4) and LSWC and NDVI is also as large as 0.6. In Southeast Asia, the r-values of xCH4 with bottom-up inventory data that includes all categories are not as high as those with the emission, as estimated from the rice category only. This is indicative of the relative importance of rice emissions among all other emission categories in Southeast Asia. (C) 2013 Elsevier Inc. All rights reserved. C1 [Hayashida, S.; Ono, A.; Yoshizaki, S.] Nara Womens Univ, Fac Sci, Kitauoya Nishimachi, Nara 6308506, Japan. [Frankenberg, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Takeuchi, W.] Univ Tokyo, Inst Ind Sci, Meguro Ku, Tokyo 1538505, Japan. [Yan, X.] Chinese Acad Sci, Inst Soil Sci, State Key Lab Soil & Sustainable Agr, Nanjing, Jiangsu, Peoples R China. RP Hayashida, S (reprint author), Nara Womens Univ, Fac Sci, Kitauoya Nishimachi, Nara 6308506, Japan. EM sachiko@ics.nara-wu.ac.jp RI Yan, Xiaoyuan/M-9840-2016; Frankenberg, Christian/A-2944-2013 OI Yan, Xiaoyuan/0000-0001-8645-4836; Frankenberg, Christian/0000-0002-0546-5857 FU Environment Research and Technology Development Fund of the Ministry of the Environment, Japan [A1202]; Green Network of Excellence, Environmental Information (GRENE-el) program FX We express our gratitude to Ms. H. Araki for her help with data analysis and drawing figures. This study was supported by a Grant-in-Aid from the Green Network of Excellence, Environmental Information (GRENE-el) program. This research was also supported by the Environment Research and Technology Development Fund of the Ministry of the Environment, Japan (A1202). Finally, we wish to thank the three anonymous reviewers for their valuable suggestions that have improved this manuscript significantly. NR 29 TC 8 Z9 8 U1 3 U2 30 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC PY 2013 VL 139 BP 246 EP 256 DI 10.1016/j.rse.2013.08.008 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 285TK UT WOS:000329417700020 ER PT J AU Schwaller, MR Southwell, CJ Emmerson, LM AF Schwaller, Mathew R. Southwell, Colin J. Emmerson, Louise M. TI Continental-scale mapping of Adelie penguin colonies from Landsat imagery SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Adelie penguin; Antarctica; Landsat; ETM; Penguin ID EAST ANTARCTICA; SOUTHERN-OCEAN; ENDERBY LAND; POPULATIONS; ROOKERIES; PERFORMANCE; ABUNDANCE; ISLANDS; CLIMATE AB Breeding distribution of the Adelie penguin, Pygoscelis adeliae, was surveyed with Landsat-7 Enhanced Thematic Mapper Plus (ETM+) data in an area covering approximately 330 degrees of longitude along the coastline of Antarctica. An algorithm was designed to minimize radiometric noise and to retrieve Adelie penguin colony location and spatial extent from the ETM+ data. In all, 9143 individual pixels were classified as belonging to an Adelie penguin colony class out of the entire dataset of 195 ETM+ scenes, where the dimension of each pixel is 30 m by 30 m, and each scene is approximately 180 km by 180 km. Pixel clustering identified a total of 187 individual Adelie penguin colonies, ranging in size from a single pixel (900 m(2)) to a maximum of 875 pixels (0.788 km(2)). Colony retrievals have a very low error of commission, on the order of 1% or less, and the error of omission was estimated to be similar to 3 to 4% by population based on comparisons with direct observations from surveys across east Antarctica. Thus, the Landsat retrievals successfully located Adelie penguin colonies that accounted for similar to 96 to 97% of the regional population used as ground truth. Geographic coordinates and the spatial extent of each colony retrieved from the Landsat data are available publically. Regional analysis found several areas where the Landsat retrievals suggest populations that are significantly larger than published estimates. Six Adelie penguin colonies were found that are believed to be previously unreported in the literature. Published by Elsevier Inc. C1 [Schwaller, Mathew R.] NASA GSFC, Greenbelt, MD 20771 USA. [Southwell, Colin J.; Emmerson, Louise M.] Australian Antarctic Div, Kingston, Tas 7050, Australia. RP Schwaller, MR (reprint author), NASA GSFC, Mail Code 587, Greenbelt, MD 20771 USA. EM mathew.r.schwaller@nasa.gov; colin.southwell@aad.gov.au; louise.emmerson@aad.gov.au FU NASA Headquarters FX The direct survey in east Antarctica was conducted under AAD ASAC project 2722 in accordance with permits issued under the Antarctic Treaty (Environmental Protection) Act 1980 and was approved by the Australian Antarctic Ethics Committee. We thank Mr. Woody Turner of NASA Headquarters for funding the publication of this paper. We also thank three anonymous reviewers for their insightful comments and suggestions, as well as Paul Ensor for sharing his observations of Mt. Biscoe and the Mackellar Islands in the 1980s, and Gary Geller, Heather Lynch, and Phil Trathan for helpful comments on a preliminary version of the manuscript. NR 47 TC 15 Z9 16 U1 0 U2 24 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC PY 2013 VL 139 BP 353 EP 364 DI 10.1016/j.rse.2013.08.009 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 285TK UT WOS:000329417700029 ER PT J AU Duncan, BN Yoshida, Y de Foy, B Lamsal, LN Streets, DG Lu, ZF Pickering, KE Krotkov, NA AF Duncan, Bryan N. Yoshida, Yasuko de Foy, Benjamin Lamsal, Lok N. Streets, David G. Lu, Zifeng Pickering, Kenneth E. Krotkov, Nickolay A. TI The observed response of Ozone Monitoring Instrument (OMI) NO2 columns to NOx emission controls on power plants in the United States: 2005-2011 SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Ozone Monitoring Instrument; Nitrogen dioxide; Air quality; Space-based observations; Power plant emissions; Emission control devices ID RETRIEVAL; SPACE AB We show that Aura Ozone Monitoring Instrument (OMI) nitrogen dioxide (NO2) tropospheric column data may be used to assess changes of the emissions of nitrogen oxides (NOx) from power plants in the United States, though careful interpretation of the data is necessary. There is a clear response for OMI NO2 data to NOx emission reductions from power plants associated with the implementation of mandated emission control devices (ECDs) over the OMI record (2005-2011). This response is scalar for all intents and purposes, whether the reduction is rapid or incremental over several years. However, it is variable among the power plants, even for those with the greatest absolute decrease in emissions. We document the primary causes of this variability, presenting case examples for specific power plants. Published by Elsevier Ltd. C1 [Duncan, Bryan N.; Yoshida, Yasuko; Lamsal, Lok N.; Pickering, Kenneth E.; Krotkov, Nickolay A.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. [Yoshida, Yasuko] Sci Syst & Applicat Inc, Lanham, MD USA. [de Foy, Benjamin] St Louis Univ, St Louis, MO 63103 USA. [Lamsal, Lok N.] Univ Space Res Assoc, Goddard Earth Sci Technol Ee Res, Columbia, MD USA. [Streets, David G.; Lu, Zifeng] Argonne Natl Lab, Argonne, IL 60439 USA. RP Duncan, BN (reprint author), NASA, Goddard Space Flight Ctr, Code 614, Greenbelt, MD 20771 USA. EM Bryan.N.Duncan@nasa.gov RI Lu, Zifeng/F-3266-2012; Pickering, Kenneth/E-6274-2012; de Foy, Benjamin/A-9902-2010; Krotkov, Nickolay/E-1541-2012; Duncan, Bryan/A-5962-2011; OI de Foy, Benjamin/0000-0003-4150-9922; Krotkov, Nickolay/0000-0001-6170-6750; Streets, David/0000-0002-0223-1350 FU NASA Air Quality Applied Sciences Team (AQAST) program FX This work was funded by the NASA Air Quality Applied Sciences Team (AQAST) program. We acknowledge the free use of 1) tropospheric NO2 column data from the Aura OMI, 2) NOx emissions data from the US EPA, and 3) EDGAR data, which is maintained as a joint project of the European Commission Joint Research Centre (JRC) and the Netherlands Environmental Assessment Agency (PBL). NR 26 TC 23 Z9 23 U1 2 U2 35 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2013 VL 81 BP 102 EP 111 DI 10.1016/j.atmosenv.2013.08.068 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 285EY UT WOS:000329377600013 ER PT J AU Kessner, AL Wang, J Levy, RC Colarco, PR AF Kessner, Amy L. Wang, Jun Levy, Robert C. Colarco, Peter R. TI Remote sensing of surface visibility from space: A look at the United States East Coast SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Visibility; Remote sensing; Aerosol optical depth; MODIS; GEOS-5 ID AEROSOL OPTICAL-THICKNESS; CLEAR-SKY VISIBILITY; PARTICULATE MATTER; AIR-QUALITY; PM2.5 MASS; SATELLITE; DEPTH; MODEL; LAND; ASSIMILATION AB Measurement of surface visibility is important for the management of air quality, human health, and transportation. Currently, visibility measurements are only available through ground-based instrumentation, such as the Automated Surface Observing System (ASOS), and therefore lack spatial coverage. In analogy to the recent work of using satellite-based aerosol optical depth (AOD) to derive surface dry aerosol mass concentration at continental-to-global scale for cloud-free conditions, this study evaluates the potential of AOD retrieved from the MODerate Resolution Imaging Spectroradiometer (MODIS) for deriving surface visibility. For this purpose of evaluation the truncated (up to similar to 16 km or 10 miles) and discrete (at the interval no less than 0.4 km or 1/4 mile) visibility data from hourly operational weather reports are not suitable, and the ASOS-measured one-minute raw surface extinction coefficient (b(ext)) values have to be used. Consequently, a method for quality control on the b(ext) data is first developed to eliminate frequent problems such as extraneous points, poor calibration, and bad formatting, after which reliable b(ext) data are obtained to estimate the surface visibility. Subsequent analysis of the AOD and b(ext) relationship on the East Coast of the United States reveals their average linear correlation coefficient (R) of 0.61 for all twelve (2000-2011) years of data at 32 ASOS stations, with the highest R value in summer and the lowest values in fall and winter. Incorporation of the Goddard Earth Observing System, Version 5 (GEOS-5) modeled vertical profile of aerosols into the derivation of visibility from AOD is evaluated for two methods, one scaling the modeled surface b(ext) with the ratio of MODIS AOD to the modeled AOD, and another scaling the ratio of modeled AOD in the boundary layer to total columnar AOD with the MODIS AOD and assuming well-mixed aerosol extinction in the boundary layer. Analysis with three summers (2003-2004, 2006) of available GEOS-5 data and ASOS data reveals that the second method is superior, and generates a regression model that, after independent evaluation for summer 2005, is found to be statistically robust with R of 0.70 and a mean bias of 0.32 km in derived visibility. This study is among the first to demonstrate the potential of using satellite-based aerosol product over land to operationally derive surface visibility. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Kessner, Amy L.; Wang, Jun] Univ Nebraska, Lincoln, NE 68588 USA. [Levy, Robert C.] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA. [Colarco, Peter R.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. RP Wang, J (reprint author), Univ Nebraska, Lincoln, NE 68588 USA. EM Agehring3@huskers.unl.edu; Jwang7@unl.edu; Robert.c.levy@nasa.gov; Peter.r.colarco@nasa.gov RI Levy, Robert/M-7764-2013; Colarco, Peter/D-8637-2012; Wang, Jun/A-2977-2008 OI Levy, Robert/0000-0002-8933-5303; Colarco, Peter/0000-0003-3525-1662; Wang, Jun/0000-0002-7334-0490 FU NASA; NASA GSFC Graduate Student Summer Program and Senior Internship Program (Kessner); NASA Applied Sciences Program FX This work was partially funded by the NASA Nebraska Space Grant student fellowship and mini-grant program as well as the NASA GSFC Graduate Student Summer Program and Senior Internship Program (Kessner). This research is also partially supported by the NASA Applied Sciences Program managed by Lawrence A. Friedl and John A. Haynes. We thank the data services provided by the Goddard Earth Science Data Center and the National Climate Data Center Online Climate Data Directory. We would like to give a special thanks to the employees of Belfort Instrument, Lorraine A. Remer, Raymond M. Hoff, and R. Bradley Pierce for their guidance and expertise. NR 55 TC 18 Z9 20 U1 4 U2 20 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2013 VL 81 BP 136 EP 147 DI 10.1016/j.atmosenv.2013.08.050 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 285EY UT WOS:000329377600017 ER PT J AU Crumeyrolle, S Weigel, R Sellegri, K Roberts, G Gomes, L Stohl, A Laj, R Momboisse, G Bourianne, T Puygrenier, V Burnet, F Chosson, F Brenguier, JL Etcheberry, JM Villani, P Pichon, JM Schwarzenboeck, A AF Crumeyrolle, S. Weigel, R. Sellegri, K. Roberts, G. Gomes, L. Stohl, A. Laj, R. Momboisse, G. Bourianne, T. Puygrenier, V. Burnet, F. Chosson, F. Brenguier, J. L. Etcheberry, J. M. Villani, P. Pichon, J. M. Schwarzenboeck, A. TI Airborne investigation of the aerosols-cloud interactions in the vicinity and within a marine stratocumulus over the North Sea during EUCAARI (2008) SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Aerosols; CCN; In-situ measurements; Stratocumulus; Activation ID CONDENSATION NUCLEI CCN; MASS-SPECTROMETER; SIZE DISTRIBUTIONS; BOUNDARY-LAYER; NONPRECIPITATING CLOUDS; MINERAL DUST; COLLECTION EFFICIENCIES; CHEMICAL-COMPOSITION; VERTICAL TRANSPORT; PARTICLE FORMATION AB Within the European Aerosol Cloud Climate and Air Quality Interactions (EUCAARI) project, the Meteo France research aircraft ATR-42 was operated from Rotterdam (Netherlands) airport during May 2008, to perform scientific flights dedicated to the investigation of aerosol-cloud interactions. The objective of this study is to illustrate the impact of cloud processing on the aerosol particle physical and chemical properties. The presented results are retrieved from measurements during flight operation with two consecutive flights, first from Rotterdam to Newcastle (United Kingdom) and subsequently reverse along the same waypoints back to Rotterdam using data measured with compact Time of Flight Aerosol Mass Spectrometer (cToF-AMS) and Scanning Mobility Particle Sizer (SMPS). Cloud-related measurements during these flights were performed over the North Sea within as well as in close vicinity of a marine stratocumulus cloud layer. Particle physical and chemical properties observed in the close vicinity, below and above the stratocumulus cloud, show strong differences: (1) the averaged aerosol size distributions, observed above and below the cloud layer, are of bimodal character with pronounced minima between Aitken and accumulation mode, very likely due to cloud processing. (2) the chemical composition of aerosol particles is strongly dependent on the position relative to the cloud layer (vicinity or below/above cloud). In general, the nitrate and organic relative mass fractions decrease with decreasing distance to the cloud, in the transit from cloud free conditions towards the cloud boundaries. This relative mass fraction decrease ranges from a factor of three to ten, thus leading to an increase of the sulfate and ammonium relative mass concentrations while approaching the cloud layer. (3), the chemical composition of cloud droplet residuals, analyzed downstream of a Counterflow virtual Impactor (CVI) inlet indicates increased fractions of mainly soluble chemical compounds such as nitrate and organics, compared to non cloud processed particles. Finally, a net overbalance of nitrate aerosol has been revealed by comparing cloud droplet residual and non cloud processed aerosol chemical compositions. Conclusively, this study highlights gaps concerning the sampling strategy that need to be addressed for the future missions. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Crumeyrolle, S.; Weigel, R.; Sellegri, K.; Laj, R.; Villani, P.; Pichon, J. M.; Schwarzenboeck, A.] Univ Clermont Ferrand, CNRS, Lab Meteorol Phys, UMR6016, Aubiere, France. [Crumeyrolle, S.] NASA, Langley Res Ctr, Hampton, VA 23666 USA. [Weigel, R.] Johannes Gutenberg Univ Mainz, Inst Atmospher Phys, D-55122 Mainz, Germany. [Roberts, G.; Gomes, L.; Momboisse, G.; Bourianne, T.; Puygrenier, V.; Burnet, F.; Brenguier, J. L.; Etcheberry, J. M.] Ctr Natl Rech Meteorol, URA 1357, Toulouse, France. [Stohl, A.] Norwegian Inst Air Res, Kjeller, Norway. [Puygrenier, V.] CNRS, Lab Sci Climat & Environm, F-75700 Paris, France. [Laj, R.] McGill Univ, Dept Atmospher Ocean & Sci, Montreal, PQ, Canada. [Chosson, F.] Univ Grenoble 1, CNRS, Lab Glaciol & Geophys Environm, UMR 5183, Grenoble, France. RP Bourianne, T (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd,MS 483,Bldg 1250,Room 125, Hampton, VA 23681 USA. EM suzanne.crumeyrolle@gmail.com RI Stohl, Andreas/A-7535-2008 OI Stohl, Andreas/0000-0002-2524-5755 FU European Commission [036833-2]; French National Research Agency (ANR) under the AEROCLOUD program [06-BLAN-0209]; CNRS [167641] FX This work has been partially funded by European Commission 6th Framework program project EUCAARI, contract no 036833-2 (EUCAARI), and by the French National Research Agency (ANR) under the AEROCLOUD program, contract no 06-BLAN-0209. Suzanne Crumeyrolle has been supported by CNRS fellowship (contract no167641). The authors wish to thank the SAFIRE (Service des Avions Francais Instruments pour la Recherche en Environnement) for preparing and delivering the research aircraft (ATR-42). NR 85 TC 1 Z9 1 U1 1 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2013 VL 81 BP 288 EP 303 DI 10.1016/j.atmosenv.2013.08.035 PG 16 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 285EY UT WOS:000329377600032 ER PT J AU Garner, GG Thompson, AM AF Garner, Gregory G. Thompson, Anne M. TI Ensemble statistical post-processing of the National Air Quality Forecast Capability: Enhancing ozone forecasts in Baltimore, Maryland SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Ensemble forecast; Air quality; Baltimore; Regression tree; Extreme value; Bootstrap ID PREDICTION AB An ensemble statistical post-processor (ESP) is developed for the National Air Quality Forecast Capability (NAQFC) to address the unique challenges of forecasting surface ozone in Baltimore, MD. Air quality and meteorological data were collected from the eight monitors that constitute the Baltimore forecast region. These data were used to build the ESP using a moving-block bootstrap, regression tree models, and extreme-value theory. The ESP was evaluated using a 10-fold cross-validation to avoid evaluation with the same data used in the development process. Results indicate that the ESP is conditionally biased, likely due to slight overfitting while training the regression tree models. When viewed from the perspective of a decision-maker, the ESP provides a wealth of additional information previously not available through the NAQFC alone. The user is provided the freedom to tailor the forecast to the decision at hand by using decision-specific probability thresholds that define a forecast for an ozone exceedance. Taking advantage of the ESP, the user not only receives an increase in value over the NAQFC, but also receives value for costly decisions that the NAQFC couldn't provide alone. (C) 2013 The Authors. Published by Elsevier Ltd. All rights reserved. C1 [Garner, Gregory G.] Penn State Univ, University Pk, PA 16802 USA. [Thompson, Anne M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Garner, GG (reprint author), Penn State Univ, 503 Walker Bldg, University Pk, PA 16802 USA. EM ggg121@psu.edu RI Thompson, Anne /C-3649-2014 OI Thompson, Anne /0000-0002-7829-0920 FU U.S. Environmental Protection Agency (EPA) [FP-91729901-1]; Pennsylvania State University from NASA DISCOVER-AQ [NNX10AR39G]; NASA Air Quality Applied Sciences Team [NNX11AQ44G] FX The author would like to acknowledge Dan Salkovitz from the Virginia Department of Environmental Quality and Laura Warren from the Maryland Department of the Environment for their useful comments and feedback on the statistical guidance product. This research was supported by a STAR fellowship (FP-91729901-1) to GGG awarded by the U.S. Environmental Protection Agency (EPA). It has not been formally reviewed by the EPA. The views expressed in this manuscript are solely those of GGG and co-authors. The EPA does not endorse any products or commercial services mentioned in this manuscript. Additional funding for this research was provided by grants to the Pennsylvania State University from NASA DISCOVER-AQ (NNX10AR39G), the NASA Air Quality Applied Sciences Team (NNX11AQ44G). NR 24 TC 4 Z9 4 U1 0 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2013 VL 81 BP 517 EP 522 DI 10.1016/j.atmosenv.2013.09.020 PG 6 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 285EY UT WOS:000329377600054 ER PT J AU Pathak, MG Patel, VC Ghiaasiaan, SM Mulcahey, TI Helvensteijn, BP Kashani, A Feller, JR AF Pathak, M. G. Patel, V. C. Ghiaasiaan, S. M. Mulcahey, T. I. Helvensteijn, B. P. Kashani, A. Feller, J. R. TI Hydrodynamic parameters for ErPr cryocooler regenerator fillers under steady and periodic flow conditions SO CRYOGENICS LA English DT Article DE Regenerators; Porous media; Periodic flow; Steady flow; Oscillatory flow; Darcy permeability; Forchheimer coefficient; CFD; ErPr rare earth; Hydrodynamics ID PULSE TUBE REFRIGERATION; POROUS-MEDIA; THERMAL DISPERSION; INERTANCE TUBE; TURBULENT-FLOW; FLUID-FLOW; SIMULATION; HEAT; PERFORMANCE; EQUATION AB The regenerator, typically a microporous structure that is subject to periodic flow of a cryogenic fluid, is the most critical component of Pulse Tube or Stirling cryocoolers, which are widely used for high-demand defense and aerospace applications. Despite the critical impact of hydrodynamic irreversibilities in the regenerator on the overall cycle efficiency, the impact of the parameters that influence these losses are poorly understood. In this investigation, experiments were conducted in which steady and oscillatory flows of helium were imposed on Er50Pr50 rare-earth regenerator filler material and mass flow and pressure drop data were recorded under ambient temperature conditions. A filler material composed of 63-75 mu m diameter Er50Pr50 spheres was selected based on current commercially available particle geometries. The flow parameters in the experiments were in the laminar flow range. A computational fluid dynamic (CFD)-assisted method was applied for the analysis and interpretation of the experimental data, with sinusoidal time variations of inlet and exit boundary conditions for the periodic flow case. The permeability and inertial coefficients that led to agreement between the experimental data and computational simulations were iteratively obtained. The resulting Darcy permeability and Forchheimer inertial coefficients are reported herein. A constant Darcy permeability value for all steady and periodic flow tests was found to correlate well to experimental data. The Forchheimer inertial coefficients were correlated and found to be functions of the system charge pressure and the pore-based Reynolds number. The results also show that the periodic flow inertial coefficients are different than the steady flow parameters typically used. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Pathak, M. G.; Patel, V. C.; Ghiaasiaan, S. M.; Mulcahey, T. I.] Georgia Inst Technol, George W Woodruff Sch Mech Engn, Georgia Tech Cryo Lab, Atlanta, GA 30332 USA. [Helvensteijn, B. P.; Kashani, A.] Atlas Sci, San Jose, CA 95120 USA. [Feller, J. R.] NASA, Ames Res Ctr, Cryogen Grp, Moffett Field, CA 94035 USA. RP Pathak, MG (reprint author), Georgia Inst Technol, George W Woodruff Sch Mech Engn, Georgia Tech Cryo Lab, Atlanta, GA 30332 USA. EM mihirgp@gmail.com FU NASA Office of the Chief Technologist's Space Technology Research Fellowship FX This work was supported by a NASA Office of the Chief Technologist's Space Technology Research Fellowship. NR 33 TC 0 Z9 0 U1 2 U2 8 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD DEC PY 2013 VL 58 BP 68 EP 77 DI 10.1016/j.cryogenics.2013.10.002 PG 10 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA 285TG UT WOS:000329417300011 ER PT J AU Hackl, M Malservisi, R Hugentobler, U Jiang, Y AF Hackl, Matthias Malservisi, Rocco Hugentobler, Urs Jiang, Yan TI Velocity covariance in the presence of anisotropic time correlated noise and transient events in GPS time series SO JOURNAL OF GEODYNAMICS LA English DT Article DE GPS time series; Colored noise; Transient event; Slow slip event ID PRINCIPAL COMPONENT ANALYSIS; SAN-ANDREAS-FAULT; SOUTHERN CALIFORNIA; STRAIN ACCUMULATION; SIGNALS; PLATE; CYCLE; ZONE AB The presence of un-modeled transient events in GPS time series significantly influences the estimate of the noise characteristics. In particular, GPS time series affected by transient events with a preferential geographical orientation are affected by a regional pattern of anisotropic noise. We provide a method to derive the covariance of GPS velocities in the presence of time-correlated noise based on the Allan variance of the rate that can account for this anisotropy. The velocity variance is calculated for different directions, allowing for the detection of direction-dependent noise properties. The resulting covariance provides realistic estimates for the uncertainties of GPS derived surface velocities and is of particular interest for the analysis of time series affected by transient signals. We show that GPS sites in subduction zones experiencing slow slip events (SSEs) exhibit a significant component of time correlated "noise" in the direction of the SSE motion and that the velocity confidence ellipses are highly eccentric in this direction. The time correlation of the noise of these sites is significantly reduced after modeling and subtracting SSEs from the time series with a concomitant reduction of the anisotropy of the estimated velocity uncertainties. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Hackl, Matthias] Univ Munich, Dept Earth & Environm Sci, D-80333 Munich, Germany. [Malservisi, Rocco] Univ S Florida, Dept Geol, Tampa, FL 33620 USA. [Hugentobler, Urs] Tech Univ Munich, Inst Astron & Phys Geodesy, D-80290 Munich, Germany. [Jiang, Yan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hackl, M (reprint author), Univ Munich, Dept Earth & Environm Sci, Theresienstr 41, D-80333 Munich, Germany. EM hackl@geophysik.uni-muenchen.de; rocco@usf.edu; urs.hugentobler@bv.tu-muenchen.de; yjiang@caltech.edu RI Hugentobler, Urs/H-5605-2011 FU Bavarian Elite Network; DFG [BA1210/18-1, MA4163/1-2] FX We used data of the Pacific Northwest Geodetic Array provided by the Central Washington University. We are grateful to Tim Melbourne and the geodetic group of Central Washington University for providing the surface displacement data due to the slow slip events. We would like to thank Tim Dixon for his comments that helped to improve this manuscript. This research was partially funded by the Bavarian Elite Network and the DFG grants BA1210/18-1, MA4163/1-2. NR 64 TC 5 Z9 5 U1 0 U2 17 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0264-3707 J9 J GEODYN JI J. Geodyn. PD DEC PY 2013 VL 72 SI SI BP 36 EP 45 DI 10.1016/j.jog.2013.08.007 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 286PZ UT WOS:000329482500004 ER PT J AU Horesh, A Stockdale, C Fox, DB Frail, DA Carpenter, J Kulkarni, SR Ofek, EO Gal-Yam, A Kasliwal, MM Arcavi, I Quimby, R Cenko, SB Nugent, PE Bloom, JS Law, NM Poznanski, D Gorbikov, E Polishook, D Yaron, O Ryder, S Weiler, KW Bauer, F Van Dyk, SD Immler, S Panagia, N Pooley, D Kassim, N AF Horesh, Assaf Stockdale, Christopher Fox, Derek B. Frail, Dale A. Carpenter, John Kulkarni, S. R. Ofek, Eran O. Gal-Yam, Avishay Kasliwal, Mansi M. Arcavi, Iair Quimby, Robert Cenko, S. Bradley Nugent, Peter E. Bloom, Joshua S. Law, Nicholas M. Poznanski, Dovi Gorbikov, Evgeny Polishook, David Yaron, Ofer Ryder, Stuart Weiler, Kurt W. Bauer, Franz Van Dyk, Schuyler D. Immler, Stefan Panagia, Nino Pooley, Dave Kassim, Namir TI An early and comprehensive millimetre and centimetre wave and X-ray study of SN 2011dh: a non-equipartition blast wave expanding into a massive stellar wind SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; supernovae: individual: SN 2011dh; radio continuum: general; X-rays: general ID IIB SUPERNOVA 2011DH; RADIO-EMISSION; 1993J; PROGENITOR; ABSORPTION AB Only a handful of supernovae (SNe) have been studied in multiwavelengths from the radio to X-rays, starting a few days after the explosion. The early detection and classification of the nearby Type IIb SN 2011dh/PTF 11eon in M51 provides a unique opportunity to conduct such observations. We present detailed data obtained at one of the youngest phase ever of a core-collapse SN (days 3-12 after the explosion) in the radio, millimetre and X-rays; when combined with optical data, this allows us to explore the early evolution of the SN blast wave and its surroundings. Our analysis shows that the expanding SN shock wave does not exhibit equipartition (epsilon(e)/epsilon(B) similar to 1000), and is expanding into circumstellar material that is consistent with a density profile falling like R-2. Within modelling uncertainties we find an average velocity of the fast parts of the ejecta of 15 000 +/- 1800 km s(-1), contrary to previous analysis. This velocity places SN 2011dh in an intermediate blast wave regime between the previously defined compact and extended SN Type IIb subtypes. Our results highlight the importance of early (similar to 1 d) high-frequency observations of future events. Moreover, we show the importance of combined radio/X-ray observations for determining the microphysics ratio epsilon(e)/epsilon(B). C1 [Horesh, Assaf; Carpenter, John; Kulkarni, S. R.; Kasliwal, Mansi M.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Stockdale, Christopher] Marquette Univ, Dept Phys, Milwaukee, WI 53201 USA. [Stockdale, Christopher] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Fox, Derek B.] Penn State Univ, Eberly Coll Sci, University Pk, PA 16802 USA. [Frail, Dale A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Ofek, Eran O.; Gal-Yam, Avishay; Arcavi, Iair; Polishook, David; Yaron, Ofer] Weizmann Inst Sci, Benoziyo Ctr Astrophys, Fac Phys, IL-76100 Rehovot, Israel. [Kasliwal, Mansi M.] Carnegie Inst Sci, Pasadena, CA 91101 USA. [Quimby, Robert] Univ Tokyo, IPMU, Kashiwa, Chiba, Japan. [Cenko, S. Bradley; Nugent, Peter E.; Bloom, Joshua S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Nugent, Peter E.; Bloom, Joshua S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Law, Nicholas M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Poznanski, Dovi; Gorbikov, Evgeny] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Polishook, David] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Ryder, Stuart] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Weiler, Kurt W.] Computat Phys Inc, Springfield, VA 22151 USA. [Bauer, Franz] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, Franz] Space Sci Inst, Boulder, CO 80301 USA. [Van Dyk, Schuyler D.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Immler, Stefan] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Immler, Stefan] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Immler, Stefan] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Panagia, Nino] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Panagia, Nino] Osserv Astrofis Catania, INAFCT, I-95123 Catania, Italy. [Panagia, Nino] Supernova Ltd, Virgin Gorda, British Virgin, W Ind Assoc St. [Pooley, Dave] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Kassim, Namir] Naval Res Lab, Washington, DC 20375 USA. RP Horesh, A (reprint author), CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. EM assafh@astro.caltech.edu RI Horesh, Assaf/O-9873-2016; OI Horesh, Assaf/0000-0002-5936-1156; Van Dyk, Schuyler/0000-0001-9038-9950 FU National Science Foundation; CARMA partner universities; NSF [AST-0908886, AST-1211916]; NASA; Israeli Science Foundation; BSF; NASA Wisconsin Space Grant Consortium; CONICYT, Chile [FONDECYT 1101024, FONDAPCATA 15010003]; Programa de Financiamiento Basal; Iniciativa Cientifica Milenio through the Millennium Center for Supernova Science [P10-064-F]; Chandra X-ray Center [SAO GO9-0086D, GO0-11095A]; Hubble Fellowship; Carnegie-Princeton Fellowship; STScI-DDRF; Office of Naval Research; Gary & Cynthia Bengier; Richard & Rhoda Goldman Fund; Sylvia & Jim Katzman Foundation; Christopher R. Redlich Fund; TABASGO Foundation FX We thank the EVLA and CARMA staff for promptly scheduling this target of opportunity. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. This work made use of data supplied by the UK SSDC. PTF is a fully automated, wide-field survey aimed at a systematic exploration of explosions and variable phenomena in optical wavelengths. The participating institutions are Caltech, Columbia University, Weizmann Institute of Science, Lawrence Berkeley Laboratory, Oxford and University of California at Berkeley. The programme is centred on a 12K x 8K, 7.8 deg2 CCD array (CFH12K) re-engineered for the 1.2-m Oschin Telescope at the Palomar Observatory by Caltech Optical Observatories. Photometric follow-up is undertaken by the automated Palomar 1.5-m telescope. Research at Caltech is supported by grants from NSF and NASA. The Weizmann PTF partnership is supported in part by the Israeli Science Foundation via grants to AG. The Weizmann-Caltech collaboration is supported by a grant from the BSF to AG and SRK. AG further acknowledges the Lord Sieff of Brimpton Foundation. CS is supported by the NASA Wisconsin Space Grant Consortium. FB acknowledges support from CONICYT, Chile, under grants FONDECYT 1101024 and FONDAPCATA 15010003, Programa de Financiamiento Basal, the Iniciativa Cientifica Milenio through the Millennium Center for Supernova Science grant P10-064-F, and Chandra X-ray Center grants SAO GO9-0086D and GO0-11095A. MMK acknowledges support from the Hubble Fellowship and the Carnegie-Princeton Fellowship. NP acknowledges partial support by STScI-DDRF grant D0001.82435. Research at the Naval Research Laboratory is supported by funding from the Office of Naval Research. SBC acknowledges generous financial assistance from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, the Sylvia & Jim Katzman Foundation, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grants AST-0908886 and AST-1211916. We thank the anonymous referee for his constructive comments. NR 30 TC 21 Z9 21 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 2 BP 1258 EP 1267 DI 10.1093/mnras/stt1645 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 258LP UT WOS:000327461100027 ER PT J AU Banyai, E Kiss, LL Bedding, TR Bellamy, B Benko, JM Bodi, A Callingham, JR Compton, D Csanyi, I Derekas, A Dorval, J Huber, D Shrier, O Simon, AE Stello, D Szabo, GM Szabo, R Szatmary, K AF Banyai, E. Kiss, L. L. Bedding, T. R. Bellamy, B. Benko, J. M. Bodi, A. Callingham, J. R. Compton, D. Csanyi, I. Derekas, A. Dorval, J. Huber, D. Shrier, O. Simon, A. E. Stello, D. Szabo, Gy. M. Szabo, R. Szatmary, K. TI Variability of M giant stars based on Kepler photometry: general characteristics SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; stars: AGB and post-AGB; stars: variables: general ID LARGE-MAGELLANIC-CLOUD; LONG-PERIOD VARIABLES; GRAVITATIONAL LENSING EXPERIMENT.; OGLE-III CATALOG; PULSATING M GIANTS; SECONDARY PERIODS; RED GIANTS; LUMINOSITY RELATIONS; SEMIREGULAR VARIABLES; MIRA VARIABLES AB M giants are among the longest period pulsating stars which is why their studies were traditionally restricted to analyses of low-precision visual observations, and, more recently, accurate ground-based data. Here we present an overview of M giant variability on a wide range of time-scales (hours to years), based on the analysis of 13 quarters of Kepler long-cadence observations (one point per every 29.4 min), with a total time-span of over 1000 d. About two-thirds of the sample stars have been selected from the All Sky Automated Survey (ASAS)-North survey of the Kepler field, with the rest supplemented from a randomly chosen M giant control sample. We first describe the correction of the light curves from different quarters, which was found to be essential. We use Fourier analysis to calculate multiple frequencies for all stars in the sample. Over 50 stars show a relatively strong signal with a period equal to the Kepler-year and a characteristic phase dependence across the whole field of view. We interpret this as a so far unidentified systematic effect in the Kepler data. We discuss the presence of regular patterns in the distribution of multiple periodicities and amplitudes. In the period-amplitude plane we find that it is possible to distinguish between solar-like oscillations and larger amplitude pulsations which are characteristic for Mira/semiregular stars. This may indicate the region of the transition between two types of oscillations as we move upward along the giant branch. C1 [Banyai, E.; Kiss, L. L.; Benko, J. M.; Derekas, A.; Simon, A. E.; Szabo, Gy. M.; Szabo, R.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, H-1121 Budapest, Hungary. [Kiss, L. L.; Bedding, T. R.; Bellamy, B.; Callingham, J. R.; Compton, D.; Derekas, A.; Dorval, J.; Huber, D.; Shrier, O.; Stello, D.] Univ Sydney, Sch Phys, SIfA, Sydney, NSW 2006, Australia. [Kiss, L. L.; Simon, A. E.; Szabo, Gy. M.] ELTE Gothard Lendulet Res Grp, H-9700 Szombathely, Hungary. [Bedding, T. R.; Stello, D.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Bodi, A.; Csanyi, I.; Szabo, Gy. M.; Szatmary, K.] Univ Szeged, Dept Expt Phys, H-6720 Szeged, Hungary. [Bodi, A.; Csanyi, I.; Szabo, Gy. M.; Szatmary, K.] Univ Szeged, Astron Observ, H-6720 Szeged, Hungary. [Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Banyai, E (reprint author), Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege M Ut 15-17, H-1121 Budapest, Hungary. EM ebanyai@konkoly.hu RI Derekas, Aliz/G-2091-2016; OI Derekas, Aliz/0000-0002-6526-9444; Bedding, Timothy/0000-0001-5943-1460; Szabo, Robert/0000-0002-3258-1909; Bedding, Tim/0000-0001-5222-4661; Callingham, Joseph/0000-0002-7167-1819 FU Hungarian OTKA [K76816, K83790, K104607]; Mag Zrt. [HUMAN MB08C 81013]; ESA PECS [C98090]; KTIA [URKUT_10-1-2011-0019]; Lendulet- Young Researchers Programme of the Hungarian Academy of Sciences and the European Community's Seventh Framework Programme (FP7) [269194]; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences; Hungarian Eotvos fellowship; NASA's Science Mission Directorate FX This project has been supported by the Hungarian OTKA Grants K76816, K83790, K104607 and HUMAN MB08C 81013 grant of Mag Zrt., ESA PECS C98090, KTIA URKUT_10-1-2011-0019 grant, the Lendulet-2009 Young Researchers Programme of the Hungarian Academy of Sciences and the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 269194 (IRSES/ASK). AD, RSz and GyMSz have been supported by the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. AD was supported by the Hungarian Eotvos fellowship. RSz acknowledges the University of Sydney IRCA grant. Funding for this Discovery Mission is provided by NASA's Science Mission Directorate. The Kepler Team and the Kepler Guest Observer Office are recognized for helping to make the mission and these data possible. NR 50 TC 16 Z9 16 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 2 BP 1576 EP 1587 DI 10.1093/mnras/stt1685 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 258LP UT WOS:000327461100053 ER PT J AU Page, MJ Kuin, NPM Breeveld, AA Hancock, B Holland, ST Marshall, FE Oates, S Roming, PWA Siegel, MH Smith, PJ Carter, M De Pasquale, M Symeonidis, M Yershov, V Beardmore, AP AF Page, M. J. Kuin, N. P. M. Breeveld, A. A. Hancock, B. Holland, S. T. Marshall, F. E. Oates, S. Roming, P. W. A. Siegel, M. H. Smith, P. J. Carter, M. De Pasquale, M. Symeonidis, M. Yershov, V. Beardmore, A. P. TI The use and calibration of read-out streaks to increase the dynamic range of the Swift Ultraviolet/Optical Telescope SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE space vehicles: instruments; techniques: photometric; ultraviolet: general ID PHOTON-COUNTING DETECTORS; MISSION AB The dynamic range of photon counting micro-channel-plate (MCP) intensified charged-coupled device (CCD) instruments such as the Swift Ultraviolet/Optical Telescope (UVOT) and the XMM-Newton Optical Monitor (XMM-OM) is limited at the bright end by coincidence loss, the superposition of multiple photons in the individual frames recorded by the CCD. Photons which arrive during the brief period in which the image frame is transferred for read out of the CCD are displaced in the transfer direction in the recorded images. For sufficiently bright sources, these displaced counts form read-out streaks. Using UVOT observations of Tycho-2 stars, we investigate the use of these read-out streaks to obtain photometry for sources which are too bright (and hence have too much coincidence loss) for normal aperture photometry to be reliable. For read-out-streak photometry, the bright-source limiting factor is coincidence loss within the MCPs rather than the CCD. We find that photometric measurements can be obtained for stars up to 2.4 mag brighter than the usual full-frame coincidence-loss limit by using the read-out streaks. The resulting bright-limit Vega magnitudes in the UVOT passbands are UVW2 = 8.80, UVM2 = 8.27, UVW1 = 8.86, u = 9.76, b = 10.53, v = 9.31 and White = 11.71; these limits are independent of the windowing mode of the camera. We find that a photometric precision of 0.1 mag can be achieved through read-out streak measurements. A suitable method for the measurement of read-out streaks is described and all necessary calibration factors are given. C1 [Page, M. J.; Kuin, N. P. M.; Breeveld, A. A.; Hancock, B.; Oates, S.; Smith, P. J.; Carter, M.; De Pasquale, M.; Symeonidis, M.; Yershov, V.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Holland, S. T.] Space Telescope Sci Ctr, Baltimore, MD 21218 USA. [Marshall, F. E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Roming, P. W. A.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78228 USA. [Roming, P. W. A.; Siegel, M. H.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Page, MJ (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM mjp@mssl.ucl.ac.uk FU United Kingdom Space Agency (UKSA) FX This work was supported by the United Kingdom Space Agency (UKSA). We thank Rhaana Starling and Julian Osborne for useful discussions. NR 23 TC 6 Z9 6 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 2 BP 1684 EP 1693 DI 10.1093/mnras/stt1689 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 258LP UT WOS:000327461100063 ER PT J AU Sofia, S Girard, TM Sofia, UJ Twigg, L Heaps, W Thuillier, G AF Sofia, S. Girard, T. M. Sofia, U. J. Twigg, L. Heaps, W. Thuillier, G. TI Variation of the diameter of the Sun as measured by the Solar Disk Sextant (SDS) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Sun: fundamental parameters ID F-MODE FREQUENCIES; RADIUS; OBLATENESS; VARIABILITY; IRRADIANCE; CONSTANCY AB The balloon-borne Solar Disk Sextant (SDS) experiment has measured the angular size of the Sun on seven occasions spanning the years 1992 to 2011. The solar half-diameter - observed in a 100 nm wide passband centred at 615 nm - is found to vary over that period by up to 200 mas, while the typical estimated uncertainty of each measure is 20 mas. The diameter variation is not in phase with the solar activity cycle; thus, the measured diameter variation cannot be explained as an observational artefact of surface activity. Other possible instrument-related explanations for the observed variation are considered but found unlikely, leading us to conclude that the variation is real. The SDS is described here in detail, as is the complete analysis procedure necessary to calibrate the instrument and allow comparison of diameter measures across decades. C1 [Sofia, S.; Girard, T. M.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Sofia, U. J.] Amer Univ, Dept Phys, Washington, DC 20016 USA. [Twigg, L.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. [Heaps, W.] NASA, Goddard Space Flight Ctr, Instrument Technol Ctr, Greenbelt, MD 20771 USA. [Thuillier, G.] LATMOS CNRS, F-78280 Guyancourt, France. RP Sofia, S (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. EM sabatino.sofia@yale.edu FU NASA; NSF; G. Unger Vetlesen Foundation; Brinson Foundation; CNES (France); CNRS (France) FX An experiment that has spanned nearly three decades is only possible with the support and collaboration of many people and institutions. Beyond the co-authors of this paper, we would first like to thank the people who assisted in its conception and design; this includes E. Maier, K. Schatten, P. Minott, H-Y. Chiu and A. Endal. The fabrication of the SDS payload could not have been accomplished without D. Silbert. Flight operations were helped by many people including D. Pesnell and W. Hoegy. We are, of course, grateful for the substantial financial support provided by a series of grants from NASA and the NSF, and more recently, from the G. Unger Vetlesen Foundation, and the Brinson Foundation. CNES (France) and CNRS (France), which support the PICARD/SODISM mission, also provided financial support for the most recent SDS flight and we thank these institutes for their contribution. Understanding of the SDS instrument response was greatly assisted by the COSI model provided by A. Shapiro and optical modelling by L. Ramos-Izquierdo as well as modelling and other contributions by W. van Altena, R. Mendez and D. Casetti. Our work benefited from previous versions of the SDS analysis pipeline constructed by J. Zhang, A. Egidi, B. Caccin and D. Djafer. Also, insightful comments from an anonymous referee led to significant improvements in the manuscript. Finally, we want to acknowledge the outstanding flight support provided by the personnel of the NASA/CSBF over the years. NR 29 TC 5 Z9 5 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 3 BP 2151 EP 2169 DI 10.1093/mnras/stt1721 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 259PY UT WOS:000327540000018 ER PT J AU van der Horst, AJ Curran, PA Miller-Jones, JCA Linford, JD Gorosabel, J Russell, DM de Ugarte Postigo, A Lundgren, AA Taylor, GB Maitra, D Guziy, S Belloni, TM Kouveliotou, C Jonker, PG Kamble, A Paragi, Z Homan, J Kuulkers, E Granot, J Altamirano, D Buxton, MM Castro-Tirado, A Fender, RP Garrett, MA Gehrels, N Hartmann, DH Kennea, JA Krimm, HA Mangano, V Ramirez-Ruiz, E Romano, P Wijers, RAMJ Wijnands, R Yang, YJ AF van der Horst, A. J. Curran, P. A. Miller-Jones, J. C. A. Linford, J. D. Gorosabel, J. Russell, D. M. de Ugarte Postigo, A. Lundgren, A. A. Taylor, G. B. Maitra, D. Guziy, S. Belloni, T. M. Kouveliotou, C. Jonker, P. G. Kamble, A. Paragi, Z. Homan, J. Kuulkers, E. Granot, J. Altamirano, D. Buxton, M. M. Castro-Tirado, A. Fender, R. P. Garrett, M. A. Gehrels, N. Hartmann, D. H. Kennea, J. A. Krimm, H. A. Mangano, V. Ramirez-Ruiz, E. Romano, P. Wijers, R. A. M. J. Wijnands, R. Yang, Y. J. TI Broad-band monitoring tracing the evolution of the jet and disc in the black hole candidate X-ray binary MAXI J1659-152 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: individual: MAXI J1659-152; X-rays: binaries; X-rays: individual: MAXI J1659-152 ID SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; QUASI-PERIODIC OSCILLATIONS; GX 339-4; COMPACT JET; XTE J1550-564; HARD STATE; FLUX CORRELATION; TIMING ANALYSIS; ACCRETION DISK; LOW/HARD STATE AB MAXI J1659-152 was discovered on 2010 September 25 as a new X-ray transient, initially identified as a gamma-ray burst, but was later shown to be a new X-ray binary with a black hole as the most likely compact object. Dips in the X-ray light curves have revealed that MAXI J1659-152 is the shortest period black hole candidate identified to date. Here we present the results of a large observing campaign at radio, submillimetre, near-infrared (nIR), optical and ultraviolet (UV) wavelengths. We have combined this very rich data set with the available X-ray observations to compile a broad-band picture of the evolution of this outburst. We have performed broad-band spectral modelling, demonstrating the presence of a spectral break at radio frequencies and a relationship between the radio spectrum and X-ray states. Also, we have determined physical parameters of the accretion disc and put them into context with respect to the other parameters of the binary system. Finally, we have investigated the radio-X-ray and nIR/optical/UV-X-ray correlations up to similar to 3 yr after the outburst onset to examine the link between the jet and the accretion disc, and found that there is no significant jet contribution to the nIR emission when the source is in the soft or intermediate X-ray spectral state, consistent with our detection of the jet break at radio frequencies during these states. C1 [van der Horst, A. J.; Altamirano, D.; Wijers, R. A. M. J.; Wijnands, R.; Yang, Y. J.] Univ Amsterdam, Astron Inst, NL-1098 XH Amsterdam, Netherlands. [Curran, P. A.; Miller-Jones, J. C. A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Linford, J. D.; Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Gorosabel, J.; de Ugarte Postigo, A.; Castro-Tirado, A.] CSIC, IAA, E-18008 Granada, Spain. [Gorosabel, J.] Univ Basque Country, EHU, CSIC,ETS Ingn, IAA,Dept Fis Aplicada 1,Unidad Asociada Grp Plane, E-48013 Bilbao, Spain. [Gorosabel, J.] Basque Fdn Sci, Ikerbasque, E-48008 Bilbao, Spain. [Russell, D. M.] IAC, E-38205 Tenerife, Spain. [de Ugarte Postigo, A.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Lundgren, A. A.] Joint ALMA Observ, Santiago, Chile. [Maitra, D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Guziy, S.] Nikolaev Natl Univ, UA-54030 Nikolayev, Ukraine. [Belloni, T. M.] INAF, Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Kouveliotou, C.] NASA, Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.; Kamble, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Paragi, Z.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Homan, J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kuulkers, E.] European Space Astron Ctr ESA ESAC, Sci Operat Dept, E-28691 Madrid, Spain. [Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel. [Buxton, M. M.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Fender, R. P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Garrett, M. A.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Garrett, M. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Gehrels, N.; Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hartmann, D. H.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Mangano, V.; Romano, P.] INAF, Ist Astrofys Spaziale Fis Cosm Palermo, I-90146 Palermo, Italy. [Ramirez-Ruiz, E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP van der Horst, AJ (reprint author), Univ Amsterdam, Astron Inst, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM a.j.vanderhorst@uva.nl RI Curran, Peter/B-5293-2013; Miller-Jones, James/B-2411-2013; OI Curran, Peter/0000-0003-3003-4626; Miller-Jones, James/0000-0003-3124-2814; Wijers, Ralph/0000-0002-3101-1808; Castro-Tirado, A. J./0000-0003-2999-3563; de Ugarte Postigo, Antonio/0000-0001-7717-5085 FU Commonwealth of Australia; CSIRO; European Research Council via Advanced Investigator [247295]; Australian Research Council's Discovery Projects [DP120102393]; Marie Curie Intra European Fellowship within the Seventh European Community Framework Programme [IEF 274805]; European Commission under the Marie Curie Career Integration Grant programme [FP7-PEOPLE-2012CIG 322307]; Dark Cosmology Centre; DNRF; Unidad Asociada IAACSIC; Ikerbasque Foundation for Science; Spanish research programs [AYA2012-39362-C02-02, AYA2011-24780/ESP, AYA200914000-C03-01/ESP, AYA2010-21887-C04-01]; PRIN-INAF; European Research Council FX We greatly appreciate the support from the VLA, WSRT, APEX, ATCA, GMRT, SMARTS, IAC80, 1.23-m CAHA, BOOTES-2 and BOOTES-3 telescopes in their help with scheduling and obtaining these observations. The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under cooperative agreement with the National Science Foundation. The WSRT is operated by ASTRON (Netherlands Institute for Radio Astronomy) with support from the Netherlands foundation for Scientific Research. APEX is a collaboration between the Max-Plank-Institut fur Radioastronomie, the European Southern Observatory and the Onsala Space Observatory. The ATCA is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The GMRT is operated by the National Center for Radio Astrophysics of the Tata Institute of Fundamental Research. The CTIO 1.3-m telescope is operated by the SMARTS consortium. The Centro Astronomico Hispano Aleman (CAHA) at Calar Alto is operated jointly by the Max-Planck Institut fur Astronomie and the Instituto de Astrofisica de Andalucia (CSIC). The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. The IAC80 is operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. The MAXI/GSC data are provided by RIKEN, JAXA and the MAXI team. This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center.; AJvdH and RAMJW acknowledge support from the European Research Council via Advanced Investigator Grant no. 247295. PAC and JCAM-J acknowledge support from the Australian Research Council's Discovery Projects funding scheme under grant DP120102393. DMR acknowledges support from a Marie Curie Intra European Fellowship within the Seventh European Community Framework Programme under contract no. IEF 274805. AdUP acknowledges support by the European Commission under the Marie Curie Career Integration Grant programme (FP7-PEOPLE-2012CIG 322307), and the Dark Cosmology Centre, funded by the DNRF. This work was supported by the Unidad Asociada IAACSIC at the group of planetary science of ETSI-UPV/EHU, by the Ikerbasque Foundation for Science, and by Spanish research programs AYA2012-39362-C02-02, AYA2011-24780/ESP, AYA200914000-C03-01/ESP and AYA2010-21887-C04-01. TMB acknowledges support from grant PRIN-INAF 2012. RW acknowledges support from the European Research Council via a Starting Grant. NR 94 TC 12 Z9 12 U1 0 U2 9 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 3 BP 2625 EP 2638 DI 10.1093/mnras/stt1767 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 259PY UT WOS:000327540000053 ER PT J AU Gruppioni, C Pozzi, F Rodighiero, G Delvecchio, I Berta, S Pozzetti, L Zamorani, G Andreani, P Cimatti, A Ilbert, O Le Floc'h, E Lutz, D Magnelli, B Marchetti, L Monaco, P Nordon, R Oliver, S Popesso, P Riguccini, L Roseboom, I Rosario, DJ Sargent, M Vaccari, M Altieri, B Aussel, H Bongiovanni, A Cepa, J Daddi, E Dominguez-Sanchez, H Elbaz, D Schreiber, NF Genzel, R Iribarrem, A Magliocchetti, M Maiolino, R Poglitsch, A Garcia, AP Sanchez-Portal, M Sturm, E Tacconi, L Valtchanov, I Amblard, A Arumugam, V Bethermin, M Bock, J Boselli, A Buat, V Burgarella, D Castro-Rodriguez, N Cava, A Chanial, P Clements, DL Conley, A Cooray, A Dowell, CD Dwek, E Eales, S Franceschini, A Glenn, J Griffin, M Hatziminaoglou, E Ibar, E Isaak, K Ivison, RJ Lagache, G Levenson, L Lu, N Madden, S Maffei, B Mainetti, G Nguyen, HT O'Halloran, B Page, MJ Panuzzo, P Papageorgiou, A Pearson, CP Perez-Fournon, I Pohlen, M Rigopoulou, D Rowan-Robinson, M Schulz, B Scott, D Seymour, N Shupe, DL Smith, AJ Stevens, JA Symeonidis, M Trichas, M Tugwell, KE Vigroux, L Wang, L Wright, G Xu, CK Zemcov, M Bardelli, S Carollo, M Contini, T Le Fevre, O Lilly, S Mainieri, V Renzini, A Scodeggio, M Zucca, E AF Gruppioni, C. Pozzi, F. Rodighiero, G. Delvecchio, I. Berta, S. Pozzetti, L. Zamorani, G. Andreani, P. Cimatti, A. Ilbert, O. Le Floc'h, E. Lutz, D. Magnelli, B. Marchetti, L. Monaco, P. Nordon, R. Oliver, S. Popesso, P. Riguccini, L. Roseboom, I. Rosario, D. J. Sargent, M. Vaccari, M. Altieri, B. Aussel, H. Bongiovanni, A. Cepa, J. Daddi, E. Dominguez-Sanchez, H. Elbaz, D. Schreiber, N. Foerster Genzel, R. Iribarrem, A. Magliocchetti, M. Maiolino, R. Poglitsch, A. Garcia, A. Perez Sanchez-Portal, M. Sturm, E. Tacconi, L. Valtchanov, I. Amblard, A. Arumugam, V. Bethermin, M. Bock, J. Boselli, A. Buat, V. Burgarella, D. Castro-Rodriguez, N. Cava, A. Chanial, P. Clements, D. L. Conley, A. Cooray, A. Dowell, C. D. Dwek, E. Eales, S. Franceschini, A. Glenn, J. Griffin, M. Hatziminaoglou, E. Ibar, E. Isaak, K. Ivison, R. J. Lagache, G. Levenson, L. Lu, N. Madden, S. Maffei, B. Mainetti, G. Nguyen, H. T. O'Halloran, B. Page, M. J. Panuzzo, P. Papageorgiou, A. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Rigopoulou, D. Rowan-Robinson, M. Schulz, B. Scott, D. Seymour, N. Shupe, D. L. Smith, A. J. Stevens, J. A. Symeonidis, M. Trichas, M. Tugwell, K. E. Vigroux, L. Wang, L. Wright, G. Xu, C. K. Zemcov, M. Bardelli, S. Carollo, M. Contini, T. Le Fevre, O. Lilly, S. Mainieri, V. Renzini, A. Scodeggio, M. Zucca, E. TI The Herschel PEP/HerMES Luminosity Function - I. Probing the Evolution of PACS selected Galaxies to z similar or equal to 4 (vol 432, pg 23, 2013) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Correction DE errata; addenda; galaxies: active; galaxies: evolution; galaxies: starburst; cosmology: observations; infrared: galaxies C1 [Gruppioni, C.; Pozzetti, L.; Zamorani, G.; Dominguez-Sanchez, H.; Bardelli, S.; Zucca, E.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Pozzi, F.; Delvecchio, I.] Univ Bologna, Dipartmento Astron, I-40127 Bologna, Italy. [Rodighiero, G.; Marchetti, L.; Franceschini, A.; Mainetti, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Berta, S.; Lutz, D.; Magnelli, B.; Nordon, R.; Popesso, P.; Rosario, D. J.; Schreiber, N. Foerster; Genzel, R.; Poglitsch, A.; Sturm, E.; Tacconi, L.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Andreani, P.; Iribarrem, A.] ESO, D-85748 Garching, Germany. [Ilbert, O.; Boselli, A.; Buat, V.; Burgarella, D.] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Le Floc'h, E.; Riguccini, L.; Sargent, M.; Aussel, H.; Daddi, E.; Bethermin, M.; Chanial, P.; Madden, S.; Panuzzo, P.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Magnelli, B.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Monaco, P.] Univ Trieste, Dipartmento Fis, Sez Astron, I-34131 Trieste, Italy. [Oliver, S.; Roseboom, I.; Smith, A. J.; Wang, L.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Roseboom, I.; Arumugam, V.; Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Bellville, South Africa. [Altieri, B.; Garcia, A. Perez; Sanchez-Portal, M.; Valtchanov, I.] ESA, Herschel Sci Ctr, E-28692 Madrid, Spain. [Bongiovanni, A.; Cepa, J.; Castro-Rodriguez, N.; Perez-Fournon, I.] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Spain. [Iribarrem, A.] Univ Fed Rio de Janeiro, Observ Valongo, BR-21941 Rio De Janeiro, Brazil. [Magliocchetti, M.] INAF, IFSI, I-00133 Rome, Italy. [Maiolino, R.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Amblard, A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bock, J.; Cooray, A.; Dowell, C. D.; Levenson, L.; Lu, N.; Nguyen, H. T.; Schulz, B.; Shupe, D. L.; Xu, C. K.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Castro-Rodriguez, N.; Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain. [Clements, D. L.; O'Halloran, B.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Conley, A.; Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dwek, E.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Eales, S.; Griffin, M.; Papageorgiou, A.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA 389 UCB, Boulder, CO 80309 USA. [Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Isaak, K.] ESA, ESTEC SRE SA, Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands. [Lagache, G.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France. [Lu, N.; Schulz, B.; Shupe, D. L.] CALTECH, Jet Prop Lab, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Maffei, B.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Page, M. J.; Symeonidis, M.; Tugwell, K. E.] Univ Coll London, Mullard Space Sci Lab, Surrey RH5 6NT, England. [Pearson, C. P.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Scott, D.] Univ British Columbia, Dept Phys & Astrophys, Vancouver, BC V6T 1Z1, Canada. [Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Stevens, J. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Trichas, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vigroux, L.] Univ Paris 06, UPMC, CNRS, Inst Astrophys Paris,UMR 7095, F-75014 Paris, France. [Carollo, M.] ETH Honggerberg, Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Contini, T.] Univ Toulouse, CNRS, Inst Rech Astrophys & Plantol, F-31400 Toulouse, France. [Renzini, A.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Scodeggio, M.] INAF IASF Milano, I-20133 Milan, Italy. RP Gruppioni, C (reprint author), Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy. EM carlotta.gruppioni@oabo.inaf.it RI Daddi, Emanuele/D-1649-2012; Bongiovanni, Angel/J-6176-2012; amblard, alexandre/L-7694-2014; Bardelli, Sandro/O-9369-2015; Zucca, Elena/O-9396-2015; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017; OI Daddi, Emanuele/0000-0002-3331-9590; amblard, alexandre/0000-0002-2212-5395; Bardelli, Sandro/0000-0002-8900-0298; Zucca, Elena/0000-0002-5845-8132; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275; Gruppioni, Carlotta/0000-0002-5836-4056 NR 1 TC 4 Z9 4 U1 1 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 3 BP 2875 EP 2876 DI 10.1093/mnras/stt1748 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 259PY UT WOS:000327540000074 ER PT J AU Khazendar, A Schodlok, MP Fenty, I Ligtenberg, SRM Rignot, E van den Broeke, MR AF Khazendar, A. Schodlok, M. P. Fenty, I. Ligtenberg, S. R. M. Rignot, E. van den Broeke, M. R. TI Observed thinning of Totten Glacier is linked to coastal polynya variability SO NATURE COMMUNICATIONS LA English DT Article ID ANTARCTIC ICE-SHEET; PINE ISLAND GLACIER; WEST ANTARCTICA; SEA-ICE; MODEL; SHELF; CIRCULATION; ACCELERATION; THICKNESS; RETREAT AB Analysis of ICESat-1 data (2003-2008) shows significant surface lowering of Totten Glacier, the glacier discharging the largest volume of ice in East Antarctica, and less change on nearby Moscow University Glacier. After accounting for firn compaction anomalies, the thinning appears to coincide with fast-flowing ice indicating a dynamical origin. Here, to elucidate these observations, we apply high-resolution ice-ocean modelling. Totten Ice Shelf is simulated to have higher, more variable basal melting rates. We link this variability to the volume of cold water, originating in polynyas upon sea ice formation, reaching the sub-ice-shelf cavity. Hence, we propose that the observed increased thinning of Totten Glacier is due to enhanced basal melting caused by a decrease in cold polynya water reaching its cavity. We support this hypothesis with passive microwave data of polynya extent variability. Considering the widespread changes in sea ice conditions, this mechanism could be contributing extensively to ice-shelf instability. C1 [Khazendar, A.; Schodlok, M. P.; Fenty, I.; Rignot, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Schodlok, M. P.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. [Ligtenberg, S. R. M.; van den Broeke, M. R.] Univ Utrecht, Inst Marine & Atmospher Res Utrecht, NL-3508 TA Utrecht, Netherlands. [Rignot, E.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. RP Khazendar, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ala.khazendar@jpl.nasa.gov RI Van den Broeke, Michiel/F-7867-2011; Rignot, Eric/A-4560-2014 OI Van den Broeke, Michiel/0000-0003-4662-7565; Rignot, Eric/0000-0002-3366-0481 FU NASA's Cryospheric Sciences Program; NASA; Utrecht University; Netherlands Polar Program; National Aeronautics and Space Administration FX This work was supported by a grant from NASA's Cryospheric Sciences Program (A. K. and M. P. S.). I. F. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. M.R.v.d.B. and S. R. M. L. acknowledge funding from Utrecht University and the Netherlands Polar Program. We are grateful to L. Padman for providing the ocean tide model, and to J. Lenaerts for providing RACMO2 accumulation data. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 58 TC 20 Z9 20 U1 1 U2 17 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD DEC PY 2013 VL 4 AR 2857 DI 10.1038/ncomms3857 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 285KV UT WOS:000329393800004 PM 24305466 ER PT J AU Goyal, R Sharma, RP Goldstein, ML Dwivedi, NK AF Goyal, R. Sharma, R. P. Goldstein, M. L. Dwivedi, N. K. TI Nonlinear interaction of proton whistler with kinetic Alfven wave to study solar wind turbulence SO PHYSICS OF PLASMAS LA English DT Article ID MAGNETIC FLUCTUATIONS; MAGNETOHYDRODYNAMICS; DISPERSION; SPECTRA AB This paper presents the nonlinear interaction between small but finite amplitude kinetic Alfven wave (KAW) and proton whistler wave using two-fluid model in intermediate beta plasma, applicable to solar wind. The nonlinearity is introduced by modification in the background density. This change in density is attributed to the nonlinear ponderomotive force due to KAW. The solutions of the model equations, governing the nonlinear interaction (and its effect on the formation of localized structures), have been obtained using semi-analytical method in solar wind at 1AU. It is concluded that the KAW properties significantly affect the threshold field required for the filament formation and their critical size (for proton whistler). The magnetic and electric field power spectra have been obtained and their relevance with the recent observations of solar wind turbulence by Cluster spacecraft has been pointed out. (C) 2013 AIP Publishing LLC. C1 [Goyal, R.; Sharma, R. P.] Indian Inst Technol, Ctr Energy Studies, Delhi 110016, India. [Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dwivedi, N. K.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. RP Goyal, R (reprint author), Indian Inst Technol, Ctr Energy Studies, Delhi 110016, India. EM ravig.iitd@gmail.com; rpsharma@ces.iitd.ac.in FU DST (India); ISRO (India) FX This work was partially supported by DST (India) and ISRO (India) under RESPOND program. NR 35 TC 1 Z9 1 U1 2 U2 4 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD DEC PY 2013 VL 20 IS 12 AR 122308 DI 10.1063/1.4849457 PG 7 WC Physics, Fluids & Plasmas SC Physics GA 282MU UT WOS:000329176800027 ER PT J AU Wendel, DE Olson, DK Hesse, M Aunai, N Kuznetsova, M Karimabadi, H Daughton, W Adrian, ML AF Wendel, D. E. Olson, D. K. Hesse, M. Aunai, N. Kuznetsova, M. Karimabadi, H. Daughton, W. Adrian, M. L. TI The relation between reconnected flux, the parallel electric field, and the reconnection rate in a three-dimensional kinetic simulation of magnetic reconnection SO PHYSICS OF PLASMAS LA English DT Article ID SOLAR CORONA; NULLS; LINES AB We investigate the distribution of parallel electric fields and their relationship to the location and rate of magnetic reconnection in a large particle-in-cell simulation of 3D turbulent magnetic reconnection with open boundary conditions. The simulation's guide field geometry inhibits the formation of simple topological features such as null points. Therefore, we derive the location of potential changes in magnetic connectivity by finding the field lines that experience a large relative change between their endpoints, i.e., the quasi-separatrix layer. We find a good correspondence between the locus of changes in magnetic connectivity or the quasi-separatrix layer and the map of large gradients in the integrated parallel electric field (or quasi-potential). Furthermore, we investigate the distribution of the parallel electric field along the reconnecting field lines. We find the reconnection rate is controlled by only the low-amplitude, zeroth and first-order trends in the parallel electric field while the contribution from fluctuations of the parallel electric field, such as electron holes, is negligible. The results impact the determination of reconnection sites and reconnection rates in models and in situ spacecraft observations of 3D turbulent reconnection. It is difficult through direct observation to isolate the loci of the reconnection parallel electric field amidst the large amplitude fluctuations. However, we demonstrate that a positive slope of the running sum of the parallel electric field along the field line as a function of field line length indicates where reconnection is occurring along the field line. (C) 2013 AIP Publishing LLC. C1 [Wendel, D. E.; Olson, D. K.; Hesse, M.; Kuznetsova, M.; Adrian, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Aunai, N.] Univ Toulouse 3, Inst Res Astrophys & Planetol, F-31062 Toulouse, France. [Karimabadi, H.] SciberQuest Inc, Del Mar, CA 92014 USA. [Karimabadi, H.] Univ Calif San Diego, Dept Comp & Elect Engn, La Jolla, CA 92093 USA. [Daughton, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Wendel, DE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI feggans, john/F-5370-2012; Wendel, Deirdre/D-4429-2012; Daughton, William/L-9661-2013; NASA MMS, Science Team/J-5393-2013 OI Wendel, Deirdre/0000-0002-1925-9413; NASA MMS, Science Team/0000-0002-9504-5214 FU NASA Goddard Space Flight Center; MMS; NASA; AGS [1104815] FX D. E. Wendel would like to thank Vadim Uritsky and John Dorelli for helpful discussions. This research was supported by a NASA Goddard Space Flight Center Science Innovation Fund award and by the MMS Interdisciplinary Science grant to the Goddard Space Flight Center. D. Olson and N. Aunai were supported by the NASA Postdoctoral Program. HK's contributions were supported by AGS grant no. 1104815 and NASA's Heliophysics Theory Program. W.D. was supported by NASA's Heliophysics Theory Program. NR 24 TC 12 Z9 12 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD DEC PY 2013 VL 20 IS 12 AR 122105 DI 10.1063/1.4833675 PG 8 WC Physics, Fluids & Plasmas SC Physics GA 282MU UT WOS:000329176800006 ER PT J AU Sadovsky, AV Davis, D Isaacson, DR AF Sadovsky, Alexander V. Davis, Damek Isaacson, Douglas R. TI Separation-compliant, optimal routing and control of scheduled arrivals in a terminal airspace SO TRANSPORTATION RESEARCH PART C-EMERGING TECHNOLOGIES LA English DT Article DE Multi-agent coordination; Route network; Roadmap; Motion planning; Optimal control; Multigraph ID HYBRID SYSTEMS AB We address the problem of navigating a set (fleet) of aircraft in an aerial route network so as to bring each aircraft to its destination at a specified time and with minimal distance separation assured between all aircraft at all times. The speed range, initial position, required destination, and required time of arrival at destination for each aircraft are assumed provided. Each aircraft's movement is governed by a controlled differential equation (state equation). The problem consists in choosing for each aircraft a path in the route network and a control strategy so as to meet the constraints and reach the destination at the required time. The main contribution of the paper is a model that allows to recast this problem as a decoupled collection of problems in classical optimal control and is easily generalized to the case when inertia cannot be neglected. Some qualitative insight into solution behavior is obtained using the Pontryagin Maximum Principle. Sample numerical solutions are computed using a numerical optimal control solver. The proposed model is first step toward increasing the fidelity of continuous-time control models of air traffic in a terminal airspace. The Pontryagin Maximum Principle implies the polygonal shape of those portions of the state trajectories away from those states in which one or more aircraft pair are at minimal separation. The model also confirms the intuition that, the narrower the allowed speed ranges of the aircraft, the smaller the space of optimal solutions, and that an instance of the optimal control problem may not have a solution at all (i.e., no control strategy that meets the separation requirement and other constraints). Published by Elsevier Ltd. C1 [Sadovsky, Alexander V.; Isaacson, Douglas R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Davis, Damek] Univ Calif Los Angeles, Dept Math, Los Angeles, CA 90095 USA. RP Sadovsky, AV (reprint author), NASA, Ames Res Ctr, Bldg 210,Mail Stop 210-6, Moffett Field, CA 94035 USA. EM alexander.v.sadovsky@nasa.gov FU NSF [DGE-0707424] FX D. Davis's research was supported by NSF Grant DGE-0707424. The authors thank D. Denery (NASA ARC) for suggesting the use of hybrid systems for ATM, W. Haskell (USC) for editing early drafts of the paper, H. Swenson (NASA ARC) and J. Mitchell (SUNY Stony Brook) for helpful suggestions, O. Diallo (NASA ARC) for help with editing in its final stages, and B. Fabien (University of Washington, Seattle) for help with the use of the OCP solver Fabien, 2011. The authors' choice of journal for this paper was based on the fact that air traffic management (ATM) in terminal space is a relatively narrow area of research, and, at that, somewhat isolated from the other areas of transportation engineering and operations research. (Research in other areas of ATM, e.g. airport surface traffic, has been published in Transportation Research journals.) We chose this journal in an attempt to break this "barrier" and reach a broader transportation research community than is commonly exposed to terminal space ATM work. NR 26 TC 2 Z9 2 U1 1 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0968-090X J9 TRANSPORT RES C-EMER JI Transp. Res. Pt. C-Emerg. Technol. PD DEC PY 2013 VL 37 BP 157 EP 176 DI 10.1016/j.trc.2013.09.017 PG 20 WC Transportation Science & Technology SC Transportation GA 285UC UT WOS:000329419500010 ER PT J AU Hueso, R Perez-Hoyos, S Sanchez-Lavega, A Wesley, A Hal, G Go, C Tachikawa, M Aoki, K Ichimaru, M Pond, JWT Korycansky, DG Palotai, C Chappe, G Rebeli, N Harrington, J Delcroix, M Wong, M de Paterm, I Fletcher, LN Hammel, H Orton, GS Tabe, I Watanabe, J Moreno, JC AF Hueso, R. Perez-Hoyos, S. Sanchez-Lavega, A. Wesley, A. Hal, G. Go, C. Tachikawa, M. Aoki, K. Ichimaru, M. Pond, J. W. T. Korycansky, D. G. Palotai, C. Chappe, G. Rebeli, N. Harrington, J. Delcroix, M. Wong, M. de Paterm, I. Fletcher, L. N. Hammel, H. Orton, G. S. Tabe, I. Watanabe, J. Moreno, J. C. TI Impact flux on Jupiter: From superbolides to large-scale collisions SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE meteorites, meteors, meteoroids; planets and satellites: atmospheres; planets and satellites: individual: Jupiter ID SHOEMAKER-LEVY-9 IMPACTS; TEMPORAL EVOLUTION; CRATERING RATE; FRIEND; CLOUD; COMET; RATES; DEBRIS; IMAGES; EARTH AB Context. Regular observations of Jupiter by a large number of amateur astronomers have resulted in the serendipitous discovery of short bright flashes in its atmosphere, which have been proposed as being caused by impacts of small objects. Three flashes were detected: one on June 3, 2010, one on August 20, 2010, and one on September 10, 2012. Aims. We show that the flashes are caused by impacting objects that we characterize in terms of their size, and we study the flux of small impacts on Jupiter. Methods. We measured the light curves of these atmospheric airbursts to extract their luminous energy and computed the masses and sizes of the objects. We ran simulations of impacts and compared them with the light curves. We analyzed the statistical significance of these events in the large pool of Jupiter observations. Results. All three objects are in the 5-20 m size category depending on their density, and they released energy comparable to the recent Chelyabinsk airburst. Model simulations approximately agree with the interpretation of the limited observations. Biases in observations of Jupiter suggest a rate of 12-60 similar impacts per year and we provide software tools for amateurs to examine the faint signature of impacts in their data to increase the number of detected collisions. Conclusions. The impact rate agrees with dynamical models of comets. More massive objects (a few 100 m) should impact with Jupiter every few years leaving atmospheric dark debris features that could be detectable about once per decade. C1 [Hueso, R.; Perez-Hoyos, S.; Sanchez-Lavega, A.] Univ Basque Country, ETS Ingn, EHU, Bilbao 48013, Spain. [Hueso, R.; Perez-Hoyos, S.; Sanchez-Lavega, A.] Univ Basque Country, CSIC, Unidad Asociada Grp Ciencias Planetarias, IAA, Bilbao 48013, Spain. [Wesley, A.] Acquerra Pty Ltd, Murrumbateman, NSW 2582, Australia. [Hal, G.] Univ Texas Dallas, Dept Phys, Richardson, TX 75080 USA. [Go, C.] Univ San Carlos, Dept Phys, Cebu 6000, Philippines. [Tachikawa, M.; Aoki, K.; Ichimaru, M.; Tabe, I.] Assoc Lunar & Planetary Observers Japan, Hino, Tokyo 1910032, Japan. [Pond, J. W. T.; Palotai, C.; Chappe, G.; Rebeli, N.; Harrington, J.] Univ Cent Florida, Dept Phys, Planetary Sci Grp, Orlando, FL 32816 USA. [Korycansky, D. G.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Delcroix, M.] Soc Astron France, Commiss Observat Planetaires, F-31170 Tournefeuille, France. [Wong, M.; de Paterm, I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fletcher, L. N.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [Hammel, H.] Space Sci Inst, Boulder, CO 80301 USA. [Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Watanabe, J.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Moreno, J. C.] Agrupac Astron Sabadell, Sabadell 08200, Spain. RP Hueso, R (reprint author), Univ Basque Country, ETS Ingn, EHU, Alameda Urquijo S-N, Bilbao 48013, Spain. EM ricardo.hueso@ehu.es RI Fletcher, Leigh/D-6093-2011; Harrington, Joseph/E-6250-2011; Perez-Hoyos, Santiago/L-7543-2014; OI Fletcher, Leigh/0000-0001-5834-9588; Perez-Hoyos, Santiago/0000-0002-2587-4682; Sanchez-Lavega, Agustin/0000-0001-7355-1522; Harrington, Joseph/0000-0002-8955-8531; Hueso, Ricardo/0000-0003-0169-123X FU Spanish MICIIN [AYA2009-10701, AYA2012-36666]; FEDER funds; Grupos Gobierno Vasco [IT765-13]; Universidad Pais Vasco UPV/EHU through program [UFI11/55]; National Science Foundation [AST-1109729]; NASA Planetary Atmospheres Program grant [NNX11AD87G]; HST [GO/DD-12119]; NASA through a grant from the Space Telescope Science Institute; NASA [NAS 5-26555]; NIRI at the Gemini Observatory [GS-2010A-DD-64, GN-2010A-DD-4]; VLT/VISIR at the European Organization for Astronomical Research in the Southern Hemisphere, Chile [60.A-9800(I)]; W. M. Keck Foundation; National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program [NNX-08AE38A] FX This work was supported by the Spanish MICIIN projects AYA2009-10701 and AYA2012-36666 with FEDER funds, by Grupos Gobierno Vasco IT765-13 and by Universidad Pais Vasco UPV/EHU through program UFI11/55. It was also supported by National Science Foundation grant AST-1109729 and NASA Planetary Atmospheres Program grant NNX11AD87G. This work is partially based on observations from the following telescopes. (1) HST (program GO/DD-12119), with support provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. (2) TRECS and NIRI at the Gemini Observatory (program GS-2010A-DD-64 and GN-2010A-DD-4), which is operated by the Association of Universities for Research in Astronomy, Inc., under agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia e Tecnologia (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). (3) VLT/VISIR (program 60.A-9800(I)) at the European Organization for Astronomical Research in the Southern Hemisphere, Chile. (4) NIRC2 at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. (5) TEXES at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. NR 57 TC 7 Z9 7 U1 1 U2 17 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2013 VL 560 AR A55 DI 10.1051/0004-6361/201322216 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 276MN UT WOS:000328754500055 ER PT J AU Rauch, T Werner, K Bohlin, R Kruk, JW AF Rauch, T. Werner, K. Bohlin, R. Kruk, J. W. TI The virtual observatory service TheoSSA: Establishing a database of synthetic stellar flux standards I. NLTE spectral analysis of the DA-type white dwarf G191-B2B SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE standards; stars: abundances; stars: atmospheres; stars: individual: G191-B2B; virtual observatory tools; white dwarfs ID LOCAL INTERSTELLAR-MEDIUM; ACCELERATED LAMBDA-ITERATION; CONSISTENT DIFFUSION-MODELS; NON-LTE ANALYSIS; HOT STARS; EFFECTIVE TEMPERATURES; MASS-DISTRIBUTION; FAR-ULTRAVIOLET; HYDROGEN-RICH; O-STARS AB Context. Hydrogen-rich, DA-type white dwarfs are particularly suited as primary standard stars for flux calibration. State-of-the-art NLTE models consider opacities of species up to trans-iron elements and provide reliable synthetic stellar-atmosphere spectra to compare with observations. Aims. We will establish a database of theoretical spectra of stellar flux standards that are easily accessible via a web interface. Methods. In the framework of the Virtual Observatory, the German Astrophysical Virtual Observatory developed the registered service TheoSSA. It provides easy access to stellar spectral energy distributions (SEDs) and is intended to ingest SEDs calculated by any model-atmosphere code. In case of the DA white dwarf G191-B2B, we demonstrate that the model reproduces not only its overall continuum shape but also the numerous metal lines exhibited in its ultraviolet spectrum. Results. TheoSSA is in operation and contains presently a variety of SEDs for DA-type white dwarfs. It will be extended in the near future and can host SEDs of all primary and secondary flux standards. The spectral analysis of G191-B2B has shown that our hydrostatic models reproduce the observations best at T-eff = 60 000 +/- 2000K and log g = 7.60 +/- 0.05. We newly identified Fe VI, Ni VI, and Zn IV lines. For the first time, we determined the photospheric zinc abundance with a logarithmic mass fraction of -4.89 (7.5 x solar). The abundances of He (upper limit), C, N, O, Al, Si, O, P, S, Fe, Ni, Ge, and Sn were precisely determined. Upper abundance limits of about 10% solar were derived for Ti, Cr, Mn, and Co. Conclusions. The TheoSSA database of theoretical SEDs of stellar flux standards guarantees that the flux calibration of all astronomical data and cross-calibration between different instruments can be based on the same models and SEDs calculated with different model-atmosphere codes and are easy to compare. C1 [Rauch, T.; Werner, K.] Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany. [Bohlin, R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rauch, T (reprint author), Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, Sand 1, D-72076 Tubingen, Germany. EM rauch@astro.uni-tuebingen.de FU German Aerospace Center (DLR) [05 OR 1301]; Federal Ministry of Education and Research (BMBF) [05 AC 6VTB, 05 AC 11 VTB]; BMBF [01 AK 804 [A-G]]; BMBF; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX TR is supported by the German Aerospace Center (DLR, grant 05 OR 1301). The GAVO project at Tubingen has been supported by the Federal Ministry of Education and Research (BMBF, grants 05 AC 6VTB, 05 AC 11 VTB). AstroGrid-D was funded by the BMBF (01 AK 804 [A-G]). The bwGRiD22 is funded within the framework of the D-Grid Project by the BMBF. This research has made use of the SIMBAD database, operated at the CDS, Strasbourg, France. This research has made use of NASA's Astrophysics Data System. This work used the WRPLOT visualization software developed by Wolf-Rainer Hamann (Potsdam) and the WRPLOT team. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. The TEUV tool (http://astro-uni-tuebingen.de/similar to TEUV) used to apply interstellar corrections to theoretical spectra was constructed as part of the activities of the German Astrophysical Virtual Observatory. The TIRO service (http://astro-uni-tuebingen.de/similar to TIRO) used to calculate opacities for this paper was constructed as part of the activities of the German Astrophysical Virtual Observatory. NR 105 TC 20 Z9 20 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2013 VL 560 AR A106 DI 10.1051/0004-6361/201322336 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 276MN UT WOS:000328754500106 ER PT J AU Chen, Y Morton, DC Jin, YF Gollatz, GJ Kasibhatla, PS van der Werf, GR DeFries, RS Randerson, JT AF Chen, Yang Morton, Douglas C. Jin, Yufang Gollatz, G. James Kasibhatla, Prasad S. van der Werf, Guido R. DeFries, Ruth S. Randerson, James T. TI Long-term trends and interannual variability of forest, savanna and agricultural fires in South America SO CARBON MANAGEMENT LA English DT Article ID BURNED AREA; AMAZONIAN FORESTS; BRAZILIAN AMAZON; SEASON SEVERITY; RADIATIVE POWER; DEFORESTATION; MODIS; CLIMATE; EMISSIONS; VALIDATION AB Background: Landscape fires in South America have considerable impacts on ecosystems, air quality and the climate system. We examined long-term trends and interannual variability of forest, savanna and agricultural fires for the continent during 2001-2012 using multiple satellite-derived fire products. Results: The annual number of active fires in tropical forests increased significantly during 2001-2005. Several satellite-derived metrics, including fire persistence, indicated that this trend was mostly driven by deforestation. Fires between 2005 and 2012 had a small decreasing trend and large year-to-year changes that were associated with climate extremes. Fires in savannas and evergreen forests increased in parallel during drought events in 2005,2007 and 2010, suggesting similar regional climate controls on fire behavior. Deforestation fire intensity (the number of fires per unit of deforested area) increased significantly within the Brazilian Amazon in areas with small-scale deforestation. Conclusion: Fires associated with forest degradation are becoming an increasingly important component of the fire regime and associated carbon emissions. C1 [Chen, Yang; Jin, Yufang; Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Morton, Douglas C.; Gollatz, G. James] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kasibhatla, Prasad S.] Duke Univ, Nicholas Sch Environm & Earth Sci, Durham, NC 27705 USA. [van der Werf, Guido R.] Vrije Univ Amsterdam, Fac Earth & Life Sci, Amsterdam, Netherlands. [DeFries, Ruth S.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. RP Chen, Y (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. EM yang.chen@uci.edu RI Morton, Douglas/D-5044-2012; van der Werf, Guido/M-8260-2016; OI van der Werf, Guido/0000-0001-9042-8630; Kasibhatla, Prasad/0000-0003-3562-3737 FU NASA [NNX08AF64G, NNX11AF96G]; Gordon and Betty Moore Foundation (CA, USA) [GBMF3269] FX This research was supported by NASA grants NNX08AF64G and NNX11AF96G, and the Gordon and Betty Moore Foundation (CA, USA; GBMF3269). The authors have no other relevant affiliations or financial involvement with any organization or entity with a financial interest in or financial conflict with the subject matter or materials discussed in the manuscript apart from those disclosed. NR 87 TC 24 Z9 24 U1 4 U2 36 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 1758-3004 EI 1758-3012 J9 CARBON MANAG JI Carbon Manag. PD DEC PY 2013 VL 4 IS 6 BP 617 EP 638 DI 10.4155/CMT.13.61 PG 22 WC Environmental Sciences; Environmental Studies SC Environmental Sciences & Ecology GA 270GM UT WOS:000328306900013 ER PT J AU Gehrels, N Razzaque, S AF Gehrels, Neil Razzaque, Soebur TI Gamma-ray bursts in the swift-Fermi era SO FRONTIERS OF PHYSICS LA English DT Review DE gamma-ray bursts (GRBs); Swift; Fermi ID HIGH-ENERGY EMISSION; SHORT GRB 090510; STAR-FORMATION HISTORY; INTERNAL SHOCK MODEL; 28 FEBRUARY 1997; X-RAY; PROMPT EMISSION; BLACK-HOLE; MAGNETIC-FIELDS; SPECTRAL COMPONENT AB Gamma-ray bursts (GRBs) are among the most violent occurrences in the universe. They are powerful explosions, visible to high redshift, and thought to be the signature of black hole birth. They are highly luminous events and provide excellent probes of the distant universe. GRB research has greatly advanced over the past 10 years with the results from Swift, Fermi and an active follow-up community. In this review we survey the interplay between these recent observations and the theoretical models of the prompt GRB emission and the subsequent afterglows. C1 [Gehrels, Neil] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Razzaque, Soebur] George Mason Univ, Fairfax, VA 22030 USA. [Razzaque, Soebur] Naval Res Lab Washington, Div Space Sci, Washington, DC 20375 USA. RP Gehrels, N (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. EM neil.gehrels@nasa.gov; srazzaqu@gmu.edu FU NASA Fermi Guest Investigator program FX We thank John Cannizzo and Charles Dermer for valuable consultation and comments on this paper. All data from the Swift and Fermi observatories are publicly available through NASA's High Energy Astrophysics Science Archive Research Center (HEASARC) at http://heasarc.gsfc.nasa.gov/. Work of S.R. was supported by NASA Fermi Guest Investigator program and was performed at the Naval Research Lab while under contract. NR 204 TC 18 Z9 19 U1 0 U2 5 PU HIGHER EDUCATION PRESS PI BEIJING PA NO 4 DEWAI DAJIE, BEIJING 100120, PEOPLES R CHINA SN 2095-0462 J9 FRONT PHYS-BEIJING JI Front. Phys. PD DEC PY 2013 VL 8 IS 6 BP 661 EP 678 DI 10.1007/s11467-013-0282-3 PG 18 WC Physics, Multidisciplinary SC Physics GA 278PH UT WOS:000328901700004 ER PT J AU Harding, AK AF Harding, Alice K. TI The neutron star zoo SO FRONTIERS OF PHYSICS LA English DT Review DE stars; neutron stars; pulsars; binary stars ID X-RAY PULSAR; LARGE-AREA TELESCOPE; SOFT GAMMA-REPEATERS; HIGH-ENERGY; MAGNETIC-FIELD; CRAB-NEBULA; SUPERNOVA REMNANT; FERMI LAT; BRIGHTNESS OSCILLATIONS; BULK COMPTONIZATION AB Neutron stars are a very diverse population, both in their observational and their physical properties. They prefer to radiate most of their energy at X-ray and gamma-ray wavelengths. But whether their emission is powered by rotation, accretion, heat, magnetic fields or nuclear reactions, they are all different species of the same animal whose magnetic field evolution and interior composition remain a mystery. This article will broadly review the properties of inhabitants of the neutron star zoo, with emphasis on their high-energy emission. C1 NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Harding, AK (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. EM Alice.K.Harding@nasa.gov NR 119 TC 20 Z9 20 U1 0 U2 9 PU HIGHER EDUCATION PRESS PI BEIJING PA NO 4 DEWAI DAJIE, BEIJING 100120, PEOPLES R CHINA SN 2095-0462 J9 FRONT PHYS-BEIJING JI Front. Phys. PD DEC PY 2013 VL 8 IS 6 BP 679 EP 692 DI 10.1007/s11467-013-0285-1 PG 14 WC Physics, Multidisciplinary SC Physics GA 278PH UT WOS:000328901700005 ER PT J AU King, MP Reed, RA Weller, RA Mendenhall, MH Schrimpf, RD Sierawski, BD Sternberg, AL Narasimham, B Wang, JK Pitta, E Bartz, B Reed, D Monzel, C Baumann, RC Deng, X Pellish, JA Berg, MD Seidleck, CM Auden, EC Weeden-Wright, SL Gaspard, NJ Zhang, CX Fleetwood, DM AF King, M. P. Reed, R. A. Weller, R. A. Mendenhall, M. H. Schrimpf, R. D. Sierawski, B. D. Sternberg, A. L. Narasimham, B. Wang, J. K. Pitta, E. Bartz, B. Reed, D. Monzel, C. Baumann, R. C. Deng, X. Pellish, J. A. Berg, M. D. Seidleck, C. M. Auden, E. C. Weeden-Wright, S. L. Gaspard, N. J. Zhang, C. X. Fleetwood, D. M. TI Electron-Induced Single-Event Upsets in Static Random Access Memory SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 50th annual IEEE Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 08-12, 2013 CL San Francisco, CA DE Energetic electron; error rate; single-event effects (SEEs); single-event upset (SEU); static random access memory (SRAM) ID SILICON-ON-INSULATOR; NM SOI SRAM; CRITICAL CHARGE; MOS DEVICES; RADIATION; ENERGY; SIMULATION; LATCHES; CELLS AB We present experimental evidence of single-event upsets in 28 and 45 nm CMOS SRAMs produced by single energetic electrons. Upsets are observed within 10% of nominal supply voltage for devices built in the 28 nm technology node. Simulation results provide supporting evidence that upsets are produced by energetic electrons generated by incident X-rays. The observed errors are shown not to be the result of "weak bits" or photocurrents resulting from the collective energy deposition from X-rays. Experimental results are consistent with the bias sensitivity of critical charge for direct ionization effects caused by low-energy protons and muons in these technologies. Monte Carlo simulations show that the contributions of electron-induced SEU to error rates in the GEO environment depend exponentially on critical charge. C1 [King, M. P.; Reed, R. A.; Weller, R. A.; Mendenhall, M. H.; Schrimpf, R. D.; Sierawski, B. D.; Sternberg, A. L.; Auden, E. C.; Weeden-Wright, S. L.; Gaspard, N. J.; Zhang, C. X.; Fleetwood, D. M.] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37237 USA. [Narasimham, B.; Wang, J. K.; Pitta, E.; Bartz, B.; Reed, D.; Monzel, C.] Broadcom Corp, Irvine, CA 92617 USA. [Baumann, R. C.; Deng, X.] Texas Instruments Inc, Dallas, TX 75243 USA. [Pellish, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Berg, M. D.; Seidleck, C. M.] MEI Technol, Seabrook, MD 20706 USA. RP King, MP (reprint author), Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37237 USA. EM michael.p.king@vanderbilt.edu RI Schrimpf, Ronald/L-5549-2013; Zhang , Cher Xuan/J-4754-2015 OI Schrimpf, Ronald/0000-0001-7419-2701; Zhang , Cher Xuan/0000-0003-0518-864X FU Defense Threat Reduction Agency; NASA FX The authors would like to thank the Defense Threat Reduction Agency Basic Research Program and the NASA Electronic Parts and Packaging Program for their support of this work. The authors offer special thanks to Dr. F. Salvat (Facultat de Fisica, Universitat de Barcelona, Spain) and M. Asai (SLAC National Accelerator Laboratory, Menlo Park, CA, USA), for making PENELOPE 2008 and a Fortran/c++ interface between it and Geant4 available to them. They also thank E. Blackmore and M. Trinczek (TRIUMF, Vancouver, BC, Canada) for their help and experiments, and Dr. L. Massengill for interesting and informative discussions regarding this work. NR 27 TC 18 Z9 18 U1 1 U2 14 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2013 VL 60 IS 6 BP 4122 EP 4129 DI 10.1109/TNS.2013.2286523 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 279NY UT WOS:000328967900012 ER PT J AU Berg, MD Kim, HS Phan, AD Seidleck, CM LaBel, KA Pellish, JA AF Berg, Melanie D. Kim, Hak S. Phan, Anthony D. Seidleck, Christina M. LaBel, Kenneth A. Pellish, Jonathan A. TI Single Event Induced Multiple Bit Errors and the Effects of Logic Masking SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 50th annual IEEE Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 08-12, 2013 CL San Francisco, CA DE Field programmable gate array (FPGA); single event transient (SET); single event upset (SEU); synchronous design ID SER ESTIMATION AB We apply a model and heavy-ion cross section data to predict the potential that one single event upset (SEU) will induce multiple bit errors (MBEs) by the next clock-cycle of a synchronous design. C1 [Berg, Melanie D.; Kim, Hak S.; Phan, Anthony D.; Seidleck, Christina M.] ASRC Fed Space & Def, Greenbelt, MD 20771 USA. [LaBel, Kenneth A.; Pellish, Jonathan A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Berg, MD (reprint author), ASRC Fed Space & Def, Greenbelt, MD 20771 USA. EM melanie.d.berg@nasa.gov FU NASA Electronic Parts and Packaging Program (NEPP); NASA Flight Projects; Defense Threat Reduction Agency (DTRA) [IACRO10-4977I, 11-4395I] FX This work was supported in part by the NASA Electronic Parts and Packaging Program (NEPP), NASA Flight Projects, and the Defense Threat Reduction Agency (DTRA) under IACRO10-4977I and 11-4395I. NR 11 TC 0 Z9 0 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2013 VL 60 IS 6 BP 4192 EP 4199 DI 10.1109/TNS.2013.2290753 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 279NY UT WOS:000328967900021 ER PT J AU Ladbury, RL Berg, MD Wilcox, EP LaBel, KA Kim, HS Phan, AM Seidleck, CM AF Ladbury, R. L. Berg, M. D. Wilcox, E. P. LaBel, K. A. Kim, H. S. Phan, A. M. Seidleck, C. M. TI Use of Commercial FPGA-Based Evaluation Boards for Single-Event Testing of DDR2 and DDR3 SDRAMs SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 50th annual IEEE Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 08-12, 2013 CL San Francisco, CA DE Probabilistic risk assessment; quality assurance; radiation effects in ICs; radiation hardness assurance; reliability estimation; testing techniques AB The speed, tight timing requirements packaging and complicated error behavior of DDR2 and DDR3 SDRAMs pose significant challenges for single-event testing. Often, each new generation will require an expensive new tester with a state-of-the-art controller for the memory. We explore the trade-offs in the use of commercial FPGA based evaluation boards for radiation testing DDR2 and DDR3 SDRAMs. We evaluate the resulting data quality and discuss tester performance while also elucidating and comparing SEE susceptibilities in DDR2 and DDR3 SDRAMs. C1 [Ladbury, R. L.; LaBel, K. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Berg, M. D.; Wilcox, E. P.; Kim, H. S.; Phan, A. M.; Seidleck, C. M.] MEI Technol, Seabrook, MD 20706 USA. RP Ladbury, RL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM raymond.l.ladbury@nasa.gov FU NASA Electronic Parts and Packaging program; Defense Threat Reduction Agency; BAE Systems in Manassas, VA FX This work was supported in part by the NASA Electronic Parts and Packaging program, the Defense Threat Reduction Agency, and BAE Systems in Manassas, VA. NR 6 TC 2 Z9 3 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2013 VL 60 IS 6 BP 4457 EP 4463 DI 10.1109/TNS.2013.2285517 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 279NY UT WOS:000328967900058 ER PT J AU Ladbury, RL Campola, MJ AF Ladbury, R. L. Campola, M. J. TI Bayesian Methods for Bounding Single-Event Related Risk in Low-Cost Satellite Missions SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 50th annual IEEE Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 08-12, 2013 CL San Francisco, CA DE Probabilistic risk assessment; quality assurance; radiation effects; radiation hardness assurance methodology; reliability estimation AB Adapting conventional SEE hardness assurance approaches to low-cost, risk tolerant missions has proven difficult. Such approaches do not have a natural approach for realizing cost savings for increased risk tolerance. We develop single-event-risk prior probability distributions based on historical and heritage data. The Priors can be used to bound SEE risk for testing, part selection and design. By adjusting the desired confidence and success probability for the prior, one can tailor it to the risk tolerance of the mission. C1 [Ladbury, R. L.; Campola, M. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ladbury, RL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM raymond.l.ladbury@nasa.gov; michael.j.campola@nasa.gov FU NASA GSFC IRAD program FX The authors would like to thank the NASA GSFC IRAD program for support of this research and Sana Rezgui of LTC for tirelessly fielding questions about fabrication processes and design. NR 8 TC 3 Z9 3 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2013 VL 60 IS 6 BP 4464 EP 4469 DI 10.1109/TNS.2013.2285519 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 279NY UT WOS:000328967900059 ER PT J AU Johnston, AH Swimm, RT Thorbourn, DO AF Johnston, A. H. Swimm, R. T. Thorbourn, D. O. TI Charge Yield at Low Electric Fields: Considerations for Bipolar Integrated Circuits SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 50th annual IEEE Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 08-12, 2013 CL San Francisco, CA DE Bipolar integrated circuit; ionizing radiation; radiation effects; recombination ID X-RAY; GAIN DEGRADATION; MOS CAPACITORS; CO-60; HOLE; TRANSPORT; DEVICES; RECOMBINATION; IRRADIATIONS; TRANSISTOR AB A significant reduction in total dose damage is observed when bipolar integrated circuits are irradiated at low temperature. This can be partially explained by the Onsager theory of recombination, which predicts a strong temperature dependence for charge yield under low-field conditions. Reduced damage occurs for biased as well as unbiased devices because the weak fringing field in thick bipolar oxides only affects charge yield near the Si/SiO2 interface, a relatively small fraction of the total oxide thickness. Lowering the temperature of bipolar ICs-either continuously, or for time periods when they are exposed to high radiation levels-provides an additional degree of freedom to improve total dose performance of bipolar circuits, particularly in space applications. C1 [Johnston, A. H.; Swimm, R. T.; Thorbourn, D. O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Johnston, AH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM JohnstonAH25@gmail.com; randall.t.swimm@jpl.nasa.gov; dennis.o.thorbourn@jpl.nasa.gov FU National Aeronautics and Space Agency (NASA) FX The research in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Agency (NASA). NR 27 TC 5 Z9 5 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2013 VL 60 IS 6 BP 4488 EP 4497 DI 10.1109/TNS.2013.2283515 PN 1 PG 10 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 279NY UT WOS:000328967900063 ER PT J AU Hong, J Allen, B Grindlay, J Rodrigues, B Ellis, JR Baker, R Barthelmy, S Mao, P Miyasaka, H Apple, J AF Hong, Jaesub Allen, Branden Grindlay, Jonathan Rodrigues, Barbara Ellis, Jon Robert Baker, Robert Barthelmy, Scott Mao, Peter Miyasaka, Hiromasa Apple, Jeff TI Tiled Array of Pixelated CZT Imaging Detectors for ProtoEXIST2 and MIRAX-HXI SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE Astrophysics; semiconductor radiation detectors; telescopes; X-ray detectors ID MISSION AB We have assembled a tiled array (220 cm(2)) of fine pixel (0.6 mm) imaging CZT detectors for a balloon borne wide-field hard X-ray telescope, ProtoEXIST2. ProtoEXIST2 is a prototype experiment for a next generation hard X-ray imager MIRAX-HXI on board Lattes, a spacecraft from the Agencia Espacial Brasilieira. MIRAX will survey the 5 to 200 keV sky of Galactic bulge, adjoining southern Galactic plane and the extragalactic sky with 6' angular resolution. This survey will open a vast discovery space in timing studies of accretion neutron stars and black holes. The ProtoEXIST2 CZT detector plane consists of 64 of 5 mm thick 2 cm 2 cm CZT crystals tiled with a minimal gap. MIRAX will consist of 4 such detector planes, each of which will be imaged with its own coded-aperture mask. We present the packaging architecture and assembly procedure of the ProtoEXIST2 detector. On 2012, Oct 10, we conducted a successful high altitude balloon experiment of the ProtoEXIST1 and 2 telescopes, which demonstrates their technology readiness for space application. During the flight both telescopes performed as well as on the ground. We report the results of ground calibration and the initial results for the detector performance in the balloon flight. C1 [Hong, Jaesub; Allen, Branden; Grindlay, Jonathan; Ellis, Jon Robert] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. [Rodrigues, Barbara] INPE, BR-12227Y01 Sao Jose Dos Campos, SP, Brazil. [Baker, Robert; Barthelmy, Scott] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mao, Peter; Miyasaka, Hiromasa] CALTECH, Pasadena, CA 91125 USA. [Apple, Jeff] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Hong, J (reprint author), Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. EM jaesub@head.cfa.harvard.edu FU NASAGgrants [NNX09AD96G, NNX11AF35G] FX This work was supported by NASAGgrants NNX09AD96G and NNX11AF35G. NR 11 TC 1 Z9 1 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2013 VL 60 IS 6 BP 4610 EP 4617 DI 10.1109/TNS.2013.2283806 PN 2 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 279PI UT WOS:000328971500005 ER PT J AU Lee, C Kim, YH Kim, JH Jee, G Won, YI Wu, DL AF Lee, Changsup Kim, Yong Ha Kim, Jeong-Han Jee, Geonhwa Won, Young-In Wu, Dong L. TI Seasonal variation of wave activities near the mesopause region observed at King Sejong Station (62.22 degrees S, 58.78 degrees W), Antarctica SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Gravity wave; Tide; Antarctic vortex; Neutral winds; Meteor radar ID ARCTIC STRATOSPHERIC VORTEX; MIDDLE ATMOSPHERE; GRAVITY-WAVES; LOWER THERMOSPHERE; MOUNTAIN WAVES; MOMENTUM FLUX; MEAN WINDS; TIDES; CLIMATOLOGY; DYNAMICS AB We analyzed the neutral wind data at altitudes' of 80-100 km obtained from a VHF meteor radar at King Sejong Station (KSS, 62.22 degrees S, 58.78 degrees W), a key location to study wave activities above the stratospheric vortex near the Antarctic Peninsula. The seasonal behavior of the semidiurnal tides is generally consistent with the prediction of Global Scale Wave Model (GSWM02) except in the altitude region above 96 km. Gravity wave (GW) activities inferred from the neutral wind variances show a seasonal variation very similar to the semidiurnal tide amplitudes, suggesting a strong interaction between gravity waves and the tide. Despite the consistent seasonal variations of the GW wind variances observed at the adjacent Rothera station, the magnitudes of the wind variance obtained at KSS are much larger than those at Rothera, especially during May-September. The enhanced GW activity at KSS is also observed by Aura Microwave Limb Sounder (MLS) from space in its temperature variance. The observed large wind variances at KSS imply that the Antarctic vortex in the stratosphere may act as an effective filter and source for the GWs in the upper atmosphere. (C) 2013 Published by Elsevier Ltd. C1 [Lee, Changsup; Kim, Yong Ha] Chungnam Natl Univ, Dept Astron & Space Sci, Taejon 305764, South Korea. [Lee, Changsup; Kim, Jeong-Han; Jee, Geonhwa] Korea Polar Res Inst, Inchon 406840, South Korea. [Won, Young-In] NASA, Goddard Space Flight Ctr, Wyle IS Natl Space Sci Data Ctr, Greenbelt, MD 20771 USA. [Wu, Dong L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kim, YH (reprint author), Chungnam Natl Univ, Dept Astron & Space Sci, 99 Daehak Ro St, Taejon 305764, South Korea. EM yhkim@cnu.ac.kr RI Wu, Dong/D-5375-2012 FU Korea Polar Research Institute [PE13010] FX This work was supported by research funds PE13010 from Korea Polar Research Institute. NR 44 TC 5 Z9 5 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD DEC PY 2013 VL 105 BP 30 EP 38 DI 10.1016/j.jastp.2013.07.006 PG 9 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 278TQ UT WOS:000328913100004 ER PT J AU Lipatov, AS Cooper, JF Sittler, EC Hartle, RE AF Lipatov, A. S. Cooper, J. F. Sittler, E. C., Jr. Hartle, R. E. TI The light (H+, H-2(+), He+) and heavy (Na+) pickup ion dynamics in the lunar-like plasma environment: 3D hybrid kinetic modeling SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Exospheres; Pickup ions; Induced magnetospheres; Satellites; Plasma modeling ID SOLAR-WIND; WAKE; SIMULATIONS; MOON; FIELD; HELIOSPHERE; ATMOSPHERE; EXOSPHERE; SODIUM; COMETS AB In this report we discuss the self-consistent dynamics of pickup ions in the solar wind flow around the lunar-like object. In our model the solar wind and pickup ions are considered as a particles, whereas the electrons, are described as a fluid. Inhomogeneous photoionization, electron-impact ionization and charge exchange are included in our model. The Moon will be chosen as a basic object for our modeling. The current modeling shows that mass loading by pickup ions H+, H-2(+), He+, and Na+ may be very important in the global dynamics of the solar wind around the Moon. In our hybrid modeling we use exponential profiles for the exospheric components. The Moon is considered as a weakly conducting body. Special attention will be paid to comparing the modeling pickup ion velocity distribution with ARTEMIS observations. Our modeling shows an asymmetry of the Mach cone due to mass loading, the upstream flow density distribution and the magnetic field. The pickup ions form an asymmetrical plasma tails that may disturb the lunar plasma wake. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Lipatov, A. S.] NASA, Goddard Space Flight Ctr, UMBC, GPHI, Greenbelt, MD 20771 USA. [Cooper, J. F.; Sittler, E. C., Jr.; Hartle, R. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lipatov, AS (reprint author), Moscow Inst Phys & Technol, Moscow, Russia. EM Alexander.Lipatov-1@nasa.gov; John.F.Cooper@nasa.gov; Edward.C.-Sittler@nasa.gov; Richard.E.Hartle@nasa.gov RI Cooper, John/D-4709-2012 FU NASA NRA: Lunar Advance Science and Exploration Research Program [NNH08ZDA001-LASER]; GPHI UMBC [670-90-315]; NASA GSFC [670-90-315] FX A.S.L., J.F.C., E.C.S., and R.E.H were supported by the Grant Solar Wind Interaction with Lunar Exosphere and Sinface (PI - J.F. Cooper) from the NASA NRA: Lunar Advance Science and Exploration Research Program (NNH08ZDA001-LASER). A.S.L. was also supported in part by the Grant/task 670-90-315 between the GPHI UMBC and NASA GSFC. Computational resources were provided by the NASA Ames Advanced Supercomputing (NAS) Division (Project SMD-11-2205 and SMP-122957). The authors thank the referees for fruitful comments. NR 50 TC 1 Z9 1 U1 0 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD DEC 1 PY 2013 VL 52 IS 11 BP 1929 EP 1938 DI 10.1016/j.asr.2013.08.023 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 273FU UT WOS:000328521500008 ER PT J AU Krause, LH Enloe, CL McHarg, MG AF Krause, L. Habash Enloe, C. L. McHarg, M. G. TI In situ measurements of ionospheric plasma turbulence over five frequency decades: Heritage flight of the Plasma Local Anomalous Noise Experiment (PLANE) SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Ionospheric turbulence; Plasma turbulence; Retarding potential analyzers; Plasma wave measurements ID LANGMUIR PROBE; BUBBLES AB Observations of ionospheric plasma density and frequency-dependent broadband plasma turbulence made during the heritage flight of the Plasma Local Anomalous Noise Experiment (PLANE) are presented. Rather than record high frequency time series data, the experiment was designed to record Power Spectral Distributions (PSDs) in five decadal frequency bins with upper limits ranging from 1.0 Hz to 10 kHz. Additionally, PLANE was designed distinguish turbulence in the ambient plasma from that local to the spacecraft. The instrument consists of two retarding potential analyzers (RPAs) connected together via a feedback loop to force one analyzer into the I-V trace retardation region at all times. Fluctuations in this measurement are believed to be ambient only as the RPA's voltage would be too high for locally turbulent plasma to surmount the potential barrier, which is nominally at ram energy. The instrument requires pointing along the spacecraft's ram velocity vector to make this measurement, thus requiring stabilization in pitch and yaw. During PLANE's heritage flight, though the satellite's attitude control system failed early in the mission, plasma data were collected during opportune times in which the instrument rotated into and out of the ram. Observations of plasma density and PSDs of high frequency plasma turbulence were recorded on several occasions. Additionally, a plasma source onboard the satellite was used to generate artificial plasma turbulence, and the PLANE data observed periodic structure presumably associated with the rotation of the spacecraft during these source firings. A brief comparison with other high frequency in situ plasma instruments is presented. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Krause, L. Habash] NASA, Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Enloe, C. L.; McHarg, M. G.] US Air Force Acad, Dept Phys, HQ USAFA DFP, Colorado Springs, CO 80840 USA. RP Krause, LH (reprint author), NASA, Marshall Space Flight Ctr, Space Sci Off, ZP13, Huntsville, AL 35812 USA. EM Linda.H.Krause@nasa.gov; Lon.Enloe@usafa.edu; Matthew.McHarg@usafa.edu NR 23 TC 0 Z9 0 U1 1 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD DEC 1 PY 2013 VL 52 IS 11 BP 2006 EP 2014 DI 10.1016/j.asr.2013.06.032 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 273FU UT WOS:000328521500016 ER PT J AU Zacny, K Paulsen, G McKay, CP Glass, B Dave, A Davila, AF Marinova, M Mellerowicz, B Heldmann, J Stoker, C Cabrol, N Hedlund, M Craft, J AF Zacny, K. Paulsen, G. McKay, C. P. Glass, B. Dave, A. Davila, A. F. Marinova, M. Mellerowicz, B. Heldmann, J. Stoker, C. Cabrol, N. Hedlund, M. Craft, J. TI Reaching 1m Deep on Mars: The Icebreaker Drill SO ASTROBIOLOGY LA English DT Article DE Drilling; Sampling; Mars; Mars drilling; Subsurface exploration; Ice; Search for life ID GROUND ICE; STRENGTH; MODEL; SITE; LIFE; TEMPERATURE; EXPLORATION; ANTARCTICA; MISSION; SURFACE AB The future exploration of Mars will require access to the subsurface, along with acquisition of samples for scientific analysis and ground-truthing of water ice and mineral reserves for in situ resource utilization. The Icebreaker drill is an integral part of the Icebreaker mission concept to search for life in ice-rich regions on Mars. Since the mission targets Mars Special Regions as defined by the Committee on Space Research (COSPAR), the drill has to meet the appropriate cleanliness standards as requested by NASA's Planetary Protection Office. In addition, the Icebreaker mission carries life-detection instruments; and in turn, the drill and sample delivery system have to meet stringent contamination requirements to prevent false positives. This paper reports on the development and testing of the Icebreaker drill, a 1m class rotary-percussive drill and triple redundant sample delivery system. The drill acquires subsurface samples in short, approximately 10cm bites, which makes the sampling system robust and prevents thawing and phase changes in the target materials. Autonomous drilling, sample acquisition, and sample transfer have been successfully demonstrated in Mars analog environments in the Arctic and the Antarctic Dry Valleys, as well as in a Mars environmental chamber. In all environments, the drill has been shown to perform at the 1-1-100-100 level; that is, it drilled to 1m depth in approximately 1 hour with less than 100N weight on bit and approximately 100 W of power. The drilled substrate varied and included pure ice, ice-rich regolith with and without rocks and with and without 2% perchlorate, and whole rocks. The drill is currently at a Technology Readiness Level (TRL) of 5. The next-generation Icebreaker drill weighs 10kg, which is representative of the flightlike model at TRL 5/6. C1 [Zacny, K.; Paulsen, G.; Mellerowicz, B.; Hedlund, M.; Craft, J.] Honeybee Robot, Pasadena, CA 91103 USA. [McKay, C. P.; Glass, B.; Dave, A.; Davila, A. F.; Heldmann, J.; Stoker, C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Marinova, M.] Space Explorat Technol Corp, Hawthorne, CA USA. [Cabrol, N.] SETI Inst, Carl Sagan Ctr Mt View, Mountain View, CA USA. [Cabrol, N.] NASA, Ames Space Sci Div, Moffett Field, CA USA. RP Zacny, K (reprint author), Honeybee Robot, 398 W Washington Blvd,Suite 200, Pasadena, CA 91103 USA. EM zacny@honeybeerobotics.com RI Davila, Alfonso/A-2198-2013 OI Davila, Alfonso/0000-0002-0977-9909 FU NASA [NNA09DA97C, NNX11AJ87G]; US Antarctic Program as part of the National Science Foundation Office of Polar Programs FX The research reported in this manuscript was funded by the National Aeronautics and Space Administration (NASA) Astrobiology Science and Technology for Exploring Planets (ASTEP) and Astrobiology Science and Technology Instrument Development (ASTID) programs: NASA Contracts NNA09DA97C "Mars Umbrella Drilling Scout (MUDS)'', and NNX11AJ87G "Robotic Investigation of Subsurface Life in the Atacama''. Testing in Antarctica was supported by the US Antarctic Program as part of the National Science Foundation Office of Polar Programs. NR 76 TC 4 Z9 5 U1 2 U2 25 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD DEC 1 PY 2013 VL 13 IS 12 BP 1166 EP 1198 DI 10.1089/ast.2013.1038 PG 33 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 273WE UT WOS:000328566200005 PM 24303959 ER PT J AU Gibson, EK Thomas-Keprta, K Clemett, S Morris-Smith, P AF Gibson, Everett K. Thomas-Keprta, Kathie Clemett, Simon Morris-Smith, Penny TI David S. McKay, 1936-2013 Tribute SO ASTROBIOLOGY LA English DT Biographical-Item C1 [Gibson, Everett K.; Thomas-Keprta, Kathie; Clemett, Simon; Morris-Smith, Penny] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. RP Gibson, EK (reprint author), NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. EM everett.k.gibson@nasa.gov NR 1 TC 0 Z9 0 U1 0 U2 2 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD DEC 1 PY 2013 VL 13 IS 12 BP 1203 EP 1206 DI 10.1089/ast.2013.8425 PG 4 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 273WE UT WOS:000328566200007 PM 23725408 ER PT J AU Birkeland, C Miller, MW Piniak, GA Eakin, CM Weijerman, M McElhany, P Dunlap, M Brainard, RE AF Birkeland, Charles Miller, Margaret W. Piniak, Gregory A. Eakin, C. Mark Weijerman, Mariska McElhany, Paul Dunlap, Matthew Brainard, Russell E. TI Safety in Numbers? Abundance May Not Safeguard Corals from Increasing Carbon Dioxide SO BIOSCIENCE LA English DT Article DE coral; density independence; depensatory; extinction; sessile ID BROADCAST-SPAWNING CORALS; ACROPORA-PALMATA; CARIBBEAN CORALS; REEFS; FERTILIZATION; DECLINE; SETTLEMENT; ANNULARIS; FECUNDITY; RECOVERY AB Marine conservation efforts are often focused on increasing stocks of species with low population abundances by reducing mortality or enhancing recruitment. However, global changes in climate and ocean chemistry are density-independent factors that can strongly affect corals whether they are scarce or abundant-sometimes, the abundant corals are most affected. Because reproductive corals are sessile, density-independent effects of global changes such as physiological stress and resultant mortality can decouple stock abundance from recruitment and may accelerate the downward spiral of their reproductive rates. C1 [Birkeland, Charles] Univ Hawaii Manoa, Dept Biol, Honolulu, HI USA. [Miller, Margaret W.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Miami, FL USA. [Piniak, Gregory A.] Natl Ctr Coastal Ocean Sci, Natl Ocean Serv, US Natl Ocean & Atmospher Adm NOAA, Silver Spring, MD USA. [Eakin, C. Mark] Ctr Satellite Applicat & Res, College Pk, MD USA. [Weijerman, Mariska; Dunlap, Matthew] Univ Hawaii Manoa, Inst Marine & Atmospher Res, Honolulu, HI USA. [McElhany, Paul] NOAA, Natl Marine Fisheries Serv, NW Fisheries Ctr, Seattle, WA 98112 USA. [Brainard, Russell E.] Natl Marine Fisheries Serv, Pacific Islands Fisheries Sci Ctr, Coral Reef Ecosyst Div, Honolulu, HI USA. RP Birkeland, C (reprint author), Univ Hawaii Manoa, Dept Biol, Honolulu, HI USA. EM charlesb@hawaii.edu RI Eakin, C. Mark/F-5585-2010 NR 40 TC 4 Z9 5 U1 0 U2 26 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA SN 0006-3568 EI 1525-3244 J9 BIOSCIENCE JI Bioscience PD DEC PY 2013 VL 63 IS 12 BP 967 EP 974 DI 10.1525/bio.2013.63.12.9 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 276AK UT WOS:000328720300011 ER PT J AU Wells, BK Schroeder, ID Santora, JA Hazen, EL Bograd, SJ Bjorkstedt, EP Loeb, VJ Mcclatchie, S Weber, ED Watson, W Thompson, AR Peterson, WT Brodeur, RD Harding, J Field, J Sakuma, K Hayes, S Mantua, N Sydeman, WJ Losekoot, M Thompson, SA Largier, J Kim, SY Chavez, FP Barcelo, C Warzybok, P Bradley, R Jahncke, J Goericke, R Campbell, GS Hildebrand, JA Melin, SR Delong, RL Gomez-Valdes, J Lavaniegos, B Gaxiola-Castro, G Golightly, RT Schneider, SR Lo, N Suryan, RM Gladics, AJ Horton, CA Fisher, J Morgan, C Peterson, J Daly, EA Auth, TD Abell, J AF Wells, Brian K. Schroeder, Isaac D. Santora, Jarrod A. Hazen, Elliott L. Bograd, Steven J. Bjorkstedt, Eric P. Loeb, Valerie J. Mcclatchie, Sam Weber, Edward D. Watson, William Thompson, Andrew R. Peterson, William T. Brodeur, Richard D. Harding, Jeff Field, John Sakuma, Keith Hayes, Sean Mantua, Nathan Sydeman, William J. Losekoot, Marcel Thompson, Sarah Ann Largier, John Kim, Sung Yong Chavez, Francisco P. Barcelo, Caren Warzybok, Pete Bradley, Russel Jahncke, Jaime Goericke, Ralf Campbell, Gregory S. Hildebrand, John A. Melin, Sharon R. Delong, Robert L. Gomez-Valdes, Jose Lavaniegos, Bertha Gaxiola-Castro, Gilberto Golightly, Richard T. Schneider, Stephanie R. Lo, Nancy Suryan, Robert M. Gladics, Amanda J. Horton, Cheryl A. Fisher, Jennifer Morgan, Cheryl Peterson, Jay Daly, Elizabeth A. Auth, Toby D. Abell, Jeffrey TI STATE OF THE CALIFORNIA CURRENT 2012-13: NO SUCH THING AS AN "AVERAGE" YEAR SO CALIFORNIA COOPERATIVE OCEANIC FISHERIES INVESTIGATIONS REPORTS LA English DT Article ID CURRENT SYSTEM; OCEANOGRAPHIC CONDITIONS; PELAGIC TUNICATES; ENGRAULIS-MORDAX; NORTHERN ANCHOVY; FOOD-WEB; ABUNDANCE; JUVENILE; KRILL; FISH AB This report reviews the state of the California Current System (CCS) between winter 2012 and spring 2013, and includes observations from Washington State to Baja California. During 2012, large-scale climate modes indicated the CCS remained in a cool, productive phase present since 2007. The upwelling season was delayed north of 42 degrees N, but regions to the south, especially 33 degrees to 36 degrees N, experienced average to above average upwelling that persisted throughout the summer. Contrary to the indication of high production suggested by the climate indices, chlorophyll observed from surveys and remote sensing was below average along much of the coast. As well, some members of the forage assemblages along the coast experienced low abundances in 2012 surveys. Specifically, the concentrations of all life-stages observed directly or from egg densities of Pacific sardine, Sardinops sagax, and northern anchovy, Engraulis mordax, were less than previous years' survey estimates. However, 2013 surveys and observations indicate an increase in abundance of northern anchovy. During winter 2011/2012, the increased presence of northern copepod species off northern California was consistent with stronger southward transport. Krill and small-fraction zooplankton abundances, where examined, were generally above average. North of 42 degrees N, salps returned to typical abundances in 2012 after greater observed concentrations in 2010 and 2011. In contrast, salp abundance off central and southern California increased after a period of southward transport during winter 2011/2012. Reproductive success of piscivorous Brandt's cormorant, Phalacrocorax penicillatus, was reduced while planktivorous Cassin's auklet, Ptychoramphus aleuticus was elevated. Differences between the productivity of these two seabirds may be related to the available forage assemblage observed in the surveys. California sea lion pups from San Miguel Island were undernourished resulting in a pup mortality event perhaps in response to changes in forage availability. Limited biological data were available for spring 2013, but strong winter upwelling coastwide indicated an early spring transition, with the strong upwelling persisting into early summer. C1 [Wells, Brian K.; Schroeder, Isaac D.; Santora, Jarrod A.; Bjorkstedt, Eric P.; Harding, Jeff; Field, John; Sakuma, Keith; Hayes, Sean; Mantua, Nathan] Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Fisheries Ecol Div, Santa Cruz, CA 95060 USA. [Hazen, Elliott L.; Bograd, Steven J.] Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Div Environm Res, Pacific Grove, CA 93950 USA. [Bjorkstedt, Eric P.] Humboldt State Univ, Dept Fisheries Biol, Arcata, CA 95521 USA. [Loeb, Valerie J.] Moss Landing Marine Labs, Moss Landing, CA 95039 USA. [Mcclatchie, Sam; Weber, Edward D.; Watson, William; Thompson, Andrew R.; Lo, Nancy] Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Fisheries Res Div, La Jolla, CA 92037 USA. [Peterson, William T.; Brodeur, Richard D.] Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Hatfield Marine Sci Ctr, Newport, OR 97365 USA. [Sydeman, William J.; Losekoot, Marcel; Thompson, Sarah Ann] Farallon Inst Adv Ecosyst Res, Petaluma, CA 94952 USA. [Largier, John] Univ Calif Davis, Bodega Marine Lab, Bodega Bay, CA 94923 USA. [Kim, Sung Yong] Korea Adv Inst Sci & Technol, Div Ocean Syst Engn, Taejon 305701, South Korea. [Chavez, Francisco P.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. [Barcelo, Caren] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvalis, OR 97331 USA. [Warzybok, Pete; Bradley, Russel; Jahncke, Jaime] PRBO Conservat Sci, Petaluma, CA 94954 USA. [Goericke, Ralf; Campbell, Gregory S.; Hildebrand, John A.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Melin, Sharon R.; Delong, Robert L.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Natl Marine Mammal Lab, Seattle, WA 98115 USA. [Gomez-Valdes, Jose; Lavaniegos, Bertha; Gaxiola-Castro, Gilberto] CICESE, Div Oceanol, Ensenada 22860, Baja California, Mexico. [Golightly, Richard T.; Schneider, Stephanie R.] Humboldt State Univ, Dept ofWildlife, Arcata, CA 95521 USA. [Lo, Nancy] Ocean Associates Inc, La Jolla, CA 92037 USA. [Suryan, Robert M.; Gladics, Amanda J.; Horton, Cheryl A.] Oregon State Univ, Dept Fisheries & Wildlife, Hatfield Marine Sci Ctr, Newport, OR 97365 USA. [Fisher, Jennifer; Morgan, Cheryl; Peterson, Jay] Oregon State Univ, Cooperat Inst Marine Resources Studies, Hatfield Marine Sci Ctr, Newport, OR 97365 USA. [Auth, Toby D.] Hatfield Marine Sci Ctr, Pacific States Marine Fisheries Cormmiss, Newport, OR 97365 USA. [Abell, Jeffrey] Humboldt State Univ, Dept Oceanog, Arcata, CA 95521 USA. RP Schroeder, ID (reprint author), Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Fisheries Ecol Div, 110 Shaffer Rd, Santa Cruz, CA 95060 USA. RI Kim, Sung Yong/B-9852-2009; Gomez-Valdes, Jose/B-9846-2016; Weber, Edward/A-6986-2009 OI Kim, Sung Yong/0000-0003-1962-8992; Gomez-Valdes, Jose/0000-0002-8528-7826; Weber, Edward/0000-0002-0942-434X FU NOAA's California Current Integrated Ecosystem Assessment (CCIEA); Integrate Ocean Observing Systems (IOOS); National Marine Fisheries Service (NMFS); Stock Assessment Improvement Pan (SAIP); Fisheries and the Environment programs (FATE); Mexico's Consejo Nacional de Ciencia y Tecnologia (CONA-CyT); U.S. National Science Foundation (NSF),; Bonneville Power Administration (BPA); United States Fish and Wildlife Service (USFWS); Navy's Living Marine Resources Program; Coastal Observing Research and Development Center; California's Ocean Protection Council; Redwood National and State Parks; Baker Trust; Marisla Foundation; Campini Foundation; Kimball Foundation; Mead Foundation FX We thank three anonymous reviewers for their comments that improved this manuscript and provided guidance for continued development of reports in the series. Financial and collaborative support comes from diverse agenecies and government entities including NOAA's California Current Integrated Ecosystem Assessment (CCIEA), Integrate Ocean Observing Systems (IOOS), National Marine Fisheries Service (NMFS) and its Stock Assessment Improvement Pan (SAIP) and Fisheries and the Environment programs (FATE), Mexico's Consejo Nacional de Ciencia y Tecnologia (CONA-CyT), the U.S. National Science Foundation (NSF), Bonneville Power Administration (BPA), United States Fish and Wildlife Service (USFWS), Navy's Living Marine Resources Program and university partners through the Coastal Observing Research and Development Center, California's Ocean Protection Council, and Redwood National and State Parks. The David and Lucile Packard Foundation supported central California morring observations. The Baker Trust, the Marisla Foundation, the Campini Foundation, the Kimball Foundation, and the Mead Foundation supported seabird work on the Southeast Farallon Island. HF radar data are available thanks to the initial investment of the State of California in establishing the array in California and to the National Science Foundation for establishing elements of the array in Oregon and California; NOAA-IOOS and participating universities (listed at http://cordc.ucsd.edu/projects/mapping/) have provided ongoing operating funds and support. We also thank the captains and crew of the vessels that supported this work, including R/V Coral Sea, R/V Francisco de Ulloa, Elahka, FS/V Ocean Starr, R/V New Horizon, FS/V Bell M. Shimada, F/V Frosti, F/V Miss Sue, F/V Piky, R/V Elahka, and F/V Excalibur. We also sincerely thank the many dedicated individuals who have participated in, advised, collaborated in, or otherwise contributed to the collection, management, and analysis of these data both in recent years and in the past. NR 43 TC 12 Z9 12 U1 2 U2 25 PU SCRIPPS INST OCEANOGRAPHY PI LA JOLLA PA A-003, LA JOLLA, CA 92093 USA SN 0575-3317 J9 CAL COOP OCEAN FISH JI Calif. Coop. Ocean. Fish. Invest. Rep. PD DEC PY 2013 VL 54 BP 37 EP 71 PG 35 WC Fisheries SC Fisheries GA 259ER UT WOS:000327510700004 ER PT J AU Saha, J Wang, ML Cucinotta, FA AF Saha, Janapriya Wang, Minli Cucinotta, Francis A. TI Investigation of switch from ATM to ATR signaling at the sites of DNA damage induced by low and high LET radiation SO DNA REPAIR LA English DT Article DE DNA repair; ATM-to-ATR switch; Resection; End processing; High LET radiation; HZE particles ID DOUBLE-STRAND BREAKS; HOMOLOGOUS RECOMBINATION REPAIR; END RESECTION; MRE11-RAD50-NBS1 COMPLEX; CHECKPOINT; ACTIVATION; EXO1; PHOSPHORYLATION; SGS1; RECOGNITION AB Upon induction of DNA damage by ionizing radiation (IR), members of the phosphatidylinositol 3-kinase-like kinase family of proteins namely ataxia-telangiectasia mutated (ATM), DNA-PKcs, and ATM- and Rad3-related (ATR) maintain genomic integrity by mounting DNA damage response (DDR). Recent reports suggest that activation of ATM and ATR are oppositely regulated by the length of single stranded overhangs generated during end processing by nucleases at the break sites. These stretches of single stranded overhangs hold the clue for the transition from ATM to ATR signaling at broken DNA ends. We investigated whether differential processing of breaks induced by low and high LET radiation augments the phenomenon of switching from ATM to ATR kinase and hence a concomitant NHEJ to HR transition at the sites of DNA damage. 82-6 human fibroblasts were irradiated with 1 or 2 Gy of gamma-rays and particle radiation of increasing LET in order to increase the complexity and variability of DNA double strand breaks (DSB) structures. The activation kinetics of ATM and ATR kinases along with their downstream substrates were determined utilizing Western blotting and immunofluorescence techniques. Our data provide evidence of a potential switch from ATM to ATR kinase signaling in cells treated with gamma-rays at approximately 2 h post irradiation, with induction and completion of resection denoted by Rad51 foci resolution kinetics and observed with a significant decline of phosphorylated ATR kinase 8 h after IR. On the other hand, irradiation with high LET 600 MeV/u Fe-56 (180 keV/mu m) and 170 MeV/u Si-28 (99 keV/mu m) particles show a similar Rad51 foci decay kinetics, however, exhibiting prolonged resection, evident by the persistent phosphorylated ATM and ATR kinase until 24 h post irradiation. This residual effect, however, was significantly reduced for 250 MeV/u O-16 particles of moderate LET (25 keV/mu m) and absent for gamma-rays. Hence, our results support the hypothesis that the transition from ATM to ATR signaling at DNA break sites is extended for longer periods of time, indicated by sustained resection due to the complex type of damage induced, a hallmark of high LET radiation, which may contribute to its increased biological effectiveness. (C) 2013 Elsevier B.V. All rights reserved. C1 [Saha, Janapriya; Wang, Minli] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA. [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Cucinotta, Francis A.] Univ Nevada, Dept Hlth Phys & Diagnost Sci, Las Vegas, NV 89154 USA. RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. EM francis.cucinotta@unlv.edu FU DoE Low Dose Program [DE-AI02-10ER64969]; University of Nevada Las Vegas FX This work was supported by DoE Low Dose Program (grant number DE-AI02-10ER64969), and the University of Nevada Las Vegas. NR 43 TC 10 Z9 10 U1 0 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1568-7864 EI 1568-7856 J9 DNA REPAIR JI DNA Repair PD DEC PY 2013 VL 12 IS 12 BP 1143 EP 1151 DI 10.1016/j.dnarep.2013.10.004 PG 9 WC Genetics & Heredity; Toxicology SC Genetics & Heredity; Toxicology GA 274GO UT WOS:000328595000016 PM 24238855 ER PT J AU Reiss, D Zimmerman, MI Lewellen, DC AF Reiss, Dennis Zimmerman, Michael I. Lewellen, David C. TI Formation of cycloidal dust devil tracks by redeposition of coarse sands in southern Peru: Implications for Mars SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Earth, Mars, dust devil; dust devil tracks; geomorphology; soil; surface; atmosphere ID RESOLUTION STEREO CAMERA; ORBITER CAMERA; SURFACE; INTENSIFICATION; DESERT; DIRECTIONS; VORTICES; MOTION AB Aeolian processes are the most active processes modifying the surface of Mars under present day climatic conditions. Besides wind streak changes and dune and ripple migrations, active dust devils occur frequently leaving numerous tracks on the Martian surface. These dust devil tracks (DDTs) are characterized by albedo changes with respect to their surroundings and are suggested to be caused by erosion of dust exposing coarser grained material. Here we show that DDTs with a cycloidal pattern analyzed in situ in southern Peru are formed by erosion of very coarse sands at the outer margins and its subsequent annular deposition in the central parts of dust devils. Field observations are supported by large-eddy simulations using typical dust devil parameters resembling the cycloidal morphology of the DDTs. Cycloidal DDTs observed on Mars resembling the Peruvian DDTs suggest an equivalent formation mechanism. Our results imply that the formation of DDTs on Mars are not solely due to dust erosion but also depositional processes and dust devils are strong enough to redistribute coarser grained material such as sands; hence they might contribute to the modification of the present day Martian landscape. (C) 2013 Elsevier B.V. All rights reserved. C1 [Reiss, Dennis] Univ Munster, Inst Planetol, D-48149 Munster, Germany. [Zimmerman, Michael I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zimmerman, Michael I.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Lewellen, David C.] W Virginia Univ, Morgantown, WV 26506 USA. RP Reiss, D (reprint author), Univ Munster, Inst Planetol, Wilhelm Klemm Str 10, D-48149 Munster, Germany. RI Reiss, Dennis/B-6211-2008; OI Reiss, Dennis/0000-0002-1836-596X FU National Science Foundation [AGS-1013154] FX D.R. thanks Roberto Penny Cabrera for his great planning and realization to stay several days in study area 1 and Nicholas Cabrera for very helpful assistance and discussions in the field. M.Z. thanks Dr. Timothy Stubbs and Dr. Timothy McClanahan at NASA Goddard Space Flight Center for generously providing computing resources for a subset of the large-eddy simulations. We thank two anonymous reviewers for their constructive and helpful reviews. We also thank Daniela Heeren at Westfalische Wilhelms-Universitat Munster for her artistic realization of the schematic sketch. D.L. is supported in part by the National Science Foundation, under Grant AGS-1013154. NR 43 TC 9 Z9 9 U1 1 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD DEC 1 PY 2013 VL 383 BP 7 EP 15 DI 10.1016/j.epsl.2013.09.033 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 274FZ UT WOS:000328593500002 ER PT J AU Vayner, BV Ferguson, DC Hoffmann, RC Wheelock, AT Likar, JJ Prebola, JL Crider, DH Schneider, TA Vaughn, JA Hoang, B Steele, K Close, S Goel, A Crofton, MW Young, JA Bodeau, JM AF Vayner, Boris V. Ferguson, Dale C. Hoffmann, Ryan C. Wheelock, Adrian T. Likar, Justin J. Prebola, John L., Jr. Crider, Dustin H. Schneider, Todd A. Vaughn, Jason A. Hoang, Bao Steele, Kenneth Close, Sigrid Goel, Ashish Crofton, Mark W. Young, Jason A. Bodeau, J. Michael TI First Preliminary Results from US Round-Robin Tests SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Article DE Plasma expansion; spacecraft arcing ID SPACECRAFT DIELECTRICS; PROPAGATION; ENVIRONMENT AB The first preliminary results are reported from the U.S. Round-Robin Test on Plasma Expansion Speed. The tests were performed at the NASA Glenn Research Center on two coupons (six strings) of International Space Station (ISS) solar cell arrays, with a separate small array to obtain arcs (because it is so difficult to get ISS arrays to arc). ISS arrays were used because they have no exposed interconnects to act as bare current collectors and confuse the experimental results. The preconstructed ISS strings were laid out approximately parallel to the plasma expansion velocity to allow for the best test of the simple plasma expansion front current waveform model. Several Langmuir probes were arranged above and to the sides of the sample to allow for measurement of the plasma propagation speed. In the initial set of tests, primary arcs and the consequent current waveforms were measured in a Low Earth Orbit-type plasma. In a second set of tests, two electron guns with diffusers were used to provide an approximately uniform Geosynchronous Earth Orbit-type environment, and primary arcs and current waveforms were obtained. The objective of this and other round-robin tests is to characterize primary arc waveforms in terms of speed and degree of discharge of arc plasmas produced by primary arcs, and their dependences on environment, capacitance per unit area, arc voltage, temperature, and so on. The final goal is to allow engineering estimates of arc current peaks and half-widths to allow confident design and construction of space solar arrays, and to allow mitigation techniques to be evaluated. This is the first in an extended series of tests to be performed at six different U.S. facilities, and with participation from ten different U.S. organizations. C1 [Vayner, Boris V.] Ohio Aerosp Inst, Brookpark, OH 44142 USA. [Ferguson, Dale C.; Hoffmann, Ryan C.; Wheelock, Adrian T.] AFRL, Albuquerque, NM 87117 USA. [Likar, Justin J.] Lockheed Martin Space Syst Co, Newtown, PA 18940 USA. [Prebola, John L., Jr.; Crider, Dustin H.] AF AEDC, Tullahoma, TN 37389 USA. [Schneider, Todd A.; Vaughn, Jason A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Hoang, Bao] Space Syst Loral, Palo Alto, CA 94303 USA. [Steele, Kenneth] ATK, Goleta, CA 93117 USA. [Close, Sigrid; Goel, Ashish] Stanford Univ, Palo Alto, CA 94305 USA. [Crofton, Mark W.; Young, Jason A.] Aerosp Corp, Los Angeles, CA 90009 USA. [Bodeau, J. Michael] Northrop Grumman, Sunnyvale, CA 90278 USA. RP Vayner, BV (reprint author), Ohio Aerosp Inst, Brookpark, OH 44142 USA. EM boris.v.vayner@nasa.gov; dale.ferguson@kirtland.af.mil; ryan.hoffmann@kirtland.af.mil; adrian.wheelock@kirtland.af.mil; justin.j.likar@lmco.com; john.prebola@arnold.af.mil; Dustin.Crider@arnold.af.mil; Todd.A.Schneider@nasa.gov; jason.a.vaughn@nasa.gov; hoangb@ssd.loral.com; kenneth.steele@atk.com; sigrid.close@stanford.edu; ashish.goel@stanford.edu; Mark.w.crofton@aero.org; jason.a.young@aero.org; michael.bodeau@ngc.com FU U.S. Air Force Research Laboratory, Space Vehicles Directorate FX This work was supported in part by the U.S. Air Force Research Laboratory, Space Vehicles Directorate. NR 12 TC 5 Z9 5 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 EI 1939-9375 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD DEC PY 2013 VL 41 IS 12 SI SI BP 3310 EP 3322 DI 10.1109/TPS.2013.2262639 PN 2 PG 13 WC Physics, Fluids & Plasmas SC Physics GA 275UO UT WOS:000328703500003 ER PT J AU Wong, FK Gardiner, G Hoang, B Redick, T Gahart, RL Wright, KH Vaughn, JA Schneider, TA AF Wong, Frankie K. Gardiner, George Hoang, Bao Redick, Tod Gahart, Richard L. Wright, Kenneth H. Vaughn, Jason A. Schneider, Todd A. TI Electrostatic Discharge Tests on Solar Array Wire Coupons Subjected to Simulated Space Environment Aging SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Article DE Electrostatic discharge (ESD); environmental life test; solar array; spacecraft charging; wire AB Solar array wire coupons have successfully completed an environmental life test that simulates 15 years at geosynchronous orbit. The environments included: ultraviolet (UV), electron, and proton irradiation; thermal cycling; electrostatic discharge (ESD); and ion thruster plume exposure on an electrostatically charged coupon. The test articles consisted of two wire coupons: one simulated the sun-facing side and the other simulated the shade side. UV irradiation was performed only on the sun-facing side coupon. Tests were performed at beginning-of-life, 7.5 years, and end-of-life. At each age point, ESD tests were performed using an electron beam at a worst case geosynchronous space environment flux of 1 nA/cm(2). The test setup included capacitance that simulated a whole panel array harness, and a solar array simulator that generated in-flight array current profiles. The test coupon configuration contained aspects of the full panel wiring topology, which included potential fault conditions on wires. Visual inspections, documented with photographs, and isolation resistance tests were performed after each environment exposure to ensure the integrity of the wire insulation. This paper/presentation discusses each environment test level, test condition, and results from the various environmental age points. C1 [Wong, Frankie K.; Gardiner, George; Hoang, Bao; Redick, Tod; Gahart, Richard L.] Space Syst Loral, Palo Alto, CA 94303 USA. [Wright, Kenneth H.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Vaughn, Jason A.; Schneider, Todd A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Wong, FK (reprint author), Space Syst Loral, Palo Alto, CA 94303 USA. EM wongf@ssd.loral.com; gardinerg@ssd.loral.com; hoang.bao@ssd.loral.com; redickt@ssd.loral.com; gahartr@ssd.loral.com; ken.wright@uah.edu; jason.a.vaughn@nasa.gov; todd.schneider@nasa.gov NR 5 TC 3 Z9 3 U1 1 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 EI 1939-9375 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD DEC PY 2013 VL 41 IS 12 SI SI BP 3359 EP 3369 DI 10.1109/TPS.2013.2277723 PN 2 PG 11 WC Physics, Fluids & Plasmas SC Physics GA 275UO UT WOS:000328703500008 ER PT J AU Ferguson, DC Cooke, D Pfaff, R Rowland, D Klenzing, J Freudenreich, H AF Ferguson, Dale C. Cooke, David Pfaff, Robert Rowland, Douglas Klenzing, Jeffrey Freudenreich, Henry TI Ram/Wake and Surface Layer Effects on DC Electric Field Measurements in LEO SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Article DE DC electric field measurements; spacecraft charging ID PLASMAS; PROBES; WAKE AB The USAF Communication/Navigation Outage Forecast System satellite, launched into an eccentric low earth orbit (401 km perigee by 867 km apogee) of 13 degrees inclination on April 16, 2008, has a set of dc electric field probes that constitute part of the Vector Electric Field Investigation (VEFI). In order to obtain the ambient electric field, the v x B component of electric field must be subtracted from the VEFI measurements. After this subtraction and the subtraction of the ambient dc electric components, a residual dc offset directed toward the spacecraft wake is still observed, which varies somewhat within an orbit and on longer timescales. One of the interesting features of these offsets is that when the satellite is occasionally rotated, the offsets are reset to their baseline values, only to come back within a month or so. Various hypotheses have been proposed to explain the residual dc offsets. In this paper, we explore the possibilities that either the influence of the spacecraft wake on the sensors or that modified surface layers on the probe surfaces are producing the offsets. Nascap-2k and EWB models are used to show the various influences of the wake and of surface materials. Finally, a hypothesis is produced that quantitatively explains many of the salient features of the offsets. The feasibility of using dc electric field probes in space is reaffirmed. Recommendations for probe construction on future spacecraft to ameliorate spurious effects are presented. C1 [Ferguson, Dale C.; Cooke, David] Air Force Res Lab, Space Vehicles Directorate, Albuquerque, NM 87117 USA. [Pfaff, Robert; Rowland, Douglas; Klenzing, Jeffrey; Freudenreich, Henry] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ferguson, DC (reprint author), Air Force Res Lab, Space Vehicles Directorate, Albuquerque, NM 87117 USA. EM dale.ferguson@kirtland.af.mil; david.cooke@kirtland.af.mil; robert.f.pfaff@nasa.gov; douglas.f.rowland@nasa.gov; jeffrey.klenzing@nasa.gov; henry.f.freudenreich@nasa.gov RI Rowland, Douglas/F-5589-2012; Klenzing, Jeff/E-2406-2011 OI Rowland, Douglas/0000-0003-0948-6257; Klenzing, Jeff/0000-0001-8321-6074 NR 30 TC 0 Z9 0 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 EI 1939-9375 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD DEC PY 2013 VL 41 IS 12 SI SI BP 3459 EP 3470 DI 10.1109/TPS.2013.2278615 PN 2 PG 12 WC Physics, Fluids & Plasmas SC Physics GA 275UO UT WOS:000328703500021 ER PT J AU Garrett, HB Close, S AF Garrett, Henry B. Close, Sigrid TI Impact-Induced ESD and EMI/EMP Effects on Spacecraft-A Review SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Article DE Debris impacts; electromagnetic pulses; electrostatic discharges (ESDs); micrometeoroid impacts; spacecraft charging ID PLASMA-WAVE INSTRUMENT; HYPERVELOCITY IMPACTS; METEOROIDS; STREAMS; SATURN; DEBRIS; EMISSIONS; RADIO; VAPOR AB Recent studies have indicated that the effects of meteoroid and debris impacts on spacecraft are not being adequately considered in spacecraft design. They imply that electrical effects, including both charging and plasma production, caused by meteoroid and debris impacts have not been sufficiently addressed. To address these concerns, this paper will present the current evidence for impact-induced electrical anomalies and the characteristics of the impact-generated plasma and electromagnetic environments associated with hypervelocity particle impacts. This paper will be limited to describing the effects of hypervelocity impacts of particles fast enough to generate a plasma or impulse sufficient to affect spacecraft systems but sufficiently small that the classic mechanical damage to the system is of limited concern. Because this failure mechanism scales highly with velocity, we consider effects from particles as small at 10-15 grams, which are far more numerous and therefore more likely to impact spacecraft. Mitigation methods will be presented that are aimed at limiting the effects of the resulting plasmas and their electrostatic discharge and electromagnetic interference/pulse effects rather than at the typical structural or mechanical failures expected from such impacts. The ultimate intent of this paper is to focus on the description and mitigation of this relatively ignored form of in-space charging and motivate further experimental studies of this interesting and rich phenomenon. C1 [Garrett, Henry B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Close, Sigrid] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA. RP Garrett, HB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM henry.b.garrett@jpl.nasa.gov; sigridc@stanford.edu FU Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration FX This work was supported by the Jet Propulsion Laboratory, California Institute of Technology, under Contract with the National Aeronautics and Space Administration. NR 62 TC 5 Z9 5 U1 1 U2 14 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 EI 1939-9375 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD DEC PY 2013 VL 41 IS 12 SI SI BP 3545 EP 3557 DI 10.1109/TPS.2013.2286181 PN 2 PG 13 WC Physics, Fluids & Plasmas SC Physics GA 275UO UT WOS:000328703500032 ER PT J AU Hristova-Veleva, SM Callahan, PS Dunbar, RS Stiles, BW Yueh, SH Huddleston, JN Hsiao, SV Neumann, G Vanhoff, BA Gaston, RW Rodriguez, E Weissman, DE AF Hristova-Veleva, S. M. Callahan, P. S. Dunbar, R. S. Stiles, B. W. Yueh, S. H. Huddleston, J. N. Hsiao, S. V. Neumann, G. Vanhoff, B. A. Gaston, R. W. Rodriguez, E. Weissman, D. E. TI Revealing the Winds under the Rain. Part I: Passive Microwave Rain Retrievals Using a New Observation-Based Parameterization of Subsatellite Rain Variability and Intensity-Algorithm Description SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article DE Precipitation; Radiative transfer; Algorithms; Microwave observations; Remote sensing; Satellite observations ID VERTICAL HYDROMETEOR PROFILES; CLOUD MODEL MICROPHYSICS; SATELLITE MEASUREMENTS; RADIATIVE-TRANSFER; PRECIPITATION RETRIEVAL; PHYSICAL RETRIEVALS; SPACE; FREQUENCIES; SENSORS; IMAGER AB Scatterometer ocean surface winds have been providing very valuable information to researchers and operational weather forecasters for over 10 years. However, the scatterometer wind retrievals are compromised when rain is present. Merely flagging all rain-affected areas removes the most dynamic and interesting areas from the wind analysis. Fortunately, the Advanced Earth Observing Satellite II (ADEOS-II) mission carried a radiometer [the Advanced Microwave Scanning Radiometer (AMSR)] and a scatterometer, allowing for independent, collocated retrievals of rain. The authors developed an algorithm that uses AMSR observations to estimate the rain inside the scatterometer beam. This is the first in a series of papers that describe their approach to providing rain estimation and correction to scatterometer observations. This paper describes the retrieval algorithm and evaluates it using simulated data. Part II will present its validation when applied to AMSR observations. This passive microwave rain retrieval algorithm addresses the issues of nonuniform beam filling and hydrometeor uncertainty in a novel way by 1) using a large number of soundings to develop the retrieval database, thus accounting for the geographically varying atmospheric parameters; 2) addressing the spatial inhomogeneity of rain by developing multiple retrieval databases with different built-in inhomogeneity and rain intensity, along with a rain indicator to select the most appropriate database for each observed scene; 3) developing a new cloud-versus-rain partitioning that allows the use of a variety of drop size distribution assumptions to account for some of the natural variability diagnosed from the soundings; and 4) retrieving atmospheric and surface parameters just outside the rainy areas, thus providing information about the environment to help decrease the uncertainty of the rain estimates. C1 [Hristova-Veleva, S. M.; Callahan, P. S.; Dunbar, R. S.; Stiles, B. W.; Yueh, S. H.; Huddleston, J. N.; Hsiao, S. V.; Neumann, G.; Gaston, R. W.; Rodriguez, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vanhoff, B. A.] Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Weissman, D. E.] Hofstra Univ, Hempstead, NY 11550 USA. RP Hristova-Veleva, SM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM svetla.veleva@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank Dr. Ziad Haddad, of JPL, for the numerous discussions during the algorithm development and for his greatly appreciated help in modifying the paper to enhance the clarity. We also thank three anonymous reviewers whose comments and insightful suggestions greatly helped in improving this paper. NR 45 TC 4 Z9 4 U1 0 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD DEC PY 2013 VL 52 IS 12 BP 2828 EP 2848 DI 10.1175/JAMC-D-12-0237.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 270WG UT WOS:000328349300014 ER PT J AU Uprety, S Cao, CY Xiong, XX Blonski, S Wu, AS Shao, X AF Uprety, Sirish Cao, Changyong Xiong, Xiaoxiong Blonski, Slawomir Wu, Aisheng Shao, Xi TI Radiometric Intercomparison between Suomi-NPP VIIRS and Aqua MODIS Reflective Solar Bands Using Simultaneous Nadir Overpass in the Low Latitudes SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Remote sensing; Satellite observations ID NEAR-INFRARED CHANNELS; IMAGING SPECTROMETER; SNOW ALBEDO; CALIBRATION; AVHRR; DEGRADATION; PERFORMANCE; SATELLITES AB On-orbit radiometric performance of the Suomi National Polar-Orbiting Partnership (Suomi-NPP) Visible Infrared Imaging Radiometer Suite (VIIRS) is studied using the extended simultaneous nadir overpass (SNO-x) approach. Unlike the traditional SNO analysis of data in the high latitudes, this study extends the analysis to the low latitudesin particular, over desert and ocean sites with relatively stable and homogeneous radiometric propertiesfor intersatellite comparisons. This approach utilizes a pixel-by-pixel match with an efficient geospatial matching algorithm to map VIIRS data into the Moderate Resolution Imaging Spectroradiometer (MODIS). VIIRS moderate-resolution bands M-1 through M-8 are compared with Aqua MODIS equivalent bands to quantify radiometric bias over the North African desert and over the ocean. Biases exist between VIIRS and MODIS in several bands, primarily because of spectral differences as well as possible calibration uncertainties, residual cloud contamination, and bidirectional reflectance distribution function (BRDF). The impact of spectral differences on bias is quantified by using the Moderate Resolution Atmospheric Transmission (MODTRAN) and hyperspectral measurements from the Earth Observing-1 (EO-1) Hyperion and the Airborne Visible and Infrared Imaging Spectrometer (AVIRIS). After accounting for spectral differences and bias uncertainties, the VIIRS radiometric bias over desert agrees with MODIS measurements within 2% except for the VIIRS shortwave infrared (SWIR) band M-8, which indicates a nearly 3% bias. Over ocean, VIIRS agrees with MODIS within 2% by the end of January 2013 with uncertainty less than 1%. Furthermore, VIIRS bias relative to MODIS is also computed at the Antarctica Dome C site for validation and the result agrees well within 1% with the bias estimated using SNO-x over desert. C1 [Uprety, Sirish] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. [Cao, Changyong] NOAA, Ctr Satellite Applicat & Res, NESDIS, College Pk, MD USA. [Xiong, Xiaoxiong] NASA, Sci & Explorat Directorate, GSFC, Greenbelt, MD USA. [Blonski, Slawomir; Shao, Xi] Univ Maryland, College Pk, MD 20742 USA. [Wu, Aisheng] Sigma Space Corp, Lanham, MD USA. RP Uprety, S (reprint author), Colorado State Univ, Cooperat Inst Res Atmosphere, 1375 Campus Delivery, Ft Collins, CO 80523 USA. EM sirish.uprety@noaa.gov RI Cao, Changyong/F-5578-2010; Shao, Xi/H-9452-2016 FU JPSS program office FX The authors thank the VIIRS SDR team members for their dedicated support in calibration/validation of VIIRS SDR data. The authors thank Ms. Yan Bai for her support in data collection and editorial work. This work is partially funded by the JPSS program office. The manuscript contents are solely the opinions of the authors and do not constitute a statement of policy, decision, or position on behalf of NOAA or the U.S. government. NR 30 TC 20 Z9 20 U1 0 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD DEC PY 2013 VL 30 IS 12 BP 2720 EP 2736 DI 10.1175/JTECH-D-13-00071.1 PG 17 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 275IK UT WOS:000328669300004 ER PT J AU Battaglia, A Tanelli, S Kollias, P AF Battaglia, Alessandro Tanelli, Simone Kollias, Pavlos TI Polarization Diversity for Millimeter Spaceborne Doppler Radars: An Answer for Observing Deep Convection? SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Convective clouds; Supercells; Radars; Radar observations; Remote sensing; Satellite observations ID VERTICAL RAINFALL VELOCITY; CLOUD-PROFILING RADAR; SCATTERING; PRECIPITATION; SIMULATIONS; ATTENUATION; PERFORMANCE; ALGORITHM; RADIATION; PROPOSAL AB Spaceborne Doppler radars have the potential to provide key missing observations of convective vertical air motions especially over the tropical oceans. Such measurements can improve understanding of the role of tropical convection in vertical energy transport and its interaction with the environment. Several millimeter wavelength Doppler radar concepts have been proposed since the 1990s. The Earth Clouds, Aerosols, and Radiation Explorer (EarthCARE) Cloud Profiling Radar (CPR) will be the first Dopplerized atmospheric radar in space but has not been optimized for Doppler measurements in deep convective clouds.The key challenge that constrains the CPR performance in convective clouds is the range-Doppler dilemma. Polarization diversity (PD) offers a solution to this constraint by decoupling the coherency (Doppler) requirement from the unambiguous range requirement. Careful modeling of the radar signal depolarization and its impact on radar receiver channel cross talk is needed to accurately assess the performance of the PD approach.The end-to-end simulator presented in this work allows reproduction of the signal sensed by a Doppler radar equipped with polarization diversity when overpassing realistic three-dimensional convective cells, with all relevant cross-talk sources accounted for. The notional study highlights that multiple scattering is the primary source of cross talk, highly detrimental for millimeter Doppler velocity accuracy. The ambitious scientific requirement of 1 m s(-1) accuracy at 500-m integration for reflectivities above -15 dBZ are within reach for a W-band radar with a 2.5-m antenna with optimal values of the pulse-pair interval between 20 and 30 s but only once multiple scattering and ghost-contaminated regions are screened out. The identification of such areas is key for Doppler accuracies and can be achieved by employing an interlaced pulse-pair mode that measures the cross and the copolar reflectivities. To mitigate the impact of attenuation and multiple scattering, the Ka band has been considered as either alternative or additional to the W band. However, a Ka system produces worse Doppler performances than a W-band system with the same 2.5-m antenna size. Furthermore, in deep convection it results in similar levels of multiple scattering and therefore it does not increase significantly the depth of penetration. In addition, the larger footprint causes stronger nonuniform beam-filling effects. One advantage of the Ka-band option is the larger Nyquist velocity that tends to reduce the Doppler accuracies. More significant benefits are derived from the Ka band when observing precipitation not as intense as the deep convection is considered here.This study demonstrates that polarization diversity indeed represents a very promising methodology capable of significantly reducing aliasing and Doppler moment estimate errors, two main error sources for Doppler velocity estimates in deep convective systems and a key step to achieving typical mission requirements for convection-oriented millimeter radar-based spaceborne missions. C1 [Battaglia, Alessandro] Univ Leicester, Leicester LE1 7RH, Leics, England. [Tanelli, Simone] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Kollias, Pavlos] McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ, Canada. RP Battaglia, A (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM ab474@le.ac.uk OI Battaglia, Alessandro/0000-0001-9243-3484 FU European Space Agency under the WISDR [ITT AO/1-6661/11/NL/LvH]; CEOI under the POLYDOROS (POLARIZATION Diversity Doppler Radar on Satellite) project FX The portion of work carried out by Battaglia and Kollias was supported by the European Space Agency under the WISDR (capability of atmospheric parameter retrieval and modeling for Wide-Swath Spaceborne Doppler Radars) activity (ITT AO/1-6661/11/NL/LvH) and by CEOI under the POLYDOROS (POLARIZATION Diversity Doppler Radar on Satellite) project. A portion of this work (Tanelli) was carried out in support to the ACE mission concept and to cloud and precipitation science at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 48 TC 8 Z9 8 U1 2 U2 11 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD DEC PY 2013 VL 30 IS 12 BP 2768 EP 2787 DI 10.1175/JTECH-D-13-00085.1 PG 20 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 275IK UT WOS:000328669300007 ER PT J AU Lolli, S Welton, EJ Campbell, JR AF Lolli, Simone Welton, Ellsworth J. Campbell, James R. TI Evaluating Light Rain Drop Size Estimates from Multiwavelength Micropulse Lidar Network Profiling SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article DE Boundary layer; Drizzle; Aerosols; Cumulus clouds; Lidars; Lidar observations; Remote sensing ID DOPPLER RADAR; DRIZZLE PARAMETERS; MELTING LAYER; CLOUD; AEROSOLS AB This paper investigates multiwavelength retrievals of median equivolumetric drop diameter D-0 suitable for drizzle and light rain, through collocated 355-/527-nm Micropulse Lidar Network (MPLNET) observations collected during precipitation occurring 9 May 2012 at the Goddard Space Flight Center (GSFC) project site. By applying a previously developed retrieval technique for infrared bands, the method exploits the differential backscatter by liquid water at 355 and 527 nm for water drops larger than approximate to 50 m. In the absence of molecular and aerosol scattering and neglecting any transmission losses, the ratio of the backscattering profiles at the two wavelengths (355 and 527 nm), measured from light rain below the cloud melting layer, can be described as a color ratio, which is directly related to D-0. The uncertainty associated with this method is related to the unknown shape of the drop size spectrum and to the measurement error. Molecular and aerosol scattering contributions and relative transmission losses due to the various atmospheric constituents should be evaluated to derive D-0 from the observed color ratio profiles. This process is responsible for increasing the uncertainty in the retrieval. Multiple scattering, especially for UV lidar, is another source of error, but it exhibits lower overall uncertainty with respect to other identified error sources. It is found that the total error upper limit on D-0 approaches 50%. The impact of this retrieval for long-term MPLNET monitoring and its global data archive is discussed. C1 [Lolli, Simone] NASA, Joint Ctr Earth Syst Technol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lolli, Simone; Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Campbell, James R.] Naval Res Lab, Monterey, CA USA. RP Lolli, S (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 612, Greenbelt, MD 20771 USA. EM simone.lolli@nasa.gov RI Campbell, James/C-4884-2012 OI Campbell, James/0000-0003-0251-4550 FU NASA [NNG12HG05I] FX The Micropulse Lidar Network is coordinated through the support of the NASA Radiation Sciences Program. The authors gratefully acknowledge the University of Wyoming's Department of Atmospheric Sciences for access to its radiosonde visualization tools. Author JRC acknowledges the support of NASA Interagency Agreement NNG12HG05I on behalf of the Micropulse Lidar Network. NR 32 TC 12 Z9 12 U1 1 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD DEC PY 2013 VL 30 IS 12 BP 2798 EP 2807 DI 10.1175/JTECH-D-13-00062.1 PG 10 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA 275IK UT WOS:000328669300009 ER PT J AU Nettles, AT Jackson, JR AF Nettles, Alan T. Jackson, Justin R. TI Compression after impact strength of out-of-autoclave processed laminates SO JOURNAL OF REINFORCED PLASTICS AND COMPOSITES LA English DT Article DE Out-of-autoclave; compression-after-impact; damage tolerance AB Out-of-autoclave processable fiber/resin systems have been gaining much attention due to the elimination of needing a costly autoclave large enough to hold the part to be cured. For large composite structures this can pose a challenge. However, for these fiber/resin systems to replace conventional autoclave fiber/resin systems for use on aerospace structures, the damage tolerance capabilities need to meet (or exceed) those of current autoclave fiber/resin systems. In this experimental study, compression-after-impact strengths of two commercially available out-of-autoclave fiber/resin systems are compared to compression-after-impact strengths of a conventional autoclave fiber/resin system used as a baseline in this study. compression-after-impact testing was chosen since this is the most common method to assess laminates damage tolerance capabilities. Three different levels of impact severity were chosen and information on damage size and morphology are assessed along with compression-after-impact strength values. The results show the two out-of-autoclave fiber/resin systems examined in this study have similar damage tolerance characteristics to the autoclave fiber/resin system used in this study. C1 [Nettles, Alan T.; Jackson, Justin R.] NASA MSFC, Huntsville, AL 35812 USA. RP Nettles, AT (reprint author), NASA MSFC, 4601 Martin Rd, Huntsville, AL 35812 USA. EM alan.t.nettles@nasa.gov FU National Aeronautics and Space Administration under the Upper Stage Program Office at Marshall Space Flight Center [136905.08.05.12] FX This work was funded by the National Aeronautics and Space Administration under the auspices of the Upper Stage Program Office at Marshall Space Flight Center (136905.08.05.12). NR 7 TC 3 Z9 4 U1 1 U2 2 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0731-6844 EI 1530-7964 J9 J REINF PLAST COMP JI J. Reinf. Plast. Compos. PD DEC PY 2013 VL 32 IS 24 BP 1887 EP 1894 DI 10.1177/0731684413495097 PG 8 WC Materials Science, Composites; Polymer Science SC Materials Science; Polymer Science GA 274IE UT WOS:000328599200002 ER PT J AU Durden, SL AF Durden, Stephen L. TI Observed Tropical Cyclone Eye Thermal Anomaly Profiles Extending above 300 hPa SO MONTHLY WEATHER REVIEW LA English DT Article DE Hurricanes; typhoons; Tropical cyclones; Dropsondes; Radiosonde observations ID EQUIVALENT POTENTIAL TEMPERATURE; HURRICANE BONNIE 1998; STORM HUMBERTO 2001; INNER-CORE; WARM-CORE; RADAR OBSERVATIONS; PART I; SIMULATION; EYEWALL; THERMODYNAMICS AB As recently pointed out by Stern and Nolan, much of our knowledge of the warm core structure of the tropical cyclone eye has come from composites of in situ data taken from multiple aircraft studies of three storms in the late 1950s and 1960s. Further observational confirmation of eye thermal structure has been lacking, since much of the dropsonde data analyzed to date have been limited to pressure levels of 500 hPa or lower. However, there exist a number of dropsonde eye profiles extending to near 250 hPa; these profiles were acquired from NASA aircraft during various field campaigns. Here, the author uses these data to calculate eye temperature anomaly profiles. These data are supplemented by several surface-based radiosonde releases in tropical cyclone eyes over the period 1944-2003. The author finds that the pressure altitude of the maximum anomaly varies between 760 and 250 hPa. The author also finds positive correlations between the maximum anomaly level and storm intensity, size, upper-level divergence, and environmental instability. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Durden, SL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sdurden@jpl.nasa.gov FU National Science Foundation; NASA [NNH09ZDA001N-HSRP] FX The author would like to thank Dr. Daniel Stern for reviewing and providing very helpful comments on an early version of this manuscript. The author is also grateful to Dr. Jonathan Vigh and two anonymous reviewers for their detailed and extensive comments and questions on the submitted manuscript; their suggestions led to significant improvements in the quality of the paper. The author thanks the University of Wyoming for making its sounding archive publicly available and NOAA/RAMMB for making the SHIPS development data available. Dropsonde data processing was provided by NCAR/EOL under sponsorship of the National Science Foundation. The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding from Dr. Ramesh Kakar at NASA headquarters under NASA Research Announcement NNH09ZDA001N-HSRP is gratefully acknowledged. NR 60 TC 7 Z9 7 U1 1 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 EI 1520-0493 J9 MON WEATHER REV JI Mon. Weather Rev. PD DEC PY 2013 VL 141 IS 12 BP 4256 EP 4268 DI 10.1175/MWR-D-13-00021.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 256AY UT WOS:000327283300005 ER PT J AU Braun, SA Sippel, JA Shie, CL Boller, RA AF Braun, Scott A. Sippel, Jason A. Shie, Chung-Lin Boller, Ryan A. TI The Evolution and Role of the Saharan Air Layer during Hurricane Helene (2006) SO MONTHLY WEATHER REVIEW LA English DT Article DE Dry intrusions; Hurricanes; Dust or dust storms; Subsidence; Satellite observations ID TROPICAL CYCLOGENETIC PROCESSES; GLOBAL DATA ASSIMILATION; PREDICTION SCHEME SHIPS; AFRICAN EASTERLY WAVES; VERTICAL WIND SHEAR; FORECAST SYSTEM; SOP-3 NAMMA; NUMERICAL SIMULATIONS; BOUNDARY-LAYER; PART II AB The Saharan air layer (SAL) has received considerable attention in recent years as a potential negative influence on the formation and development of Atlantic tropical cyclones. Observations of substantial Saharan dust in the near environment of Hurricane Helene (2006) during the National Aeronautics and Space Administration (NASA) African Monsoon Multidisciplinary Activities (AMMA) Experiment (NAMMA) field campaign led to suggestions about the suppressing influence of the SAL in this case. In this study, a suite of satellite remote sensing data, global meteorological analyses, and airborne data are used to characterize the evolution of the SAL in the environment of Helene and assess its possible impact on the intensity of the storm. The influence of the SAL on Helene appears to be limited to the earliest stages of development, although the magnitude of that impact is difficult to determine observationally. Saharan dust was observed on the periphery of the storm during the first two days of development after genesis when intensification was slow. Much of the dust was observed to move well westward of the storm thereafter, with little SAL air present during the remainder of the storm's lifetime and with the storm gradually becoming a category-3 strength storm four days later. Dry air observed to wrap around the periphery of Helene was diagnosed to be primarily non-Saharan in origin (the result of subsidence) and appeared to have little impact on storm intensity. The eventual weakening of the storm is suggested to result from an eyewall replacement cycle and substantial reduction of the sea surface temperatures beneath the hurricane as its forward motion decreased. C1 [Braun, Scott A.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Processes Lab, Greenbelt, MD 20771 USA. [Sippel, Jason A.] Morgan State Univ, NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Shie, Chung-Lin] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. [Boller, Ryan A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Braun, SA (reprint author), NASA, GSFC, Mail Code 612, Greenbelt, MD 20771 USA. EM scott.a.braun@nasa.gov FU NASA FX We thank John Knaff and two anonymous reviewers for their comments on the manuscript. This work was supported by Dr. Ramesh Kakar at NASA Headquarters with funds from the NASA Hurricane Science Research Program. The TRMM and AMSR-E SST data were produced by Remote Sensing Systems who has been sponsored by NASA Earth Science programs. LASE data were provided by Drs. Ed Browell, Richard Ferrare, and Syed Ismail from NASA Langley Research Center. NR 60 TC 4 Z9 4 U1 4 U2 19 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 EI 1520-0493 J9 MON WEATHER REV JI Mon. Weather Rev. PD DEC PY 2013 VL 141 IS 12 BP 4269 EP 4295 DI 10.1175/MWR-D-13-00045.1 PG 27 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 256AY UT WOS:000327283300006 ER PT J AU Busch, DS Boughton, DA Cooney, T Lawson, P Lindley, ST McClure, M Ruckelshaus, MH Sands, NJ Spence, BC Wainwright, TC Williams, TH McElhany, P AF Busch, D. Shallin Boughton, David A. Cooney, Thomas Lawson, Peter Lindley, Steven T. McClure, Michelle Ruckelshaus, Mary H. Sands, Norma Jean Spence, Brian C. Wainwright, Thomas C. Williams, Thomas H. McElhany, Paul TI A Practical Comparison of Viability Models Used for Management of Endangered and Threatened Anadromous Pacific Salmonids SO NORTH AMERICAN JOURNAL OF FISHERIES MANAGEMENT LA English DT Article ID POPULATION VIABILITY; EXTINCTION PARAMETERS; DENSITY-DEPENDENCE; CHINOOK SALMON; UNCERTAINTY; HABITAT; CONSERVATION; PROTOCOLS; HARVEST; GROWTH AB This study considered whether different population viability analyses give similar estimates of extinction risk across management contexts. We compared the performance of population viability analyses developed by numerous scientific teams to estimate extinction risk of anadromous Pacific salmonids listed under the U.S. Endangered Species Act and challenged each analysis with data from 34 populations. We found variation in estimated extinction risk among analytical techniques, which was driven by varying model assumptions and the inherent uncertainty of risk forecasts. This result indicates that the scientific teams developed techniques that perform differently. We recommend that managers minimize uncertainty in risk estimates by using multiple models tailored to the local ecology. Assessment of relative extinction risk was less sensitive to model assumptions than was assessment of absolute extinction risk. Thus, the former method is better for comparing population status and raises caution about conclusions regarding absolute extinction risk. C1 [Busch, D. Shallin; McElhany, Paul] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA. [Boughton, David A.; Lindley, Steven T.; Spence, Brian C.; Williams, Thomas H.] NOAA, Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Santa Cruz, CA 95060 USA. [Cooney, Thomas] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Portland, OR 97232 USA. [Lawson, Peter; Wainwright, Thomas C.] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Newport, OR 97365 USA. [McClure, Michelle; Ruckelshaus, Mary H.; Sands, Norma Jean] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98125 USA. RP Busch, DS (reprint author), NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, 2725 Montlake Blvd East, Seattle, WA 98112 USA. EM shallin.busch@noaa.gov RI Wainwright, Thomas/F-4550-2010; Lindley, Steven/G-3997-2014; McClure, Michelle/O-7853-2015 OI Wainwright, Thomas/0000-0001-5147-479X; Lindley, Steven/0000-0001-9556-0411; McClure, Michelle/0000-0003-4791-8719 FU National Research Council FX The population extinction risk estimates presented in this study are for academic use only and are not appropriate for use in management or regulation actions. We thank the following individuals for help with data, analyses, and preparation of this manuscript: P. Adams, K. Burnett, M. Chilcote, J. Davies, M. Ford, A. Guerry, L. Hayward, D. Holzer, M. Sheer, and three anonymous reviewers. D.S.B. was supported by a National Research Council postdoctoral fellowship. NR 50 TC 3 Z9 3 U1 1 U2 19 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0275-5947 EI 1548-8675 J9 N AM J FISH MANAGE JI North Am. J. Fish Manage. PD DEC 1 PY 2013 VL 33 IS 6 BP 1125 EP 1141 DI 10.1080/02755947.2013.824933 PG 17 WC Fisheries SC Fisheries GA 274JL UT WOS:000328602500007 ER PT J AU Szkody, P Albright, M Linnell, AP Everett, ME McMillan, R Saurage, G Huehnerhoff, J Howell, SB Simonsen, M Hunt-Walker, N AF Szkody, Paula Albright, Meagan Linnell, Albert P. Everett, Mark E. McMillan, Russet Saurage, Gabrelle Huehnerhoff, Joseph Howell, Steve B. Simonsen, Mike Hunt-Walker, Nick TI A Study of the Unusual Z Cam Systems IW Andromedae and V513 Cassiopeia SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID DWARF-NOVA OUTBURSTS; CATACLYSMIC VARIABLES; ULTRAVIOLET-SPECTRUM; Z-CAMELOPARDALIS; ACCRETION DISKS; STARS; MODEL; PROGRAM AB The Z Camelopardalis stars IW And and V513 Cas are unusual in having outbursts following their standstills, in contrast to the usual Z Cam behavior of quiescence following standstills. In order to gain further understanding of these little-studied systems, we obtained spectra correlated with photometry from the AAVSO throughout a 3--4 month interval in 2011. In addition, time-resolved spectra were obtained in 2012 that provided orbital periods of 3.7hr for IW And and 5.2hr for V513 Cas. The photometry of V513 Cas revealed a regular pattern of standstills and outbursts with little time at quiescence, while IW And underwent many excursions from quiescence to outburst to short standstills. The spectra of IW And are similar to normal dwarf novae, with strong Balmer emission at quiescence and absorption at outburst. In contrast, V513 Cas shows a much flatter/redder spectrum near outburst with strong He II emission and prominent emission cores in the Balmer lines. Part of this continuum difference may be due to reddening effects. While our attempts to model the outburst and standstill states of IW And indicate a mass accretion rate near 3xx10(-9)Myr(-1), we could find no obvious reason why these systems behave differently following standstill, compared to normal Z Cam stars. C1 [Szkody, Paula; Albright, Meagan; Linnell, Albert P.; Hunt-Walker, Nick] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [McMillan, Russet; Saurage, Gabrelle; Huehnerhoff, Joseph] Apache Point Observ, Sunspot, NM 88349 USA. [Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Simonsen, Mike] AAVSO, Cambridge, MA 02138 USA. RP Szkody, P (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA. EM szkody@astro.washington.edu; mikesimonsen@aavso.org FU NSF [AST-1008734] FX We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. We are also grateful to Thomas Harrison for obtaining a spectrum as part of this program. This work was partially supported by NSF grant AST-1008734. NR 21 TC 4 Z9 4 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC 1 PY 2013 VL 125 IS 934 BP 1421 EP 1428 DI 10.1086/674170 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 272MZ UT WOS:000328466200003 ER PT J AU Rauscher, BJ Antonille, SR Boehm, N Davila, PS Foltz, R Greenhouse, MA Gum, JS Hill, RJ Kimble, RA Lindler, D Madison, TJ Mott, DB Ohl, RG Waczynski, A AF Rauscher, Bernard J. Antonille, Scott R. Boehm, Nicholas Davila, Pamela S. Foltz, Roger Greenhouse, Matthew A. Gum, Jeffrey S. Hill, Robert J. Kimble, Randy A. Lindler, Don Madison, Timothy J. Mott, D. Brent Ohl, Raymond G. Waczynski, Augustyn TI Overlight testing for the James Webb Space Telescope SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE Astronomical Instrumentation AB We describe the overlight test that was done for JWST''s Teledyne H2RG HgCdTe near-infrared detector arrays. We projected many very bright =632.8nm spots onto one flight representative, substrate-removed, HgCdTe 5m cutoff detector array. We allowed individual spots to burn in for as long as approximate to approximate to 1000s before turning off the laser. We did not detect any permanent change in detector performance for extreme over illuminations as bright as 320Wpixel(-1) (1Wm(-2)) after the array had been returned to ambient laboratory temperature and pressure. The brightest individual spot contained roughly 4mW of power spread over a 100m diameter circular area. This is brighter than the brightest lasers that are planned for use during JWST integration and testing. It is also approximate to approximate to 10(3)xx brighter than any 632.8nm astronomical source in the night sky. C1 [Rauscher, Bernard J.; Antonille, Scott R.; Boehm, Nicholas] Global Sci & Technol, Greenbelt, MD 20770 USA. [Davila, Pamela S.; Foltz, Roger; Greenhouse, Matthew A.; Gum, Jeffrey S.; Hill, Robert J.] Conceptual Analyt LLC, Glenn Dale, MD USA. [Kimble, Randy A.; Lindler, Don] Sigma Space Corp, Lanham, MD 20706 USA. [Madison, Timothy J.; Mott, D. Brent; Ohl, Raymond G.; Waczynski, Augustyn] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rauscher, BJ (reprint author), Global Sci & Technol, 7855 Walker Dr,Suite 200, Greenbelt, MD 20770 USA. EM Bernard.J.Rauscher@nasa.gov FU NASA FX This work was supported by NASA as part of the James Webb Space Telescope Project. NR 7 TC 1 Z9 1 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC 1 PY 2013 VL 125 IS 934 BP 1465 EP 1473 DI 10.1086/674176 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 272MZ UT WOS:000328466200008 ER PT J AU Shapiro, C Rowe, BTP Goodsall, T Hirata, C Fucik, J Rhodes, J Seshadri, S Smith, R AF Shapiro, C. Rowe, B. T. P. Goodsall, T. Hirata, C. Fucik, J. Rhodes, J. Seshadri, S. Smith, R. TI Weak Gravitational Lensing Systematics from Image Combination SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE Data Analysis and Techniques ID POINT-SPREAD FUNCTION; TELESCOPE; REQUIREMENTS; DETECTORS; CFHTLENS AB Extremely accurate shape measurements of galaxy images are needed to probe dark energy properties with weak gravitational lensing surveys. To increase survey area with a fixed observing time and pixel count, images from surveys such as the Wide Field Infrared Survey Telescope (WFIRST) or Euclid will necessarily be undersampled and therefore distorted by aliasing. Oversampled, unaliased images can be obtained by combining multiple, dithered exposures of the same source with a suitable reconstruction algorithm. Any such reconstruction must minimally distort the reconstructed images for weak lensing analyses to be unbiased. In this paper, we use the image combination (IMCOM) algorithm of Rowe, Hirata, and Rhodes to investigate the effect of image combination on shape measurements (size and ellipticity). We simulate dithered images of sources with varying amounts of ellipticity and undersampling, reconstruct oversampled output images from them using IMCOM, and measure shape distortions in the output. Our simulations show that IMCOM creates no significant distortions when the relative offsets between dithered images are precisely known. Distortions increase with the uncertainty in those offsets, but become problematic only with relatively poor astrometric precision; e.g., for images similar to those from the Astrophysics Focused Telescope Asset (AFTA) implementation of WFIRST, combining eight undersampled images (sampling ratio Q=1) with highly pessimistic uncertainty in astrometric registration (sigma sigma(d)approximate to approximate to 10(-3) pixels) yields an rms shear error of O(10(-4)). Our analysis pipeline is adapted from that of the Precision Projector Laboratorya joint project between NASA Jet Propulsion Laboratory and Caltech that characterizes image sensors using laboratory emulations of astronomical data. C1 [Shapiro, C.; Rowe, B. T. P.; Goodsall, T.; Rhodes, J.; Seshadri, S.] CALTECH, Jet Prop Lab, La Canada Flintridge, CA 91109 USA. [Rowe, B. T. P.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Hirata, C.; Fucik, J.; Rhodes, J.; Smith, R.] CALTECH, Pasadena, CA 91125 USA. [Hirata, C.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. RP Shapiro, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, La Canada Flintridge, CA 91109 USA. EM Charles.A.Shapiro@jpl.nasa.gov OI Rowe, Barnaby/0000-0002-7042-9174 FU National Aeronautics and Space Administration; JPL Research and Technology Development (RTD) program; Director's Research Development Fund (DRDF) program; US Department of Energy's (DOE); NASA Wide Field IR Survey Telescope (WFIRST) project office; NASA Joint Dark Energy Mission (JDEM) project office; NASA Oak Ridge Associated Universities; European Research Council [240672] FX We thank E. Jullo of Laboratoire d'Astrophysique de Marseille and V. Velur for their contributions to the analysis pipeline. This research was carried out at the Jet Propulsion Laboratory and California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We are grateful to the following organizations and programs for their support of this effort: internal JPL Research and Technology Development (RTD) and Director's Research Development Fund (DRDF) programs; US Department of Energy's (DOE) Supernova Acceleration Probe (SNAP) and Joint Dark Energy Mission (JDEM) projects; the NASA Wide Field IR Survey Telescope (WFIRST) and Joint Dark Energy Mission (JDEM) project offices. CS was supported by a NASA Postdoctoral Program Fellowship from Oak Ridge Associated Universities. BR acknowledges support from European Research Council in the form of a Starting Grant with number 240672. JPL is run by the California Institute of Technology under a contract for NASA. Thanks also to our anonymous referee for improvements to this manuscript. NR 41 TC 2 Z9 2 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC 1 PY 2013 VL 125 IS 934 BP 1496 EP 1513 DI 10.1086/674415 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 272MZ UT WOS:000328466200010 ER PT J AU Mancone, CL Gonzalez, AH Moustakas, LA Price, A AF Mancone, Conor L. Gonzalez, Anthony H. Moustakas, Leonidas A. Price, Andrew TI PyGFit: A Tool for Extracting PSF Matched Photometry SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE Data Analysis and Techniques ID HUBBLE-DEEP-FIELD; ARRAY CAMERA IRAC; DECOMPOSITION AB We present PyGFit, a program designed to measure PSF-matched photometry from images with disparate pixel scales and PSF sizes. While PyGFit has a number of uses, its primary purpose is to extract robust spectral energy distributions (SEDs) from crowded images. It does this by fitting blended sources in crowded, low-resolution images with models generated from a higher-resolution image. This approach minimizes the impact of crowding and also yields consistently measured fluxes in different filters, minimizing systematic uncertainty in the final SEDs. We present an example of applying PyGFit to real data and perform simulations to test its fidelity. The uncertainty in the best-fit flux rises sharply as a function of nearest-neighbor distance for objects with a neighbor within 60% of the PSF size. Similarly, the uncertainty increases quickly for objects blended with a neighbor 4 times brighter. For all other objects, the fidelity of PyGFit''s results depends only on flux, and the uncertainty is primarily limited by sky noise. C1 [Mancone, Conor L.; Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Moustakas, Leonidas A.; Price, Andrew] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mancone, CL (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA. EM cmancone@astro.ufl.edu OI Price, Andrew/0000-0002-1782-7587; Moustakas, Leonidas/0000-0003-3030-2360 FU National Science Foundation [AST-0070849]; HST programs by NASA through Space Telescope Science Institute [11597, 11663]; NASA [NAS 5-26555] FX The authors thank Chien Peng for helpful discussions at the outset of this project and thank the referee for helpful suggestions ot improve the usability of the code. The authors acknowledge support of this work from the National Science Foundation under grant AST-0070849. The authors also acknowledge support through HST programs 11597 and 11663, provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. The work of LAM was performed at the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 16 TC 5 Z9 5 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC 1 PY 2013 VL 125 IS 934 BP 1514 EP 1524 DI 10.1086/674431 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 272MZ UT WOS:000328466200011 ER PT J AU Teplitz, HI Rafelski, M Kurczynski, P Bond, NA Grogin, N Koekemoer, AM Atek, H Brown, TM Coe, D Colbert, JW Ferguson, HC Finkelstein, SL Gardner, JP Gawiser, E Giavalisco, M Gronwall, C Hanish, DJ Lee, KS De Mello, DF Ravindranath, S Ryan, RE Siana, BD Scarlata, C Soto, E Voyer, EN Wolfe, AM AF Teplitz, Harry I. Rafelski, Marc Kurczynski, Peter Bond, Nicholas A. Grogin, Norman Koekemoer, Anton M. Atek, Hakim Brown, Thomas M. Coe, Dan Colbert, James W. Ferguson, Henry C. Finkelstein, Steven L. Gardner, Jonathan P. Gawiser, Eric Giavalisco, Mauro Gronwall, Caryl Hanish, Daniel J. Lee, Kyoung-Soo De Mello, Duilia F. Ravindranath, Swara Ryan, Russell E. Siana, Brian D. Scarlata, Claudia Soto, Emmaris Voyer, Elysse N. Wolfe, Arthur M. TI UVUDF: ULTRAVIOLET IMAGING OF THE HUBBLE ULTRA DEEP FIELD WITH WIDE-FIELD CAMERA 3 SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: high-redshift ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; GOODS-SOUTH FIELD; CHARGE-TRANSFER INEFFICIENCY; SIMILAR-TO 2; EXTRAGALACTIC LEGACY SURVEY; REST-FRAME ULTRAVIOLET; UV LUMINOSITY FUNCTION; PIXEL-BASED CORRECTION; MU-M OBSERVATIONS AB We present an overview of a 90 orbit Hubble Space Telescope treasury program to obtain near-ultraviolet imaging of the Hubble Ultra Deep Field using the Wide Field Camera 3 UVIS detector with the F225W, F275W, and F336W filters. This survey is designed to: (1) investigate the episode of peak star formation activity in galaxies at 1 < z < 2.5; (2) probe the evolution of massive galaxies by resolving sub-galactic units (clumps); (3) examine the escape fraction of ionizing radiation from galaxies at z similar to 2-3; (4) greatly improve the reliability of photometric redshift estimates; and (5) measure the star formation rate efficiency of neutral atomic-dominated hydrogen gas at z similar to 1-3. In this overview paper, we describe the survey details and data reduction challenges, including both the necessity of specialized calibrations and the effects of charge transfer inefficiency. We provide a stark demonstration of the effects of charge transfer inefficiency on resultant data products, which when uncorrected, result in uncertain photometry, elongation of morphology in the readout direction, and loss of faint sources far from the readout. We agree with the STScI recommendation that future UVIS observations that require very sensitive measurements use the instrument's capability to add background light through a "post-flash." Preliminary results on number counts of UV-selected galaxies and morphology of galaxies at z similar to 1 are presented. We find that the number density of UV dropouts at redshifts 1.7, 2.1, and 2.7 is largely consistent with the number predicted by published luminosity functions. We also confirm that the image mosaics have sufficient sensitivity and resolution to support the analysis of the evolution of star-forming clumps, reaching 28-29th magnitude depth at 5 sigma in a 0 ''.2 radius aperture depending on filter and observing epoch. C1 [Teplitz, Harry I.; Rafelski, Marc; Colbert, James W.; Hanish, Daniel J.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Kurczynski, Peter; Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Bond, Nicholas A.; Gardner, Jonathan P.; De Mello, Duilia F.] Goddard Space Flight Ctr, Lab Observat Cosmol, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Grogin, Norman; Koekemoer, Anton M.; Brown, Thomas M.; Coe, Dan; Ferguson, Henry C.; Ryan, Russell E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Atek, Hakim] EPFL, Astrophys Lab, CH-1290 Sauverny, Switzerland. [Finkelstein, Steven L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Giavalisco, Mauro] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Gronwall, Caryl] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Gronwall, Caryl] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Lee, Kyoung-Soo] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [De Mello, Duilia F.; Soto, Emmaris] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Ravindranath, Swara] InterUniv Ctr Astron & Astrophys, Pune, Maharashtra, India. [Siana, Brian D.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Scarlata, Claudia] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Voyer, Elysse N.] Aix Marseille Univ, CNRS, LAM, F-13388 Marseille, France. [Wolfe, Arthur M.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Wolfe, Arthur M.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. RP Teplitz, HI (reprint author), CALTECH, Ctr Infrared Proc & Anal, MS 100-22, Pasadena, CA 91125 USA. EM hit@ipac.caltech.edu OI Koekemoer, Anton/0000-0002-6610-2048; Brown, Thomas/0000-0002-1793-9968 FU NASA through Space Telescope Science Institute [GO-12534]; NASA [NAS5-26555] FX We would like to thank the WFC3 team at the Space Telescope Science Institute for their help with solving new calibration and CTE challenges in the binned data. We also thank our Program Coordinator, Anthony Roman, and our Contact Scientist, John Mackenty. Support for HST Program GO-12534 was provided by NASA through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. NR 122 TC 18 Z9 19 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2013 VL 146 IS 6 AR 159 DI 10.1088/0004-6256/146/6/159 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262PC UT WOS:000327747700022 ER PT J AU Gill, Z AF Gill, Zann TI The Other Edge of Ockham's Razor: The A-PR Hypothesis and the Origin of Mind SO BIOSEMIOTICS LA English DT Article DE A-PR cycles; Evolution; Ockham's Razor; Origin of mind; Struggle for existence ID ORGANIZATION; LIFE AB Charles Darwin's theory of evolution characterized all life as engaged in a "struggle for existence". To struggle requires internal data processing to detect and interpret patterns to guide behavior, a mechanism to struggle for existence. The cognitive bootstrapping A-PR cycle (Autonomy | Pattern Recognition) couples the origin of life and mind, enabling their symbiotic co-evolution. Life processes energy to create order. Mind processes data to create meaning. Life and mind co-evolve toward increased functional effectiveness, using A-PR feedback cycles that reflect the two Laws deduced from Ockham's Razor. The Law of Parsimony is only one of two laws that have emerged from debate about Ockham's Razor. Less well known is the "other edge of Ockham's Razor", the Law of Succinctness which, when viewed through the lens of Charles Darwin's theory of evolution, enables the A-PR Hypothesis to fulfill the criteria of Ockham's Razor. C1 NASA, Ames Res Ctr, MM Forum, Los Altos, CA 94024 USA. RP Gill, Z (reprint author), NASA, Ames Res Ctr, MM Forum, POB 4001, Los Altos, CA 94024 USA. EM zg@microbes-mind.net NR 63 TC 0 Z9 0 U1 1 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1875-1342 EI 1875-1350 J9 BIOSEMIOTICS-NETH JI Biosemiotics PD DEC PY 2013 VL 6 IS 3 BP 403 EP 419 DI 10.1007/s12304-013-9176-6 PG 17 WC Humanities, Multidisciplinary; History & Philosophy Of Science SC Arts & Humanities - Other Topics; History & Philosophy of Science GA 270QH UT WOS:000328333000010 ER PT J AU Camp, J Barthelmy, S Blackburn, L Carpenter, KG Gehrels, N Kanner, J Marshall, FE Racusin, JL Sakamoto, T AF Camp, J. Barthelmy, S. Blackburn, L. Carpenter, K. G. Gehrels, N. Kanner, J. Marshall, F. E. Racusin, J. L. Sakamoto, T. TI Using ISS telescopes for electromagnetic follow-up of gravitational wave detections of NS-NS and NS-BH mergers SO EXPERIMENTAL ASTRONOMY LA English DT Article DE Gravitational waves; Gamma-ray bursts ID GAMMA-RAY BURSTS; ALL-SKY SURVEY; X-RAY; COUNTERPARTS; SEARCH; PERFORMANCE; LIGO AB The International Space Station offers a unique platform for rapid and inexpensive deployment of space telescopes. A scientific opportunity of great potential later this decade is the use of telescopes for the electromagnetic follow-up of ground-based gravitational wave detections of neutron star and black hole mergers. We describe this possibility for OpTIIX, an ISS technology demonstration of a 1.5 m diffraction limited optical telescope assembled in space, and ISS-Lobster, a wide-field imaging X-ray telescope now under study as a potential NASA mission. Both telescopes will be mounted on pointing platforms, allowing rapid positioning to the source of a gravitational wave event. Electromagnetic follow-up rates of several per year appear likely, offering a wealth of complementary science on the mergers of black holes and neutron stars. C1 [Camp, J.; Barthelmy, S.; Blackburn, L.; Carpenter, K. G.; Gehrels, N.; Kanner, J.; Marshall, F. E.; Racusin, J. L.; Sakamoto, T.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Blackburn, L (reprint author), NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD USA. EM lindy.l.blackburn@nasa.gov OI Kanner, Jonah/0000-0001-8115-0577 NR 40 TC 7 Z9 7 U1 0 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 EI 1572-9508 J9 EXP ASTRON JI Exp. Astron. PD DEC PY 2013 VL 36 IS 3 BP 505 EP 522 DI 10.1007/s10686-013-9343-4 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 269BB UT WOS:000328214000004 ER PT J AU Soffitta, P Barcons, X Bellazzini, R Braga, J Costa, E Fraser, GW Gburek, S Huovelin, J Matt, G Pearce, M Poutanen, J Reglero, V Santangelo, A Sunyaev, RA Tagliaferri, G Weisskopf, M Aloisio, R Amato, E Attina, P Axelsson, M Baldini, L Basso, S Bianchi, S Blasi, P Bregeon, J Brez, A Bucciantini, N Burderi, L Burwitz, V Casella, P Churazov, E Civitani, M Covino, S da Silva, RMC Cusumano, G Dadina, M D'Amico, F De Rosa, A Di Cosimo, S Di Persio, G Di Salvo, T Dovciak, M Elsner, R Eyles, CJ Fabian, AC Fabiani, S Feng, H Giarrusso, S Goosmann, RW Grandi, P Grosso, N Israel, G Jackson, M Kaaret, P Karas, V Kuss, M Lai, D La Rosa, G Larsson, J Larsson, S Latronico, L Maggio, A Maia, J Marin, F Massai, MM Mineo, T Minuti, M Moretti, E Muleri, F O'Dell, SL Pareschi, G Peres, G Pesce, M Petrucci, PO Pinchera, M Porquet, D Ramsey, B Rea, N Reale, F Rodrigo, JM Rozanska, A Rubini, A Rudawy, P Ryde, F Salvati, M de Santiago, VA Sazonov, S Sgro, C Silver, E Spandre, G Spiga, D Stella, L Tamagawa, T Tamborra, F Tavecchio, F Dias, TT van Adelsberg, M Wu, K Zane, S AF Soffitta, Paolo Barcons, Xavier Bellazzini, Ronaldo Braga, Joao Costa, Enrico Fraser, George W. Gburek, Szymon Huovelin, Juhani Matt, Giorgio Pearce, Mark Poutanen, Juri Reglero, Victor Santangelo, Andrea Sunyaev, Rashid A. Tagliaferri, Gianpiero Weisskopf, Martin Aloisio, Roberto Amato, Elena Attina, Primo Axelsson, Magnus Baldini, Luca Basso, Stefano Bianchi, Stefano Blasi, Pasquale Bregeon, Johan Brez, Alessandro Bucciantini, Niccolo Burderi, Luciano Burwitz, Vadim Casella, Piergiorgio Churazov, Eugene Civitani, Marta Covino, Stefano Curado da Silva, Rui Miguel Cusumano, Giancarlo Dadina, Mauro D'Amico, Flavio De Rosa, Alessandra Di Cosimo, Sergio Di Persio, Giuseppe Di Salvo, Tiziana Dovciak, Michal Elsner, Ronald Eyles, Chris J. Fabian, Andrew C. Fabiani, Sergio Feng, Hua Giarrusso, Salvatore Goosmann, Rene W. Grandi, Paola Grosso, Nicolas Israel, Gianluca Jackson, Miranda Kaaret, Philip Karas, Vladimir Kuss, Michael Lai, Dong La Rosa, Giovanni Larsson, Josefin Larsson, Stefan Latronico, Luca Maggio, Antonio Maia, Jorge Marin, Frederic Massai, Marco Maria Mineo, Teresa Minuti, Massimo Moretti, Elena Muleri, Fabio O'Dell, Stephen L. Pareschi, Giovanni Peres, Giovanni Pesce, Melissa Petrucci, Pierre-Olivier Pinchera, Michele Porquet, Delphine Ramsey, Brian Rea, Nanda Reale, Fabio Rodrigo, Juana Maria Rozanska, Agata Rubini, Alda Rudawy, Pawel Ryde, Felix Salvati, Marco de Santiago, Valdivino Alexandre, Jr. Sazonov, Sergey Sgro, Carmelo Silver, Eric Spandre, Gloria Spiga, Daniele Stella, Luigi Tamagawa, Toru Tamborra, Francesco Tavecchio, Fabrizio Dias, Teresa Teixeira van Adelsberg, Matthew Wu, Kinwah Zane, Silvia TI XIPE: the X-ray imaging polarimetry explorer SO EXPERIMENTAL ASTRONOMY LA English DT Article DE Astronomy; X-ray; Polarimetry ID GAS PIXEL DETECTOR; ACCRETING BLACK-HOLES; SOLAR-FLARES; GALACTIC-CENTER; NEUTRON-STARS; CRAB-NEBULA; COMPTON-SCATTERING; QUANTUM-GRAVITY; POLARIZATION MEASUREMENTS; CHANDRA OBSERVATIONS AB X-ray polarimetry, sometimes alone, and sometimes coupled to spectral and temporal variability measurements and to imaging, allows a wealth of physical phenomena in astrophysics to be studied. X-ray polarimetry investigates the acceleration process, for example, including those typical of magnetic reconnection in solar flares, but also emission in the strong magnetic fields of neutron stars and white dwarfs. It detects scattering in asymmetric structures such as accretion disks and columns, and in the so-called molecular torus and ionization cones. In addition, it allows fundamental physics in regimes of gravity and of magnetic field intensity not accessible to experiments on the Earth to be probed. Finally, models that describe fundamental interactions (e.g. quantum gravity and the extension of the Standard Model) can be tested. We describe in this paper the X-ray Imaging Polarimetry Explorer (XIPE), proposed in June 2012 to the first ESA call for a small mission with a launch in 2017. The proposal was, unfortunately, not selected. To be compliant with this schedule, we designed the payload mostly with existing items. The XIPE proposal takes advantage of the completed phase A of POLARIX for an ASI small mission program that was cancelled, but is different in many aspects: the detectors, the presence of a solar flare polarimeter and photometer and the use of a light platform derived by a mass production for a cluster of satellites. XIPE is composed of two out of the three existing JET-X telescopes with two Gas Pixel Detectors (GPD) filled with a He-DME mixture at their focus. Two additional GPDs filled with a 3-bar Ar-DME mixture always face the Sun to detect polarization from solar flares. The Minimum Detectable Polarization of a 1 mCrab source reaches 14 % in the 2-10 keV band in 10(5) s for pointed observations, and 0.6 % for an X10 class solar flare in the 15-35 keV energy band. The imaging capability is 24 arcsec Half Energy Width (HEW) in a Field of View of 14.7 arcmin x 14.7 arcmin. The spectral resolution is 20 % at 6 keV and the time resolution is 8 mu s. The imaging capabilities of the JET-X optics and of the GPD have been demonstrated by a recent calibration campaign at PANTER X-ray test facility of the Max-Planck-Institut fur extraterrestrische Physik (MPE, Germany). XIPE takes advantage of a low-earth equatorial orbit with Malindi as down-link station and of a Mission Operation Center (MOC) at INPE (Brazil). The data policy is organized with a Core Program that comprises three months of Science Verification Phase and 25 % of net observing time in the following 2 years. A competitive Guest Observer program covers the remaining 75 % of the net observing time. C1 [Soffitta, Paolo; Costa, Enrico; De Rosa, Alessandra; Di Cosimo, Sergio; Di Persio, Giuseppe; Fabiani, Sergio; Muleri, Fabio; Rubini, Alda] IAPS INAF, I-00133 Rome, Italy. [Barcons, Xavier] Inst Fis Cantabria CSIC UC, Santander 39005, Spain. [Bellazzini, Ronaldo; Bregeon, Johan; Brez, Alessandro; Kuss, Michael; Latronico, Luca; Minuti, Massimo; Pesce, Melissa; Pinchera, Michele; Sgro, Carmelo; Spandre, Gloria] INFN Pisa, I-56127 Pisa, Italy. [Braga, Joao; D'Amico, Flavio; de Santiago, Valdivino Alexandre, Jr.] INPE Div Astrofs, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [Fraser, George W.] Univ Leicester, Dept Phys & Astron, Space Res Ctr, Leicester LE1 7RH, Leics, England. [Gburek, Szymon] Polish Acad Sci, Space Res Ctr, Solar Phys Div, PL-51622 Wroclaw, Poland. [Huovelin, Juhani] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland. [Matt, Giorgio; Bianchi, Stefano; Tamborra, Francesco] Univ Studi Roma Tre, Dipartimento Fis E Amaldi, I-00146 Rome, Italy. [Pearce, Mark; Axelsson, Magnus; Jackson, Miranda; Larsson, Josefin; Larsson, Stefan; Moretti, Elena; Ryde, Felix] Royal Inst Technol, Dept Phys, KTH, Stockholm, Sweden. [Pearce, Mark; Axelsson, Magnus; Jackson, Miranda; Larsson, Josefin; Larsson, Stefan; Moretti, Elena; Ryde, Felix] AlbaNova Univ Ctr, Oskar Klein Ctr Cosmoparticle Phys, Stockholm, Sweden. [Poutanen, Juri] Univ Oulu, Dept Phys, Astron Div, Oulu 90014, Finland. [Reglero, Victor; Rodrigo, Juana Maria] Univ Valencia Astron & Astrofis, Inst Ciencias Mat, Burjassot 46100, Spain. [Santangelo, Andrea] Iniversitat Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Sunyaev, Rashid A.; Churazov, Eugene] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Tagliaferri, Gianpiero; Basso, Stefano; Civitani, Marta; Covino, Stefano; Pareschi, Giovanni; Spiga, Daniele; Tavecchio, Fabrizio] INAF Osservatorio Astron Brera, I-23807 Merate, Lc, Italy. [Weisskopf, Martin; Elsner, Ronald; O'Dell, Stephen L.; Ramsey, Brian] NASA Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Attina, Primo] Thales Alenia Space Italia S P A, I-10146 Turin, Italy. [Baldini, Luca; Massai, Marco Maria] Univ Pisa, Dipartimento Fis, I-56127 Pisa, Italy. [Baldini, Luca; Massai, Marco Maria] INFN Pisa, Dipartimento Fis, I-56127 Pisa, Italy. [Aloisio, Roberto; Amato, Elena; Blasi, Pasquale; Bucciantini, Niccolo; Salvati, Marco] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Burderi, Luciano] Univ Cagliari, Dipartimento Fis, I-09042 Cagliari, Italy. [Burwitz, Vadim] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Burwitz, Vadim] Panter Xray Test Facil, D-82061 Neuried, Germany. [Casella, Piergiorgio; Israel, Gianluca; Stella, Luigi] INAF Osservatorio Astrofis Roma, I-00040 Rome, Italy. [Curado da Silva, Rui Miguel; Maia, Jorge; Dias, Teresa Teixeira] Univ Coimbra, Dept Fis, P-3004516 Coimbra, Portugal. [Cusumano, Giancarlo; Giarrusso, Salvatore; La Rosa, Giovanni; Mineo, Teresa] INAF IASF Palermo, I-90146 Palermo, Italy. [Dadina, Mauro; Grandi, Paola] INAF IASF Bologna, I-40129 Bologna, Italy. [Di Salvo, Tiziana; Peres, Giovanni; Reale, Fabio] Univ Studi Palermo, DiFC, I-90123 Palermo, Italy. [Dovciak, Michal; Karas, Vladimir] Acad Sci Czech Republic, Astron Inst, Prague 14131, Czech Republic. [Eyles, Chris J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Feng, Hua] Tsinghua Univ, Dept Engn Phys, Beijing 100084, Peoples R China. [Feng, Hua] Tsinghua Univ, Ctr Astrophys, Beijing 100084, Peoples R China. [Fabian, Andrew C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Goosmann, Rene W.; Grosso, Nicolas; Marin, Frederic; Porquet, Delphine] Observ Astronom Strasbourg, F-67000 Strasbourg, France. [Kaaret, Philip] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Lai, Dong] Cornell Univ, Ithaca, NY 14853 USA. [Maggio, Antonio] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Petrucci, Pierre-Olivier] UJF Grenoble 1, IPAG, CNRS INSU, UMR 5274, F-38041 Grenoble, France. [Rea, Nanda] Fac Ciencies, CSIC IEEC, Inst Space Sci, Barcelona 08193, Spain. [Rozanska, Agata] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Rudawy, Pawel] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Sazonov, Sergey] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [Sazonov, Sergey] Moscow Phys Tech Inst, Dolgoprudnyi 141700, Russia. [Silver, Eric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tamagawa, Toru] RIKEN, Wako, Saitama 3510198, Japan. [van Adelsberg, Matthew] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Wu, Kinwah; Zane, Silvia] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Soffitta, P (reprint author), IAPS INAF, Via Fosso Cavaliere 100, I-00133 Rome, Italy. EM paolo.soffitta@iaps.inaf.it RI Bianchi, Stefano/B-4804-2010; Karas, Vladimir/C-1559-2013; Dovciak, Michal/F-4258-2014; Barcons, Xavier/L-3335-2014; Marin, Frederic/A-3737-2015; Churazov, Eugene/A-7783-2013; Rea, Nanda/I-2853-2015; Maia, Jorge/K-1344-2015; Aloisio, Roberto/I-9533-2012; Blasi, Pasquale/O-9345-2015; Amato, Elena/P-2938-2015; Maggio, Antonio/P-5700-2015; Poutanen, Juri/H-6651-2016; Sgro, Carmelo/K-3395-2016; OI Bianchi, Stefano/0000-0002-4622-4240; Karas, Vladimir/0000-0002-5760-0459; Dovciak, Michal/0000-0003-0079-1239; Barcons, Xavier/0000-0003-1081-8861; Rea, Nanda/0000-0003-2177-6388; Maia, Jorge/0000-0002-9314-1763; Aloisio, Roberto/0000-0003-0161-5923; Blasi, Pasquale/0000-0003-2480-599X; Amato, Elena/0000-0002-9881-8112; Maggio, Antonio/0000-0001-5154-6108; Poutanen, Juri/0000-0002-0983-0049; Curado da Silva, Rui Miguel/0000-0002-9961-965X; Spiga, Daniele/0000-0003-1163-7843; Burderi, Luciano/0000-0001-5458-891X; Pareschi, Giovanni/0000-0003-3967-403X; Dias, Teresa/0000-0001-5101-4902; Bucciantini, Niccolo'/0000-0002-8848-1392; Porquet, Delphine/0000-0001-9731-0352; GIARRUSSO, SALVATORE/0000-0002-0738-2940; O'Dell, Stephen/0000-0002-1868-8056; Mineo, Teresa/0000-0002-4931-8445; Soffitta, Paolo/0000-0002-7781-4104; Dadina, Mauro/0000-0002-7858-7564; Cusumano, Giancarlo/0000-0002-8151-1990; Pesce-Rollins, Melissa/0000-0003-1790-8018; Grandi, Paola/0000-0003-1848-6013; Costa, Enrico/0000-0003-4925-8523; Israel, GianLuca/0000-0001-5480-6438; Sgro', Carmelo/0000-0001-5676-6214; PERES, Giovanni/0000-0002-6033-8180; Reale, Fabio/0000-0002-1820-4824; /0000-0003-0065-2933; Axelsson, Magnus/0000-0003-4378-8785; Casella, Piergiorgio/0000-0002-0752-3301; Moretti, Elena/0000-0001-5477-9097; Covino, Stefano/0000-0001-9078-5507; Baldini, Luca/0000-0002-9785-7726; Tagliaferri, Gianpiero/0000-0003-0121-0723; Tavecchio, Fabrizio/0000-0003-0256-0995 FU ASI; INAF; INFN FX This work is partially funded by ASI, INAF and INFN. NR 148 TC 34 Z9 34 U1 10 U2 40 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 EI 1572-9508 J9 EXP ASTRON JI Exp. Astron. PD DEC PY 2013 VL 36 IS 3 BP 523 EP 567 DI 10.1007/s10686-013-9344-3 PG 45 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 269BB UT WOS:000328214000005 ER PT J AU MacLachlan, GA Shenoy, A Sonbas, E Coyne, R Dhuga, KS Eskandarian, A Maximon, LC Parke, WC AF MacLachlan, G. A. Shenoy, A. Sonbas, E. Coyne, R. Dhuga, K. S. Eskandarian, A. Maximon, L. C. Parke, W. C. TI The Hurst exponent of Fermi gamma-ray bursts SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; methods: statistical; gamma-ray burst: general ID FRACTIONAL BROWNIAN-MOTION; CATACLYSMIC VARIABLES; WAVELET; VARIABILITY; LONG; CONJECTURE; SCALE; GRBS AB Using a wavelet decomposition technique, we have extracted the Hurst exponent for a sample of 46 long and 22 short gamma-ray bursts (GRBs) detected by the Gamma-ray Burst Monitor aboard the Fermi satellite. This exponent is a scaling parameter that provides a measure of long-range behaviour in a time series. The mean Hurst exponent for the short GRBs is significantly smaller than that for the long GRBs. The separation may serve as an unbiased criterion for distinguishing short and long GRBs. C1 [MacLachlan, G. A.; Shenoy, A.; Coyne, R.; Dhuga, K. S.; Eskandarian, A.; Maximon, L. C.; Parke, W. C.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Sonbas, E.] Adiyaman Univ, Dept Phys, TR-02040 Adiyaman, Turkey. [Sonbas, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP MacLachlan, GA (reprint author), George Washington Univ, Dept Phys, Washington, DC 20052 USA. EM maclach@gwu.edu FU NASA [NNX11AE36G] FX The NASA grant NNX11AE36G provided partial support for this work and is gratefully acknowledged. The authors (GAM and KSD) acknowledge very useful discussions with Tilan Ukwatta. NR 32 TC 4 Z9 4 U1 2 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 4 BP 2907 EP 2914 DI 10.1093/mnras/stt1701 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263HL UT WOS:000327798100003 ER PT J AU Sing, DK Des Etangs, AL Fortney, JJ Burrows, AS Pont, F Wakeford, HR Ballester, GE Nikolov, N Henry, GW Aigrain, S Deming, D Evans, TM Gibson, NP Huitson, CM Knutson, H Showman, AP Vidal-Madjar, A Wilson, PA Williamson, MH Zahnle, K AF Sing, D. K. Des Etangs, A. Lecavelier Fortney, J. J. Burrows, A. S. Pont, F. Wakeford, H. R. Ballester, G. E. Nikolov, N. Henry, G. W. Aigrain, S. Deming, D. Evans, T. M. Gibson, N. P. Huitson, C. M. Knutson, H. Showman, A. P. Vidal-Madjar, A. Wilson, P. A. Williamson, M. H. Zahnle, K. TI HST hot-Jupiter transmission spectral survey: evidence for aerosols and lack of TiO in the atmosphere of WASP-12b SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: spectroscopic; planets and satellites: atmospheres; planets and satellites: individual: WASP-12b; stars: individual: WASP-12; planetary systems ID HUBBLE-SPACE-TELESCOPE; TRANSITING PLANET ATMOSPHERES; EXTRASOLAR GIANT PLANETS; EXOPLANET HD 189733B; MU-M; THERMAL EMISSION; HOST STARS; C/O RATIO; HYDROCARBON AEROSOLS; STELLAR COMPANIONS AB We present Hubble Space Telescope (HST) optical transmission spectra of the transiting hot-Jupiter WASP-12b, taken with the Space Telescope Imaging Spectrograph instrument. The resulting spectra cover the range 2900-10 300 A which we combined with archival Wide Field Camera 3 spectra and Spitzer photometry to cover the full optical to infrared wavelength regions. With high spatial resolution, we are able to resolve WASP-12A's stellar companion in both our images and spectra, revealing that the companion is in fact a close binary M0V pair, with the three stars forming a triple-star configuration. We derive refined physical parameters of the WASP-12 system, including the orbital ephemeris, finding the exoplanet's density is similar to 20 per cent lower than previously estimated. From the transmission spectra, we are able to decisively rule out prominent absorption by TiO in the exoplanet's atmosphere, as there are no signs of the molecule's characteristic broad features nor individual bandheads. Strong pressure-broadened Na and K absorption signatures are also excluded, as are significant metal-hydride features. We compare our combined broad-band spectrum to a wide variety of existing aerosol-free atmospheric models, though none are satisfactory fits. However, we do find that the full transmission spectrum can be described by models which include significant opacity from aerosols: including Rayleigh scattering, Mie scattering, tholin haze and settling dust profiles. The transmission spectrum follows an effective extinction cross-section with a power law of index alpha, with the slope of the transmission spectrum constraining the quantity alpha T = -3528 +/- 660 K, where T is the atmospheric temperature. Rayleigh scattering (alpha = -4) is among the best-fitting models, though requires low terminator temperatures near 900 K. Sub-micron size aerosol particles can provide equally good fits to the entire transmission spectrum for a wide range of temperatures, and we explore corundum as a plausible dust aerosol. The presence of atmospheric aerosols also helps to explain the modestly bright albedo implied by Spitzer observations, as well as the near blackbody nature of the emission spectrum. Ti-bearing condensates on the cooler night-side is the most natural explanation for the overall lack of TiO signatures in WASP-12b, indicating the day/night cold trap is an important effect for very hot Jupiters. These findings indicate that aerosols can play a significant atmospheric role for the entire wide range of hot-Jupiter atmospheres, potentially affecting their overall spectrum and energy balance. C1 [Sing, D. K.; Pont, F.; Wakeford, H. R.; Nikolov, N.; Huitson, C. M.; Wilson, P. A.] Univ Exeter, Sch Phys, Astrophys Grp, Exeter EX4 4QL, Devon, England. [Des Etangs, A. Lecavelier; Vidal-Madjar, A.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Fortney, J. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Burrows, A. S.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Ballester, G. E.; Williamson, M. H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Henry, G. W.] Tennessee State Univ, Nashville, TN 37209 USA. [Aigrain, S.; Evans, T. M.; Showman, A. P.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Deming, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Gibson, N. P.] European So Observ, D-85748 Garching, Germany. [Knutson, H.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Zahnle, K.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Sing, DK (reprint author), Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England. EM sing@astro.ex.ac.uk RI Nikolov, Nikolay/H-6183-2015; OI Nikolov, Nikolay/0000-0002-6500-3574; Sing, David /0000-0001-6050-7645; Fortney, Jonathan/0000-0002-9843-4354; Wakeford, Hannah/0000-0003-4328-3867; Gibson, Neale/0000-0002-9308-2353 FU NASA from the STScI [HST-GO-12473]; UK Science and Technology Facilities Council (STFC); STFC [ST/J0016/1]; French Agence Nationale de la Recherche (ANR) [ANR-12-BS05-0012] FX This work is based on observations with the NASA/ESA HST, obtained at the Space Telescope Science Institute (STScI) operated by AURA, Inc. Support for this work was provided by NASA through grants under the HST-GO-12473 programme from the STScI. We thank I. Baraffe for useful discussions, and the anonymous referee for their comments. We also warmly thank Jason W. Ferguson for providing the optical constants for CaTiO3. CMH, PAW and HRW acknowledge support from the UK Science and Technology Facilities Council (STFC). DKS, FP and, NN acknowledge support from STFC consolidated grant ST/J0016/1. ALE and AVM acknowledge support from the French Agence Nationale de la Recherche (ANR), under programme ANR-12-BS05-0012 'Exo-Atmos'. NR 87 TC 69 Z9 70 U1 3 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 4 BP 2956 EP 2973 DI 10.1093/mnras/stt1782 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263HL UT WOS:000327798100007 ER PT J AU Tiburzi, C Johnston, S Bailes, M Bates, SD Bhat, NDR Burgay, M Burke-Spolaor, S Champion, D Coster, P D'Amico, N Keith, MJ Kramer, M Levin, L Milia, S Ng, C Possenti, A Stappers, BW Thornton, D van Straten, W AF Tiburzi, C. Johnston, S. Bailes, M. Bates, S. D. Bhat, N. D. R. Burgay, M. Burke-Spolaor, S. Champion, D. Coster, P. D'Amico, N. Keith, M. J. Kramer, M. Levin, L. Milia, S. Ng, C. Possenti, A. Stappers, B. W. Thornton, D. van Straten, W. TI The High Time Resolution Universe survey - IX. Polarimetry of long-period pulsars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE magnetic fields; polarization; methods: observational; pulsars: general ID GALACTIC MAGNETIC-FIELD; 5 MILLISECOND PULSARS; ROTATION MEASURES; RADIO PULSARS; CIRCULAR-POLARIZATION; LINEAR-POLARIZATION; EMPIRICAL-THEORY; INTEGRATED PROFILES; FARADAY-ROTATION; SOUTHERN PULSARS AB We present a polarimetric analysis of 49 long-period pulsars discovered as part of the High Time Resolution Universe (HTRU) southern survey. The sources exhibit the typical characteristics of 'old' pulsars, with low fractional linear and circular polarization and narrow, multi-component profiles. Although the position angle swings are generally complex, for two of the analysed pulsars (J1622-3751 and J1710-2616) we obtained an indication of the geometry via the rotating vector model. We were able to determine a value of the rotation measure (RM) for 34 of the sources which, when combined with their dispersion measures (DM), yields an integrated magnetic field strength along the line of sight. With the data presented here, the total number of values of RM associated with pulsars discovered during the HTRU southern survey sums to 51. The RMs are not consistent with the hypothesis of a counter-clockwise direction of the Galactic magnetic field within an annulus included between 4 and 6 kpc from the Galactic Centre. A partial agreement with a counter-clockwise sense of the Galactic magnetic field within the spiral arms is, however, found in the area of the Carina-Sagittarius arm. C1 [Tiburzi, C.; Burgay, M.; D'Amico, N.; Milia, S.; Possenti, A.] INAF Osservatorio Astron Cagliari, I-09047 Selargius, CA, Italy. [Tiburzi, C.; D'Amico, N.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, CA, Italy. [Johnston, S.; Coster, P.; Thornton, D.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Bailes, M.; Coster, P.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Bailes, M.; Bhat, N. D. R.; van Straten, W.] ARC Ctr Excellence All Sky Astrophys, Sydney, NSW 2016, Australia. [Bates, S. D.; Levin, L.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Bhat, N. D. R.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Burke-Spolaor, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91104 USA. [Champion, D.; Kramer, M.; Ng, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Keith, M. J.; Kramer, M.; Stappers, B. W.; Thornton, D.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Tiburzi, C (reprint author), INAF Osservatorio Astron Cagliari, Via Sci, I-09047 Selargius, CA, Italy. EM ctiburzi@oa-cagliari.inaf.it OI Champion, David/0000-0003-1361-7723; Burgay, Marta/0000-0002-8265-4344; van Straten, Willem/0000-0003-2519-7375 FU Commonwealth of Australia; National Aeronautics and Space Administration FX The Parkes radio telescope is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. CT also thanks Delphine Perrodin for her help. NR 62 TC 4 Z9 4 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 4 BP 3557 EP 3572 DI 10.1093/mnras/stt1834 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263HL UT WOS:000327798100052 ER PT J AU LaMassa, SM Urry, CM Cappelluti, N Civano, F Ranalli, P Glikman, E Treister, E Richards, G Ballantyne, D Stern, D Comastri, A Cardamone, C Schawinski, K Bohringer, H Chon, G Murray, SS Green, P Nandra, K AF LaMassa, Stephanie M. Urry, C. Megan Cappelluti, Nico Civano, Francesca Ranalli, Piero Glikman, Eilat Treister, Ezequiel Richards, Gordon Ballantyne, David Stern, Daniel Comastri, Andrea Cardamone, Carie Schawinski, Kevin Boehringer, Hans Chon, Gayoung Murray, Stephen S. Green, Paul Nandra, Kirpal TI Finding rare AGN: XMM-Newton and Chandra observations of SDSS Stripe 82 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE catalogues; surveys; galaxies: active; quasars: general; quasars: supermassive black holes; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; POINT-SOURCE CATALOG; DIGITAL SKY SURVEY; RAY SOURCE CATALOG; HIGHEST REDSHIFT QUASARS; X-RAY; NUMBER COUNTS; LUMINOSITY FUNCTION; COSMOS FIELD AB We have analysed the XMM-Newton and Chandra data overlapping similar to 16.5 deg(2) of Sloan Digital Sky Survey Stripe 82, including similar to 4.6 deg(2) of proprietary XMM-Newton data that we present here. In total, 3362 unique X-ray sources are detected at high significance. We derive the XMM-Newton number counts and compare them with our previously reported Chandra logN-logS relations and other X-ray surveys. The Stripe 82 X-ray source lists have been matched to multiwavelength catalogues using a maximum likelihood estimator algorithm. We discovered the highest redshift (z = 5.86) quasar yet identified in an X-ray survey. We find 2.5 times more high-luminosity (L-x >= 10(45) erg s(-1)) AGN than the smaller area Chandra and XMM-Newton survey of COSMOS and 1.3 times as many identified by XBootes. Comparing the high-luminosity active galactic nuclei (AGN) we have identified with those predicted by population synthesis models, our results suggest that this AGN population is a more important component of cosmic black hole growth than previously appreciated. Approximately a third of the X-ray sources not detected in the optical are identified in the infrared, making them candidates for the elusive population of obscured high-luminosity AGN in the early universe. C1 [LaMassa, Stephanie M.; Urry, C. Megan; Glikman, Eilat] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Cappelluti, Nico; Ranalli, Piero; Comastri, Andrea] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Cappelluti, Nico] Univ Maryland Baltimore Coll, Ctr Space Sci & Technol, Dept Phys, Baltimore, MD 21250 USA. [Civano, Francesca; Murray, Stephen S.; Green, Paul] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Civano, Francesca] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ranalli, Piero] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, GR-15236 Athens, Greece. [Treister, Ezequiel] Univ Concepcion, Concepcion, Chile. [Richards, Gordon] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Ballantyne, David] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cardamone, Carie] Brown Univ, Harriet W Sheridan Ctr Teaching & Learning, Providence, RI 02912 USA. [Schawinski, Kevin] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. [Boehringer, Hans; Chon, Gayoung; Nandra, Kirpal] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP LaMassa, SM (reprint author), Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, POB 208120, New Haven, CT 06520 USA. EM stephanie.lamassa@yale.edu RI Ranalli, Piero/K-6363-2013; Comastri, Andrea/O-9543-2015; OI Ranalli, Piero/0000-0003-3956-755X; Comastri, Andrea/0000-0003-3451-9970; Cappelluti, Nico/0000-0002-1697-186X; Schawinski, Kevin/0000-0001-5464-0888; Urry, Meg/0000-0002-0745-9792 FU National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX This publication makes use of data products from the WISE, which is a joint project of the University of California, Los Angeles and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the U.S. Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/. NR 90 TC 21 Z9 21 U1 1 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 4 BP 3581 EP 3601 DI 10.1093/mnras/stt1837 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263HL UT WOS:000327798100054 ER PT J AU Shivvers, I Mazzali, P Silverman, JM Botyaanszki, J Cenko, SB Filippenko, AV Kasen, D Van Dyk, SD Clubb, KI AF Shivvers, Isaac Mazzali, Paolo Silverman, Jeffrey M. Botyanszki, Janos Cenko, S. Bradley Filippenko, Alexei V. Kasen, Daniel Van Dyk, Schuyler D. Clubb, Kelsey I. TI Nebular spectroscopy of the nearby Type IIb supernova 2011dh SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: spectroscopic; supernovae: general; supernovae: individual: SN 2011dh ID CORE-COLLAPSE SUPERNOVAE; O-I LAMBDA-LAMBDA-6300; SN 2011DH; STRIPPED-ENVELOPE; CIRCUMSTELLAR INTERACTION; SUPERGIANT PROGENITOR; OPTICAL SPECTROSCOPY; LINE-PROFILES; MASS-LOSS; SPECTRA AB We present nebular spectra of the nearby Type IIb supernova (SN) 2011dh taken between 201 and 678 d after core collapse. At these late times, SN 2011dh exhibits strong emission lines including a broad and persistent H alpha feature. New models of the nebular spectra confirm that the progenitor of SN 2011dh was a low-mass giant (M approximate to 13-15 M-circle dot) that ejected similar to 0.07 M-circle dot of Ni-56 and similar to 0.27 M-circle dot of oxygen at the time of explosion, consistent with the recent disappearance of a candidate yellow supergiant progenitor. We show that light from the SN location is dominated by the fading SN at very late times (similar to 2 yr) and not, for example, by a binary companion or a background source. We present evidence for interaction between the expanding SN blast wave and a circumstellar medium at late times and show that the SN is likely powered by positron deposition greater than or similar to 1 yr after explosion. We also examine the geometry of the ejecta and show that the nebular line profiles of SN 2011dh indicate a roughly spherical explosion with aspherical components or clumps. C1 [Shivvers, Isaac; Cenko, S. Bradley; Filippenko, Alexei V.; Kasen, Daniel; Clubb, Kelsey I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Mazzali, Paolo] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5UZ, Merseyside, England. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Silverman, Jeffrey M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Botyanszki, Janos] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Kasen, Daniel] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Nucl Sci Div, Berkeley, CA 94720 USA. [Van Dyk, Schuyler D.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Shivvers, I (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM ishivvers@astro.berkeley.edu OI Shivvers, Isaac/0000-0003-3373-8047; Van Dyk, Schuyler/0000-0001-9038-9950 FU W. M. Keck Foundation; National Science Foundation (NSF) Graduate Research Fellowship [DGE 1106400]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; Richard and Rhoda Goldman Fund; Christopher R. Redlich Fund; TABASGO Foundation; NSF [AST-1211916] FX Sincere thanks to all of the supernova experts who contributed through discussions, including (but not limited to) Brad Tucker, WeiKang Zheng, Ori Fox, Patrick Kelly and J. Craig Wheeler (whose keen eye identified a significant typo in the manuscript). We thank the referee for suggestions that helped to improve this paper. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration (NASA); the observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations from this mountain.; This material is partially based upon work supported by a National Science Foundation (NSF) Graduate Research Fellowship to JB under grant no. DGE 1106400. JMS is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. AVF and his SN group at UC Berkeley acknowledge generous support from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation and NSF grant AST-1211916. This research has made use of NASA's Astrophysics Data System Bibliographic Services, as well as the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 86 TC 13 Z9 13 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 4 BP 3614 EP 3625 DI 10.1093/mnras/stt1839 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263HL UT WOS:000327798100056 ER PT J AU Madura, TI Gull, TR Okazaki, AT Russell, CMP Owocki, SP Groh, JH Corcoran, MF Hamaguchi, K Teodoro, M AF Madura, T. I. Gull, T. R. Okazaki, A. T. Russell, C. M. P. Owocki, S. P. Groh, J. H. Corcoran, M. F. Hamaguchi, K. Teodoro, M. TI Constraints on decreases in eta Carinae's mass-loss from 3D hydrodynamic simulations of its binary colliding winds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; binaries: close; stars: mass-loss; stars: individual: Eta Carinae; stars: winds outflows ID SMOOTHED PARTICLE HYDRODYNAMICS; HEII LAMBDA-4686 LINE; HOT-STAR WINDS; X-RAY MINIMUM; STELLAR WIND; SPECTROSCOPIC EVENT; LUMINOUS SUPERNOVA; DYNAMICAL MODEL; EMISSION-LINES; LIGHT-CURVE AB Recent work suggests that the mass-loss rate of the primary star eta(A) in the massive colliding wind binary eta Carinae dropped by a factor of 2-3 between 1999 and 2010. We present results from large- (+/- 1545 au) and small-(+/- 155 au) domain, 3D smoothed particle hydrodynamics (SPH) simulations of eta Car's colliding winds for three eta(A) mass-loss rates ((M) over dot(eta A)= 2.4, 4.8 and 8.5 x 10(-4) M-circle dot yr(-1)), investigating the effects on the dynamics of the binary wind-wind collision (WWC). These simulations include orbital motion, optically thin radiative cooling and radiative forces. We find that (M) over dot(eta A) greatly affects the time-dependent hydrodynamics at all spatial scales investigated. The simulations also show that the post-shock wind of the companion star eta(B) switches from the adiabatic to the radiative-cooling regime during periastron passage (phi approximate to 0.985-1.02). This switchover starts later and ends earlier the lower the value of (M) over dot(eta A) and is caused by the encroachment of the wind of eta(A) into the acceleration zone of eta(B) 's wind, plus radiative inhibition of eta(B) 's wind by eta(A). The SPH simulations together with 1D radiative transfer models of eta(A) 's spectra reveal that a factor of 2 or more drop in (M) over dot(eta A) should lead to substantial changes in numerous multiwavelength observables. Recent observations are not fully consistent with the model predictions, indicating that any drop in (M) over dot(eta A) was likely by a factor of less than or similar to 2 and occurred after 2004. We speculate that most of the recent observed changes in eta Car are due to a small increase in the WWC opening angle that produces significant effects because our line of sight to the system lies close to the dense walls of the WWC zone. A modest decrease in (M) over dot(eta A) may be responsible, but changes in the wind/stellar parameters of eta(B), while less likely, cannot yet be fully ruled out. We suggest observations during eta Car's next periastron in 2014 to further test for decreases in (M) over dot(eta A). If (M) over dot(eta A) is declining and continues to do so, the 2014 X-ray minimum should be even shorter than that of 2009. C1 [Madura, T. I.; Gull, T. R.; Teodoro, M.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Okazaki, A. T.; Russell, C. M. P.] Hokkai Gakuen Univ, Toyohira Ku, Sapporo, Hokkaido 0628605, Japan. [Owocki, S. P.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Groh, J. H.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [Corcoran, M. F.; Hamaguchi, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Corcoran, M. F.; Hamaguchi, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Hamaguchi, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. RP Madura, TI (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 667, Greenbelt, MD 20771 USA. EM thomas.i.madura@nasa.gov FU NASA; CNPq/MCT-Brazil [201978/2012-1] FX TIM is supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. MT is supported by CNPq/MCT-Brazil through grant 201978/2012-1. NR 97 TC 31 Z9 31 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2013 VL 436 IS 4 BP 3820 EP 3855 DI 10.1093/mnras/stt1871 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 263HL UT WOS:000327798100073 ER PT J AU Dominguez, JA Tate, LC Wright, MC Caraccio, A AF Dominguez, Jesus A. Tate, Lanetra C. Wright, M. Clara Caraccio, Anne TI Fuzzy Reasoning to More Accurately Determine Void Areas on Optical Micrographs of Composite Structures SO APPLIED COMPOSITE MATERIALS LA English DT Article DE Composite void analysis; Optical micrographs analysis; Void content composites; Void content resin; Void content matrix; Fuzzy reasoning; Fuzzy logic; Image segmentation; Image binarization; Binary segmentation AB Accomplishing the best-performing composite matrix (resin) requires that not only the processing method but also the cure cycle generate low-void-content structures. If voids are present, the performance of the composite matrix will be significantly reduced. This is usually noticed by significant reductions in matrix-dominated properties, such as compression and shear strength. Voids in composite materials are areas that are absent of the composite components: matrix and fibers. The characteristics of the voids and their accurate estimation are critical to determine for high performance composite structures. One widely used method of performing void analysis on a composite structure sample is acquiring optical micrographs or Scanning Electron Microscope (SEM) images of lateral sides of the sample and retrieving the void areas within the micrographs/images using an image analysis technique. Segmentation for the retrieval and subsequent computation of void areas within the micrographs/images is challenging as the gray-scaled values of the void areas are close to the gray-scaled values of the matrix leading to the need ofmanually performing the segmentation based on the histogram of the micrographs/images to retrieve the void areas. The use of an algorithm developed by NASA and based on Fuzzy Reasoning (FR) proved to overcome the difficulty of suitably differentiate void and matrix image areas with similar gray-scaled values leading not only to a more accurate estimation of void areas on composite matrix micrographs but also to a faster void analysis process as the algorithm is fully autonomous. C1 [Dominguez, Jesus A.] QinetiQ North Amer Inc, Kennedy Space Ctr, FL 32899 USA. [Tate, Lanetra C.; Wright, M. Clara; Caraccio, Anne] NASA, Kennedy Space Ctr, FL 32899 USA. RP Dominguez, JA (reprint author), QinetiQ North Amer Inc, Mail Stop ESC 58, Kennedy Space Ctr, FL 32899 USA. EM jesus.a.dominguez@nasa.gov; lanetra.c.tate@nasa.gov; m.clara.wright@nasa.gov; anne.caraccio@nasa.gov FU NASA FX This work was funded under the NASA Composites for Exploration Project and Composite Cryotank Project and the authors would like to acknowledge Air Force Research Laboratory (AFRL), Defense Advanced Research Projects Agency (DARPA) and Boeing for material and technical consultancy. NR 6 TC 0 Z9 0 U1 2 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0929-189X EI 1573-4897 J9 APPL COMPOS MATER JI Appl. Compos. Mater. PD DEC PY 2013 VL 20 IS 6 BP 1125 EP 1134 DI 10.1007/s10443-013-9324-9 PG 10 WC Materials Science, Composites SC Materials Science GA 268WQ UT WOS:000328201800010 ER PT J AU Bachetti, M Rana, V Walton, DJ Barret, D Harrison, FA Boggs, SE Christensen, FE Craig, WW Fabian, AC Furst, F Grefenstette, BW Hailey, CJ Hornschemeier, A Madsen, KK Miller, JM Ptak, AF Stern, D Webb, NA Zhang, WW AF Bachetti, Matteo Rana, Vikram Walton, Dominic J. Barret, Didier Harrison, Fiona A. Boggs, Steven E. Christensen, Finn E. Craig, William W. Fabian, Andrew C. Fuerst, Felix Grefenstette, Brian W. Hailey, Charles J. Hornschemeier, Ann Madsen, Kristin K. Miller, Jon M. Ptak, Andrew F. Stern, Daniel Webb, Natalie A. Zhang, William W. TI THE ULTRALUMINOUS X-RAY SOURCES NGC 1313 X-1 AND X-2: A BROADBAND STUDY WITH NuSTAR AND XMM-Newton SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; stars: black holes; X-rays: individual (NGC 1313 X-1, NGC 1313 X-2); X-rays: stars ID MASS BLACK-HOLES; QUASI-PERIODIC OSCILLATIONS; SUPER-EDDINGTON ACCRETION; ACTIVE GALAXIES; BINARY-SYSTEMS; ESO 243-49; SLIM DISK; VARIABILITY; STATE; SPECTRA AB We present the results of NuSTAR and XMM-Newton observations of the two ultraluminous X-ray sources: NGC 1313 X-1 and X-2. The combined spectral bandpass of the two satellites enables us to produce the first spectrum of X-1 between 0.3 and 30 keV, while X-2 is not significantly detected by NuSTAR above 10 keV. The NuSTAR data demonstrate that X-1 has a clear cutoff above 10 keV, whose presence was only marginally detectable with previous X-ray observations. This cutoff rules out the interpretation of X-1 as a black hole in a standard low/hard state, and it is deeper than predicted for the downturn of a broadened iron line in a reflection-dominated regime. The cutoff differs from the prediction of a single-temperature Comptonization model. Further, a cold disk-like blackbody component at similar to 0.3 keV is required by the data, confirming previous measurements by XMM-Newton only. We observe a spectral transition in X- 2, from a state with high luminosity and strong variability to a lower-luminosity state with no detectable variability, and we link this behavior to a transition from a super-Eddington to a sub-Eddington regime. C1 [Bachetti, Matteo; Barret, Didier; Webb, Natalie A.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Bachetti, Matteo; Barret, Didier; Webb, Natalie A.] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Rana, Vikram; Walton, Dominic J.; Harrison, Fiona A.; Fuerst, Felix; Grefenstette, Brian W.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Fabian, Andrew C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hornschemeier, Ann; Ptak, Andrew F.; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bachetti, M (reprint author), Univ Toulouse, UPS OMP, IRAP, Toulouse, France. EM matteo.bachetti@irap.omp.eu RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337; Madsen, Kristin/0000-0003-1252-4891; Rana, Vikram/0000-0003-1703-8796 FU Centre National d'Etudes Spatiales (CNES); NASA [NNG08FD60C]; National Aeronautics and Space Administration; ESA Member States; NASA FX M.B. wishes to acknowledge the support from the Centre National d'Etudes Spatiales (CNES). This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work also makes use of observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and of observations made by the Chandra X-ray Observatory. For timing analysis and plotting, a set of Python codes making use of the NumPy and Scipy libraries was used. For some plots, we used the Veusz software. The authors wish to thank Olivier Godet and Chris Done for interesting discussions, and the referee Matt Middleton, whose comments and suggestions substantively improved the quality of the manuscript. NR 71 TC 64 Z9 64 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 163 DI 10.1088/0004-637X/778/2/163 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800078 ER PT J AU Bedregal, AG Scarlata, C Henry, AL Atek, H Rafelski, M Teplitz, HI Dominguez, A Siana, B Colbert, JW Malkan, M Ross, NR Martin, CL Dressler, A Bridge, C Hathi, NP Masters, D McCarthy, PJ Rutkowski, MJ AF Bedregal, A. G. Scarlata, C. Henry, A. L. Atek, H. Rafelski, M. Teplitz, H. I. Dominguez, A. Siana, B. Colbert, J. W. Malkan, M. Ross, N. R. Martin, C. L. Dressler, A. Bridge, C. Hathi, N. P. Masters, D. McCarthy, P. J. Rutkowski, M. J. TI HST/WFC3 NEAR-INFRARED SPECTROSCOPY OF QUENCHED GALAXIES AT z similar to 1.5 FROM THE WISP SURVEY: STELLAR POPULATION PROPERTIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: formation; galaxies: high-redshift; galaxies: stellar content; Galaxy: evolution; nfrared: galaxies; surveys ID INITIAL MASS FUNCTION; PASSIVELY EVOLVING GALAXIES; HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; ULTRA-DEEP-FIELD; RED-SEQUENCE; VELOCITY DISPERSION; QUIESCENT GALAXIES; DISTANT CLUSTERS; SIZE EVOLUTION AB We combine Hubble Space Telescope (HST) G102 and G141 near-IR (NIR) grism spectroscopy with HST/WFC3UVIS, HST/WFC3-IR, and Spitzer/IRAC [3.6 mu m] photometry to assemble a sample ofmassive (log(M-star/M-circle dot) similar to 11.0) and quenched (specific star formation rate < 0.01 Gyr-1) galaxies at z similar to 1.5. Our sample of 41 galaxies is the largest with G102+G141 NIR spectroscopy for quenched sources at these redshifts. In contrast to the local universe, z similar to 1.5 quenched galaxies in the high-mass range have a wide range of stellar population properties. We find that their spectral energy distributions (SEDs) are well fitted with exponentially decreasing star formation histories and short star formation timescales (tau <= 100 Myr). Quenched galaxies also show a wide distribution in ages, between 1 and 4 Gyr. In the (u - r)(0)-versus-mass space quenched galaxies have a large spread in rest-frame color at a given mass. Most quenched galaxies populate the z similar to 1.5 red sequence (RS), but an important fraction of them (32%) have substantially bluer colors. Although with a large spread, we find that the quenched galaxies on the RS have older median ages (3.1 Gyr) than the quenched galaxies off the RS (1.5 Gyr). We also show that a rejuvenated SED cannot reproduce the observed stacked spectra of (the bluer) quenched galaxies off the RS. We derive the upper limit on the fraction of massive galaxies on the RS at z similar to 1.5 to be < 43%. We speculate that the young quenched galaxies off the RS are in a transition phase between vigorous star formation at z > 2 and the z similar to 1.5 RS. According to their estimated ages, the time required for quenched galaxies off the RS to join their counterparts on the z similar to 1.5 RS is of the order of similar to 1Gyr. C1 [Bedregal, A. G.; Scarlata, C.; Rutkowski, M. J.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Bedregal, A. G.] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. [Henry, A. L.; Martin, C. L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Henry, A. L.] Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Atek, H.; Colbert, J. W.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Atek, H.] Ecole Polytech Fed Lausanne, Observ Sauverny, Lab Astrophys, CH-1290 Versoix, Switzerland. [Rafelski, M.; Teplitz, H. I.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Dominguez, A.; Siana, B.; Masters, D.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Malkan, M.; Ross, N. R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Dressler, A.; Bridge, C.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Hathi, N. P.; Masters, D.; McCarthy, P. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. RP Bedregal, AG (reprint author), Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. EM alejandro.bedregal@tufts.edu RI Hathi, Nimish/J-7092-2014; OI Hathi, Nimish/0000-0001-6145-5090; Dominguez, Alberto/0000-0002-3433-4610 NR 90 TC 13 Z9 13 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR UNSP 126 DI 10.1088/0004-637X/778/2/126 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800041 ER PT J AU Blain, AW Assef, R Stern, D Tsai, CW Eisenhardt, P Bridge, C Benford, D Jarrett, T Cutri, R Petty, S Wu, JW Wright, EL AF Blain, Andrew W. Assef, Roberto Stern, Daniel Tsai, Chao-Wei Eisenhardt, Peter Bridge, Carrie Benford, Dominic Jarrett, Tom Cutri, Roc Petty, Sara Wu, Jingwen Wright, Edward L. TI WISE DETECTIONS OF KNOWN QSOs AT REDSHIFTS GREATER THAN SIX SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; infrared: galaxies; quasars: general ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; Z QUASAR SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; MIDINFRARED SELECTION; Z-GREATER-THAN-5.7 QUASARS; ADDITIONAL QUASARS; HOST GALAXIES; Z-SIMILAR-TO-6 QUASARS; SPITZER OBSERVATIONS AB We present WISE All-Sky mid-infrared (IR) survey detections of 55% (17/31) of the known QSOs at z > 6 from a range of surveys: the SDSS, the CFHT-LS, FIRST, Spitzer, and UKIDSS. The WISE catalog thus provides a substantial increase in the quantity of IR data available for these sources: 17 are detected in the WISE W1 (3.4 mu m) band, 16 in W2 (4.6 mu m), 3 in W3 (12 mu m), and 0 in W4 (22 mu m). This is particularly important with Spitzer in its warm-mission phase and no faint follow-up capability at wavelengths longward of 5 mu m until the launch of James Webb Space Telescope (JWST). WISE thus provides a useful tool for understanding QSOs found in forthcoming large-area optical/IR sky surveys using PanSTARRS, SkyMapper, VISTA, DES, and LSST. The rest-UV properties of the WISE-detected and the WISE-non-detected samples differ: the detections have brighter i/z-band magnitudes and redder rest-UV colors. This suggests that a more aggressive hunt for very high redshift QSOs by combining WISE W1 and W2 data with red, observed optical colors could be effective at least for a subset of dusty candidate QSOs. Stacking the WISE images of the WISE-non-detected QSOs indicates that they are, on average, significantly fainter than the WISE-detected examples, and are thus not narrowly missing detection in the WISE catalog. The WISE catalog detection of three of our sample in the W3 band indicates that their mid-IR flux can be detected individually, although there is no stacked W3 detection of sources detected in W1 but not W3. Stacking analyses of WISE data for large active galactic nucleus samples will be a useful tool, and high-redshift QSOs of all types will be easy targets for JWST. C1 [Blain, Andrew W.] Univ Leicester, Leicester LE1 7RH, Leics, England. [Assef, Roberto; Stern, Daniel; Tsai, Chao-Wei; Eisenhardt, Peter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bridge, Carrie] CALTECH, Pasadena, CA 91125 USA. [Benford, Dominic] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jarrett, Tom] Univ Cape Town, Dept Astron, ZA-7700 Rondebosch, South Africa. [Cutri, Roc] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Petty, Sara] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Assef, Roberto; Wu, Jingwen; Wright, Edward L.] Univ Calif Los Angeles, Div Astron & Astrophys, Los Angeles, CA 90095 USA. RP Blain, AW (reprint author), Univ Leicester, 1 Univ Rd, Leicester LE1 7RH, Leics, England. EM ab520@le.ac.uk RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 FU National Aeronautics and Space Administration FX We thank the anonymous referee for a careful reading and helpful suggestions. This publication makes use of data products from the Wide-field Infrared Survey Explorer (WISE). WISE is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of both the NASA/IPAC Infrared Science Archive (IRSA) and the NASA/IPAC Extragalactic Database (NED), which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. R.J.A. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. NR 47 TC 16 Z9 16 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 113 DI 10.1088/0004-637X/778/2/113 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800028 ER PT J AU da Costa, E Tsurutani, BT Alves, MV Echer, E Lakhina, GS AF da Costa, Edio, Jr. Tsurutani, Bruce T. Alves, Maria Virginia Echer, Ezequiel Lakhina, Gurbax S. TI CROSS-FIELD DIFFUSION OF ENERGETIC (100 keV to 2 MeV) PROTONS IN INTERPLANETARY SPACE SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffusion; magnetic fields; methods: data analysis; methods: numerical; Sun: heliosphere ID NONLINEAR ALFVEN WAVES; MAGNETIC DECREASES MDS; SOLAR-WIND; COSMIC-RAYS; CHARGED-PARTICLES; DRIVEN SHOCKS; ACCELERATION; HOLES; ULYSSES; DISCONTINUITIES AB Magnetic field magnitude decreases (MDs) are observed in several regions of the interplanetary medium. In this paper, we characterize MDs observed by the Ulysses spacecraft instrumentation over the solar south pole by using magnetic field data to obtain the empirical size, magnetic field MD, and frequency of occurrence distribution functions. The interaction of energetic (100 keV to 2 MeV) protons with these MDs is investigated. Charged particle and MD interactions can be described by a geometrical model allowing the calculation of the guiding center shift after each interaction. Using the distribution functions for the MD characteristics, Monte Carlo simulations are used to obtain the cross-field diffusion coefficients as a function of particle kinetic energy. It is found that the protons under consideration cross-field diffuse at a rate of up to approximate to 11% of the Bohm rate. The same method used in this paper can be applied to other space regions where MDs are observed, once their local features are well known. C1 [da Costa, Edio, Jr.] IFMG, BR-35400000 Ouro Preto, MG, Brazil. [Tsurutani, Bruce T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Alves, Maria Virginia; Echer, Ezequiel] INPE, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [Lakhina, Gurbax S.] Indian Inst Geomagnetism, Navi Mumbai 410218, India. RP da Costa, E (reprint author), IFMG, BR-35400000 Ouro Preto, MG, Brazil. EM edio.junior@ifmg.edu.br RI Alves, Maria Virginia/G-3325-2014; OI Lakhina, Gurbax /0000-0002-8956-486X FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico [140441/2006-9, CNPq/PQ 301233/2011-0, 305373/2012-2]; Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES); Fundacao de Amparo a Pesquisa do Estado de Sao Paulo [2008/01288-0]; National Academy of Sciences, India, for support under NASI-Senior Scientist Platinum Jubilee Fellowship and FAPESP [2012/05397-3] FX The Brazilian authors thank the Brazilian agencies Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq-projects 140441/2006-9, CNPq/PQ 301233/2011-0, and 305373/2012-2), Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES), and Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP-project 2008/01288-0) for financial support. Portions of this research were carried out at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. G.S.L. thanks the National Academy of Sciences, India, for support under NASI-Senior Scientist Platinum Jubilee Fellowship and FAPESP (2012/05397-3) for a Visiting Professor fellowship. NR 32 TC 3 Z9 3 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 180 DI 10.1088/0004-637X/778/2/180 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800095 ER PT J AU Hosokawa, T Yorke, HW Inayoshi, K Omukai, K Yoshida, N AF Hosokawa, Takashi Yorke, Harold W. Inayoshi, Kohei Omukai, Kazuyuki Yoshida, Naoki TI FORMATION OF PRIMORDIAL SUPERMASSIVE STARS BY RAPID MASS ACCRETION SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; cosmology: theory; early universe; galaxies: formation; stars: formation ID BLACK-HOLE FORMATION; MAIN-SEQUENCE STARS; HYDRODYNAMIC MODEL-CALCULATIONS; 1ST STARS; PROTOSTELLAR FEEDBACK; VIRIAL TEMPERATURES; DIRECT COLLAPSE; POPULATION III; SUPERGIANT PROTOSTARS; NONLINEAR PULSATIONS AB Supermassive stars (SMSs) forming via very rapid mass accretion (M* greater than or similar to 0.1M circle dot yr(-1)) could be precursors of supermassive black holes observed beyond a redshift of about six. Extending our previous work, here we study the evolution of primordial stars growing under such rapid mass accretion until the stellar mass reaches 10(4) M-5 circle dot. Our stellar evolution calculations show that a star becomes supermassive while passing through the "supergiant protostar" stage, whereby the star has a very bloated envelope and a contracting inner core. The stellar radius increases monotonically with the stellarmass until similar or equal to 100 AU for M* greater than or similar to 10(4) M circle dot, after which the star begins to slowly contract. Because of the large radius, the effective temperature is always less than 104 K during rapid accretion. The accreting material is thus almost completely transparent to the stellar radiation. Only for M* greater than or similar to 10(5) M circle dot can stellar UV feedback operate and disturb the mass accretion flow. We also examine the pulsation stability of accreting SMSs, showing that the pulsation-driven mass loss does not prevent stellar mass growth. Observational signatures of bloated SMSs should be detectable with future observational facilities such as the James Webb Space Telescope. Our results predict that an inner core of the accreting SMS should suffer from the general relativistic instability soon after the stellar mass exceeds 10(5)M circle dot. An extremely massive black hole should form after the collapse of the inner C1 [Hosokawa, Takashi; Yoshida, Naoki] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Hosokawa, Takashi; Yoshida, Naoki] Univ Tokyo, Res Ctr Early Universe, Tokyo 1130033, Japan. [Hosokawa, Takashi; Yorke, Harold W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Inayoshi, Kohei; Omukai, Kazuyuki] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan. [Omukai, Kazuyuki] Tohoku Univ, Astron Inst, Sendai, Miyagi 9808578, Japan. [Yoshida, Naoki] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan. RP Hosokawa, T (reprint author), Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. EM takashi.hosokawa@phys.s.u-tokyo.ac.jp; hosokwtk@gmail.com FU Fellowship of the Japan Society for the Promotion of Science for Research Abroad; Ministry of Education, Science and Culture of Japan [23.838, 2168407, 21244021, 25287050] FX The authors thank Hideyuki Umeda, Yuichiro Sekiguchi, Neal Turner, Dominik Schleicher, and Francesco Palla for fruitful discussions and comments. T.H. appreciates the support by Fellowship of the Japan Society for the Promotion of Science for Research Abroad. K.I., K.O., and N.Y. are supported by the Grants-in-Aid by the Ministry of Education, Science and Culture of Japan (23.838, 2168407, 21244021, and 25287050). Portions of this work were conducted at the Jet Propulsion Laboratory, California Institute of Technology, operating under a contract with the National Aeronautics and Space Administration (NASA). NR 80 TC 61 Z9 61 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 178 DI 10.1088/0004-637X/778/2/178 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800093 ER PT J AU Hung, CL Sanders, DB Casey, CM Lee, N Barnes, JE Capak, P Kartaltepe, JS Koss, M Larson, KL Le Floc'h, E Lockhart, K Man, AWS Mann, AW Riguccini, L Scoville, N Symeonidis, M AF Hung, Chao-Ling Sanders, D. B. Casey, C. M. Lee, N. Barnes, J. E. Capak, P. Kartaltepe, J. S. Koss, M. Larson, K. L. Le Floc'h, E. Lockhart, K. Man, A. W. S. Mann, A. W. Riguccini, L. Scoville, N. Symeonidis, M. TI THE ROLE OF GALAXY INTERACTION IN THE SFR-M-* RELATION: CHARACTERIZING MORPHOLOGICAL PROPERTIES OF Herschel-SELECTED GALAXIES AT 0.2 < z < 1.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: structure; infrared: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMING GALAXIES; SIMILAR-TO 2; EXTRAGALACTIC LEGACY SURVEY; AEGIS FIELD GALAXIES; SKY LIRG SURVEY; ADVANCED CAMERA; HIGH-REDSHIFT; COSMOS SURVEY; COLD STREAMS AB Galaxy interactions/mergers have been shown to dominate the population of IR-luminous galaxies (L-IR greater than or similar to 10(11.6) L-circle dot) in the local universe (z less than or similar to 0.25). Recent studies based on the relation between galaxies' star formation rates and stellar mass (the SFR-M-* relation or the "galaxy main sequence") have suggested that galaxy interaction/mergers may only become significant when galaxies fall well above the galaxy main sequence. Since the typical SFR at a given M-* increases with redshift, the existence of the galaxy main sequence implies that massive, IR-luminous galaxies at high z may not necessarily be driven by galaxy interactions. We examine the role of galaxy interactions in the SFR-M-* relation by carrying out a morphological analysis of 2084 Herschel-selected galaxies at 0.2 < z < 1.5 in the COSMOS field. Using a detailed visual classification scheme, we show that the fraction of " disk galaxies" decreases and the fraction of " irregular" galaxies increases systematically with increasing LIR out to z less than or similar to 1.5 and z less than or similar to 1.0, respectively. At L-IR > 10(11.5) L-circle dot, greater than or similar to 50% of the objects showevident features of strongly interacting/ merger systems, where this percentage is similar to the studies of local IR-luminous galaxies. The fraction of interacting/merger systems also systematically increases with the deviation from the SFR-M-* relation, supporting the view that galaxies falling above the main sequence are more dominated by mergers than the main-sequence galaxies. Meanwhile, we find that similar to 18% of massive IR-luminous "main-sequence galaxies" are classified as interacting systems, where this population may not evolve through the evolutionary track predicted by a simple gas exhaustion model. C1 [Hung, Chao-Ling; Sanders, D. B.; Casey, C. M.; Lee, N.; Barnes, J. E.; Koss, M.; Larson, K. L.; Lockhart, K.; Man, A. W. S.; Mann, A. W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Capak, P.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Kartaltepe, J. S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Le Floc'h, E.] CEA Saclay, CEA CNRS UP7, UMR AIM, F-91191 Gif Sur Yvette, France. [Man, A. W. S.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-1168 Copenhagen, Denmark. [Riguccini, L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Riguccini, L.] BAER Inst, Santa Rosa, CA USA. [Scoville, N.] CALTECH, Pasadena, CA 91125 USA. [Symeonidis, M.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dept Space & Climate, Dorking RH5 6NT, Surrey, England. RP Hung, CL (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM clhung@ifa.hawaii.edu RI Koss, Michael/B-1585-2015 OI Koss, Michael/0000-0002-7998-9581 FU National Science Foundation [PHY-1066293]; Hubble Fellowship from Space Telescope Science Institute [HST-HF-51268.01-A]; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain) FX C.-L. Hung thanks V. U and J. Chu for their help with visual classification at the early stage of this project. D. B. Sanders and C. M. Casey acknowledge the hospitality of the Aspen Center for Physics, which is supported by the National Science Foundation grant No. PHY-1066293. C. M. Casey is generously supported by a Hubble Fellowship from Space Telescope Science Institute, grant HST-HF-51268.01-A.; PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); and IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; and the Canada-France-Hawaii Telescope operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France, and the University of Hawaii. NR 64 TC 26 Z9 26 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 129 DI 10.1088/0004-637X/778/2/129 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800044 ER PT J AU Inostroza, N Fortenberry, RC Huang, XC Lee, TJ AF Inostroza, Natalia Fortenberry, Ryan C. Huang, Xinchuan Lee, Timothy J. TI ROVIBRATIONAL SPECTROSCOPIC CONSTANTS AND FUNDAMENTAL VIBRATIONAL FREQUENCIES FOR ISOTOPOLOGUES OF CYCLIC AND BENT SINGLET HC2N ISOMERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; circumstellar matter; ISM: lines and bands; ISM: molecules; molecular data; radio lines: ISM ID QUARTIC FORCE-FIELD; ASTRONOMICAL DETECTION; AB-INITIO; LINEAR C3H3+; IDENTIFICATION; MOLECULES; CYCLOPROPENYLIDENE; ENERGIES; SPACE; CH2CN AB Through established, highly accurate ab initio quartic force fields, a complete set of fundamental vibrational frequencies, rotational constants, and rovibrational coupling and centrifugal distortion constants have been determined for both the cyclic 1 (1)A' and bent 2 (1)A' DCCN, (HCCN)-C-13, (HCCN)-C-13, and (HCCN)-N-15 isotopologues of HCCN. Spectroscopic constants are computed for all isotopologues using second-order vibrational perturbation theory (VPT2), and the fundamental vibrational frequencies are computed with VPT2 and vibrational configuration interaction (VCI) theory. Agreement between VPT2 and VCI results is quite good, with the fundamental vibrational frequencies of the bent isomer isotopologues in accord to within a 0.1- 3.2 cm(-1) range. Similar accuracies are present for the cyclic isomer isotopologues. The data generated here serve as a reference for astronomical observations of these closed-shell, highly dipolar molecules using new, high-resolution telescopes and as reference for laboratory studies where isotopic labeling may lead to elucidation of the formation mechanism for the known interstellar molecule: X (3)A' HCCN. C1 [Inostroza, Natalia; Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. RP Inostroza, N (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Timothy.J.Lee@nasa.gov RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013 FU NASA [08-APRA08-0050, 10-APRA10-0096]; Fondecyt [3110007]; Oak Ridge Associated Universities through the NASA Postdoctoral Program; NASA/SETI Institute Cooperative Agreement [NNX12AG96A]; NASA's Laboratory Astrophysics [NNH10ZDA001N] FX This work has been supported by NASA grants 08-APRA08-0050, 10-APRA10-0096, and Fondecyt grant 3110007. Additionally, R.C.F. received support from Oak Ridge Associated Universities through the NASA Postdoctoral Program. NASA/SETI Institute Cooperative Agreement NNX12AG96A has funded the work undertaken by X. H. Support from NASA's Laboratory Astrophysics "Carbon in the Galaxy" Consortium Grant (NNH10ZDA001N) is also gratefully acknowledged. NR 35 TC 4 Z9 4 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 160 DI 10.1088/0004-637X/778/2/160 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800075 ER PT J AU Johnson, TJ Guillemot, L Kerr, M Cognard, I Ray, PS Wolff, MT Begin, S Janssen, GH Romani, RW Venter, C Grove, JE Freire, PCC Wood, M Cheung, CC Casandjian, JM Stairs, IH Camilo, F Espinoza, CM Ferrara, EC Harding, AK Johnston, S Kramer, M Lyne, AG Michelson, PF Ransom, SM Shannon, R Smith, DA Stappers, BW Theureau, G Thorsett, SE AF Johnson, T. J. Guillemot, L. Kerr, M. Cognard, I. Ray, P. S. Wolff, M. T. Begin, S. Janssen, G. H. Romani, R. W. Venter, C. Grove, J. E. Freire, P. C. C. Wood, M. Cheung, C. C. Casandjian, J. M. Stairs, I. H. Camilo, F. Espinoza, C. M. Ferrara, E. C. Harding, A. K. Johnston, S. Kramer, M. Lyne, A. G. Michelson, P. F. Ransom, S. M. Shannon, R. Smith, D. A. Stappers, B. W. Theureau, G. Thorsett, S. E. TI BROADBAND PULSATIONS FROM PSR B1821-24: IMPLICATIONS FOR EMISSION MODELS AND THE PULSAR POPULATION OF M28 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: stars; globular clusters: individual (M28); pulsars: individual (B1821-24) ID LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; GLOBULAR-CLUSTER M28; MILLISECOND PULSARS; X-RAY; LIGHT CURVES; TIMING OBSERVATIONS; SPACE-TELESCOPE; RADIO-EMISSION; NEUTRON-STARS AB We report a 5.4 sigma detection of pulsed gamma rays from PSR B1821-24 in the globular cluster M28 using similar to 44 months of Fermi Large Area Telescope (LAT) data that have been reprocessed with improved instrument calibration constants. We constructed a phase-coherent ephemeris, with post-fit residual rms of 3 mu s, using radio data spanning similar to 23.2 yr, enabling measurements of the multi-wavelength light-curve properties of PSR B1821-24 at the milliperiod level. We fold RXTE observations of PSR B1821-24 from 1996 to 2007 and discuss implications on the emission zones. The gamma-ray light curve consists of two peaks separated by 0.41 +/- 0.02 in phase, with the first gamma-ray peak lagging behind the first radio peak by 0.05 +/- 0.02 in phase, consistent with the phase of giant radio pulses. We observe significant emission in the off-peak interval of PSR B1821-24 with a best-fit LAT position inconsistent with the core of M28. We do not detect significant gamma-ray pulsations at the spin or orbital periods from any other known pulsar in M28, and we place limits on the number of energetic pulsars in the cluster. The derived gamma-ray efficiency, similar to 2%, is typical of other gamma-ray pulsars with comparable spin-down power, suggesting that the measured spin-down rate (2.2 x 10(36) erg s(-1)) is not appreciably distorted by acceleration in the cluster potential. This confirms PSR B1821-24 as the second very energetic millisecond pulsar in a globular cluster and raises the question of whether these represent a separate class of objects that only form in regions of very high stellar density. C1 [Johnson, T. J.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Guillemot, L.; Freire, P. C. C.; Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kerr, M.; Romani, R. W.; Wood, M.; Michelson, P. F.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Kerr, M.; Romani, R. W.; Wood, M.; Michelson, P. F.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Cognard, I.; Theureau, G.] LPCE UMR 6115 CNRS, Lab Phys & Chim Environm, F-45071 Orleans, France. [Cognard, I.] CNRS INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France. [Ray, P. S.; Wolff, M. T.; Grove, J. E.; Cheung, C. C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Begin, S.] Univ Laval, Dept Phys Genie Phys & Opt, Quebec City, PQ, Canada. [Janssen, G. H.; Espinoza, C. M.; Kramer, M.; Lyne, A. G.; Stappers, B. W.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Venter, C.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Casandjian, J. M.] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM,CEA IRFU,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Stairs, I. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Camilo, F.] Arecibo Observ, Arecibo, PR 00612 USA. [Espinoza, C. M.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile. [Ferrara, E. C.; Harding, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Johnston, S.; Shannon, R.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Smith, D. A.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Fradignan, F-33175 Gradignan, France. [Thorsett, S. E.] Willamette Univ, Dept Phys, Salem, OR 97031 USA. RP Johnson, TJ (reprint author), Naval Res Lab, Washington, DC 20375 USA. EM tyrel.j.johnson@gmail.com; guillemo@mpifr-bonn.mpg.de; kerrm@stanford.edu; icognard@cnrs-orleans.fr; Paul.Ray@nrl.navy.mil RI Venter, Christo/E-6884-2011; OI Venter, Christo/0000-0002-2666-4812; Thorsett, Stephen/0000-0002-2025-9613; Shannon, Ryan/0000-0002-7285-6348; Ransom, Scott/0000-0001-5799-9714; Ray, Paul/0000-0002-5297-5278 FU NSERC Discovery Grant; Canada Foundation for Innovation; NASA DPR [S-15633-Y] FX Pulsar research at the University of British Columbia is supported by an NSERC Discovery Grant and by the Canada Foundation for Innovation.; Portions of this research performed at the Naval Research Laboratory are sponsored by NASA DPR S-15633-Y. NR 88 TC 21 Z9 21 U1 2 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR UNSP 106 DI 10.1088/0004-637X/778/2/106 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800021 ER PT J AU Lee, N Sanders, DB Casey, CM Scoville, NZ Hung, CL Le Floc'h, E Ilbert, O Aussel, H Capak, P Kartaltepe, JS Roseboom, I Salvato, M Aravena, M Berta, S Bock, J Oliver, SJ Riguccini, L Symeonidis, M AF Lee, Nicholas Sanders, D. B. Casey, Caitlin M. Scoville, N. Z. Hung, Chao-Ling Le Floc'h, Emeric Ilbert, Olivier Aussel, Herve Capak, Peter Kartaltepe, Jeyhan S. Roseboom, Isaac Salvato, Mara Aravena, M. Berta, S. Bock, J. Oliver, S. J. Riguccini, L. Symeonidis, M. TI MULTI-WAVELENGTH SEDs OF HERSCHEL-SELECTED GALAXIES IN THE COSMOS FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMING GALAXIES; LUMINOUS INFRARED GALAXIES; AZTEC MILLIMETER SURVEY; EVOLUTION SURVEY COSMOS; LESS-THAN 2; HIGH-REDSHIFT; MU-M; ULTRALUMINOUS GALAXIES AB We combine Herschel Photodetector Array Camera and Spectrometer and Spectral and Photometric Imaging Receiver maps of the full 2 deg(2) Cosmic Evolution Survey (COSMOS) field with existing multi-wavelength data to obtain template and model-independent optical-to-far-infrared spectral energy distributions (SEDs) for 4218 Herschel-selected sources with log(L-IR/L-circle dot) = 9.4-13.6 and z = 0.02-3.54. Median SEDs are created by binning the optical to far-infrared (FIR) bands available in COSMOS as a function of infrared luminosity. Herschel probes rest-frame wavelengths where the bulk of the infrared radiation is emitted, allowing us to more accurately determine fundamental dust properties of our sample of infrared luminous galaxies. We find that the SED peak wavelength (lambda(peak)) decreases and the dust mass (M-dust) increases with increasing total infrared luminosity (LIR). In the lowest infrared luminosity galaxies (log(L-IR/L-circle dot) = 10.0-11.5), we see evidence of polycyclic aromatic hydrocarbon (PAH) features (lambda similar to 7-9 mu m), while in the highest infrared luminosity galaxies (L-IR > 10(12) L-circle dot) we see an increasing contribution of hot dust and/or power-law emission, consistent with the presence of heating from an active galactic nucleus (AGN). We study the relationship between stellar mass and star formation rate of our sample of infrared luminous galaxies and find no evidence that Herschel-selected galaxies follow the SFR/M-* "main sequence" as previously determined from studies of optically selected, star-forming galaxies. Finally, we compare the mid-infrared to FIR properties of our infrared luminous galaxies using the previously defined diagnostic, IR8 L-IR/L-8, and find that galaxies with L-IR greater than or similar to 10(11.3) L-circle dot tend to systematically lie above (x3-5) the IR8 "infrared main sequence," suggesting either suppressed PAH emission or an increasing contribution from AGN heating. C1 [Lee, Nicholas; Sanders, D. B.; Casey, Caitlin M.; Hung, Chao-Ling] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Scoville, N. Z.; Capak, Peter; Bock, J.] CALTECH, Pasadena, CA 91125 USA. [Le Floc'h, Emeric; Aussel, Herve] CEA Saclay, UMR AIM CEA CNRS UP7, F-91191 Gif Sur Yvette, France. [Ilbert, Olivier] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Capak, Peter] Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Kartaltepe, Jeyhan S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Roseboom, Isaac; Oliver, S. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Salvato, Mara] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Salvato, Mara] Cluster Excellence, D-85748 Garching, Germany. [Aravena, M.] European So Observ, Vitacura Santiago, Chile. [Aravena, M.] Univ Diego Portales, Fac Engn, Santiago, Chile. [Berta, S.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Riguccini, L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Riguccini, L.] BAER Inst, Santa Rosa, CA USA. [Symeonidis, M.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Lee, N (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. RI Aravena, Manuel/O-2361-2014; OI Casey, Caitlin/0000-0002-0930-6466 FU National Science Foundation [PHY-1066293]; Space Telescope Science Institute [HST-HF-51268.01-A] FX D. B. Sanders and C. M. Casey acknowledge the hospitality of the Aspen Center for Physics, which is supported by the National Science Foundation grant No. PHY-1066293. C. M. Casey is generously supported by a Hubble Fellowship from Space Telescope Science Institute, grant HST-HF-51268.01-A. NR 71 TC 25 Z9 25 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 131 DI 10.1088/0004-637X/778/2/131 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800046 ER PT J AU Lin, L Gogus, E Kaneko, Y Kouveliotou, C AF Lin, Lin Gogus, Ersin Kaneko, Yuki Kouveliotou, Chryssa TI DETAILED INVESTIGATIONS OF THE DIMMEST BURSTS FROM TWO MAGNETARS, SGR J0501+4516 AND SGR J1550-5418 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (SGR J0501+4516, SGR J1550-5418); stars: neutron; X-rays: bursts ID X-RAY PULSAR; MAGNETIZED NEUTRON-STARS; SOFT GAMMA-REPEATERS; 1E 1547.0-5408; SPECTRAL EVOLUTION; EXTENDED EMISSION; RXTE OBSERVATIONS; 2009 OUTBURSTS; DISCOVERY; 1E-1547.0-5408 AB We applied the Bayesian blocks representation technique to search for the dimmest bursts from two magnetars: we identified 320 events from SGR J0501 + 4516 using a deep XMM-Newton observation and 404 bursts from SGR J1550-5418 using two Swift/X-Ray Telescope pointings. The fluence level of our sample for both sources is about one to two orders of magnitude lower than earlier studies. We systematically investigated the morphological characteristics and duration distributions of these bursts, as these properties are directly obtained from their Bayesian blocks profiles. We also studied the spectral behavior of the dimmest bursts, which were grouped based on the morphological types and fluences. Our results helped us further differentiate the spectral nature of very dim bursts from that of the persistent emission, both fitted with physically motivated continuum emission models. Moreover, we generated the differential burst fluence distribution for these two magnetars in the lowest fluence regime. C1 [Lin, Lin; Gogus, Ersin; Kaneko, Yuki] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey. [Kouveliotou, Chryssa] NASA Marshall Space Flight Ctr, Sci & Technol Off, Huntsville, AL 35812 USA. RP Lin, L (reprint author), Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey. EM lin198361@gmail.com FU Turkish Academy of Sciences (TUBA) FX L.L. is funded through the Post-Doctoral Research Fellowship of the Turkish Academy of Sciences (TUBA). L.L. thanks her grandmother Mrs. Liu Shufen for her endless love and support. NR 47 TC 8 Z9 8 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR UNSP 105 DI 10.1088/0004-637X/778/2/105 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800020 ER PT J AU Pereira, TMD Leenaarts, J De Pontieu, B Carlsson, M Uitenbroek, H AF Pereira, T. M. D. Leenaarts, J. De Pontieu, B. Carlsson, M. Uitenbroek, H. TI THE FORMATION OF IRIS DIAGNOSTICS. III. NEAR-ULTRAVIOLET SPECTRA AND IMAGES SO ASTROPHYSICAL JOURNAL LA English DT Article DE radiative transfer; Sun: atmosphere; Sun: chromosphere ID SOLAR OPTICAL TELESCOPE; MG-II; K-LINES; PARTIAL REDISTRIBUTION; RADIATIVE-TRANSFER; MAGNETIC-FIELD; OSCILLATIONS; ATMOSPHERE; PROFILES; DOUBLET AB The Mg II h&k lines are the prime chromospheric diagnostics of NASA's Interface Region Imaging Spectrograph (IRIS). In the previous papers of this series, we used a realistic three-dimensional radiative magnetohydrodynamics model to calculate the h&k lines in detail and investigated how their spectral features relate to the underlying atmosphere. In this work, we employ the same approach to investigate how the h&k diagnostics fare when taking into account the finite resolution of IRIS and different noise levels. In addition, we investigate the diagnostic potential of several other photospheric lines and near-continuum regions present in the near-ultraviolet (NUV) window of IRIS and study the formation of the NUV slit-jaw images. We find that the instrumental resolution of IRIS has a small effect on the quality of the h&k diagnostics; the relations between the spectral features and atmospheric properties are mostly unchanged. The peak separation is the most affected diagnostic, but mainly due to limitations of the simulation. The effects of noise start to be noticeable at a signal-to-noise ratio (S/N) of 20, but we show that with noise filtering one can obtain reliable diagnostics at least down to a S/N of 5. The many photospheric lines present in the NUV window provide velocity information for at least eight distinct photospheric heights. Using line-free regions in the h&k far wings, we derive good estimates of photospheric temperature for at least three heights. Both of these diagnostics, in particular the latter, can be obtained even at S/Ns as low as 5. C1 [Pereira, T. M. D.; Leenaarts, J.; De Pontieu, B.; Carlsson, M.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Pereira, T. M. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Pereira, T. M. D.; De Pontieu, B.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Uitenbroek, H.] NSO Sacramento Peak, Sunspot, NM 88349 USA. RP Pereira, TMD (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, NO-0315 Oslo, Norway. EM tiago.pereira@astro.uio.no; jorritl@astro.uio.no; bdp@lmsal.com; mats.carlsson@astro.uio.no; huitenbroek@nso.edu RI Pereira, Tiago/G-4079-2014; OI Pereira, Tiago/0000-0003-4747-4329; Leenaarts, Jorrit/0000-0003-4936-4211 FU NASA Postdoctoral Program at Ames Research Center [NNH06CC03B]; Research Council of Norway through the grant "Solar Atmospheric Modeling"; European Research Council under the European Union's Seventh Framework Programme [291058]; High End Computing Division of NASA [s1061]; NASA [NNX08AH45G, NNX08BA99G, NNX11AN98G, NNM07AA01C, NNG09FA40C] FX T. M. D. P. was supported by the NASA Postdoctoral Program at Ames Research Center (grant NNH06CC03B). This research was supported by the Research Council of Norway through the grant "Solar Atmospheric Modeling" and through grants of computing time from the Programme for Supercomputing, by the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ ERC grant agreement No. 291058, and by computing project s1061 from the High End Computing Division of NASA. B.D.P. acknowledges support from NASA grants NNX08AH45G, NNX08BA99G, NNX11AN98G, NNM07AA01C (Hinode), and NNG09FA40C (IRIS). We thank the referee for several useful suggestions that improved the manuscript. NR 40 TC 30 Z9 30 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR UNSP 143 DI 10.1088/0004-637X/778/2/143 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800058 ER PT J AU Perley, DA Levan, AJ Tanvir, NR Cenko, SB Bloom, JS Hjorth, J Kruhler, T Filippenko, AV Fruchter, A Fynbo, JPU Jakobsson, P Kalirai, J Milvang-Jensen, B Morgan, AN Prochaska, JX Silverman, JM AF Perley, D. A. Levan, A. J. Tanvir, N. R. Cenko, S. B. Bloom, J. S. Hjorth, J. Kruhler, T. Filippenko, A. V. Fruchter, A. Fynbo, J. P. U. Jakobsson, P. Kalirai, J. Milvang-Jensen, B. Morgan, A. N. Prochaska, J. X. Silverman, J. M. TI A POPULATION OF MASSIVE, LUMINOUS GALAXIES HOSTING HEAVILY DUST-OBSCURED GAMMA-RAY BURSTS: IMPLICATIONS FOR THE USE OF GRBs AS TRACERS OF COSMIC STAR FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies: star formation; gamma-ray burst: general; ISM: structure ID SIMILAR-TO 2; DIGITAL SKY SURVEY; SPITZER-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; LYMAN BREAK GALAXIES; CORE-COLLAPSE SUPERNOVAE; HIGH-METALLICITY HOST; DEEP-FIELD-SOUTH; FORMING GALAXIES; STELLAR MASS AB We present observations and analysis of the host galaxies of 23 heavily dust-obscured gamma-ray bursts (GRBs) observed by the Swift satellite during the years 2005-2009, representing all GRBs with an unambiguous host-frame extinction of AV >1 mag from this period. Deep observations with Keck, Gemini, Very Large Telescope, Hubble Space Telescope, and Spitzer successfully detect the host galaxies and establish spectroscopic or photometric redshifts for all 23 events, enabling us to provide measurements of the intrinsic host star formation rates, stellar masses, and mean extinctions. Compared to the hosts of unobscured GRBs at similar redshifts, we find that the hosts of dust-obscured GRBs are (on average) more massive by about an order of magnitude and also more rapidly star forming and dust obscured. While this demonstrates that GRBs populate all types of star-forming galaxies, including the most massive, luminous systems at z approximate to 2, at redshifts below 1.5 the overall GRB population continues to show a highly significant aversion to massive galaxies and a preference for low-mass systems relative to what would be expected given a purely star-formation-rate-selected galaxy sample. This supports the notion that the GRB rate is strongly dependent on metallicity, and may suggest that the most massive galaxies in the universe underwent a transition in their chemical properties similar to 9 Gyr ago. We also conclude that, based on the absence of unobscured GRBs in massive galaxies and the absence of obscured GRBs in low-mass galaxies, the dust distributions of the lowest-mass and the highest-mass galaxies are relatively homogeneous, while intermediate-mass galaxies (similar to 10(9)M(circle dot)) have diverse internal properties. C1 [Perley, D. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Cenko, S. B.; Bloom, J. S.; Filippenko, A. V.; Morgan, A. N.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hjorth, J.; Kruhler, T.; Fynbo, J. P. U.; Milvang-Jensen, B.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Fruchter, A.; Kalirai, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Jakobsson, P.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Prochaska, J. X.] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Silverman, J. M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Perley, DA (reprint author), CALTECH, Dept Astron, MC 249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA. EM dperley@astro.caltech.edu RI Fynbo, Johan/L-8496-2014; Hjorth, Jens/M-5787-2014; Jakobsson, Pall/L-9950-2015; OI Fynbo, Johan/0000-0002-8149-8298; Hjorth, Jens/0000-0002-4571-2306; Jakobsson, Pall/0000-0002-9404-5650; Kruehler, Thomas/0000-0002-8682-2384 FU NASA [HST-HF-51296.01-A]; Space Telescope Science Institute (STScI); Danish National Science Foundation; ERC-StG grant [EGGS-278202]; European Commission; Gary & Cynthia Bengier; NASA/Swift [NNX10AI21G, NNX12AD73G, NNX07AE94G, NNX12AD74G, NNX08AN84G]; TABASGO Foundation; NSF [AST-1211916]; Association of Universities for Research in Astronomy, Inc., under NASA [NAS 5-26555]; HST programs [GO-11840, GO-12378, GO-12674]; Harvard University Milton Fund; SAO; UC Berkeley; [GO-10908]; [11343]; [11840]; [12307]; [12378]; [12764]; [12949]; [GN-2006A-Q-14]; [GN-2006B-Q-21]; [GN-2007A-Q-19]; [GS-2008A-Q-20]; [GN-2007B-Q-99]; [GN-2008B-Q-6]; [GN-2009A-Q-26]; [GN-2009A-Q-84]; [GN-2010A-C-8]; [GN-2010B-C-2] FX Support for this work was provided by NASA through Hubble Fellowship grant HST-HF-51296.01-A awarded by the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., for NASA, under contract NAS 5-26555. The Dark Cosmology Centre is supported by the Danish National Science Foundation. J.P.U.F. and B.M.J. acknowledge support from ERC-StG grant EGGS-278202. T.K. acknowledges support by the European Commission under the Marie Curie Intra-European Fellowship Programme in FP7. A.V.F. and his group acknowledge generous financial assistance from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, the Christopher R. Redlich Fund, NASA/Swift grants NNX10AI21G and NNX12AD73G, the TABASGO Foundation, and NSF grant AST-1211916. J.X.P. acknowledges support from NASA/Swift grants NNX07AE94G and NNX12AD74G.; This work is based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs GO-10908, 11343, 11840, 12307, 12378, 12764, and 12949. Support for HST programs GO-11840, GO-12378, and GO-12674 was provided by NASA through a grant from STScI, which is operated by AURA, Inc., under NASA contract NAS 5-26555. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Partial support for this work was provided by NASA through an award issued by JPL/Caltech. It is also based in part on observations obtained at the Gemini Observatory, which is operated by AURA, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the NSF (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inova,cao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). Observations were acquired under Program IDs GN-2006A-Q-14, GN-2006B-Q-21, GN-2007A-Q-19, GS-2008A-Q-20, GN-2007B-Q-99, GN-2008B-Q-6, GN-2009A-Q-26, GN-2009A-Q-84, GN-2010A-C-8, and GN-2010B-C-2. PAIRITEL is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, a camera loan from the University of Virginia, and continued support of the SAO and UC Berkeley. The PAIRITEL project is further supported by NASA/Swift Guest Investigator grant NNX08AN84G. NR 235 TC 68 Z9 68 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 128 DI 10.1088/0004-637X/778/2/128 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800043 ER PT J AU Raymond, JC Ghavamian, P Williams, BJ Blair, WP Borkowski, KJ Gaetz, TJ Sankrit, R AF Raymond, John C. Ghavamian, Parviz Williams, Brian J. Blair, William P. Borkowski, Kazimierz J. Gaetz, Terrance J. Sankrit, Ravi TI GRAIN DESTRUCTION IN A SUPERNOVA REMNANT SHOCK WAVE SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: individual objects (Cygnus Loop); ISM: supernova remnants; shock waves; ultraviolet: ISM ID LARGE-MAGELLANIC-CLOUD; COSMIC ORIGINS SPECTROGRAPH; CYGNUS-LOOP; DUST DESTRUCTION; INTERSTELLAR-MEDIUM; CHEMICAL-COMPOSITION; NONRADIATIVE SHOCKS; ELEMENTS HYDROGEN; INFRARED-EMISSION; OPTICAL-EMISSION AB Dust grains are sputtered away in the hot gas behind shock fronts in supernova remnants (SNRs), gradually enriching the gas phase with refractory elements. We have measured emission in C IV lambda 1550 from C atoms sputtered from dust in the gas behind a non-radiative shock wave in the northern Cygnus Loop. Overall, the intensity observed behind the shock agrees approximately with predictions from model calculations that match the Spitzer 24 mu m and the X-ray intensity profiles. Thus, these observations confirm the overall picture of dust destruction in SNR shocks and the sputtering rates used in models. However, there is a discrepancy in that the C IV intensity 10 '' behind the shock is too high compared with the intensities at the shock and 25 '' behind it. Variations in the density, hydrogen neutral fraction, and the dust properties over parsec scales in the pre-shock medium limit our ability to test dust destruction models in detail. C1 [Raymond, John C.; Gaetz, Terrance J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ghavamian, Parviz] Towson Univ, Dept Phys Astron & Geosci, Towson, MD 21252 USA. [Williams, Brian J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Borkowski, Kazimierz J.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Sankrit, Ravi] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. RP Raymond, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jraymond@cfa.harvard.edu FU NASA [NAS8-03060]; [HST-GO-12885]; [HST-GO-12545.08] FX This work was performed under grant HST-GO-12885 to the Smithsonian Astrophysical Observatory. P.G was supported under grant HST-GO-12545.08 and T.J.G. acknowledges support under NASA contract NAS8-03060. NR 53 TC 9 Z9 9 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 161 DI 10.1088/0004-637X/778/2/161 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800076 ER PT J AU Tinker, JL Leauthaud, A Bundy, K George, MR Behroozi, P Massey, R Rhodes, J Wechsler, RH AF Tinker, Jeremy L. Leauthaud, Alexie Bundy, Kevin George, Matthew R. Behroozi, Peter Massey, Richard Rhodes, Jason Wechsler, Risa H. TI EVOLUTION OF THE STELLAR-TO-DARK MATTER RELATION: SEPARATING STAR-FORMING AND PASSIVE GALAXIES FROM z=1 TO 0 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: halos ID HALO OCCUPATION DISTRIBUTION; DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; LUMINOUS RED GALAXIES; INITIAL MASS FUNCTION; LARGE-SCALE STRUCTURE; FIELD GALAXIES; REDSHIFT SURVEY; FORMATION HISTORIES; COMPREHENSIVE ANALYSIS AB We use measurements of the stellar mass function, galaxy clustering, and galaxy-galaxy lensing within the COSMOS survey to constrain the stellar-to-halo mass relation (SHMR) of star forming and quiescent galaxies over the redshift range z = [0.2,1.0]. For massive galaxies, M* >= 10(10.6) M-circle dot, our results indicate that star-forming galaxies grow proportionately as fast as their dark matter halos while quiescent galaxies are outpaced by dark matter growth. At lower masses, there is minimal difference in the SHMRs, implying that the majority low-mass quiescent galaxies have only recently been quenched of their star formation. Our analysis also affords a breakdown of all COSMOS galaxies into the relative numbers of central and satellite galaxies for both populations. At z = 1, satellite galaxies dominate the red sequence below the knee in the stellar mass function. But the number of quiescent satellites exhibits minimal redshift evolution; all evolution in the red sequence is due to low-mass central galaxies being quenched of their star formation. At M* similar to 10(10) M-circle dot , the fraction of central galaxies on the red sequence increases by a factor of 10 over our redshift baseline, while the fraction of quenched satellite galaxies at that mass is constant with redshift. We define a "migration rate" to the red sequence as the time derivative of the passive galaxy abundances. We find that the migration rate of central galaxies to the red sequence increases by nearly an order of magnitude from z = 1 to z = 0. These results imply that the efficiency of quenching star formation for centrals is increasing with cosmic time, while the mechanisms that quench the star formation of satellite galaxies in groups and clusters is losing efficiency. C1 [Tinker, Jeremy L.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Leauthaud, Alexie; Bundy, Kevin] Univ Tokyo, Todai Inst Adv Study, WPI, Kavli IPMU, Kashiwa, Chiba 2778583, Japan. [George, Matthew R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [George, Matthew R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Behroozi, Peter; Wechsler, Risa H.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Behroozi, Peter; Wechsler, Risa H.] SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Massey, Richard] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Rhodes, Jason] CALTECH, Pasadena, CA 91125 USA. [Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tinker, JL (reprint author), NYU, Dept Phys, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. EM jeremy.tinker@nyu.edu FU World Premier International Research Center Initiative (WPI Initiative); MEXT, Japan; NASA [HST-GO-09822] FX We thank the referee for many helpful comments and suggestions that have improved this work. This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We wish to thank Tony Roman, Denise Taylor, and David Soderblom for their assistance in planning and scheduling of the extensive COSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at http://cosmos.astro.caltech.edu/. It is a pleasure the acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman and John Good) in providing online archive and server capabilities for the COSMOS data-sets. NR 103 TC 46 Z9 46 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 93 DI 10.1088/0004-637X/778/2/93 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800008 ER PT J AU Wang, SX Brandt, WN Luo, B Smail, I Alexander, DM Danielson, ALR Hodge, JA Karim, A Lehmer, BD Simpson, JM Swinbank, AM Walter, F Wardlow, JL Xue, YQ Chapman, SC Coppin, KEK Dannerbauer, H De Breuck, C Menten, KM van der Werf, P AF Wang, S. X. Brandt, W. N. Luo, B. Smail, I. Alexander, D. M. Danielson, A. L. R. Hodge, J. A. Karim, A. Lehmer, B. D. Simpson, J. M. Swinbank, A. M. Walter, F. Wardlow, J. L. Xue, Y. Q. Chapman, S. C. Coppin, K. E. K. Dannerbauer, H. De Breuck, C. Menten, K. M. van der Werf, P. TI AN ALMA SURVEY OF SUBMILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD-SOUTH: THE AGN FRACTION AND X-RAY PROPERTIES OF SUBMILLIMETER GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: high-redshift; galaxies: starburst; submillimeter: galaxies; X-rays: galaxies; X-rays: general ID ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; DEGREE EXTRAGALACTIC SURVEY; SUPERMASSIVE BLACK-HOLES; POINT-SOURCE CATALOGS; MS SOURCE CATALOGS; SIMILAR-TO 1; HIGH-REDSHIFT; PHOTOMETRIC REDSHIFTS AB The large gas and dust reservoirs of submillimeter galaxies (SMGs) could potentially provide ample fuel to trigger an active galactic nucleus (AGN), but previous studies of the AGN fraction in SMGs have been controversial largely due to the inhomogeneity and limited angular resolution of the available submillimeter surveys. Here we set improved constraints on the AGN fraction and X-ray properties of the SMGs with Atacama Large Millimeter/submillimeter Array (ALMA) and Chandra observations in the Extended Chandra Deep Field-South (E-CDF-S). This study is the first among similar works to have unambiguously identified the X-ray counterparts of SMGs; this is accomplished using the fully submillimeter-identified, statistically reliable SMG catalog with 99 SMGs from the ALMA LABOCA E-CDF-S Submillimeter Survey. We found 10 X-ray sources associated with SMGs (median redshift z = 2.3), of which eight were identified as AGNs using several techniques that enable cross-checking. The other two X-ray detected SMGs have levels of X-ray emission that can be plausibly explained by their star formation activity. Six of the eight SMG-AGNs are moderately/highly absorbed, with N-H > 10(23) cm(-2). An analysis of the AGN fraction, taking into account the spatial variation of X-ray sensitivity, yields an AGN fraction of 17(-6)(+16)% for AGNs with rest-frame 0.5-8 keV absorption-corrected luminosity >= 7.8 x 10(42.) erg s(-1); we provide estimated AGN fractions as a function of X-ray flux and luminosity. ALMA's high angular resolution also enables direct X-ray stacking at the precise positions of SMGs for the first time, and we found four potential SMG-AGNs in our stacking sample. C1 [Wang, S. X.; Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Smail, I.; Alexander, D. M.; Danielson, A. L. R.; Karim, A.; Simpson, J. M.; Swinbank, A. M.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Hodge, J. A.; Walter, F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Karim, A.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Lehmer, B. D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Lehmer, B. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wardlow, J. L.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Xue, Y. Q.] Univ Sci & Technol China, Chinese Acad Sci, Dept Astron, Key Lab Res Galaxies & Cosmol,Ctr Astrophys, Hefei 230026, Anhui, Peoples R China. [Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Coppin, K. E. K.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys, Hatfield AL10 9AB, Herts, England. [Dannerbauer, H.] Univ Vienna, Inst Astrophys, A-1180 Vienna, Austria. [De Breuck, C.] European So Observ, D-85748 Garching, Germany. [Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Wang, SX (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM xxw131@psu.edu; niel@astro.psu.edu RI Smail, Ian/M-5161-2013; Wardlow, Julie/C-9903-2015; Brandt, William/N-2844-2015; OI Smail, Ian/0000-0003-3037-257X; Wardlow, Julie/0000-0003-2376-8971; Brandt, William/0000-0002-0167-2453; De Breuck, Carlos/0000-0002-6637-3315; Alexander, David/0000-0002-5896-6313 FU SAO [AR3-14015X]; HST [GO-12866.01-A]; NASA ADP [NNX11AJ59G]; ACIS Instrument Team [SV4-74018]; STFC [ST/I001573/1]; Leverhulme Fellowship; ERC Advanced Investigator program [DUSTYGAL 321334]; Royal Society/Wolfson Merit Award; Leverhulme Trust; STFC studentship; STFC as well as the Collaborative Research Council 956; Deutsche Forschungsgemeinschaft; Thousand Young Talents (QingNian-QianRen) program [KJ2030220004]; USTC startup funding [ZC9850290195]; National Natural Science Foundation of China [NSFC-11243008] FX We gratefully acknowledge financial support from SAO grant AR3-14015X (S.X.W., W.N.B., B.L.), HST grant GO-12866.01-A (S.X.W., W.N.B., B.L.), NASA ADP grant NNX11AJ59G (S.X.W., W.N.B., B.L.), and ACIS Instrument Team contract SV4-74018 (S.X.W., W.N.B., B.L.). I.R.S.acknowledges support from STFC (ST/I001573/1), a Leverhulme Fellowship, the ERC Advanced Investigator program DUSTYGAL 321334, and a Royal Society/Wolfson Merit Award. We also acknowledge financial support from the Leverhulme Trust (DMA), the STFC (DMA), STFC studentship (ALRD). A.K.acknowledges support from STFC as well as the Collaborative Research Council 956 funded by the Deutsche Forschungsgemeinschaft (DFG). Y.Q.X.acknowledges the financial support of the Thousand Young Talents (QingNian-QianRen) program (KJ2030220004), USTC startup funding (ZC9850290195), and the National Natural Science Foundation of China through NSFC-11243008. NR 152 TC 34 Z9 34 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 179 DI 10.1088/0004-637X/778/2/179 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800094 ER PT J AU Wicks, RT Roberts, DA Mallet, A Schekochihin, AA Horbury, TS Chen, CHK AF Wicks, R. T. Roberts, D. A. Mallet, A. Schekochihin, A. A. Horbury, T. S. Chen, C. H. K. TI CORRELATIONS AT LARGE SCALES AND THE ONSET OF TURBULENCE IN THE FAST SOLAR WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); plasmas; solar wind; turbulence ID RADIAL EVOLUTION; MAGNETIC-FIELD; MHD TURBULENCE; ALFVEN WAVES; STREAM STRUCTURE; RESIDUAL ENERGY; 1/F NOISE; FLUCTUATIONS; DEPENDENCE; SPECTRA AB We show that the scaling of structure functions of magnetic and velocity fields in a mostly highly Alfvenic fast solar wind stream depends strongly on the joint distribution of the dimensionless measures of cross helicity and residual energy. Already at very low frequencies, fluctuations that are both more balanced (cross helicity similar to 0) and equipartitioned (residual energy similar to 0) have steep structure functions reminiscent of "turbulent" scalings usually associated with the inertial range. Fluctuations that are magnetically dominated (residual energy similar to -1), and so have closely anti-aligned Elsasser-field vectors, or are imbalanced (cross helicity similar to 1), and so have closely aligned magnetic and velocity vectors, have wide "1/f" ranges typical of fast solar wind. We conclude that the strength of nonlinear interactions of individual fluctuations within a stream, diagnosed by the degree of correlation in direction and magnitude of magnetic and velocity fluctuations, determines the extent of the 1/f region observed, and thus the onset scale for the turbulent cascade. C1 [Wicks, R. T.; Roberts, D. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Mallet, A.; Schekochihin, A. A.] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England. [Horbury, T. S.] Univ London Imperial Coll Sci Technol & Med, Space & Atmospher Phys Grp, London SW7 2AZ, England. [Chen, C. H. K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Wicks, RT (reprint author), NASA, Goddard Space Flight Ctr, Code 672, Greenbelt, MD USA. EM robert.t.wicks@nasa.gov RI Wicks, Robert/A-1180-2009 OI Wicks, Robert/0000-0002-0622-5302 FU NASA Postdoctoral Program at the Goddard Space Flight Center; STFC; NASA [NNN06AA01C, NAS5-02099]; Leverhulme Trust Network for Magnetized Plasma Turbulence FX This research was supported by the NASA Postdoctoral Program at the Goddard Space Flight Center (R.T.W.); STFC (A.M., T.S.H.); NASA contracts NNN06AA01C and NAS5-02099 (C.H.K.C.); and the Leverhulme Trust Network for Magnetized Plasma Turbulence. Wind data were obtained from the SPDF Web site http://spdf.gsfc.nasa.gov. NR 34 TC 10 Z9 10 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2013 VL 778 IS 2 AR 177 DI 10.1088/0004-637X/778/2/177 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 262UH UT WOS:000327762800092 ER PT J AU Ackermann, M Ajello, M Allafort, A Atwood, WB Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Belfiore, A Bellazzini, R Bernieri, E Bissaldi, E Bloom, ED Bonamente, E Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Burnett, TH Buson, S Caliandro, GA Cameron, RA Campana, R Caraveo, PA Casandjian, JM Cavazzuti, E Cecchi, C Charles, E Chaves, RCG Chekhtman, A Cheung, CC Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Cominsky, LR Conrad, J Cutini, S D'Ammando, F De Angelis, A De Palma, F Dermer, CD Desiante, R Digel, SW Di Venere, L Drell, PS Drlica-Wagner, A Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Fortin, P Franckowiak, A Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giommi, P Giordano, F Giroletti, M Godfrey, G Gomez-Vargas, GA Grenier, IA Guiriec, S Hadasch, D Hanabata, Y Harding, AK Hayashida, M Hays, E Hewitt, J Hill, AB Horan, D Hughes, RE Jogler, T Johannesson, G Johnson, AS Johnson, TJ Johnson, WN Kamae, T Kataoka, J Kawano, T Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Lemoine-Goumard, M Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Massaro, E Mayer, M Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mizuno, T Moiseev, AA Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nemmen, R Nuss, E Ohsugi, T Okumura, A Orienti, M Ormes, JF Paneque, D Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Porter, TA Raino, S Razzano, M Reimer, A Reimer, O Reposeur, T Ritz, S Romani, RW Roth, M Parkinson, PMS Schulz, A Sgro, C Siskind, EJ Smith, DA Spandre, G Spinelli, P Stawarz, L Strong, AW Suson, DJ Takahashi, H Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Torres, DF Tosti, G Troja, E Uchiyama, Y Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Werner, M Winer, BL Wood, KS Wood, M AF Ackermann, M. Ajello, M. Allafort, A. Atwood, W. B. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Belfiore, A. Bellazzini, R. Bernieri, E. Bissaldi, E. Bloom, E. D. Bonamente, E. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Burnett, T. H. Buson, S. Caliandro, G. A. Cameron, R. A. Campana, R. Caraveo, P. A. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Charles, E. Chaves, R. C. G. Chekhtman, A. Cheung, C. C. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Cominsky, L. R. Conrad, J. Cutini, S. D'Ammando, F. De Angelis, A. De Palma, F. Dermer, C. D. Desiante, R. Digel, S. W. Di Venere, L. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Fortin, P. Franckowiak, A. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Godfrey, G. Gomez-Vargas, G. A. Grenier, I. A. Guiriec, S. Hadasch, D. Hanabata, Y. Harding, A. K. Hayashida, M. Hays, E. Hewitt, J. Hill, A. B. Horan, D. Hughes, R. E. Jogler, T. Johannesson, G. Johnson, A. S. Johnson, T. J. Johnson, W. N. Kamae, T. Kataoka, J. Kawano, T. Knodlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lemoine-Goumard, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Massaro, E. Mayer, M. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nemmen, R. Nuss, E. Ohsugi, T. Okumura, A. Orienti, M. Ormes, J. F. Paneque, D. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Porter, T. A. Raino, S. Razzano, M. Reimer, A. Reimer, O. Reposeur, T. Ritz, S. Romani, R. W. Roth, M. Parkinson, P. M. Saz Schulz, A. Sgro, C. Siskind, E. J. Smith, D. A. Spandre, G. Spinelli, P. Stawarz, Lukasz Strong, A. W. Suson, D. J. Takahashi, H. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Uchiyama, Y. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Werner, M. Winer, B. L. Wood, K. S. Wood, M. TI THE FIRST FERMI-LAT CATALOG OF SOURCES ABOVE 10 GeV SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; gamma rays: general ID LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; PULSAR WIND NEBULA; BLIND FREQUENCY SEARCHES; NANCAY RADIO TELESCOPE; SUPERNOVA REMNANT; SPACE-TELESCOPE; MILLISECOND PULSARS; CRAB PULSAR; MULTIWAVELENGTH OBSERVATIONS AB We present a catalog of gamma-ray sources at energies above 10 GeV based on data from the Large Area Telescope (LAT) accumulated during the first 3 yr of the Fermi Gamma-ray Space Telescope mission. The first Fermi catalog of > 10 GeV sources (1FHL) has 514 sources. For each source we present location, spectrum, a measure of variability, and associations with cataloged sources at other wavelengths. We found that 449 (87%) could be associated with known sources, of which 393 (76% of the 1FHL sources) are active galactic nuclei. Of the 27 sources associated with known pulsars, we find 20 (12) to have significant pulsations in the range > 10 GeV (> 25 GeV). In this work we also report that, at energies above 10 GeV, unresolved sources account for 27% +/- 8% of the isotropic. gamma-ray background, while the unresolved Galactic population contributes only at the few percent level to the Galactic diffuse background. We also highlight the subset of the 1FHL sources that are best candidates for detection at energies above 50-100 GeV with current and future ground-based gamma-ray observatories. C1 [Ackermann, M.; Buehler, R.; Mayer, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Allafort, A.; Bechtol, K.; Bloom, E. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Funk, S.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Okumura, A.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Allafort, A.; Bechtol, K.; Bloom, E. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Funk, S.; Godfrey, G.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Okumura, A.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Atwood, W. B.; Belfiore, A.; Ritz, S.; Parkinson, P. M. 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[Brigida, M.; De Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; De Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; De Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Burnett, T. H.; Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Campana, R.] INAF IASF Bologna, I-40129 Bologna, Italy. [Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Giommi, P.] ASI, Sci Data Ctr, I-00044 Frascati, Roma, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Cheung, C. C.; Dermer, C. D.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Roma, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, F-34095 Montpellier, France. [Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Conrad, J.; Larsson, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.; Larsson, S.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden. [D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [De Angelis, A.; Drlica-Wagner, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [De Angelis, A.; Drlica-Wagner, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Fortin, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Gomez-Vargas, G. A.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. [Gomez-Vargas, G. A.] Univ Autonoma Madrid, Inst Fis Teor IFT UAM CSIC, E-28049 Madrid, Spain. [Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Hanabata, Y.; Hayashida, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Johnson, T. J.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Kawano, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Knodlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knodlseder, J.] Univ Toulouse, GAHEC, IRAP, UPS OMP, F-31028 Toulouse, France. [Paneque, D.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Lemoine-Goumard, M.; Lott, B.; Mehault, J.; Reposeur, T.; Smith, D. A.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, IN2P3, CNRS, F-33175 Gradignan, France. [Massaro, E.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA. [Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Murgia, S.] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA. [Okumura, A.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Parkinson, P. M. Saz] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Stawarz, Lukasz] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Stawarz, Lukasz] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Schulz, A.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Torres, D. F.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain. [Gomez-Vargas, G. A.] ICREA, E-08010 Barcelona, Spain. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM digel@stanford.edu; fortin@veritas.sao.arizona.edu; dpaneque@mppmu.mpg.de RI Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Gomez-Vargas, German/C-7138-2015; Campana, Riccardo/F-5272-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Torres, Diego/O-9422-2016; Di Venere, Leonardo/C-7619-2017; OI orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; Campana, Riccardo/0000-0002-4794-5453; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Bissaldi, Elisabetta/0000-0001-9935-8106; Torres, Diego/0000-0002-1522-9065; Di Venere, Leonardo/0000-0003-0703-824X; giommi, paolo/0000-0002-2265-5003; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Hill, Adam/0000-0003-3470-4834; Bastieri, Denis/0000-0002-6954-8862; Pesce-Rollins, Melissa/0000-0003-1790-8018 NR 131 TC 85 Z9 87 U1 1 U2 25 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2013 VL 209 IS 2 AR UNSP 34 DI 10.1088/0067-0049/209/2/34 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266YG UT WOS:000328059500016 ER PT J AU Ashby, MLN Stanford, SA Brodwin, M Gonzalez, AH Martinez-Manso, J Bartlett, JG Benson, BA Bleem, LE Crawford, TM Dey, A Dressler, A Eisenhardt, PRM Galametz, A Jannuzi, BT Marrone, DP Mei, S Muzzin, A Pacaud, F Pierre, M Stern, D Vieira, JD AF Ashby, M. L. N. Stanford, S. A. Brodwin, M. Gonzalez, A. H. Martinez-Manso, J. Bartlett, J. G. Benson, B. A. Bleem, L. E. Crawford, T. M. Dey, A. Dressler, A. Eisenhardt, P. R. M. Galametz, A. Jannuzi, B. T. Marrone, D. P. Mei, S. Muzzin, A. Pacaud, F. Pierre, M. Stern, D. Vieira, J. D. TI THE SPITZER SOUTH POLE TELESCOPE DEEP FIELD: SURVEY DESIGN AND INFRARED ARRAY CAMERA CATALOGS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies: clusters: general; infrared: galaxies; surveys ID IRAC SHALLOW SURVEY; GALAXY CLUSTERS; SUNYAEV-ZELDOVICH; SPACE-TELESCOPE; MASS FRACTIONS; SKY; PERFORMANCE; MODEL; GAS; CALIBRATION AB The Spitzer South Pole Telescope Deep Field (SSDF) is a wide-area survey using Spitzer's Infrared Array Camera (IRAC) to cover 94 deg(2) of extragalactic sky, making it the largest IRAC survey completed to date outside the Milky Way midplane. The SSDF is centered at (alpha, delta) = (23:30, -55:00), in a region that combines observations spanning a broad wavelength range from numerous facilities. These include millimeter imaging from the South Pole Telescope, far-infrared observations from Herschel/SPIRE, X-ray observations from the XMM XXL survey, near-infrared observations from the VISTA Hemisphere Survey, and radio-wavelength imaging from the Australia Telescope Compact Array, in a panchromatic project designed to address major outstanding questions surrounding galaxy clusters and the baryon budget. Here we describe the Spitzer/IRAC observations of the SSDF, including the survey design, observations, processing, source extraction, and publicly available data products. In particular, we present two band-merged catalogs, one for each of the two warm IRAC selection bands. They contain roughly 5.5 and 3.7 million distinct sources, the vast majority of which are galaxies, down to the SSDF 5 sigma sensitivity limits of 19.0 and 18.2 Vega mag (7.0 and 9.4 mu Jy) at 3.6 and 4.5 mu m, respectively. C1 [Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Gonzalez, A. H.; Martinez-Manso, J.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Bartlett, J. G.] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA IRFU, F-75205 Paris 13, France. [Benson, B. A.; Bleem, L. E.; Crawford, T. M.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Crawford, T. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Dey, A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Dressler, A.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Eisenhardt, P. R. M.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Galametz, A.] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Jannuzi, B. T.; Marrone, D. P.] Univ Arizona, Dept Astron, Tucson, AZ 85719 USA. [Jannuzi, B. T.; Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA. [Mei, S.] Observ Paris, GEPI, Sect Meudon, F-92190 Meudon, France. [Mei, S.] Univ Paris Denis Diderot, F-75205 Paris 13, France. [Mei, S.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Muzzin, A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Pacaud, F.] Argelander Inst Astron, D-53121 Bonn, Germany. [Pierre, M.] CEA, DSM, AIM IRFU, Serv Astrophys, F-91190 Gif Sur Yvette, France. [Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. RP Ashby, MLN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mashby@cfa.harvard.edu OI Marrone, Daniel/0000-0002-2367-1080 FU NASA [1439357]; U. S. Department of Energy, National Nuclear Security Administration [DE-AC52-07NA27344]; Deutches Zenturm fur Luft-und Raumfahrt (DLR) [50 OR 1117] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration (NASA). Support was provided by NASA through contract number 1439357 issued by JPL/Caltech. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. Lawrence Livermore National Laboratory is operated by Lawrence Livermore National Security, LLC, for the U. S. Department of Energy, National Nuclear Security Administration under Contract DE-AC52-07NA27344. F.P. acknowledges support from grant 50 OR 1117 of the Deutches Zenturm fur Luft-und Raumfahrt (DLR). We thank Dave Nair for his efforts in characterizing a preliminary reduction of the SSDF images. We also thank Richard G. Arendt, who kindly computed the Milky Way star count models shown in Figure 8. NR 45 TC 16 Z9 16 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2013 VL 209 IS 2 AR UNSP 22 DI 10.1088/0067-0049/209/2/22 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266YG UT WOS:000328059500004 ER PT J AU Grupe, D Nousek, JA Veres, P Zhang, BB Gehrels, N AF Grupe, Dirk Nousek, John A. Veres, Peter Zhang, Bin-Bin Gehrels, Neil TI EVIDENCE FOR NEW RELATIONS BETWEEN GAMMA-RAY BURST PROMPT AND X-RAY AFTERGLOW EMISSION FROM 9 YEARS OF SWIFT SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; gamma-ray burst: general ID LIGHT CURVES; LUMINOSITY FUNCTION; COMPLETE SAMPLE; COMPREHENSIVE ANALYSIS; ENERGY INJECTION; XRT DATA; REDSHIFT DISTRIBUTION; STATISTICAL-ANALYSIS; SPECTRAL EVOLUTION; PHYSICAL ORIGINS AB When a massive star explodes as a gamma-ray burst (GRB), information about the explosion is retained in the properties of the prompt and afterglow emission. We report on new relations between the prompt and X-ray afterglow emission of Swift-detected GRBs found from Burst Alert Telescope (BAT) and X-Ray Telescope data covering 2004 December to 2013 August (754 in total). These relations suggest that the prompt and afterglow emission are closely linked. In particular, we find very strong correlations between the BAT 15-150 keV T-90 and the break times before and after the plateau phase in the 0.3-10 keV X-ray afterglow light curves. We also find a strong anticorrelation between the photon index of the GRB prompt emission and the X-ray spectral slope of the afterglow. Moreover, anticorrelations exist between the rest-frame peak energy in the prompt emission E-peak,E-z and the X-ray afterglow decay slope during the plateau phase and the break times after the plateau phase. The rest-frame break times before and after the plateau phase are also anticorrelated with the rest-frame 15-150 keV luminosity and the isotropic energy during the prompt emission. A principal component analysis suggests that the GRB properties are primarily driven by the luminosity/energy release in the 15-150 keV band. Luminosity functions derived at different redshifts from a log N-log S analysis indicate that the density of bright bursts is significantly lower in the local universe than in the universe at z approximate to 3, where the density of bright GRBs peaks. Using cluster analysis, we find that the duration of BAT-detected short GRBs is less than 1 s. We also present a catalog of all Swift onboard-detected bursts. C1 [Grupe, Dirk; Nousek, John A.] Swift Mission Operat Ctr, State Coll, PA 16801 USA. [Grupe, Dirk; Nousek, John A.; Veres, Peter; Zhang, Bin-Bin] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Zhang, Bin-Bin] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Gehrels, Neil] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. RP Grupe, D (reprint author), Swift Mission Operat Ctr, 2582 Gateway Dr, State Coll, PA 16801 USA. EM dgrupe007@gmail.com FU NASA [NNX13AH50G]; OTKA [K077795]; NASA Swift program [NAS5-00136] FX We would like to thank all observers at ground-based optical telescopes for their efforts to obtain redshifts from Swift after-glows. We would also like to thank the anonymous referee for detailed and supportive reports. We thank Raffaella Margutti for discussions about the PCA in her 2013 paper. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center, Italy; data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA Goddard Space Flight Center; and data supplied by the UK Swift Science Data Centre at the University of Leicester. P. V. acknowledges NASA grant NNX13AH50G and OTKA grant K077795 and thanks Peter Meszaros for discussions. At Penn State we acknowledge support from the NASA Swift program through contract NAS5-00136. NR 138 TC 15 Z9 15 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2013 VL 209 IS 2 AR UNSP 20 DI 10.1088/0067-0049/209/2/20 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 266YG UT WOS:000328059500002 ER PT J AU Prud'homme, G Dobbin, NA Sun, L Burnett, RT Martin, RV Davidson, A Cakmak, S Villeneuve, PJ Lamsal, LN van Donkelaar, A Peters, PA Johnson, M AF Prud'homme, Genevieve Dobbin, Nina A. Sun, Liu Burnett, Richard T. Martin, Randall V. Davidson, Andrew Cakmak, Sabit Villeneuve, Paul J. Lamsal, Lok N. van Donkelaar, Aaron Peters, Paul A. Johnson, Markey TI Comparison of remote sensing and fixed-site monitoring approaches for examining air pollution and health in a national study population SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Air pollution; Satellite remote sensing; Regulatory monitoring; Asthma; Allergy; Population health; Epidemiology ID LONG-TERM EXPOSURE; FINE PARTICULATE MATTER; AMERICAN-CANCER-SOCIETY; NITROGEN-DIOXIDE; CHILDHOOD ASTHMA; PUBLIC-HEALTH; CARDIOVASCULAR-DISEASE; UNITED-STATES; PROMISED LAND; QUALITY AB Satellite remote sensing (RS) has emerged as a cutting edge approach for estimating ground level ambient air pollution. Previous studies have reported a high correlation between ground level PM2.5 and NO2 estimated by RS and measurements collected at regulatory monitoring sites. The current study examined associations between air pollution and adverse respiratory and allergic health outcomes using multi-year averages of NO2 and PM2.5 from RS and from regulatory monitoring. RS estimates were derived using satellite measurements from OMI, MODIS, and MISR instruments. Regulatory monitoring data were obtained from Canada's National Air Pollution Surveillance Network. Self-reported prevalence of doctor-diagnosed asthma, current asthma, allergies, and chronic bronchitis were obtained from the Canadian Community Health Survey (a national sample of individuals 12 years of age and older). Multi-year ambient pollutant averages were assigned to each study participant based on their six digit postal code at the time of health survey, and were used as a marker for long-term exposure to air pollution. RS derived estimates of NO2 and PM2.5 were associated with 6-10% increases in respiratory and allergic health outcomes per interquartile range (3.97 mu g m(-3) for PM2.5 and 1.03 ppb for NO2) among adults (aged 20-64) in the national study population. Risk estimates for air pollution and respiratory/allergic health outcomes based on RS were similar to risk estimates based on regulatory monitoring for areas where regulatory monitoring data were available (within 40 km of a regulatory monitoring station). RS derived estimates of air pollution were also associated with adverse health outcomes among participants residing outside the catchment area of the regulatory monitoring network (p < 0.05). The consistency between risk estimates based on RS and regulatory monitoring as well as the associations between air pollution and health among participants living outside the catchment area for regulatory monitoring suggest that RS can provide useful estimates of long-term ambient air pollution in epidemiologic studies. This is particularly important in rural communities and other areas where monitoring and modeled air pollution data are limited or unavailable. Crown Copyright (C) 2013 Published by Elsevier Ltd. All rights reserved. C1 [Prud'homme, Genevieve; Dobbin, Nina A.; Sun, Liu; Johnson, Markey] Hlth Canada, Air Hlth Sci Div, Ottawa, ON K1A 0K9, Canada. [Burnett, Richard T.; Cakmak, Sabit; Villeneuve, Paul J.] Hlth Canada, Populat Studies Div, Ottawa, ON K1A 0K9, Canada. [Martin, Randall V.; van Donkelaar, Aaron] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Davidson, Andrew] Agr & Agri Food Canada, Earth Observat Serv, Ottawa, ON, Canada. [Davidson, Andrew] Carleton Univ, Dept Geog & Environm Studies, Ottawa, ON K1S 5B6, Canada. [Villeneuve, Paul J.] Carleton Univ, Inst Hlth Sci Technol & Policy, Ottawa, ON K1S 5B6, Canada. [Villeneuve, Paul J.] Univ Toronto, Dalla Lana Sch Publ Hlth, Toronto, ON, Canada. [Lamsal, Lok N.] Univ Space Res Assoc, Columbia, MD USA. [Lamsal, Lok N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Peters, Paul A.] STAT Canada, Hlth Anal Div, Ottawa, ON, Canada. RP Johnson, M (reprint author), Hlth Canada, Water & Air Qual Bur, Air Hlth Sci Div, 269 Laurier Ave West,Room 4-039, Ottawa, ON K1A 0K9, Canada. EM markey.johnson@hc-sc.gc.ca RI Mashamba-Thompson, Tivani /B-6087-2014; Martin, Randall/C-1205-2014; OI Martin, Randall/0000-0003-2632-8402; Cakmak, Sabit/0000-0001-9921-2107; Peters, Paul/0000-0001-5225-2005 NR 90 TC 4 Z9 5 U1 2 U2 51 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2013 VL 80 BP 161 EP 171 DI 10.1016/j.atmosenv.2013.07.020 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 267JV UT WOS:000328094800017 ER PT J AU Baker, KR Misenis, C Obland, MD Ferrare, RA Scarino, AJ Kelly, JT AF Baker, Kirk R. Misenis, Chris Obland, Michael D. Ferrare, Richard A. Scarino, Amy J. Kelly, James T. TI Evaluation of surface and upper air fine scale WRF meteorological modeling of the May and June 2010 CalNex period in California SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE WRF; California; CalNex; HSRL; South Coast; San Joaquin ID ATMOSPHERIC BOUNDARY-LAYER; NONLOCAL CLOSURE-MODEL; LOW-LEVEL WINDS; PART I; HYDROLOGY MODEL; QUALITY MODELS; AEROSOL; SENSITIVITY; VALLEY; OZONE AB Prognostic meteorological models such as Mesoscale Model (MM5) and Weather Research and Forecasting (WRF) are often used to supply inputs for retrospective air quality modeling done to support ozone and PM2.5 emission control demonstrations. In this study, multiple configurations of the WRF model are applied at 4 km grid resolution and compared to routine meteorological measurements and special study measurements taken in California during May-June 2010. One configuration is routinely used by US EPA to generate meteorological inputs for regulatory air quality modeling and another that is used by research scientists for evaluating meteorology and air quality. Mixing layer heights estimated from airborne High Spectral Resolution Lidar (HSRL) measurements of aerosol backscatter are compared with WRF modeled planetary boundary layer (PBL) height estimates. Both WRF configurations generally capture the variability in HSRL mixing height between days, hour-to-hour, and between surface features such as terrain and land water interfaces. Fractional bias over all flights and both model configurations range from -38% to 32% and fractional error ranges from 22% to 58%. Surface and upper level measurements of temperature, water mixing ratio, and winds are generally well characterized by both WRF model configurations, often more closely matching surface observations than the input analysis data (12-NAM). The WRF model generally captures orographic and mesoscale meteorological features in the central Valley (bifurcation of wind flow from the San Francisco bay into the Sacramento and San Joaquin valleys) and Los Angeles air basin (ocean-land flows) during this summer period. Published by Elsevier Ltd. C1 [Baker, Kirk R.; Misenis, Chris; Kelly, James T.] US EPA, Res Triangle Pk, NC 27711 USA. [Obland, Michael D.; Ferrare, Richard A.; Scarino, Amy J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Scarino, Amy J.] Sci Syst & Applicat Inc, Hampton, VA USA. RP Baker, KR (reprint author), US EPA, Res Triangle Pk, NC 27711 USA. EM baker.kirk@epa.gov RI Kelly, James/F-8135-2010 OI Kelly, James/0000-0001-6574-5714 FU NASA HQ Science Mission Directorate Radiation Sciences Program [B-200/HSRL]; NASA CALIPSO project; DOE ASR Program [DE-AI02-05ER63985]; NASA [B-200]; HSRL FX The authors appreciate the contribution from Robert Gilliam, Lara Reynolds, Brian Eder, Pat Dolwick, and Ann Marie Carlton. The authors thank the NASA B-200 and HSRL teams for the outstanding work in support of the CALNEX mission. Funding for the B-200/HSRL deployment and investigations came from the NASA HQ Science Mission Directorate Radiation Sciences Program, the NASA CALIPSO project, and the DOE ASR Program, via Interagency Agreement No. DE-AI02-05ER63985. NR 40 TC 20 Z9 20 U1 1 U2 36 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2013 VL 80 BP 299 EP 309 DI 10.1016/j.atmosenv.2013.08.006 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 267JV UT WOS:000328094800032 ER PT J AU Hsu, A Reuben, A Shindell, D de Sherbinin, A Levy, M AF Hsu, Angel Reuben, Aaron Shindell, Drew de Sherbinin, Alex Levy, Marc TI Toward the next generation of air quality monitoring indicators SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Air pollution; Indicators; Ozone; Particulate matter; Persistent Organic Pollutants; Mercury ID POLLUTION; INFORMATION; KNOWLEDGE; EXPOSURE; IMPACTS; INDEXES; MATTER; POLICY; WORLD AB This paper introduces an initiative to bridge the state of scientific knowledge on air pollution with the needs of policymakers and stakeholders to design the "next generation" of air quality indicators. As a first step this initiative assesses current monitoring and modeling associated with a number of important pollutants with an eye toward identifying knowledge gaps and scientific needs that are a barrier to reducing air pollution impacts on human and ecosystem health across the globe. Four outdoor air pollutants were considered particulate matter, ozone, mercury, and Persistent Organic Pollutants (POPS) because of their clear adverse impacts on human and ecosystem health and because of the availability of baseline data for assessment for each. While other papers appearing in this issue will address each pollutant separately, this paper serves as a summary of the initiative and presents recommendations for needed investments to provide improved measurement, monitoring, and modeling data for policy-relevant indicators. The ultimate goal of this effort is to enable enhanced public policy responses to air pollution by linking improved data and measurement methods to decision-making through the development of indicators that can allow policymakers to better understand the impacts of air pollution and, along with source attribution based on modeling and measurements, facilitate improved policies to solve it. The development of indicators represents a crucial next step in this process. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Hsu, Angel] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Reuben, Aaron] Yale Ctr Environm Law & Policy, New Haven, CT 06511 USA. [Shindell, Drew] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [de Sherbinin, Alex; Levy, Marc] Columbia Univ, Earth Inst, Ctr Int Earth Sci Informat Network, Palisades, NY 10964 USA. RP Hsu, A (reprint author), Yale Univ, Sch Forestry & Environm Studies, 195 Prospect St, New Haven, CT 06511 USA. EM angel.hsu@yale.edu; aaron.reuben@gmail.com; drew.t.shindell@nasa.gov; alex.desherbinin@ciesin.columbia.edu; marc.levy@ciesin.columbia.edu RI Shindell, Drew/D-4636-2012; OI de Sherbinin, Alex/0000-0002-8875-4864; Levy, Marc/0000-0002-1111-2222 NR 38 TC 9 Z9 9 U1 0 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2013 VL 80 BP 561 EP 570 DI 10.1016/j.atmosenv.2013.07.036 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 267JV UT WOS:000328094800062 ER PT J AU Ponchak, GE AF Ponchak, George E. TI SPECIAL ISSUE ON 2013 INTERNATIONAL MICROWAVE SYMPOSIUM SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES LA English DT Editorial Material C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Ponchak, GE (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 0 TC 0 Z9 0 U1 1 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9480 EI 1557-9670 J9 IEEE T MICROW THEORY JI IEEE Trans. Microw. Theory Tech. PD DEC PY 2013 VL 61 IS 12 BP 4292 EP 4292 DI 10.1109/TMTT.2013.2288892 PG 1 WC Engineering, Electrical & Electronic SC Engineering GA 265LB UT WOS:000327952100032 ER PT J AU Backhaus, S Bent, R Bono, J Lee, R Tracey, B Wolpert, D Xie, DP Yildiz, Y AF Backhaus, Scott Bent, Russell Bono, James Lee, Ritchie Tracey, Brendan Wolpert, David Xie, Dongping Yildiz, Yildiray TI Cyber-Physical Security: A Game Theory Model of Humans Interacting Over Control Systems SO IEEE TRANSACTIONS ON SMART GRID LA English DT Article DE Power system security; SCADA system; voltage control AB Recent years have seen increased interest in the design and deployment of smart grid devices and control algorithms. Each of these smart communicating devices represents a potential access point for an intruder spurring research into intruder prevention and detection. However, no security measures are complete, and intruding attackers will compromise smart grid devices leading to the attacker and the system operator interacting via the grid and its control systems. The outcome of these machine-mediated human-human interactions will depend on the design of the physical and control systems mediating the interactions. If these outcomes can be predicted via simulation, they can be used as a tool for designing attack-resilient grids and control systems. However, accurate predictions require good models of not just the physical and control systems, but also of the human decision making. In this manuscript, we present an approach to develop such tools, i.e., models of the decisions of the cyber-physical intruder who is attacking the systems and the system operator who is defending it, and demonstrate its usefulness for design. C1 [Backhaus, Scott; Bent, Russell; Wolpert, David] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Bono, James; Xie, Dongping] Amer Univ, Washington, DC 20016 USA. [Lee, Ritchie; Yildiz, Yildiray] NASA Ames, Mountain View, CA 94035 USA. [Tracey, Brendan] Stanford Univ, Stanford, CA 94305 USA. RP Backhaus, S (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA. OI Backhaus, Scott/0000-0002-0344-6791; Bent, Russell/0000-0002-7300-151X NR 24 TC 11 Z9 13 U1 8 U2 37 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1949-3053 J9 IEEE T SMART GRID JI IEEE Trans. Smart Grid PD DEC PY 2013 VL 4 IS 4 BP 2320 EP 2327 DI 10.1109/TSG.2013.2270291 PG 8 WC Engineering, Electrical & Electronic SC Engineering GA 266ZT UT WOS:000328064100060 ER PT J AU Brainard, RE Weijerman, M Eakin, CM Mcelhany, P Miller, MW Patterson, M Piniak, GA Dunlap, MJ Birkeland, C AF Brainard, Russell E. Weijerman, Mariska Eakin, C. Mark Mcelhany, Paul Miller, Margaret W. Patterson, Matt Piniak, Gregory A. Dunlap, Matthew J. Birkeland, Charles TI Incorporating Climate and Ocean Change into Extinction Risk Assessments for 82 Coral Species SO CONSERVATION BIOLOGY LA English DT Article DE Climate and ocean change; coral; data-limited species; extinction risk; ESA; risk assessment ID REEF CORALS; ACIDIFICATION; VULNERABILITY; IMPACTS; LIMITS AB Many marine invertebrate species facing potential extinction have uncertain taxonomies and poorly known demographic and ecological traits. Uncertainties are compounded when potential extinction drivers are climate and ocean changes whose effects on even widespread and abundant species are only partially understood. The U.S. Endangered Species Act mandates conservation management decisions founded on the extinction risk to species based on the best available science at the time of considerationrequiring prompt action rather than awaiting better information. We developed an expert-opinion threat-based approach that entails a structured voting system to assess extinction risk from climate and ocean changes and other threats to 82 coral species for which population status and threat response information was limited. Such methods are urgently needed because constrained budgets and manpower will continue to hinder the availability of desired data for many potentially vulnerable marine species. Significant species-specific information gaps and uncertainties precluded quantitative assessments of habitat loss or population declines and necessitated increased reliance on demographic characteristics and threat vulnerabilities at genus or family levels. Adapting some methods (e.g., a structured voting system) used during other assessments and developing some new approaches (e.g., integrated assessment of threats and demographic characteristics), we rated the importance of threats contributing to coral extinction risk and assessed those threats against population status and trend information to evaluate each species' extinction risk over the 21st century. This qualitative assessment resulted in a ranking with an uncertainty range for each species according to their estimated likelihood of extinction. We offer guidance on approaches for future biological extinction risk assessments, especially in cases of data-limited species likely to be affected by global-scale threats. C1 [Brainard, Russell E.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96814 USA. [Weijerman, Mariska; Dunlap, Matthew J.] Univ Hawaii Manoa, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA. [Eakin, C. Mark] NOAA, Ctr Satellite Applicat & Res, Data & Informat Serv, NOAA Coral Reef Watch, College Pk, MD 20737 USA. [Mcelhany, Paul] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA. [Miller, Margaret W.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Miami, FL 33149 USA. [Patterson, Matt] South Florida Inventory & Monitoring Network, Natl Pk Serv, Miami, FL 33157 USA. [Piniak, Gregory A.] NOAA, Natl Ctr Coastal Ocean Sci, Natl Ocean Serv, Silver Spring, MD 20910 USA. [Birkeland, Charles] Univ Hawaii Manoa, Dept Biol, Honolulu, HI 96822 USA. RP Brainard, RE (reprint author), NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, 1125B Ala Moana Blvd, Honolulu, HI 96814 USA. EM rusty.brainard@noaa.gov RI Eakin, C. Mark/F-5585-2010 NR 47 TC 4 Z9 4 U1 6 U2 77 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD DEC PY 2013 VL 27 IS 6 BP 1169 EP 1178 DI 10.1111/cobi.12171 PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 259ZH UT WOS:000327564300006 PM 24299083 ER PT J AU Mcclure, MM Alexander, M Borggaard, D Boughton, D Crozier, L Griffis, R Jorgensen, JC Lindley, ST Nye, J Rowland, MJ Seney, EE Snover, A Toole, C Van Houtan, K AF Mcclure, Michelle M. Alexander, Michael Borggaard, Diane Boughton, David Crozier, Lisa Griffis, Roger Jorgensen, Jeffrey C. Lindley, Steven T. Nye, Janet Rowland, Melanie J. Seney, Erin E. Snover, Amy Toole, Christopher Van Houtan, Kyle TI Incorporating Climate Science in Applications of the U.S. Endangered Species Act for Aquatic Species SO CONSERVATION BIOLOGY LA English DT Article DE climate change; conservation planning; effects analysis; population models; recovery planning; risk assessment; vulnerability ID CHANGING CLIMATE; SOCKEYE-SALMON; PACIFIC SALMON; CHINOOK SALMON; RIVER-BASIN; IMPACTS; CONSERVATION; OCEAN; SCENARIOS; EVOLUTIONARY AB Aquatic species are threatened by climate change but have received comparatively less attention than terrestrial species. We gleaned key strategies for scientists and managers seeking to address climate change in aquatic conservation planning from the literature and existing knowledge. We address 3 categories of conservation effort that rely on scientific analysis and have particular application under the U.S. Endangered Species Act (ESA): assessment of overall risk to a species; long-term recovery planning; and evaluation of effects of specific actions or perturbations. Fewer data are available for aquatic species to support these analyses, and climate effects on aquatic systems are poorly characterized. Thus, we recommend scientists conducting analyses supporting ESA decisions develop a conceptual model that links climate, habitat, ecosystem, and species response to changing conditions and use this model to organize analyses and future research. We recommend that current climate conditions are not appropriate for projections used in ESA analyses and that long-term projections of climate-change effects provide temporal context as a species-wide assessment provides spatial context. In these projections, climate change should not be discounted solely because the magnitude of projected change at a particular time is uncertain when directionality of climate change is clear. Identifying likely future habitat at the species scale will indicate key refuges and potential range shifts. However, the risks and benefits associated with errors in modeling future habitat are not equivalent. The ESA offers mechanisms for increasing the overall resilience and resistance of species to climate changes, including establishing recovery goals requiring increased genetic and phenotypic diversity, specifying critical habitat in areas not currently occupied but likely to become important, and using adaptive management. C1 [Mcclure, Michelle M.; Crozier, Lisa; Jorgensen, Jeffrey C.] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA. [Alexander, Michael] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA. [Borggaard, Diane] NOAA, Natl Marine Fisheries Serv, Northeast Reg Off, Gloucester, MA 01930 USA. [Boughton, David; Lindley, Steven T.] NOAA, Natl Marine Fisheries Serv, Southwest Fisheries Sci Ctr, Santa Cruz, CA 95060 USA. [Griffis, Roger; Seney, Erin E.] NOAA, Natl Marine Fisheries Serv, Off Sci & Technol, Silver Spring, MD 20910 USA. [Nye, Janet] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA. [Rowland, Melanie J.] NOAA, Off Gen Counsel, Northwest Sect, Seattle, WA USA. [Rowland, Melanie J.] Melanie J Rowland Consulting, Twisp, WA 98856 USA. [Seney, Erin E.] Erin Seney Consulting LLC, Woodbridge, VA 22192 USA. [Snover, Amy] Univ Washington, Climate Impacts Grp, Seattle, WA 98105 USA. [Toole, Christopher] NOAA, Natl Marine Fisheries Serv, Portland, OR 97232 USA. [Van Houtan, Kyle] NOAA, Natl Marine Fisheries Serv, Pacific Islands Sci Ctr, Honolulu, HI 96814 USA. [Van Houtan, Kyle] Duke Univ, Nicholas Sch Environm & Earth Sci, Durham, NC 27708 USA. RP Mcclure, MM (reprint author), NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, 2725 Montlake Blvd, Seattle, WA 98112 USA. EM michelle.mcclure@noaa.gov RI Lindley, Steven/G-3997-2014; McClure, Michelle/O-7853-2015; Alexander, Michael/A-7097-2013; OI Lindley, Steven/0000-0001-9556-0411; McClure, Michelle/0000-0003-4791-8719; Alexander, Michael/0000-0001-9646-6427; Van Houtan, Kyle/0000-0001-5725-1773 NR 64 TC 16 Z9 16 U1 2 U2 32 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD DEC PY 2013 VL 27 IS 6 BP 1222 EP 1233 DI 10.1111/cobi.12166 PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 259ZH UT WOS:000327564300011 PM 24299088 ER PT J AU Menzies, T Brady, A Keung, J Hihn, J Williams, S El-Rawas, O Green, P Boehm, B AF Menzies, Tim Brady, Adam Keung, Jacky Hihn, Jairus Williams, Steven El-Rawas, Oussama Green, Phillip Boehm, Barry TI Learning Project Management Decisions: A Case Study with Case-Based Reasoning versus Data Farming SO IEEE TRANSACTIONS ON SOFTWARE ENGINEERING LA English DT Article DE Search-based software engineering; case-based reasoning; data farming; COCOMO ID SOFTWARE COST ESTIMATION; STATIC CODE ATTRIBUTES; ESTIMATION MODELS; DEFECT PREDICTORS; SELECTION; VALIDATION; SIZE AB Background: Given information on just a few prior projects, how do we learn the best and fewest changes for current projects? Aim: To conduct a case study comparing two ways to recommend project changes. 1) Data farmers use Monte Carlo sampling to survey and summarize the space of possible outcomes. 2) Case-based reasoners (CBR) explore the neighborhood around test instances. Method: We applied a state-of-the data farmer (SEESAW) and a CBR tool (W2) to software project data. Results: CBR with W2 was more effective than SEESAW's data farming for learning best and recommended project changes, effectively reducing runtime, effort, and defects. Further, CBR with W2 was comparably easier to build, maintain, and apply in novel domains, especially on noisy data sets. Conclusion: Use CBR tools like W2 when data are scarce or noisy or when project data cannot be expressed in the required form of a data farmer. Future Work: This study applied our own CBR tool to several small data sets. Future work could apply other CBR tools and data farmers to other data (perhaps to explore other goals such as, say, minimizing maintenance effort). C1 [Menzies, Tim; Brady, Adam; El-Rawas, Oussama; Green, Phillip] W Virginia Univ, Lane Dept Comp Sci & Elect Engn, Morgantown, WV 26506 USA. [Keung, Jacky] City Univ Hong Kong, Dept Comp Sci, Kowloon, Hong Kong, Peoples R China. [Hihn, Jairus] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Williams, Steven] Indiana Univ, Sch Informat & Comp, Bloomington, IN USA. [Boehm, Barry] Univ So Calif, Los Angeles, CA 90089 USA. RP Menzies, T (reprint author), W Virginia Univ, Lane Dept Comp Sci & Elect Engn, Morgantown, WV 26506 USA. EM tim@menzies.us; adam.m.brady@gmail.com; jacky.keung@cityu.edu.hk; jairus.hihn@jpl.nasa.gov; stevencwilliams@gmail.com; orawas@gmail.com; deathcheese@yahoo.com; boehm@sunset.usc.edu FU US National Science Foundation (NSF), CISE [0810879] FX This research was conducted at West Virginia University, the University of Southern California, and the NASA Jet Propulsion Laboratory under a NASA subcontract. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the US Government. This research was funded in part by the US National Science Foundation (NSF), CISE, project #0810879. NR 100 TC 2 Z9 2 U1 3 U2 22 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 0098-5589 EI 1939-3520 J9 IEEE T SOFTWARE ENG JI IEEE Trans. Softw. Eng. PD DEC PY 2013 VL 39 IS 12 BP 1698 EP 1713 DI 10.1109/TSE.2013.43 PG 16 WC Computer Science, Software Engineering; Engineering, Electrical & Electronic SC Computer Science; Engineering GA 260PO UT WOS:000327607000005 ER PT J AU Scully, RR Lam, CW James, JT AF Scully, Robert R. Lam, Chiu-Wing James, John T. TI Estimating safe human exposure levels for lunar dust using benchmark dose modeling of data from inhalation studies in rats SO INHALATION TOXICOLOGY LA English DT Article DE Benchmark dose; biomarker; inhalation; lunar dust; mineral dust; toxicity ID PARTICLE-SIZE; CRYSTALLINE SILICA; VARIABLE ENTITY; QUARTZ HAZARD; TOXICITY; INFLAMMATION; NANOSCALE; CELLS AB The pulmonary toxicity of airborne lunar dust was assessed in rats exposed by nose-only inhalation to 0, 2.1, 6.8, 20.8 and 60.6 mg/m(3) of respirable size lunar dust. Rats were exposed for 6 h/d, 5 d/week, for 4 weeks (120 h). Biomarkers of toxicity were assessed in bronchial alveolar lavage fluid (BALF) collected at 1 d, 1 week, 4 weeks or 13 weeks post-exposure for a total of 76 endpoints. Benchmark dose (BMD) analysis was conducted on endpoints that appeared to be sensitive to dose. The number of endpoints that met criteria for modeling was 30. This number was composed of 13 endpoints that produced data suitable for parametric analysis and 17 that produced non-normal data. Mean BMD values determined from models generated from non-normal data were lower but not significantly different from the mean BMD of models derived from normally distributed data. Thus BMDs ranged from a minimum of 10.4 (using the average BMD from all 30 modeled endpoints) to a maximum of 16.6 (using the average BMD from the most restricted set of models). This range of BMDs yields safe exposure estimate (SEE) values of 0.6 and 0.9 mg/m(3), respectively, when BMDs are extrapolated to humans, using a species factor of 3 and extrapolated from a 1-month exposure to an anticipated 6-month lunar surface exposure. This estimate is very similar to a no-observable-adverse-effect-level (NOAEL) determined from the same studies (0.4 mg/m(3)) and a SEE derived from a study of rats that were intratracheally instilled with lunar dusts (0.5-1.0 mg/m(3)). C1 [Scully, Robert R.; Lam, Chiu-Wing] Wyle Sci Technol & Engn Grp, Houston, TX USA. [James, John T.] NASA, Johnson Space Ctr, Space Toxicol Off, Houston, TX USA. RP Scully, RR (reprint author), Mail Code Wyle HAC-W7,1290 Hercules Ave, Houston, TX 77058 USA. EM robert.r.scully@nasa.gov FU NASA Human Research Program FX This project was funded by the NASA Human Research Program. The authors report no conflicts of interest. The exposure limits are proposals. They are not NASA's official exposure standard for lunar dust. NR 46 TC 3 Z9 3 U1 0 U2 9 PU INFORMA HEALTHCARE PI LONDON PA TELEPHONE HOUSE, 69-77 PAUL STREET, LONDON EC2A 4LQ, ENGLAND SN 0895-8378 EI 1091-7691 J9 INHAL TOXICOL JI Inhal. Toxicol. PD DEC PY 2013 VL 25 IS 14 BP 785 EP 793 DI 10.3109/08958378.2013.849315 PG 9 WC Toxicology SC Toxicology GA 264OZ UT WOS:000327889900004 PM 24304305 ER PT J AU Konishi, C Mudawar, I Hasan, MM AF Konishi, Christopher Mudawar, Issam Hasan, Mohammad M. TI Investigation of localized dryout versus CHF in saturated flow boiling SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER LA English DT Article DE Flow boiling; Critical heat flux; Flow orientation ID CRITICAL HEAT-FLUX; CHANNEL COOLING SCHEME; TRIGGER MECHANISM; BODY FORCE; MODEL; WALL; JET; ORIENTATION; SINGLE; MICROGRAVITY AB Determining flow boiling critical heat flux (CHF) using mechanistic models or empirical correlations requires careful validation with the aid of reliable databases. But, while many new databases are being made available in the literature, the methods used to detect CHF vary greatly, producing different CHF estimates for the same fluid and operating conditions. The variations in detection method are the result of both heated wall design and criteria used to terminate an experiment in response to wall temperature excursions. This study investigates the interfacial phenomena preceding the occurrence of CHF for flow boiling with a finite inlet vapor void. Experiments are conducted with FC-72 in a rectangular channel that is heated along one side. Temporal records of the heated wall temperatures are used to track the complex transient response of the heated wall, and identify differences between temperature excursions associated with momentary localized dryout and those with true CHF. It is shown that the flow enters the channel fully separated, with a liquid layer sheathing all four channel walls surrounding a central vapor core. At high heat fluxes, a wavy vapor layer begins to form beneath the liquid layer adjacent to the heated wall, and cooling is provided mostly through wetting fronts associated with the wave troughs in accordance with the Interfacial Lift-off Model. However, depending on mass velocity, inlet quality and flow orientation, conditions may arise that cause breakup of the heated wall liquid layer into ligaments that are entrained in the vapor core. This phenomenon causes localized dryout and wall temperature excursions at heat fluxes well below CHF, but the wall is able to recover from these excursions by a combination of reattachment of ligaments with the heated wall and lateral heat conduction within the wall itself. Recommendations are made concerning construction of the heated wall and CHF detection in pursuit of reliable CHF data. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Konishi, Christopher; Mudawar, Issam] Purdue Univ, Sch Mech Engn, BTPFL, W Lafayette, IN 47907 USA. [Hasan, Mohammad M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Mudawar, I (reprint author), Purdue Univ, Sch Mech Engn, BTPFL, 585 Purdue Mall, W Lafayette, IN 47907 USA. EM mudawar@ecn.purdue.edu FU National Aeronautics and Space Administration (NASA) [NNX13AC83G] FX The authors are grateful for the support of this project by the National Aeronautics and Space Administration (NASA) under Grant no. NNX13AC83G. NR 53 TC 7 Z9 8 U1 1 U2 19 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0017-9310 EI 1879-2189 J9 INT J HEAT MASS TRAN JI Int. J. Heat Mass Transf. PD DEC PY 2013 VL 67 BP 131 EP 146 DI 10.1016/j.ijheatmasstransfer.2013.07.082 PG 16 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA 259YL UT WOS:000327562100011 ER PT J AU Udom, I Ram, MK Stefanakos, EK Hepp, AF Goswami, DY AF Udom, Innocent Ram, Manoj K. Stefanakos, Elias K. Hepp, Aloysius F. Goswami, D. Yogi TI One dimensional-ZnO nanostructures: Synthesis, properties and environmental applications SO MATERIALS SCIENCE IN SEMICONDUCTOR PROCESSING LA English DT Review DE ZnO; Nanowire; Nanorod; Nanostructures; Photocatalyst; Dye; Remediation ID ULTRASOUND-ASSISTED SYNTHESIS; VISIBLE-LIGHT PHOTOCATALYSIS; ADVANCED OXIDATION PROCESSES; ZINC-OXIDE NANOSTRUCTURES; PHYSICAL VAPOR-DEPOSITION; DRINKING-WATER TREATMENT; PULSED-LASER DEPOSITION; SINGLE-CRYSTAL GROWTH; WASTE-WATER; NANOWIRE ARRAYS AB One-dimensional (1D) zinc oxide (ZnO) nanostructures such as rods, wires, belts and tubes have attracted much attention due to their unique physical, chemical, optical, and electrochemical properties enabling remarkable performance in photonics, sensors, photocatalysis, optics and photovoltaic devices. This paper presents a review of recent research in 1D ZnO nanostructures with emphasis on ZnO-based nanowires (NWs or NRs) used as photocatalysts for the degradation of environmental pollutants, particularly textile and industrial dyes, under appropriate light irradiation. Compared to other ZnO nanostructures, the higher aspect ratio (large surface to volume ratio) of 1D ZnO NWs offers highly desirable photocatalytic applications that depend on surface reactions or other phenomena that occur at interface surfaces, and eliminate the cost and requirement for post treatment. In addition, a review of several syntheses, fabrication methods and characterization studies of several types of ZnO NWs is presented. Finally, the photocatalytic degradation of selected dyes is highlighted. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Udom, Innocent; Ram, Manoj K.; Stefanakos, Elias K.; Goswami, D. Yogi] Univ S Florida, Coll Engn, Clean Energy Res Ctr, Tampa, FL 33620 USA. [Hepp, Aloysius F.] NASA, Glenn Res Ctr, Res & Technol Directorate, Cleveland, OH 44135 USA. RP Ram, MK (reprint author), Univ S Florida, Coll Engn, Clean Energy Res Ctr, Tampa, FL 33620 USA. EM mkram@usf.edu OI Ram, Manoj/0000-0002-6833-5566 FU National Aeronautics and Space Administration (NASA)-Harriett Jenkins Pre-doctoral Fellowship; State of Florida through the Florida Energy Systems Consortium (FESC) funds FX This work was supported by National Aeronautics and Space Administration (NASA)-Harriett Jenkins Pre-doctoral Fellowship and the State of Florida through the Florida Energy Systems Consortium (FESC) funds. NR 164 TC 45 Z9 46 U1 40 U2 336 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1369-8001 EI 1873-4081 J9 MAT SCI SEMICON PROC JI Mater. Sci. Semicond. Process PD DEC PY 2013 VL 16 IS 6 BP 2070 EP 2083 DI 10.1016/j.mssp.2013.06.017 PG 14 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA 254LB UT WOS:000327166000113 ER PT J AU Peng, TS Saxena, A Goebel, K Xiang, YB Sankararaman, S Liu, YM AF Peng, Tishun Saxena, Abhinav Goebel, Kai Xiang, Yibing Sankararaman, Shankar Liu, Yongming TI A novel Bayesian imaging method for probabilistic delamination detection of composite materials SO SMART MATERIALS AND STRUCTURES LA English DT Article AB A probabilistic framework for location and size determination for delamination in carbon-carbon composites is proposed in this paper. A probability image of delaminated area using Lamb wave-based damage detection features is constructed with the Bayesian updating technique. First, the algorithm for the probabilistic delamination detection framework using the proposed Bayesian imaging method (BIM) is presented. Next, a fatigue testing setup for carbon-carbon composite coupons is described. The Lamb wave-based diagnostic signal is then interpreted and processed. Next, the obtained signal features are incorporated in the Bayesian imaging method for delamination size and location detection, as well as the corresponding uncertainty bounds prediction. The damage detection results using the proposed methodology are compared with x-ray images for verification and validation. Finally, some conclusions are drawn and suggestions made for future works based on the study presented in this paper. C1 [Peng, Tishun; Xiang, Yibing; Liu, Yongming] Arizona State Univ, Sch Engn Matter Transport & Energy, Tempe, AZ 85287 USA. [Saxena, Abhinav; Sankararaman, Shankar] NASA, SGT, Ames Res Ctr, Moffett Field, CA 94035 USA. [Goebel, Kai] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Peng, TS (reprint author), Arizona State Univ, Sch Engn Matter Transport & Energy, Tempe, AZ 85287 USA. EM yongming.liu@asu.edu FU NASA Global Engineering and Materials, Inc.(GEM) [NNX12CA86C] FX The research reported in this paper was partially supported by the NASA through Global Engineering and Materials, Inc. (GEM) under the project NNX12CA86C. The support is gratefully acknowledged. NR 29 TC 8 Z9 8 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0964-1726 EI 1361-665X J9 SMART MATER STRUCT JI Smart Mater. Struct. PD DEC PY 2013 VL 22 IS 12 AR 125019 DI 10.1088/0964-1726/22/12/125019 PG 9 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA 258YC UT WOS:000327493600020 ER PT J AU Allodi, MA Baragiola, RA Baratta, GA Barucci, MA Blake, GA Boduch, P Brucato, JR Contreras, C Cuylle, SH Fulvio, D Gudipati, MS Ioppolo, S Kanuchova, Z Lignell, A Linnartz, H Palumbo, ME Raut, U Rothard, H Salama, F Savchenko, EV Sciamma-O'Brien, E Strazzulla, G AF Allodi, M. A. Baragiola, R. A. Baratta, G. A. Barucci, M. A. Blake, G. A. Boduch, P. Brucato, J. R. Contreras, C. Cuylle, S. H. Fulvio, D. Gudipati, M. S. Ioppolo, S. Kanuchova, Z. Lignell, A. Linnartz, H. Palumbo, M. E. Raut, U. Rothard, H. Salama, F. Savchenko, E. V. Sciamma-O'Brien, E. Strazzulla, G. TI Complementary and Emerging Techniques for Astrophysical Ices Processed in the Laboratory SO SPACE SCIENCE REVIEWS LA English DT Review DE Laboratory astrophysics; Solid state astrochemistry; Inter- and circumstellar medium; Molecular astrophysics; Astronomical ice analogues ID SPITZER SPECTROSCOPIC SURVEY; YOUNG STELLAR OBJECTS; RARE-GAS SOLIDS; POLYCYCLIC AROMATIC-HYDROCARBONS; PULSED DISCHARGE ENVIRONMENT; PARTIAL-PRESSURE ANALYZERS; FAR-INFRARED SPECTRA; HE+ ION-BOMBARDMENT; WATER-ICE; INTERSTELLAR ICE AB Inter- and circumstellar ices comprise different molecules accreted on cold dust particles. These icy dust grains provide a molecule reservoir where particles can interact and react. As the grain acts as a third body, capable of absorbing energy, icy surfaces in space have a catalytic effect. Chemical reactions are triggered by a number of possible processes; (i) irradiation by light, typically UV photons from the interstellar radiation field and Ly-alpha radiation emitted by excited hydrogen, but also X-rays, (ii) bombardment by particles, free atoms (most noticeably hydrogen, but also N, C, O and D-atoms), electrons, low energy ions and cosmic rays, and (iii) thermal processing. All these effects cause ices to (photo)desorb, induce fragmentation or ionization in the ice, and eventual recombination will make molecules to react and to form more and more complex species. The effects of this solid state astrochemistry are observed by astronomers; nearly 180 different molecules (not including isotopologues) have been unambiguously identified in the inter- and circumstellar medium, and the abundances of a substantial part of these species cannot be explained by gas phase reaction schemes only and must involve solid state chemistry. Icy dust grains in space experience different chemical stages. In the diffuse medium grains are barely covered by molecules, but upon gravitational collapse and darkening of the cloud, temperatures drop and dust grains start acting as micrometer sized cryopumps. More and more species accrete, until even the most volatile species are frozen. In parallel (non)energetic processing can take place, particularly during planet and star formation when radiation and particle fluxes are intense. The physical and chemical properties of ice clearly provide a snapshotroot to characterize the cosmological chemical evolution. In order to fully interpret the astronomical observations, therefore, dedicated laboratory experiments are needed that simulate dust grain formation and processing as well as ice mantle chemistry under astronomical conditions and in full control of the relevant parameters; ice morphology (i.e., structure), composition, temperature, UV and particle fluxes, etc., yielding parameters that can be used for astrochemical modeling and for comparison with the observations. This is the topic of the present manuscript. Laboratory experiments simulating the conditions in space are conducted for decades all over the world, but particularly in recent years new techniques have made it possible to study reactions involving inter- and circumstellar dust and ice analogues at an unprecedented level of detail. Whereas in the past "top-down scenarios" allowed to conclude on the importance of the solid state for the chemical enrichment of space, presently "bottom-up approaches" make it possible to fully quantify the involved reactions, and to provide information on processes at the molecular level. The recent progress in the field of "solid state laboratory astrophysics" is a consequence of the use of ultra high vacuum systems, of new radiation sources, such as synchrotrons and laser systems that allow extensions to wavelength domains that long have not been accessible, including the THz domain, and the use of highly sensitive gas phase detection techniques, explicitly applied to characterize the solid state such as fluorescence, luminescence, cavity ring-down spectroscopy and sophisticated mass spectrometric techniques. This paper presents an overview of the techniques being used in astrochemical laboratories worldwide, but it is incomplete in the sense that it summarizes the outcome of a 3-day workshop of the authors in November 2012 (at the Observatoire de Meudon in France), with several laboratories represented, but not all. The paper references earlier work, but it is incomplete with regard to latest developments of techniques used in laboratories not represented at the workshop. C1 [Allodi, M. A.; Blake, G. A.] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. [Baragiola, R. A.; Fulvio, D.; Raut, U.] Univ Virginia, Lab Atom & Surface Phys, Charlottesville, VA 22904 USA. [Baratta, G. A.; Kanuchova, Z.; Palumbo, M. E.; Strazzulla, G.] INAF, Osservatorio Astrofis Catania, Catania, Italy. [Barucci, M. A.] Observ Paris, LESIA, F-75014 Paris, France. [Blake, G. A.; Ioppolo, S.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Boduch, P.; Rothard, H.] CIMAP CIRIL Ganil, CEA, CNRS, ENSICAEN,UCBN,Ctr Rech Ion Mat & Photon, F-14070 Caen 5, France. [Brucato, J. R.] INAF, Osservatorio Astrofis Arcetri, Florence, Italy. [Contreras, C.; Salama, F.; Sciamma-O'Brien, E.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Cuylle, S. H.; Linnartz, H.] Leiden Univ, Leiden Observ, Raymond & Beverly Sackler Lab Astrophys, NL-2300 RA Leiden, Netherlands. [Gudipati, M. S.; Lignell, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gudipati, M. S.] Univ Maryland, IPST, College Pk, MD 20742 USA. [Savchenko, E. V.] NASU, Verkin Inst Low Temp Phys & Engn, UA-61103 Kharkov, Ukraine. RP Strazzulla, G (reprint author), INAF, Osservatorio Astrofis Catania, Catania, Italy. EM mallodi@caltech.edu; raul@virginia.edu; gbaratta@oact.inaf.it; antonella.barucci@obspm.fr; gab@gps.caltech.edu; boduch@ganil.fr; jbrucato@arcetri.astro.it; df6vz@virginia.edu; murthy.gudipati@jpl.nasa.gov; ioppolo@caltech.edu; zkanuch@ta3.sk; linnartz@strw.leidenuniv.nl; mepalumbo@oact.inaf.it; raut@virginia.edu; rothard@ganil.fr; farid.salama@nasa.gov; elena.savchenko@gmail.com; gianni@oact.inaf.it RI Lignell, Antti/C-2146-2009; Gudipati, Murthy/F-7575-2011; Sciamma-O'Brien, Ella/M-2043-2014; Salama, Farid/A-8787-2009; OI Lignell, Antti/0000-0001-7664-5583; Brucato, John Robert/0000-0002-4738-5521; Sciamma-O'Brien, Ella/0000-0002-1883-552X; Salama, Farid/0000-0002-6064-4401; Allodi, Marco A./0000-0002-3289-1659; Baratta, Giuseppe/0000-0002-3688-160X; Palumbo, MariaElisabetta/0000-0002-9122-491X; Strazzulla, Giovanni/0000-0003-1412-4023 FU NWO; NOVA; Marie Curie programs; Marie Curie Fellowship [FP7-PEOPLE-2011-IOF-300957]; VEGA-The Slovak Agency for Science [2/0022/10]; European COST Action [CM 0805] FX H. Linnartz: Grants within NWO, NOVA and Marie Curie programs. The setups and conclusions presented here have been the outcome of dedicated work by several PhD students, postdocs, and scientific collaborators. Special thanks go to Karin Oberg, Jordy Bouwman, Edith Fayolle, Steven Cuylle, Lou Allamandola, Jean-Hugues Fillion and Mathieu Bertin.; S. Ioppolo: NASA SARA and Exobiology/Astrobiology programs, Niels Stensen Foundation (NSS) through a bursary and a Marie Curie Fellowship (FP7-PEOPLE-2011-IOF-300957).; Z. Kanuchova: VEGA-The Slovak Agency for Science, grant no. 2/0022/10 and the European COST Action CM 0805: The Chemical Cosmos: Understanding Chemistry in Astronomical Environments. NR 238 TC 31 Z9 31 U1 6 U2 64 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD DEC PY 2013 VL 180 IS 1-4 BP 101 EP 175 DI 10.1007/s11214-013-0020-8 PG 75 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 264QP UT WOS:000327895500004 ER PT J AU Liu, C Deng, N Lee, J Wiegelmann, T Moore, RL Wang, HM AF Liu, Chang Deng, Na Lee, Jeongwoo Wiegelmann, Thomas Moore, Ronald L. Wang, Haimin TI EVIDENCE FOR SOLAR TETHER-CUTTING MAGNETIC RECONNECTION FROM CORONAL FIELD EXTRAPOLATIONS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: activity; Sun: flares; Sun: magnetic fields; Sun: X-rays, gamma rays ID ACTIVE-REGION 11158; MASS EJECTIONS; ENERGY; FLARES; RECONSTRUCTION; AMBIGUITY; ERUPTION; RHESSI AB Magnetic reconnection is one of the primary mechanisms for triggering solar eruptive events, but direct observation of this rapid process has been a challenge. In this Letter, using a nonlinear force-free field (NLFFF) extrapolation technique, we present a visualization of field line connectivity changes resulting from tether-cutting reconnection over about 30 minutes during the 2011 February 13 M6.6 flare in NOAA AR 11158. Evidence for the tether-cutting reconnection was first collected through multiwavelength observations and then by analysis of the field lines traced from positions of four conspicuous flare 1700 angstrom footpoints observed at the event onset. Right before the flare, the four footpoints are located very close to the regions of local maxima of the magnetic twist index. In particular, the field lines from the inner two footpoints form two strongly twisted flux bundles (up to similar to 1.2 turns), which shear past each other and reach out close to the outer two footpoints, respectively. Immediately after the flare, the twist index of regions around the footpoints diminishes greatly and the above field lines become low-lying and less twisted (less than or similar to 0.6 turns), overarched by loops linking the two flare ribbons formed later. About 10% of the flux (similar to 3 x 10(19) Mx) from the inner footpoints undergoes a footpoint exchange. This portion of flux originates from the edge regions of the inner footpoints that are brightened first. These rapid changes of magnetic field connectivity inferred from the NLFFF extrapolation are consistent with the tether-cutting magnetic reconnection model. C1 [Liu, Chang; Deng, Na; Lee, Jeongwoo; Wang, Haimin] New Jersey Inst Technol, Space Weather Res Lab, Ctr Solar Terr Res, Newark, NJ 07102 USA. [Lee, Jeongwoo] Kyung Hee Univ, Sch Space Res, Yongin 446701, South Korea. [Wiegelmann, Thomas] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Moore, Ronald L.] NASA, George C Marshall Space Flight Ctr, Heliophys & Planetary Sci Off, Huntsville, AL 35812 USA. RP Liu, C (reprint author), New Jersey Inst Technol, Space Weather Res Lab, Ctr Solar Terr Res, Newark, NJ 07102 USA. EM chang.liu@njit.edu OI Deng, Na/0000-0001-8179-812X; Liu, Chang/0000-0002-6178-7471 FU NASA [NNX13AF76G, NNX13AG13G, NNX11AO70G]; Kyung Hee University; DLR [50 OC 0904]; DFG [WI 3211/2-1] FX We thank the SDO/HMI and AIA, RHESSI, and Fermi teams for excellent data, and the referees for valuable comments. C. L., N.D., and H. W. were supported by NASA grants NNX13AF76G, NNX13AG13G, and NNX11AO70G. J.L. was supported by the international scholarship of Kyung Hee University. T. W. was supported by DLR grant 50 OC 0904 and DFG grant WI 3211/2-1. NR 36 TC 15 Z9 15 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 1 PY 2013 VL 778 IS 2 AR L36 DI 10.1088/2041-8205/778/2/L36 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 258AA UT WOS:000327428400014 ER PT J AU Nynka, M Hailey, CJ Mori, K Baganoff, FK Bauer, FE Boggs, SE Craig, WW Christensen, FE Gotthelf, EV Harrison, FA Hong, J Perez, KM Stern, D Zhang, S Zhang, WW AF Nynka, Melania Hailey, Charles J. Mori, Kaya Baganoff, Frederick K. Bauer, Franz E. Boggs, Steven E. Craig, William W. Christensen, Finn E. Gotthelf, Eric V. Harrison, Fiona A. Hong, Jaesub Perez, Kerstin M. Stern, Daniel Zhang, Shuo Zhang, William W. TI HIGH-ENERGY X-RAYS FROM J174545.5-285829, THE CANNONBALL: A CANDIDATE PULSAR WIND NEBULA ASSOCIATED WITH Sgr A EAST SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: center; ISM: individual objects (Sagittarius A, Sagittarius A East); ISM: supernova remnants; stars: neutron; X-rays: individual (Cannonball) ID SAGITTARIUS-A-EAST; SUPERNOVA-REMNANT SAGITTARIUS; GALACTIC-CENTER; RADIATION; CHANDRA AB We report the unambiguous detection of non-thermal X-ray emission up to 30 keV from the Cannonball, a few-arcsecond long diffuse X-ray feature near the Galactic Center, using the NuSTAR X-ray observatory. The Cannonball is a high-velocity (v(proj) similar to 500 km s (1)) pulsar candidate with a cometary pulsar wind nebula (PWN) located similar to 2' north-east from Sgr A*, just outside the radio shell of the supernova remnant Sagittarius A (Sgr A) East. Its non-thermal X-ray spectrum, measured up to 30 keV, is well characterized by a Gamma similar to 1.6 power law, typical of a PWN, and has an X-ray luminosity of L(3-30 keV) = 1.3 x 10(34) erg s(-1). The spectral and spatial results derived from X-ray and radio data strongly suggest a runaway neutron star born in the Sgr A East supernova event. We do not find any pulsed signal from the Cannonball. The NuSTAR observations allow us to deduce the PWN magnetic field and show that it is consistent with the lower limit obtained from radio observations. C1 [Nynka, Melania; Hailey, Charles J.; Mori, Kaya; Gotthelf, Eric V.; Zhang, Shuo] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Baganoff, Frederick K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Hong, Jaesub] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Perez, Kerstin M.] Columbia Univ, New York, NY 10027 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Nynka, M (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. RI Boggs, Steven/E-4170-2015 OI Boggs, Steven/0000-0001-9567-4224 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration FX This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The authors wish to thank Jules Halpern for useful discussions. NR 25 TC 10 Z9 10 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 1 PY 2013 VL 778 IS 2 AR UNSP L31 DI 10.1088/2041-8205/778/2/L31 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 258AA UT WOS:000327428400009 ER PT J AU Robock, A MacMartin, DG Duren, R Christensen, MW AF Robock, Alan MacMartin, Douglas G. Duren, Riley Christensen, Matthew W. TI Studying geoengineering with natural and anthropogenic analogs SO CLIMATIC CHANGE LA English DT Article ID MICROPHYSICAL SIMULATIONS; VOLCANIC-ERUPTIONS; MOUNT-PINATUBO; STRATOSPHERIC AEROSOL; MARINE STRATOCUMULUS; MODEL SIMULATIONS; OZONE DEPLETION; SHIP TRACKS; CLIMATE; CLOUDS AB Solar radiation management (SRM) has been proposed as a possible option for offsetting some anthropogenic radiative forcing, with the goal of reducing some of the associated climatic changes. There are clearly significant uncertainties associated with SRM, and even small-scale experiments that might reduce uncertainty would carry some risk. However, there are also natural and anthropogenic analogs to SRM, such as volcanic eruptions in the case of stratospheric aerosol injection and ship tracks in the case of marine cloud albedo modification. It is essential to understand what we can learn from these analogs in order to validate models, particularly because of the problematic nature of outdoor experiments. It is also important to understand what we cannot learn, as this might better focus attention on what risks would need to be solely examined by numerical models. Stratospheric conditions following a major volcanic eruption, for example, are not the same as those to be expected from intentional geoengineering, both because of confounding effects of volcanic ash and the differences between continuous and impulsive injection of material into the stratosphere. Nonetheless, better data would help validate models; we thus recommend an appropriate plan be developed to better monitor the next large volcanic eruption. Similarly, more could be learned about cloud albedo modification from careful study not only of ship tracks, but of ship and other aerosol emission sources in cloud regimes beyond the narrow conditions under which ship tracks form; this would benefit from improved satellite observing capabilities. C1 [Robock, Alan] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08901 USA. [MacMartin, Douglas G.] CALTECH, Pasadena, CA 91125 USA. [Duren, Riley] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Christensen, Matthew W.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RP Robock, A (reprint author), Rutgers State Univ, Dept Environm Sci, 14 Coll Farm Rd, New Brunswick, NJ 08901 USA. EM robock@envsci.rutgers.edu RI Christensen, Matthew/C-5733-2013; MacMartin, Douglas/A-6333-2016; Robock, Alan/B-6385-2016; OI MacMartin, Douglas/0000-0003-1987-9417; Robock, Alan/0000-0002-6319-5656 FU Keck Institute for Space Studies; NSF [AGS-1157525]; National Aeronautics and Space Administration FX We thank the Keck Institute for Space Studies for funding two workshops at the California Institute of Technology where we discussed topics in this paper, and all of the participants of these workshops who contributed (http://www.kiss.caltech.edu/study/geoengineering). A. Robock is supported by NSF grant AGS-1157525. The work by R. Duren was done at the Jet Propulsion Laboratory, a division of the California Institute of Technology under contract to the National Aeronautics and Space Administration. NR 79 TC 23 Z9 24 U1 4 U2 51 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0165-0009 EI 1573-1480 J9 CLIMATIC CHANGE JI Clim. Change PD DEC PY 2013 VL 121 IS 3 SI SI BP 445 EP 458 DI 10.1007/s10584-013-0777-5 PG 14 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 256OH UT WOS:000327322700003 ER PT J AU O'Brien, DM Polonsky, I O'Dell, C Kuze, A Kikuchi, N Yoshida, Y Natraj, V AF O'Brien, Denis M. Polonsky, Igor O'Dell, Chris Kuze, Akihiko Kikuchi, Nobuhiro Yoshida, Yukio Natraj, Vijay TI Testing the Polarization Model for TANSO-FTS on GOSAT Against Clear-Sky Observations of Sun Glint Over the Ocean SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Near infrared; ocean; optical polarization; remote sensing ID GASES OBSERVING SATELLITE; CO2; RETRIEVAL; SPECTRA; BAND; CH4 AB A model is developed to relate the polarized signals measured by the thermal and near infrared sensor for carbon observations-Fourier transform spectrometer (TANSO-FTS) on Japan's Greenhouse Gases Observing Satellite to Stokes' vector for radiation leaving the target. The model requires the position and velocity of the satellite, the yaw angle between TANSO-FTS and the satellite bus, the reflectance and phase shift properties of the pointing mirror of TANSO-FTS, and the radiometric calibration coefficients. The accuracy of the polarization model is tested by comparing the degree of polarization observed in clear sky over sun glint on the ocean against the value predicted by Fresnel reflection from a rough sea surface. Observations from April 2009 to December 2011 suggest that the polarization characteristics of TANSO-FTS have remained stable. C1 [O'Brien, Denis M.; Polonsky, Igor; O'Dell, Chris] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. [Kuze, Akihiko] Japan Aerosp Explorat Agcy, Tokyo 1046023, Japan. [Kikuchi, Nobuhiro; Yoshida, Yukio] Natl Inst Environm Studies, Satellite Remote Sensing Res Sect, Ctr Global Environm Res, Tsukuba, Ibaraki 3058506, Japan. [Natraj, Vijay] NASA, Jet Prop Lab, La Canada Flintridge, CA 91011 USA. RP O'Brien, DM (reprint author), Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. EM obrien@atmos.colostate.edu; polonsky@atmos.colostate.edu; odell@atmos.colostate.edu; kuze.akihiko@jaxa.jp; kikuchi.nobuhiroi@nies.go.jp; yoshida.yukio@nies.go.jp; vijay.natraj@jpl.nasa.gov RI KUZE, AKIHIKO/J-2074-2016 OI KUZE, AKIHIKO/0000-0001-5415-3377 FU National Aeronautics and Space Administration [1380533] FX The work at Colorado State University was supported by National Aeronautics and Space Administration contract 1380533. NR 18 TC 5 Z9 5 U1 0 U2 13 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD DEC PY 2013 VL 51 IS 12 BP 5199 EP 5209 DI 10.1109/TGRS.2012.2232673 PG 11 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 259VE UT WOS:000327553600002 ER PT J AU Williams, BA AF Williams, Brent A. TI A Fieldwise Retrieval Approach to the Noise Versus Resolution Tradeoff in Wind Scatterometry SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Bayes estimation; maximum a posteriori estimation; wind scatterometry ID MODEL-BASED ESTIMATION; AMBIGUITY REMOVAL; SEASAT SCATTEROMETER; SEAWINDS; OCEAN; ASSIMILATION; ALGORITHM; ACCURACY; SPECTRUM; NSCAT AB This paper approaches the noise versus resolution tradeoff in wind scatterometry from a fieldwise retrieval perspective. Theoretical considerations are discussed, and a practical implementation is developed and applied to the SeaWinds scatterometer. The approach is compared with conventional approaches, as well as numerical weather predictions and buoys. The new method incorporates knowledge of the wind spectrum to reduce the impact of components of the wind signal that are expected to be noisy while enabling reconstruction of fine-scale features that are distinguishable from noise. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Williams, BA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Brent.A.Williams@jpl.nasa.gov FU National Aeronautics and Space Administration FX The work described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. Government sponsorship acknowledged. NR 35 TC 0 Z9 0 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD DEC PY 2013 VL 51 IS 12 BP 5259 EP 5272 DI 10.1109/TGRS.2012.2233481 PG 14 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 259VE UT WOS:000327553600007 ER PT J AU Potter, C AF Potter, Christopher TI Ten years of land cover change on the California coast detected using landsat satellite image analysis: part 1-Marin and San Francisco counties SO JOURNAL OF COASTAL CONSERVATION LA English DT Article DE Landsat; Coastal vegetation; Disturbance; Regrowth; Restoration ID PHYTOPHTHORA-RAMORUM; FOREST; FIRE; USA AB Landsat satellite imagery was analyzed to generate a detailed record of 10 years of vegetation disturbance and regrowth for Pacific coastal areas of Marin and San Francisco Counties. The Landsat Ecosystem Disturbance Adaptive Processing System (LEDAPS) methodology, a transformation of Tasseled-Cap data space, was applied to detected changes in perennial coastal shrubland, woodland, and forest cover from 1999 to 2009. Results showed several principal points of interest, within which extensive contiguous areas of similar LEDAPS vegetation change (either disturbed or restored) were detected. Regrowth areas were delineated as burned forest areas in the Point Reyes National Seashore (PRNS) from the 1995 Vision Fire. LEDAPS-detected disturbance patterns on Inverness Ridge, PRNS in areas observed with dieback of tanoak and bay laurel trees was consistent with defoliation by sudden oak death (Phytophthora ramorum). LEDAPS regrowth pixels were detected over much of the predominantly grassland/herbaceous cover of the Olema Valley ranchland near PRNS. Extensive restoration of perennial vegetation cover on Crissy Field, Baker Beach and Lobos Creek dunes in San Francisco was identified. Based on these examples, the LEDAPS methodology will be capable of fulfilling much of the need for continual, low-cost monitoring of emerging changes to coastal ecosystems. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Potter, C (reprint author), NASA, Ames Res Ctr, Mail Stop 232-21, Moffett Field, CA 94035 USA. EM chris.potter@nasa.gov FU NASA Ames Research FX This work was supported by grants from NASA Ames Research. The author thanks Steven Skartvedt and Robert Steers of the National Park Service for assistance with image interpretations and historical information on the GGNRA. NR 24 TC 2 Z9 2 U1 2 U2 29 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1400-0350 EI 1874-7841 J9 J COAST CONSERV JI J. Coast. Conserv. PD DEC PY 2013 VL 17 IS 4 BP 697 EP 707 DI 10.1007/s11852-013-0255-2 PG 11 WC Biodiversity Conservation; Environmental Sciences; Marine & Freshwater Biology; Water Resources SC Biodiversity & Conservation; Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 259AI UT WOS:000327499400001 ER PT J AU Potter, C AF Potter, Christopher TI Ten years of land cover change on the California coast detected using Landsat satellite image analysis: Part 2-San Mateo and Santa Cruz counties SO JOURNAL OF COASTAL CONSERVATION LA English DT Article DE Landsat; Coastal vegetation; Disturbance; Regrowth; Restoration AB Landsat satellite imagery was analyzed to generate a detailed record of 10 years of vegetation disturbance and regrowth for Pacific coastal areas of San Mateo and Santa Cruz Counties. The Landsat Ecosystem Disturbance Adaptive Processing System (LEDAPS) methodology, a transformation of Tasseled-Cap data space, was applied to detected changes in perennial coastal shrubland, woodland, and forest cover from 1999 to 2009. Results showed several principal points of interest, within which extensive contiguous areas of similar LEDAPS vegetation change (either disturbed or restored) were detected. Regrowth of evergreen shrub and tree cover was prevalent along the several long stretches of the coast highway (CA Route 1) between the cities of Half Moon Bay and Santa Cruz. A number of state parks areas showed measurable vegetation restoration as well. The most prominent loss of perennial coastal vegetation over decade was in the Pescadero Marsh area, where the continued presence of levees has historically reduced flood conveyance capacity into and through the marshlands. Based on these examples, the LEDAPS methodology was determined to be capable of fulfilling much of the need for continual, low-cost monitoring of emerging changes to coastal ecosystems. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Potter, C (reprint author), NASA, Ames Res Ctr, Mail Stop 232-21, Moffett Field, CA 94035 USA. EM chris.potter@nasa.gov FU NASA Ames Research FX This work was supported by grants from NASA Ames Research. The author thanks Tim Hyland, Environmental Scientist, California State Parks for assistance with image interpretations and historical information on the Ano Nuevo State Reserve area. NR 14 TC 1 Z9 1 U1 2 U2 14 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1400-0350 EI 1874-7841 J9 J COAST CONSERV JI J. Coast. Conserv. PD DEC PY 2013 VL 17 IS 4 BP 709 EP 718 DI 10.1007/s11852-013-0270-3 PG 10 WC Biodiversity Conservation; Environmental Sciences; Marine & Freshwater Biology; Water Resources SC Biodiversity & Conservation; Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 259AI UT WOS:000327499400002 ER PT J AU Johnson, C Inall, M Hakkinen, S AF Johnson, Clare Inall, Mark Haekkinen, Sirpa TI Declining nutrient concentrations in the northeast Atlantic as a result of a weakening Subpolar Gyre SO DEEP-SEA RESEARCH PART I-OCEANOGRAPHIC RESEARCH PAPERS LA English DT Article DE Subpolar Gyre; Rockall Trough; Atlantic Water; Nutrients; Time-series; Variability ID WATER MASSES; ROCKALL TROUGH; CIRCULATION; OCEAN; SHELF; WEST; SLOPE; TEMPERATURE; GREENLAND; PHOSPHATE AB Between 1996 and the mid-2000s the upper waters (200-700 m) of the Rockall Trough became warmer (+0.72 degrees C), saltier (+0.088) and reduced in nitrate and phosphate (-2.00 mu M and -0.14 mu M respectively). These changes, out-with calculated errors, can be explained by the varying influence of southern versus subpolar water masses in the basin as the Subpolar Gyre weakened and contracted. Upper water properties strongly correlate with a measure of the strength of the Subpolar Gyre (the first principal component of sea surface height over the Subpolar North Atlantic) prior to the mid-2000s. As the gyre weakens, the upper layers of the trough become warmer (r-0.85), more saline (r-0.86) and reduced in nitrate and phosphate (r+0.81 and r+0.87 respectively). Further the proportion of subpolar waters in the basin decreases from around 50% to less than 20% (r+0.88). Since the mid-2000s the Subpolar Gyre has been particularly weak. During this period temperatures decreased slightly (-0.21 degrees C), salinities remained near constant (35.410 +/- 0.005) and phosphate levels low and stable (0.68 +/- 0.02 mu M). These relative lack of changes are thought to be related to the maximum proportion of southern water masses within the Rockall Trough having been reached. Thus the upper water properties are no longer controlled by changes in the relative importance of different water masses in the basin (as prior to the mid-2000s), but rather a different process. We suggest that when the gyre is particularly weak the interannual changes in upper water properties in the Rockall Trough reflect changes in the source properties of the southern water masses. Since the early-2000s the Subpolar Gyre has been weaker than observed since 1992, or modelled since 1960-1970. Hence upper waters within the Rockall Trough may be warmer, saltier and more depleted in nitrate and phosphate than at any time in the last half century. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Johnson, Clare; Inall, Mark] Scottish Marine Inst, SAMS, Oban PA37 1QA, Argyll, Scotland. [Haekkinen, Sirpa] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Johnson, C (reprint author), Scottish Marine Inst, SAMS, Oban PA37 1QA, Argyll, Scotland. EM cljo@sams.ac.uk RI Inall, Mark/I-4835-2014; OI Inall, Mark/0000-0002-1624-4275; Clare, Johnson/0000-0002-8213-2554 FU University of the Highlands and Islands; Department for Environment, Food and Rural Affairs; UK National Environment Research Council; Marine Scotland-Science trips; Scottish Executive FX We thank all crew, scientists and technicians involved in the collection and processing of data during the numerous Ellett Line cruises used within this paper. The Ellett Line is funded by the UK National Environment Research Council with Marine Scotland-Science trips funded by the Scottish Executive. We also acknowledge the useful discussions with Professor Toby Sherwin and the comments of the two reviewers which greatly improved this manuscript. This work was funded by the University of the Highlands and Islands and the Department for Environment, Food and Rural Affairs. NR 65 TC 12 Z9 13 U1 0 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0637 EI 1879-0119 J9 DEEP-SEA RES PT I JI Deep-Sea Res. Part I-Oceanogr. Res. Pap. PD DEC PY 2013 VL 82 BP 95 EP 107 DI 10.1016/j.dsr.2013.08.007 PG 13 WC Oceanography SC Oceanography GA 254MF UT WOS:000327169100010 ER PT J AU Iskovitz, I Kassemi, M Thomas, JD AF Iskovitz, Ilana Kassemi, Mohammad Thomas, James D. TI Impact of Weightlessness on Cardiac Shape and Left Ventricular Stress/Strain Distributions SO JOURNAL OF BIOMECHANICAL ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article ID CANINE LEFT-VENTRICLE; WALL MECHANICS; MATHEMATICAL-MODEL; FLUID VOLUME; DOG HEART; SPACEFLIGHT; MYOCARDIUM; STRESS; SHEAR; FRAMEWORK AB In this paper, a finite element model of the heart is developed to investigate the impact of different gravitational loadings of Earth, Mars, Moon, and microgravity on the cardiac shape and strain/stress distributions in the left ventricle. The finite element model is based on realistic 3D heart geometry, detailed fiber/sheet micro-architecture, and a validated orthotropic cardiac tissue model and constitutive relationship that capture the passive behavior of the heart at end-diastole. The model predicts the trend and magnitude of cardiac shape change at different gravitational levels with great fidelity in comparison to recent cardiac sphericity measurements performed during simulated reduced-gravity parabolic flight experiments. Moreover, the numerical predictions indicate that although the left ventricular strain distributions remain relatively unaltered across the gravitational fields and the strain extrema values occur at the same relative locations, their values change noticeably with decreasing gravity. As for the stress, however, both the magnitude and location of the extrema change with a decrease in the gravitational field. Consequently, tension regions of the heart on Earth can change into compression regions in space. C1 [Iskovitz, Ilana; Kassemi, Mohammad] NASA, Glenn Res Ctr, NCSER, Cleveland, OH 44135 USA. [Thomas, James D.] Cleveland Clin Fdn, Dept Cardiovasc Med, Cleveland, OH 44195 USA. RP Iskovitz, I (reprint author), NASA, Glenn Res Ctr, NCSER, Cleveland, OH 44135 USA. EM Ilana.Iskovitz@nasa.gov; Mohammad.Kassemi@nasa.gov FU NSBRI [09-2-NSBRI_09-0039, NCC-9058-172]; NASA FX Funding Supports from NSBRI (09-2-NSBRI_09-0039, under grant NCC-9058-172) and NASA Human Research Program (HRP) are gratefully acknowledged. The authors also gratefully acknowledge online access to the cardiac geometrical data provided by the Bioengineering Institute at University of Auckland and to the code Continuity provided by the Cardiac Mechanics Research Group, University of California San Diego that were used for preparation and verification of the heart geometry used in this analysis. NR 42 TC 1 Z9 2 U1 2 U2 12 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0148-0731 EI 1528-8951 J9 J BIOMECH ENG-T ASME JI J. Biomech. Eng.-Trans. ASME PD DEC PY 2013 VL 135 IS 12 AR 121008 DI 10.1115/1.4025464 PG 11 WC Biophysics; Engineering, Biomedical SC Biophysics; Engineering GA 253NZ UT WOS:000327096500008 PM 24048335 ER PT J AU Livneh, B Rosenberg, EA Lin, CY Nijssen, B Mishra, V Andreadis, KM Maurer, EP Lettenmaier, DP AF Livneh, Ben Rosenberg, Eric A. Lin, Chiyu Nijssen, Bart Mishra, Vimal Andreadis, Kostas M. Maurer, Edwin P. Lettenmaier, Dennis P. TI A Long-Term Hydrologically Based Dataset of Land Surface Fluxes and States for the Conterminous United States: Update and Extensions SO JOURNAL OF CLIMATE LA English DT Article DE Forcing; Hydrometeorology; Surface observations ID DAILY SOLAR-RADIATION; CLIMATE-CHANGE; RIVER-BASIN; EXPERIMENT DESIGN; MODEL; PRECIPITATION; TEMPERATURE; STREAMFLOW; HUMIDITY; SNOW AB This paper describes a publicly available, long-term (1915-2011), hydrologically consistent dataset for the conterminous United States, intended to aid in studies of water and energy exchanges at the land surface. These data are gridded at a spatial resolution of 1/16 degrees latitude/longitude and are derived from daily temperature and precipitation observations from approximately 20 000 NOAA Cooperative Observer (COOP) stations. The available meteorological data include temperature, precipitation, and wind, as well as derived humidity and downwelling solar and infrared radiation estimated via algorithms that index these quantities to the daily mean temperature, temperature range, and precipitation, and disaggregate them to 3-hourly time steps. Furthermore, the authors employ the variable infiltration capacity (VIC) model to produce 3-hourly estimates of soil moisture, snow water equivalent, discharge, and surface heat fluxes. Relative to an earlier similar dataset by Maurer and others, the improved dataset has 1) extended the period of analysis (1915-2011 versus 1950-2000), 2) increased the spatial resolution from 1/8 degrees to 1/16 degrees, and 3) used an updated version of VIC. The previous dataset has been widely used in water and energy budget studies, climate change assessments, drought reconstructions, and for many other purposes. It is anticipated that the spatial refinement and temporal extension will be of interest to a wide cross section of the scientific community. C1 [Livneh, Ben; Lettenmaier, Dennis P.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Rosenberg, Eric A.; Lin, Chiyu; Nijssen, Bart; Mishra, Vimal] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA. [Andreadis, Kostas M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Maurer, Edwin P.] Santa Clara Univ, Dept Civil Engn, Santa Clara, CA 95053 USA. RP Livneh, B (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, 216 UCB, Boulder, CO 80309 USA. EM blivneh@hydro.washington.edu RI Maurer, Edwin/C-7190-2009; Livneh, Ben/I-2939-2015; Nijssen, Bart/B-1013-2012; OI Maurer, Edwin/0000-0001-7134-487X; Nijssen, Bart/0000-0002-4062-0322; LIVNEH, BEN/0000-0001-5445-2473 NR 38 TC 95 Z9 95 U1 1 U2 39 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD DEC PY 2013 VL 26 IS 23 BP 9384 EP 9392 DI 10.1175/JCLI-D-12-00508.1 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 253AN UT WOS:000327054100008 ER PT J AU Mace, GG Wrenn, FJ AF Mace, Gerald G. Wrenn, Forrest J. TI Evaluation of the Hydrometeor Layers in the East and West Pacific within ISCCP Cloud-Top Pressure-Optical Depth Bins Using Merged CloudSat and CALIPSO Data SO JOURNAL OF CLIMATE LA English DT Article DE Clouds; Cloud retrieval; Remote sensing; Satellite observations ID MICROPHYSICAL PROPERTY RETRIEVALS; INFRARED RADIANCE MEASUREMENTS; VERTICAL STRUCTURE; OBJECTIVE ASSESSMENT; INFORMATION-CONTENT; STATISTICAL-MODEL; GLOBAL OCEANS; REGIMES; ATMOSPHERE; VALIDATION AB The International Satellite Cloud Climatology Project (ISCCP) provides a multidecadal and global description of cloud properties that are often grouped into joint histograms of column visible optical depth and effective cloud-top pressure P-top. It has not been possible until recently to know the actual distributions of hydrometeor layers within the ISCCP P-top- bins. Distributions of hydrometeor layers within the ISCCP P-top- conditional probability space using measurements from the CloudSat Cloud Profiling Radar and the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) lidar within two 40 degrees x 40 degrees regions in the eastern and western equatorial Pacific over a 2-yr period are examined. With the exception of thin cirrus and stratocumulus, the authors show that of the P-top- types that are commonly analyzed, none of the types contain unique distributions of geometrically defined layer types but tend to be populated by diverse sets of hydrometeor layers whose bulk profile properties conspire to render specific radiative signatures when interpreted by two-channel visible and IR sensors from space. In comparing the geometric distribution of cloud layers for common P-top- types, it is found that the ISCCP Cirrostratus, Deep Convection, and Stratocumulus types appear to have been drawn from a common geometric distribution of hydrometeor layers. The other six common ISCCP P-top- types do not share this feature. The authors can confidently reject an assumption that even though they have common top-of-atmosphere radiative signatures, they do not appear to share a common distribution of cloud layers and therefore are likely to have significantly different radiative heating profiles and different surface radiative forcing even though their top-of-atmosphere radiative signatures are similar. C1 [Mace, Gerald G.] Univ Utah, Salt Lake City, UT 84112 USA. [Wrenn, Forrest J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Mace, GG (reprint author), Univ Utah, Dept Atmospher Sci, 201 S 1460 E Rm 819 WBB, Salt Lake City, UT 84112 USA. EM jay.mace@utah.edu FU NASA Jet Propulsion Laboratory [1228646]; NASA [NNX07AT45G, NNX10AM42G] FX This work benefited from the expertise of Sally Benson in porting the ISCCP simulator algorithm from Fortran to IDL. Stephanie Avey (while very pregnant) and Sally Benson implemented the analysis code in an operational environment. Dr. Steve Cooper provided his implementation of the Radiant model. Qiuqing Zhang helped in creating several of the cloud occurrence figures. This work benefitted greatly from significant and valuable critical comments provided by Dr. George Tselioudis during several revisions of the manuscript. Support was provided by NASA Jet Propulsion Laboratory (Award 1228646) and NASA Grants NNX07AT45G and NNX10AM42G. NR 43 TC 10 Z9 11 U1 0 U2 20 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD DEC PY 2013 VL 26 IS 23 BP 9429 EP 9444 DI 10.1175/JCLI-D-12-00207.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 253AN UT WOS:000327054100013 ER PT J AU Goldstein, ME Afsar, MZ Leib, SJ AF Goldstein, M. E. Afsar, M. Z. Leib, S. J. TI Non-homogeneous rapid distortion theory on transversely sheared mean flows SO JOURNAL OF FLUID MECHANICS LA English DT Article DE aeroacoustics; turbulence modelling; turbulence theory ID UNSTEADY MOTION; TURBULENT-FLOW; AERODYNAMIC SOUND; JET NOISE; SCATTERING; PLATE AB This paper is concerned with the small-amplitude unsteady motion of an inviscid non-heat-conducting compressible fluid on a transversely sheared mean flow. It extends previous analyses (Goldstein, J. Fluid Mech., vol. 84, 1978b, pp. 305-329; Goldstein, J. Fluid Mech., vol. 91, 1979a, pp. 601-632), which show that the hydrodynamic component of the motion is determined by two arbitrary convected quantities in the absence of solid surfaces and hydrodynamic instabilities. These results can be used to specify appropriate upstream boundary conditions for unsteady surface interaction problems on transversely sheared mean flows in the same way that the vortical component of the Kovasznay (J. Aero. Sci., vol. 20, 1953, pp. 657-674) decomposition is used to specify these conditions for surface interaction problems on uniform mean flows. But unlike Kovasznay's result, the arbitrary convected quantities no longer bear a simple relation to the physical variables. A major purpose of this paper is to complete the formalism developed in Goldstein's earlier two papers by obtaining the necessary relations between these quantities and the measurable flow variables. The results are important because they enable the complete extension of non-homogeneous rapid distortion theory to transversely sheared mean flows. Another purpose of the paper is to derive a generalization of the famous Ffowcs Williams and Hall (J. Fluid Mech., vol. 40, 1970, pp. 657-670) formula for the sound produced by the interaction of turbulence with an edge, which is frequently used as a starting point for predicting sound generation by turbulence-solid surface interactions. We illustrate the utility of this result by using it to calculate the sound radiation produced by the interaction of a two-dimensional jet with the downstream edge of a flat plate. C1 [Goldstein, M. E.; Afsar, M. Z.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Leib, S. J.] Ohio Aerosp Inst, Cleveland, OH 44142 USA. RP Goldstein, ME (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM Marvin.E.Goldstein@nasa.gov FU NASA Post-doctoral Program (NPP); NASA FX The authors would like to thank Drs K. Zaman, J. Bridges and C. Brown for providing their experimental data and their helpful comments. They would also like to thank Miss D. Frank (Ph.D. candidate, Department of Applied Mathematics and Theoretical Physics, University of Cambridge, UK) for her excellent translation of the Mohring paper. M.Z.A. would like to thank the NASA Post-doctoral Program (NPP) for financial support (NPP liaison, Dr D. Kankam). This work was also supported by the NASA Fundamental Aeronautics Program's High-Speed and Fixed Wing Projects. NR 39 TC 6 Z9 6 U1 0 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-1120 EI 1469-7645 J9 J FLUID MECH JI J. Fluid Mech. PD DEC PY 2013 VL 736 BP 532 EP 569 DI 10.1017/jfm.2013.518 PG 38 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA 254BZ UT WOS:000327138000023 ER PT J AU Orth, R Koster, RD Seneviratne, SI AF Orth, Rene Koster, Randal D. Seneviratne, Sonia I. TI Inferring Soil Moisture Memory from Streamflow Observations Using a Simple Water Balance Model SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Runoff; Hydrologic models; Model evaluation; performance; Interannual variability; Seasonal cycle ID VARIABILITY; FORECASTS; SCALE; PRECIPITATION; GRASSLAND; FLUXNET; CLOSURE; IMPACT; SNOW AB Soil moisture is known for its integrative behavior and resulting memory characteristics. Soil moisture anomalies can persist for weeks or even months into the future, making initial soil moisture a potentially important contributor to skill in weather forecasting. A major difficulty when investigating soil moisture and its memory using observations is the sparse availability of long-term measurements and their limited spatial representativeness. In contrast, there is an abundance of long-term streamflow measurements for catchments of various sizes across the world. The authors investigate in this study whether such streamflow measurements can be used to infer and characterize soil moisture memory in respective catchments. Their approach uses a simple water balance model in which evapotranspiration and runoff ratios are expressed as simple functions of soil moisture; optimized functions for the model are determined using streamflow observations, and the optimized model in turn provides information on soil moisture memory on the catchment scale. The validity of the approach is demonstrated with data from three heavily monitored catchments. The approach is then applied to streamflow data in several small catchments across Switzerland to obtain a spatially distributed description of soil moisture memory and to show how memory varies, for example, with altitude and topography. C1 [Orth, Rene; Seneviratne, Sonia I.] ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland. [Koster, Randal D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Orth, R (reprint author), ETH, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland. EM rene.orth@env.ethz.ch RI Koster, Randal/F-5881-2012; Seneviratne, Sonia/G-8761-2011 OI Koster, Randal/0000-0001-6418-6383; Seneviratne, Sonia/0000-0001-9528-2917 FU Swiss National Foundation through the NRP61 DROUGHT-CH project; EU-FP7 DROUGHT-RSPI project FX We acknowledge the Swiss Federal Office for the Environment (FOEN) for providing streamflow data for the 13 Swiss catchments and the Swiss weather service (MeteoSwiss) for providing the corresponding precipitation data. We thank Massimiliano Zappa for sharing these data with us, as well as Guenther Seufert and Christoph Ammann for providing data from San Rossore and Oensingen, respectively. We also thank three anonymous reviewers for helpful comments on the manuscript and Gerd Vogel and Guenther Seufert for advice on the CEOP and Carboeurope databases, which we acknowledge for sharing the Falkenberg, Kehrigk, and San Rossore data, as well as the hydrological service of the Tuscany Region for providing the streamflow data of the Arno River. We acknowledge financial support from the Swiss National Foundation through the NRP61 DROUGHT-CH project, as well as partial support from the EU-FP7 DROUGHT-RSPI project. NR 32 TC 11 Z9 11 U1 0 U2 22 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD DEC PY 2013 VL 14 IS 6 BP 1773 EP 1790 DI 10.1175/JHM-D-12-099.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 255QF UT WOS:000327254200006 ER PT J AU Chen, S Kirstetter, PE Hong, Y Gourley, JJ Tian, YD Qi, YC Cao, Q Zhang, J Howard, K Hu, JJ Xue, XW AF Chen, S. Kirstetter, P. E. Hong, Y. Gourley, J. J. Tian, Y. D. Qi, Y. C. Cao, Q. Zhang, J. Howard, K. Hu, J. J. Xue, X. W. TI Evaluation of Spatial Errors of Precipitation Rates and Types from TRMM Spaceborne Radar over the Southern CONUS SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Precipitation; Atmosphere-land interaction; Hydrometeorology ID MEASURING MISSION TRMM; RAIN PROFILING ALGORITHM; HYDROLOGICAL MODEL; GROUND VALIDATION; UNITED-STATES; SATELLITE; QPE; SYSTEM; AFRICA; SCALES AB In this paper, the authors estimate the uncertainty of the rainfall products from NASA and Japan Aerospace Exploration Agency's (JAXA) Tropical Rainfall Measurement Mission (TRMM) Precipitation Radar (PR) so that they may be used in a quantitative manner for applications like hydrologic modeling or merging with other rainfall products. The spatial error structure of TRMM PR surface rain rates and types was systematically studied by comparing them with NOAA/National Severe Storms Laboratory's (NSSL) next generation, high-resolution (1 km/5 min) National Mosaic and Multi-Sensor Quantitative Precipitation Estimation (QPE; NMQ/Q2) over the TRMM-covered continental United States (CONUS). Data pairs are first matched at the PR footprint scale (5 km/instantaneous) and then grouped into 0.25 degrees grid cells to yield spatially distributed error maps and statistics using data from December 2009 through November 2010. Careful quality control steps (including bias correction with rain gauges and quality filtering) are applied to the ground radar measurements prior to considering them as reference data. The results show that PR captures well the spatial pattern of total rainfall amounts with a high correlation coefficient (CC; 0.91) with Q2, but this decreases to 0.56 for instantaneous rain rates. In terms of precipitation types, Q2 and PR convective echoes are spatially correlated with a CC of 0.63. Despite this correlation, PR's total annual precipitation from convection is 48.82% less than that by Q2, which points to potential issues in the PR algorithm's attenuation correction, nonuniform beam filling, and/or reflectivity-to-rainfall relation. Finally, the spatial analysis identifies regime-dependent errors, in particular in the mountainous west. It is likely that the surface reference technique is triggered over complex terrain, resulting in high-amplitude biases. C1 [Chen, S.; Kirstetter, P. E.; Hong, Y.; Cao, Q.; Xue, X. W.] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA. [Chen, S.; Kirstetter, P. E.; Hong, Y.; Cao, Q.; Xue, X. W.] Natl Weather Ctr, Adv Radar Res Ctr, Norman, OK 73072 USA. [Kirstetter, P. E.; Gourley, J. J.; Qi, Y. C.; Zhang, J.; Howard, K.] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA. [Tian, Y. D.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Tian, Y. D.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Qi, Y. C.] Univ Oklahoma, Cooperat Inst Mesoscale Meteorol Studies, Norman, OK 73019 USA. [Hu, J. J.] Univ Oklahoma, Sch Comp Sci, Norman, OK 73019 USA. RP Hong, Y (reprint author), Natl Weather Ctr, Adv Radar Res Ctr, Suite 4610,120 David L Boren Blvd, Norman, OK 73072 USA. EM yanghong@ou.edu RI Hong, Yang/D-5132-2009; Kirstetter, Pierre/E-2305-2013; Gourley, Jonathan/C-7929-2016; Xue, Xianwu/C-8006-2016; Measurement, Global/C-4698-2015 OI Hong, Yang/0000-0001-8720-242X; Kirstetter, Pierre/0000-0002-7381-0229; Gourley, Jonathan/0000-0001-7363-3755; Xue, Xianwu/0000-0002-2106-6370; FU NASA; University of Oklahoma Advanced Radar Research Center; NOAA/Office of Oceanic and Atmospheric Research under NOAA-University of Oklahoma [NA17RJ1227] FX The authors wish to acknowledge the OU and NOAA/NSSL team for providing the NMQ/Q2 products. This work was funded by a postdoctoral grant from the NASA Global Precipitation Measurement Mission Ground Validation Program and was also supported by the Multi-function Phased-Array Radar (MPAR) Project at the University of Oklahoma Advanced Radar Research Center. Partial funding was provided by the NOAA/Office of Oceanic and Atmospheric Research under NOAA-University of Oklahoma Cooperative Agreement NA17RJ1227. NR 31 TC 14 Z9 14 U1 1 U2 19 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD DEC PY 2013 VL 14 IS 6 BP 1884 EP 1896 DI 10.1175/JHM-D-13-027.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 255QF UT WOS:000327254200013 ER PT J AU Sun, WB Videen, G Fu, Q Hu, YX AF Sun, Wenbo Videen, Gorden Fu, Qiang Hu, Yongxiang TI Scattered-field FDTD and PSTD algorithms with CPML absorbing boundary conditions for light scattering by aerosols SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Finite-difference time domain; Pseudo-spectral time-domain; Light scattering; Aerosol particle ID TIME-DOMAIN METHOD; DISCRETE-DIPOLE APPROXIMATION; PERFECTLY MATCHED LAYER; NONSPHERICAL PARTICLES; MAXWELLS EQUATIONS; NUMERICAL-SOLUTION; MEDIA; SIMULATIONS; ABSORPTION; MATRIX AB As fundamental parameters for polarized-radiative-transfer calculations, the single-scattering phase matrix of irregularly shaped aerosol particles must be accurately modeled. In this study, a scattered-field finite-difference time-domain (FDTD) model and a scattered-field pseudospectral time-domain (PSTD) model are developed for light scattering by arbitrarily shaped dielectric aerosols. The convolutional perfectly matched layer (CPML) absorbing boundary condition (ABC) is used to truncate the computational domain. It is found that the PSTD method is generally more accurate than the FDTD in calculation of the single-scattering properties given similar spatial cell sizes. Since the PSTD can use a coarser grid for large particles, it can lower the memory requirement in the calculation. However, the Fourier transformations in the PSTD need significantly more CPU time than simple subtractions in the FDTD, and the fast Fourier transform requires a power of 2 elements in calculations, thus using the PSTD could not significantly reduce the CPU time required in the numerical modeling. Furthermore, because the scattered-field FDTD/PSTD equations include incident-wave source terms, the FDTD/PSTD model allows for the inclusion of an arbitrarily incident wave source, including a plane parallel wave or a Gaussian beam like those emitted by lasers usually used in laboratory particle characterizations, etc. The scattered-field FDTD and PSTD light-scattering models can be used to calculate single-scattering properties of arbitrarily shaped aerosol particles over broad size and wavelength ranges. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Sun, Wenbo] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Videen, Gorden] US Army Res Lab, Adelphi, MD 20783 USA. [Fu, Qiang] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Sun, Wenbo; Hu, Yongxiang] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Sun, WB (reprint author), NASA, Langley Res Ctr, Mail Stop 420,21 Langley Blvd, Hampton, VA 23681 USA. EM Wenbo.Sun-1@nasa.gov RI Hu, Yongxiang/K-4426-2012; Richards, Amber/K-8203-2015 FU NASA [09-GLORY09-0027] FX This work was supported by NASA Glory fund 09-GLORY09-0027. The authors thank Michael I. Mishchenko and Hal B. Maring for support on this work. NR 31 TC 9 Z9 9 U1 2 U2 15 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD DEC PY 2013 VL 131 SI SI BP 166 EP 174 DI 10.1016/j.jqsrt.2013.07.015 PG 9 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 255GK UT WOS:000327227200022 ER PT J AU Schmidt, MA Goodwin, TJ AF Schmidt, Michael A. Goodwin, Thomas J. TI Personalized medicine in human space flight: using Omics based analyses to develop individualized countermeasures that enhance astronaut safety and performance SO METABOLOMICS LA English DT Review DE Omics; Genomics; Proteomics; Transcriptomics; Metabolomics; Personalized medicine; Space flight; Human; Astronaut health; Exploration; Systems biology; Single nucleotide polymorphism; Oxidative stress; Human performance; Essential inputs; Micronutrient; DNA stability; DNA repair ID RADIATION-INDUCED MICRONUCLEI; NUTRITIONAL-STATUS ASSESSMENT; LONG-DURATION SPACEFLIGHT; BONE TURNOVER MARKERS; FOLIC-ACID DEFICIENCY; ONE-CARBON METABOLISM; POSTMENOPAUSAL WOMEN; DNA-DAMAGE; METHYLENETETRAHYDROFOLATE REDUCTASE; URACIL MISINCORPORATION AB Space flight is one of the most extreme conditions encountered by humans. Advances in Omics methodologies (genomics, transcriptomics, proteomics, and metabolomics) have revealed that unique differences exist between individuals. These differences can be amplified in extreme conditions, such as space flight. A better understanding of individual differences may allow us to develop personalized countermeasure packages that optimize the safety and performance of each astronaut. In this review, we explore the role of "Omics" in advancing our ability to: (1) more thoroughly describe the biological response of humans in space; (2) describe molecular attributes of individual astronauts that alter the risk profile prior to entering the space environment; (3) deploy Omics techniques in the development of personalized countermeasures; and (4) develop a comprehensive Omics-based assessment and countermeasure platform that will guide human space flight in the future. In this review, we advance the concept of personalized medicine in human space flight, with the goal of enhancing astronaut safety and performance. Because the field is vast, we explore selected examples where biochemical individuality might significantly impact countermeasure development. These include gene and small molecule variants associated with: (1) metabolism of therapeutic drugs used in space; (2) one carbon metabolism and DNA stability; (3) iron metabolism, oxidative stress and damage, and DNA stability; and (4) essential input (Mg and Zn) effects on DNA repair. From these examples, we advance the case that widespread Omics profiling should serve as the foundation for aerospace medicine and research, explore methodological considerations to advance the field, and suggest why personalized medicine may become the standard of care for humans in space. C1 [Schmidt, Michael A.] Colorado State Univ, MetaboLogics LLC, Adv Pattern Anal & Countermeasures Grp, Ft Collins, CO 80521 USA. [Goodwin, Thomas J.] NASA, Johnson Space Ctr, Dis Modeling & Tissue Analogues Lab, Biomed Res & Environm Sci Div, Houston, TX 77058 USA. RP Schmidt, MA (reprint author), Colorado State Univ, MetaboLogics LLC, Adv Pattern Anal & Countermeasures Grp, Infect Dis Res Complex,3185 Rampart Rd, Ft Collins, CO 80521 USA. EM mschmidtphd@metabologics.net; thomas.j.goodwin@nasa.gov NR 98 TC 9 Z9 10 U1 3 U2 22 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1573-3882 EI 1573-3890 J9 METABOLOMICS JI Metabolomics PD DEC PY 2013 VL 9 IS 6 BP 1134 EP 1156 DI 10.1007/s11306-013-0556-3 PG 23 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 251KF UT WOS:000326926700003 ER PT J AU Laviola, S Levizzani, V Cattani, E Kidd, C AF Laviola, Sante Levizzani, Vincenzo Cattani, Elsa Kidd, Chris TI The 183-WSL fast rain rate retrieval algorithm. Part II: Validation using ground radar measurements SO ATMOSPHERIC RESEARCH LA English DT Article DE Microwave; Precipitation; Satellites; Validation; Radar; Winter ID PRECIPITATION; INTENSITY AB The Water vapor Strong Lines at 183 GHz (183-WSL) algorithm is a method for the retrieval of rain rates and precipitation type classification (convective/stratiform). It exploits the water vapor absorption line observations centered at 18331 GHz of the Advanced Microwave Sounding Unit module B (AMSU-B) and of the Microwave Humidity Sounder (MHS) flying on NOAA-15/-17 and NOAA-18-19/MetOp-A satellite series, respectively. The characteristics of this algorithm were described in Part I of this paper together with comparisons against analogous precipitation products. The focus of Part II is the analysis of the performance of the 183-WSL technique based on surface radar measurements. The "ground truth" dataset consists of 2 years and 7 months of rainfall intensity fields from the NIMROD radar network, which covers North-Western Europe. The investigation of the 183-WSL retrieval performance is based on a twofold approach: 1) the dichotomous statistic is used to evaluate the capabilities of the method to identify rain and no-rain clouds and 2) the accuracy statistic is applied to quantify the errors in the estimation of rain rates. The results reveal that the 183-WSL technique shows good skills in the detection of rain/no-rain areas and in the quantification of rain rate intensities. The categorical analysis shows annual values of the Probability Of Detection (POD), False Alarm Ratio (FAR) and Hanssen-Kuiper discriminant (HK) indices varying in the range 0.80-0.82, 0.33-0.36 and 0.39-0.46, respectively. The RMSE value is 2.8 mm h(-1) for the whole period despite an overestimation in the retrieved rain rates. Of note is the distribution of the 183-WSL monthly mean rain rate with respect to radar: the seasonal fluctuations of the average rainfalls measured by radar are reproduced by the 183-WSL. However, the retrieval method appears to suffer during winter seasonal conditions especially when the soil is partially frozen and the surface emissivity drastically changes. This is verified by the discrepancy distribution diagrams where the 183-WSL performs better during the warm months, while during the winter time the discrepancies with radar measurements tend to maximum values. The stable behavior of the 183-WSL algorithm is demonstrated over the whole study period by an overall overestimation for rain rate intensities less than 1 mm h(-1). This threshold is especially crucial in wintertime when the classification of low-intensity precipitation regimes is difficult. (C) 2013 Elsevier B.V. All rights reserved. C1 [Laviola, Sante; Levizzani, Vincenzo; Cattani, Elsa] CNR ISAC, I-40129 Bologna, Italy. [Kidd, Chris] Univ Maryland, NASA GSFC, College Pk, MD 20742 USA. [Kidd, Chris] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Laviola, S (reprint author), CNR ISAC, Via Gobetti 101, I-40129 Bologna, Italy. EM s.laviola@isac.cnr.it RI Levizzani, Vincenzo/A-9070-2013; Kidd, Christopher/H-9910-2014 OI Levizzani, Vincenzo/0000-0002-7620-5235; FU EUMETSAT's "Satellite Application Facility on support to Hydrology and Operational Water Management" (H-SAF); European Commission [FP7-2010-1.1-04, 262255] FX The work was supported by EUMETSAT's "Satellite Application Facility on support to Hydrology and Operational Water Management" (H-SAF, http://hsaf.meteoam.it/) and by the European Commission 7th Framework Programme FP7-2010-1.1-04 GMES project Global Water Scarcity Information Service (GLOWASIS, http://glowasis.eu/) grant no. 262255. The essential contribution of two anonymous reviewers in improving the paper is gratefully acknowledged. NR 25 TC 7 Z9 7 U1 2 U2 13 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0169-8095 EI 1873-2895 J9 ATMOS RES JI Atmos. Res. PD DEC 1 PY 2013 VL 134 BP 77 EP 86 DI 10.1016/j.atmosres.2013.07.013 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 246RJ UT WOS:000326556500008 ER PT J AU Estes, LD Beukes, H Bradley, BA Debats, SR Oppenheimer, M Ruane, AC Schulze, R Tadross, M AF Estes, Lyndon D. Beukes, Hein Bradley, Bethany A. Debats, Stephanie R. Oppenheimer, Michael Ruane, Alex C. Schulze, Roland Tadross, Mark TI Projected climate impacts to South African maize and wheat production in 2055: a comparison of empirical and mechanistic modeling approaches SO GLOBAL CHANGE BIOLOGY LA English DT Article DE climate change; crop model; downscaling; DSSAT; empirical; generalized additive model; mechanistic; South Africa; Triticum aestivum; Zea mays ID CROP YIELD; SPECIES DISTRIBUTIONS; FOOD SECURITY; ADAPTATION; CO2; VULNERABILITY; AGRICULTURE; UNCERTAINTY; SUITABILITY; PREDICT AB Crop model-specific biases are a key uncertainty affecting our understanding of climate change impacts to agriculture. There is increasing research focus on intermodel variation, but comparisons between mechanistic (MMs) and empirical models (EMs) are rare despite both being used widely in this field. We combined MMs and EMs to project future (2055) changes in the potential distribution (suitability) and productivity of maize and spring wheat in South Africa under 18 downscaled climate scenarios (9 models run under 2 emissions scenarios). EMs projected larger yield losses or smaller gains than MMs. The EMs' median-projected maize and wheat yield changes were -3.6% and 6.2%, respectively, compared to 6.5% and 15.2% for the MM. The EM projected a 10% reduction in the potential maize growing area, where the MM projected a 9% gain. Both models showed increases in the potential spring wheat production region (EM=48%, MM=20%), but these results were more equivocal because both models (particularly the EM) substantially overestimated the extent of current suitability. The substantial water-use efficiency gains simulated by the MMs under elevated CO2 accounted for much of the EM-MM difference, but EMs may have more accurately represented crop temperature sensitivities. Our results align with earlier studies showing that EMs may show larger climate change losses than MMs. Crop forecasting efforts should expand to include EM-MM comparisons to provide a fuller picture of crop-climate response uncertainties. C1 [Estes, Lyndon D.; Oppenheimer, Michael] Princeton Univ, Woodrow Wilson Sch, Program Sci Technol & Environm Policy, Princeton, NJ 08544 USA. [Estes, Lyndon D.; Debats, Stephanie R.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. [Beukes, Hein] Agr Res Council, Inst Soil Climate & Water, ZA-2599 Stellenbosch, South Africa. [Bradley, Bethany A.] Univ Massachusetts, Dept Environm Conservat, Amherst, MA 01003 USA. [Oppenheimer, Michael] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Ruane, Alex C.] NASA, GISS Climate Impacts Grp SSP, New York, NY 10025 USA. [Schulze, Roland] Univ KwaZulu Natal, Sch Bioresources Engn & Environm Hydrol, ZA-3209 Pietermaritzburg, South Africa. [Tadross, Mark] Univ Cape Town, Climate Syst Anal Grp, ZA-7701 Rondebosch, South Africa. RP Estes, LD (reprint author), Princeton Univ, Woodrow Wilson Sch, Program Sci Technol & Environm Policy, Princeton, NJ 08544 USA. EM lestes@princeton.edu RI Bradley, Bethany/B-1964-2008 OI Bradley, Bethany/0000-0003-4912-4971 FU Princeton Environmental Institutes Grand Challenges Program FX We gratefully acknowledge funding from the Princeton Environmental Institutes Grand Challenges Program. We thank Anneliza Collet and Rona Beukes of the National Department of Agriculture, Terry Newby and Dave Turner of the Agricultural Research Council, Fanie Ferreira and Mark Thompson of GeoTerraImage, Eugene du Preez of SiQ, and Lisa Coop of the University of Cape Town for providing data used in developing models, and three reviewers for their helpful feedback. NR 56 TC 18 Z9 18 U1 0 U2 64 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD DEC PY 2013 VL 19 IS 12 BP 3762 EP 3774 DI 10.1111/gcb.12325 PG 13 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 250FN UT WOS:000326836000018 PM 23864352 ER PT J AU Khalsa, SJS Ramachandran, R AF Khalsa, Siri Jodha S. Ramachandran, Rahul TI Earth Science Informatics Comes of Age SO IEEE GEOSCIENCE AND REMOTE SENSING MAGAZINE LA English DT Editorial Material C1 [Khalsa, Siri Jodha S.] Univ Colorado, NSIDC, Boulder, CO 80309 USA. [Ramachandran, Rahul] NASA, MSFC, Washington, DC 20546 USA. RP Khalsa, SJS (reprint author), Univ Colorado, NSIDC, Boulder, CO 80309 USA. EM rama-chr@uah.edu OI Khalsa, Siri Jodha/0000-0001-9217-5550 NR 4 TC 1 Z9 1 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2168-6831 J9 IEEE GEOSC REM SEN M JI IEEE Geosci. Remote Sens. Mag. PD DEC PY 2013 VL 1 IS 4 BP 19 EP 21 DI 10.1109/MGRS.2013.2289817 PG 3 WC Geochemistry & Geophysics; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Remote Sensing; Imaging Science & Photographic Technology GA V45KX UT WOS:000209816600004 ER PT J AU Lee, CH Juang, JN AF Lee, Cheh-Han Juang, Jer-Nan TI Deterministic Bilinear System Identification SO JOURNAL OF THE ASTRONAUTICAL SCIENCES LA English DT Article DE System realization; System identification; Bilinear system identification AB A unified identification method is proposed for system realization of a deterministic continuous-time/discrete-time bilinear models from input and output measurement data. A generalized Hankel matrix is formed with the output measurements obtained by applying a set of repeated input sequences to a bilinear system. A computational procedure is developed to extract a time varying discrete-time state-space model from the generalized Hankel matrix. The bilinear system models are realized by transforming the identified time varying discrete-time model to the bilinear models. Numerical simulations are given to show the effectiveness of the proposed identification method. C1 [Lee, Cheh-Han; Juang, Jer-Nan] Natl Cheng Kung Univ, Dept Engn Sci, Tainan 701, Taiwan. [Juang, Jer-Nan] Texas A&M Univ, Colege Stn, TX USA. [Juang, Jer-Nan] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Juang, JN (reprint author), Natl Cheng Kung Univ, Dept Engn Sci, Tainan 701, Taiwan. EM jjuang88@gmail.com; jason491.lee@gmail.com NR 32 TC 0 Z9 0 U1 0 U2 0 PU AMER ASTRONAUTICAL SOC PI SPRINGFIELD PA 6352 ROLLING MILL PLACE SUITE 102, SPRINGFIELD, VA 22152 USA SN 0021-9142 EI 2195-0571 J9 J ASTRONAUT SCI JI J. Astronaut. Sci. PD DEC PY 2013 VL 60 IS 3-4 BP 237 EP 257 DI 10.1007/s40295-015-0047-z PG 21 WC Engineering, Aerospace SC Engineering GA V41VW UT WOS:000209574700001 ER PT J AU Markley, FL AF Markley, F. Landis TI Equivalence of Two Solutions of Wahba's Problem SO JOURNAL OF THE ASTRONAUTICAL SCIENCES LA English DT Article DE Attitude estimation; Wahba's problem AB Many attitude estimation methods are based on an optimization problem posed in 1965 by Grace Wahba. All these methods yield the same optimal estimate, except for inevitable computer roundoff errors. This note shows shows that Shuster's Quaternion Estimator (QUEST) and Mortari's Estimator of the Optimal Quaternion (ESOQ) are essentially identical even in the presence of roundoff errors. It also shows some connections between two other algorithms for solving Wahba's problem: Davenport's q method and the Singular Value Decomposition (SVD) method. C1 [Markley, F. Landis] NASA, Goddard Space Flight Ctr, Attitude Control Syst Engn Branch, Greenbelt, MD USA. RP Markley, FL (reprint author), NASA, Goddard Space Flight Ctr, Attitude Control Syst Engn Branch, Greenbelt, MD USA. EM landis.markley@nasa.gov NR 14 TC 1 Z9 1 U1 0 U2 0 PU AMER ASTRONAUTICAL SOC PI SPRINGFIELD PA 6352 ROLLING MILL PLACE SUITE 102, SPRINGFIELD, VA 22152 USA SN 0021-9142 EI 2195-0571 J9 J ASTRONAUT SCI JI J. Astronaut. Sci. PD DEC PY 2013 VL 60 IS 3-4 BP 303 EP 312 DI 10.1007/s40295-015-0049-x PG 10 WC Engineering, Aerospace SC Engineering GA V41VW UT WOS:000209574700004 ER PT J AU Balas, MJ Frost, SA AF Balas, Mark J. Frost, Susan A. TI Evolving Systems: Nonlinear Adaptive Key Component Control with Persistent Disturbance Rejection SO JOURNAL OF THE ASTRONAUTICAL SCIENCES LA English DT Article DE Evolving systems; Aerospace systems; Adaptive systems AB This paper presents an introduction to Evolving Systems, which are autonomously controlled subsystems that self-assemble into a new Evolved System with a higher purpose. Evolving Systems of aerospace structures often require additional control when assembling to maintain stability during the entire evolution process. This is the concept of adaptive key component control which operates through one specific component to maintain stability during the evolution. In addition this control must overcome persistent disturbances that occur while the evolution is in progress. We present theoretical results for the successful operation of non-linear adaptive key component control in the presence of such disturbances and an illustrative example. C1 [Balas, Mark J.] Embry Riddle Aeronaut Univ, Dept Aerosp Engn, Daytona Beach, FL 32114 USA. [Frost, Susan A.] NASA, Intelligent Syst Div, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Balas, MJ (reprint author), Embry Riddle Aeronaut Univ, Dept Aerosp Engn, Daytona Beach, FL 32114 USA. EM balasm@erau.edu NR 11 TC 0 Z9 0 U1 0 U2 0 PU AMER ASTRONAUTICAL SOC PI SPRINGFIELD PA 6352 ROLLING MILL PLACE SUITE 102, SPRINGFIELD, VA 22152 USA SN 0021-9142 EI 2195-0571 J9 J ASTRONAUT SCI JI J. Astronaut. Sci. PD DEC PY 2013 VL 60 IS 3-4 BP 366 EP 377 DI 10.1007/s40295-015-0067-8 PG 12 WC Engineering, Aerospace SC Engineering GA V41VW UT WOS:000209574700007 ER PT J AU Juang, JN Hung, CH Wilkie, WK AF Juang, Jer-Nan Hung, Chung-Han Wilkie, William K. TI Dynamics of a Slender Spinning Membrane SO JOURNAL OF THE ASTRONAUTICAL SCIENCES LA English DT Article DE Heliogyro solar sail; Spinning membrane; Structural dynamics AB A novel approach is introduced to conduct dynamic analysis of a spinning, high aspect ratio membrane. In this formulation, an inextensible, long, slender membrane is modeled using a discrete set of lumped masses. Lagranges equations are used to derive the highly coupled ordinary differential equations for in-plane, out-of-plane, and twisting motions for the spinning membrane. The generalized and uncoupled linear equations for small motion are used to compute the vibration mode frequencies which are compared to results from an uncoupled analysis of blade motion using rotor dynamics. Linearized behavior is shown to reduce to the linearized solutions for the spinning membrane blade developed by MacNeal. Numerical simulations along with 3-D animations are used to study the linear and nonlinear uncoupled dynamics of the spinning membrane. C1 [Juang, Jer-Nan; Hung, Chung-Han] Natl Cheng Kung Univ, Dept Engn Sci, Tainan 701, Taiwan. [Juang, Jer-Nan] Texas A&M Univ, Dept Aerosp Engn, College Stn, TX 77843 USA. [Juang, Jer-Nan; Hung, Chung-Han] Natl Inst Aerosp, Hampton, VA USA. [Wilkie, William K.] NASA, Langley Res Ctr, Struct Dynam Branch, Hampton, VA 23665 USA. RP Juang, JN (reprint author), Natl Cheng Kung Univ, Dept Engn Sci, Tainan 701, Taiwan. EM jjuang88@gmail.com FU NCKU (National Cheng Kung University); National Institute of Aerospace, Hampton, Virginia FX This research activity is supported in part by NCKU (National Cheng Kung University) Academic Summit Program and Student Exchange Program of National Institute of Aerospace, Hampton, Virginia. The authors are grateful to Dr. Yu-Ru Huang of NCKU Department of Engineering Science for revising the equations of twisting motion. NR 13 TC 0 Z9 0 U1 0 U2 0 PU AMER ASTRONAUTICAL SOC PI SPRINGFIELD PA 6352 ROLLING MILL PLACE SUITE 102, SPRINGFIELD, VA 22152 USA SN 0021-9142 EI 2195-0571 J9 J ASTRONAUT SCI JI J. Astronaut. Sci. PD DEC PY 2013 VL 60 IS 3-4 BP 494 EP 516 DI 10.1007/s40295-015-0062-0 PG 23 WC Engineering, Aerospace SC Engineering GA V41VW UT WOS:000209574700013 ER PT J AU Zanetti, R D'Souza, C AF Zanetti, Renato D'Souza, Christopher TI Recursive Implementations of the Schmidt-Kalman 'Consider' Filter SO JOURNAL OF THE ASTRONAUTICAL SCIENCES LA English DT Article AB One method to account for parameters errors in the Kalman filter is to 'consider' their effect in the so-called Schmidt-Kalman filter. This paper addresses issues that arise when implementing a consider Kalman filter as a real-time, recursive algorithm. A favorite implementation of the Kalman filter as an onboard navigation subsystem is the UDU formulation. A new way to implement a UDU Schmidt Kalman filter is proposed. The non-optimality of the recursive Schmidt-Kalman filter is also analyzed, and a modified algorithm is proposed to overcome this limitation. C1 [Zanetti, Renato] Charles Stark Draper Lab, Vehicle Dynam & Controls, 17629 El Camino Real,Suite 470, Houston, TX 77058 USA. [Zanetti, Renato] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [D'Souza, Christopher] NASA, GN & C Autonomous Flight Syst Branch, Aerosci & Flight Mech Div, Johnson Space Ctr EG6, Houston, TX 77058 USA. RP Zanetti, R (reprint author), Charles Stark Draper Lab, Vehicle Dynam & Controls, 17629 El Camino Real,Suite 470, Houston, TX 77058 USA. EM renato.zanetti@nasa.gov; chris.dsouza@nasa.gov NR 15 TC 0 Z9 0 U1 1 U2 1 PU AMER ASTRONAUTICAL SOC PI SPRINGFIELD PA 6352 ROLLING MILL PLACE SUITE 102, SPRINGFIELD, VA 22152 USA SN 0021-9142 EI 2195-0571 J9 J ASTRONAUT SCI JI J. Astronaut. Sci. PD DEC PY 2013 VL 60 IS 3-4 BP 672 EP 685 DI 10.1007/s40295-015-0068-7 PG 14 WC Engineering, Aerospace SC Engineering GA V41VW UT WOS:000209574700021 ER PT J AU Barsi, S Kassemi, M AF Barsi, Stephen Kassemi, Mohammad TI Investigation of Tank Pressurization and Pressure Control-Part I: Experimental Study SO JOURNAL OF THERMAL SCIENCE AND ENGINEERING APPLICATIONS LA English DT Article AB Self-pressurization and pressure control of cryogenic storage tanks have important design consequences for propellant and life support systems currently being planned for long duration space missions. During self-pressurization, the tank's liquid fill level and the heat load from the surroundings can have significant effects on the tank's thermal stratification and pressurization rate. When controlling pressure with a mixing jet, the velocity and temperature of the jet are important design parameters affecting the thermal destratification and pressure reduction time constants. In this work, a small-scale ground-based experiment was performed, as a precursor to a microgravity experiment, to investigate the effects of these variables on the pressurization and pressure control time constants in the tank and to assess the feasibility of using a forced jet mixer for reduced boil-off pressure control. Local pointwise temperature and pressure measurements, together with qualitative contours of the thermal field in the liquid, vapor, and wall region, were made to identify and characterize important self-pressurization and pressure control trends in 1 g. C1 [Barsi, Stephen] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Kassemi, Mohammad] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. RP Barsi, S (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM stephen.j.barsi@nasa.gov; mohammad.kassemi@nasa.gov FU Space Life and Physical Sciences Research and Applications Program; International Space Station Program at NASA FX Funding support from the Space Life and Physical Sciences Research and Applications Program and the International Space Station Program at NASA are gratefully acknowledged. NR 32 TC 1 Z9 1 U1 0 U2 1 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 1948-5085 EI 1948-5093 J9 J THERM SCI ENG APPL JI J. Therm. Sci. Eng. Appl. PD DEC PY 2013 VL 5 IS 4 AR 041005 DI 10.1115/1.4023891 PG 20 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA V40YZ UT WOS:000209515200005 ER PT J AU Barsi, S Kassemi, M AF Barsi, Stephen Kassemi, Mohammad TI Investigation of Tank Pressurization and Pressure Control-Part II: Numerical Modeling SO JOURNAL OF THERMAL SCIENCE AND ENGINEERING APPLICATIONS LA English DT Article AB A multizone model is used to predict both the self-pressurization and pressure control behavior of a ground-based experiment. The multizone model couples a finite element heat conduction model of the tank wall to the bulk conservation equations in the ullage and the liquid. Comparisons are made to the experimental data presented in a companion paper. Results suggest that the multizone model can predict self-pressurization behavior over a variety of test conditions. The model is also used to predict the pressure control behavior when a subcooled axial mixing jet is used to thermally destratify and cool the bulk liquid. For fast jet speeds, the multizone model does a reasonably predict the pressure collapse behavior. Comparisons were also made between the data and a homogeneous thermodynamic model. These comparisons highlight the deficiencies of the homogeneous modeling approach. C1 [Barsi, Stephen] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. [Kassemi, Mohammad] NASA Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. RP Barsi, S (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA. EM stephen.j.barsi@nasa.gov; mohammad.kassemi@nasa.gov FU Space Life and Physical Sciences Research and Applications Program; International Space Station Program at NASA FX Funding support from the Space Life and Physical Sciences Research and Applications Program and the International Space Station Program at NASA are gratefully acknowledged. NR 26 TC 1 Z9 1 U1 0 U2 0 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 1948-5085 EI 1948-5093 J9 J THERM SCI ENG APPL JI J. Therm. Sci. Eng. Appl. PD DEC PY 2013 VL 5 IS 4 AR 041006 DI 10.1115/1.4023892 PG 9 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA V40YZ UT WOS:000209515200006 ER PT J AU Benafan, O Noebe, RD Padula, SA Garg, A Clausen, B Vogel, S Vaidyanathan, R AF Benafan, O. Noebe, R. D. Padula, S. A., II Garg, A. Clausen, B. Vogel, S. Vaidyanathan, R. TI Temperature dependent deformation of the B2 austenite phase of a NiTi shape memory alloy SO INTERNATIONAL JOURNAL OF PLASTICITY LA English DT Article DE Shape memory alloy; Austenite deformation; Neutron diffraction; Stress induced martensite; Deformation map ID INDUCED MARTENSITIC-TRANSFORMATION; SITU NEUTRON-DIFFRACTION; SINGLE-CRYSTAL NITI; TI-NI; SUPERELASTIC NITI; CYCLIC DEFORMATION; CONSTITUTIVE MODEL; TEXTURE ANALYSIS; PSEUDOELASTICITY CHARACTERISTICS; MECHANICAL-PROPERTIES AB Temperature dependent deformation of the B2 austenite phase of a polycrystalline Ni49.9Ti50.1 (at.%) shape memory alloy was studied through combined macroscopic and microstructural characterization efforts. The objective was to determine mechanisms responsible for the macroscopic inelastic strains during isothermal loading of NiTi to 18% strain at temperatures above which the austenite phase exists in the nominally unloaded or stress-free condition (i.e., above the austenite finish temperature, A(f)). This study included in situ time-of-flight (TOF) neutron diffraction experiments used to follow the evolution of the lattice strains, texture, and phase fractions during deformation, ex situ macroscopic tensile experiments, and hot stage transmission electron microscopy (TEM). It was found that stress-induced martensite (SIM) formed at temperatures up to 310 degrees C, which is well above the stress-free A(f) of 105 degrees C. However, the stress induced martensite formed concurrently with general <001> slip processes and twinning by [114}(B2) compound deformation twins, and did not occur as a separate distinguishable mechanism. Above the temperature that martensite cannot form with stress or the martensite desist temperature, M-d, deformation was governed by the same slip and deformation twinning mechanisms, in addition to diffusion-assisted deformation processes. The overall results were combined to generate a deformation map that contained limits over which each of the identified deformation mechanisms was dominant in this Ni49.9Ti50.1 alloy. Published by Elsevier Ltd. C1 [Benafan, O.; Vaidyanathan, R.] Univ Cent Florida, Mech Mat & Aerosp Engn Dept, Adv Mat Proc & Anal Ctr AMPAC, Orlando, FL 32816 USA. [Benafan, O.; Noebe, R. D.; Padula, S. A., II; Garg, A.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. [Garg, A.] Univ Toledo, Toledo, OH 43606 USA. [Clausen, B.; Vogel, S.] Los Alamos Natl Lab, Lujan Ctr, Los Alamos, NM 87545 USA. RP Benafan, O (reprint author), NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. EM othmane.benafan@nasa.gov RI Clausen, Bjorn/B-3618-2015; OI Clausen, Bjorn/0000-0003-3906-846X; Vogel, Sven C./0000-0003-2049-0361 FU Supersonics Project [NNX08AB51A]; Aeronautical Sciences Project; NASA Fundamental Aeronautics Program; Los Alamos National Security LLC under DOE [DE-AC52-06NA25396] FX Funding from the NASA Fundamental Aeronautics Program, Supersonics Project including Grant No. NNX08AB51A, and Aeronautical Sciences Project is gratefully acknowledged. The authors thank D.W. Brown, T. Sisneros and M. Reiche at LANL and D. Gaydosh, G. Bigelow and S. Raj at NASA GRC for technical support and helpful discussions. D.E. Nicholson's help in performing the neutron diffraction experiments is gratefully acknowledged. This work has benefited from the use of the Lujan Neutron Scattering Center at LANSCE, which is funded by the Office of Basic Energy Sciences DOE. LANL is operated by Los Alamos National Security LLC under DOE Contract No. DE-AC52-06NA25396. NR 95 TC 29 Z9 29 U1 3 U2 39 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0749-6419 EI 1879-2154 J9 INT J PLASTICITY JI Int. J. Plast. PD DEC PY 2013 VL 51 BP 103 EP 121 DI 10.1016/j.ijplas.2013.06.003 PG 19 WC Engineering, Mechanical; Materials Science, Multidisciplinary; Mechanics SC Engineering; Materials Science; Mechanics GA 245AC UT WOS:000326430300006 ER PT J AU Iurlaro, L Gherlone, M Di Sciuva, M Tessler, A AF Iurlaro, L. Gherlone, M. Di Sciuva, M. Tessler, A. TI Assessment of the Refined Zigzag Theory for bending, vibration, and buckling of sandwich plates: a comparative study of different theories SO COMPOSITE STRUCTURES LA English DT Article DE Sandwich plate; Free vibration; Buckling; Refined Zigzag Theory; Shear correction factor ID CONTINUOUS INTERLAMINAR STRESSES; LAMINATED COMPOSITE; FINITE-ELEMENT; CORE; SHEAR; MODELS; BEAMS; DEFORMATION; FORMULATION; STABILITY AB The Refined Zigzag Theory (RZT) belongs to the zigzag class of approximations for the analysis of laminated composite and sandwich structures. This paper presents the derivation of the non-linear equations of motion and consistent boundary conditions of RZT for multilayered plates. Subsequently, the equations are specialized to the linear boundary value problem of bending and the linear eigenvalue problems of free vibrations and buckling. In order to assess the accuracy of RZT, results concerning the static response, the free vibration frequencies and modal shapes, and the buckling loads of symmetric and un-symmetric sandwich plates, both simply supported and clamped and subjected to several loading conditions, are compared to the three-dimensional exact elasticity solution, high-fidelity FEM solutions, classical and zigzag theories, and accurate layer-wise models or solutions obtained in the open literature by means of other methods. The numerical investigation shows that RZT is highly accurate in predicting the static response, the natural frequencies and the buckling loads of sandwich plates without requiring any shear correction factors. In virtue of its accuracy and of the C-0-continuity requirement for shape functions, RZT can be adopted to derive reliable and computationally efficient finite elements suited for large-scale analyses of sandwich structures. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Iurlaro, L.; Gherlone, M.; Di Sciuva, M.] Politecn Torino, Dept Mech & Aerosp Engn, I-10129 Turin, Italy. [Tessler, A.] NASA, Struct Mech & Concepts Branch, Langley Res Ctr, Hampton, VA 23681 USA. RP Iurlaro, L (reprint author), Politecn Torino, Dept Mech & Aerosp Engn, Corso Duca Abruzzi 24, I-10129 Turin, Italy. EM luigi.iurlaro@polito.it; marco.gherlone@polito.it; marco.disciuva@polito.it; alexander.tessler-1@nasa.gov OI Gherlone, Marco/0000-0002-5711-0046 NR 59 TC 11 Z9 11 U1 2 U2 25 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0263-8223 EI 1879-1085 J9 COMPOS STRUCT JI Compos. Struct. PD DEC PY 2013 VL 106 BP 777 EP 792 DI 10.1016/j.compstruct.2013.07.019 PG 16 WC Materials Science, Composites SC Materials Science GA 231VY UT WOS:000325447700072 ER PT J AU Barut, A Madenci, E Tessler, A AF Barut, A. Madenci, E. Tessler, A. TI C-0-continuous triangular plate element for laminated composite and sandwich plates using the {2,2} - Refined Zigzag Theory SO COMPOSITE STRUCTURES LA English DT Article DE Sandwich construction; Zigzag functions; Single-layer theory; Finite element ID SHEAR-DEFORMATION-THEORY; SHELLS; BEAMS; FLEXURE; STRESS; PANELS AB Most of the existing plate elements assume constant transverse displacement across the thickness resulting in zero transverse stretch deformation. This study presents a new triangular finite element for modeling thick laminates and sandwich panels based on the {2,2}order refined zigzag plate theory. It adopts quadratic through-thickness variation of the in-plane and transverse displacement components. The transverse normal strain is calculated based on the assumption of cubic representation of the transverse normal stress. The zigzag functions are piecewise linear through the thickness. The element consists of 3 corner nodes and 3 mid-side nodes along the edges. Each corner and mid-side node has 11 and 3 degrees of freedom (DOF), respectively. This C-0 ontinuous element is free of geometric locking, and does not require shear correction factors. It provides robust and accurate prediction of all six stress components (in-plane and transverse normal and shear stresses) in the analysis of highly heterogeneous laminates and sandwich plates. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Barut, A.; Madenci, E.] Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA. [Tessler, A.] NASA, Struct Mech & Concepts Branch, Langley Res Ctr, Hampton, VA 23665 USA. RP Madenci, E (reprint author), Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA. EM atila@email.arizona.edu; madenci@email.arizona.edu; Alexander.Tessler-1@nasa.gov NR 42 TC 5 Z9 5 U1 1 U2 14 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0263-8223 EI 1879-1085 J9 COMPOS STRUCT JI Compos. Struct. PD DEC PY 2013 VL 106 BP 835 EP 853 DI 10.1016/j.compstruct.2013.07.024 PG 19 WC Materials Science, Composites SC Materials Science GA 231VY UT WOS:000325447700077 ER PT J AU Ganesan, D Lindvall, M McComas, D Bartholomew, M Siegel, S Medina, B Krikhaar, R Verhoef, C Montgomery, LP AF Ganesan, Dharmalingam Lindvall, Mikael McComas, David Bartholomew, Maureen Siegel, Steve Medina, Barbara Krikhaar, Rene Verhoef, Chris Montgomery, Lisa P. TI An analysis of unit tests of a flight software product line SO SCIENCE OF COMPUTER PROGRAMMING LA English DT Article DE Unit testing; Stub; Metrics; Software architecture; Self-testable components; Flight software AB This paper presents an analysis of the unit testing approach developed and used by the Core Flight Software System (CFS) product line team at the NASA Goddard Space Flight Center (GSFC). The goal of the analysis is to understand, review, and recommend strategies for improving the CFS' existing unit testing infrastructure as well as to capture lessons learned and best practices that can be used by other software product line (SPL) teams for their unit testing. The results of the analysis show that the core and application modules of the CFS are unit tested in isolation using a stub framework developed by the CFS team. The application developers can unit test their code without waiting for the core modules to be completed, and vice versa. The analysis found that this unit testing approach incorporates many practical and useful solutions such as allowing for unit testing without requiring hardware and special OS features in-the-loop by defining stub implementations of dependent modules. These solutions are worth considering when deciding how to design the testing architecture for a SPL. (C) 2012 Elsevier B.V. All rights reserved. C1 [Ganesan, Dharmalingam; Lindvall, Mikael] Fraunhofer Ctr Expt Software Engn, College Pk, MD 20740 USA. [McComas, David; Bartholomew, Maureen; Siegel, Steve; Medina, Barbara] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krikhaar, Rene; Verhoef, Chris] Vrije Univ Amsterdam, Dept Comp Sci, NL-1081 HV Amsterdam, Netherlands. [Montgomery, Lisa P.] NASA, Independent Verificat & Validat Facil, Fairmont, WV 26554 USA. RP Ganesan, D (reprint author), Fraunhofer Ctr Expt Software Engn, College Pk, MD 20740 USA. EM dganesan@fc-md.umd.edu; mlindvall@fc-md.umd.edu; david.c.mccomas@nasa.gov; maureen.o.bartholomew@nasa.gov; steve.slegel@nasa.gov; barbara.b.medina@nasa.gov; rkrikhaa@few.vu.nl; x@cs.vu.nl; lisa.p.montgomery@nasa.gov NR 25 TC 2 Z9 2 U1 0 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-6423 EI 1872-7964 J9 SCI COMPUT PROGRAM JI Sci. Comput. Program. PD DEC 1 PY 2013 VL 78 IS 12 BP 2360 EP 2380 DI 10.1016/j.scico.2012.02.006 PG 21 WC Computer Science, Software Engineering SC Computer Science GA 234SL UT WOS:000325664500006 ER PT J AU Wang, H Harrison, KW AF Wang, Hui Harrison, Kenneth W. TI Bayesian approach to contaminant source characterization in water distribution systems: adaptive sampling framework SO STOCHASTIC ENVIRONMENTAL RESEARCH AND RISK ASSESSMENT LA English DT Article DE Uncertainty; Inverse modeling; Source identification; Adaptive sampling; Value of information; Data worth framework; Bayesian preposterior analysis ID CLIMATE-CHANGE UNCERTAINTY; DECISION-ANALYSIS; NETWORKS; WORTH; IDENTIFICATION; REMEDIATION; DESIGN AB Bayesian analysis can yield a probabilistic contaminant source characterization conditioned on available sensor data and accounting for system stochastic processes. This paper is based on a previously proposed Markov chain Monte Carlo (MCMC) approach tailored for water distribution systems and incorporating stochastic water demands. The observations can include those from fixed sensors and, the focus of this paper, mobile sensors. Decision makers, such as utility managers, need not wait until new observations are available from an existing sparse network of fixed sensors. This paper addresses a key research question: where is the best location in the network to gather additional measurements so as to maximize the reduction in the source uncertainty? Although this has been done in groundwater management, it has not been well addressed in water distribution networks. In this study, an adaptive framework is proposed to guide the strategic placement of mobile sensors to complement the fixed sensor network. MCMC is the core component of the proposed adaptive framework, while several other pieces are indispensable: Bayesian preposterior analysis, value of information criterion and the search strategy for identifying an optimal location. Such a framework is demonstrated with an illustrative example, where four candidate sampling locations in the small water distribution network are investigated. Use of different value-of-information criteria reveals that while each may lead to different outcomes, they share some common characteristics. The results demonstrate the potential of Bayesian analysis and the MCMC method for contaminant event management. C1 [Wang, Hui] Univ Texas Austin, Bur Econ Geol, Austin, TX 78758 USA. [Harrison, Kenneth W.] Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Harrison, Kenneth W.] NASA, Hydrol Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wang, H (reprint author), Univ Texas Austin, Bur Econ Geol, Austin, TX 78758 USA. EM hui.wang@beg.utexas.edu FU National Science Foundation (NSF) [0849064] FX This work was supported by National Science Foundation (NSF) under Award No. 0849064. Any opinions, findings and conclusion expressed in this materials are those of the authors and do not necessarily reflect the views of the NSF. NR 26 TC 3 Z9 3 U1 2 U2 24 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1436-3240 J9 STOCH ENV RES RISK A JI Stoch. Environ. Res. Risk Assess. PD DEC PY 2013 VL 27 IS 8 BP 1921 EP 1928 DI 10.1007/s00477-013-0727-9 PG 8 WC Engineering, Environmental; Engineering, Civil; Environmental Sciences; Statistics & Probability; Water Resources SC Engineering; Environmental Sciences & Ecology; Mathematics; Water Resources GA 230WI UT WOS:000325373600011 ER PT J AU Seidt, JD Pereira, JM Gilat, A Revilock, DM Nandwana, K AF Seidt, Jeremy D. Pereira, J. Michael Gilat, Amos Revilock, Duane M. Nandwana, Kapil TI Ballistic impact of anisotropic 2024 aluminum sheet and plate SO INTERNATIONAL JOURNAL OF IMPACT ENGINEERING LA English DT Article DE Aluminum; Sheet; Plate; Plasticity; Anisotropy ID NOSE STEEL PROJECTILES; SHAPED CHARGE; PERFORATION; METALS; PENETRATION AB 2024 Aluminum sheet and plate are known to have anisotropic strength characteristics with regard to plasticity. However, numerical investigations of the impact behavior of sheet metals rarely consider anisotropic behavior. The effect of anisotropy in an impacted 2024 aluminum target is investigated experimentally and numerically. Normal impact experiments of titanium alloy and tool steel projectiles, with impact velocities ranging from 190 to 299 m/s, into 3.175 mm thick 2024-T3 sheet and 12.7 mm thick 2024-T351 plate are presented. Rear surface strains and displacements are measured using three-dimensional digital image correlation (DIC). Simulations of selected impact experiments, using a six-component anisotropic plasticity model for the target, are compared to the experimental data. Two model parameter sets are used. The first set accounts for initial anisotropic strength properties of the target, while the second reduces to an isotropic (von Mises) yield function. The objective of the numerical simulations is to study the difference in the results between the anisotropic and isotropic parameter sets. Results show that the yield function parameters used for simulations of both the 3.175 mm sheet and 12.7 mm plate have a significant effect on the calculated residual velocity of the projectile. The anisotropic parameter set simulations agree with experimental rear surface panel displacements and strains for both target thicknesses. There is experimental evidence of anisotropic deformation behavior only in the case of the 3.175 mm thick 2024-T3 target panels. The results demonstrate that the form of the yield function has a significant effect on the results of the impact simulations. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Seidt, Jeremy D.; Gilat, Amos; Nandwana, Kapil] Ohio State Univ, Dept Mech & Aerosp Engn, Columbus, OH 43210 USA. [Pereira, J. Michael; Revilock, Duane M.] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Seidt, JD (reprint author), Ohio State Univ, Dept Mech & Aerosp Engn, Columbus, OH 43210 USA. EM seidt.2@osu.edu FU Federal Aviation Administration (FAA) FX This work was funded by the Federal Aviation Administration (FAA). Thanks to Don Altobelli, Bill Emmerling and Dr. Chip Queitzsch of the FAA. The authors would like to acknowledge the useful advice and assistance of Kelly Carney and Charles Ruggeri of the NASA Glenn Research Center Ballistic Impact Facility and Murat Buyuk of the George Washington University National Crash Analysis Center. This work was supported in part by an allocation of computing time from the Ohio Supercomputer Center (OSC). NR 32 TC 3 Z9 3 U1 1 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0734-743X J9 INT J IMPACT ENG JI Int. J. Impact Eng. PD DEC PY 2013 VL 62 BP 27 EP 34 DI 10.1016/j.ijimpeng.2013.06.001 PG 8 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA 224OZ UT WOS:000324899300003 ER PT J AU Fortenberry, RC AF Fortenberry, Ryan C. TI Singlet excited states of anions with higher main group elements SO MOLECULAR PHYSICS LA English DT Article DE anions; electronically excited states; valence excited states; dipole-bound states; coupled cluster theory ID DIFFUSE INTERSTELLAR BANDS; COUPLED-CLUSTER METHOD; CORRELATED MOLECULAR CALCULATIONS; ACETALDEHYDE ENOLATE ANION; NEUTRAL-NEUTRAL REACTION; DIPOLE-BOUND ANIONS; GAUSSIAN-BASIS SETS; AB-INITIO; AUTODETACHMENT SPECTROSCOPY; ELECTRONIC STATES AB Previous studies have shown that dipole-bound excited states exist for certain small anions. However, valence excited states have been reported for some closed-shell anions, but those with singlet valence excited states have, thus far, contained a single silicon atom. This work uses high-level coupled cluster theory previously shown to reproduce excited state energies to better than 0.1 eV compared with experiment in order to examine the electronic excited state properties of anions containing silicon and other higher main group atoms as well as their first row analogues. Of the 14 anions involved in this study, 9 possess bound excited states of some kind: CH2SN-, C3H-, CCSiH-, CCSH-, CCNH2-, CCPH2-, BH3PH2-, AlH3NH2- and AlH3PH2-. Two possess clear valence states: CCSiH- and its first row analogue C3H-. Substantial mixing appears to be present in the valence and dipole-bound characters for the first excited state wavefunctions of many of the systems reporting excited states, but the mixing is most pronounced with the ammonia borane-like AlH3NH2-, and AlH3PH2- anions. Inclusion of second row atoms in anions whose corresponding radical is strongly dipolar increases the likelihood for the existence of excited states of any kind, but among the systems considered to date with this methodology, only the nature of group 14 atoms in small, closed-shell anions has yet been shown to allow valence singlet excited states. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Fortenberry, RC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM ryan.c.fortenberry@nasa.gov FU NASA; U.S. National Science Foundation [CHE-1058420]; Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) [CHE-0741927]; Virginia Space Grant Consortium FX RCF is currently funded by the NASA Postdoctoral Program administered through Oak Ridge Associated Universities. Funding for this work has also come from the U.S. National Science Foundation: award CHE-1058420 and a Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) award CHE-0741927 and by the Virginia Space Grant Consortium in the form of a Graduate Research Fellowship for RCF. The figures were generated in part with the CheMVP program made available by Dr. Andrew Simmonett of the University of Georgia. RCF would like to thank Dr. David Woon of the University of Illinois for discussions regarding the bonding of the higher row atoms and Dr. Fabio Carelli of Spienza-University of Rome for insights into the nature of electronic excitations and binding in anions. Dr. Timothy J. Lee of the NASA Ames Research Center is also due thanks for his encouragement on finalising this project. The author acknowledges Lauren F. Fortenberry for her continual support and for her assistance in editing the manuscript. Finally, a tremendous debt of gratitude is owed to Prof. T. Daniel Crawford of Virginia Tech for many things including, but not limited to, providing the computer resources necessary to execute the computations for this study, guiding many aspects of the research, and for assistance in editing the manuscript. NR 82 TC 15 Z9 15 U1 0 U2 4 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0026-8976 EI 1362-3028 J9 MOL PHYS JI Mol. Phys. PD NOV 30 PY 2013 VL 111 IS 21 BP 3265 EP 3275 DI 10.1080/00268976.2013.780105 PG 11 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 267WI UT WOS:000328128600011 ER PT J AU Popova, OP Jenniskens, P Emel'yanenko, V Kartashova, A Biryukov, E Khaibrakhmanov, S Shuvalov, V Rybnov, Y Dudorov, A Grokhovsky, VI Badyukov, DD Yin, QZ Gural, PS Albers, J Granvik, M Evers, LG Kuiper, J Kharlamov, V Solovyov, A Rusakov, YS Korotkiy, S Serdyuk, I Korochantsev, AV Larionov, MY Glazachev, D Mayer, AE Gisler, G Gladkovsky, SV Wimpenny, J Sanborn, ME Yamakawa, A Verosub, KL Rowland, DJ Roeske, S Botto, NW Friedrich, JM Zolensky, ME Le, L Ross, D Ziegler, K Nakamura, T Ahn, I Lee, JI Zhou, Q Li, XH Li, QL Liu, Y Tang, GQ Hiroi, T Sears, D Weinstein, IA Vokhmintsev, AS Ishchenko, AV Schmitt-Kopplin, P Hertkorn, N Nagao, K Haba, MK Komatsu, M Mikouchi, T AF Popova, Olga P. Jenniskens, Peter Emel'yanenko, Vacheslav Kartashova, Anna Biryukov, Eugeny Khaibrakhmanov, Sergey Shuvalov, Valery Rybnov, Yurij Dudorov, Alexandr Grokhovsky, Victor I. Badyukov, Dmitry D. Yin, Qing-Zhu Gural, Peter S. Albers, Jim Granvik, Mikael Evers, Laslo G. Kuiper, Jacob Kharlamov, Vladimir Solovyov, Andrey Rusakov, Yuri S. Korotkiy, Stanislav Serdyuk, Ilya Korochantsev, Alexander V. Larionov, Michail Yu. Glazachev, Dmitry Mayer, Alexander E. Gisler, Galen Gladkovsky, Sergei V. Wimpenny, Josh Sanborn, Matthew E. Yamakawa, Akane Verosub, Kenneth L. Rowland, Douglas J. Roeske, Sarah Botto, Nicholas W. Friedrich, Jon M. Zolensky, Michael E. Le, Loan Ross, Daniel Ziegler, Karen Nakamura, Tomoki Ahn, Insu Lee, Jong Ik Zhou, Qin Li, Xian-Hua Li, Qiu-Li Liu, Yu Tang, Guo-Qiang Hiroi, Takahiro Sears, Derek Weinstein, Ilya A. Vokhmintsev, Alexander S. Ishchenko, Alexei V. Schmitt-Kopplin, Phillipe Hertkorn, Norbert Nagao, Keisuke Haba, Makiko K. Komatsu, Mutsumi Mikouchi, Takashi CA Chelyabinsk Airburst Consortiu TI Chelyabinsk Airburst, Damage Assessment, Meteorite Recovery, and Characterization SO SCIENCE LA English DT Article ID ORDINARY CHONDRITES; ASTEROIDS; FAMILY; EARTH; METEOROIDS; PHOSPHATES; ITOKAWA; ORIGIN; FALLS AB The asteroid impact near the Russian city of Chelyabinsk on 15 February 2013 was the largest airburst on Earth since the 1908 Tunguska event, causing a natural disaster in an area with a population exceeding one million. Because it occurred in an era with modern consumer electronics, field sensors, and laboratory techniques, unprecedented measurements were made of the impact event and the meteoroid that caused it. Here, we document the account of what happened, as understood now, using comprehensive data obtained from astronomy, planetary science, geophysics, meteorology, meteoritics, and cosmochemistry and from social science surveys. A good understanding of the Chelyabinsk incident provides an opportunity to calibrate the event, with implications for the study of near-Earth objects and developing hazard mitigation strategies for planetary protection. C1 [Popova, Olga P.; Shuvalov, Valery; Rybnov, Yurij; Kharlamov, Vladimir; Glazachev, Dmitry] Russian Acad Sci, Inst Dynam Geospheres, Moscow 119334, Russia. [Jenniskens, Peter; Gural, Peter S.; Albers, Jim] SETI Inst, Mountain View, CA 94043 USA. [Emel'yanenko, Vacheslav; Kartashova, Anna] Russian Acad Sci, Inst Astron, Moscow 119017, Russia. [Biryukov, Eugeny] South Ural State Univ, Dept Theoret Mech, Chelyabinsk 454080, Russia. [Khaibrakhmanov, Sergey; Dudorov, Alexandr; Mayer, Alexander E.] Chelyabinsk State Univ, Chelyabinsk 454001, Russia. [Grokhovsky, Victor I.; Larionov, Michail Yu.; Weinstein, Ilya A.; Vokhmintsev, Alexander S.; Ishchenko, Alexei V.] Ural Fed Univ, Inst Phys & Technol, Ekaterinburg 620002, Russia. [Badyukov, Dmitry D.; Korochantsev, Alexander V.] RAS, Vernadsky Inst Geochem & Analyt Chem, Moscow 119991, Russia. [Yin, Qing-Zhu; Wimpenny, Josh; Sanborn, Matthew E.; Yamakawa, Akane; Verosub, Kenneth L.; Roeske, Sarah; Botto, Nicholas W.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Granvik, Mikael] Univ Helsinki, Dept Phys, Helsinki 00014, Finland. [Evers, Laslo G.; Kuiper, Jacob] Koninklijk Nederlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. [Evers, Laslo G.] Delft Univ Technol, Fac Civil Engn & Geosci, Dept Geosci & Engn, NL-2600 GA Delft, Netherlands. [Solovyov, Andrey] Tomsk State Univ, Tomsk 634050, Russia. [Rusakov, Yuri S.] Res & Prod Assoc Typhoon, Obninsk 249032, Russia. [Korotkiy, Stanislav] Support Fdn Astron Ka Dar, Razvilka 142717, Russia. [Weinstein, Ilya A.] Social & Youth Initiat Org, Sci & Technol Ctr, Moscow 119415, Russia. [Gisler, Galen] Univ Oslo, N-0316 Oslo, Norway. [Gladkovsky, Sergei V.] Russian Acad Sci, Inst Engn Sci, Urals Branch, Ekaterinburg 620049, Russia. [Rowland, Douglas J.] Univ Calif Davis, Ctr Mol & Genom Imaging, Davis, CA 95616 USA. [Friedrich, Jon M.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. [Friedrich, Jon M.] Fordham Univ, Dept Chem, Bronx, NY 10458 USA. [Zolensky, Michael E.; Le, Loan; Ross, Daniel] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Le, Loan; Ross, Daniel] Jacobs Technol, Houston, TX 77058 USA. [Ziegler, Karen] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Nakamura, Tomoki; Ahn, Insu] Tohoku Univ, Dept Earth & Planetary Mat Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Lee, Jong Ik] Korea Polar Res Inst, Div Polar Earth Syst Sci, Inchon 406840, South Korea. [Zhou, Qin] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Zhou, Qin; Li, Xian-Hua; Li, Qiu-Li; Liu, Yu; Tang, Guo-Qiang] Chinese Acad Sci, Inst Geol & Geophys, State Key Lab Lithospher Evolut, Beijing 100029, Peoples R China. [Hiroi, Takahiro] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Schmitt-Kopplin, Phillipe; Hertkorn, Norbert] Helmoltz Zentrum Muenchen, D-85764 Obeschleissheim, Germany. [Schmitt-Kopplin, Phillipe] Tech Univ Munich, D-85354 Freising Weihenstephan, Germany. [Nagao, Keisuke; Haba, Makiko K.] Univ Tokyo, Geochem Res Ctr, Bunkyo Ku, Tokyo 1130033, Japan. [Komatsu, Mutsumi] Waseda Univ, Waseda Inst Adv Study, Shinjuku Ku, Tokyo 1698050, Japan. [Mikouchi, Takashi] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan. RP Jenniskens, P (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA. EM petrus.m.jenniskens@nasa.gov RI Schmitt-Kopplin, Philippe/H-6271-2011; Dudorov, Alexander/P-4773-2015; Weinstein, Ilya/K-8178-2012; Gladkovsky, Sergei/E-5731-2016; Popova, Olga/K-1885-2012; Yin, Qing-Zhu/B-8198-2009; Kartashova, Anna/N-3468-2013; Emel'yanenko, Vacheslav/A-4087-2014; Shuvalov, Valery/C-6618-2014; Ishchenko, Aleksey/E-1017-2014; Evers, Laslo/E-5707-2011; Rowland, Douglas/F-3104-2014; Solovyov, Andrey/G-8268-2014; Soloviev, Andrey/P-1761-2014; Mayer, Alexander/I-3069-2013; Khaibrakhmanov, Sergey/G-7264-2015 OI Schmitt-Kopplin, Philippe/0000-0003-0824-2664; Weinstein, Ilya/0000-0002-5573-7128; Gladkovsky, Sergei/0000-0002-3542-6242; Li, Qiuli/0000-0002-7280-5508; Sanborn, Matthew/0000-0003-3218-1195; Granvik, Mikael/0000-0002-5624-1888; Yin, Qing-Zhu/0000-0002-4445-5096; Kartashova, Anna/0000-0003-4320-5105; Ishchenko, Aleksey/0000-0002-9883-6652; Evers, Laslo/0000-0003-2825-6211; Rowland, Douglas/0000-0001-8059-6905; Mayer, Alexander/0000-0002-8765-6373; Khaibrakhmanov, Sergey/0000-0002-4439-6831 FU Institute for Dynamics of Geospheres; Federal Targeted Program Scientific and Educational Human Resources of Innovation-Driven Russia; RAS Presidium Program Fundamental Problems of Investigation and Exploration of the Solar System; NASA FX The Russian Academy of Sciences (RAS) field study of the Chelyabinsk airburst was supported by the Institute for Dynamics of Geospheres and grants of the Federal Targeted Program Scientific and Educational Human Resources of Innovation-Driven Russia and the RAS Presidium Program Fundamental Problems of Investigation and Exploration of the Solar System. The office of Chelyabinsk Oblast Governor Mikhail Yurevich provided assistance. S. Petukhov and I. Talyukin from the Universe History Museum in Dedovsk contributed samples, as did M. Boslough of Sandia National Laboratories. U. Johann (Astrium Satellites GmbH) calculated the Chebarkul hole position from Pleiades 1A satellite observations. D. F. Blake provided use of a petrographic microscope. P.J. acknowledges support from the NASA Near Earth Object Observation Program, Q.Z.Y. and M.E.Z. from the NASA Cosmochemistry Program, and M. G. from the Academy of Finland. NR 39 TC 118 Z9 122 U1 10 U2 97 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD NOV 29 PY 2013 VL 342 IS 6162 BP 1069 EP 1073 DI 10.1126/science.1242642 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 259HS UT WOS:000327518600050 PM 24200813 ER PT J AU Olsen, SC Brasseur, GP Wuebbles, DJ Barrett, SRH Dang, HY Eastham, SD Jacobson, MZ Khodayari, A Selkirk, H Sokolov, A Unger, N AF Olsen, Seth C. Brasseur, Guy P. Wuebbles, Donald J. Barrett, Steven R. H. Dang, Hongyan Eastham, Sebastian D. Jacobson, Mark Z. Khodayari, Arezoo Selkirk, Henry Sokolov, Andrei Unger, Nadine TI Comparison of model estimates of the effects of aviation emissions on atmospheric ozone and methane SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE aviation; radiative forcing; climate ID AIRCRAFT NOX EMISSIONS; TRAFFIC EMISSIONS; CLIMATE; IMPACT; CHEMISTRY; SIMULATIONS; OH AB One of the significant uncertainties in understanding the effects of aviation on climate is the effects of aviation emissions on ozone and atmospheric chemistry. In this study the effects of aviation emissions on atmospheric ozone for 2006 and two projections for 2050 are compared among seven models. The models range in complexity from a two-dimensional coupled model to three-dimensional offline and fully coupled three-dimensional chemistry-climate models. This study is the first step in a critical assessment and comparison among these model results. Changes in tropospheric O-3 burdens range from 2.3 Tg-O-3/Tg-N to 3.0 Tg-O-3/Tg-N, ozone radiative forcings range from 6 to 37 mW/m(2), and methane radiative forcings range from -8.3 to -12.5 mW/m(2) for the 2006 aviation emissions. As a group, the chemistry transport models tend to have similar responses while the fully coupled models tend to separate from this group and do not show similar responses to each other. C1 [Olsen, Seth C.; Wuebbles, Donald J.] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA. [Brasseur, Guy P.] Helmholtz Zentrum Geesthacht, Climate Serv Ctr, Hamburg, Germany. [Brasseur, Guy P.] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Barrett, Steven R. H.; Eastham, Sebastian D.] MIT, Dept Aeronaut & Astronaut, Lab Aviat & Environm, Cambridge, MA 02139 USA. [Dang, Hongyan; Unger, Nadine] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Jacobson, Mark Z.] Stanford Univ, Dept Civil & Environm Engn, Stanford, CA 94305 USA. [Khodayari, Arezoo] Univ Illinois, Dept Civil & Environm Engn, Urbana, IL 61801 USA. [Selkirk, Henry] NASA, Goddard Space Flight Ctr, Goddard Earth Sci Technol & Res, Greenbelt, MD 20771 USA. [Sokolov, Andrei] MIT, Ctr Global Change Sci, Cambridge, MA 02139 USA. RP Olsen, SC (reprint author), Univ Illinois, Dept Atmospher Sci, 105 S Gregory, Urbana, IL 61801 USA. EM solsen@illinois.edu RI Unger, Nadine/M-9360-2015; OI Eastham, Sebastian/0000-0002-2476-4801 FU Federal Aviation Administration, Aviation Climate Change Research Initiative (ACCRI) [10-C-NE-UI amendment 001]; U.S. Department of Transportation; Illinois Department of Transportation; Transportation Research and Analysis Computing Center FX The authors would like to thank the Federal Aviation Administration, Aviation Climate Change Research Initiative (ACCRI) for support under contract: 10-C-NE-UI amendment 001 and The Partnership for Air Transportation Noise and Emissions Reduction (PARTNER). The opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of ACCRI, PARTNER, or the FAA. This work was partially supported by the U.S. Department of Transportation, the Illinois Department of Transportation, and the Transportation Research and Analysis Computing Center. NR 35 TC 6 Z9 6 U1 2 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 28 PY 2013 VL 40 IS 22 BP 6004 EP 6009 DI 10.1002/2013GL057660 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 268ZX UT WOS:000328210600033 ER PT J AU Zwart, SR Parsons, H Kimlin, M Innis, SM Locke, JP Smith, SM AF Zwart, Sara R. Parsons, Howard Kimlin, Michael Innis, Sheila M. Locke, James P. Smith, Scott M. TI A 250 mu g/week dose of vitamin D was as effective as a 50 mu g/d dose in healthy adults, but a regimen of four weekly followed by monthly doses of 1250 mu g raised the risk of hypercalciuria SO BRITISH JOURNAL OF NUTRITION LA English DT Article DE Vitamin D; Dietary supplements; Hypercalciuria; Sunlight ID D DEFICIENCY; SUPPLEMENTATION; CALCIUM; PREVENTION; WINTER; D-2 AB The risk of vitamin D insufficiency is increased in persons having limited sunlight exposure and dietary vitamin D. Supplementation compliance might be improved with larger doses taken less often, but this may increase the potential for side effects. The objective of the present study was to determine whether a weekly or weekly/monthly regimen of vitamin D supplementation is as effective as daily supplementation without increasing the risk of side effects. Participants were forty-eight healthy adults who were randomly assigned for 3 months to placebo or one of three supplementation regimens: 50 mu g/d (2000 IU/d, analysed dose 70 mu g/d), 250 mu g/week (10 000 IU/week, analysed dose 331 mu g/week) or 1250 mu g/week (50 000 IU/week, analysed dose 1544 mu g/week) for 4 weeks and then 1250 mu g/month for 2 months. Daily and weekly doses were equally effective at increasing serum 25-hydroxyvitamin D, which was significantly greater than baseline in all the supplemented groups after 30 d of treatment. Subjects in the 1250 mu g treatment group, who had a BMI >26 kg/m(2), had a steady increase in urinary Ca in the first 3 weeks of supplementation, and, overall, the relative risk of hypercalciuria was higher in the 1250 mu g group than in the placebo group (P = 0.01). Although vitamin D supplementation remains a controversial issue, these data document that supplementing with <= 250 mu g/week (<= 10 000 IU/week) can improve or maintain vitamin D status in healthy populations without the risk of hypercalciuria, but 24 h urinary Ca excretion should be evaluated in healthy persons receiving vitamin D-3 supplementation in weekly single doses of 1250 mu g (50 000 IU). C1 [Zwart, Sara R.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA. [Parsons, Howard; Innis, Sheila M.] British Columbia Childrens Hosp, Dept Paediat, Div GI Nutr, Vancouver, BC V6H 3V4, Canada. [Kimlin, Michael] Queensland Univ Technol, Inst Hlth & Biomed Innovat, Brisbane, Qld 4001, Australia. [Locke, James P.; Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Human Hlth & Performance Directorate, Houston, TX 77058 USA. RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Human Hlth & Performance Directorate, Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA. EM scott.m.smith@nasa.gov FU NASA Flight Analogs Project of NASA's Human Research Program FX The authors are indebted to the participants for their time and efforts in completing the study. We also thank the National Aeronautics and Space Administration (NASA) Nutritional Biochemistry Laboratory for their efforts in the implementation and sample processing for the study. We thank Jane Krauhs for editorial assistance. The present study was funded by the NASA Flight Analogs Project of NASA's Human Research Program. All authors had input to the design of the study. S. R. Z. and S. M. S. oversaw the data collection, management and statistical analysis. S. R. Z., M. K. and S. M. I. analysed the data. All authors interpreted the results of the experiments. S. R. Z. and S. M. S. drafted the manuscript. All authors edited and revised the manuscript, and approved the final version of the manuscript. The authors declare that they have no conflicts of interest. NR 23 TC 1 Z9 1 U1 0 U2 5 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND SN 0007-1145 EI 1475-2662 J9 BRIT J NUTR JI Br. J. Nutr. PD NOV 28 PY 2013 VL 110 IS 10 BP 1866 EP 1872 DI 10.1017/S000711451300113X PG 7 WC Nutrition & Dietetics SC Nutrition & Dietetics GA 250VF UT WOS:000326883600014 PM 23595003 ER PT J AU Martin, AC Krishnamurti, TN Lau, WKM AF Martin, Andrew C. Krishnamurti, T. N. Lau, William K. M. TI Absorbing aerosol-induced change in the early monsoon Arabian Sea low-level jet: Modeled transfer from anomalous heating to nondivergent kinetic energy SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Aerosols; Monsoon; Onset; Low-level Jet ID ASIAN SUMMER MONSOON; TIBETAN PLATEAU; SOUTH-ASIA; ONSET; PARAMETERIZATION; CLOUDS; DEFINITION; WIDESPREAD; CHEMISTRY; POLLUTION AB This study examines the impact of anomalous differential generation of available potential energy by absorbing aerosols on the transition and early active phases of the South Asian summer monsoon. Aerosol direct and indirect radiative forcings can modify tropospheric temperature profiles through direct absorption, scattering, and extended cloud lifetimes. Recent studies have suggested that over monthly and seasonal time scales, these effects can lead to modified flow and rainfall regimes in the South Asian monsoon region. Of special interest is the covariance of heating and temperature prior to active monsoon onset. It can be shown that anomalous generation of available potential energy due to absorption of shortwave radiation by aerosols can impact the cascade of energy from the local Hadley circulation to the monsoon nondivergent flow. In order to quantify the potential impact of aerosol radiative forcing and the resulting changes in monsoon onset timing and intensity, an ensemble of Weather Research and Forecasting with Chemistry regional weather and chemistry model forecasts are created for the South Asian summer monsoon region during May, June, and July. The forecasts including shortwave absorption by aerosol are compared to control forecasts in which aerosols only scatter shortwave radiation. The evolution of irrotational and nondivergent kinetic energy, generation of available potential energy and rainfall are presented. It is found that the ensemble with aerosol shortwave absorption contains on average a more intense dynamical onset over South India which is statistically significant compared to the ensemble variability. The more intense monsoon onset is related to a more intense Arabian Sea low-level jet. In the ensemble with shortwave absorption by aerosol, the early season monsoon rainfall is diminished over South India and enhanced over the Northeastern Indian states. C1 [Martin, Andrew C.; Krishnamurti, T. N.] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA. [Martin, Andrew C.] Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA. [Lau, William K. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Martin, AC (reprint author), Univ Calif San Diego, Dept Chem & Biochem, 2108 Urey Hall,9500 Gilman Dr, La Jolla, CA 92093 USA. EM mc@ucsd.edu RI Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 FU NASA GSRP [NNX09AL41H] FX NASA GSRP grant no. NNX09AL41H provided funding for this research. NR 43 TC 1 Z9 1 U1 1 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 27 PY 2013 VL 118 IS 22 BP 12566 EP 12576 DI 10.1002/2013JD019808 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297OY UT WOS:000330266000035 ER PT J AU Witek, ML Garay, MJ Diner, DJ Smirnov, A AF Witek, Marcin L. Garay, Michael J. Diner, David J. Smirnov, Alexander TI Aerosol optical depths over oceans: A view from MISR retrievals and collocated MAN and AERONET in situ observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosols; MISR; AOD retrievals; MAN; AERONET ID UNIFIED SATELLITE CLIMATOLOGY; SUN PHOTOMETERS; CLOUD DETECTION; MODIS; PRODUCTS; NETWORK; TREND; ASSIMILATION; CALIBRATION; VALIDATION AB In this study, aerosol optical depths over oceans are analyzed from satellite and surface perspectives. Multiangle Imaging SpectroRadiometer (MISR) aerosol retrievals are investigated and validated primarily against Maritime Aerosol Network (MAN) observations. Furthermore, AErosol RObotic NETwork (AERONET) data from 19 island and coastal sites is incorporated in this study. The 270 MISR/MAN comparison points scattered across all oceans were identified. MISR on average overestimates aerosol optical depths (AODs) by 0.04 as compared to MAN; the correlation coefficient and root-mean-square error are 0.95 and 0.06, respectively. A new screening procedure based on retrieval region characterization is proposed, which is capable of substantially reducing MISR retrieval biases. Over 1000 additional MISR/AERONET comparison points are added to the analysis to confirm the validity of the method. The bias reduction is effective within all AOD ranges. Setting a clear flag fraction threshold to 0.6 reduces the bias to below 0.02, which is close to a typical ground-based measurement uncertainty. Twelve years of MISR data are analyzed with the new screening procedure. The average over ocean AOD is reduced by 0.03, from 0.15 to 0.12. The largest AOD decrease is observed in high latitudes of both hemispheres, regions with climatologically high cloud cover. It is postulated that the screening procedure eliminates spurious retrieval errors associated with cloud contamination and cloud adjacency effects. The proposed filtering method can be used for validating aerosol and chemical transport models. C1 [Witek, Marcin L.; Garay, Michael J.; Diner, David J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Smirnov, Alexander] Sigma Space Corp, Lanham, MD USA. RP Witek, ML (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM marcin.l.witek@jpl.nasa.gov RI Witek, Marcin/G-9440-2016; Smirnov, Alexander/C-2121-2009 OI Smirnov, Alexander/0000-0002-8208-1304 FU National Aeronautics and Space Administration FX We thank the PIs and their staff for establishing and maintaining the 19 AERONET sites used in this investigation. We acknowledge the MAN program principal investigators and their staff for providing the data. We also thank three anonymous reviewers for their useful comments and criticism. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 65 TC 7 Z9 7 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 27 PY 2013 VL 118 IS 22 BP 12620 EP 12633 DI 10.1002/2013JD020393 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297OY UT WOS:000330266000001 ER PT J AU Gianelli, SM Lacis, AA Carlson, BE Hameed, S AF Gianelli, Scott M. Lacis, Andrew A. Carlson, Barbara E. Hameed, Sultan TI Evidence of a weakly absorbing intermediate mode of aerosols in AERONET data from Saharan and Sahelian sites SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE aerosols; Saharan dust; size distribution; AERONET ID OPTICAL DEPTH; MINERAL DUST; GLOBAL BURDEN; WEST-AFRICA; DESERT DUST; INSTRUMENT; RADIOMETER; RETRIEVAL; CAMPAIGN; AIRBORNE AB Accurate retrievals of aerosol size distribution are necessary to estimate aerosols' impact on climate and human health. The inversions of the Aerosol Robotic Network (AERONET) usually retrieve bimodal distributions. However, when the inversion is applied to Saharan and Sahelian dust, an additional mode of intermediate size between the coarse and fine modes is sometimes seen. This mode explains peculiarities in the behavior of the angstrom ngstrom exponent, along with the fine mode fraction retrieved using the spectral deconvolution algorithm, observed in a March 2006 dust storm. For this study, 15 AERONET sites in northern Africa and on the Atlantic are examined to determine the frequency and properties of the intermediate mode. The mode is observed most frequently at Ilorin in Nigeria. It is also observed at Capo Verde and multiple sites located within the Sahel but much less frequently at sites in the northern Sahara and the Canary Islands. The presence of the intermediate mode coincides with increases in angstrom ngstrom exponent, fine mode fraction, single-scattering albedo, and to a lesser extent percent sphericity. The angstrom ngstrom exponent decreases with increasing optical depth at most sites when the intermediate mode is present, but the fine mode fraction does not. Single-scattering albedo does not steadily decrease with fine mode fraction when the intermediate mode is present, as it does in typical mixtures of dust and biomass-burning aerosols. Continued investigation is needed to further define the intermediate mode's properties, determine why it differs from most Saharan dust, and identify its climate and health effects. C1 [Gianelli, Scott M.; Hameed, Sultan] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11790 USA. [Gianelli, Scott M.] St Josephs Coll, Dept Phys Sci, Patchogue, NY USA. [Gianelli, Scott M.] Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11550 USA. [Lacis, Andrew A.; Carlson, Barbara E.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Gianelli, SM (reprint author), SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11790 USA. EM sgianell@yahoo.com FU NASA [NNX07AP74A] FX The research for this project was funded through the NASA cooperative agreement NNX07AP74A. The authors are very thankful to AERONET and PHOTONS for establishing and maintaining the sites used in this work. The sun photometers are operated by Service d'Observation PHOTONS from CNRS-Lille 1 University. The principal investigators at the AERONET sites are Phillipe Goloub (Agoufou, Izana), Didier Tanre (Banizoumbou, Capo Verde, Dakar, DMN Maine Soroa, Ouagadougou), Brent Holben (Blida), Jean Louis Rajot (DMN Maine Soroa, Zinder Airport), Bernadette Chatenet (IER Cinzana, Zinder Airport), Rachel T. Pinker (Ilorin), Emilio Cuevas-Agullo (Izana, Santa Cruz Tenerife, Tamanrasset IMN), Francisco Javier Expssito Gonzalez (La Laguna), Bernard Mougenot (Saada), Benoit Duchemin (Saada), and Mohamed Mimouni (Tamanrasset IMN). The site managers are Franck Timouk (Agoufou), Bernadette Chatenet (Banizoumbou, Capo Verde, DMN Maine Soroa, IER Cinzana), Menouer Boughedaoui (Blida), Aboubacry Diallo (Dakar), Modibo Coulibaly (IER Cinzana), Issa Kone (IER Cinzana), Clement Akoshile (Ilorin), Ramon Ramos (Izana, Santa Cruz Tenerife, Tamanrasset IMN), Luc Blarel (Izana), Juan Pedro Diaz Gonzalez (La Laguna), Zouhair Benkhaldoun (Saada), Aziza Bounhir (Saada), Lahouari Zeudmi-Sahraoui (Tamanrasset IMN), Moussa Abdou Saley (Zinder Airport), and Moussa Mahamadou (Zinder Airport). The authors would also like to thank the reviewers, whose constructive criticism substantially improved the final manuscript. NR 34 TC 1 Z9 1 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 27 PY 2013 VL 118 IS 22 BP 12661 EP 12672 DI 10.1002/2013JD020342 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297OY UT WOS:000330266000011 ER PT J AU Han, Y Revercomb, H Cromp, M Gu, DG Johnson, D Mooney, D Scott, D Strow, L Bingham, G Borg, L Chen, Y DeSlover, D Esplin, M Hagan, D Jin, X Knuteson, R Motteler, H Predina, J Suwinski, L Taylor, J Tobin, D Tremblay, D Wang, CM Wang, LH Wang, LK Zavyalov, V AF Han, Yong Revercomb, Henry Cromp, Mike Gu, Degui Johnson, David Mooney, Daniel Scott, Deron Strow, Larrabee Bingham, Gail Borg, Lori Chen, Yong DeSlover, Daniel Esplin, Mark Hagan, Denise Jin, Xin Knuteson, Robert Motteler, Howard Predina, Joe Suwinski, Lawrence Taylor, Joe Tobin, David Tremblay, Denis Wang, Chunming Wang, Lihong Wang, Likun Zavyalov, Vladimir TI Suomi NPP CrIS measurements, sensor data record algorithm, calibration and validation activities, and record data quality SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE CrIS; CrIS SDR; Suomi NPP; JPSS; calibration; validation ID RADIOMETRIC CALIBRATION; SOUNDER AB The Cross-Track Infrared Sounder (CrIS) is a Fourier Transform Michelson interferometer instrument launched on board the Suomi National Polar-Orbiting Partnership (Suomi NPP) satellite on 28 October 2011. CrIS provides measurements of Earth view interferograms in three infrared spectral bands at 30 cross-track positions, each with a 3x3 array of field of views. The CrIS ground processing software transforms the measured interferograms into calibrated and geolocated spectra in the form of Sensor Data Records (SDRs) that cover spectral bands from 650 to 1095cm(-1), 1210 to 1750cm(-1), and 2155 to 2550cm(-1) with spectral resolutions of 0.625cm(-1), 1.25cm(-1), and 2.5cm(-1), respectively. During the time since launch a team of subject matter experts from government, academia, and industry has been engaged in postlaunch CrIS calibration and validation activities. The CrIS SDR product is defined by three validation stages: Beta, Provisional, and Validated. The product reached Beta and Provisional validation stages on 19 April 2012 and 31 January 2013, respectively. For Beta and Provisional SDR data, the estimated absolute spectral calibration uncertainty is less than 3ppm in the long-wave and midwave bands, and the estimated 3 sigma radiometric uncertainty for all Earth scenes is less than 0.3K in the long-wave band and less than 0.2K in the midwave and short-wave bands. The geolocation uncertainty for near nadir pixels is less than 0.4km in the cross-track and in-track directions. C1 [Han, Yong] NOAA, Ctr Satellite Applicat & Res, Natl Environm Satellite Data & Informat Serv, College Pk, MD 20740 USA. [Revercomb, Henry; Borg, Lori; DeSlover, Daniel; Knuteson, Robert; Taylor, Joe; Tobin, David] Univ Wisconsin, SSEC, Madison, WI USA. [Cromp, Mike; Predina, Joe; Suwinski, Lawrence] Exelis Inc, Ft Wayne, IN USA. [Gu, Degui; Hagan, Denise; Wang, Chunming; Wang, Lihong] Northrop Grumman Aerosp Syst, Redondo Beach, CA USA. [Johnson, David] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Mooney, Daniel] MIT, Lincoln Lab, Lexington, MA 02173 USA. [Scott, Deron; Bingham, Gail; Esplin, Mark; Zavyalov, Vladimir] Space Dynam Lab, North Logan, UT USA. [Strow, Larrabee; Motteler, Howard] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA. [Chen, Yong; Wang, Likun] Univ Maryland, ESSIC, College Pk, MD 20742 USA. [Jin, Xin; Tremblay, Denis] Earth Resources Technol Inc, Laurel, MD USA. RP Han, Y (reprint author), NOAA, Ctr Satellite Applicat & Res, Natl Environm Satellite Data & Informat Serv, College Pk, MD 20740 USA. EM yong.han@noaa.gov RI Han, Yong/F-5590-2010; Wang, Likun/B-7524-2008; Johnson, David/F-2376-2015; Chen, Yong/E-4321-2010 OI Han, Yong/0000-0002-0183-7270; Wang, Likun/0000-0001-5646-9746; Johnson, David/0000-0003-4399-5653; Chen, Yong/0000-0002-0279-9405 NR 26 TC 29 Z9 29 U1 2 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 27 PY 2013 VL 118 IS 22 BP 12734 EP 12748 DI 10.1002/2013JD020344 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297OY UT WOS:000330266000023 ER PT J AU Whaley, C Strong, K Adams, C Bourassa, AE Daffer, WH Degenstein, DA Fast, H Fogal, PF Manney, GL Mittermeier, RL Pavlovic, B Wiacek, A AF Whaley, C. Strong, K. Adams, C. Bourassa, A. E. Daffer, W. H. Degenstein, D. A. Fast, H. Fogal, P. F. Manney, G. L. Mittermeier, R. L. Pavlovic, B. Wiacek, A. TI Using FTIR measurements of stratospheric composition to identify midlatitude polar vortex intrusions over Toronto SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE ozone; polar vortex; filaments; intrusions; Toronto; FTIR ID FOURIER-TRANSFORM SPECTROMETER; GROUND-BASED OBSERVATIONS; CHEMICAL-TRANSPORT MODEL; ARCTIC OZONE LOSS; POTENTIAL VORTICITY; TRAJECTORY CALCULATIONS; SATELLITE-OBSERVATIONS; WAVE BREAKING; O-3 LOSS; WINTER AB Using 11 years of trace gas measurements made at the University of Toronto Atmospheric Observatory (43.66 degrees N, 79.40 degrees W) and Environment Canada's Centre for Atmospheric Research Experiments (44.23 degrees N, 79.78 degrees W), along with derived meteorological products, we identify a number of polar intrusion events, which are excursions of the polar vortex or filaments from the polar vortex extending down to midlatitudes. These events are characterized by enhanced stratospheric columns (12-50km) of hydrogen fluoride (HF), by diminished stratospheric columns of nitrous oxide (N2O), and by a scaled potential vorticity above 1.2 x 10(-4)s(-1). The events comprise 16%of winter/spring (November to April inclusive) Fourier transform infrared (FTIR) spectroscopic measurements from January 2002 to March 2013, and we find at least two events per year. The events are corroborated by Modele Isentrope du transport Meso-echelle de l'Ozone Stratospherique par Advection, Modern-Era Retrospective Analysis for Research and Applications potential vorticity maps, and Global Modeling Initiative N2O maps. During polar intrusion events, the stratospheric ozone (O-3) columns over Toronto are usually greater than when there is no event. Our O-3 measurements agree with the Optical Spectrograph and Infrared Imaging System satellite instrument and are further verified with the Earth Probe Total Ozone Mapping Spectrometer and Ozone Monitoring Instrument satellite observations. We find six cases out of 53 for which chemical O(3)depletion within the polar vortex led to a reduction in stratospheric O-3 columns over Toronto. We have thus identified a dynamical cause for most of the winter/spring variability of stratospheric trace gas columns observed at our midlatitude site. While there have been a number of prior polar intrusion studies, this is the first study to report in the context of 11 years of ground-based FTIR column measurements, providing insight into the frequency of midlatitude polar vortex intrusions and observations of upper stratospheric (25-50 km) intrusions. It is also the first to present HF measurements during multiple polar intrusions, which provided an excellent tracer for their identification. Key Points Polar vortex intrusions to mid-latitude detected in Toronto FTIR measurements Mid-latitude polar intrusions confirmed with MIMOSA, MERRA, GMI, OSIRIS, DMPs Dynamical cause for variability in 11 years of FTIR HCl, HF and N2O data C1 [Whaley, C.; Strong, K.; Adams, C.; Pavlovic, B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Adams, C.; Bourassa, A. E.; Degenstein, D. A.] Univ Saskatchewan, Dept Phys & Engn Phys, Saskatoon, SK, Canada. [Daffer, W. H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Fast, H.; Fogal, P. F.; Mittermeier, R. L.] Environm Canada, Air Qual Res Div, Atmospher Sci & Technol Directorate, Sci & Technol Branch, Toronto, ON, Canada. [Manney, G. L.] NorthWest Res Associates, Socorro, NM USA. [Manney, G. L.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. [Pavlovic, B.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Wiacek, A.] St Marys Univ, Halifax, NS B3H 3C3, Canada. RP Whaley, C (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada. EM cwhaley@atmosp.physics.utoronto.ca RI Strong, Kimberly/D-2563-2012; OI Whaley, Cynthia/0000-0002-0028-1514 FU Natural Sciences and Engineering Research Council of Canada; Canadian Space Agency (CSA); Environment Canada; Canadian Foundation for Climate and Atmospheric Sciences; ABB Bomem; Canada Foundation for Innovation; Ontario Research and Development Challenge Fund; Premier's Research Excellence Award; University of Toronto FX Funding for this work was provided by the Natural Sciences and Engineering Research Council of Canada, the Canadian Space Agency (CSA), and Environment Canada. The TAO measurements have been supported in the past by the Canadian Foundation for Climate and Atmospheric Sciences, ABB Bomem, the Canada Foundation for Innovation, the Ontario Research and Development Challenge Fund, the Premier's Research Excellence Award, and the University of Toronto. We also wish to thank the many students, postdocs, and interns who have contributed to TAO data acquisition since 2001. NR 74 TC 1 Z9 1 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 27 PY 2013 VL 118 IS 22 BP 12766 EP 12783 DI 10.1002/2013JD020577 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297OY UT WOS:000330266000010 ER PT J AU Huang, M Bowman, KW Carmichael, GR Pierce, RB Worden, HM Luo, M Cooper, OR Pollack, IB Ryerson, TB Brown, SS AF Huang, Min Bowman, Kevin W. Carmichael, Gregory R. Pierce, R. Bradley Worden, Helen M. Luo, Ming Cooper, Owen R. Pollack, Ilana B. Ryerson, Thomas B. Brown, Steven S. TI Impact of Southern California anthropogenic emissions on ozone pollution in the mountain states: Model analysis and observational evidence from space SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE SoCal pollution export; mountain states ozone; concurrent transport ID TRANSPORTED BACKGROUND OZONE; ADJOINT SENSITIVITY-ANALYSIS; CONTINENTAL UNITED-STATES; AIR-QUALITY MODELS; LOS-ANGELES BASIN; SURFACE OZONE; FREE TROPOSPHERE; NORTH-AMERICA; GLOBAL-MODEL; WEST-COAST AB The impact of Southern California (SoCal) anthropogenic emissions on ozone (O-3) in the mountain states in May 2010 is studied using the Sulfur Transport and Deposition Model. We identified two to six major transport events from SoCal to different subregions in the mountain states, with transport times of 0-2days indicated by trajectories, time-lag correlations, and forward/adjoint sensitivities. Based on forward sensitivity analysis, the contributions from SoCal anthropogenic emissions to the monthly mean daily maximum 8 h average (MDA8) surface O-3 in the mountain states decrease with distance from SoCal, and they range from <1 ppbv (in Wyoming) to 15 ppbv (in western Arizona). These contributions show medium (>0.6) to strong (>0.8) positive correlations with the modeled total surface MDA8 O-3. For the most strongly affected states of Arizona and New Mexico, these contributions have median values of similar to 3, similar to 2, similar to 5, and similar to 15 ppbv when the total surface MDA8 O-3 exceeded thresholds of 60, 65, 70, and 75 ppbv, respectively. Surface MDA8 O-3 values in SoCal show strong nonlinear responses to varied magnitudes of perturbation (e.g., 50% and 100%) in SoCal anthropogenic emissions and weak nonlinear responses in the mountain states. Case studies show that different scales of transport (e.g., trans-Pacific, stratospheric intrusions, and interstate) can be dynamically and chemically coupled and simultaneously affect O-3 in the mountain states when the meteorological conditions are favorable. During some of these strong transport periods, the contributions of SoCal anthropogenic emissions to hourly O-3 in the mountain states can exceed 20 ppbv, close to the magnitude during a summer event reported by Langford et al. (2010). Satellite observations from the Tropospheric Emission Spectrometer and the Measurements of Pollution in the Troposphere multispectral retrievals qualitatively demonstrate large and interstate scales of transport, respectively. Suggestions are made for future satellite missions to measure O-3 with improved spatial coverage, temporal frequency, and near-surface sensitivity to provide better observational constraints on interstate pollution transport studies. C1 [Huang, Min; Bowman, Kevin W.; Luo, Ming] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Huang, Min; Carmichael, Gregory R.] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA USA. [Pierce, R. Bradley] NOAA, Natl Environm Satellite Data & Informat Serv, Madison, WI USA. [Worden, Helen M.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Cooper, Owen R.; Pollack, Ilana B.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Cooper, Owen R.; Pollack, Ilana B.; Ryerson, Thomas B.; Brown, Steven S.] NOAA, Earth Syst Res Lab, Boulder, CO USA. RP Huang, M (reprint author), CALTECH, Jet Prop Lab, MS 233-200,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM min.huang@jpl.nasa.gov RI Pierce, Robert Bradley/F-5609-2010; Cooper, Owen/H-4875-2013; Pollack, Ilana/F-9875-2012; Ryerson, Tom/C-9611-2009; Brown, Steven/I-1762-2013; Manager, CSD Publications/B-2789-2015 OI Pierce, Robert Bradley/0000-0002-2767-1643; FU NASA [NNX11AI52G] FX This work was initiated at the University of Iowa and supported by a NASA award NNX11AI52G. It was then continued at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA, and was supported by the NASA Aura project. The authors would like to thank the editors and three anonymous reviewers for their efforts on earlier drafts of the paper. We thank the CalNex science team (especially Carsten Warneke for HCHO aircraft measurements and Jochen Stutz, Barry Lefer, Rebecca Washenfelder, and Bernhard Rappenglueck for their measurements at CalTech supersite) and the people who made the AQS, CASTNET, MOPITT and TES measurements. We thank C. Wiedinmyer and T. Duhl (NCAR) for helping with the MEGAN model and FINN data. We also thank computational resources at the University of Iowa and at NASA Ames. The views, opinions, and findings contained in this paper are those of the authors and should not be construed as an official NOAA or U.S. Government position, policy, or decision. NR 78 TC 13 Z9 13 U1 3 U2 32 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 27 PY 2013 VL 118 IS 22 BP 12784 EP 12803 DI 10.1002/2013JD020205 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 297OY UT WOS:000330266000027 ER PT J AU Polzin, KA Sankaran, K Ritchie, AG Reneau, JP AF Polzin, K. A. Sankaran, K. Ritchie, A. G. Reneau, J. P. TI Inductive pulsed plasma thruster model with time-evolution of energy and state properties SO JOURNAL OF PHYSICS D-APPLIED PHYSICS LA English DT Article ID ACCELERATION AB A model for pulsed inductive plasma acceleration is presented that consists of a set of circuit equations coupled to both a one-dimensional (1D) equation of motion and an equation governing the partitioning of energy. The latter two equations are obtained for the plasma current sheet by treating it as a single element of finite volume and integrating the governing equations over that volume. The integrated terms are replaced where necessary by physically equivalent approximations that are calculated through the solution of other parts of the governing equation set. The model improves upon previous 1D performance models by permitting the time-evolution of the temperature consistent with the time-varying energy flux into the plasma. The plasma state properties are also more realistically modelled and evolved in time, allowing for the tailoring of the model to different gases that may be chosen as propellants. Computational results for argon propellant are presented to demonstrate the efficacy of the model. The model produces a result where efficiency is maximized at a given value of the electrodynamic scaling term known as the dynamic impedance parameter. The scaling of different energy sinks as a function of the dynamic impedance parameter provides insight into the global energy partitioning in these types of accelerators. Results from the present model deviate from the previous version where temperature is selected as an input without regard for the energy that would be deposited to heat the gas to that temperature. Qualitatively and quantitatively, the model predicts specific impulse values that compare favourably with those measured for two separate inductive pulsed plasma thrusters. Efficiency is underpredicted in the regime where data are available, but the trends in the data and simulations follow similar trajectories that appear to be converging towards a predicted peak efficiency as the dynamic impedance parameter is increased. C1 [Polzin, K. A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Sankaran, K.; Ritchie, A. G.] Whitworth Univ, Dept Phys, Spokane, WA 99251 USA. [Reneau, J. P.] Mississippi State Univ, Dept Aerosp Engn, Starkville, MS 39759 USA. RP Polzin, KA (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM kurt.a.polzin@nasa.gov FU Washington NASA Space Grant Consortium FX The authors would like to thank Dr Michael LaPointe for providing several helpful comments during the preparation of this manuscript. The MSFC coauthors appreciate the continued NASA-MSFC management support of Mr Jim Martin and Mr J Boise Pearson. The Whitworth University coauthors acknowledge the support of the Washington NASA Space Grant Consortium. NR 16 TC 3 Z9 3 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0022-3727 EI 1361-6463 J9 J PHYS D APPL PHYS JI J. Phys. D-Appl. Phys. PD NOV 27 PY 2013 VL 46 IS 47 AR 475201 DI 10.1088/0022-3727/46/47/475201 PG 14 WC Physics, Applied SC Physics GA 252DK UT WOS:000326984800013 ER PT J AU Hastings, JL Kowal, J Daniels, J Shibata, S Platts, SH Hamilton, DR Page, RL Ng, J Goldberger, JJ Bungo, MW Levine, BD AF Hastings, Jeffrey L. Kowal, Jaime Daniels, James Shibata, Shigeki Platts, Steven H. Hamilton, Doug R. Page, Richard L. Ng, Jason Goldberger, Jeffrey J. Bungo, Michael W. Levine, Benjamin D. TI Cardiac Arrhythmias During Long Duration Spaceflight SO CIRCULATION LA English DT Meeting Abstract CT Scientific Sessions and Resuscitation Science Symposium of the American-Heart-Association CY NOV 16-17, 2013 CL Dallas, TX SP Amer Heart Assoc DE Electrophysiology; Atrial arrhythmias; Ventricular arrhythmia; Signal averaging C1 [Hastings, Jeffrey L.] UT Southwestern Med Cntr VA North Texas, Dallas, TX USA. [Kowal, Jaime; Shibata, Shigeki] Inst Exercise & Environm Med, Dallas, TX USA. [Daniels, James] UT Southwestern Med Cntr, Dallas, TX USA. [Platts, Steven H.] NASA, Johnson Space Cntr, Houston, TX USA. [Hamilton, Doug R.] NASA, Wyle Labs, Houston, TX USA. [Page, Richard L.] Univ Wisconsin, Madison, WI USA. [Ng, Jason; Goldberger, Jeffrey J.] Northwestern Univ, Feinberg Sch Med, Chicago, IL 60611 USA. [Bungo, Michael W.] Univ Texas Med Sch Houston, Houston, TX USA. [Levine, Benjamin D.] UT Southwestern Med Cntr, Inst Exercise & Environm Med, Dallas, TX USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0009-7322 EI 1524-4539 J9 CIRCULATION JI Circulation PD NOV 26 PY 2013 VL 128 IS 22 SU S MA 18904 PG 2 WC Cardiac & Cardiovascular Systems; Peripheral Vascular Disease SC Cardiovascular System & Cardiology GA AC0CR UT WOS:000332162908035 ER PT J AU Shibata, S Hastings, JL Abdullah, SM Bungo, MW Platts, S Hamilton, DR Levine, BD AF Shibata, Shigeki Hastings, Jeffrey L. Abdullah, Shuaib M. Bungo, Michael W. Platts, Steven Hamilton, Douglas R. Levine, Benjamin D. TI Determinants of Cardiac Loading During Long Duration Spaceflight SO CIRCULATION LA English DT Meeting Abstract CT Scientific Sessions and Resuscitation Science Symposium of the American-Heart-Association CY NOV 16-17, 2013 CL Dallas, TX SP Amer Heart Assoc DE Cardiac volume; Physical activity C1 [Shibata, Shigeki; Hastings, Jeffrey L.; Levine, Benjamin D.] Inst Exercise & Environm Med, Dallas, TX USA. [Abdullah, Shuaib M.] UT Southwestern Med Cntr, Dallas, TX USA. [Bungo, Michael W.] Univ Texas Med Sch Houston, Div Cardiovasc Med, Houston, TX USA. [Platts, Steven] NASA, Johnson Space Cntr, Cardiovasc Lab, Houston, TX USA. [Hamilton, Douglas R.] Univ Calgary, Calgary, AB, Canada. NR 0 TC 0 Z9 0 U1 0 U2 1 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0009-7322 EI 1524-4539 J9 CIRCULATION JI Circulation PD NOV 26 PY 2013 VL 128 IS 22 SU S MA 18500 PG 1 WC Cardiac & Cardiovascular Systems; Peripheral Vascular Disease SC Cardiovascular System & Cardiology GA AC0CR UT WOS:000332162907403 ER PT J AU Hoglund, L Ting, DZ Khoshakhlagh, A Soibel, A Hill, CJ Fisher, A Keo, S Gunapala, SD AF Hoeglund, L. Ting, D. Z. Khoshakhlagh, A. Soibel, A. Hill, C. J. Fisher, A. Keo, S. Gunapala, S. D. TI Influence of radiative and non-radiative recombination on the minority carrier lifetime in midwave infrared InAs/InAsSb superlattices SO APPLIED PHYSICS LETTERS LA English DT Article ID HGCDTE; GAAS AB Optical modulation response is used to study the influence of radiative, Shockley-Read-Hall, and Auger recombination processes on the minority carrier lifetime in a mid-wave infrared InAs/InAsSb superlattice. A comparison of calculated and measured temperature dependencies shows that the lifetime is influenced mainly by radiative recombination at low temperatures, resulting in an increase of the minority carrier lifetime from 1.8 mu s at 77K to 2.8 mu s at 200 K. At temperatures above 200 K, Auger recombination increases rapidly and limits the lifetime. Shockley-Read-Hall limited lifetimes on the order of 10 mu s are predicted for superlattices with lower background doping concentration. (C) 2013 AIP Publishing LLC. C1 [Hoeglund, L.; Ting, D. Z.; Khoshakhlagh, A.; Soibel, A.; Hill, C. J.; Fisher, A.; Keo, S.; Gunapala, S. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hoglund, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Soibel, Alexander/A-1313-2007 NR 18 TC 27 Z9 27 U1 3 U2 43 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD NOV 25 PY 2013 VL 103 IS 22 AR 221908 DI 10.1063/1.4835055 PG 5 WC Physics, Applied SC Physics GA 261WW UT WOS:000327696300029 ER PT J AU Strekalov, DV Erkmen, BI Yu, N AF Strekalov, Dmitry V. Erkmen, Baris I. Yu, Nan TI Intensity interferometry for observation of dark objects SO PHYSICAL REVIEW A LA English DT Article ID PHASE RETRIEVAL AB We analyze an intensity interferometry measurement carried out with two pointlike detectors facing a distant source (e,g., a star) that may be partially occluded by an absorptive object (e,g., a planet). Such a measurement, based on the perturbation of the observed covariance function due to the object's presence, can provide information of the object complementary to a direct optical intensity measurement. In particular, one can infer the orientation of the object's transient trajectory. We identify the key parameters that impact this perturbation and show that its magnitude is equal to the magnitude of the intensity variation caused by the same object. In astronomy applications, this value may be very small, so a differential measurement may be necessary. Finally, we discuss the signal-to-noise ratio that may be expected in this type of measurement. C1 [Strekalov, Dmitry V.; Erkmen, Baris I.; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Strekalov, DV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration FX This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. D. V. S. thanks Dr. Igor Kulikov for fruitful discussions. NR 22 TC 8 Z9 13 U1 2 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD NOV 25 PY 2013 VL 88 IS 5 AR 053837 DI 10.1103/PhysRevA.88.053837 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 256MH UT WOS:000327314400018 ER PT J AU Acar, E Karaca, HE Tobe, H Noebe, RD Chumlyakov, YI AF Acar, E. Karaca, H. E. Tobe, H. Noebe, R. D. Chumlyakov, Y. I. TI Characterization of the shape memory properties of a Ni45.3Ti39.7Hf10Pd5 alloy SO JOURNAL OF ALLOYS AND COMPOUNDS LA English DT Article DE NiTiHfPd alloys; Microstructure; TWSME; High work output; High strength SMAs; Shape memory alloys ID NITIHFPD SINGLE-CRYSTALS; INDUCED MARTENSITIC-TRANSFORMATION; COMPRESSIVE RESPONSE; ELECTRON-MICROSCOPY; BEHAVIOR; STRENGTH; SUBSTRUCTURE AB The load-biased shape memory and superelastic responses of a Ni45.3Ti39.7Hf10Pd5 polycrystalline alloy were investigated in compression. Transformation strain of up to 4.6% and work output of up to 29 J cm(-3) were determined from load-biased thermal cycling experiments. The alloy showed good superelastic behavior at 90 degrees C with recoverable strain of over 4%. It was also determined that the Ni45.3Ti39.7Hf10Pd5 alloy could develop two-way shape memory strain of 1.6% without an intense training process. Transmission electron microscopy (TEM) revealed that the internal twins formed in the martensite variants were < 0 1 1 > type II twins. (c) 2013 Elsevier B.V. All rights reserved. C1 [Acar, E.; Karaca, H. E.; Tobe, H.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA. [Noebe, R. D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. [Chumlyakov, Y. I.] Tomsk State Univ, Siberian Phys Tech Inst, Tomsk 634050, Russia. [Acar, E.] Erciyes Univ, TR-38039 Kayseri, Turkey. RP Karaca, HE (reprint author), Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA. EM karaca@engr.uky.edu RI Chumlyakov, Yuriy/R-6496-2016 FU NASA [NNX11AQ31A, 3049024332]; RFBR [10-03-0154-a] FX This work was supported by the NASA Fundamental Aeronautics Program, Aeronautical Sciences Project and the NASA EPSCOR program under Grant No.: NNX11AQ31A, KY EPSCoR RID program under Grant No.: 3049024332 and RFBR project with Grant No.: 10-03-0154-a. NR 33 TC 10 Z9 10 U1 2 U2 30 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-8388 EI 1873-4669 J9 J ALLOY COMPD JI J. Alloy. Compd. PD NOV 25 PY 2013 VL 578 BP 297 EP 302 DI 10.1016/j.jallcom.2013.06.030 PG 6 WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering GA 216WI UT WOS:000324316400049 ER PT J AU Rury, AS AF Rury, Aaron S. TI Coherent control of plasmonic spectra using the orbital angular momentum of light SO PHYSICAL REVIEW B LA English DT Article ID METAMATERIALS; TRANSMISSION; MODULATION; SHIFTS AB This study proposes a method to control the frequency-dependent scattering spectra from plasmonic spheres via the conservation of incident orbital angular momentum (OAM) in classical light scattering. By providing controllable distributions of OAM content, fractional vortex beams allow selective tailoring of Fano features present in coherent scattering processes. The applicability of this control methodology is briefly discussed in the context of plasmonic crystals that recent studies have shown possess modes described by a well-defined OAM content. C1 [Rury, Aaron S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rury, Aaron S.] Univ Michigan, Appl Phys Program, Ann Arbor, MI 48109 USA. RP Rury, AS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM arury@caltech.edu OI Rury, Aaron/0000-0002-1836-1424 FU Defense Threat Reduction Agency-Joint Science and Technology Office for Chemical and Biological Defense [HDTRA1-09-1-0005] FX This work was supported by the Defense Threat Reduction Agency-Joint Science and Technology Office for Chemical and Biological Defense (Grant HDTRA1-09-1-0005). NR 24 TC 4 Z9 4 U1 1 U2 25 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 EI 1550-235X J9 PHYS REV B JI Phys. Rev. B PD NOV 22 PY 2013 VL 88 IS 20 AR 205132 DI 10.1103/PhysRevB.88.205132 PG 5 WC Physics, Condensed Matter SC Physics GA 255LD UT WOS:000327239600003 ER PT J AU Bagheri, M Frez, C Kelly, B Gupta, JA Forouhar, S AF Bagheri, M. Frez, C. Kelly, B. Gupta, J. A. Forouhar, S. TI High output power, fibre-coupled distributed feedback lasers operating near 2.05 mu m wavelength range SO ELECTRONICS LETTERS LA English DT Article DE distributed feedback lasers; electronics packaging; extinction coefficients; laser modes; laser tuning; optical fibre couplers; optical fibre polarisation; semiconductor lasers; high output power fibre-coupled distributed feedback lasers; single-mode operation; fibre-pigtailed distributed feedback semiconductor lasers; packaging; standard butterfly modules; polarisation maintaining optical fibre; side mode suppression ratios; mode-hop free tunability; linear polarisation; extinction ratio; operating current; operating temperatures; wavelength 2; 05 mum; power 10 mW ID DIODE-LASERS AB Single-mode operation of fibre-pigtailed distributed feedback semiconductor lasers in the 2.05 m range has been demonstrated. The lasers are packaged inside standard butterfly modules with output powers in excess of 10 mW at the end of polarisation maintaining optical fibre. The fibre-pigtailed lasers show excellent sidemode suppression ratios ( > 50 dB) and have a mode-hop free tunability larger than 1 nm. The output of the optical fibre has linear polarisation with better than 20 dB extinction over the operating current and temperatures. C1 [Bagheri, M.; Frez, C.; Forouhar, S.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Kelly, B.] Eblana Photon, Dublin, Ireland. [Gupta, J. A.] Natl Res Council Canada, Inst Microstruct Sci, Ottawa, ON, Canada. RP Bagheri, M (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA. EM mahmood.bagheri@jpl.nasa.gov FU National Aeronautics and Space Administration's (NASA) Earth and Science Technology Office (ESTO); NASA FX This work was supported under the Advanced Component Technology (ACT) program of the National Aeronautics and Space Administration's (NASA) Earth and Science Technology Office (ESTO) and performed at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the NASA. The authors thank G. Komar, J. Hyon and I. Eastwood for their support and encouragement. NR 10 TC 3 Z9 3 U1 1 U2 7 PU INST ENGINEERING TECHNOLOGY-IET PI HERTFORD PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND SN 0013-5194 EI 1350-911X J9 ELECTRON LETT JI Electron. Lett. PD NOV 21 PY 2013 VL 49 IS 24 BP 1552 EP + DI 10.1049/el.2013.2503 PG 2 WC Engineering, Electrical & Electronic SC Engineering GA 270QF UT WOS:000328332800035 ER PT J AU Burke-Spolaor, S AF Burke-Spolaor, Sarah TI Multi-messenger approaches to binary supermassive black holes in the 'continuous-wave' regime SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article ID ACTIVE GALACTIC NUCLEI; PULSAR TIMING ARRAYS; DIGITAL SKY SURVEY; GALAXY 3C 66B; GRAVITATIONAL-WAVES; TIDAL DISRUPTION; X-RAY; SYSTEMATIC SEARCH; LINE DIAGNOSIS; MERGERS AB Pulsar timing arrays are sensitive to gravitational waves from supermassive black hole (SMBH) binaries at orbital separations of << 1 pc. There is currently an observational paucity of such systems, although they are central figures in studies of galaxy evolution, merger dynamics, and active nucleus formation. We review the prospects of detecting SMBH binaries through electromagnetic radiative processes thought to be associated with galaxy mergers and late-stage binary evolution. We then discuss the scientific goals of joint pulsar timing and electromagnetic studies of these systems, including the facilitation of binary parameter estimation, identifying galactic hosts of gravitational wave emitters, and relevant studies of merger dynamics and cosmology. The use of upcoming high-precision timing arrays with the International pulsar timing array and the square kilometre array, combined with ongoing electromagnetic observing campaigns to identify active SMBH binaries, provide generous possibilities for multi-messenger astrophysics in the near future. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Burke-Spolaor, S (reprint author), CALTECH, Jet Prop Lab, M-S 138-310,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM sarah.burke-spolaor@jpl.nasa.gov NR 94 TC 11 Z9 11 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD NOV 21 PY 2013 VL 30 IS 22 AR 224013 DI 10.1088/0264-9381/30/22/224013 PG 14 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 248GL UT WOS:000326684900014 ER PT J AU Lazio, TJ AF Lazio, T. J. W. TI The Square Kilometre Array pulsar timing array SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article ID BLACK-HOLE BINARIES; EQUATION-OF-STATE; SCINTILLATION-INDUCED VARIABILITY; GRAVITATIONAL-WAVE MEMORY; MILLISECOND PULSAR; GENERAL-RELATIVITY; FAST TRANSIENTS; NEUTRON-STARS; LIMITS; CONSTRAINTS AB The Square Kilometre Array (SKA) is envisioned as the meter-and centimeter-wavelength telescope of the 21st century, and gravitational wave studies via a pulsar timing array (PTA) form a key aspect of its science program. In its ultimate implementation, the SKA (phase 2) should enable the construction of a PTA consisting of as many as 100 spin-stable millisecond pulsars. The sensitivity of the SKA-PTA could approach gravitational wave strain amplitudes of 6 x 10(-16) or better at fiducial gravitational wave frequencies of order 1 yr(-1), at least an order of magnitude improvement in the gravitational wave strain amplitude that can be measured. Any nearby individual supermassive black hole binaries could be detected, and the existence of non-tensor modes can be tested. Beyond its PTA capabilities, the SKA will also enable a range of other tests of fundamental physics, such as tests of gravity in ultra-relativistic binaries and constraints on the nuclear equation of state. C1 [Lazio, T. J. W.] Jodrell Bank Observ, Off SKA Org, Macclesfield SK11 9DL, Cheshire, England. [Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lazio, TJ (reprint author), Jodrell Bank Observ, Off SKA Org, Macclesfield SK11 9DL, Cheshire, England. EM Joseph.Lazio@jpl.nasa.gov NR 95 TC 12 Z9 12 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD NOV 21 PY 2013 VL 30 IS 22 AR 224011 DI 10.1088/0264-9381/30/22/224011 PG 14 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 248GL UT WOS:000326684900012 ER PT J AU Johnson, BC Litorja, M Fowler, JB Shirley, EL Barnes, RA Butler, JJ AF Johnson, B. Carol Litorja, Maritoni Fowler, Joel B. Shirley, Eric L. Barnes, Robert A. Butler, James J. TI Results of aperture area comparisons for exo-atmospheric total solar irradiance measurements SO APPLIED OPTICS LA English DT Article ID RADIATION BUDGET EXPERIMENT; ACTIVE CAVITY RADIOMETER; INTERNATIONAL-SPACE-STATION; EARTH OBSERVING SYSTEM; CONSTANT OBSERVATIONS; CRYOGENIC RADIOMETER; BOARD EURECA; VARIABILITY; ACCURACY; SCALE AB Exo-atmospheric solar irradiance measurements made by the solar irradiance community since 1978 have incorporated limiting apertures with diameters measured by a number of metrology laboratories using a variety of techniques. Knowledge of the aperture area is a critical component in the conversion of radiant flux measurements to solar irradiance. A National Aeronautics and Space Administration (NASA) Earth Observing System (EOS) sponsored international comparison of aperture area measurements of limiting apertures provided by solar irradiance researchers was performed, the effort being executed by the National Institute of Standards and Technology (NIST) in coordination with the EOS Project Science Office. Apertures that had institutional heritage with historical solar irradiance measurements were measured using the absolute aperture measurement facility at NIST. The measurement technique employed noncontact video microscopy using high-accuracy translation stages. We have quantified the differences between the participating institutions' aperture area measurements and find no evidence to support the hypothesis that preflight aperture area measurements were the root cause of discrepancies in long-term total solar irradiance satellite measurements. Another result is the assessment of uncertainties assigned to methods used by participants. We find that uncertainties assigned to a participant's values may be underestimated. C1 [Johnson, B. Carol; Litorja, Maritoni; Fowler, Joel B.; Shirley, Eric L.] NIST, Gaithersburg, MD 20899 USA. [Barnes, Robert A.] Sci Applicat Int Corp, Beltsville, MD 20705 USA. [Butler, James J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Johnson, BC (reprint author), NIST, Gaithersburg, MD 20899 USA. EM cjohnson@nist.gov RI Butler, James/D-4188-2013 FU The NASA EOS Project Science Office [S 41365 F] FX The authors are grateful to Dominique A. Crommelynck and Steven Dewitte of the Institut Royal Meteorologique de Belgique, Brussels, Belgium; Claus Frohlich and Wolfgang Finsterle of the Physikalisch-Meteorologisches Observatorium Davos/World Radiation Centre, Davos, Switzerland; Robert B. Lee III of the National Aeronautics and Space Administration, Langley Research Center, Hampton, Virginia, USA; Richard C. Willson of Columbia University, Coronado, California, USA; and Roger S. Helizon of the National Aeronautics and Space Administration, Jet Propulsion Laboratory, Pasadena, California, USA for submission of the comparison apertures, associated documentation, and useful discussions. Greg Kopp of the University of Colorado's LASP facility provided useful discussions. The comments and suggestions of the anonymous reviewers were helpful in finalizing the text. Vladimir Khromchenko and Curtis Suplee of NIST provided technical assistance. The NASA EOS Project Science Office provided support (S 41365 F). NR 95 TC 1 Z9 1 U1 0 U2 6 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD NOV 20 PY 2013 VL 52 IS 33 BP 7963 EP 7980 DI 10.1364/AO.52.007963 PG 18 WC Optics SC Optics GA 258NY UT WOS:000327467200015 PM 24513747 ER PT J AU Ackermann, M Ajello, M Allafort, A Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bloom, ED Bonamente, E Borgland, AW Bottacini, E Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Busetto, G Buson, S Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cecchi, C Charles, E Chekhtman, A Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J D'Ammando, F de Angelis, A de Palma, F Dermer, CD Digel, SW Silva, EDE Drell, PS Drlica-Wagner, A Falletti, L Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Fukazawa, Y Fukui, Y Funk, S Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grondin, MH Grove, JE Guiriec, S Hadasch, D Hanabata, Y Harding, AK Hayashi, K Horan, D Hou, X Hughes, RE Itoh, R Jackson, MS Johannesson, G Johnson, AS Kamae, T Katagiri, H Kataoka, J Knodlseder, J Kuss, M Lande, J Larsson, S Lee, SH Lemoine-Goumard, M Longo, F Loparco, F Lovellette, MN Lubrano, P Martin, P Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Naumann-Godo, M Nemmen, R Nishino, S Norris, JP Nuss, E Ohno, M Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Ozaki, M Paneque, D Panetta, JH Parent, D Pesce-Rollins, M Pierbattista, M Piron, F Pivato, G Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Romoli, C Roth, M Sada, T Sadrozinski, HFW Sanchez, DA Sbarra, C Sgro, C Siskind, EJ Spandre, G Spinelli, P Strong, AW Suson, DJ Takahashi, H Takahashi, T Tanaka, T Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tibolla, O Tinivella, M Torres, DF Tosti, G Tramacere, A Troja, E Uchiyama, Y Uehara, T Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Yamamoto, H Yang, Z Zimmer, S AF Ackermann, M. Ajello, M. Allafort, A. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Bottacini, E. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Busetto, G. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cecchi, C. Charles, E. Chekhtman, A. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. D'Ammando, F. de Angelis, A. de Palma, F. Dermer, C. D. Digel, S. W. do Couto E Silva, E. Drell, P. S. Drlica-Wagner, A. Falletti, L. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Fukazawa, Y. Fukui, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grondin, M-H. Grove, J. E. Guiriec, S. Hadasch, D. Hanabata, Y. Harding, A. K. Hayashi, K. Horan, D. Hou, X. Hughes, R. E. Itoh, R. Jackson, M. S. Johannesson, G. Johnson, A. S. Kamae, T. Katagiri, H. Kataoka, J. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Lee, S-H. Lemoine-Goumard, M. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Martin, P. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Naumann-Godo, M. Nemmen, R. Nishino, S. Norris, J. P. Nuss, E. Ohno, M. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Panetta, J. H. Parent, D. Pesce-Rollins, M. Pierbattista, M. Piron, F. Pivato, G. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Romoli, C. Roth, M. Sada, T. Sadrozinski, H. F-W. Sanchez, D. A. Sbarra, C. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Strong, A. W. Suson, D. J. Takahashi, H. Takahashi, T. Tanaka, T. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tibolla, O. Tinivella, M. Torres, D. F. Tosti, G. Tramacere, A. Troja, E. Uchiyama, Y. Uehara, T. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Yamamoto, H. Yang, Z. Zimmer, S. TI FERMI LARGE AREA TELESCOPE STUDY OF COSMIC-RAYS AND THE INTERSTELLAR MEDIUM IN NEARBY MOLECULAR CLOUDS (vol 755, 22, 2012) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto E Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto E Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Moiseev, A. A.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. 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[Hayashi, K.; Ohno, M.; Okumura, A.; Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Hou, X.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, IN2P3, CNRS, F-33175 Gradignan, France. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Jackson, M. S.] Royal Inst Technol KTH, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Katagiri, H.] Ibaraki Univ, Coll Sci, Bunkyo Ku, Mito, Ibaraki 3108512, Japan. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Lee, S-H.] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan. [Lemoine-Goumard, M.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Martin, P.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA. [Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 4398526, Japan. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Razzano, M.; Sadrozinski, H. F-W.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Razzano, M.; Sadrozinski, H. F-W.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Torres, D. F.] ICREA, Barcelona, Spain. [Tramacere, A.; Vianello, G.] CIFS, I-10133 Turin, Italy. [Tramacere, A.] INTEGRAL, Sci Data Ctr, CH-1290 Versoix, Switzerland. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM khayashi@astro.isas.jaxa.jp; mizuno@hirax6.hepl.hiroshima-u.ac.jp RI Orlando, E/R-5594-2016; Ozaki, Masanobu/K-1165-2013; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016 OI Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Torres, Diego/0000-0002-1522-9065 NR 1 TC 3 Z9 3 U1 0 U2 15 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR UNSP 82 DI 10.1088/0004-637X/778/1/82 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700082 ER PT J AU Corbet, RHD Krimm, HA AF Corbet, Robin H. D. Krimm, Hans A. TI SUPERORBITAL PERIODIC MODULATION IN WIND-ACCRETION HIGH-MASS X-RAY BINARIES FROM SWIFT BURST ALERT TELESCOPE OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: individual (2S 0114+650, 1E 1145.1-6141, IGR J16393-4643, IGR J16418-4532, IGR J16479-4514); stars: neutron; X-rays: stars ID PULSAR 1E 1145.1-6141; UNEVENLY SPACED DATA; TIME-SERIES ANALYSIS; ALL-SKY MONITOR; IGR J16418-4532; TIMING-EXPLORER; ORBITAL PERIOD; 2S 0114+650; XMM-NEWTON; MULTIWAVELENGTH OBSERVATIONS AB We report the discovery using data from the Swift-Burst Alert Telescope ( BAT) of superorbital modulation in the wind-accretion supergiant high-mass X-ray binaries 4U 1909+07 (= X 1908+075), IGR J16418-4532, and IGR J16479-4514. Together with already known superorbital periodicities in 2S 0114+650 and IGR J16493-4348, the systems exhibit a monotonic relationship between superorbital and orbital periods. These systems include both supergiant fast X-ray transients and classical supergiant systems, and have a range of inclination angles. This suggests an underlying physical mechanism which is connected to the orbital period. In addition to these sources with clear detections of superorbital periods, IGR J16393-4643 (= AX J16390.4-4642) is identified as a system that may have superorbital modulation due to the coincidence of low-amplitude peaks in power spectra derived from BAT, Rossi X-Ray Timing Explorer Proportional Counter Array, and International Gamma-Ray Astrophysics Laboratory light curves. 1E 1145.1-6141 may also be worthy of further attention due to the amount of low-frequency modulation of its light curve. However, we find that the presence of superorbital modulation is not a universal feature of wind-accretion supergiant X-ray binaries. C1 [Corbet, Robin H. D.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Corbet, Robin H. D.] NASA, Goddard Space Flight Ctr, CRESST Mail Code 662, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Krimm, Hans A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Krimm, Hans A.] NASA, Goddard Space Flight Ctr, CRESST Mail Code 661, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. RP Corbet, RHD (reprint author), Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. EM corbet@umbc.edu FU NASA under Swift Guest Observer [NNX09AU85G, NNX12AD32G, NNX12AE57G, NNX13AC75G] FX We thank an anonymous referee for useful comments. This paper used Swift-BAT transient monitor results provided by the Swift-BAT team. The Swift-BAT transient monitor and H.A.K. are supported by NASA under Swift Guest Observer grants NNX09AU85G, NNX12AD32G, NNX12AE57G, and NNX13AC75G. NR 83 TC 9 Z9 10 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 45 DI 10.1088/0004-637X/778/1/45 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700045 ER PT J AU D'Angelo, G Bodenheimer, P AF D'Angelo, Gennaro Bodenheimer, Peter TI THREE-DIMENSIONAL RADIATION-HYDRODYNAMICS CALCULATIONS OF THE ENVELOPES OF YOUNG PLANETS EMBEDDED IN PROTOPLANETARY DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; hydrodynamics; methods: numerical; planet-disk interactions; planets and satellites: formation; protoplanetary disks ID FLUX-LIMITED DIFFUSION; ACCRETION DISKS; GIANT PLANETS; CIRCUMSTELLAR DISKS; BINARY-SYSTEMS; GAS ACCRETION; NESTED GRIDS; MASS PLANETS; SOLID CORES; MIGRATION AB We perform global three-dimensional (3D) radiation-hydrodynamics calculations of the envelopes surrounding young planetary cores of 5, 10, and 15 Earth masses, located in a protoplanetary disk at 5 and 10AU from a solar-mass star. We apply a nested-grid technique to resolve the thermodynamics of the disk at the orbital-radius length scale and that of the envelope at the core-radius length scale. The gas is modeled as a solar mixture of molecular and atomic hydrogen, helium, and their ions. The equation of state accounts for both gas and radiation, and gas energy includes contributions from rotational and vibrational states of molecular hydrogen and from ionization of atomic species. Dust opacities are computed from first principles, applying the full Mie theory. One-dimensional (1D) calculations of planet formation are used to supplement the 3D calculations by providing energy deposition rates in the envelope due to solids accretion. We compare 1D and 3D envelopes and find that masses and gas accretion rates agree within factors of 2, and so do envelope temperatures. The trajectories of passive tracers are used to define the size of 3D envelopes, resulting in radii much smaller than the Hill radius and smaller than the Bondi radius. The moments of inertia and angular momentum of the envelopes are determined and the rotation rates are derived from the rigid-body approximation, resulting in slow bulk rotation. We find that the polar flattening is less than or similar to 0.05. The dynamics of the accretion flow are examined by tracking the motion of tracers that move into the envelope. The anisotropy of this flow is characterized in terms of both its origin and impact site at the envelope surface. Gas merges with the envelope preferentially at mid- to high latitudes. C1 [D'Angelo, Gennaro] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [D'Angelo, Gennaro] SETI Inst, Mountain View, CA 94043 USA. [Bodenheimer, Peter] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. RP D'Angelo, G (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA. EM gennaro.dangelo@nasa.gov; peter@ucolick.org RI D'Angelo, Gennaro/L-7676-2014 OI D'Angelo, Gennaro/0000-0002-2064-0801 FU NASA Outer Planets Research Program [202844.02.02.01.75]; NASA Origins of Solar Systems [NNX11AK54G] FX We are grateful to Jack Lissauer, Morris Podolak, and Uma Gorti for useful feedback on this work. We thank the referee for constructive and helpful comments. Primary support for this project was provided by NASA Outer Planets Research Program grant 202844.02.02.01.75; additional support was provided by NASA Origins of Solar Systems grant NNX11AK54G. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. G. D. thanks Los Alamos National Laboratory for its hospitality. NR 78 TC 13 Z9 13 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 77 DI 10.1088/0004-637X/778/1/77 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700077 ER PT J AU Gatuzz, E Garcia, J Mendoza, C Kallman, TR Witthoeft, M Lohfink, A Bautista, MA Palmeri, P Quinet, P AF Gatuzz, E. Garcia, J. Mendoza, C. Kallman, T. R. Witthoeft, M. Lohfink, A. Bautista, M. A. Palmeri, P. Quinet, P. TI PHOTOIONIZATION MODELING OF OXYGEN K ABSORPTION IN THE INTERSTELLAR MEDIUM, THE CHANDRA GRATING SPECTRA OF XTE J1817-330 (vol 768, 60, 2013) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Gatuzz, E.; Mendoza, C.] IVIC, Ctr Fis, Caracas 1020A, Venezuela. [Garcia, J.; Lohfink, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Garcia, J.; Lohfink, A.] Univ Maryland, Maryland Astron Ctr Theory & Computat, College Pk, MD 20742 USA. [Garcia, J.; Kallman, T. R.; Witthoeft, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mendoza, C.] Univ Los Andes CeCalCULA, Ctr Nacl Calculo Cient, Corp Parque Tecnol Merida, Merida 5101, Venezuela. [Bautista, M. A.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Palmeri, P.; Quinet, P.] Univ Mons UMONS, B-7000 Mons, Belgium. [Quinet, P.] Univ Liege, IPNAS, B-4000 Liege, Belgium. RP Gatuzz, E (reprint author), IVIC, Ctr Fis, POB 20632, Caracas 1020A, Venezuela. EM egatuzz@ivic.gob.ve; javier@astro.umd.edu; claudio@ivic.gob.ve; timothy.r.kallman@nasa.gov; michael.c.witthoeft@nasa.gov; alohfink@astro.umd.edu; manuel.bautista@wmich.edu; palmeri@umons.ac.be; quinet@umons.ac.be NR 2 TC 7 Z9 7 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 83 DI 10.1088/0004-637X/778/1/83 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700083 ER PT J AU Kettula, K Finoguenov, A Massey, R Rhodes, J Hoekstra, H Taylor, JE Spinelli, PF Tanaka, M Ilbert, O Capak, P McCracken, HJ Koekemoer, A AF Kettula, K. Finoguenov, A. Massey, R. Rhodes, J. Hoekstra, H. Taylor, J. E. Spinelli, P. F. Tanaka, M. Ilbert, O. Capak, P. McCracken, H. J. Koekemoer, A. TI WEAK LENSING CALIBRATED M-T SCALING RELATION OF GALAXY GROUPS IN THE COSMOS FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: groups: general; gravitational lensing: weak ID HUBBLE-SPACE-TELESCOPE; EVOLUTION SURVEY COSMOS; DEGREE ROSAT SURVEY; X-RAY-PROPERTIES; XMM-NEWTON; CLUSTER COSMOLOGY; SOURCE CATALOG; RICH CLUSTERS; MASS; CHANDRA AB The scaling between X-ray observables and mass for galaxy clusters and groups is instrumental for cluster-based cosmology and an important probe for the thermodynamics of the intracluster gas. We calibrate a scaling relation between the weak lensing mass and X-ray spectroscopic temperature for 10 galaxy groups in the COSMOS field, combined with 55 higher-mass clusters from the literature. The COSMOS data includes Hubble Space Telescope imaging and redshift measurements of 46 source galaxies per arcminute(2), enabling us to perform unique weak lensing measurements of low-mass systems. Our sample extends the mass range of the lensing calibrated M-T relation an order of magnitude lower than any previous study, resulting in a power-law slope of 1.48(-0.09)(+0.13). The slope is consistent with the self-similar model, predictions from simulations, and observations of clusters. However, X-ray observations relying on mass measurements derived under the assumption of hydrostatic equilibrium have indicated that masses at group scales are lower than expected. Both simulations and observations suggest that hydrostatic mass measurements can be biased low. Our external weak lensing masses provide the first observational support for hydrostatic mass bias at group level, showing an increasing bias with decreasing temperature and reaching a level of 30%-50% at 1 keV. C1 [Kettula, K.; Finoguenov, A.] Univ Helsinki, Dept Phys, FI-00014 Helsinki, Finland. [Massey, R.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Massey, R.] CALTECH, Pasadena, CA 91125 USA. [Rhodes, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hoekstra, H.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [Taylor, J. E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Spinelli, P. F.] Inst Astron Geofis & Ciencias Atmosfer IAG, BR-05508090 Sao Paulo, Brazil. [Spinelli, P. F.] Museu Astron & Ciencias Afins MAST, BR-20921030 Rio De Janeiro, RJ, Brazil. [Tanaka, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Ilbert, O.] Univ Aix Marseille, CNRS, LAM, F-13013 Marseille, France. [Capak, P.] 314 6 Caltech, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [McCracken, H. J.] Inst Astrophys, UMR 7095, F-75014 Paris, France. [Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Kettula, K (reprint author), Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2A, FI-00014 Helsinki, Finland. EM kimmo.kettula@iki.fi OI SPINELLI, Paolo/0000-0001-6688-8864; Koekemoer, Anton/0000-0002-6610-2048 FU Magnus Ehrnrooth Foundation; Royal Society University Research Fellowship; ERC [MIRG-CT-208994]; JPL; NWO Vidi grant [639.042.814] FX The authors thank F. Miniati for useful discussion. K. K. acknowledges support from the Magnus Ehrnrooth Foundation. A. F. acknowledges the Academy of Finland (decision 266918). R. M. is supported by a Royal Society University Research Fellowship and ERC grant MIRG-CT-208994. J.R. was supported by JPL, which is run by Caltech under a contract for NASA. H. H. acknowledges NWO Vidi grant 639.042.814. This research has made use of NASA's Astrophysics Data System. NR 56 TC 14 Z9 14 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 74 DI 10.1088/0004-637X/778/1/74 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700074 ER PT J AU Kozarev, KA Evans, RM Schwadron, NA Dayeh, MA Opher, M Korreck, KE van der Holst, B AF Kozarev, Kamen A. Evans, Rebekah M. Schwadron, Nathan A. Dayeh, Maher A. Opher, Merav Korreck, Kelly E. van der Holst, Bart TI GLOBAL NUMERICAL MODELING OF ENERGETIC PROTON ACCELERATION IN A CORONAL MASS EJECTION TRAVELING THROUGH THE SOLAR CORONA SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; magnetohydrodynamics (MHD); shock waves; Sun: coronal mass ejections (CMEs); Sun: heliosphere; Sun: particle emission ID SELF-GENERATED TURBULENCE; GROUND-LEVEL EVENTS; PARTICLE-ACCELERATION; DRIVEN SHOCKS; COSMIC-RAYS; COLLISIONLESS SHOCKS; CHARGED-PARTICLES; SHEATH STRUCTURES; CYCLE VARIATIONS; MAGNETIC-FIELDS AB The acceleration of protons and electrons to high (sometimes GeV/nucleon) energies by solar phenomena is a key component of space weather. These solar energetic particle (SEP) events can damage spacecraft and communications, as well as present radiation hazards to humans. In-depth particle acceleration simulations have been performed for idealized magnetic fields for diffusive acceleration and particle propagation, and at the same time the quality of MHD simulations of coronal mass ejections (CMEs) has improved significantly. However, to date these two pieces of the same puzzle have remained largely decoupled. Such structures may contain not just a shock but also sizable sheath and pileup compression regions behind it, and may vary considerably with longitude and latitude based on the underlying coronal conditions. In this work, we have coupled results from a detailed global three-dimensional MHD time-dependent CME simulation to a global proton acceleration and transport model, in order to study time-dependent effects of SEP acceleration between 1.8 and 8 solar radii in the 2005 May 13 CME. We find that the source population is accelerated to at least 100 MeV, with distributions enhanced up to six orders of magnitude. Acceleration efficiency varies strongly along field lines probing different regions of the dynamically evolving CME, whose dynamics is influenced by the large-scale coronal magnetic field structure. We observe strong acceleration in sheath regions immediately behind the shock. C1 [Kozarev, Kamen A.; Opher, Merav] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Kozarev, Kamen A.; Korreck, Kelly E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Evans, Rebekah M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Schwadron, Nathan A.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Dayeh, Maher A.] Southwest Res Inst, Dept Space Sci, San Antonio, TX USA. [van der Holst, Bart] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. RP Kozarev, KA (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. RI van der Holst, Bart/A-3557-2013 FU NASA LWS EMMREM [NNX07AC14G]; NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program; NASA Postdoctoral Program at GSFC FX This work was supported under NASA LWS EMMREM project and grant no. NNX07AC14G. K.A.K. was partially supported under the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program, administered by the UCAR Visiting Scientist Programs. R.M.E. is supported through an appointment to the NASA Postdoctoral Program at GSFC, administered by Oak Ridge Associated Universities through a contract with NASA. NR 61 TC 11 Z9 11 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 43 DI 10.1088/0004-637X/778/1/43 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700043 ER PT J AU Ramesh, R Kishore, P Mulay, SM Barve, IV Kathiravan, C Wang, TJ AF Ramesh, R. Kishore, P. Mulay, Sargam M. Barve, Indrajit V. Kathiravan, C. Wang, T. J. TI LOW-FREQUENCY OBSERVATIONS OF DRIFTING, NON-THERMAL CONTINUUM RADIO EMISSION ASSOCIATED WITH THE SOLAR CORONAL MASS EJECTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: magnetic fields; Sun: radio radiation ID MAGNETIC-FIELD; GAURIBIDANUR RADIOHELIOGRAPH; VLA OBSERVATIONS; PLASMA EMISSION; SOURCE REGION; QUIET SUN; BURSTS; IV; WAVELENGTHS; ECLIPSE AB Low-frequency (80 MHz) imaging and spectral (approximate to 85-20 MHz) observations of moving type IV radio bursts associated with coronal mass ejections (CMEs) from the Sun on three different days are reported. The estimated drift speed of the bursts is in the range approximate to 150-500 km s(-1). We find that all three bursts are most likely due to second harmonic plasma emission from the enhanced electron density in the associated white-light CMEs. The derived maximum magnetic field strength of the latter is B approximate to 4 G at a radial distance of r approximate to 1.6 R-circle dot C1 [Ramesh, R.; Kishore, P.; Barve, Indrajit V.; Kathiravan, C.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Mulay, Sargam M.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Wang, T. J.] Catholic Univ Amer, Dept Phys, Greenbelt, MD 20771 USA. [Wang, T. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ramesh, R (reprint author), Indian Inst Astrophys, Bangalore 560034, Karnataka, India. EM ramesh@iiap.res.in FU NASA [NNG11PL10A, NNX12AB34G] FX It is a pleasure to thank the staff of the Gauribidanur observatory for their help in observations and maintenance of the antenna and receiver systems there. R.R. thanks O.C. St. Cyr for his kind help in connection with the use of STEREO-COR1 data. The SOHO data are produced by a consortium of the Naval Research Laboratory (USA), Max-Planck-Institut fur Aeronomie (Germany), Laboratoire d'Astronomie (France), and the University of Birmingham (UK). SOHO is a project of international cooperation between ESA and NASA. The SOHO-LASCO CMEcatalog is generated and maintained at the CDAW Data Center by NASA and the Catholic University of America in cooperation with the Naval Research Laboratory. The SDO/AIA data are courtesy of the NASA/SDO and the AIA science teams. The work was carried out when one of the authors (S.M.M.) was a Visiting Intern at the Indian Institute of Astrophysics. The work of T.J.W. was supported by NASA Cooperative Agreement NNG11PL10A to CUA and NASA grant NNX12AB34G. We thank the referee for his/her comments and suggestions that helped us to bring out the results more clearly. NR 70 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 30 DI 10.1088/0004-637X/778/1/30 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700030 ER PT J AU Ryan, DF Chamberlin, PC Milligan, RO Gallagher, PT AF Ryan, Daniel F. Chamberlin, Phillip C. Milligan, Ryan O. Gallagher, Peter T. TI DECAY-PHASE COOLING AND INFERRED HEATING OF M- AND X-CLASS SOLAR FLARES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: flares; Sun: general ID RAY TELESCOPE XRT; CORONAL LOOPS; MULTIWAVELENGTH OBSERVATIONS; ATOMIC DATABASE; PLASMAS; TEMPERATURE; DIAGNOSTICS; EVOLUTION; CHIANTI; DESIGN AB In this paper, the cooling of 72 M- and X-class flares is examined using GOES/XRS and SDO/EVE. The observed cooling rates are quantified and the observed total cooling times are compared with the predictions of an analytical zero-dimensional hydrodynamic model. We find that the model does not fit the observations well, but does provide a well-defined lower limit on a flare's total cooling time. The discrepancy between observations and the model is then assumed to be primarily due to heating during the decay phase. The decay-phase heating necessary to account for the discrepancy is quantified and found be similar to 50% of the total thermally radiated energy, as calculated with GOES. This decay-phase heating is found to scale with the observed peak thermal energy. It is predicted that approximating the total thermal energy from the peak is minimally affected by the decay-phase heating in small flares. However, in the most energetic flares the decay-phase heating inferred from the model can be several times greater than the peak thermal energy. C1 [Ryan, Daniel F.; Gallagher, Peter T.] Univ Dublin Trinity Coll, Sch Phys, Dublin 2, Ireland. [Ryan, Daniel F.; Chamberlin, Phillip C.; Milligan, Ryan O.] NASA, Goddard Space Flight Ctr, Solar Phys Lab Code 671, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Ryan, Daniel F.; Milligan, Ryan O.] Catholic Univ Amer, Washington, DC 20064 USA. [Milligan, Ryan O.] Queens Univ Belfast, Belfast BT7 1NN, Antrim, North Ireland. RP Ryan, DF (reprint author), Univ Dublin Trinity Coll, Sch Phys, Dublin 2, Ireland. RI Chamberlin, Phillip/C-9531-2012; Gallagher, Peter/C-7717-2011 OI Chamberlin, Phillip/0000-0003-4372-7405; Gallagher, Peter/0000-0001-9745-0400 FU Fulbright Association; Living With a Star Targeted Research and Technology Program; Leverhulme Trust [F/00203/X]; NASA [NNX11AQ53G] FX We thank the anonymous referee for providing constructive feedback on this manuscript. D. F. R. thanks Arthur J. White, Trevor A. Bowen, Dr. Jim Klimchuk, Dr. Joel C. Allred, and Dr. C. Alex Young for their helpful discussions. He thanks the Fulbright Association for funding the research. P. C. C. and D. F. R. acknowledge funding from the Living With a Star Targeted Research and Technology Program. R.O.M. is grateful to the Leverhulme Trust for financial support from grant F/00203/X and to NASA for LWS/TR&T grant NNX11AQ53G. NR 44 TC 10 Z9 10 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 68 DI 10.1088/0004-637X/778/1/68 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700068 ER PT J AU Sayers, J Mroczkowski, T Zemcov, M Korngut, PM Bock, J Bulbul, E Czakon, NG Egami, E Golwala, SR Koch, PM Lin, KY Mantz, A Molnar, SM Moustakas, L Pierpaoli, E Rawle, TD Reese, ED Rex, M Shitanishi, JA Siegel, S Umetsu, K AF Sayers, J. Mroczkowski, T. Zemcov, M. Korngut, P. M. Bock, J. Bulbul, E. Czakon, N. G. Egami, E. Golwala, S. R. Koch, P. M. Lin, K. -Y. Mantz, A. Molnar, S. M. Moustakas, L. Pierpaoli, E. Rawle, T. D. Reese, E. D. Rex, M. Shitanishi, J. A. Siegel, S. Umetsu, K. TI A MEASUREMENT OF THE KINETIC SUNYAEV-ZEL'DOVICH SIGNAL TOWARD MACS J0717.5+3745 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (MACS J0717.5+3745); galaxies: clusters: intracluster medium ID MASSIVE GALAXY CLUSTERS; SOUTH-POLE TELESCOPE; STAR-FORMING GALAXIES; 2 DISTANT CLUSTERS; X-RAY; RELATIVISTIC CORRECTIONS; LAMBDA-CDM; BULK FLOW; XMM-NEWTON; BACKGROUND ANISOTROPIES AB We report our analysis of MACS J0717.5+3745 using 140 and 268 GHz Bolocam data collected at the Caltech Submillimeter Observatory. We detect extended Sunyaev-Zel'dovich (SZ) effect signal at high significance in both Bolocam bands, and we employ Herschel-SPIRE observations to subtract the signal from dusty background galaxies in the 268 GHz data. We constrain the two-band SZ surface brightness toward two of the sub-clusters of MACS J0717.5+3745: the main sub-cluster (named C), and a sub-cluster identified in spectroscopic optical data to have a line-of-sight velocity of +3200 km s (1) (named B). We determine the surface brightness in two separate ways: via fits of parametric models and via direct integration of the images. For both sub-clusters, we find consistent surface brightnesses from both analysis methods. We constrain spectral templates consisting of relativistically corrected thermal and kinetic SZ signals, using a jointly-derived electron temperature from Chandra and XMM-Newton under the assumption that each sub-cluster is isothermal. The data show no evidence for a kinetic SZ signal toward sub-cluster C, but they do indicate a significant kinetic SZ signal toward sub-cluster B. The model-derived surface brightnesses for sub-cluster B yield a best-fit, line-of-sight velocity of v(z) = +3450 +/- 900 km s(-1), with (1 - Prob[v(z) >= 0]) = 1.3 x 10(-5) (4.2 sigma away from 0 for a Gaussian distribution). The directly integrated sub-cluster B SZ surface brightnesses provide a best-fit v(z) = +2550 +/- 1050 km s(-1), with (1 - Prob[ v(z) >= 0]) = 2.2 x 10(-3) (2.9 sigma). C1 [Sayers, J.; Mroczkowski, T.; Zemcov, M.; Bock, J.; Czakon, N. G.; Golwala, S. R.; Siegel, S.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Mroczkowski, T.; Zemcov, M.; Korngut, P. M.; Bock, J.; Moustakas, L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bulbul, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Egami, E.; Rawle, T. D.; Rex, M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Koch, P. M.; Lin, K. -Y.; Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Mantz, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Molnar, S. M.] Natl Taiwan Univ, LeCosPA Ctr, Taipei 10617, Taiwan. [Pierpaoli, E.; Shitanishi, J. A.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Reese, E. D.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Reese, E. D.] Moorpark Coll, Dept Phys Astron & Engn, Moorpark, CA 93021 USA. RP Sayers, J (reprint author), CALTECH, Div Phys Math & Astron, 1200 East Calif Blvd, Pasadena, CA 91125 USA. EM jack@caltech.edu OI Mroczkowski, Tony/0000-0003-3816-5372; Umetsu, Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360; Pierpaoli, Elena/0000-0002-7957-8993 FU Gordon and Betty Moore Foundation; Norris Foundation CCAT Postdoctoral Fellowship; NASA [PF0-110077, NAS8-0360]; Chandra X-ray Center; NASA Postdoctoral Program Fellowship; NASA Graduate Student Research Fellowship; NASA Earth and Space Science Fellowship [NASA/NNX12AL62H]; National Science Council of Taiwan [NSC100-2112-M-001-008-MY3]; Academia Sinica Career Development Award; [NSF/AST-0838261]; [NASA/NNX11AB07G]; [NSF/AST-0838187]; [NSF/AST-1140019]; [NASA/NNX07AH59G] FX We acknowledge the assistance of: the day crew and Hilo staff of the Caltech Submillimeter Observatory, who provided invaluable assistance during data-taking for this data set; Kathy Deniston, Barbara Wertz, and Diana Bisel, who provided effective administrative support at Caltech and in Hilo; the Bolocam observations were partially supported by the Gordon and Betty Moore Foundation. J.S. was supported by NSF/AST-0838261, NASA/NNX11AB07G, and the Norris Foundation CCAT Postdoctoral Fellowship; support for T.M. was provided by NASA through Einstein Fellowship Program grant No. PF0-110077 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060; P.M.K. was supported by a NASA Postdoctoral Program Fellowship; N.C. was partially supported by a NASA Graduate Student Research Fellowship; A.M. was partially supported by NSF/AST-0838187 and NSF/AST-1140019; E.P. and J. A. S. were partially supported by NASA/NNX07AH59G; S.S. was supported by NASA Earth and Space Science Fellowship NASA/NNX12AL62H; K.U. acknowledges partial support from the National Science Council of Taiwan grant NSC100-2112-M-001-008-MY3 and from the Academia Sinica Career Development Award. A portion of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This research made use of the Caltech Submillimeter Observatory, which was operated at the time by the California Institute of Technology under cooperative agreement with the National Science Foundation (NSF/AST-0838261). This work is also based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with a significant participation by NASA. Partial support for this work was provided by NASA through an award issued by JPL/Caltech. NR 101 TC 23 Z9 23 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 52 DI 10.1088/0004-637X/778/1/52 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700052 ER PT J AU Sekanina, Z Kracht, R AF Sekanina, Zdenek Kracht, Rainer TI POPULATION OF SOHO/STEREO KREUTZ SUNGRAZERS AND THE ARRIVAL OF COMET C/2011 W3 (LOVEJOY) SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: general; comets: individual (X/1106 C1, C/1843 D1, D/1993 F2, C/1996 Y1, C/2001 G2, C/2003 F5, C/2003 K7, C/2004 A4, C/2004 P5, C/2005 U5, C/2006 A5, C/2006 U8, C/2006 V2, C/2007 S4, C/2008 K4, C/2009 C3, C/2009 D4, C/2009 Y4, C/2010 B3, C/2010 C4, C/2010 E6, C/2010 G4, C/2010 U8, C/2010 V8, C/2010 W2, C/2010 X11-X17, C/2010 Y1-Y16, C/2011 N3, C/2011 W3, C/2012 E2, C/2013 F4, SOHO-2062,-2072,-2143,-2505,-2571,-2574); methods: data analysis ID SOLAR AB We examine properties of the population of SOHO/STEREO (dwarf) Kreutz sungrazing comets from 2004 to 2013, including the arrival rates, peculiar gaps, and a potential relationship to the spectacular comet C/2011W3(Lovejoy). Selection effects, influencing the observed distribution, are largely absent among bright dwarf sungrazers, whose temporal sequence implies the presence of a swarm, with objects brighter at maximum than an apparent magnitude of 3 arriving at a peak rate of similar to 4.6 yr(-1) in late 2010, while those brighter than magnitude 2 arrived at a peak rate of similar to 4.3 yr(-1) in early 2011, both a few times the pre-swarm rate. The entire population of SOHO/STEREO Kreutz sungrazers also peaked about one year before the appearance of C/2011 W3. Orbital data show, however, that a great majority of bright dwarf sungrazers moved in paths similar to that of comet C/1843 D1, deviating 10 degrees or more from the orbit of C/2011 W3 in the angular elements. The evidence from the swarm and the overall elevated arrival rates suggests the existence of a fragmented sizable sungrazer that shortly preceded C/2011 W3 but was independent of it. On the other hand, these findings represent another warning signal that the expected 21st century cluster of spectacular Kreutz comets is on its way to perihelion, to arrive during the coming decades. It is only in this sense that we find a parallel link between C/2011 W3 and the spikes in the population of SOHO/STEREO Kreutz sungrazers. C1 [Sekanina, Zdenek] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sekanina, Z (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Zdenek.Sekanina@jpl.nasa.gov; r.kracht@t-online.de FU National Aeronautics and Space Administration FX This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 14 TC 6 Z9 6 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR UNSP 24 DI 10.1088/0004-637X/778/1/24 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700024 ER PT J AU Shenoy, A Sonbas, E Dermer, C Maximon, LC Dhuga, KS Bhat, PN Hakkila, J Parke, WC Maclachlan, GA Eskandarian, A Ukwatta, TN AF Shenoy, A. Sonbas, E. Dermer, C. Maximon, L. C. Dhuga, K. S. Bhat, P. N. Hakkila, J. Parke, W. C. Maclachlan, G. A. Eskandarian, Ali Ukwatta, T. N. TI PROBING CURVATURE EFFECTS IN THE FERMI GRB 110920 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general ID GAMMA-RAY-BURSTS; SPECTRAL LAGS; PULSE-WIDTH; LUMINOSITY RELATION; ENERGY; FIREBALLS; EMISSION; EVOLUTION; LONG; CONNECTION AB Curvature effects in gamma-ray bursts (GRBs) have long been a source of considerable interest. In a collimated relativistic GRB jet, photons that are off-axis relative to the observer arrive at later times than on-axis photons and are also expected to be spectrally softer. In this work, we invoke a relatively simple kinematic two-shell collision model for a uniform jet profile and compare its predictions to GRB prompt-emission data for observations that have been attributed to curvature effects such as the peak-flux-peak-frequency relation, i.e., the relation between the nu F-nu flux and the spectral peak, E-pk in the decay phase of a GRB pulse, and spectral lags. In addition, we explore the behavior of pulse widths with energy. We present the case of the single-pulse Fermi GRB 110920 as a test for the predictions of the model against observations. C1 [Shenoy, A.; Maximon, L. C.; Dhuga, K. S.; Parke, W. C.; Maclachlan, G. A.; Eskandarian, Ali] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Sonbas, E.] Adiyaman Univ, Dept Phys, TR-02040 Adiyaman, Turkey. [Sonbas, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dermer, C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Bhat, P. N.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA. [Hakkila, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Ukwatta, T. N.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Shenoy, A (reprint author), George Washington Univ, Dept Phys, Washington, DC 20052 USA. EM ashwinsp469@gmail.com FU George Washington University FX The authors (A. S. and K. S. D.) would like to acknowledge O. Kargaltsev (George Washington University) for his valuable contributions to the discussions as well as the financial support provided by him to A. Shenoy at various stages of this work. NR 39 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 3 DI 10.1088/0004-637X/778/1/3 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700003 ER PT J AU Uritsky, VM Davila, JM Viall, NM Ofman, L AF Uritsky, Vadim M. Davila, Joseph M. Viall, Nicholeen M. Ofman, Leon TI MEASURING TEMPERATURE-DEPENDENT PROPAGATING DISTURBANCES IN CORONAL FAN LOOPS USING MULTIPLE SDO/AIA CHANNELS AND THE SURFING TRANSFORM TECHNIQUE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: atmosphere; Sun: corona; Sun: UV radiation; waves ID SLOW MAGNETOACOUSTIC WAVES; X-RAY LINES; ACTIVE-REGION OUTFLOWS; MAGNETOSONIC WAVES; SOLAR CORONA; ATOMIC DATA; SPECTROSCOPIC OBSERVATIONS; HINODE/EIS OBSERVATIONS; UPFLOWS; ASTROPHYSICS AB A set of co-aligned high-resolution images from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory is used to investigate propagating disturbances (PDs) in warm fan loops at the periphery of a non-flaring active region NOAA AR 11082. To measure PD speeds at multiple coronal temperatures, a new data analysis methodology is proposed enabling a quantitative description of subvisual coronal motions with low signal-to-noise ratios of the order of 0.1%. The technique operates with a set of one-dimensional "surfing" signals extracted from position-time plots of several AIA channels through a modified version of Radon transform. The signals are used to evaluate a two-dimensional power spectral density distribution in the frequency-velocity space that exhibits a resonance in the presence of quasi-periodic PDs. By applying this analysis to the same fan loop structures observed in several AIA channels, we found that the traveling velocity of PDs increases with the temperature of the coronal plasma following the square-root dependence predicted for slow mode magneto-acoustic waves which seem to be the dominating wave mode in the loop structures studied. This result extends recent observations by Kiddie et al. to a more general class of fan loop system not associated with sunspots and demonstrating consistent slow mode activity in up to four AIA channels. C1 [Uritsky, Vadim M.; Ofman, Leon] Catholic Univ Amer, Washington, DC 20064 USA. [Uritsky, Vadim M.; Davila, Joseph M.; Viall, Nicholeen M.; Ofman, Leon] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Uritsky, VM (reprint author), Catholic Univ Amer, Washington, DC 20064 USA. FU NASA through the CUAs Institute for Astrophysics and Computational Sciences [NNG11PL10A 670.002]; NASA [NNX12AB34G] FX The authors thank James Klimchuk and Tongjian Wang for useful discussions. V.U. was supported by the NASA Grant NNG11PL10A 670.002 through the CUAs Institute for Astrophysics and Computational Sciences. L.O. was supported by NASA grant NNX12AB34G. N.V. thanks Harry Warren for help with the derotation methodology. NR 44 TC 10 Z9 11 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 26 DI 10.1088/0004-637X/778/1/26 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700026 ER PT J AU Virgili, FJ Mundell, CG Pal'Shin, V Guidorzi, C Margutti, R Melandri, A Harrison, R Kobayashi, S Chornock, R Henden, A Updike, AC Cenko, SB Tanvir, NR Steele, IA Cucchiara, A Gomboc, A Levan, A Cano, Z Mottram, CJ Clay, NR Bersier, D Kopac, D Japelj, J Filippenko, AV Li, W Svinkin, D Golenetskii, S Hartmann, DH Milne, PA Williams, G O'Brien, PT Fox, DB Berger, E AF Virgili, F. J. Mundell, C. G. Pal'Shin, V. Guidorzi, C. Margutti, R. Melandri, A. Harrison, R. Kobayashi, S. Chornock, R. Henden, A. Updike, A. C. Cenko, S. B. Tanvir, N. R. Steele, I. A. Cucchiara, A. Gomboc, A. Levan, A. Cano, Z. Mottram, C. J. Clay, N. R. Bersier, D. Kopac, D. Japelj, J. Filippenko, A. V. Li, W. Svinkin, D. Golenetskii, S. Hartmann, D. H. Milne, P. A. Williams, G. O'Brien, P. T. Fox, D. B. Berger, E. TI GRB 091024A AND THE NATURE OF ULTRA-LONG GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual (GRB 091024A) ID AUTOMATIC IMAGING TELESCOPE; REVERSE SHOCK EMISSION; CENTRAL ENGINE; LIGHT CURVES; PROMPT EMISSION; SPECTRAL EVOLUTION; AFTERGLOW EMISSION; OPTICAL-EMISSION; QUIESCENT TIMES; KINETIC-ENERGY AB We present a broadband study of gamma-ray burst (GRB) 091024A within the context of other ultra-long-duration GRBs. An unusually long burst detected by Konus-Wind (KW), Swift, and Fermi, GRB 091024A has prompt emission episodes covering similar to 1300 s, accompanied by bright and highly structured optical emission captured by various rapid-response facilities, including the 2 m autonomous robotic Faulkes North and Liverpool Telescopes, KAIT, S-LOTIS, and the Sonoita Research Observatory. We also observed the burst with 8 and 10 m class telescopes and determine the redshift to be z = 1.0924 +/- 0.0004. We find no correlation between the optical and gamma-ray peaks and interpret the optical light curve as being of external origin, caused by the reverse and forward shock of a highly magnetized jet (R-B approximate to 100-200). Low-level emission is detected throughout the near-background quiescent period between the first two emission episodes of the KW data, suggesting continued central-engine activity; we discuss the implications of this ongoing emission and its impact on the afterglow evolution and predictions. We summarize the varied sample of historical GRBs with exceptionally long durations in gamma-rays ( greater than or similar to 1000 s) and discuss the likelihood of these events being from a separate population; we suggest ultra-long GRBs represent the tail of the duration distribution of the long GRB population. C1 [Virgili, F. J.; Mundell, C. G.; Harrison, R.; Kobayashi, S.; Steele, I. A.; Mottram, C. J.; Clay, N. R.; Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Pal'Shin, V.; Svinkin, D.; Golenetskii, S.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Guidorzi, C.] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy. [Margutti, R.; Chornock, R.; Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Melandri, A.] INAF Brera Astron Observ, I-23807 Merate, LC, Italy. [Henden, A.] AAVSO, Cambridge, MA 02138 USA. [Updike, A. C.] Roger Williams Univ, Dept Chem & Phys, Bristol, RI 02809 USA. [Cenko, S. B.; Filippenko, A. V.; Li, W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Tanvir, N. R.; O'Brien, P. T.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Cucchiara, A.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Gomboc, A.; Kopac, D.; Japelj, J.] Univ Ljubljana, Fac Math & Phys, Ljubljana 1000, Slovenia. [Levan, A.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Cano, Z.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Hartmann, D. H.] Clemson Univ, Dept Phys & Astron, Kinard Lab 118, Clemson, SC 29631 USA. [Milne, P. A.; Williams, G.] Univ Arizona, MMT Observ, Tucson, AZ 85719 USA. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. RP Virgili, FJ (reprint author), Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. EM F.J.Virgili@ljmu.ac.uk RI Svinkin, Dmitry/C-1934-2014; Pal'shin, Valentin/F-3973-2014; Golenetskii, Sergey/B-3818-2015 FU UK Science and Technology Facilities Council; Royal Society; Wolfson Foundation; Sun Microsys-tems, Inc.; Hewlett-Packard Company; AutoScope Corporation; Lick Observatory; NSF; University of California; Sylvia and Jim Katzman Foundation; TABASGO Foundation; W. M. Keck Foundation; Gary and Cynthia Bengier; Christopher R. Redlich Fund; Richard and Rhoda Goldman Fund; NSF [AST-1211916]; NASA/Swift [NNX10AI21G, NNX12AD73G] FX F.J.V. acknowledges support from the UK Science and Technology Facilities Council. C.G.M. acknowledges funding from the Royal Society, the Wolfson Foundation, and the UK Science and Technology Facilities Council. We are grateful for excellent staff assistance at the various observatories where we obtained data. The Liverpool Telescope is operated by Liverpool John Moores University at the Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The Faulkes Telescopes, now owned by the Las Cumbres Observatory Global Telescope network, are operated with support from the Dill Faulkes Educational Trust. KAIT and its ongoing operation were made possible by donations from Sun Microsys-tems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia and Jim Katzman Foundation, and the TABASGO Foundation. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The Konus-Wind experiment is supported by a Russian Space Agency contract and RFBR grant 12-02-00032-a. Swift, launched in 2004 November, is a NASA mission in partnership with the Italian Space Agency and the UK Space Agency. A.V.F.'s group at UC Berkeley has received generous financial assistance from Gary and Cynthia Bengier, the Christopher R. Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, NSF grant AST-1211916, and NASA/Swift grants NNX10AI21G and NNX12AD73G. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. NR 137 TC 36 Z9 36 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 54 DI 10.1088/0004-637X/778/1/54 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700054 ER PT J AU Wang, J Fischer, DA Barclay, T Boyajian, TS Crepp, JR Schwamb, ME Lintott, C Jek, KJ Smith, AM Parrish, M Schawinski, K Schmitt, JR Giguere, MJ Brewer, JM Lynn, S Simpson, R Hoekstra, AJ Jacobs, TL LaCourse, D Schwengeler, HM Chopin, M Herszkowicz, R AF Wang, Ji Fischer, Debra A. Barclay, Thomas Boyajian, Tabetha S. Crepp, Justin R. Schwamb, Megan E. Lintott, Chris Jek, Kian J. Smith, Arfon M. Parrish, Michael Schawinski, Kevin Schmitt, Joseph R. Giguere, Matthew J. Brewer, John M. Lynn, Stuart Simpson, Robert Hoekstra, Abe J. Jacobs, Thomas Lee LaCourse, Daryll Schwengeler, Hans Martin Chopin, Mike Herszkowicz, Rafal TI PLANET HUNTERS. V. A CONFIRMED JUPITER-SIZE PLANET IN THE HABITABLE ZONE AND 42 PLANET CANDIDATES FROM THE KEPLER ARCHIVE DATA (vol 776, pg 10, 2013) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Wang, Ji; Fischer, Debra A.; Boyajian, Tabetha S.; Schmitt, Joseph R.; Giguere, Matthew J.; Brewer, John M.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barclay, Thomas] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Schwamb, Megan E.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Schwamb, Megan E.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Lintott, Chris; Simpson, Robert] Oxford Astrophys, Oxford OX1 3RH, England. [Lintott, Chris; Smith, Arfon M.; Parrish, Michael; Lynn, Stuart] Adler Planetarium, Chicago, IL 60605 USA. [Schawinski, Kevin] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. RP Wang, J (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA. EM ji.wang@yale.edu NR 1 TC 0 Z9 0 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2013 VL 778 IS 1 AR 84 DI 10.1088/0004-637X/778/1/84 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 254AI UT WOS:000327131700084 ER PT J AU Burlaga, LF Ness, NF Gurnett, DA Kurth, WS AF Burlaga, L. F. Ness, N. F. Gurnett, D. A. Kurth, W. S. TI EVIDENCE FOR A SHOCK IN INTERSTELLAR PLASMA: VOYAGER 1 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE local interstellar matter; magnetic fields; Sun: heliosphere ID WIND TERMINATION SHOCK; GALACTIC COSMIC-RAYS; EARTHS BOW SHOCK; SOLAR-WIND; WAVE OBSERVATIONS; REGION; HELIOPAUSE; FREQUENCY; UPSTREAM; SATURN AB Voyager 1 (V1) observed electron plasma oscillations preceding a jump by a factor of 1.4 in the magnetic field intensity B near the end of 2012. The frequency of the electron plasma oscillations gives an electron density n(e) = 0.05 cm(-3), which implies that V1 was immersed in plasma from the interstellar medium. The last day on which plasma oscillations were observed is day 332, 2012, and the jump in the B was centered on day 335, 2012 after a data gap in the wave data. The close association between the electron plasma oscillations and the jump in B suggests a causal connection, such as that frequently observed between electron plasma oscillations and interplanetary shocks at 1 AU. Based on the observed parameters and the smooth profile of B(t), the jump in B appears to be associated with a weak, subcritical, laminar, low beta, quasi-perpendicular, resistive, collisionless shock. However, the width of the jump is of the order of 10(4) times that expected for such a stationary shock at 1 AU. The large width of the jump in B might be the result of differences between the structure of shocks in the interstellar medium and the plasma near 1 AU. Alternatively, the subcritical resistive shock might have decayed during a few days after producing the plasma waves, leaving a broad profile in B(t) without significantly changing ambient parameters. Another possibility is that the jump in B is a pressure wave. C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Gurnett, D. A.; Kurth, W. S.] Univ Iowa, Iowa City, IA 52242 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA. EM lburlagahsp@verizon.net; nfnudel@yahoo.com; donald-gurnett@uiowa.edu; william-kurth@uiowa.edu OI Kurth, William/0000-0002-5471-6202 FU NASA [NNX12AC63G, NNG13PM04P, 1415150]; Jet Propulsion Laboratory FX T. McClanahan and S. Kramer provided support in the processing of the data. D. Berdichevsky computed correction tables for the three sensors on each of the two magnetometers. N. F. Ness was supported by NASA Grant NNX12AC63G to the Catholic University of America. L. F. Burlaga was supported by NASA Contract NNG13PM04P. The research at the University of Iowa was supported by NASA through contract 1415150 with the Jet Propulsion Laboratory. NR 35 TC 21 Z9 21 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 20 PY 2013 VL 778 IS 1 AR UNSP L3 DI 10.1088/2041-8205/778/1/L3 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 253VF UT WOS:000327116700003 ER PT J AU Gupta, H Gottlieb, CA Lattanzi, V Pearson, JC McCarthy, MC AF Gupta, H. Gottlieb, C. A. Lattanzi, V. Pearson, J. C. McCarthy, M. C. TI LABORATORY MEASUREMENTS AND TENTATIVE ASTRONOMICAL IDENTIFICATION OF H2NCO+ SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: molecules ID GALACTIC-CENTER REGION; DIFFUSE INTERSTELLAR-MEDIUM; PROTONATED ISOCYANIC ACID; RAY IONIZATION RATE; LOW-TEMPERATURE; SAGITTARIUS B2; FULMINIC ACID; SGR B2; GAS; HNCO AB The rotational spectrum of H2NCO+, the ground-state isomer of protonated HNCO, has been measured in a molecular beam in the centimeter band with a Fourier transform microwave spectrometer and in a low-pressure laboratory discharge in absorption in the millimeter band. Spectroscopic constants, including the nitrogen-14 hyperfine coupling constant, derived from 30 a-type transitions between 20 and 367 GHz with J <= 18 and K-a <= 3 allow the principal rotational transitions to be calculated to 1 km s(-1) or better in equivalent radial velocity well into the far IR. Two low-lying rotational transitions of H2NCO+ in the centimeter band (0(0,0)-1(0,1) and 1(1,0)-2(1,1)) were tentatively identified in absorption in the PRIMOS spectral line survey of Sgr B2(N) with the Green Bank Telescope. The lines of H2NCO+ arise in a region of the Sgr B2(N) halo whose density is low (n < 1 x 10(4) cm(-3)). The derived column density of (6-14) x 10(11) cm(-2) implies that the fractional abundance is similar to 10(-12). Owing to the ubiquity of HNCO in galactic molecular clouds, H2NCO+ is a good candidate for detection in sources spanning a wide range of physical conditions. C1 [Gupta, H.; Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gottlieb, C. A.; Lattanzi, V.; McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gupta, H (reprint author), CALTECH, Infrared Proc & Anal Ctr, 770 S Wilson Ave, Pasadena, CA 91125 USA. FU NASA [NNX13AE59G, NNX08AE05G, NNX08AI41G]; National Aeronautics and Space Administration FX We are indebted to P. F. Goldsmith, M. Gerin, and D. C. Lis for helpful discussions; S. Thorwirth for communicating results of his high-level coupled cluster quantum calculations; J. Neill for sharing unpublished measurements of HNCO in Sgr B2(N) with Herschel; and F. Crim for advice and D. Kokkin for assistance with the preparation of the HNCO precursor in the laboratory experiments. The work in Cambridge was supported by NASA Grants NNX13AE59G, NNX08AE05G, and NNX08AI41G. A portion of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 35 TC 5 Z9 5 U1 1 U2 17 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 20 PY 2013 VL 778 IS 1 AR L1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 253VF UT WOS:000327116700001 ER PT J AU Janson, M Brandt, TD Kuzuhara, M Spiegel, DS Thalmann, C Currie, T Bonnefoy, M Zimmerman, N Sorahana, S Kotani, T Schlieder, J Hashimoto, J Kudo, T Kusakabe, N Abe, L Brandner, W Carson, JC Egner, S Feldt, M Goto, M Grady, CA Guyon, O Hayano, Y Hayashi, M Hayashi, S Henning, T Hodapp, KW Ishii, M Iye, M Kandori, R Knapp, GR Kwon, J Matsuo, T McElwain, MW Mede, K Miyama, S Morino, JI Moro-Martin, A Nakagawa, T Nishimura, T Pyo, TS Serabyn, E Suenaga, T Suto, H Suzuki, R Takahashi, Y Takami, M Takato, N Terada, H Tomono, D Turner, EL Watanabe, M Wisniewski, J Yamada, T Takami, H Usuda, T Tamura, M AF Janson, Markus Brandt, Timothy D. Kuzuhara, Masayuki Spiegel, David S. Thalmann, Christian Currie, Thayne Bonnefoy, Mickael Zimmerman, Neil Sorahana, Satoko Kotani, Takayuki Schlieder, Joshua Hashimoto, Jun Kudo, Tomoyuki Kusakabe, Nobuhiko Abe, Lyu Brandner, Wolfgang Carson, Joseph C. Egner, Sebastian Feldt, Markus Goto, Miwa Grady, Carol A. Guyon, Olivier Hayano, Yutaka Hayashi, Masahiko Hayashi, Saeko Henning, Thomas Hodapp, Klaus W. Ishii, Miki Iye, Masanori Kandori, Ryo Knapp, Gillian R. Kwon, Jungmi Matsuo, Taro McElwain, Michael W. Mede, Kyle Miyama, Shoken Morino, Jun-Ichi Moro-Martin, Amaya Nakagawa, Takao Nishimura, Tetsuro Pyo, Tae-Soo Serabyn, Eugene Suenaga, Takuya Suto, Hiroshi Suzuki, Ryuji Takahashi, Yasuhiro Takami, Michihiro Takato, Naruhisa Terada, Hiroshi Tomono, Daego Turner, Edwin L. Watanabe, Makoto Wisniewski, John Yamada, Toru Takami, Hideki Usuda, Tomonori Tamura, Motohide TI DIRECT IMAGING DETECTION OF METHANE IN THE ATMOSPHERE OF GJ 504 b SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: solar-type; techniques: photometric ID ORBITING HR 8799; SUN-LIKE STAR; BROWN DWARFS; SUBSTELLAR COMPANION; EVOLUTIONARY MODELS; GIANT PLANETS; ROSS 458C; T DWARFS; MU-M; SPECTROSCOPY AB Most exoplanets detected by direct imaging thus far have been characterized by relatively hot (greater than or similar to 1000 K) and cloudy atmospheres. A surprising feature in some of their atmospheres has been a distinct lack of methane, possibly implying non-equilibrium chemistry. Recently, we reported the discovery of a planetary companion to the Sun-like star GJ 504 using Subaru/HiCIAO within the Strategic Exploration of Exoplanets and Disks with Subaru survey. The planet is substantially colder (<600 K) than previously imaged planets, and has indications of fewer clouds, which implies that it represents a new class of planetary atmospheres with expected similarities to late T-type brown dwarfs in the same temperature range. If so, one might also expect the presence of significant methane absorption, which is characteristic of such objects. Here, we report the detection of deep methane absorption in the atmosphere of GJ 504 b, using the Spectral Differential Imaging mode of HiCIAO to distinguish the absorption features around 1.6 mu m. We also report updated JHK photometry based on new K-s-band data and a re-analysis of the existing data. The results support the notion that GJ 504 b has atmospheric properties distinct from other imaged exoplanets, and will become a useful reference object for future planets in the same temperature range. C1 [Janson, Markus] Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Janson, Markus; Brandt, Timothy D.; Knapp, Gillian R.; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Kuzuhara, Masayuki; Mede, Kyle] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. [Kuzuhara, Masayuki; Kotani, Takayuki; Hashimoto, Jun; Kusakabe, Nobuhiko; Hayashi, Masahiko; Iye, Masanori; Kandori, Ryo; Morino, Jun-Ichi; Suto, Hiroshi; Tamura, Motohide] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Spiegel, David S.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA. [Thalmann, Christian] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Currie, Thayne] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. [Bonnefoy, Mickael; Zimmerman, Neil; Schlieder, Joshua; Brandner, Wolfgang; Feldt, Markus; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Sorahana, Satoko] Nagoya Univ, Div Particle & Astrophys Sci, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Kudo, Tomoyuki; Egner, Sebastian; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko; Ishii, Miki; Nishimura, Tetsuro; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daego; Takami, Hideki; Usuda, Tomonori] Subaru Telescope, Hilo, HI 96720 USA. [Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7239, F-06300 Nice, France. [Carson, Joseph C.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Goto, Miwa] Univ Munich, Univ Sternwarte, D-81679 Munich, Germany. [Grady, Carol A.; McElwain, Michael W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Grady, Carol A.] Eureka Sci, Oakland, CA 96002 USA. [Hodapp, Klaus W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Kwon, Jungmi; Suenaga, Takuya; Tamura, Motohide] Grad Univ Adv Studies Sokendai, Dept Astron Sci, Tokyo 1818588, Japan. [Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Miyama, Shoken] Hiroshima Univ, Off President, Hagashi Hiroshima, Japan. [Moro-Martin, Amaya] CSIC, INTA, CAB, Dept Astrophys, E-28850 Madrid, Spain. [Nakagawa, Takao] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. [Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Suzuki, Ryuji] TMT Observ Corp, Pasadena, CA 91105 USA. [Takahashi, Yasuhiro] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan. [Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan. [Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. RP Janson, M (reprint author), Queens Univ Belfast, Astrophys Res Ctr, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland. EM m.janson@qub.ac.uk RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016; OI Watanabe, Makoto/0000-0002-3656-4081; Zimmerman, Neil/0000-0001-5484-1516 FU NASA [HF-51290.01, NAS 5-26555]; Space Telescope Science Institute; NSF [1009203] FX Part of this work was supported by NASA through Hubble Fellowship grant HF-51290.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555, and through NSF award 1009203. We thank the referee, Adam Burgasser, for his very useful comments. This study made use of the CDS services SIMBAD and VizieR, as well as the SAO/NASA ADS service. The study has benefitted from the SpeX Prism Spectral Libraries at http://www.browndwarfs.org/spexprism. NR 45 TC 36 Z9 37 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 20 PY 2013 VL 778 IS 1 AR L4 DI 10.1088/2041-8205/778/1/L4 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 253VF UT WOS:000327116700004 ER PT J AU Maseda, MV van der Wel, A da Cunha, E Rix, HW Pacifici, C Momcheva, I Brammer, GB Franx, M van Dokkum, P Bell, EF Fumagalli, M Grogin, NA Kocevski, DD Koekemoer, AM Lundgren, BF Marchesini, D Nelson, EJ Patel, SG Skelton, RE Straughn, AN Trump, JR Weiner, BJ Whitaker, KE Wuyts, S AF Maseda, Michael V. van der Wel, Arjen da Cunha, Elisabete Rix, Hans-Walter Pacifici, Camilla Momcheva, Ivelina Brammer, Gabriel B. Franx, Marijn van Dokkum, Pieter Bell, Eric F. Fumagalli, Mattia Grogin, Norman A. Kocevski, Dale D. Koekemoer, Anton M. Lundgren, Britt F. Marchesini, Danilo Nelson, Erica J. Patel, Shannon G. Skelton, Rosalind E. Straughn, Amber N. Trump, Jonathan R. Weiner, Benjamin J. Whitaker, Katherine E. Wuyts, Stijn TI CONFIRMATION OF SMALL DYNAMICAL AND STELLAR MASSES FOR EXTREME EMISSION LINE GALAXIES AT z similar to 2 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: dwarf; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: starburst ID STAR-FORMING GALAXIES; EXTRAGALACTIC LEGACY SURVEY; DWARF SPHEROIDAL GALAXIES; HUBBLE-SPACE-TELESCOPE; CANDIDATE UDFJ-39546284; CANDELS; FIELD; GAS; KINEMATICS; PARAMETERS AB Spectroscopic observations from the Large Binocular Telescope and the Very Large Telescope reveal kinematically narrow lines (similar to 50 km s(-1)) for a sample of 14 extreme emission line galaxies at redshifts 1.4 < z < 2.3. These measurements imply that the total dynamical masses of these systems are low (less than or similar to 3 x 10(9) M-circle dot). Their large [O III] lambda 5007 equivalent widths (500-1100 angstrom) and faint blue continuum emission imply young ages of 10-100 Myr and stellar masses of 10(8)-10(9) M-circle dot, confirming the presence of a violent starburst. The dynamical masses represent the first such determinations for low-mass galaxies at z > 1. The stellar mass formed in this vigorous starburst phase represents a large fraction of the total (dynamical) mass, without a significantly massive underlying population of older stars. The occurrence of such intense events in shallow potentials strongly suggests that supernova-driven winds must be of critical importance in the subsequent evolution of these systems. C1 [Maseda, Michael V.; van der Wel, Arjen; da Cunha, Elisabete; Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Pacifici, Camilla] Yonsei Univ, Yonsei Univ Observ, Seoul 120749, South Korea. [Momcheva, Ivelina; van Dokkum, Pieter; Nelson, Erica J.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Brammer, Gabriel B.; Grogin, Norman A.; Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Franx, Marijn; Fumagalli, Mattia; Patel, Shannon G.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Kocevski, Dale D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Lundgren, Britt F.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Marchesini, Danilo] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. [Skelton, Rosalind E.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Straughn, Amber N.; Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Trump, Jonathan R.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Trump, Jonathan R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Weiner, Benjamin J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Maseda, MV (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM maseda@mpia.de RI Skelton, Rosalind/S-1845-2016; OI Skelton, Rosalind/0000-0001-7393-3336; Koekemoer, Anton/0000-0002-6610-2048; da Cunha, Elisabete/0000-0001-9759-4797; Bell, Eric/0000-0002-5564-9873 FU NASA [NAS5-26555]; European Southern Observatory, Chile [089.B-0236(A)] FX M.V.M. is a member of the International Max Planck Research School for Astronomy and Cosmic Physics at the University of Heidelberg, IMPRS-HD, Germany. This work is based on observations taken by the 3D-HST Treasury Program and the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555, and at the European Southern Observatory, Chile, Program 089.B-0236(A). NR 39 TC 16 Z9 16 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 20 PY 2013 VL 778 IS 1 AR UNSP L22 DI 10.1088/2041-8205/778/1/L22 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 253VF UT WOS:000327116700022 ER PT J AU Zheng, WK Silverman, JM Filippenko, AV Kasen, D Nugent, PE Graham, M Wang, XF Valenti, S Ciabattari, F Kelly, PL Fox, OD Shivvers, I Clubb, KI Cenko, SB Balam, D Howell, DA Hsiao, E Li, WD Marion, GH Sand, D Vinko, J Wheeler, JC Zhang, JJ AF Zheng, WeiKang Silverman, Jeffrey M. Filippenko, Alexei V. Kasen, Daniel Nugent, Peter E. Graham, Melissa Wang, Xiaofeng Valenti, Stefano Ciabattari, Fabrizio Kelly, Patrick L. Fox, Ori D. Shivvers, Isaac Clubb, Kelsey I. Cenko, S. Bradley Balam, Dave Howell, D. Andrew Hsiao, Eric Li, Weidong Marion, G. Howie Sand, David Vinko, Jozsef Wheeler, J. Craig Zhang, JuJia TI THE VERY YOUNG TYPE Ia SUPERNOVA 2013dy: DISCOVERY, AND STRONG CARBON ABSORPTION IN EARLY-TIME SPECTRA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE supernovae: general; supernovae: individual (SN 2013dy) ID WHITE-DWARF STAR; SPECTROSCOPIC OBSERVATIONS; LIGHT CURVES; SN 2011FE; TELESCOPE; PROGRAM; 2009DC; SPECTROGRAPH; ULTRAVIOLET; PROGENITOR AB The Type Ia supernova (SN Ia) 2013dy in NGC 7250 (d approximate to 13.7 Mpc) was discovered by the Lick Observatory Supernova Search. Combined with a prediscovery detection by the Italian Supernova Search Project, we are able to constrain the first-light time of SN 2013dy to be only 0.10 +/- 0.05 days (2.4 +/- 1.2 hr) before the first detection. This makes SN 2013dy the earliest known detection of an SN Ia. We infer an upper limit on the radius of the progenitor star of R-0 less than or similar to 0.25 R-circle dot, consistent with that of a white dwarf. The light curve exhibits a broken power law with exponents of 0.88 and then 1.80. A spectrum taken 1.63 days after first light reveals a C II absorption line comparable in strength to Si II. This is the strongest C II feature ever detected in a normal SN Ia, suggesting that the progenitor star had significant unburned material. The C II line in SN 2013dy weakens rapidly and is undetected in a spectrum 7 days later, indicating that C II is detectable for only a very short time in some SNe Ia. SN 2013dy reached a B-band maximum of M-B = -18.72 +/- 0.03 mag similar to 17.7 days after first light. C1 [Zheng, WeiKang; Filippenko, Alexei V.; Nugent, Peter E.; Graham, Melissa; Kelly, Patrick L.; Fox, Ori D.; Shivvers, Isaac; Clubb, Kelsey I.; Li, Weidong] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Silverman, Jeffrey M.; Marion, G. Howie; Vinko, Jozsef; Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Kasen, Daniel; Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Kasen, Daniel] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Graham, Melissa; Valenti, Stefano; Howell, D. Andrew] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Graham, Melissa; Valenti, Stefano; Howell, D. Andrew] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wang, Xiaofeng] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Ciabattari, Fabrizio] Monte Agliale Observ, I-55023 Borgo A Mozzano, Lucca, Italy. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Balam, Dave] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Astrophys Observ, Victoria, BC V9E 2E7, Canada. [Hsiao, Eric] Las Campanas Observ, Carnegie Observ, Colina El Pino, Chile. [Marion, G. Howie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sand, David] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Vinko, Jozsef] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Zhang, JuJia] Chinese Acad Sci, Yunan Astron Observ, Beijing 650011, Yunnan, Peoples R China. [Zhang, JuJia] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650011, Peoples R China. RP Zheng, WK (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM zwk@astro.berkeley.edu RI Wang, Xiaofeng/J-5390-2015; OI Shivvers, Isaac/0000-0003-3373-8047 FU TABASGO Foundation; Sylvia and Jim Katzman Foundation; Christopher R. Redlich Fund; NSF [AST-1211916, AST-1302771, AST-1109801]; NNSFC [11073013, 11178003]; Foundation of Tsinghua University [2011Z02170]; Major State Basic Research Development Program [2013CB834903]; Hungarian OTKA [NN 107637]; DoE [DE-AC02-05CH11231]; W. M. Keck Foundation FX A.V.F.'s group (and KAIT) at UC Berkeley have received financial assistance from the TABASGO Foundation, the Sylvia and Jim Katzman Foundation, the Christopher R. Redlich Fund, and NSF grant AST-1211916. J.M.S. is supported by an NSF postdoctoral fellowship under award AST-1302771. X. Wang acknowledges NNSFC grants 11073013 and 11178003, the Foundation of Tsinghua University (2011Z02170), and the Major State Basic Research Development Program (2013CB834903). J.V. is grateful for Hungarian OTKA grant NN 107637. J.C.W. acknowledge support from NSF AST-1109801. This research used resources of NERSC, supported by DoE under Contract DE-AC02-05CH11231. Some data were obtained at the W. M. Keck Observatory, which was made possible by the generous financial support of the W. M. Keck Foundation. We thank the staffs of the various observatories at which data were obtained. We also thank the anonymous referee for useful suggestions which improved the Letter. NR 42 TC 28 Z9 28 U1 0 U2 17 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 20 PY 2013 VL 778 IS 1 AR L15 DI 10.1088/2041-8205/778/1/L15 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 253VF UT WOS:000327116700015 ER PT J AU Cable, ML Kirby, JP Gray, HB Ponce, A AF Cable, Morgan L. Kirby, James P. Gray, Harry B. Ponce, Adrian TI Enhancement of Anion Binding in Lanthanide Optical Sensors SO ACCOUNTS OF CHEMICAL RESEARCH LA English DT Review ID TRANSITION-METAL IONS; BACTERIAL SPORE GERMINATION; EARTH CHLORIDE SOLUTIONS; RARE-EARTH; CAPILLARY-ELECTROPHORESIS; PHOTOPHYSICAL PROPERTIES; SENSITIZED LUMINESCENCE; TERBIUM(III) COMPLEXES; EXCHANGE DYNAMICS; AQUEOUS-SOLUTION AB In the design of molecular sensors, researchers exploit binding interactions that are usually defined in terms of topology and charge complementarity. The formation of complementary arrays of highly cooperative, noncovalent bonding networks facilitates protein-ligand binding, leading to motifs such as the "lock-and-key". Synthetic molecular sensors often employ metal complexes as key design elements as a way to construct a binding site with the desired shape and charge to achieve target selectivity. In transition metal complexes, coordination number, structure and ligand dynamics are governed primarily by a combination of inner-sphere covalent and outer-sphere noncovalent interactions. These interactions provide a rich variable space that researchers can use to tune structure, stability, and dynamics. In contrast, lanthanide(III)-ligand complex formation and ligand-exchange dynamics are dominated by reversible electrostatic and steric interactions, because the unfilled f shell Is shielded by the larger, filled d shell. Luminescent lanthanides such as terbium, europium, dysprosium, and samarium display many photophysical properties that make them excellent candidates for molecular sensor applications. Complexes of lanthanide ions act as receptors that exhibit a detectable change in metal-based luminescence upon binding of an anion. In our work on sensors for detection of dipicolinate, the unique biomarker of bacterial spores, we discovered that the incorporation of an ancillary ligand (AL) can enhance binding constants of target anions to lanthanide ions by as much as two orders of magnitude. In this Account, we show that selected ALs in lanthanide/anion systems greatly improve sensor performance for medical, planetary science, and biodefense applications. We suggest that the observed anion binding enhancement could result from an AL-induced increase in positive charge at the lanthanide ion binding site. This effect depends on lanthanide polarizability, which can be established from the ionization energy of Ln(3+) -> Ln(4+). These results account for the order Tb3+ > Dy3+ > Eu3+ approximate to Sm3+. As with many lanthanide properties, ranging from hydration enthalpy to vaporization energy, this AL-induced enhancement shows a large discrepancy between Tb3+ and Eu3+ despite their similarity in size, a phenomenon known as the "gadolinium break". This discrepancy, based on the unusual stabilities of the Eu2+ and Tb4+ oxidation states, results from the half-shell effect, as both of these ions have half-filled 4f-shells. The high polarizability of Tb3+ explains the extraordinarily large increase in the binding affinity of anions for terbium compared to other lanthanides. We recommend that researchers consider this AL-induced enhancement when designing lanthanide-macrocycle optical sensors. Ancillary ligands also can reduce the impact of interfering species such as phosphate commonly found in environmental and physiological samples. C1 [Cable, Morgan L.; Ponce, Adrian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gray, Harry B.] CALTECH, Beckman Inst, Pasadena, CA 91125 USA. [Kirby, James P.] Planetary Sci Inst, Tucson, AZ 85719 USA. RP Gray, HB (reprint author), CALTECH, Beckman Inst, Pasadena, CA 91125 USA. EM hbgray@caltech.edu; Adrian.Ponce@jpl.nasa.gov FU NASA; Department of Homeland Security's Chemical and Biological Research & Development Program; NIH [DKO19038]; Arnold and Mabel Beckman Foundation FX We dedicate this Account to the memory of Michael Day, a wonderful colleague and great friend. The authors would also like to acknowledge helpful comments by the reviewers of this manuscript. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautic and Space Administration and was sponsored by NASA's Astrobiology and Planetary Protection Programs (A.P., J.P.K.), the Department of Homeland Security's Chemical and Biological Research & Development Program (A.P.), and the NASA Graduate Student Research Program (M.L.C). Work at Caltech was supported NIH Grant DKO19038 and the Arnold and Mabel Beckman Foundation. NR 87 TC 22 Z9 22 U1 12 U2 130 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0001-4842 EI 1520-4898 J9 ACCOUNTS CHEM RES JI Accounts Chem. Res. PD NOV 19 PY 2013 VL 46 IS 11 BP 2576 EP 2584 DI 10.1021/ar400050t PG 9 WC Chemistry, Multidisciplinary SC Chemistry GA 257CJ UT WOS:000327360800022 PM 24032446 ER PT J AU Ramanathan, A Mao, JP Allan, GR Riris, H Weaver, CJ Hasselbrack, WE Browell, EV Abshire, JB AF Ramanathan, Anand Mao, Jianping Allan, Graham R. Riris, Haris Weaver, Clark J. Hasselbrack, William E. Browell, Edward V. Abshire, James B. TI Spectroscopic measurements of a CO2 absorption line in an open vertical path using an airborne lidar SO APPLIED PHYSICS LETTERS LA English DT Article ID CARBON-DIOXIDE; MU-M; COLUMN ABSORPTION; INFRARED-SPECTRA; RANGE; SHIFT; DATABASE AB We used an airborne pulsed integrated path differential absorption lidar to make spectroscopic measurements of the pressure-induced line broadening and line center shift of atmospheric carbon dioxide at the 1572.335 nm absorption line. We scanned the lidar wavelength over 13 GHz (110 pm) and measured the absorption lineshape at 30 discrete wavelengths in the vertical column between the aircraft and ground. A comparison of our measured absorption lineshape to calculations based on HIgh-resolution TRANsmission molecular absorption database shows excellent agreement with the peak optical depth accurate to within 0.3%. Additionally, we measure changes in the line center position to within 5.2MHz of calculations and the absorption linewidth to within 0.6% of calculations. These measurements highlight the high precision of our technique, which can be applied to suitable absorption lines of any atmospheric gas. (C) 2013 AIP Publishing LLC. C1 [Ramanathan, Anand; Mao, Jianping; Weaver, Clark J.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Allan, Graham R.; Hasselbrack, William E.] Sigma Space Corp, Lanham, MD 20706 USA. [Riris, Haris; Abshire, James B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Browell, Edward V.] NASA, Langley Res Ctr, STARSS Affiliate 2, Hampton, VA 23681 USA. RP Ramanathan, A (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. EM anand.ramanathan@nasa.gov OI Ramanathan, Anand/0000-0002-1865-0904 FU NASA ESTO IIP-10 program; NASA ASCENDS definition program; NASA Postdoctoral Program FX This work was funded by the NASA ESTO IIP-10 program and the NASA ASCENDS definition program. AR acknowledges extensive support from the NASA Postdoctoral Program. We also thank the AVOCET team of NASA LaRC for providing the in situ CO2 concentration measurements and the NASA DAOF DC-8 team for help conducting the flight campaign. NR 25 TC 4 Z9 4 U1 2 U2 16 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD NOV 18 PY 2013 VL 103 IS 21 AR 214102 DI 10.1063/1.4832616 PG 4 WC Physics, Applied SC Physics GA 260JF UT WOS:000327590400091 ER PT J AU Aasi, J Abadie, J Abbott, BP Abbott, R Abbott, T Abernathy, MR Accadia, T Acernese, F Adams, C Adams, T Adhikari, RX Affeldt, C Agathos, M Aggarwal, N Aguiar, OD Ajith, P Allen, B Allocca, A Ceron, EA Amariutei, D Anderson, RA Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, C Areeda, J Ast, S Aston, SM Astone, P Aufmuth, P Aulbert, C Austin, L Aylott, BE Babak, S Baker, PT Ballardin, G Ballmer, SW Barayoga, JC Barker, D Barnum, SH Barone, F Barr, B Barsotti, L Barsuglia, M Barton, MA Bartos, I Bassiri, R Basti, A Batch, J Bauchrowitz, J Bauer, TS Bebronne, M Behnke, B Bejger, M Beker, MG Bell, AS Bell, C Belopolski, I Bergmann, G Berliner, JM Bertolini, A Bessis, D Betzwieser, J Beyersdorf, PT Bhadbhade, T Bilenko, IA Billingsley, G Birch, J Bitossi, M Bizouard, MA Black, E Blackburn, JK Blackburn, L Blair, D Blom, M Bock, O Bodiya, TP Boer, M Bogan, C Bond, C Bondu, F Bonelli, L Bonnand, R Bork, R Born, M Bose, S Bosi, L Bowers, J Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brannen, CA Brau, JE Breyer, J Briant, T Bridges, DO Brillet, A Brinkmann, M Brisson, V Britzger, M Brooks, AF Brown, DA Brown, DD Brueckner, F Bulik, T Bulten, HJ Buonanno, A Buskulic, D Buy, C Byer, RL Cadonati, L Cagnoli, G Bustillo, JC Calloni, E Camp, JB Campsie, P Cannon, KC Canuel, B Cao, J Capano, CD Carbognani, F Carbone, L Caride, S Castiglia, A Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Cella, G Cepeda, C Cesarini, E Chakraborty, R Chalermsongsak, T Chao, S Charlton, P Chassande-Mottin, E Chen, X Chen, Y Chincarini, A Chiummo, A Cho, HS Chow, J Christensen, N Chu, Q Chua, SSY Chung, S Ciani, G Clara, F Clark, DE Clark, JA Cleva, F Coccia, E Cohadon, PF Colla, A Colombini, M Constancio, M Conte, A Conte, R Cook, D Corbitt, TR Cordier, M Cornish, N Corsi, A Costa, CA Coughlin, MW Coulon, JP Countryman, S Couvares, P Coward, DM Cowart, M Coyne, DC Craig, K Creighton, JDE Creighton, TD Crowder, SG Cumming, A Cunningham, L Cuoco, E Dahl, K Dal Canton, T Damjanic, M Danilishin, SL D'Antonio, S Danzmann, K Dattilo, V Daudert, B Daveloza, H Davier, M Davies, GS Daw, EJ Day, R Dayanga, T De Rosa, R Debreczeni, G Degallaix, J Del Pozzo, W Deleeuw, E Deleglise, S Denker, T Dent, T Dereli, H Dergachev, V DeRosa, R DeSalvo, R Dhurandhar, S Di Fiore, L Di Lieto, A Di Palma, I Di Virgilio, A Diaz, M Dietz, A Dmitry, K Donovan, F Dooley, KL Doravari, S Drago, M Drever, RWP Driggers, JC Du, Z Dumas, JC Dwyer, S Eberle, T Edwards, M Effler, A Ehrens, P Eichholz, J Eikenberry, SS Endroczi, G Essick, R Etzel, T Evans, K Evans, M Evans, T Factourovich, M Fafone, V Fairhurst, S Fang, Q Farr, B Farr, W Favata, M Fazi, D Fehrmann, H Feldbaum, D Ferrante, I Ferrini, F Fidecaro, F Finn, LS Fiori, I Fisher, R Flaminio, R Foley, E Foley, S Forsi, E Forte, LA Fotopoulos, N Fournier, JD Franco, S Frasca, S Frasconi, F Frede, M Frei, M Frei, Z Freise, A Frey, R Fricke, TT Fritschel, P Frolov, VV Fujimoto, MK Fulda, P Fyffe, M Gair, J Gammaitoni, L Garcia, J Garufi, F Gehrels, N Gemme, G Genin, E Gennai, A Gergely, L Ghosh, S Giaime, JA Giampanis, S Giardina, KD Giazotto, A Gil-Casanova, S Gill, C Gleason, J Goetz, E Goetz, R Gondan, L Gonzalez, G Gordon, N Gorodetsky, ML Gossan, S Gossler, S Gouaty, R Graef, C Graff, PB Granata, M Grant, A Gras, S Gray, C Greenhalgh, RJS Gretarsson, AM Griffo, C Grote, H Grover, K Grunewald, S Guidi, GM Guido, C Gushwa, KE Gustafson, EK Gustafson, R Hall, B Hall, E Hammer, D Hammond, G Hanke, M Hanks, J Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Hartman, MT Haughian, K Hayama, K Heefner, J Heidmann, A Heintze, M Heitmann, H Hello, P Hemming, G Hendry, M Heng, IS Heptonstall, AW Heurs, M Hild, S Hoak, D Hodge, KA Holt, K Holtrop, M Hong, T Hooper, S Horrom, T Hosken, DJ Hough, J Howell, EJ Hu, Y Hua, Z Huang, V Huerta, EA Hughey, B Husa, S Huttner, SH Huynh, M Huynh-Dinh, T Iafrate, J Ingram, DR Inta, R Isogai, T Ivanov, A Iyer, BR Izumi, K Jacobson, M James, E Jang, H Jang, YJ Jaranowski, P Jimenez-Forteza, F Johnson, WW Jones, D Jones, DI Jones, R Jonker, RJG Ju, L Haris, K Kalmus, P Kalogera, V Kandhasamy, S Kang, G Kanner, JB Kasprzack, M Kasturi, R Katsavounidis, E Katzman, W Kaufer, H Kaufman, K Kawabe, K Kawamura, S Kawazoe, F Kefelian, F Keitel, D Kelley, DB Kells, W Keppel, DG Khalaidovski, A Khalili, FY Khazanov, EA Kim, BK Kim, C Kim, K Kim, N Kim, W Kim, YM King, EJ King, PJ Kinzel, DL Kissel, JS Klimenko, S Kline, J Koehlenbeck, S Kokeyama, K Kondrashov, V Koranda, S Korth, WZ Kowalska, I Kozak, D Kremin, A Kringel, V Krishnan, B Krolak, A Kucharczyk, C Kudla, S Kuehn, G Kumar, A Kumar, P Kumar, R Kurdyumov, R Kwee, P Landry, M Lantz, B Larson, S Lasky, PD Lawrie, C Lazzarini, A Le Roux, A Leaci, P Lebigot, EO Lee, CH Lee, HK Lee, HM Lee, J Lee, J Leonardi, M Leong, JR Leroy, N Letendre, N Levine, B Lewis, JB Lhuillier, V Li, TGF Lin, AC Littenberg, TB Litvine, V Liu, F Liu, H Liu, Y Liu, Z Lloyd, D Lockerbie, NA Lockett, V Lodhia, D Loew, K Logue, J Lombardi, AL Lorenzini, M Loriette, V Lormand, M Losurdo, G Lough, J Luan, J Lubinski, MJ Luck, H Lundgren, AP Macarthur, J Macdonald, E Machenschalk, B MacInnis, M Macleod, DM Magana-Sandoval, F Mageswaran, M Mailand, K Majorana, E Maksimovic, I Malvezzi, V Man, N Manca, GM Mandel, I Mandic, V Mangano, V Mantovani, M Marchesoni, F Marion, F Marka, S Marka, Z Markosyan, A Maros, E Marque, J Martelli, F Martin, IW Martin, RM Martinelli, L Martynov, D Marx, JN Mason, K Masserot, A Massinger, TJ Matichard, F Matone, L Matzner, RA Mavalvala, N May, G Mazumder, N Mazzolo, G McCarthy, R McClelland, DE McGuire, SC McIntyre, G McIver, J Meacher, D Meadors, GD Mehmet, M Meidam, J Meier, T Melatos, A Mendell, G Mercer, RA Meshkov, S Messenger, C Meyer, MS Miao, H Michel, C Mikhailov, EE Milano, L Miller, J Minenkov, Y Mingarelli, CMF Mitra, S Mitrofanov, VP Mitselmakher, 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CA LIGO Sci Collaboration Virgo Collaboration TI Directed search for continuous gravitational waves from the Galactic center SO PHYSICAL REVIEW D LA English DT Article ID SAGITTARIUS-A-ASTERISK; SPIN-DOWN LIMIT; BLACK-HOLE; RADIO PULSARS; CONSTRAINTS; DISCOVERY; EMISSION; CATALOG; MILKY; MASS AB We present the results of a directed search for continuous gravitational waves from unknown, isolated neutron stars in the Galactic center region, performed on two years of data from LIGO's fifth science run from two LIGO detectors. The search uses a semicoherent approach, analyzing coherently 630 segments, each spanning 11.5 hours, and then incoherently combining the results of the single segments. It covers gravitational wave frequencies in a range from 78 to 496 Hz and a frequency-dependent range of first-order spindown values down to -7.86 x 10(-8) Hz/s at the highest frequency. No gravitational waves were detected. The 90% confidence upper limits on the gravitational wave amplitude of sources at the Galactic center are similar to 3.35 x 10(-25) for frequencies near 150 Hz. These upper limits are the most constraining to date for a large-parameter-space search for continuous gravitational wave signals. C1 [Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Ajith, P.; Anderson, R. A.; Anderson, S. B.; Arai, K.; Araya, M. C.; Austin, L.; Barayoga, J. C.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chakraborty, R.; Chalermsongsak, T.; Coyne, D. C.; Daudert, B.; Dergachev, V.; Driggers, J. C.; Ehrens, P.; Etzel, T.; Fotopoulos, N.; Gushwa, K. E.; Gustafson, E. K.; Hall, E.; Harms, J.; Heefner, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; James, E.; Kalmus, P.; Kells, W.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D.; Lazzarini, A.; Lewis, J. 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RP Behnke, B (reprint author), Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. EM berit.behnke@aei.mpg.de; maria.alessandra.papa@aei.mpg.de RI Ward, Robert/I-8032-2014; Howell, Eric/H-5072-2014; Travasso, Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Cesarini, Elisabetta/C-4507-2017; Costa, Cesar/G-7588-2012; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Aggarwal, Nancy/M-7203-2015; Shaddock, Daniel/A-7534-2011; Vicere, Andrea/J-1742-2012; Rocchi, Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Strain, Kenneth/D-5236-2011; Gehring, Tobias/A-8596-2016; Heidmann, Antoine/G-4295-2016; Zhu, Xingjiang/E-1501-2016; Frasconi, Franco/K-1068-2016; Pinto, Innocenzo/L-3520-2016; Ferrante, Isidoro/F-1017-2012; M, Manjunath/N-4000-2014; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Finn, Lee Samuel/A-3452-2009; Leonardi, Matteo/G-9694-2015; 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Principe, Maria/0000-0002-6327-0628; Matichard, Fabrice/0000-0001-8982-8418; Papa, M.Alessandra/0000-0002-1007-5298; Aulbert, Carsten/0000-0002-1481-8319; Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Guidi, Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431; Pierro, Vincenzo/0000-0002-6020-5521; Jaranowski, Piotr/0000-0001-8085-3414; Prix, Reinhard/0000-0002-3789-6424; Swinkels, Bas/0000-0002-3066-3601; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Whelan, John/0000-0001-5710-6576; Vedovato, Gabriele/0000-0001-7226-1320; Howell, Eric/0000-0001-7891-2817; Travasso, Flavio/0000-0002-4653-6156; Punturo, Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Shaddock, Daniel/0000-0002-6885-3494; Vicere, Andrea/0000-0003-0624-6231; Rocchi, Alessio/0000-0002-1382-9016; Martelli, Filippo/0000-0003-3761-8616; Strain, Kenneth/0000-0002-2066-5355; Gehring, Tobias/0000-0002-4311-2593; Heidmann, Antoine/0000-0002-0784-5175; Zhu, Xingjiang/0000-0001-7049-6468; Frasconi, Franco/0000-0003-4204-6587; Ferrante, Isidoro/0000-0002-0083-7228; M, Manjunath/0000-0001-8710-0730; Vecchio, Alberto/0000-0002-6254-1617; Finn, Lee Samuel/0000-0002-3937-0688; Sigg, Daniel/0000-0003-4606-6526; Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168; Deleglise, Samuel/0000-0002-8680-5170; Neri, Igor/0000-0002-9047-9822; Losurdo, Giovanni/0000-0003-0452-746X; Steinlechner, Sebastian/0000-0003-4710-8548; Danilishin, Stefan/0000-0001-7758-7493; Gammaitoni, Luca/0000-0002-4972-7062; Iyer, Bala R./0000-0002-4141-5179; Lee, Chang-Hwan/0000-0003-3221-1171; McClelland, David/0000-0001-6210-5842; Miao, Haixing/0000-0003-4101-9958; Marchesoni, Fabio/0000-0001-9240-6793; Gemme, Gianluca/0000-0002-1127-7406; Zhao, Chunnong/0000-0001-5825-2401; prodi, giovanni/0000-0001-5256-915X; Gorodetsky, Michael/0000-0002-5159-2742; Bell, Angus/0000-0003-1523-0821 FU Australian Research Council; International Science Linkages program of the Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Foundation for Fundamental Research on Matter; Netherlands Organisation for Scientific Research; Polish Ministry of Science and Higher Education; FOCUS Programme of Foundation for Polish Science; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; OTKA of Hungary; Lyon Institute of Origins (LIO); National Research Foundation of Korea; Industry Canada; Province of Ontario through the Ministry of Economic Development and Innovation; National Science and Engineering Research Council Canada; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P. Sloan Foundation FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, OTKA of Hungary, the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the National Science and Engineering Research Council Canada, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. This document has been assigned LIGO Laboratory Document No. LIGO-P1300037. NR 49 TC 24 Z9 24 U1 5 U2 62 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD NOV 18 PY 2013 VL 88 IS 10 AR 102002 DI 10.1103/PhysRevD.88.102002 PG 13 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 255BD UT WOS:000327213300001 ER PT J AU Papa, F Frappart, F Guntner, A Prigent, C Aires, F Getirana, ACV Maurer, R AF Papa, Fabrice Frappart, Frederic Guentner, Andreas Prigent, Catherine Aires, Filipe Getirana, Augusto C. V. Maurer, Raffael TI Surface freshwater storage and variability in the Amazon basin from multi-satellite observations, 1993-2007 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SEA-LEVEL; SATELLITE ALTIMETRY; WETLAND DYNAMICS; RIVER DISCHARGES; IN-SITU; GRACE; DROUGHT; DEM; PROJECT; EMISSIVITIES AB The amount of water stored and moving through the surface water bodies of large river basins (river, floodplains, wetlands) plays a major role in the global water and biochemical cycles and is a critical parameter for water resources management. However, the spatiotemporal variations of these freshwater reservoirs are still widely unknown at the global scale. Here, we propose a hypsographic curve approach to estimate surface freshwater storage variations over the Amazon basin combining surface water extent from a multi-satellite-technique with topographic data from the Global Digital Elevation Model (GDEM) from Advance Spaceborne Thermal Emission and Reflection Radiometer (ASTER). Monthly surface water storage variations for 1993-2007 are presented, showing a strong seasonal and interannual variability, and are evaluated against in situ river discharge and precipitation. The basin-scale mean annual amplitude of similar to 1200 km(3) is in the range of previous estimates and contributes to about half of the Gravity Recovery And Climate Experiment (GRACE) total water storage variations. For the first time, we map the surface water volume anomaly during the extreme droughts of 1997 (October-November) and 2005 (September-October) and found that during these dry events the water stored in the river and floodplains of the Amazon basin was, respectively, similar to 230 (similar to 40%) and 210 (similar to 50%) km(3) below the 1993-2007 average. This new 15 year data set of surface water volume represents an unprecedented source of information for future hydrological or climate modeling of the Amazon. It is also a first step toward the development of such database at the global scale. C1 [Papa, Fabrice] IRD, LEGOS, Toulouse, France. [Papa, Fabrice] Indian Inst Sci, IRD IISc Joint Int Lab, IFCWS, Bangalore 560012, Karnataka, India. [Frappart, Frederic] Univ Toulouse, Toulouse, France. [Frappart, Frederic] OMP GET UPS, UPS, Toulouse, France. [Guentner, Andreas] German Res Ctr Geosci, GFZ, Potsdam, Germany. [Prigent, Catherine; Aires, Filipe] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Aires, Filipe] Estellus, Paris, France. [Getirana, Augusto C. V.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Maurer, Raffael] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY USA. RP Papa, F (reprint author), IRD LEGOS, Inst Rech Dev, Toulouse, France. EM fabrice.papa@ird.fr RI Papa, Fabrice/D-3695-2009; Getirana, Augusto/G-4630-2011; Guntner, Andreas/C-9892-2011; IFCWS, LMI/C-5187-2013; Frappart, Frederic/D-2950-2009; OI Papa, Fabrice/0000-0001-6305-6253; Guntner, Andreas/0000-0001-6233-8478; Frappart, Frederic/0000-0002-4661-8274 FU CNES TOSCA; OSTST; NASA's NEWS [NNDX7AO90E] FX This work was supported by the CNES TOSCA and OSTST grants "Variability of terrestrial freshwater storage in the Tropics from multi-satellite observations" managed by S. Cherchali and by NASA's NEWS grant NNDX7AO90E managed by Jared K. Entin. We thank Robert Dickinson and two anonymous reviewers for their constructive comments and suggestions. NR 88 TC 6 Z9 6 U1 0 U2 21 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 16 PY 2013 VL 118 IS 21 BP 11951 EP 11965 DI 10.1002/2013JD020500 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 302NS UT WOS:000330611800004 ER EF