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48 results on '"M. H. Finger"'

1. Magnetar twists: Fermi/Gamma-ray Burst Monitor detection of SGR J1550-5418

Author: Ersin Gogus, A. von Kienlin, C. A. Wilson-Hodge, N. Gehrels, P. M. Woods, E. Ramirez-Ruiz, Anna L. Watts, M. van der Klis, A. J. van der Horst, Yuki Kaneko, M. H. Finger, Chryssa Kouveliotou, Jonathan Granot, Asaf Pe'er, Stefanie Wachter, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, Neutron star, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Soft gamma repeater, Astronomy and Astrophysics, Hot spot (veterinary medicine), Black-body radiation, Emission spectrum, Astrophysics, Gamma-ray burst, Magnetar, Fermi Gamma-ray Space Telescope
Abstract: SGR J1550-5418 (previously known as AXP 1E 1547.0-5408 or PSR J1550-5418) went into three active bursting episodes in 2008 October and in 2009 January and March, emitting hundreds of typical soft gamma repeater bursts in soft gamma rays. The second episode was especially intense, and our untriggered burst search on Fermi/Gamma-ray Burst Monitor (GBM) data (8-1000 keV) revealed similar to 450 bursts emitted over 24 hr during the peak of this activity. Using the GBM data, we identified a similar to 150 s long enhanced persistent emission during 2009 January 22 that exhibited intriguing timing and spectral properties: (1) clear pulsations up to similar to 110 keV at the spin period of the neutron star (P similar to 2.07 s, the fastest of all magnetars); (2) an additional (to a power-law) blackbody component required for the enhanced emission spectra with kT similar to 17 keV; and (3) pulsed fraction that is strongly energy dependent and highest in the 50-74 keV energy band. A total isotropic-equivalent energy emitted during this enhanced emission is estimated to be 2.9x10(40)(D/5 kpc)(2) erg. The estimated area of the blackbody emitting region of approximate to 0.046(D/5 kpc)(2) km(2) (roughly a few x 10(-5) of the neutron star area) is the smallest "hot spot" ever measured for a magnetar and most likely corresponds to the size of magnetically confined plasma near the neutron star surface.
Published: 2010

2. NEW TORQUE REVERSAL AND SPIN-UP OF 4U 1626-67 OBSERVED BYFERMI/GAMMA-RAY BURST MONITOR ANDSWIFT/BURST ALERT TELESCOPE

Author: M. H. Finger, E. Beklen, A. Camero-Arranz, N. R. Ikhsanov, and C. A. Wilson-Hodge
Subjects: Physics, Pulsar, Space and Planetary Science, Hardness ratio, Astrophysics::High Energy Astrophysical Phenomena, Flux, Torque, Astronomy and Astrophysics, Astrophysics, Spin-up, Fermi Gamma-ray Space Telescope
Abstract: After about 18 yr of steadily spinning down, the accretion-powered pulsar 4U 1626-67 experienced a new torque reversal at the beginning of 2008. For the present study, we have used all available Fermi/Gamma-ray Burst Monitor data since its launch in 2008 June 11 and over 5 yr of hard X-ray Swift/Burst Alert Telescope observations (starting from 2004 October up to the present time). From 2004 up to the end of 2007 the spin-down rate averaged at a mean rate of similar to(nu) over dot = -4.8 x 10(-13) Hz s(-1) until the torque reversal reported here. This second detected torque reversal was centered near MJD 54500 (2008 February 4) and it lasted approximately 150 days. During the reversal, the source also underwent an increase in flux by a fraction of similar to 2.5. Since then it has been following a steady spin-up at a mean rate of similar to (nu) over dot = 4 x 10(-13) Hz s(-1). We present a detailed long-term timing analysis of this source and a long-term spectral hardness ratio study in order to see whether there are spectral changes around this new observed torque reversal.
Published: 2009

3. Experiment SPHERE status 2008

Author: M. Sonsky, E.A. Bronvech, Dmitry Chernov, V. I. Galkin, W. Tkaczyk, T. I. Sysoeva, S. B. Shaulov, N. V. Kabanova, A.M. Anyuhina, S. P. Besshapov, M. H. Finger, and R.A. Antonov
Subjects: Nuclear and High Energy Physics, Geography, Meteorology, Stage (hydrology), Snow, Atomic and Molecular Physics, and Optics
Abstract: The expedition carried out in March, 2008 to Lake Baikal became an important stage in the development of the SPHERE experiment. During the expedition the SPHERE-2 installation was hoisted, for the first time, on a tethered balloon, APA, to a height of 700 m over the lake surface covered with ice and snow. A series of test measurements were made. Preliminary results of the data processing are presented. The next plan of the SPHERE experiment is to begin a set of statistics for constructing the CR spectrum in the energy range 10 16 – 10 18 eV .
Published: 2009

4. Experiment SPHERE status – 2006 and CR composition determination by means of Cherenkov light LDF

Author: D.A. Pushkarev, M. Sonsky, Dmitry Chernov, A.A. Lubnin, A.M. Anyuhina, F.O. Shihaliev, R.A. Antonov, M. H. Finger, E.A. Bronvech, W. Tkaczyk, T. I. Sysoeva, V. I. Galkin, and S. B. Shaulov
Subjects: Surface (mathematics), Physics, Nuclear and High Energy Physics, Range (particle radiation), SIMPLE (dark matter experiment), business.industry, Detector, Curved mirror, Cosmic ray, Snow, Atomic and Molecular Physics, and Optics, Optics, business, Cherenkov radiation
Abstract: The modern status of the SPHERE experiment and the method to determine the primary energy and the kind of the primary nuclear particles is presented. The SPHERE experiment is based on A.E.Chudakov's suggestion to use a new method for investigating the ultra high energy primary cosmic ray energy spectrum [A.E. Chudakov, Trudy conf. po cosm. lutcham, (in Russian), p.69, Yakutsk, 1972]. A small device lifted above the snow surface of the Earth detects the Cherenkov light of extensive air showers reflected from the surface. The relatively simple detector SPHERE-2 (spherical mirror 1.5m diameter and retina of 100 pixels) is presented. The next plan of the SPHERE experiment is to start measurements of the cosmic ray spectrum in the energy range 10 16 – 10 18 eV above the snow surface of Lake Baikal.
Published: 2008

5. Antarctic balloon-borne detector of high-energy cosmic rays (SPHERE project)

Author: W. Tkaczyk, Dmitry Chernov, L. A. Kuzmichev, T. I. Sysoeva, S. P. Chernikov, O. A. Maksimuk, M. I. Panasyuk, M. H. Finger, S. A. Slavatinsky, S. B. Shaulov, E. E. Korosteleva, R.A. Antonov, and M. Sonsky
Subjects: Physics, Radiation, Air shower, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Curved mirror, Astronomy, Satellite, Cosmic ray, Ultra-high-energy cosmic ray, Cherenkov radiation, Starlight
Abstract: The experiment SPHERE is based on a A.E. Chudakov's suggestion to use a new method for investigations of the energy spectrum of ultrahigh-energy primary cosmic rays. A small device lifted up off a snowed surface of the Earth detects Cherenkov light of an extensive air shower that is reflected from the surface. A contemporary status of the experiment SPHERE, a description of the method, the first measurements of the background night starlight in the region of the Russian Antarctic station Novolazarevskaya are presented. A relatively simple detector SPHERE-2 including a spherical mirror of the diameter 1.5 m and a 100-pixel retina is developed for Antarctic balloon-borne measurements of the cosmic ray spectrum. A long-time winter flight makes it possible to measure the spectrum above 10 20 eV . A comparison with satellite and ISS projects of the nearest future shows that efficiency of this detector is sufficiently high.
Published: 2006

6. Chandra observations of the peculiar X-ray transient IGR J16358-4726

Author: Andrew J. King, P. M. Woods, Chryssa Kouveliotou, Allyn F. Tennant, S. K. Patel, M. H. Finger, P. Ubertini, T. J. L. Courvoisier, C. Winkler, M. van der Klis, and Stefanie Wachter
Subjects: Physics, Nuclear and High Energy Physics, X-ray transient, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Orbital period, Atomic and Molecular Physics, and Optics, Spectral line, Luminosity, Neutron star, Pulsar, Low Mass
Abstract: The new transient IGR J16358-4726 was discovered on 2003 March 19 with INTEGRAL. We detected the source serendipitously during our 2003 March 24 observation of SGR 1627 – 41 with the CHANDRA X-ray Observatory at the 1.7 × 10−10 ergs s−1 cm−2 flux level (2–10 keV) with a very high absorption column (NH=3.3×1023 cm−2) and a hard power law spectrum of photon index 0.5(1). We discovered a very strong flux modulation with a period of 5880(50) s and peak-to-peak pulse fraction of 70(6) % (2–10 keV), clearly visible in the x-ray data. The nature, however, of IGR 16357-4726 remains unresolved. Most likely, we are looking at a galactic binary neutron star system as evidenced by the detection of rest frame fluorescence line emission from neutral Fe K (6.4 keV) in the Chandra spectrum. If the detected modulation is a spin period, this transient is a new kind of object, belonging to a class of very hard transients recently revealed with the unique INTEGRAL capabilities. The only neutron star systems known with similar spin periods are low luminosity persistent wind-fed pulsars, which exhibit very soft X-ray spectra. If this is an orbital period, then the system could be a compact Low Mass X-ray Binary.
Published: 2004

7. A Comprehensive Study of Pulse Profile Evolution in SGR 1806-20 and SGR 1900+14 with the Rossi X-Ray Timing Explorer Proportional Counter Array

Author: Christopher Thompson, Ersin Gogus, N. Frank Six, Chryssa Kouveliotou, M. H. Finger, P. M. Woods, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, Unsteady flow, Space and Planetary Science, Gamma ray, Proportional counter, Astronomy and Astrophysics, Astrophysics, Pulse (physics)
Abstract: Soft Gamma Repeaters undergo pulse profile changes in connection with the burst activity. Here we construct a comprehensive pulse profile history of SGR 1806-20 and SGR 1900+14 in different energy bands using Rossi X-ray Timing Explorer/Proportional Counter Array observations. We quantify the pulse profile evolution using the Fourier harmonic powers of profiles. Moreover, we determined the RMS pulsed count rates (PCRs) of each profile. We show that the pulse profiles SGR 1806$-$20 remain as single pulsed while those of SGR 1900+14 alter remarkable in all energy bands. Highly significant pulsations form SGR 1900+14 following August 27 and April 19 bursts enabled us to study not only decay of PCRs in different energy bands and also their correlations with one another.
Published: 2002

8. The Large Observatory For x-ray Timing

Author: Antonios Manousakis, S. Boutloukos, F. Zwart, Jose M. Torrejon, C. Pittori, Alessandro Drago, Dieter H. Hartmann, Feryal Özel, T. J. L. Courvoisier, Tim Johannsen, Jordi José, M. Michalska, Christian Schmid, I. Rashevskaya, Gottfried Kanbach, V. Petracek, L. Bradley, Allan Hornstrup, M. H. Erkut, Sergio Campana, Rudy Wijnands, Andrew Cumming, Nils Andersson, Tomaso Belloni, M. C. Miller, Roman Wawrzaszek, Stefano Bianchi, Enrique García-Berro, Sandro Mereghetti, C. Guidorzi, C. Corral Van Damme, Søren Brandt, Francesco Tombesi, Felix Ryde, Didier Barret, Simon Vaughan, Marco Feroci, T. Di Salvo, C. van Baren, Angelo Antonelli, Marc Ribó, J. L. Atteia, P. Soleri, Alessio Trois, Silvia Zane, G. Mouret, Ersin Gogus, Emanuele Perinati, J. Coker, Piero Malcovati, V. Mangano, F. Jetter, P. Uter, P. Romano, M. Nowak, Roberto Turolla, Laura Tolos, Antonino D'Ai, Laura Alvarez, C. Amoros, Simone Scaringi, A. Possenti, David M. Smith, M. Falanga, A. Goldwurm, René Hudec, Ignacio Negueruela, M. van der Klis, Francesco Longo, José A. Pons, I. M. McHardy, R. Rohlfs, P. Cais, Luigi Stella, S. Di Cosimo, Antoine Rousseau, M. Ayre, M. Gschwender, D. Klochkov, Niels Lund, Chryssa Kouveliotou, P. Azzarello, F. Château, Michael Gabler, S. Vercellone, Martin Durant, I. Donnarumma, Giorgio Matt, Mauro Orlandini, P. Kaaret, Patrick Smith, P. T. O'Brien, A. Argan, M. Orienti, Marco Grassi, Claudio Labanti, Edward F. Brown, Christopher S. Reynolds, Gloria Sala, Y. Evangelista, Gabriel Török, José Braga, Riccardo Campana, Alan Smith, C. Gouiffes, Nevin N. Weinberg, Leonardo Gualtieri, Yannick Favre, P.G. Jonker, Gabriele Giovannini, D. de Martino, Irfan Kuvvetli, S. Motta, Teresa Mineo, Paul J. Groot, Pablo Reig, Martino Marisaldi, Andrea Sanna, Lorenzo Amati, G. L. Israel, D. Macera, K. S. Wood, Pablo Cerdá-Durán, F. Fuschino, Suvi Gezari, Mariano Mendez, Slawomir Suchy, Damien Rambaud, Nanda Rea, R. Artigue, J.-Y. Seyler, S. N. Shore, Frederick K. Lamb, Jörn Wilms, Mark G. Alford, Margarita Hernanz, Thomas M. Tauris, Luca Izzo, Tobias Boenke, J. J. M. in 't Zand, J. Mulačová, P. Binko, Daniel Maier, Jan Schee, Bruce Gendre, Enrico Bozzo, Paul S. Ray, Giuseppe Bertuccio, Simone Migliari, Ignazio Bombaci, Vladimir Karas, Nikolaos Stergioulas, P. P. Laubert, D. Karelin, A. C. Fabian, Giovanni Miniutti, Dacheng Lin, L. Guy, Martine Mouchet, Colleen A. Wilson-Hodge, Valeria Ferrari, Kai Hebeler, Mark H. Finger, Shigeto Watanabe, Pawel Haensel, H. Jacobs, Adrian Martindale, A. A. Zdziarski, Andrea Santangelo, Giuseppe Baldazzi, Piergiorgio Casella, Fabio Muleri, M. Hailey, Antonio Bianchini, Giuseppe Lodato, E. Del Monte, M. Rapisarda, Zdeněk Stuchlík, Alain Cros, V. Sochora, Laurens Keek, Jorge Casares, Andrew Melatos, Pere Blay, E. Rossi, A. P. Spencer, G. Stratta, Conrado Albertus, J. M. Paredes, M. Ahangarianabhari, Anna L. Watts, M. Del Santo, I. Kreykenbohm, Alessandro Patruno, G. A. Caliandro, C. Feldman, M. Pohl, Fabrizio Tamburini, G. Zampa, Marina Orio, Flemming Hansen, P. Ramon, Ruben Salvaterra, David H. Lumb, Edward M. Cackett, Andrew Shearer, Sharon M. Morsink, L. Pacciani, J.-M. Bonnet Bidaud, A. De Luca, Jérôme Chenevez, Sebastian Diebold, N. Zampa, Carole A. Haswell, Luciano Burderi, E. Cavazzuti, Adam Ingram, Dhiren Kataria, Berend Winter, A. Vacchi, W. Hermsen, P. Giommi, Dong Lai, N. A. Webb, P. Bodin, Dom Walton, Solen Balman, Benjamin Stappers, M. Burgay, Luca Zampieri, Carl Budtz-Jørgensen, Ralph A. M. J. Wijers, Giancarlo Cusumano, J. L. Galvez Sanchez, Raffaella Schneider, Luciano Rezzolla, Alexander Heger, S. Korpela, Dimitrios Emmanoulopoulos, Biswajit Paul, Diego Götz, B. Artigues, Paolo Soffitta, M. H. Finger, J. W. den Herder, Paolo Esposito, Kazushi Iwasawa, Poul Erik Holmdahl Olsen, J. Neilsen, Marco Barbera, Deepto Chakrabarty, R. A. Osten, M. Reina Aranda, A. J. Castro-Tirado, Andrea Tramacere, D. Haas, Johannes Dercksen, John A. Tomsick, A. V. Penacchioni, V. D'Elia, Alfonso Collura, Altan Baykal, P. Le Provost, S. Turriziani, Kostas D. Kokkotas, Duncan K. Galloway, Ron Remillard, Juhani Huovelin, Somak Bhattacharyya, Pavel Bakala, Phil Uttley, Richard E. Cole, Mahesh Prakash, L. Kuiper, T. Munoz-Darias, Diego F. Torres, S. Mahmoodifar, G. Ramsay, Andrew Norton, T. Kennedy, Achim Schwenk, L. Zdunik, A. B. Giles, Jerome Rodriguez, C. Motch, Ilya Mandel, Marcello Giroletti, Dimitrios Psaltis, J. Sandberg, Fiamma Capitanio, Remon Cornelisse, M. R. Gilfanov, Peggy Varniere, Franck Cadoux, Peter J. Wheatley, M. de Pasquale, Juri Poutanen, S. Maestre, A. Pellizzoni, Axel Schwope, Diego Altamirano, Piotr Orleanski, V. Vrba, Agata Różańska, Kateřina Goluchová, P. Rodríguez Gil, Niccolò Bucciantini, Stéphane Schanne, Carlo Ferrigno, Thomas J. Maccarone, H. Wende, Tod E. Strohmayer, Tadayuki Takahashi, Francois Lebrun, E. Kuulkers, Jeroen Homan, Maurizio Paolillo, M. A. Perez, J. P. Osborne, A. Alpar, Sanjay Reddy, G.W. Fraser, V. Sulemainov, D. Linder, L. Sabau-Graziati, A. Rachevski, Bing Zhang, Alessandro Papitto, C. Tenzer, Alex Markowitz, J. Portell, Roberto Mignani, Fabrizio Bocchino, Arnau Rios, R. de la Rie, M. Wille, A. de Rosa, Alessandro Riggio, M. Frericks, Andrew W. Steiner, Michal Bursa, Federico Bernardini, Jon M. Miller, W. Kluzniak, INAF - Osservatorio Astronomico di Roma ( OAR ), Istituto Nazionale di Astrofisica ( INAF ), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées ( LATT ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Variable Energy Cyclotron Centre, Institut Pasteur de Montevideo, Réseau International des Instituts Pasteur ( RIIP ) -Institut Pasteur de Montevideo, Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), FORMATION STELLAIRE 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux ( L3AB ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Interactions et dynamique des environnements de surface ( IDES ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Licryl Laboratory ( CNR-IPCF UOS Cosenza ), University of Calabria, Laboratori Nazionali di Frascati ( LNF ), National Institute for Nuclear Physics ( INFN ), PCAS, Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano ( IASF-MI ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Canada's National Laboratory for Particle and Nuclear Physics ( TRIUMF ), NRC, Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] ( UNIBO ), Institut de recherches sur la catalyse et l'environnement de Lyon ( IRCELYON ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Spectrochimie Infrarouge et Raman - UMR 8516 ( LASIR ), Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Dipartimento di Scienze Fisiche [Naples], Università degli studi di Napoli Federico II, Energétique, propulsion, espace, environnement ( EPEE ), Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Physics and Astronomy [Hanover], Dartmouth College [Hanover], Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d’Optique Atmosphérique - UMR 8518 ( LOA ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Institut de Biologie du Développement de Marseille ( IBDM ), Aix Marseille Université ( AMU ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Centre National de la Recherche Scientifique ( CNRS ), Universitat Politècnica de Catalunya [Barcelona] ( UPC ), INAF-IASF Milano, Climate and Environmental Physics [Bern], University of Bern, Centre National d'Etudes Spatiales ( CNES ), Institute of Geology, Eidgenössische Technische Hochschule [Zürich] ( ETH Zürich ), IEEC-CSIC, Universitat Autònoma de Barcelona [Barcelona] ( UAB ), MedisysResearch Lab ( Medisys ), Philips Research, European Space Astronomy Center ( ESAC ), European Space Agency ( ESA ), High Energy Astrophys. & Astropart. Phys (API, FNWI), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Réseau International des Instituts Pasteur (RIIP), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Interactions et dynamique des environnements de surface (IDES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Licryl Laboratory (CNR-IPCF UOS Cosenza), Università della Calabria [Arcavacata di Rende] (Unical), Laboratori Nazionali di Frascati (LNF), Istituto Nazionale di Fisica Nucleare (INFN), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Canada's particle accelerator centre (TRIUMF), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Laboratoire Avancé de Spectroscopie pour les Intéractions la Réactivité et l'Environnement - UMR 8516 (LASIRE), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), University of Naples Federico II = Università degli studi di Napoli Federico II, Energétique, propulsion, espace, environnement (EPEE), Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Laboratoire d’Optique Atmosphérique - UMR 8518 (LOA), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Institut de Biologie du Développement de Marseille (IBDM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Universitat Politècnica de Catalunya [Barcelona] (UPC), Climate and Environmental Physics [Bern] (CEP), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE)-Universität Bern [Bern] (UNIBE), Centre National d'Études Spatiales [Toulouse] (CNES), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Universitat Autònoma de Barcelona (UAB), MedisysResearch Lab (Medisys), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), SPIE, Takahashi, Tadayuki, Feroci M., Den Herder J.W., Bozzo E., Barret D., Brandt S., Hernanz M., Van Der Klis M., Pohl M., Santangelo A., Stella L., Watts A., Wilms J., Zane S., Ahangarianabhari M., Albertus C., Alford M., Alpar A., Altamirano D., Alvarez L., Amati L., Amoros C., Andersson N., Antonelli A., Argan A., Artigue R., Artigues B., Atteia J.-L., Azzarello P., Bakala P., Baldazzi G., Balman S., Barbera M., Van Baren C., Bhattacharyya S., Baykal A., Belloni T., Bernardini F., Bertuccio G., Bianchi S., Bianchini A., Binko P., Blay P., Bocchino F., Bodin P., Bombaci I., Bonnet Bidaud J.-M., Boutloukos S., Bradley L., Braga J., Brown E., Bucciantini N., Burderi L., Burgay M., Bursa M., Budtz-Jorgensen C., Cackett E., Cadoux F.R., Cais P., Caliandro G.A., Campana R., Campana S., Capitanio F., Casares J., Casella P., Castro-Tirado A.J., Cavazzuti E., Cerda-Duran P., Chakrabarty D., Chateau F., Chenevez J., Coker J., Cole R., Collura A., Cornelisse R., Courvoisier T., Cros A., Cumming A., Cusumano G., D'ai A., D'elia V., Del Monte E., De Luca A., De Martino D., Dercksen J.P.C., De Pasquale M., De Rosa A., Del Santo M., Di Cosimo S., Diebold S., Di Salvo T., Donnarumma I., Drago A., Durant M., Emmanoulopoulos D., Erkut M.H., Esposito P., Evangelista Y., Fabian A., Falanga M., Favre Y., Feldman C., Ferrari V., Ferrigno C., Finger M., Finger M.H., Fraser G.W., Frericks M., Fuschino F., Gabler M., Galloway D.K., Galvez Sanchez J.L., Garcia-Berro E., Gendre B., Gezari S., Giles A.B., Gilfanov M., Giommi P., Giovannini G., Giroletti M., Gogus E., Goldwurm A., Goluchova K., Gotz D., Gouiffes C., Grassi M., Groot P., Gschwender M., Gualtieri L., Guidorzi C., Guy L., Haas D., Haensel P., Hailey M., Hansen F., Hartmann D.H., Haswell C.A., Hebeler K., Heger A., Hermsen W., Homan J., Hornstrup A., Hudec R., Huovelin J., Ingram A., In't Zand J.J.M., Israel G., Iwasawa K., Izzo L., Jacobs H.M., Jetter F., Johannsen T., Jonker P., Jose J., Kaaret P., Kanbach G., Karas V., Karelin D., Kataria D., Keek L., Kennedy T., Klochkov D., Kluzniak W., Kokkotas K., Korpela S., Kouveliotou C., Kreykenbohm I., Kuiper L.M., Kuvvetli I., Labanti C., Lai D., Lamb F.K., Laubert P.P., Lebrun F., Lin D., Linder D., Lodato G., Longo F., Lund N., Maccarone T.J., Macera D., Maestre S., Mahmoodifar S., Maier D., Malcovati P., Mandel I., Mangano V., Manousakis A., Marisaldi M., Markowitz A., Martindale A., Matt G., Mchardy I.M., Melatos A., Mendez M., Mereghetti S., Michalska M., Migliari S., Mignani R., Miller M.C., Miller J.M., Mineo T., Miniutti G., Morsink S., Motch C., Motta S., Mouchet M., Mouret G., Mulaova J., Muleri F., Munoz-Darias T., Negueruela I., Neilsen J., Norton A.J., Nowak M., O'brien P., Olsen P.E.H., Orienti M., Orio M., Orlandini M., Orleaaski P., Osborne J.P., Osten R., Ozel F., Pacciani L., Paolillo M., Papitto A., Paredes J.M., Patruno A., Paul B., Perinati E., Pellizzoni A., Penacchioni A.V., Perez M.A., Petracek V., Pittori C., Pons J., Portell J., Possenti A., Poutanen J., Prakash M., Le Provost P., Psaltis D., Rambaud D., Ramon P., Ramsay G., Rapisarda M., Rachevski A., Rashevskaya I., Ray P.S., Rea N., Reddy S., Reig P., Reina Aranda M., Remillard R., Reynolds C., Rezzolla L., Ribo M., De La Rie R., Riggio A., Rios A., Rodriguez-Gil P., Rodriguez J., Rohlfs R., Romano P., Rossi E.M.R., Rozanska A., Rousseau A., Ryde F., Sabau-Graziati L., Sala G., Salvaterra R., Sanna A., Sandberg J., Scaringi S., Schanne S., Schee J., Schmid C., Shore S., Schneider R., Schwenk A., Schwope A.D., Seyler J.-Y., Shearer A., Smith A., Smith D.M., Smith P.J., Sochora V., Soffitta P., Soleri P., Spencer A., Stappers B., Steiner A.W., Stergioulas N., Stratta G., Strohmayer T.E., Stuchlik Z., Suchy S., Sulemainov V., Takahashi T., Tamburini F., Tauris T., Tenzer C., Tolos L., Tombesi F., Tomsick J., Torok G., Torrejon J.M., Torres D.F., Tramacere A., Trois A., Turolla R., Turriziani S., Uter P., Uttley P., Vacchi A., Varniere P., Vaughan S., Vercellone S., Vrba V., Walton D., Watanabe S., Wawrzaszek R., Webb N., Weinberg N., Wende H., Wheatley P., Wijers R., Wijnands R., Wille M., Wilson-Hodge C.A., Winter B., Wood K., Zampa G., Zampa N., Zampieri L., Zdunik L., Zdziarski A., Zhang B., Zwart F., Ayre M., Boenke T., Corral Van Damme C., Kuulkers E., Lumb D., Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Universität Bern [Bern]-Universität Bern [Bern], European Space Agency (ESA), Feroci, M., den Herder, J., Bozzo, E., Barret, D., Brandt, S., Hernanz, M., van der Klis, M., Pohl, M., Santangelo, A., Stella, L., Watts, A., Wilms, J., Zane, S., Ahangarianabhari, M., Albertus, C., Alford, M., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, N., Antonelli, A., Argan, A., Artigue, R., Artigues, B., Atteia, J., Azzarello, P., Bakala, P., Baldazzi, G., Balman, S., Barbera, M., van Baren, C., Bhattacharyya, S., Baykal, A., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bodin, P., Bombaci, I., Bonnet Bidaud, J., Boutloukos, S., Bradley, L., Braga, J., Brown, E., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz Jørgensen, C., Cackett, E., Cadoux, F., Caïs, P., Caliandro, G., Campana, R., Campana, S., Capitanio, F., Casares, J., Casella, P., Castro Tirado, A., Cavazzuti, E., Cerda Duran, P., Chakrabarty, D., Château, F., Chenevez, J., Coker, J., Cole, R., Collura, A., Cornelisse, R., Courvoisier, T., Cros, A., Cumming, A., Cusumano, G., D'Ai', A., D'Elia, V., Del Monte, E., de Luca, A., de Martino, D., Dercksen, J., de Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Diebold, S., DI SALVO, T., Donnarumma, I., Drago, A., Durant, M., Emmanoulopoulos, D., Erkut, M., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Ferrari, V., Ferrigno, C., Finger, M., Fraser, G., Frericks, M., Fuschino, F., Gabler, M., Galloway, D., Galvez Sanchez, J., Garcia Berro, E., Gendre, B., Gezari, S., Giles, A., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gouiffes, C., Grassi, M., Groot, P., Gschwender, M., Gualtieri, L., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hansen, F., Hartmann, D., Haswell, C., Hebeler, K., Heger, A., Hermsen, W., Homan, J., Hornstrup, A., Hudec, R., Huovelin, J., Ingram, A., In't Zand, J., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H., Jetter, F., Johannsen, T., Jonker, P., Josè, J., Kaaret, P., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Kokkotas, K., Korpela, S., Kouveliotou, C., Kreykenbohm, I., Kuiper, L., Kuvvetli, I., Labanti, C., Lai, D., Lamb, F., Laubert, P., Lebrun, F., Lin, D., Linder, D., Lodato, G., Longo, F., Lund, N., Maccarone, T., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Mandel, I., Mangano, V., Manousakis, A., Marisaldi, M., Markowitz, A., Martindale, A., Matt, G., Mchardy, I., Melatos, A., Mendez, M., Mereghetti, S., Michalska, M., Migliari, S., Mignani, R., Miller, M., Miller, J., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Mouret, G., Mulačová, J., Muleri, F., Muñoz Darias, T., Negueruela, I., Neilsen, J., Norton, A., Nowak, M., O'Brien, P., Olsen, P., Orienti, M., Orio, M., Orlandini, M., Orleański, P., Osborne, J., Osten, R., Ozel, F., Pacciani, L., Paolillo, M., Papitto, A., Paredes, J., Patruno, A., Paul, B., Perinati, E., Pellizzoni, A., Penacchioni, A., Perez, M., Petracek, V., Pittori, C., Pons, J., Portell, J., Possenti, A., Poutanen, J., Prakash, M., Le Provost, P., Psaltis, D., Rambaud, D., Ramon, P., Ramsay, G., Rapisarda, M., Rachevski, A., Rashevskaya, I., Ray, P., Rea, N., Reddy, S., Reig, P., Reina Aranda, M., Remillard, R., Reynolds, C., Rezzolla, L., Ribo, M., de la Rie, R., Riggio, A., Rios, A., Rodríguez Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E., Rozanska, A., Rousseau, A., Ryde, F., Sabau Graziati, L., Sala, G., Salvaterra, R., Sanna, A., Sandberg, J., Scaringi, S., Schanne, S., Schee, J., Schmid, C., Shore, S., Schneider, R., Schwenk, A., Schwope, A., Seyler, J., Shearer, A., Smith, A., Smith, D., Smith, P., Sochora, V., Soffitta, P., Soleri, P., Spencer, A., Stappers, B., Steiner, A., Stergioulas, N., Stratta, G., Strohmayer, T., Stuchlik, Z., Suchy, S., Sulemainov, V., Takahashi, T., Tamburini, F., Tauris, T., Tenzer, C., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J., Torres, D., Tramacere, A., Trois, A., Turolla, R., Turriziani, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vrba, V., Walton, D., Watanabe, S., Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, M., Wilson Hodge, C., Winter, B., Wood, K., Zampa, G., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zhang, B., Zwart, F., Ayre, M., Boenke, T., Corral van Damme, C., Kuulkers, E., Lumb, D., Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), National Institute for Nuclear Physics (INFN), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Canada's National Laboratory for Particle and Nuclear Physics (TRIUMF), Università di Bologna [Bologna] (UNIBO), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Spectrochimie Infrarouge et Raman - UMR 8516 (LASIR), Centre National de la Recherche Scientifique (CNRS)-Université de Lille, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Lille, Aix Marseille Université (AMU)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Universitat Autònoma de Barcelona [Barcelona] (UAB), Astronomy, den Herder, J. W., Atteia, J. L., Bonnet Bidaud, J. M., Cadoux, F. R., Cais, P., Caliandro, G. A., Castro Tirado, A. J., D'Aì, A., De Luca, A., De Martino, D., Dercksen, J. P. C., De Pasquale, M., Di Salvo, T., Erkut, M. H., Finger, M. H., Fraser, G. W., Galloway, D. K., Galvez Sanchez, J. L., Giles, A. B., Hartmann, D. H., Haswell, C. A., in't Zand, J. J. M., Jacobs, H. M., Kuiper, L. M., Lamb, F. K., Laubert, P. P., Maccarone, T. J., Mchardy, I. M., Miller, M. C., Miller, J. M., Norton, A. J., Olsen, P. E. H., Orleanski, P., Osborne, J. P., Paolillo, Maurizio, Paredes, J. M., Penacchioni, A. V., Perez, M. A., Ray, P. S., Rossi, E. M. R., Schwope, A. D., Seyler, J. Y., Smith, D. M., Smith, P. J., Steiner, A. W., Strohmayer, T. E., Torrejon, J. M., Torres, D. F., and Wilson Hodge, C. A.
Subjects: x-ray and γ-ray instrumentation, compact objects, microchannel plates, X-ray detectors, X-ray imaging, X-ray spectroscopy, X-ray timing, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Applied Mathematics, Electrical and Electronic Engineering, Vision, Observatories, Field of view, 01 natural sciences, 7. Clean energy, neutron stars, Observatory, 010303 astronomy & astrophysics, Physics, Equipment and services, Astrophysics::Instrumentation and Methods for Astrophysics, Steradian, [ SDU.ASTR.IM ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics - Instrumentation and Methods for Astrophysics, X-ray detector, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cosmic Vision, Spectral resolution, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, NO, microchannel plate, Settore FIS/05 - Astronomia e Astrofisica, X-rays, compact object, 0103 physical sciences, Electronic, Optical and Magnetic Materials, Instrumentation and Methods for Astrophysics (astro-ph.IM), dense hadronic matter, Sensors, 010308 nuclear & particles physics, Astronomy, Accretion (astrophysics), [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Neutron star, 13. Climate action, [ PHYS.ASTR.IM ] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Gamma-ray burst, astro-ph.IM
Abstract: The Large Observatory For x-ray Timing (LOFT) was studied within ESA M3 Cosmic Vision framework and participated in the final down-selection for a launch slot in 2022-2024. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument, LOFT will study the behaviour of matter under extreme conditions, such as the strong gravitational field in the innermost regions of accretion flows close to black holes and neutron stars, and the supra-nuclear densities in the interior of neutron stars. The science payload is based on a Large Area Detector (LAD, 10 m 2 effective area, 2-30 keV, 240 eV spectral resolution, 1 deg collimated field of view) and a WideField Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g. GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the status of the mission at the end of its Phase A study., Proc. SPIE 9144, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 91442T
Published: 2014

9. [ITAL]Chandra[/ITAL] Observations of the Anomalous X-Ray Pulsar 1E 2259+586

Author: M. H. Finger, E. Goguse, T. M. Belloni, P. M. Woods, Martin C. Weisskopf, S. K. Patel, Chryssa Kouveliotou, Allyn F. Tennant, and M. van der Klis
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics, Spectral line, Anomalous X-ray pulsar, Interstellar medium, Pulsar, Space and Planetary Science, Observatory, Black-body radiation, Spectroscopy, Supernova remnant, Astrophysics::Galaxy Astrophysics
Abstract: We present X-ray imaging, timing, and phase resolved spectroscopy of the anomalous X-ray pulsar 1E 2259+58.6 using the Chandra X-ray Observatory. The spectrum is well described by a power law plus blackbody model with power law index = 3.6(1), kT_BB = 0.412(6) keV, and N_H=0.93(3) x 10^{22} cm^{-2}; we find no evidence for spectral features (0.5-7.0 keV). We derive a new, precise X-ray position for the source and determine its spin period, P=6.978977(24) s. Time resolved X-ray spectra show no significant variation as a function of pulse phase. We have detected excess emission beyond 4 arcsec from the central source extending to beyond 100 arcsec, due to the supernova remnant and possibly dust scattering from the interstellar medium.
Published: 2001

10. Results on the primary CR spectrum and composition reconstructed with the SPHERE-2 detector

Author: N. V. Kabanova, M. H. Finger, R.A. Antonov, Dmitry Chernov, E. A. Bonvech, Timur Dzhatdoev, A. S. Petkun, T. I. Sysoeva, V. I. Galkin, S. B. Shaulov, T. M. Roganova, M. Finger, D. A. Podgrudkov, and S. P. Beschapov
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), History, Range (particle radiation), Spectrum (functional analysis), Detector, FOS: Physical sciences, Cosmic ray, Radiation, Snow, Computer Science Applications, Education, Computational physics, Distribution function, Primary (astronomy), Astrophysics - High Energy Astrophysical Phenomena
Abstract: First preliminary results of the balloon-borne experiment SPHERE-2 on the all-nuclei primary cosmic rays (PCR) spectrum and primary composition are presented. The primary spectrum in the energy range $10^{16}$--$5\cdot10^{17}$ eV was reconstructed using characteristics of Vavilov-Cherenkov radiation of extensive air showers (EAS), reflected from a snow surface. Several sources of systematic uncertainties of the spectrum were analysed. A method for separation of the primary nuclei' groups based on the lateral distribution function' (LDF) steepness parameter is presented. Preliminary estimate of the mean light nuclei' fraction $f_{30-150}$ at energies $3\cdot10^{16}$--$1.5\cdot10^{17}$ eV was performed and yielded $f_{30-150}$= (21$\pm$11)%., Comment: 4 pages, 2 figures, Proc. 23rd European Cosmic Ray Symposium, to appear in J. Phys. Conf. Ser
Published: 2012
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11. A maskless gamma-ray all-sky imager: BATSE/CGRO

Author: W. S. Paciesas, M. H. Finger, C. A. Meegan, Brad C. Rubin, B. A. Harmon, R. B. Wilson, Gerald J. Fishman, and Shuang-Nan Zhang
Subjects: Physics, Nuclear and High Energy Physics, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Gamma ray, X-ray detector, Astronomy, Gamma-ray astronomy, Astrophysics, Particle detector, Nuclear Energy and Engineering, Pulsar, Observatory, Sky, Astrophysics::Earth and Planetary Astrophysics, Electrical and Electronic Engineering, Gamma-ray burst, media_common
Abstract: The non-collimated detectors of BATSE (Burst And Transient Source Experiment) on the Compton Gamma Ray Observatory (CGRO) can be used as a high sensitivity hard X-ray and low energy gamma-ray all-sky imager in the energy range between 20 keV and 2 MeV. The fluxes from sources in the sky are modulated as the spacecraft orbits the Earth. The CGRO orbital precession further allows sampling of the sky in strips corresponding to the limb of the Earth at any given time. The modulation data are transformed into images by various reconstruction methods. High sensitivity images of location accuracy of about 0.1/spl deg/ and source separation of about 1/spl deg/ are obtained. >
Published: 1994

12. New Timing Results of the X-ray Binary Pulsar OAO 1657-415

Author: P. A. Jenke, M. H. Finger, C. A. Wilson-Hodge, A. Camero-Arranz, Ersin Göğüş, Ünal Ertan, and Tomaso Belloni
Subjects: Physics, Pulsar, Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, Astronomy, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Timing results, Ephemeris, Gamma-ray burst, Orbital decay, Binary pulsar
Abstract: OAO 1657‐415 is an eclipsing X‐ray binary pulsar that has undergone several torque reversals throughout its long history of observation. We present a frequency history spanning nearly 19 years of observations from the Burst and Transient Source Experiment (BATSE) and from the Gamma‐Ray Burst Monitor (GBM). Orbital ephemerides of the pulsar system is obtained at several intervals throughout this history. With these ephemerides, statistically significant orbital decay is established.
Published: 2011

13. A 0535+26: an X-ray∕Optical Tour

Author: A. Camero-Arranz, M. H. Finger, C. A. Wilson-Hodge, P. Jenke, M. J. Coe, I. Steele, I. Caballero, J. Gutierrez-Soto, P. Kretschmar, J. Suso, V. A. McBride, J. Rodríguez, Ersin Göğüş, Ünal Ertan, and Tomaso Belloni
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, FOS: Physical sciences, Binary number, Astrophysics, Accretion (astrophysics), Neutron star, Pulsar, Observatory, Binary system, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract: We compiled X-ray and Optical observations of the accreting X-ray binary system A 0535+262 since its discovery in 1975, that will allow us to shed light on the unpredictable behavior of this binary system. We present the data in terms of the Be-disk interaction with the neutron star companion. In addition, we show recent results from the continuous monitoring of this source by the Gamma-ray Burst Monitor(GBM), on board the Fermi observatory, since its launch in 2008 June 11., Comment: 4 pages, 5 figures, Conference proceeding of "Astrophysics of Neutron Stars 2010 - a conference in honor of M. Ali Alpar", 2-6 August 2010, Cesme, Izmir, Turkey
Published: 2011

14. Spectral and Temporal Monitoring of the Isolated Neutron Star RX J1308.6+2127 with XMM-Newton

Author: C. Airhart, P. M. Woods, V. E. Zavlin, M. H. Finger, M. H. van Kerkwijk, D. L. Kaplan, C. Kouveliotou, G. G. Pavlov, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi
Subjects: Physics, Neutron star, Pulsar, Astrophysics::High Energy Astrophysical Phenomena, Monitoring data, Energy spectrum, Spectral properties, Pulse frequency, Astronomy, Black-body radiation, Astrophysics, Magnetar
Abstract: The isolated neutron star (INS) RX J1308.6+2127 has been observed with Chandra and XMM‐Newton several times between 2000 and 2007. The six most recent XMM‐Newton observations are part of a monitoring campaign we initiated to study the long‐term temporal and spectral properties of INSs. The primary goal of this investigation is to better quantify the similarities and differences between INSs and magnetar candidates (i.e. Anomalous X‐ray Pulsars and Soft Gamma Repeaters) in terms of their spectral and temporal variability. Here, we present our analysis of the current data set and show that (i) the energy spectrum is well modeled by a blackbody with two absorption lines, (ii) the spectral parameters do not show significant time variability over the last seven years, (iii) the pulse profile is strongly energy dependent, but stationary, and (iv) the pulse frequency evolution is consistent with monotonic spin‐down. Our spectral and temporal results are consistent with earlier analyses by Schwope et al. [8] and Kaplan and van Kerkwijk [5], respectively. The inclusion of the new monitoring data provides more precise constraints on both spectral and temporal parameters of this INS. For isolated neutron stars whose X‐ray emission is not powered by spin‐down (INSs, AXPs and SGRs), RX J1308.6+2127 is among the most stable members.
Published: 2008

15. A 0535+26 in the August/September 2005 outburst observed by RXTE and INTEGRAL

Author: I. Kreykenbohm, D. Klochkov, Jörn Wilms, A. Camero, Andrea Santangelo, Rüdiger Staubert, A. Segreto, Katja Pottschmidt, Slawomir Suchy, Isabel Caballero, Peter Kretschmar, R. E. Rothschild, Colleen A. Wilson, G. Schoenherr, M. H. Finger, Vanessa McBride, and Carlo Ferrigno
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Cyclotron, Cyclotron resonance, Flux, FOS: Physical sciences, Astrophysics, UNESCO::ASTRONOMÍA Y ASTROFÍSICA, Spectral line, law.invention, law, X-rays, Line (formation), Physics, Scattering, Astrophysics (astro-ph), Astronomy and Astrophysics, Individual Star, Stars, ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia [UNESCO], Pulse (physics), binaries, Magnetic fields, A0535+26, Space and Planetary Science, Harmonic, UNESCO::ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia, ASTRONOMÍA Y ASTROFÍSICA [UNESCO]
Abstract: In this Letter we present results from INTEGRAL and RXTE observations of the spectral and timing behavior of the High Mass X-ray Binary A 0535+26 during its August/September 2005 normal (type I) outburst with an average flux F(5-100keV)~400mCrab. The search for cyclotron resonance scattering features (fundamental and harmonic) is one major focus of the paper. Our analysis is based on data from INTEGRAL and RXTE Target of Opportunity Observations performed during the outburst. The pulse period is determined. X-ray pulse profiles in different energy ranges are analyzed. The broad band INTEGRAL and RXTE pulse phase averaged X-ray spectra are studied. The evolution of the fundamental cyclotron line at different luminosities is analyzed. The pulse period P is measured to be 103.39315(5)s at MJD 53614.5137. Two absorption features are detected in the phase averaged spectra at E_1~45keV and E_2~100keV. These can be interpreted as the fundamental cyclotron resonance scattering feature and its first harmonic and therefore the magnetic field can be estimated to be B~4x10^12G., 4 pages, 5 figures, accepted for publication in A&A Letters
Published: 2007

16. The Peculiar X-ray Transient IGR 16358-4726

Author: S. K. Patel, C. Kouveliotou, A. Tennant, P. M. Woods, A. King, M. H. Finger, P. Ubertini, C. Winkler, T. J.-L. Courvoisier, M. van der Klis, S. Wachter, B. M. Gaensler, C. J. Phillips, High Energy Astrophys. & Astropart. Phys (API, FNWI), and API (FNWI)
Subjects: Physics, X-ray transient, Astrophysics (astro-ph), Flux, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Orbital period, Luminosity, Neutron star, Pulsar, Space and Planetary Science, Observatory, Low Mass
Abstract: The new transient IGR 16358-4726 was discovered on 2003 March 19 with INTEGRAL. We detected the source serendipitously during our 2003 March 24 observation of SGR 1627-41 with the Chandra X-ray Observatory at the 1.7 x 10^{-10} ergs s^{-1} cm^{-2} flux level (2-10 keV) with a very high absorption column (N_H=3.3(1) x 10^{23} cm^{-2}) and a hard power law spectrum of index 0.5(1). We discovered a very strong flux modulation with a period of 5880(50) s and peak-to-peak pulse fraction of 70(6)% (2-10 keV), clearly visible in the x-ray data. The nature of IGR 16358-4726 remains unresolved. The only neutron star systems known with similar spin periods are low luminosity persistent wind-fed pulsars; if this is a spin period, this transient is a new kind of object. If this is an orbital period, then the system could be a compact Low Mass X-ray Binary (LMXB)., Comment: 4 pages, 3 figures, Submitted to The Astrophysical Journal Letters
Published: 2003
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17. A Puzzling Paucity of Double Peaked X-ray Pulsars

Author: Tatehiro Mihara, M. H. Finger, D. Gondek-Rosi{ń}ska, Tomasz Bulik, Miljenko Čemeljić, and Andrea Santangelo
Subjects: Physics, Line-of-sight, Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Spin axis, Rotation, Magnetic axis, Pulsar, Space and Planetary Science
Abstract: Accretion powered pulsars exhibit a variety of lightcurves. In this paper we propose to classify the observed lightcurves as single or double pulsed.We analyze the lightcurves of 86 accretion powered pulsars and assign them to these classes. We present three datasets: first in which the classification can be easily done, second for which the classification is more difficult and not certain, and third for which we were unable to classify the pulsar because of lack of published data. We analyze a simple model in which the angles between the magnetic and rotation axis $\beta$, and between the rotation axis and the line of sight $\theta$ are random, and show that it is inconsistent with the data. We also present a model in whichthe angle between the magnetic axis and rotation axis is restricted and compare it with the data. This leads to an upper limit on the angle $\beta < 40^\circ$. We conclude that there must be a mechanism that leads to alignment of the magnetic and spin axis in X-ray pulsars., Comment: submitted to A&A
Published: 2002

18. Physical mechanisms for the variable spin-down and light curve of SGR 1900+14

Author: P. M. Woods, Chryssa Kouveliotou, J. van Paradijs, Robert C. Duncan, M. H. Finger, Christopher Thompson, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Soft gamma repeater, Magnetosphere, Astronomy and Astrophysics, Astrophysics, Magnetar, law.invention, Neutron star, Pulsar, Space and Planetary Science, law, Astrophysics::Solar and Stellar Astrophysics, Glitch (astronomy), Magnetic dipole, Flare
Abstract: We consider the physical implications of the rapid spin-down of soft gamma repeater SGR 1900+14 reported by Woods and colleagues in 1999. During an 80 day interval between 1998 June and the large outburst on 1998 August 27, the mean spin-down rate increased by a factor of 2.3, resulting in a positive period offset of ΔP/P = 10-4. A radiation-hydrodynamical outflow associated with the August 27 event could impart the required torque, but only if the dipole magnetic field is stronger than ~1014 G and the outflow lasts longer and/or is more energetic than the observed X-ray flare. A positive period increment is also a natural consequence of a gradual, plastic deformation of the neutron star crust by an intense magnetic field, which forces the neutron superfluid to rotate more slowly than the crust. Sudden unpinning of the neutron vortex lines during the August 27 event would then induce a glitch opposite in sign to those observed in young pulsars, but of a much larger magnitude as a result of the slower rotation. The change in the persistent X-ray light curve following the August 27 event is ascribed to continued particle heating in the active region of that outburst. The enhanced X-ray output can be powered by a steady current flowing through the magnetosphere, induced by the twisting motion of the crust. The long-term rate of spin-down appears to be accelerated with respect to a simple magnetic dipole torque. Accelerated spin-down of a seismically active magnetar will occur when its persistent output of Alfvén waves and particles exceeds its spin-down luminosity or if particle flows modulate the ratio of conduction to displacement currents in the outer magnetosphere. We suggest that SGRs experience some episodes of relative inactivity, with diminished , and that such inactive magnetars are observed as anomalous X-ray pulsars (AXPs). The reappearance of persistent X-ray emission from SGR 1900+14 within one day of the August 27 event provides strong evidence that the persistent emission is not powered by accretion.
Published: 2000

19. Estimation of GRB detection by FiberGLAST

Author: W. R. Binns, Thomas A. Parnell, T. G. Guzik, J. H. Buckley, Donald B. Wallace, Gerald J. Fishman, G. Richardson, Mark L. McConnell, James M. Ryan, Paul L. Hink, K. Aisaka, Robert S. Mallozzi, R. D. Preece, J. G. Stacy, David B. Cline, Keith Rielage, M. H. Israel, M. Atac, Tumay O. Tumer, S. C. Kappadath, J. R. Macri, R. M. Kippen, Surasak Phengchamnan, M. H. Finger, W. S. Paciesas, J. W. Epstein, Robert B. Wilson, G. N. Pendleton, Yuriy Pischalnikov, P. F. Dowkontt, Michael Cherry, and G. R. Karr
Subjects: Physics, biology, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astronomy, Field of view, Astrophysics, biology.organism_classification, Spitzer Space Telescope, Sky brightness, Egret, Sensitivity (control systems), Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract: FiberGLAST is one of several instrument concepts being developed for possible inclusion as the primary Gamma-ray Large Area Space Telescope (GLAST) instrument. The predicted FiberGLAST effective area is more than 12,000 cm2 for energies between 30 MeV and 300 GeV, with a field of view that is essentially flat from 0°–80°. The detector will achieve a sensitivity more than 10 times that of EGRET. We present results of simulations that illustrate the sensitivity of FiberGLAST for the detection of gamma-ray bursts.
Published: 2000

20. GRO J2058+42 x-ray observations

Author: Tod E. Strohmayer, Robert B. Wilson, Colleen A. Wilson, Deepto Chakrabarty, B. A. Harmon, and M. H. Finger
Subjects: Physics, Neutron star, Pulsar, Astrophysics::High Energy Astrophysical Phenomena, Stellar rotation, X-ray binary, X-ray, Astronomy, Proportional counter, Astrophysics, Occultation, Pulse (physics)
Abstract: GRO J2058+42, a transient 198 second x-ray pulsar, was discovered by BATSE during a giant outburst in 1995 September–October. The total flux peaked at about 300 mCrab (20–50 keV) as measured by Earth occultation. The pulse period decreased from 198 s to 196 s during the 46-day outburst. BATSE has observed five additional weak outbursts from GRO J2058+42 with peak pulsed fluxes of about 15 mCrab (20–50 keV) that were spaced by about 110 days. The periodicity of the outbursts allowed a ToO observation by the Rossi X-ray Timing Explorer (RXTE) Proportional Counter Array (PCA) which localized the source to a 4′ error circle. We present pulse frequency history, flux histories from pulsed and Earth occultation data, and representative pulse profiles.
Published: 1997

21. Observation of a long term spin-up trend in 4U1538-52

Author: Robert B. Wilson, D. M. Scott, M. H. Finger, and Brad C. Rubin
Subjects: Physics, Neutron star, Accretion (meteorology), Pulsar, Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, Astronomy, White noise, Astrophysics, Gamma-ray burst, Power law, Term (time)
Abstract: The high mass x-ray pulsar 4U1538-52 has been continually monitored by the BATSE (Burst and Transient Source Experiment) on CGRO (Compton Gamma-ray Observatory). The frequency history reveals that a reversal of the long term trend in the accretion torque, from spinning down to spinning up, has occurred, probably in 1988. This is the first time a long term change is known to have occurred for this source. The magnitude of the average |ν/ν|∼10−11s−1 over an interval of ∼5 years is similar during spin-down and spin-up. Shorter term pulse frequency variations of either sign are also observed. The power density spectrum of fluctuations in angular acceleration is consistent with white noise on timescales from 16 to 1600 days. It can be well fit with a power law with power law index 0.10±0.21 and white noise strength (7.6±1.6)×10−21(Hz/s)2Hz−1.
Published: 1997

22. Using BATSE to measure gamma-ray burst polarization

Author: D. J. Forrest, Mark L. McConnell, M. H. Finger, and W. T. Vestrand
Subjects: Physics, Scattering cross-section, Brewster's angle, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Gamma ray, Polarimetry, Polarization (waves), symbols.namesake, Optics, Angular distribution, symbols, business, Gamma-ray burst
Abstract: We describe a technique for measuring the polarization of hard x-rays from γ-ray bursts based on the angular distribution of that portion of the flux which is scattered off the top of the Earth’s atmosphere. The scattering cross section depends not only on the scatter angle itself, but on the orientation of the scatter angle with respect to the incident polarization vector. Consequently, the distribution of the observed albedo flux will depend on the direction and the polarization properties (i.e., the level of polarization and polarization angle) of the source. Although the BATSE design (with its large field-of-view for each detector) is not optimized for albedo polarimetry, we have nonetheless investigated the feasibility of this technique using BATSE data.
Published: 1996

23. Hard X-ray polarimetry of solar flares with BATSE

Author: W. T. Vestrand, D. J. Forrest, Mark L. McConnell, and M. H. Finger
Subjects: Physics, Brewster's angle, Solar flare, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Antenna aperture, Polarimetry, Astrophysics, Electron, Polarization (waves), symbols.namesake, Optics, Observatory, symbols, Astrophysics::Earth and Planetary Astrophysics, business
Abstract: We describe a technique for measuring the polarization of hard X‐rays from solar flares based on the angular distribution of that portion of the flux which is scattered off the top of the Earth’s atmosphere. The scattering cross section depends not only on the scatter angle itself, but on the orientation of the scatter angle with respect to the incident polarization vector. Consequently, the distribution of the observed albedo flux will depend on the direction and the polarization properties (i.e., the level of polarization and polarization angle) of the source. Since the albedo component can represent a relatively large fraction (up to 40%) of the direct source flux, there will generally be sufficient signal for making such a measurement. The sensitivity of this approach is therefore dictated by the effective area and the ability of a detector system to ‘image’ the albedo flux. The 4π coverage of the BATSE detectors on the Compton Gamma‐Ray Observatory provides an opportunity to measure both the direct a...
Published: 1996

24. X-RAY AND OPTICAL OBSERVATIONS OF A 0535+26

Author: Jingzhi Yan, M. J. Coe, Ascension Camero-Arranz, C. A. Wilson-Hodge, M. H. Finger, Juan Gutiérrez-Soto, Isabel Caballero, Iain A. Steele, Peter Kretschmar, J. Suso, Michael Cherry, Sylvain Guiriec, G. L. Case, P. A. Jenke, Juan J. Rodriguez, and Vanessa McBride
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Brightness, Oscillation, Astrophysics::High Energy Astrophysical Phenomena, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Neutron star, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, General pattern, Astrophysics - High Energy Astrophysical Phenomena, Line (formation), Fermi Gamma-ray Space Telescope
Abstract: We present recent contemporaneous X-ray and optical observations of the Be/X-ray binary system A\,0535+26 with the \textit{Fermi}/Gamma-ray Burst Monitor (GBM) and several ground-based observatories. These new observations are put into the context of the rich historical data (since $\sim$1978) and discussed in terms of the neutron star Be-disk interaction. The Be circumstellar disk was exceptionally large just before the 2009 December giant outburst, which may explain the origin of the unusual recent X-ray activity of this source. We found a peculiar evolution of the pulse profile during this giant outburst, with the two main components evolving in opposite ways with energy. A hard 30-70 mHz X-ray QPO was detected with GBM during this 2009 December giant outburst. It becomes stronger with increasing energy and disappears at energies below 25\,keV. In the long-term a strong optical/X-ray correlation was found for this system, however in the medium-term the H$_\alpha$ EW and the V-band brightness showed an anti-correlation after $\sim$2002 Agust. Each giant X-ray outburst occurred during a decline phase of the optical brightness, while the H$_\alpha$ showed a strong emission. In late 2010 and before the 2011 February outburst, rapid V/R variations are observed in the strength of the two peaks of the H$_\alpha$ line. These had a period of $\sim$\,25 days and we suggest the presence of a global one-armed oscillation to explain this scenario. A general pattern might be inferred, where the disk becomes weaker and shows V/R variability beginning $\sim$\,6 months following a giant outburst., Comment: 18, 11 figures, 1 table
Published: 2012

25. BATSE observations of 4U1538-52: A 530 second pulsar

Author: Deepto Chakrabarty, T. J. Prince, B. C. Rubin, Robert B. Wilson, J. Chiu, W. S. Paciesas, M. H. Finger, Gerald J. Fishman, and C. A. Meegan
Subjects: Physics, Orbital elements, Background subtraction, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, X-ray binary, Astronomy, Astrophysics, Orbital period, Binary pulsar, Pulsar, Sky, Supergiant, media_common
Abstract: The BATSE experiment on CGRO, a nearly continuous all sky monitor, is capable of detecting and monitoring pulsars in the hard x‐ray/gamma‐ray energy range. Using data processed with a global background subtraction method, we are able to construct pulsed intensity and pulse period histories for the accreting binary x‐ray pulsar 4U1538‐52 in the 20–50 keV energy band. This pulsar, which has a pulse period of approximately 530 seconds, is believed to be a wind accretor with a high mass companion. It was observed by previous experiments to be in secular spin down during the 1976–1988 period. Here we report observing, for the first time, a secular spin up trend. We are able to use this data to improve the upper limit on orbital period changes.
Published: 1994

26. BATSE observations of GS 0834-430

Author: C. A. Wilson, B. A. Harmon, R. B. Wilson, G. J. Fishman, and M. H. Finger
Published: 1994

27. BATSE observations of Her X-1: The 35 day cycle, orbit determination, and torque studies

Author: M. H. Finger, L. Bildsten, G. N. Pendleton, R. B. Wilson, and M. Briggs
Subjects: Physics, Orbital elements, Neutron star, Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, Flux, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Orbital period, Orbit determination, Rotation, Luminosity
Abstract: Results of timing and spectral analyses of Her X‐1 are presented, utilizing observations by the BATSE experiment from the CGRO mission to date. A correlation is observed between the hard x‐ray pulsed flux and spin frequency derivative, a measure of the torque acting on the neutron star. An apparent correlation is also found between the 35 day cycle start times and the pulsed flux. Orbital parameters are obtained from the BATSE data, with evidence found for an orbital period derivative slightly less than that reported in Deeter et al. (1991).
Published: 1994

28. BATSE observations of GX 354-0

Author: W. S. Paciesas, B. A. Harmon, R. B. Wilson, C. A. Meegan, Shuang-Nan Zhang, B. C. Rubin, M. H. Finger, and G. J. Fishman
Subjects: Physics, Observatory, Galactic Center, Astronomy, Astrophysics, Imaging technique, Light curve, Occultation
Abstract: The transient hard x‐ray source and burster GX 354‐0 (MXB 1728‐34) has been detected several times since April 1991 using the newly‐developed occultation transform imaging to process data from the BATSE large area detectors (20‐1800 keV) on the COMPTON Observatory. One period corresponds to observations of an outburst seen by GRANAT/SIGMA in February 1992 (Goldwurm et al. 1992). This exploratory effort uses the occultation imaging technique to guide the identification of bright galactic center region sources within a few‐degree field. Then, using this information, temporal and spectral information is extracted with the standard occultation software.
Published: 1994

29. BATSE discovery of a hard X-ray pulsar:GRO J1008-57

Author: R. B. Wilson, M. Briggs, T. A. Prince, L. Bildsten, B. A. Harmon, C. Chakrabarty, G. N. Pendleton, Shuang-Nan Zhang, M. T. Stollberg, G. J. Fishman, B. C. Rubin, and M. H. Finger
Subjects: Physics, Range (particle radiation), Solar System, Pulsar, Binary star, ROSAT, Bremsstrahlung, Astronomy, Astrophysics, X-ray pulsar, Intensity (physics)
Abstract: BATSE detection of a new hard x‐ray pulsar is reported. The source was first observed on 14 Jul 1993, reached a maximum intensity on 25 Jul 1993, then declined smoothly until it fell below the detection threshold on 16 Aug 1993. The BATSE location was sufficiently well determined to permit OSSE, ASCA, & ROSAT observations, leading to an improved source location. The observed period at the solar system barycenter was 93.548±0.002s, 93.5665±0.0005s, and 93.541±0.004 on 15 Jul 1993, 23 Jul 1993, and 10 Aug 1993, respectively. The source is detected between ∼20 keV and 160 keV, with a spectrum fit by an optically thin thermal bremsstrahlung form, having a kT of 25.4±2.1 keV during the rise to maximum intensity, decreasing monotonically during the remainder of the outburst to 17.1±2.5 keV on 5 Aug 1993. The pulse profile in this energy range has a single broad peak, with the maximum occurring later at higher energies. The pulse profile, intensity history, and spectral behavior observed by BATSE during the outb...
Published: 1994

30. BATSE images of the galactic center region

Author: C. A. Meegan, B. C. Rubin, W. S. Paciesas, M. H. Finger, Shuang-Nan Zhang, G. J. Fishman, R. B. Wilson, and B. A. Harmon
Subjects: Physics, Radon transform, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Galactic Center, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy, Field of view, Astrophysics, Occultation, Sky, Observatory, Gamma-ray burst, media_common
Abstract: The non‐collimated detectors of BATSE (Burst And Transient Source Experiment) on the Compton Gamma Ray Observatory (CGRO) have been used to produce wide field images of celestial hard X‐ray and gamma‐ray sources in the energy range between 20 keV and 500 keV. The occultation process is modeled as a Radon transform and then available Radon inversion software packages are applied to produce images. BATSE can simultaneously image 70% of the sky in as little as a few days and the whole sky in 3‐4 weeks. A field of view of a single image can be chosen in software to be from 5°×5° to 40°×40°. Multiple images with different FOVs centered on different parts of the sky can be produced simultaneously. Selected images obtained from this method for the galactic center region are presented here.
Published: 1994

31. BATSE observations of GS 0834−430

Author: C. A. Wilson, B. A. Harmon, R. B. WIlson, G. J. Fishman, C. A. Meegan, D. Chakrabarty, J. M. Grunsfeld, T. A. Prince, M. H. Finger, W. S. Paciesas, and G. N. Pendleton
Subjects: Physics, Orbital elements, Radiation flux, Pulsar, Astrophysics::High Energy Astrophysical Phenomena, Harmonics, Gamma ray, X-ray binary, Flux, Astrophysics, Pulse (physics)
Abstract: GS 0834‐430 has been observed in seven outbursts with the Large Area Detectors (LAD’s) of the Burst and Transient Source Experiment (BATSE) on the Compton Gamma Ray Observatory. We have fit observed pulse frequencies and total flux with a model that assumes binary motion and a relationship between the total flux and accretion induced torque. In addition, we have fit the first five harmonics of 4–6 day summed pulse profiles with a template pulse profile for each channel to detect changes in pulse shape. We present the history of the total flux and the pulsed frequency, pulse profiles, and orbital parameters.
Published: 1993

32. Observation of a hard state outburst in the GX339−4 system

Author: Colleen A. Wilson, B. C. Rubin, C. A. Meegan, J. C. Ling, Geoffrey N. Pendleton, R. B. Wilson, W. A. Wheaton, B. A. Harmon, W. S. Paciesas, G. J. Fishman, Robert T. Skelton, and M. H. Finger
Subjects: Physics, Radiation flux, Spectral index, Observatory, Astrophysics::High Energy Astrophysical Phenomena, Binary star, Gamma ray, Astronomy, Flux, Astrophysics, Compact star, Orbital period
Abstract: Monitoring of the x‐ray binary system GX339−4 with the Burst and Transient Source Experiment (BATSE) on the Compton Gamma Ray Observatory indicated that the compact object in this system had entered its hard emission state in late June of 1991. X‐ray flux between 20 keV and approximately 300 keV was observed to increase over a period of about 60 days, peaking at 300–400 mCrab. From late August to early October, from flux GX339−4 dropped in intensity (with spectral softening) until it was not observable above 20 keV. We discuss this observation and compare it to other studies of GX339−4. We report results of a search for the 0.6 day orbital period, as well as for quasi‐periodic oscillations that have been seen in the hard state.
Published: 1993

33. BATSE observations of Cen X-3

Author: R. B. Wilson, B. A. Harmon, G. J. Fishman, W. S. Paciesas, M. H. Finger, and C. A. Meegan
Subjects: Orbital elements, Physics, Radiation flux, Pulsar, Observatory, Astrophysics::High Energy Astrophysical Phenomena, Binary star, Gamma ray, Astronomy, Flux, Astrophysics, Binary pulsar
Abstract: We present results from 520 days of continuous hard x‐ray observation of the x‐ray binary pulsar Cen X‐3. These observations were made with the Burst And Transient Source Experiment (BASTE) on the Compton Gamma Ray Observatory. Results of this analysis include a new determination of the binary orbital parameters, and histories of the pulse frequency and pulsed flux during the observation.
Published: 1993

34. Correlated optical observations of Sco X-1 using the BATSE spectroscopy detectors

Author: R. B. Wilson, G. J. Fishman, B. A. Harmon, G. Fitzgibbons, W. S. Paciesas, B. C. Rubin, C. A. Meegan, B. McNamara, and M. H. Finger
Subjects: Physics, High energy, Range (particle radiation), Detector, Binary star, Astronomy, Astrophysics, Visible radiation, Light curve, Spectroscopy
Abstract: We have investigated the feasibility of using the 8–16 keV energy channel of the BATSE spectroscopy detectors to study the correlated short and long term optical and high energy behavior of Sco X‐1. We have found that in this energy range, the spectroscopy detectors are well suited to these tasks. To demonstrate its short period monotoring potential, simultaneous BATSE 8–16 keV and optical Sco X‐1 light curves are presented. Longer term activity cycles also appear to be present. BATSE spectroscopy data covering a 50 day period show distinct episodes of Sco X‐1 activity.
Published: 1993

35. Earth occultation measurements of galactic hard X-ray/gamma-ray sources: A survey of BATSE results

Author: W. S. Paciesas, M. H. Finger, C. A. Meegan, Geoffrey N. Pendleton, Colleen A. Wilson, B. C. Rubin, G. J. Fishman, Martin N. Brock, R. B. Wilson, and B. A. Harmon
Subjects: Physics, Radiation flux, Observatory, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, X-ray, Astronomy, Flux, Transient (oscillation), Astrophysics, Occultation, Spectral line
Abstract: The large area detectors on the Burst and Transient Source Experiment (BATSE) on the Compton Gamma Ray Observatory (CGRO) are being used to monitor about 40 sources in the energy range of 20–1800 keV and to search for transients on a daily basis. We present an overview of the sources which have been detected with the BATSE instrument, and discuss some of the properties of these sources which can be studied. Time histories of the flux and energy spectra of recently detected transient hard x‐ray sources are presented.
Published: 1993

36. BATSE observations of the massive X-ray binary 4U1700−37/HD153919

Author: Robert B. Wilson, Brad C. Rubin, W. S. Paciesas, C. A. Meegan, Gerald J. Fishman, B. A. Harmon, M. H. Finger, and Michael S. Briggs
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, Flux, Binary number, Astronomy, Astrophysics, Occultation, Radiation flux, Stars, Crab Nebula, Physics::Space Physics, Binary star, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The Earth occultation technique has been used to monitor the massive x‐ray binary (MXRB) 4U1700−37/HD153919 with BATSE. This source has been important in the study of stellar winds from O‐type stars and of radiation and flaring mechanisms of MXRB. We have detected several large flaring episodes, during which the 20 to 50 keV flux from this binary exceeds the flux from the Crab Nebula in the same energy range.
Published: 1993

37. BATSE observations of EXO 2030+375

Author: R. B. Wilson, G. J. Fishman, Geoffrey N. Pendleton, Mark Stollberg, Colleen A. Wilson, W. S. Paciesas, B. A. Harmon, C. A. Meegan, and M. H. Finger
Subjects: Physics, Pulsar, Binary star, Astronomy, Astrophysics, Orbital period, Binary pulsar
Abstract: The transient x‐ray pulsar EXO 2030+375, first detected by EXOSAT in 1985 May–August, has also been detected by the Large Area Detectors (LAD’s) of BATSE. A major outburst occurred during 9–19 February 1992. BATSE has also seen this source on six other occasions at intervals of about 46 days. We present the pulse profile, spectrum, period history, and a refined orbital period for this binary pulsar.
Published: 1993

38. Modeling the gamma-ray background on BATSE

Author: W. S. Paciesas, Brad C. Rubin, B. A. Harmon, Gerald J. Fishman, Duane E. Gruber, Robert B. Wilson, James C. Ling, Martin N. Brock, M. H. Finger, W. A. Wheaton, Robert T. Skelton, and C. A. Meegan
Subjects: Physics, Background subtraction, COSMIC cancer database, Mathematical model, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Gamma ray, Astronomy, Astrophysics, Particle detector, Background noise, Pulsar, Sky, media_common
Abstract: The gamma‐ray background on the BATSE experiment is a complex, time‐varying combination of several factors. These include diffuse galactic and cosmic background; activation induced by particle fluxes in the SAA; atmospheric gamma‐rays; discrete source contributions; and other factors. We have developed techniques for fitting the Continuous and Discriminator BATSE data with multi‐component models. Some of these components are intended to directly represent factors comprising the background, while others are more empirical in nature. The model is used to ‘‘detrend’’ the data and can be used for on‐ground folding in pulsar analysis and searches for long period pulsations, searches for weak, long duration gamma‐ray bursts and transients, background subtraction from known gamma‐ray bursts and other transients, and construction of the burst sky exposure map. Components of these models can be used to measure the diffuse background and obtain refined measurements of discrete sources.
Published: 1993

39. Quasi-periodic Oscillations during a Giant Outburst of A0535+262

Author: Robert B. Wilson, M. H. Finger, and B. A. Harmon
Subjects: Physics, Space and Planetary Science, Astronomy, Astronomy and Astrophysics, Astrophysics, Quasi periodic
Published: 1996

40. Observation of GX 339-4 hard state outbursts in 1991 and 1992

Author: W. S. Paciesas, Robert B. Wilson, C. A. Wilson, Martin N. Brock, B. A. Harmon, Geoffrey N. Pendleton, B. C. Rubin, Gerald J. Fishman, M. H. Finger, Michael S. Briggs, and C. A. Meegan
Subjects: Physics, X-ray astronomy, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy, Astronomy and Astrophysics, Gamma-ray astronomy, State (functional analysis), Astrophysics, Power law, Space and Planetary Science, Observatory, Binary star, Spectrum analysis
Abstract: Two hard state (X-ray low state) outbursts in the GX 339-4 system in 1991 June-October and 1992 September-1993 January were detected and monitored by the Burst and Transient Source Experiment (BATSE) on the Compton Gamma Ray Observatory (CGRO). The outbursts were remarkably similar in both temporal and spectral aspects. The spectrum in the 20-300 keV band evolves from a hard, Comptonized shape to a steeper (alpha approximately equals -3) power law during each outburst.
Published: 1994

41. New outburst of A0535+26 observed with INTEGRAL, RXTE and Suzaku

Author: Slawomir Suchy, R. E. Rothschild, Y. Terada, Andrea Santangelo, Wataru Iwakiri, Rüdiger Staubert, D. Klochkov, Laura Barragan, T. Mihara, A. Camero-Arranz, Kazuo Makishima, Jörn Wilms, M. H. Finger, Katja Pottschmidt, Peter Kretschmar, Motoki Nakajima, Carlo Ferrigno, I. Kreykenbohm, Teruaki Enoto, and Isabel Caballero

42. X-ray flux related timing and spectral features of 2S 1417-62

Author: M. H. Finger, D. M. Scott, Altan Baykal, Sıtkı Çağdaş İnam, J. H. Swank, and OpenMETU
Subjects: Physics, Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Flux, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Power law, Spectral line, Pulse (physics), Pulsar, Space and Planetary Science, Sign (mathematics), Line (formation)
Abstract: RXTE observations of the X-ray transient pulsar 2S 1417-62 between 1999 November and 2000 August with a total exposure of $\sim 394$ ksec were analyzed. Observations include a main outburst followed by a series of mini outbursts. Changes in pulse morphology and pulse fraction were found to be related to the changes in X-ray flux. Particularly low X-ray flux regions were found to have significantly lower pulse fractions with different pulse morphologies. The 3-60 keV PCA-HEXTE main outburst spectrum was modeled with an absorbed power law model with high energy cut-off and a Gaussian Iron line complex feature. Using the same spectral model, individual 3-20 keV PCA spectra were found to be softer and less absorbed in low X-ray flux regions between outbursts. Spectral studies showed that hydrogen column density was correlated, and the power law index was anti-correlated with the 3-20 keV X-ray flux. X-ray flux related spectral and timing features in 2S 1417-62 except for low X-ray flux regions were interpreted as a sign of disc accretion with a similar accretion geometry with a varying mass accretion rate ($\dot{M}$), whereas spectral and timing features of the low X-ray flux regions were interpreted as a sign of possible temporary accretion geometry change prior to the next periastron where $\dot{M}$ increases again to restore the original accretion geometry., Comment: 14 pages, 6 figures, accepted for publication in MNRAS

43. THE FERMI–GBM THREE-YEAR X-RAY BURST CATALOG.

Author: P. A. Jenke, M. Linares, V. Connaughton, E. Beklen, A. Camero-Arranz, M. H. Finger, and C. A. Wilson-Hodge
Subjects: GAMMA ray measurement, GAMMA ray bursts, FERMI Gamma-ray Space Telescope (Spacecraft), NEUTRON stars, X-ray spectra, BLACKBODY radiation, EQUIPMENT & supplies
Abstract: The Fermi Gamma-ray Burst Monitor (GBM) is an all-sky gamma-ray monitor well known in the gamma-ray burst (GRB) community. Although GBM excels in detecting the hard, bright extragalactic GRBs, its sensitivity above 8 keV and its all-sky view make it an excellent instrument for the detection of rare, short-lived Galactic transients. In 2010 March, we initiated a systematic search for transients using GBM data. We conclude this phase of the search by presenting a three-year catalog of 1084 X-ray bursts. Using spectral analysis, location, and spatial distributions we classified the 1084 events into 752 thermonuclear X-ray bursts, 267 transient events from accretion flares and X-ray pulses, and 65 untriggered gamma-ray bursts. All thermonuclear bursts have peak blackbody temperatures broadly consistent with photospheric radius expansion (PRE) bursts. We find an average rate of 1.4 PRE bursts per day, integrated over all Galactic bursters within about 10 kpc. These include 33 and 10 bursts from the ultra-compact X-ray binaries 4U 0614+09 and 2S 0918-549, respectively. We discuss these recurrence times and estimate the total mass ejected by PRE bursts in our Galaxy. [ABSTRACT FROM AUTHOR]
Published: 2016
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44. FERMI GBM OBSERVATIONS OF V404 CYG DURING ITS 2015 OUTBURST.

Author: P. A. Jenke, C. A. Wilson-Hodge, Jeroen Homan, P. Veres, M. S. Briggs, E. Burns, V. Connaughton, M. H. Finger, and M. Hui
Subjects: BINARY black holes, ASTROCHEMISTRY, GAMMA ray bursts, MOLECULES, LUMINOSITY
Abstract: V404 Cygni was discovered in 1989 by the Ginga X-ray satellite during its only previously observed X-ray outburst and soon after confirmed as a black hole binary. On 2015 June 15, the Gamma-ray Burst Monitor (GBM) triggered on a new outburst of V404 Cygni. We present 13 days of GBM observations of this outburst, including Earth occultation flux measurements and spectral and temporal analysis. The Earth occultation fluxes reached 30 Crab with detected emission to 100 keV and determined, via hardness ratios, that the source was in a hard state. At high luminosity, spectral analysis between 8 and 300 keV showed that the electron temperature decreased with increasing luminosity. This is expected if the protons and electrons are in thermal equilibrium during an outburst with the electrons cooled by the Compton scattering of softer seed photons from the disk. However, the implied seed photon temperatures are unusually high, suggesting a contribution from another source, such as the jet. No evidence of state transitions is seen during this time period. The temporal analysis reveals power spectra that can be modeled with two or three strong, broad Lorentzians, similar to the power spectra of black hole binaries in their hard state. [ABSTRACT FROM AUTHOR]
Published: 2016
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45. SIMULTANEOUS NuSTAR/CHANDRA OBSERVATIONS OF THE BURSTING PULSAR GRO J1744-28 DURING ITS THIRD REACTIVATION.

Author: G. Younes, C. Kouveliotou, B. W. Grefenstette, J. A. Tomsick, A. Tennant, M. H. Finger, F. Fürst, K. Pottschmidt, V. Bhalerao, S. E. Boggs, L. Boirin, D. Chakrabarty, F. E. Christensen, W. W. Craig, N. Degenaar, A. C. Fabian, P. Gandhi, E. Göğüş, C. J. Hailey, and F. A. Harrison
Subjects: PULSARS, PULSATING stars, GAMMA ray bursts, GAMMA ray astronomy, RADIATION sources
Abstract: We report on a 10 ks simultaneous Chandra/High Energy Transmission Grating (HETG)–Nuclear Spectroscopic Telescope Array (NuSTAR) observation of the Bursting Pulsar, GRO J1744-28, during its third detected outburst since discovery and after nearly 18 yr of quiescence. The source is detected up to 60 keV with an Eddington persistent flux level. Seven bursts, followed by dips, are seen with Chandra, three of which are also detected with NuSTAR. Timing analysis reveals a slight increase in the persistent emission pulsed fraction with energy (from 10% to 15%) up to 10 keV, above which it remains constant. The 0.5–70 keV spectra of the persistent and dip emission are the same within errors and well described by a blackbody (BB), a power-law (PL) with an exponential rolloff, a 10 keV feature, and a 6.7 keV emission feature, all modified by neutral absorption. Assuming that the BB emission originates in an accretion disk, we estimate its inner (magnetospheric) radius to be about 4 × 107 cm, which translates to a surface dipole field B ≈ 9 × 1010 G. The Chandra/HETG spectrum resolves the 6.7 keV feature into (quasi-)neutral and highly ionized Fe xxv and Fe xxvi emission lines. XSTAR modeling shows these lines to also emanate from a truncated accretion disk. The burst spectra, with a peak flux more than an order of magnitude higher than Eddington, are well fit with a PL with an exponential rolloff and a 10 keV feature, with similar fit values compared to the persistent and dip spectra. The burst spectra lack a thermal component and any Fe features. Anisotropic (beamed) burst emission would explain both the lack of the BB and any Fe components. [ABSTRACT FROM AUTHOR]
Published: 2015
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46. THE FIVE YEAR FERMI/GBM MAGNETAR BURST CATALOG.

Author: A. C. Collazzi, C. Kouveliotou, A. J. van der Horst, G. A. Younes, Y. Kaneko, E. Göğüş, L. Lin, J. Granot, M. H. Finger, V. L. Chaplin, D. Huppenkothen, A. L. Watts, A. von Kienlin, M. G. Baring, D. Gruber, P. N. Bhat, M. H. Gibby, N. Gehrels, J. McEnery, and M. van der Klis
Published: 2015
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47. The LOFT mission concept: a status update

Author: Feroci, M, Bozzo, E, Brandt, S, Hernanz, M, Van Der Klis, M, Liu, L, Orleanski, P, Pohl, M, Santangelo, A, Schanne, S, Stella, L, Takahashi, T, Tamura, H, Watts, A, Wilms, J, Zane, S, Zhang, S, Bhattacharyya, S, Agudo, I, Ahangarianabhari, M, Albertus, C, Alford, M, Alpar, A, Altamirano, D, Alvarez, L, Amati, L, Amoros, C, Andersson, N, Antonelli, A, Argan, A, Artigue, R, Artigues, B, Atteia, J, Azzarello, P, Bakala, P, Ballantyne, Dr, Baldazzi, G, Baldo, M, Balman, S, Barbera, M, Van Baren, C, Barret, D, Baykal, A, Begelman, M, Behar, E, Behar, O, Belloni, T, Bellutti, P, Bernardini, F, Bertuccio, G, Bianchi, S, Bianchini, A, Binko, P, Blay, P, Bocchino, F, Bode, M, Bodin, P, Bombaci, I, Bonnet Bidaud, J, Borghi, G, Boutloukos, S, Bouyjou, F, Bradley, L, Braga, J, Briggs, Ms, Brown, E, Buballa, M, Bucciantini, N, Burderi, L, Burgay, M, Bursa, M, Budtz-Jorgensen, C, Cackett, E, Cadoux, Fr, Cais, P, Caliandro, Ga, Campana, R, Campana, S, Cao, X, Capitanio, F, Casares, J, Casella, P, Castro-Tirado, Aj, Cavazzuti, E, Cavechi, Y, Celestin, S, Cerda-Duran, P, Chakrabarty, D, Chamel, N, Chateau, F, Chen, C, Chen, Y, Chenevez, J, Chernyakova, M, Coker, J, Cole, R, Collura, A, Coriat, M, Cornelisse, R, Costamante, L, Cros, A, Cui, W, Cumming, A, Cusumano, G, Czerny, B, D'Ai, A, D'Ammando, F, D'Elia, V, Dai, Z, Del Monte, E, De Luca, A, De Martino, D, Dercksen, Jpc, De Pasquale, M, De Rosa, A, Del Santo, M, Di Cosimo, S, Degenaar, N, Den Herder, Jw, Diebold, S, Di Salvo, T, Dong, Y, Donnarumma, I, Doroshenko, V, Doyle, G, Drake, Sa, Durant, M, Emmanoulopoulos, D, Enoto, T, Erkut, Mh, Esposito, P, Evangelista, Y, Fabian, A, Falanga, M, Favre, Y, Feldman, C, Fender, R, Feng, H, Ferrari, V, Ferrigno, C, Ficorella, F, Finger, M, Finger, Mh, Fraser, Gw, Frericks, M, Fullekrug, M, Fuschino, F, Gabler, M, Galloway, Dk, Galvez Sanchez, Jl, Gandhi, P, Gao, Z, Garcia-Berro, E, Gendre, B, Gevin, O, Gezari, S, Giles, Ab, Gilfanov, M, Giommi, P, Giovannini, G, Giroletti, M, Gogus, E, Goldwurm, A, Goluchova, K, Gotz, D, Gou, L, Gouiffes, C, Grandi, P, Grassi, M, Greiner, J, Grinberg, V, Groot, P, Gschwender, M, Gualtieri, L, Guedel, M, Guidorzi, C, Guy, L, Haas, D, Haensel, P, Hailey, M, Hamuguchi, K, Hansen, F, Hartmann, Dh, Haswell, Ca, Hebeler, K, Heger, A, Hempel, M, Hermsen, W, Homan, J, Hornstrup, A, Hudec, R, Huovelin, J, Huppenkothen, D, Inam, Sc, Ingram, A, In'Tzand, Jjm, Israel, G, Iwasawa, K, Izzo, L, Jacobs, Hm, Jetter, F, Johannsen, T, Jenke, Pa, Jonker, P, Jose, J, Kaaret, P, Kalamkar, M, Kalemci, E, Kanbach, G, Karas, V, Karelin, D, Kataria, D, Keek, L, Kennedy, T, Klochkov, D, Kluzniak, W, Koerding, E, Kokkotas, K, Komossa, S, Korpela, S, Kouveliotou, C, Kowalski, Af, Kreykenbohm, I, Kuiper, Lm, Kunneriath, D, Kurkela, A, Kuvvetli, I, La Franca, F, Labanti, C, Lai, D, Lamb, Fk, Lachaud, C, Laubert, Pp, Lebrun, F, Li, X, Liang, E, Limousin, O, Lin, D, Linares, M, Linder, D, Lodato, G, Longo, F, Lu, F, Lund, N, Maccarone, Tj, Macera, D, Maestre, S, Mahmoodifar, S, Maier, D, Malcovati, P, Malzac, J, Malone, C, Mandel, I, Mangano, V, Manousakis, A, Marelli, M, Margueron, J, Marisaldi, M, Markoff, Sb, Markowitz, A, Marinucci, A, Martindale, A, Martinez, G, Mchardy, Im, Medina-Tanco, G, Mehdipour, M, Melatos, A, Mendez, M, Mereghetti, S, Migliari, S, Mignani, R, Michalska, M, Mihara, T, Miller, Mc, Miller, Jm, Mineo, T, Miniutti, G, Morsink, S, Motch, C, Motta, S, Mouchet, M, Mouret, G, Mulacova, J, Muleri, F, Munoz-Darias, T, Negueruela, I, Neilsen, J, Neubert, T, Norton, Aj, Nowak, M, Nucita, A, O'Brien, P, Oertel, M, Olsen, Peh, Orienti, M, Orio, M, Orlandini, M, Osborne, Jp, Osten, R, Ozel, F, Pacciani, L, Paerels, F, Paltani, S, Paolillo, M, Papadakis, I, Papitto, A, Paragi, Z, Paredes, Jm, Patruno, A, Paul, B, Pederiva, F, Perinati, E, Pellizzoni, A, Penacchioni, Av, Peretz, U, Perez, Ma, Perez-Torres, M, Peterson, Bm, Petracek, V, Picciotto, A, Piemonte, C, Pittori, C, Pons, J, Portell, J, Possenti, A, Postnov, K, Poutanen, J, Prakash, M, Prandoni, I, Le Provost, H, Psaltis, D, Pye, J, Qu, J, Rambaud, D, Ramon, P, Ramsay, G, Rapisarda, M, Rachevski, A, Rashevskaya, I, Ray, Ps, Rea, N, Reddy, S, Reig, P, Reina Aranda, M, Remillard, R, Reynolds, C, Rezzolla, L, Ribo, M, De La Rie, R, Riggio, A, Rios, A, Rischke, Dh, Rodriguez-Gil, P, Rodriguez, J, Rohlfs, R, Romano, P, Rossi, Emr, Rozanska, A, Rousseau, A, Rudak, B, Russell, Dm, Ryde, F, Sabau-Graziati, L, Sakamoto, T, Sala, G, Salvaterra, R, Salvetti, D, Sanna, A, Sandberg, J, Savolainen, T, Scaringi, S, Schaffner-Bielich, J, Schatz, H, Schee, J, Schmid, C, Serino, M, Shakura, N, Shore, S, Schnittman, Jd, Schneider, R, Schwenk, A, Schwope, Ad, Sedrakian, A, Seyler, J, Shearer, A, Slowikowska, A, Sims, M, Smith, A, Smith, Dm, Smith, Pj, Sobolewska, M, Sochora, V, Soffitta, P, Soleri, P, Song, L, Spencer, A, Stamerra, A, Stappers, B, Staubert, R, Steiner, Aw, Stergioulas, N, Stevens, Al, Stratta, G, Strohmayer, Te, Stuchlik, Z, Suchy, S, Suleimanov, V, Tamburini, F, Tauris, T, Tavecchio, F, Tenzer, C, Thielemann, Fk, Tiengo, A, Tolos, L, Tombesi, F, Tomsick, J, Torok, G, Torrejon, Jm, Torres, Df, Torresi, E, Tramacere, A, Traulsen, I, Trois, A, Turolla, R, Turriziani, S, Typel, S, Uter, P, Uttley, P, Vacchi, A, Varniere, P, Vaughan, S, Vercellone, S, Vietri, M, Vincent, Fh, Vrba, V, Walton, D, Wang, J, Wang, Z, Watanabe, S, Wawrzaszek, R, Webb, N, Weinberg, N, Wende, H, Wheatley, P, Wijers, R, Wijnands, R, Wille, M, Wilson-Hodge, Ca, Winter, B, Walk, Sj, Wood, K, Woosley, Se, Wu, X, Xiao, L, Xu, R, Yu, W, Yuan, F, Yuan, W, Yuan, Y, Zampa, G, Zampa, N, Zampieri, L, Zdunik, L, Zdziarski, A, Zech, A, Zhang, B, Zhang, C, Zingale, M, Zorzi, N, Zwart, F, High Energy Astrophys. & Astropart. Phys (API, FNWI), ISDC Data Centre for Astrophysics, Université de Genève = University of Geneva (UNIGE), Icahn School of Medicine at Mount Sinai [New York] (MSSM), Rutgers, The State University of New Jersey [New Brunswick] (RU), Rutgers University System (Rutgers), Institut für Astronomie und Astrophysik [Tübingen] (IAAT), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Scienze e Tecnologie Chimiche, Università degli Studi di Roma Tor Vergata [Roma], Graduate School of the Natural Science and Technology [Kanazawa], Kanazawa University (KU), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Centre Interdisciplinaire de Nanoscience de Marseille (CINaM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Tampere University of Technology [Tampere] (TUT), University of Maryland [College Park], University of Maryland System, Department of Biological Sciences [Mississippi], University of Southern Mississippi (USM), School of Physics and Astronomy [Southampton], University of Southampton, Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), Università di Roma La Sapienza, Università di Roma Tor Vergata, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Swedish Institute of Space Physics [Uppsala] (IRF), INAF - Osservatorio Astronomico di Brera (OAB), Department of Computer Sciences [Scheffield], University of Sheffield [Sheffield], Colgate University, Bibliothèque nationale de France (BnF), Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), ARC Centre of Excellence for Environmental Decisions (ARC CEED), The University of Western Australia (UWA)-Australian National University (ANU)-University of Queensland [Brisbane]-Royal Melbourne Institute of Technology University (RMIT University)-School of BioSciences [Melbourne], Faculty of Science [Melbourne], University of Melbourne-University of Melbourne-Faculty of Science [Melbourne], University of Melbourne-University of Melbourne, ARC Centre of Excellence for Coral Reef Studies (CoralCoE), James Cook University (JCU), Lund University [Lund], Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Anthropologie Moléculaire et Imagerie de Synthèse (AMIS), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de synthèse organique (DCSO), École polytechnique (X)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), University of Alabama at Birmingham [ Birmingham] (UAB), INAF - Osservatorio Astronomico di Cagliari (OAC), ELECTRONIQUE 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Modèles Statistiques (LPTMS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), School of Geosciences, Monash University [Clayton], Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université libre de Bruxelles (ULB), National Oceanography Centre [Southampton] (NOC), Dublin Institute for Advanced Studies (DIAS), Dublin City University [Dublin] (DCU), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Institut Parisien de Chimie Moléculaire (IPCM), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Chinese Academy of Sciences [Beijing] (CAS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), China Information Technology Security Evaluation Center (CNITSEC), Department of Applied Mathematics and Computer Science [Lyngby] (DTU Compute), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), PCAS, Anton Pannekoek Institute for Astronomy, Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), International Space Science Institute [Bern] (ISSI), Université Grenoble Alpes - UFR Médecine (UGA UFRM), Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), CALVIN research group [Edinburgh], Institute of Perception, Action and Behaviour (IPAB), University of Edinburgh-University of Edinburgh, Department of Electronics and Electrical Engineering [Bath], University of Bath [Bath], United States Geological Survey [Reston] (USGS), Sr. PLM Consultant, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Dept Ind Engn & Informat Techonolgy, Università degli studi di Trieste = University of Trieste, Max-Planck-Institut für Extraterrestrische Physik (MPE), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology (MIT), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Matériaux, ingénierie et science [Villeurbanne] (MATEIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Wisconsin Regional Primate Research Center, University of Wisconsin-Madison, SRON Netherlands Institute for Space Research (SRON), Opole University of Technology, University of Technology (Opole), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen]-Radboud University [Nijmegen], Radboud University [Nijmegen], NASA Goddard Space Flight Center (GSFC), Dept Fis Aplicada, Universidad de Granada = University of Granada (UGR), Victoria University [Melbourne], The Hong Kong Polytechnic University [Hong Kong] (POLYU), Chinese Academy of Sciences [Changchun Branch] (CAS), Department of Physics, Chemistry and Biology [Linköping] (IFM), Linköping University (LIU), Institut de Chimie des Substances Naturelles (ICSN), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), Centre de recherche en Biologie cellulaire de Montpellier (CRBM), Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy, University of Zielona Góra, Department of Electronics and Computer Systems, Takushoku University, Instituto Nacional de Pesquisas da Amazônia (INPA), Università degli studi di Catania = University of Catania (Unict), Centre d'Ecologie et des Sciences de la COnservation (CESCO), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Ecologie Alpine (LECA ), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire de Physico-Chimie de l'Atmosphère (LPCA), Université du Littoral Côte d'Opale (ULCO)-Centre National de la Recherche Scientifique (CNRS), HEPL, Solar Physics, Stanford University, Institut des Sciences Moléculaires de Marseille (ISM2), Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Space Telescope Science Institute (STSci), Dipartimento di Scienze Fisiche [Naples], University of Naples Federico II = Università degli studi di Napoli Federico II, Columbia University [New York], Laboratoire de Biométrie et Biologie Evolutive - UMR 5558 (LBBE), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique (Inria)-VetAgro Sup - Institut national d'enseignement supérieur et de recherche en alimentation, santé animale, sciences agronomiques et de l'environnement (VAS)-Centre National de la Recherche Scientifique (CNRS), Department of Anthropology [University of Arkansas], University of Arkansas [Fayetteville], Hu county ventre for disease control and prevention of Shaanxi province, Istituto Nazionale di Fisica Nucleare, Sezione di Trieste (INFN, Sezione di Trieste), Istituto Nazionale di Fisica Nucleare (INFN), Institut Jean le Rond d'Alembert (DALEMBERT), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of Reading (UOR), Departamento de Matemática Aplicada, Universidade de Santiago de Compostela [Spain] (USC ), Osservatorio Astrofisico di Catania, Équipe Robotique et InteractionS (LAAS-RIS), Laboratoire d'analyse et d'architecture des systèmes (LAAS), Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT), Centro Euro-Mediterraneo per i Cambiamenti Climatici [Bologna] (CMCC), Institut für Theoretische Physik, Universität Heidelberg [Heidelberg] = Heidelberg University, Augsburg Hospital, Leibniz-Institut für Astrophysik Potsdam (AIP), Daimler Chrysler AG (Daimler), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Montserrat Volcano Observatory (MVO), Institut Armand Frappier (INRS-IAF), Institut National de la Recherche Scientifique [Québec] (INRS)-Réseau International des Instituts Pasteur (RIIP), Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], FICLIT, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Max-Planck-Institut für Radioastronomie (MPIFR), Argelander-Institut für Astronomie (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Christian-Albrechts-Universität zu Kiel (CAU), Dipartimento di Fisica e Astronomia 'Galileo Galilei', Università degli Studi di Padova = University of Padua (Unipd), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Cahill Center for Astronomy and Astrophysics, California Institute of Technology (CALTECH), Xinjiang Astronomical Observatory, Mitsubishi Electric Research Laboratories (MERL), Mitsubishi Research Institute, Inc., School of Urban and Regional Planning, University of Southern California (USC), National University of Defense Technology [China], Princeton University, Department of Microtechnology and Nanoscience (MC2), Chalmers University of Technology [Gothenburg, Sweden], Feroci, M., Bozzo, E., Brandt, S., Hernanz, M., van der Klis, M., Liu, L., Orleanski, P., Pohl, M., Santangelo, A., Schanne, S., Stella, L., Takahashi, T., Tamura, H., Watts, A., Wilms, J., Zane, S., Zhang, S., Bhattacharyya, S., Agudo, I., Ahangarianabhari, M., Albertus, C., Alford, M., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, N., Antonelli, A., Argan, A., Artigue, R., Artigues, B., Atteia, J., Azzarello, P., Bakala, P., Ballantyne, D., Baldazzi, G., Baldo, M., Balman, S., Barbera, M., van Baren, C., Barret, D., Baykal, A., Begelman, M., Behar, E., Behar, O., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bode, M., Bodin, P., Bombaci, I., Bonnet Bidaud, J., Boutloukos, S., Bouyjou, F., Bradley, L., Braga, J., Briggs, M., Brown, E., Buballa, M., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz Jørgensen, C., Cackett, E., Cadoux, F., Cais, P., Caliandro, G., Campana, R., Campana, S., Cao, X., Capitanio, F., Casares, J., Casella, P., Castro Tirado, A., Cavazzuti, E., Cavechi, Y., Celestin, S., Cerda Duran, P., Chakrabarty, D., Chamel, N., Château, F., Chen, C., Chen, Y., Chenevez, J., Chernyakova, M., Coker, J., Cole, R., Collura, A., Coriat, M., Cornelisse, R., Costamante, L., Cros, A., Cui, W., Cumming, A., Cusumano, G., Czerny, B., D'Aì, A., D'Ammando, F., D'Elia, V., Dai, Z., Del Monte, E., De Luca, A., De Martino, D., Dercksen, J., De Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Degenaar, N., den Herder, J., Diebold, S., DI SALVO, T., Dong, Y., Donnarumma, I., Doroshenko, V., Doyle, G., Drake, S., Durant, M., Emmanoulopoulos, D., Enoto, T., Erkut, M., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Fender, R., Feng, H., Ferrari, V., Ferrigno, C., Finger, M., Fraser, G., Frericks, M., Fullekrug, M., Fuschino, F., Gabler, M., Galloway, D., Gálvez Sanchez, J., Gandhi, P., Gao, Z., Garcia Berro, E., Gendre, B., Gevin, O., Gezari, S., Giles, A., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gou, L., Gouiffes, C., Grandi, P., Grassi, M., Greiner, J., Grinberg, V., Groot, P., Gschwender, M., Gualtieri, L., Guedel, M., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hamuguchi, K., Hansen, F., Hartmann, D., Haswell, C., Hebeler, K., Heger, A., Hempel, M., Hermsen, W., Homan, J., Hornstrup, A., Hudec, R., Huovelin, J., Huppenkothen, D., Inam, S., Ingram, A., In't Zand, J., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H., Jetter, F., Johannsen, T., Jenke, P., Jonker, P., Josè, J., Kaaret, P., Kalamkar, K., Kalemci, E., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Koerding, E., Kokkotas, K., Komossa, S., Korpela, S., Kouveliotou, C., Kowalski, A., Kreykenbohm, I., Kuiper, L., Kunneriath, D., Kurkela, A., Kuvvetli, I., La Franca, F., Labanti, C., Lai, D., Lamb, F., Lachaud, C., Laubert, P., Lebrun, F., Li, X., Liang, E., Limousin, O., Lin, D., Linares, M., Linder, D., Lodato, G., Longo, F., Lu, F., Lund, N., Maccarone, T., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Malzac, J., Malone, C., Mandel, I., Mangano, V., Manousakis, A., Marelli, M., Margueron, J., Marisaldi, M., Markoff, S., Markowitz, A., Marinucci, A., Martindale, A., Martínez, G., Mchardy, I., Medina Tanco, G., Mehdipour, M., Melatos, A., Mendez, M., Mereghetti, S., Migliari, S., Mignani, R., Michalska, M., Mihara, T., Miller, M., Miller, J., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Mouret, G., Mulačová, J., Muleri, F., Muñoz Darias, T., Negueruela, I., Neilsen, J., Neubert, T., Norton, A., Nowak, M., Nucita, A., O'Brien, P., Oertel, M., Olsen, P., Orienti, M., Orio, M., Orlandini, M., Osborne, J., Osten, R., Ozel, F., Pacciani, L., Paerels, F., Paltani, S., Paolillo, M., Papadakis, I., Papitto, A., Paragi, Z., Paredes, J., Patruno, A., Paul, B., Pederiva, F., Perinati, E., Pellizzoni, A., Penacchioni, A., Peretz, U., Perez, M., Perez Torres, M., Peterson, B., Petracek, V., Pittori, C., Pons, J., Portell, J., Possenti, A., Postnov, K., Poutanen, J., Prakash, M., Prandoni, I., Le Provost, H., Psaltis, D., Pye, J., Qu, J., Rambaud, D., Ramon, P., Ramsay, G., Rapisarda, M., Rashevski, A., Rashevskaya, I., Ray, P., Rea, N., Reddy, S., Reig, P., Reina Aranda, M., Remillard, R., Reynolds, C., Rezzolla, L., Ribo, M., de la Rie, R., Riggio, A., Rios, A., Rischke, D., Rodríguez Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E., Rozanska, A., Rousseau, A., Rudak, B., Russell, D., Ryde, F., Sabau Graziati, L., Sakamoto, T., Sala, G., Salvaterra, R., Salvetti, D., Sanna, A., Sandberg, J., Savolainen, T., Scaringi, S., Schaffner Bielich, J., Schatz, H., Schee, J., Schmid, C., Serino, M., Shakura, N., Shore, S., Schnittman, J., Schneider, R., Schwenk, A., Schwope, A., Sedrakian, A., Seyler, J., Shearer, A., Slowikowska, A., Sims, M., Smith, A., Smith, D., Smith, P., Sobolewska, M., Sochora, V., Soffitta, P., Soleri, P., Song, L., Spencer, A., Stamerra, A., Stappers, B., Staubert, R., Steiner, A., Stergioulas, N., Stevens, A., Stratta, G., Strohmayer, T., Stuchlik, Z., Suchy, S., Suleimanov, V., Tamburini, F., Tauris, T., Tavecchio, F., Tenzer, C., Thielemann, F., Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J., Torres, D., Torresi, E., Tramacere, A., Traulsen, I., Trois, A., Turolla, R., Turriziani, S., Typel, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vietri, M., Vincent, F., Vrba, V., Walton, D., Wang, J., Wang, Z., Watanabe, S., Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, M., Wilson Hodge, C., Winter, B., Walk, S., Wood, K., Woosley, S., Wu, X., Xu, R., Yu, W., Yuan, F., Yuan, W., Yuan, Y., Zampa, G., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zech, A., Zhang, B., Zhang, C., Zingale, M., Zwart, F., University of Geneva [Switzerland], Eberhard Karls Universität Tübingen, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Graduate School of the Natural Science and Technology, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), School of BioSciences [Melbourne], University of Melbourne-University of Melbourne-Royal Melbourne Institute of Technology University (RMIT University)-University of Queensland [Brisbane]-Australian National University (ANU)-The University of Western Australia (UWA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université Libre de Bruxelles [Bruxelles] (ULB), Dublin City University, Dublin 9, Ireland, Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), China Information Technology Security Evaluation Center, Technical University of Denmark [Lyngby] (DTU), Université Grenoble Alpes (UGA), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Trieste, Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Institut de Biologie Intégrative de la Cellule (I2BC), Université Paris-Sud - Paris 11 (UP11)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Università degli Studi di Roma 'La Sapienza' [Rome], Radboud university [Nijmegen]-Radboud university [Nijmegen], Radboud university [Nijmegen], Universidad de Granada (UGR), Centre National de la Recherche Scientifique (CNRS), Centre de recherche en Biologie Cellulaire (CRBM), Université Montpellier 1 (UM1)-Université Montpellier 2 - Sciences et Techniques (UM2)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Università degli studi di Catania [Catania], Laboratoire d'Ecologie Alpine (LECA), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA), Centre National de la Recherche Scientifique (CNRS)-Université du Littoral Côte d'Opale, Stanford University [Stanford], Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Aix Marseille Université (AMU), Università degli studi di Napoli Federico II, IFP Energies nouvelles (IFPEN), National Institute for Nuclear Physics (INFN), Institut Jean Le Rond d'Alembert (DALEMBERT), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J), Ingénierie des Matériaux Polymères (IMP), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet [Saint-Étienne] (UJM)-Centre National de la Recherche Scientifique (CNRS), Centro Euro-Mediterraneo per i Cambiamenti Climatici (CMCC), Universität Heidelberg [Heidelberg], Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Réseau International des Instituts Pasteur (RIIP)-Institut National de la Recherche Scientifique [Québec] (INRS), Università di Bologna [Bologna] (UNIBO), University of California [Berkeley], University of California-University of California, Universita degli Studi di Padova, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Chalmers University of Technology [Göteborg], Astronomy, Jan-Willem A. den Herder, Shouleh Nikzad, Kazuhiro Nakazawa, Van Der Klis, M., Liu, L. -P., Zhang, S. -N., Atteia, J. -L., Ballantyne, D. R., Van Baren, C., Bellutti, P., Bonnet Bidaud, J. -M., Borghi, G., Briggs, M. S., Budtz-Jorgensen, C., Cadoux, F. R., Caliandro, G. A., Castro-Tirado, A. J., Cerda-Duran, P., Chateau, F., D'Ai, A., Dercksen, J. P. C., Den Herder, J. W., Di Salvo, T., Drake, S. A., Erkut, M. H., Ficorella, F., Finger, M. H., Fraser, G. W., Galloway, D. K., Galvez Sanchez, J. L., Garcia-Berro, E., Giles, A. B., Goluchova, K., Gotz, D., Hartmann, D. H., Haswell, C. A., Inam, S. C., In'Tzand, J. J. M., Jacobs, H. M., Jenke, P. A., Jose, J., Kalamkar, M., Kowalski, A. F., Kuiper, L. M., Lamb, F. K., Laubert, P. P., Maccarone, T. J., Markoff, S. B., Martinez, G., Mchardy, I. M., Medina-Tanco, G., Miller, M. C., Miller, J. M., Mulacova, J., Munoz-Darias, T., Norton, A. J., Olsen, P. E. H., Osborne, J. P., Paredes, J. M., Penacchioni, A. V., Perez, M. A., Perez-Torres, M., Peterson, B. M., Picciotto, A., Piemonte, C., Rachevski, A., Ray, P. S., De La Rie, R., Rischke, D. H., Rodriguez-Gil, P., Rossi, E. M. R., Russell, D. M., Sabau-Graziati, L., Schaffner-Bielich, J., Schnittman, J. D., Schwope, A. D., Seyler, J. -Y., Smith, D. M., Smith, P. J., Steiner, A. W., Stevens, A. L., Strohmayer, T. E., Thielemann, F. K., Torrejon, J. M., Torres, D. F., Vincent, F. H., Wilson-Hodge, C. A., Walk, S. J., Woosley, S. E., Xiao, L., Zorzi, N., Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Institut de Chimie du CNRS (INC)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Montpellier 2 - Sciences et Techniques (UM2)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Université Montpellier 1 (UM1), Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Muséum national d'Histoire naturelle (MNHN), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Institut de Chimie du CNRS (INC), Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Department of Psychiatry (Icahn School of Medicine at Mount Sinai) ( ISMMS ), Rutgers, The State University of New Jersey [New Brunswick] ( RUTGERS ), Institut fur Astronomie und Astrophysik, Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Kanazawa University ( KU ), Department of Earth Sciences, University of Oxford [Oxford], Centre Interdisciplinaire de Nanoscience de Marseille ( CINaM ), Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ), Tampere University of Technology [Tampere] ( TUT ), University of Southern Mississippi ( USM ), University of Southampton [Southampton], Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano ( IASF-MI ), Istituto Nazionale di Astrofisica ( INAF ), Istituto di Astrofisica e Planetologia Spaziali ( IAPS ), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées ( LATT ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Swedish Institute of Space Physics [Uppsala] ( IRF ), Osservatorio Astronomico di Brera ( INAF ), Bibliothèque nationale de France ( BnF ), Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo ( IASF-Pa ), ARC Centre of Excellence for Environmental Decisions ( ARC CEED ), The University of Western Australia ( UWA ) -Australian National University ( ANU ) -University of Queensland [Brisbane]-RMIT University [Melbourne]-University of Melbourne, ARC Centre of Excellence for Coral Reef Studies ( CoralCoE ), James Cook University ( JCU ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Anthropologie Moléculaire et Imagerie de Synthèse ( AMIS ), PRES Université de Toulouse-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de synthèse organique ( DCSO ), École polytechnique ( X ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Pathology, University of Alabama at Birmingham, University of Alabama at Birmingham Comprehensive Cancer Center, Birmingham, Alabama, INAF-Osservatorio di Cagliari, Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Théorique et Modèles Statistiques ( LPTMS ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Université Libre de Bruxelles [Bruxelles] ( ULB ), Ocean and Earth Sciences, National Oceanography Centre Southampton, Dublin Institute for advanced studies, 31 Fitzwilliam Place, Dublin 2, Ireland, Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Institut Parisien de Chimie Moléculaire ( IPCM ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Chinese Academy of Sciences [Beijing] ( CAS ), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Applied Mathematics and Computer Science [Lyngby] ( DTU Compute ), Technical University of Denmark [Lyngby] ( DTU ), Institut für Astronomie und Astrophysik ( IAAT ), Anton Pannekoek Institute for Astronomy, University of Amsterdam, University of Cambridge [UK] ( CAM ), International Space Science Institute ( ISSI ), Université Grenoble Alpes - UFR Médecine ( UGA UFRM ), Université Grenoble Alpes ( UGA ), Institute of Perception, Action and Behaviour ( IPAB ), United States Geological Survey [Reston] ( USGS ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Max-Planck-Institut für Extraterrestrische Physik ( MPE ), Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology ( MIT ), Institut de Physique du Globe de Paris ( IPGP ), Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Biologie Intégrative de la Cellule ( I2BC ), Université Paris-Sud - Paris 11 ( UP11 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Centre National de la Recherche Scientifique ( CNRS ), Matériaux, ingénierie et science [Villeurbanne] ( MATEIS ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ) -Institut National des Sciences Appliquées de Lyon ( INSA Lyon ), Université de Lyon-Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ), University of Wisconsin-Madison [Madison], SRON Netherlands Institute for Space Research ( SRON ), University of Technology ( Opole ), Institute for Mathematics, Astrophysics and Particle Physics ( IMAPP ), Grp Fis Atmosfera, Ctr Andaluz Medio Ambiente CEAMA, Universidad de Granada ( UGR ), The Hong Kong Polytechnic University [Hong Kong] ( POLYU ), Chinese Academy of Sciences [Changchun Branch] ( CAS ), Department of Physics, Chemistry and Biology, Linköping University ( LIU ), Institut de Chimie des Substances Naturelles ( ICSN ), Centre National de la Recherche Scientifique ( CNRS ), Institut de Physique Nucléaire de Lyon ( IPNL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Astronomical Institute Anton Pannekoek ( AI PANNEKOEK ), University of Amsterdam [Amsterdam] ( UvA ), Erlangen Centre for Astroparticle Physics ( ECAP ), Friedrich-Alexander Universität Erlangen-Nürnberg ( FAU ), Centre de recherches de biochimie macromoléculaire ( CRBM ), Université Montpellier 1 ( UM1 ) -Université Montpellier 2 - Sciences et Techniques ( UM2 ) -Université de Montpellier ( UM ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto Nacional de Pesquisas da Amazônia ( INPA ), Instituto Nacional de Pesquisas da Amazônia, Centre d'Ecologie et des Sciences de la COnservation ( CESCO ), Muséum National d'Histoire Naturelle ( MNHN ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Ecologie Alpine ( LECA ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physico-Chimie de l'Atmosphère ( LPCA ), Université du Littoral Côte d'Opale-Centre National de la Recherche Scientifique ( CNRS ), Institut des Sciences Moléculaires de Marseille ( ISM2 ), Aix Marseille Université ( AMU ) -Ecole Centrale de Marseille ( ECM ) -Centre National de la Recherche Scientifique ( CNRS ), Space Telescope Science Institute ( STSci ), IFP Energies nouvelles ( IFPEN ), Laboratoire de Biométrie et Biologie Evolutive ( LBBE ), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique ( Inria ) -Centre National de la Recherche Scientifique ( CNRS ), University of Arkansas, Istituto Nazionale di Fisica Nucleare, Sezione di Trieste ( INFN, Sezione di Trieste ), National Institute for Nuclear Physics ( INFN ), Institut Jean Le Rond d'Alembert ( DALEMBERT ), Institut de Ciencies de l'Espai [Barcelona] ( ICE-CSIC ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), University of Reading ( UOR ), Universidade de Santiago de Compostela, Équipe Robotique et InteractionS ( LAAS-RIS ), Laboratoire d'analyse et d'architecture des systèmes [Toulouse] ( LAAS ), Institut National Polytechnique [Toulouse] ( INP ) -Institut National des Sciences Appliquées - Toulouse ( INSA Toulouse ), Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Université Paul Sabatier - Toulouse 3 ( UPS ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National Polytechnique [Toulouse] ( INP ) -Institut National des Sciences Appliquées - Toulouse ( INSA Toulouse ), Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Université Paul Sabatier - Toulouse 3 ( UPS ) -Centre National de la Recherche Scientifique ( CNRS ), Ingénierie des Matériaux Polymères - Site INSA Lyon ( IMP ), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon ( INSA Lyon ), Université de Lyon-Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Université Jean Monnet [Saint-Étienne] ( UJM ) -Centre National de la Recherche Scientifique ( CNRS ), Leibniz-Institut für Astrophysik Potsdam ( AIP ), Daimler Chrysler AG ( Daimler ), Centre d'Etudes Nucléaires de Bordeaux Gradignan ( CENBG ), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Montserrat Volcano Observatory ( MVO ), Institut Armand Frappier ( INRS-IAF ), Institut National de la Recherche Scientifique [Québec] ( INRS ) -Réseau International des Instituts Pasteur ( RIIP ) -Institut Armand Frappier, Università di Bologna [Bologna] ( UNIBO ), Max-Planck-Institut für Radioastronomie, Argelander Institut für Astronomie, Bonn Universität [Bonn], Space Sciences Laboratory [Berkeley] ( SSL ), Christian-Albrechts-Universität zu Kiel ( CAU ), Universita degli Studi di Padova = University of Padua = Université de Padoue, APC - Gravitation ( APC-Gravitation ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, California Institute of Technology ( CALTECH ), Mitsubishi Electric Research Laboratories ( MERL ), Mitsubishi Electric Research Laboratories, Institute for Astronomy, University of Amsterdam, The Netherland, University of Southern California ( USC ), National University of Defense Technology [Changsha], Department of Microtechnology and Nanoscience ( MC2 ), Université Chalmers, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Nice Sophia Antipolis (UNS), Université Paris-Sud - Paris 11 (UP11)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Centre National de la Recherche Scientifique (CNRS), Den Herder, Jan-Willem A., Bautz, M., den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Jan-Willem A. den Herder, Tadayuki Takahashi, Marshall Bautz, Liu, L. P., Zhang, S. N., Atteia, J. L., Bonnet Bidaud, J. M., Castro Tirado, A. J., D'Aı, A., den Herder, J. W., Gálvez Sanchez, J. L., In't Zand, J. J. M., Nucita, Achille, Seyler, J. Y., Wilson Hodge, C. A., Baldazzi, Giuseppe, Fuschino, Fabio, Bianchi, Stefano, Casella, Piergiorgio, DE ROSA, Alessandra, Giovannini, Gabriele, LA FRANCA, Fabio, Marinucci, Andrea, Paredes, M. J., Schneider, Raffaella, Vietri, Mario, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), M., Feroci, E., Bozzo, S., Brandt, M., Hernanz, M., van der Kli, L. P., Liu, P., Orleanski, M., Pohl, A., Santangelo, S., Schanne, L., Stella, T., Takahashi, H., Tamura, A., Watt, J., Wilm, S., Zane, S. N., Zhang, S., Bhattacharyya, I., Agudo, M., Ahangarianabhari, C., Albertu, M., Alford, A., Alpar, D., Altamirano, L., Alvarez, L., Amati, C., Amoro, N., Andersson, A., Antonelli, A., Argan, R., Artigue, B., Artigue, J. L., Atteia, P., Azzarello, P., Bakala, D., Ballantyne, G., Baldazzi, M., Baldo, S., Balman, M., Barbera, C., van Baren, D., Barret, A., Baykal, M., Begelman, E., Behar, O., Behar, T., Belloni, F., Bernardini, G., Bertuccio, S., Bianchi, A., Bianchini, P., Binko, P., Blay, F., Bocchino, M., Bode, P., Bodin, I., Bombaci, J. M., Bonnet Bidaud, S., Boutlouko, F., Bouyjou, L., Bradley, J., Braga, M. S., Brigg, E., Brown, M., Buballa, N., Bucciantini, L., Burderi, M., Burgay, M., Bursa, C., Budtz Jørgensen, E., Cackett, F., Cadoux, P., Cai, G. A., Caliandro, R., Campana, S., Campana, X., Cao, F., Capitanio, J., Casare, P., Casella, A. J., Castro Tirado, E., Cavazzuti, Y., Cavechi, S., Celestin, P., Cerda Duran, D., Chakrabarty, N., Chamel, F., Château, C., Chen, Y., Chen, J., Chenevez, M., Chernyakova, J., Coker, R., Cole, A., Collura, M., Coriat, R., Cornelisse, L., Costamante, A., Cro, W., Cui, A., Cumming, G., Cusumano, B., Czerny, A., D'Aì, F., D'Ammando, V., D'Elia, Z., Dai, E., Del Monte, A., De Luca, D., De Martino, J. P. C., Dercksen, M., De Pasquale, A., De Rosa, M., Del Santo, S., Di Cosimo, N., Degenaar, J. W., den Herder, S., Diebold, T., Di Salvo, Y., Dong, I., Donnarumma, V., Doroshenko, G., Doyle, S. A., Drake, M., Durant, D., Emmanoulopoulo, T., Enoto, M. H., Erkut, P., Esposito, Y., Evangelista, A., Fabian, M., Falanga, Y., Favre, C., Feldman, R., Fender, H., Feng, V., Ferrari, C., Ferrigno, M., Finger, M. H., Finger, G. W., Fraser, M., Frerick, M., Fullekrug, F., Fuschino, M., Gabler, D. K., Galloway, J. L., Gálvez Sanchez, P., Gandhi, Z., Gao, E., Garcia Berro, B., Gendre, O., Gevin, S., Gezari, A. B., Gile, M., Gilfanov, P., Giommi, G., Giovannini, M., Giroletti, E., Gogu, A., Goldwurm, K., Goluchová, D., Götz, L., Gou, C., Gouiffe, P., Grandi, M., Grassi, J., Greiner, V., Grinberg, P., Groot, M., Gschwender, L., Gualtieri, M., Guedel, C., Guidorzi, L., Guy, D., Haa, P., Haensel, M., Hailey, K., Hamuguchi, F., Hansen, D. H., Hartmann, C. A., Haswell, K., Hebeler, A., Heger, M., Hempel, W., Hermsen, J., Homan, A., Hornstrup, R., Hudec, J., Huovelin, D., Huppenkothen, S. C., Inam, A., Ingram, J. J. M., In't Zand, G., Israel, K., Iwasawa, L., Izzo, H. M., Jacob, F., Jetter, T., Johannsen, P. A., Jenke, P., Jonker, J., Josè, P., Kaaret, K., Kalamkar, E., Kalemci, G., Kanbach, V., Kara, D., Karelin, D., Kataria, L., Keek, T., Kennedy, D., Klochkov, W., Kluzniak, E., Koerding, K., Kokkota, S., Komossa, S., Korpela, C., Kouveliotou, A. F., Kowalski, I., Kreykenbohm, L. M., Kuiper, D., Kunneriath, A., Kurkela, I., Kuvvetli, F., La Franca, C., Labanti, D., Lai, F. K., Lamb, C., Lachaud, P. P., Laubert, F., Lebrun, X., Li, E., Liang, O., Limousin, D., Lin, M., Linare, D., Linder, G., Lodato, F., Longo, F., Lu, N., Lund, T. J., Maccarone, D., Macera, S., Maestre, S., Mahmoodifar, D., Maier, P., Malcovati, J., Malzac, C., Malone, I., Mandel, V., Mangano, A., Manousaki, M., Marelli, J., Margueron, M., Marisaldi, S. B., Markoff, A., Markowitz, A., Marinucci, A., Martindale, G., Martínez, I. M., Mchardy, G., Medina Tanco, M., Mehdipour, A., Melato, M., Mendez, S., Mereghetti, S., Migliari, R., Mignani, M., Michalska, T., Mihara, M. C., Miller, J. M., Miller, T., Mineo, G., Miniutti, S., Morsink, C., Motch, S., Motta, M., Mouchet, G., Mouret, J., Mulačová, F., Muleri, T., Muñoz Daria, I., Negueruela, J., Neilsen, T., Neubert, A. J., Norton, M., Nowak, A., Nucita, P., O'Brien, M., Oertel, P. E. H., Olsen, M., Orienti, M., Orio, M., Orlandini, J. 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Subjects: X-ray timing, [ SDU.ASTR.GA ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Field of view, Astrophysics, 01 natural sciences, law.invention, law, Observatory, timing, 010303 astronomy & astrophysics, QB, Physics, microchannel plates. PROPORTIONAL COUNTER ARRAY, CALIBRATION, X-ray astronomy, Electronic, Optical and Magnetic Material, Applied Mathematics, Astrophysics::Instrumentation and Methods for Astrophysics, Computer Science Applications1707 Computer Vision and Pattern Recognition, X-ray detectors, Condensed Matter Physics, compact objects, X-ray spectroscopy, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], spectroscopy, Cosmic Vision, [ INFO ] Computer Science [cs], Silicon detector, Astrophysics::High Energy Astrophysical Phenomena, Condensed Matter Physic, Telescope, X-ray, Silicon detectors, Electronic, Optical and Magnetic Materials, Electrical and Electronic Engineering, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Electronic, [INFO]Computer Science [cs], Optical and Magnetic Materials, Spectral resolution, DETECTOR, ta115, X-ray astronomy, Silicon detectors, timing, spectroscopy, 010308 nuclear & particles physics, X-ray imaging, Applied Mathematic, Neutron star, QB460-466 Astrophysics, Large Observatory For x-ray Timing (LOFT), Large Area Detector (LAD), Wide Field Monitor (WFM), Large Area Silicon Drift Detectors (SDD), Gamma-ray burst
Abstract: The Large Observatory For x-ray Timing (LOFT) is a mission concept which was proposed to ESA as M3 and M4 candidate in the framework of the Cosmic Vision 2015-2025 program. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument and the uniquely large field of view of its wide field monitor, LOFT will be able to study the behaviour of matter in extreme conditions such as the strong gravitational field in the innermost regions close to black holes and neutron stars and the supra-nuclear densities in the interiors of neutron stars. The science payload is based on a Large Area Detector (LAD, >8m2 effective area, 2-30 keV, 240 eV spectral resolution, 1 degree collimated field of view) and a Wide Field Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g., GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the current technical and programmatic status of the mission. © (2016) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Published: 2016

48. SGR J1550-5418 Bursts Detected with the Fermi Gamma-Ray Burst Monitor during its Most Prolific Activity

Author: Asaf Pe'er, Arne Rau, Chryssa Kouveliotou, Ersin Gogus, David Gruber, Matthew G. Baring, Adam Goldstein, A. von Kienlin, Jonathan Granot, Robert D. Preece, Charles A. Meegan, Paul M. Woods, Lex Kaper, Elisabetta Bissaldi, A. J. van der Horst, Misty Giles, Mark H. Finger, Anna L. Watts, W. S. Paciesas, P. N. Bhat, Yuki Kaneko, M. van der Klis, Sylvain Guiriec, Enrico Ramirez-Ruiz, Alice K. Harding, Julie McEnery, Neil Gehrels, N. M. Gorgone, Ralph A. M. J. Wijers, Colleen A. Wilson-Hodge, Vandiver Chaplin, Lin Lin, Melissa Gibby, Sheila McBreen, Stefanie Wachter, A. J., van der Horst, C., Kouveliotou, N. M., Gorgone, Y., Kaneko, M. G., Baring, S., Guiriec, E., Gogu, J., Granot, A. L., Watt, L., Lin, P. N., Bhat, Bissaldi, Elisabetta, V. L., Chaplin, M. H., Finger, N., Gehrel, M. H., Gibby, M. M., Gile, A., Goldstein, D., Gruber, A. K., Harding, L., Kaper, A., von Kienlin, M., van der Kli, S., Mcbreen, J., Mcenery, C. A., Meegan, W. S., Paciesa, A., Pe'Er, R. D., Preece, E., Ramirez Ruiz, A., Rau, S., Wachter, C., Wilson Hodge, P. M., Wood, R. A. M. J., Wijers, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, PSR J1550-5418), FOS: Physical sciences, Context (language use), Astrophysics, Magnetar, 01 natural sciences, 7. Clean energy, Spectral line, 1E 1547.0-5408, individual: SGR J1550–5418 1E 1547.0–5408 PSR J1550–5418 [pulsars], stars: neutron, X-rays: bursts, pulsars: individual: SGR J1550–5418 1E 1547.0–5408 PSR J1550–5418, neutron [stars], 0103 physical sciences, Black-body radiation, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Bremsstrahlung, Astronomy and Astrophysics, Neutron star, 13. Climate action, Space and Planetary Science, Pulsars: individual (SGR J1550-5418, burst [X-rays], Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, Pulsars: individual (SGR J1550-5418, 1E 1547.0-5408, PSR J1550-5418), Fermi Gamma-ray Space Telescope
Abstract: We have performed detailed temporal and time-integrated spectral analysis of 286 bursts from SGR J1550-5418 detected with the Fermi Gamma-ray Burst Monitor (GBM) in January 2009, resulting in the largest uniform sample of temporal and spectral properties of SGR J1550-5418 bursts. We have used the combination of broadband and high time-resolution data provided with GBM to perform statistical studies for the source properties. We determine the durations, emission times, duty cycles and rise times for all bursts, and find that they are typical of SGR bursts. We explore various models in our spectral analysis, and conclude that the spectra of SGR J1550-5418 bursts in the 8-200 keV band are equally well described by optically thin thermal bremsstrahlung (OTTB), a power law with an exponential cutoff (Comptonized model), and two black-body functions (BB+BB). In the spectral fits with the Comptonized model we find a mean power-law index of -0.92, close to the OTTB index of -1. We show that there is an anti-correlation between the Comptonized Epeak and the burst fluence and average flux. For the BB+BB fits we find that the fluences and emission areas of the two blackbody functions are correlated. The low-temperature BB has an emission area comparable to the neutron star surface area, independent of the temperature, while the high-temperature blackbody has a much smaller area and shows an anti-correlation between emission area and temperature. We compare the properties of these bursts with bursts observed from other SGR sources during extreme activations, and discuss the implications of our results in the context of magnetar burst models., 13 pages, 10 figures, 2 tables; minor changes, ApJ in press
Published: 2012

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