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1. INTEGRAL reloaded: Spacecraft, instruments and ground system

Author: Kuulkers, Erik, Ferrigno, Carlo, Kretschmar, Peter, Alfonso-Garzón, Julia, Baab, Marius, Bazzano, Angela, Bélanger, Guillaume, Benson, Ian, Bird, Antony J., Bozzo, Enrico, Brandt, Søren, Coe, Elliott, Caballero, Isabel, Cangemi, Floriane, Chenevez, Jérôme, Cenko, Bradley, Cinar, Nebil, Coleiro, Alexis, De Padova, Stefano, Diehl, Roland, Dietze, Claudia, Domingo, Albert, Drapes, Mark, D’uva, Eleonora, Ehle, Matthias, Ebrero, Jacobo, Edirimanne, Mithrajith, Eismont, Natan A., Finn, Timothy, Fiocchi, Mariateresa, Tomas, Elena Garcia, Gaudenzi, Gianluca, Godard, Thomas, Goldwurm, Andrea, Götz, Diego, Gouiffès, Christian, Grebenev, Sergei A., Greiner, Jochen, Gros, Aleksandra, Hajdas, Wojciech, Hanlon, Lorraine, Hermsen, Wim, Hernández, Cristina, Hernanz, Margarita, Hübner, Jutta, Jourdain, Elisabeth, La Rosa, Giovanni, Labanti, Claudio, Laurent, Philippe, Lehanka, Alexander, Lund, Niels, Madison, James, Malzac, Julien, Martin, Jim, Mas-Hesse, J. Miguel, McBreen, Brian, McDonald, Alastair, McEnery, Julie, Mereghetti, Sandro, Natalucci, Lorenzo, Ness, Jan-Uwe, Oxborrow, Carol Anne, Palmer, John, Peschke, Sibylle, Petrucciani, Francesco, Pfeil, Norbert, Reichenbaecher, Michael, Rodi, James, Rodriguez, Jérôme, Roques, Jean-Pierre, Doñate, Emilio Salazar, Salt, Dave, Sánchez-Fernández, Celia, Sauvageon, Aymeric, Savchenko, Volodymyr, Sazonov, Sergey Yu., Scaglioni, Stefano, Schartel, Norbert, Siegert, Thomas, Southworth, Richard, Sunyaev, Rashid A., Toma, Liviu, Ubertini, Pietro, van den Heuvel, Edward P.J., von Kienlin, Andreas, von Krusenstiern, Nikolai, Winkler, Christoph, and Zannoni, Ugo
Published: 2021
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2. Unsung Psychology Pioneers: A Content Analysis of Who Makes History (and Who Doesn't)

Author: Alvarez, Leslie D. Cramblet, Leach, Jonah L., Rodriguez, Jerome L., and Jones, K. Nicole
Published: 2020
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3. Advances in Understanding High-Mass X-ray Binaries with INTEGRALand Future Directions

Author: Kretschmar, Peter, Fürst, Felix, Sidoli, Lara, Bozzo, Enrico, Alfonso-Garzón, Julia, Bodaghee, Arash, Chaty, Sylvain, Chernyakova, Masha, Ferrigno, Carlo, Manousakis, Antonios, Negueruela, Ignacio, Postnov, Konstantin, Paizis, Adamantia, Reig, Pablo, Rodes-Roca, José Joaquín, Tsygankov, Sergey, Bird, Antony J., Bissinger né Kühnel, Matthias, Blay, Pere, Caballero, Isabel, Coe, Malcolm J., Domingo, Albert, Doroshenko, Victor, Ducci, Lorenzo, Falanga, Maurizio, Grebenev, Sergei A., Grinberg, Victoria, Hemphill, Paul, Kreykenbohm, Ingo, Kreykenbohm né Fritz, Sonja, Li, Jian, Lutovinov, Alexander A., Martínez-Núñez, Silvia, Mas-Hesse, J. Miguel, Masetti, Nicola, McBride, Vanessa A., Neronov, Andrii, Pottschmidt, Katja, Rodriguez, Jérôme, Romano, Patrizia, Rothschild, Richard E., Santangelo, Andrea, Sguera, Vito, Staubert, Rüdiger, Tomsick, John A., Torrejón, José Miguel, Torres, Diego F., Walter, Roland, Wilms, Jörn, Wilson-Hodge, Colleen A., and Zhang, Shu
Published: 2019
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4. INTEGRAL results on gamma-ray bursts and polarization of hard X-ray sources

Author: Götz, Diego, Gouiffès, Christian, Rodriguez, Jérôme, Laurent, Philippe, Jourdain, Elisabeth, Roques, Jean-Pierre, Mereghetti, Sandro, Lutovinov, Alexander, Savchenko, Volodymyr, Hanlon, Lorraine, Martin-Carrillo, Antonio, and Moran, Paul
Published: 2019
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5. Accretion in strong field gravity with eXTP

Author: Rosa, Alessandra De, Uttley, Phil, Gou, LiJun, Liu, Yuan, Bambi, Cosimo, Barret, Didier, Belloni, Tomaso, Berti, Emanuele, Bianchi, Stefano, Caiazzo, Ilaria, Casella, Piergiorgio, Feroci, Marco, Ferrari, Valeria, Gualtieri, Leonardo, Heyl, Jeremy, Ingram, Adam, Karas, Vladimir, Lu, FangJun, Luo, Bin, Matt, Giorgio, Motta, Sara, Neilsen, Joseph, Pani, Paolo, Santangelo, Andrea, Shu, XinWen, Wang, JunFeng, Wang, Jian-Min, Xue, YongQuan, Xu, YuPeng, Yuan, WeiMin, Yuan, YeFei, Zhang, Shuang-Nan, Zhang, Shu, Agudo, Ivan, Amati, Lorenzo, Andersson, Nils, Baglio, Cristina, Bakala, Pavel, Baykal, Altan, Bhattacharyya, Sudip, Bombaci, Ignazio, Bucciantini, Niccoló, Capitanio, Fiamma, Ciolfi, Riccardo, Cui, Wei K., D’Ammando, Filippo, Dauser, Thomas, Del Santo, Melania, De Marco, Barbara, Di Salvo, Tiziana, Done, Chris, Dovčiak, Michal, Fabian, Andrew C., Falanga, Maurizio, Gambino, Angelo Francesco, Gendre, Bruce, Grinberg, Victoria, Heger, Alexander, Homan, Jeroen, Iaria, Rosario, Jiang, JiaChen, Jin, ChiChuan, Koerding, Elmar, Linares, Manu, Liu, Zhu, Maccarone, Thomas J., Malzac, Julien, Manousakis, Antonios, Marin, Frédéric, Marinucci, Andrea, Mehdipour, Missagh, Méndez, Mariano, Migliari, Simone, Miller, Cole, Miniutti, Giovanni, Nardini, Emanuele, O’Brien, Paul T., Osborne, Julian P., Petrucci, Pierre Olivier, Possenti, Andrea, Riggio, Alessandro, Rodriguez, Jerome, Sanna, Andrea, Shao, LiJing, Sobolewska, Malgosia, Sramkova, Eva, Stevens, Abigail L., Stiele, Holger, Stratta, Giulia, Stuchlik, Zdenek, Svoboda, Jiri, Tamburini, Fabrizio, Tauris, Thomas M., Tombesi, Francesco, Torok, Gabriel, Urbanec, Martin, Vincent, Frederic, Wu, QingWen, Yuan, Feng, in’ t Zand, Jean J. M., Zdziarski, Andrzej A., and Zhou, XinLin
Published: 2018
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6. The enhanced X-ray Timing and Polarimetry mission—eXTP

Author: Zhang, ShuangNan, Santangelo, Andrea, Feroci, Marco, Xu, YuPeng, Lu, FangJun, Chen, Yong, Feng, Hua, Zhang, Shu, Brandt, Søren, Hernanz, Margarita, Baldini, Luca, Bozzo, Enrico, Campana, Riccardo, De Rosa, Alessandra, Dong, YongWei, Evangelista, Yuri, Karas, Vladimir, Meidinger, Norbert, Meuris, Aline, Nandra, Kirpal, Pan, Teng, Pareschi, Giovanni, Orleanski, Piotr, Huang, QiuShi, Schanne, Stephane, Sironi, Giorgia, Spiga, Daniele, Svoboda, Jiri, Tagliaferri, Gianpiero, Tenzer, Christoph, Vacchi, Andrea, Zane, Silvia, Walton, Dave, Wang, ZhanShan, Winter, Berend, Wu, Xin, in’ t Zand, Jean J. M., Ahangarianabhari, Mahdi, Ambrosi, Giovanni, Ambrosino, Filippo, Barbera, Marco, Basso, Stefano, Bayer, Jörg, Bellazzini, Ronaldo, Bellutti, Pierluigi, Bertucci, Bruna, Bertuccio, Giuseppe, Borghi, Giacomo, Cao, XueLei, Cadoux, Franck, Campana, Riccardo, Ceraudo, Francesco, Chen, TianXiang, Chen, YuPeng, Chevenez, Jerome, Civitani, Marta, Cui, Wei, Cui, WeiWei, Dauser, Thomas, Del Monte, Ettore, Di Cosimo, Sergio, Diebold, Sebastian, Doroshenko, Victor, Dovciak, Michal, Du, YuanYuan, Ducci, Lorenzo, Fan, QingMei, Favre, Yannick, Fuschino, Fabio, Gálvez, José Luis, Gao, Min, Ge, MingYu, Gevin, Olivier, Grassi, Marco, Gu, QuanYing, Gu, YuDong, Han, DaWei, Hong, Bin, Hu, Wei, Ji, Long, Jia, ShuMei, Jiang, WeiChun, Kennedy, Thomas, Kreykenbohm, Ingo, Kuvvetli, Irfan, Labanti, Claudio, Latronico, Luca, Li, Gang, Li, MaoShun, Li, Xian, Li, Wei, Li, ZhengWei, Limousin, Olivier, Liu, HongWei, Liu, XiaoJing, Lu, Bo, Luo, Tao, Macera, Daniele, Malcovati, Piero, Martindale, Adrian, Michalska, Malgorzata, Meng, Bin, Minuti, Massimo, Morbidini, Alfredo, Muleri, Fabio, Paltani, Stephane, Perinati, Emanuele, Picciotto, Antonino, Piemonte, Claudio, Qu, JinLu, Rachevski, Alexandre, Rashevskaya, Irina, Rodriguez, Jerome, Schanz, Thomas, Shen, ZhengXiang, Sheng, LiZhi, Song, JiangBo, Song, LiMing, Sgro, Carmelo, Sun, Liang, Tan, Ying, Uttley, Phil, Wang, Bo, Wang, DianLong, Wang, GuoFeng, Wang, Juan, Wang, LangPing, Wang, YuSa, Watts, Anna L., Wen, XiangYang, Wilms, Jörn, Xiong, ShaoLin, Yang, JiaWei, Yang, Sheng, Yang, YanJi, Yu, Nian, Zhang, WenDa, Zampa, Gianluigi, Zampa, Nicola, Zdziarski, Andrzej A., Zhang, AiMei, Zhang, ChengMo, Zhang, Fan, Zhang, Long, Zhang, Tong, Zhang, Yi, Zhang, XiaoLi, Zhang, ZiLiang, Zhao, BaoSheng, Zheng, ShiJie, Zhou, YuPeng, Zorzi, Nicola, and Zwart, J. Frans
Published: 2018
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7. Observatory science with eXTP

Author: in ’t Zand, Jean J. M., Bozzo, Enrico, Qu, JinLu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, XueFeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, ChiChuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D’Aì, Antonino, Dai, Zi-Gao, D’Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D’Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, XiLong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, MingYu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, FangJun, Lutovinov, Alexander A., Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, YunPeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O’Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, LiJing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jir̆í, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, JunFeng, Watts, Anna L., Weng, ShanShan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, ShaoLin, Xu, YuPeng, Yan, Zhen, Younes, George, Yu, WenFei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, and Zingale, Michael
Published: 2018
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8. Positron annihilation signatures associated with the outburst of the microquasar V404 Cygni

Author: Siegert, Thomas, Diehl, Roland, Greiner, Jochen, Krause, Martin G.H., Beloborodov, Andrei M., Bel, Marion Cadolle, Guglielmetti, Fabrizia, Rodriguez, Jerome, Strong, Andrew W., and Zhang, Xiaoling
Subjects: Black holes (Astronomy) -- Analysis, Positron annihilation -- Analysis, Stars, Double -- Analysis, Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract: Microquasars (1-4) are stellar-mass black holes accreting matter from a companion star (5) and ejecting plasma jets at almost the speed of light. They are analogues of quasars that contain [...]
Published: 2016

9. A Multiwavelength Study of GRS 1716-249 in Outburst

Author: Saikia, Payaswini, Russell, David M., Baglio, M. C., Bramich, D. M., Casella, Piergiorgio, Trigo, Maria Diaz, Gandhi, Poshak, Jiang, Jiachen, Maccarone, Thomas, Soria, Roberto, Al Noori, Hind, Al Yazeedi, Aisha, Alabarta, Kevin, Belloni, Tomaso, Bel, Marion Cadolle, Ceccobello, Chiara, Corbel, Stéphane, Fender, Rob, Gallo, Elena, Homan, Jeroen, Koljonen, Karri, Lewis, Fraser, Markoff, Sera B., Miller-Jones, James C.A., Rodriguez, Jerome, Russell, Thomas D., Shahbaz, Tariq, Sivakoff, Gregory R., Testa, Vincenzo, Tetarenko, Alexandra J., New York University Abu Dhabi, Osservatorio Astronomico Roma, European Southern Observatory, University of Southampton, University of Cambridge, Texas Tech University, University of Chinese Academy of Sciences, University of California Santa Barbara, Osservatorio Astronomico di Brera, Chalmers University of Technology, IRFM-CEA, University of Oxford, University of Michigan, Ann Arbor, Eureka Scientific, Inc., Metsähovi Radio Observatory, Cardiff University, University of Amsterdam, Curtin University, National Institute for Astrophysics, Instituto de Astrofísica de Canarias, University of Alberta, Aalto-yliopisto, and Aalto University
Abstract: Funding Information: The authors thank the anonymous referee for useful comments and suggestions. The authors also thank Lian Tao for the revised black hole mass estimation using the updated distance. D.M.R. and D.M.B. acknowledge the support of the NYU Abu Dhabi Research Enhancement Fund under grant RE124. J.J. acknowledges the support of the Leverhulme Trust, the Isaac Newton Trust, and St. Edmund’s college, University of Cambridge. R.S. acknowledges grant No. 12073029 from the Natural National Science Foundation of China (NSFC). S.M. is thankful for support by Dutch Research Council (NWO) VICI award, grant Nr. 639.043.513. T.M.B. acknowledges financial contribution from the agreement ASI- INAF n.2017-14-H.0 and from PRIN-INAF 2019 N.15. T.D.R. acknowledges financial contribution from the agreement ASI-INAF n.2017-14-H.0. T.S. acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under grant PID2020-114822GB-I00. G.R.S. is supported by NSERC Discovery Grants RGPIN-2016-06569 and RGPIN-2021-0400. K.I.I.K. acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 101002352) and from the Academy of Finland projects 320045 and 320085. This work uses data from the Faulkes Telescope Project, which is an education partner of Las Cumbres Observatory (LCO). The Faulkes Telescopes are maintained and operated by LCO. This work also uses observations made with the REM Telescope, INAF Chile. It is also based on observations collected at the European Southern Observatory under ESO programmes 098.D-0893 and 099.D-0884 (PI: D. Russell). Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51494.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. This work also makes use of data supplied by the UK Swift Science Data Centre at the University of Leicester, and the MAXI data provided by RIKEN, JAXA, and the MAXI team. Publisher Copyright: © 2022. The Author(s). Published by the American Astronomical Society. We present a detailed study of the evolution of the Galactic black hole transient GRS 1716-249 during its 2016-2017 outburst at optical (Las Cumbres Observatory), mid-infrared (Very Large Telescope), near-infrared (Rapid Eye Mount telescope), and ultraviolet (the Neil Gehrels Swift Observatory Ultraviolet/Optical Telescope) wavelengths, along with archival radio and X-ray data. We show that the optical/near-infrared and UV emission of the source mainly originates from a multi-temperature accretion disk, while the mid-infrared and radio emission are dominated by synchrotron emission from a compact jet. The optical/UV flux density is correlated with the X-ray emission when the source is in the hard state, consistent with an X-ray irradiated accretion disk with an additional contribution from the viscous disk during the outburst fade. We find evidence for a weak, but highly variable jet component at mid-infrared wavelengths. We also report the long-term optical light curve of the source and find that the quiescent i′ -band magnitude is 21.39 ± 0.15 mag. Furthermore, we discuss how previous estimates of the system parameters of the source are based on various incorrect assumptions, and so are likely to be inaccurate. By comparing our GRS 1716-249 data set to those of other outbursting black hole X-ray binaries, we find that while GRS 1716-249 shows similar X-ray behavior, it is noticeably optically fainter, if the literature distance of 2.4 kpc is adopted. Using several lines of reasoning, we argue that the source distance is further than previously assumed in the literature, likely within 4-17 kpc, with a most likely range of ∼4-8 kpc.
Published: 2022

10. Absorption lines from magnetically driven winds in X-ray binaries – II. High resolution observational signatures expected from future X-ray observatories.

Author: Chakravorty, Susmita, Petrucci, Pierre-Olivier, Datta, Sudeb Ranjan, Ferreira, Jonathan, Wilms, Joern, Jacquemin-Ide, Jonatan, Clavel, Maica, Marcel, Gregoire, Rodriguez, Jerome, Malzac, Julien, Belmont, Renaud, Corbel, Stephane, Coriat, Mickael, Henri, Gilles, and Parra, Maxime
Subjects: BINARY black holes, OBSERVATORIES, X-ray spectra, ACCRETION disks, ABSORPTION, X-ray astronomy
Abstract: In our self-similar, analytical, magnetohydrodynamic (MHD) accretion–ejection solution, the density at the base of the outflow is explicitly dependent on the disc accretion rate – a unique property of this class of solutions. We had earlier found that the ejection index |$p \gt \sim 0.1 (\dot{M}_{\rm{acc}} \propto r^p)$| is a key MHD parameter that decides if the flow can cause absorption lines in the high resolution X-ray spectra of black hole binaries. Here, we choose three dense warm solutions with p = 0.1, 0.3, 0.45 and carefully develop a methodology to generate spectra which are convolved with the Athena and XRISM response functions to predict what they will observe seeing through such MHD outflows. In this paper two other external parameters were varied – extent of the disc, |$\rm {r_o|_{\rm{max}}} = 10^5, \, 10^6 \, \, \rm {r_G}$|⁠ , and the angle of the line of sight, i ∼ 10–25°. Resultant absorption lines (H and He-like Fe, Ca, Ar) change in strength and their profiles manifest varying degrees of asymmetry. We checked if (a) the lines and (ii) the line asymmetries are detected, in our suit of synthetic Athena and XRISM spectra. Our analysis shows that Athena should detect the lines and their asymmetries for a standard 100 ks observation of a 100 mCrab source – lines with equivalent width as low as a few eV should be detected if the 6–8 keV counts are larger than 104–105 even for the least favourable simulated cases. [ABSTRACT FROM AUTHOR]
Published: 2023
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11. Observatory science with eXTP

Author: in't Zand, Jean J. M., Bozzo, Enrico, Qu, Jinlu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, De Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, Xuefeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, Joao, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, Chichuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D'Aì, Antonino, Dai, Zi-Gao, D'Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D'Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, Xilong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, Mingyu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, Fangjun, Lutovinov, Alexander A., Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, Yunpeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O'Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, Lijing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jir̆í, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, Junfeng, Watts, Anna L., Weng, Shanshan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, Shaolin, Xu, Yupeng, Yan, Zhen, Younes, George, Yu, Wenfei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, Zingale, Michael, in ’t Zand, Jean, Drake, Stephen, Jenke, Peter, Maccarone, Thomas, Rossi, Elena, Tauris, Thomas, Andersson, Nils, Ballantyne, David, Brown, Edward, Cackett, Edward, D’Aì, Antonino, D’Ammando, Filippo, D’Elia, Valerio, Ferdman, Robert, Galloway, Duncan, Gambino, Angelo, Heinke, Craig, Jonker, Peter, Kaastra, Jelle, Lutovinov, Alexander, Mignani, Roberto, O’Brien, Paul, Osborne, Julian, Papadakis, Iossif, Pérez Torres, Miguel, Shore, Steven, Stappers, Ben, Strohmayer, Tod, Suleimanov, Valery, Torres, Diego, Watts, Anna, Weinberg, Nevin, Wheatley, Peter, Woods, Tyrone, Woosley, Stan, Zdziarski, Andrzej, in ’t Zand, Jean J. M., Bozzo, Enrico, Qu, JinLu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, XueFeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, ChiChuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D’Aì, Antonino, Dai, Zi-Gao, D’Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D’Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, XiLong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, MingYu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Lauren, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, FangJun, Lutovinov, Alexander A., Malyshev, Deny, Malzac, Julien, Manousakis, Antonio, McHardy, Ian, Mehdipour, Missagh, Men, YunPeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joona, Nardini, Emanuele, Neubert, Torsten, O’Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuoma, Schanne, Stéphane, Schatz, Hendrik, Shao, LiJing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jirí, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, JunFeng, Watts, Anna L., Weng, ShanShan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, ShaoLin, Xu, YuPeng, Yan, Zhen, Younes, George, Yu, WenFei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, Zingale, Michael, Institut de recherche en astrophysique et planétologie (IRAP), 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), 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), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), eXTP, Centre National de la Recherche Scientifique (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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), 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 de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre de Recherche en Information Biomédicale sino-français (CRIBS), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Southeast University [Jiangsu]-Institut National de la Santé et de la Recherche Médicale (INSERM), Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), ASI Science Data Center (ASDC), Italian Space Agency, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Anthropobiologie (LA), École des hautes études en sciences sociales (EHESS)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), SRON Netherlands Institute for Space Research (SRON), Istituto di Radioastronomia [Bologna] (IRA), KAUST Catalysis Center (KCC), King Abdullah University of Sciences & Technologie, IASF, Area di Ricerca di Tor Vergata, Laboratoire Univers et Théories (LUTH (UMR_8102)), 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 Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Southampton], University of Southampton, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut für Astrophysik [Wien], Universität Wien, Sabanci University [Istanbul], The George Washington University (GW), Department of Physics, Tokyo Institute of Technology [Tokyo] (TITECH), Deakin University [Burwood], Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), University of New Hampshire (UNH), Department of Mechanical and Industrial Engineering [Trondheim] (MTP NTNU), Norwegian University of Science and Technology [Trondheim] (NTNU), Norwegian University of Science and Technology (NTNU)-Norwegian University of Science and Technology (NTNU), Ethoikos, Radicondoli, Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Sichuan University [Chengdu] (SCU), University of Warwick [Coventry], U.S. Department of Energy [Washington] (DOE), University College of London [London] (UCL), Medical School (University of Nanjing), Nanjing University (NJU), Beijing Municipal Climate Center, Max-Planck-Institut für Radioastronomie (MPIFR), Laboratorio de Investigación y Formación en Informática Avanzada [La Plata] (LIFIA), Facultad de Informática [La Plata], Universidad Nacional de la Plata [Argentine] (UNLP)-Universidad Nacional de la Plata [Argentine] (UNLP), NLD, Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos (ICCUB), MDM-2014-0369, National Natural Science Foundation of China (NSFC), European Research Council (ERC), National Aeronautics and Space Administration (NASA), Agencia Estatal de Investigación (AEI), Royal Society, Strategic Priority Research Program of the Chinese Academy of Sciences, National Science Centre, Poland (NCN), 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), 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), Royal Society (UK), European Research Council, European Commission, National Natural Science Foundation of China, National Basic Research Program (China), National Science Foundation (US), Ministerio de Economía y Competitividad (España), Polish Academy of Sciences, Astronomy, Discrete Technology and Production Automation, in't Zand, Jean J. M., Qu, Jinlu, Tauris, Thomas M., Wilm, Joern, Wu, Xuefeng, Jin, Chichuan, D'Aì, Antonino, D'Ammando, Filippo, D'Elia, Valerio, Fan, Xilong, Ge, Mingyu, Lu, Fangjun, Mchardy, Ian, Men, Yunpeng, O'Brien, Paul T., Shao, Lijing, Svoboda, Jir̆í, Thielemann, F. -K., Wang, Junfeng, Weng, Shanshan, Xiong, Shaolin, Xu, Yupeng, Yu, Wenfei, Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, Institut de Mathématiques de Toulouse UMR5219 (IMT), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Osservatorio Astronomico di Brera, Istituto di Radioastronomia (IRA), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), George Washington University (GW), Department of Mechanical and Industrial Engineering [Trondheim], Sichuan University, U.S. Department of Energy (DOE), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), SRON Netherlands Institute for Space Research, University of Geneva, CAS - Institute of High Energy Physics, Nanjing University, INAF/IASF Bologna, National Institute for Astrophysics, University of Tübingen, NASA Goddard Space Flight Center, ICREA, University of Alabama in Huntsville, Texas Tech University, Osservatorio Astronomico di Capodimonte, Leiden University, University of Amsterdam, Polytechnic University of Catalonia, University of Urbino, Max Planck Institute for Radio Astronomy, Friedrich-Alexander University Erlangen-Nürnberg, CAS - Purple Mountain Observatory, CSIC, IRAP, New York University Abu Dhabi, Georgia Institute of Technology, Middle East Technical University, Technion-Israel Institute of Technology, Tata Institute of Fundamental Research, Roma Tre University, Instituto de Astrofísica de Canarias, Instituto Nacional de Pesquisas Espaciais, Danmarks Tekniske Universitet, Michigan State University, Osservatorio Astrofisico Di Arcetri, Florence, University of Cagliari, Wayne State University, Osservatorio Astronomico Roma, CAS - Shanghai Astronomical Observatory, Department of Electronics and Nanoengineering, Aalto-yliopisto, and Aalto University
Subjects: cataclysmic binaries, Astronomy, FIELD CAMERAS OBSERVATIONS, space research instruments nuclear astrophysics flare stars accretion and accretion disks mass loss and stellar winds cataclysmic binaries X-ray binaries supernova remnants active galactic nuclei X-ray bursts gamma-ray bursts gravitational waves, General Physics and Astronomy, gamma-ray burst, space research instrument, 01 natural sciences, Gamma ray bursts, Observatory, Accretion and accretion disks, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, gravitational wave, accretion and accretion disk, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), supernova remnants, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], flare stars, gamma-ray bursts, Astrophysics::Instrumentation and Methods for Astrophysics, accretion and accretion disks, active galactic nuclei, gravitational waves, mass loss and stellar winds, nuclear astrophysics, space research instruments, X-ray binaries, X-ray bursts, Physics and Astronomy (all), Space research instruments, X ray burst, Supernova, QUIET, High mass, X-ray binarie, Mass loss and stellar winds, Nuclear astrophysics, Gamma-ray bursts, Astrophysics - High Energy Astrophysical Phenomena, PULSAR-WIND NEBULAE, FAST RADIO-BURSTS, Astrofísica nuclear, Active galactic nucleus, TIDAL DISRUPTION, Supernova remnants, Astrophysics::High Energy Astrophysical Phenomena, Polarimetry, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, ACCRETING NEUTRON-STARS, Gravitational waves, cataclysmic binarie, Settore FIS/05 - Astronomia e Astrofisica, SUPERMASSIVE BLACK-HOLES, 0103 physical sciences, 010306 general physics, X-ray burst, Astrophysics::Galaxy Astrophysics, Cataclysmic binaries, Active galactic nuclei, flare star, White dwarf, Flare stars, Stars, supernova remnant, QB460-466 Astrophysics, [SDU]Sciences of the Universe [physics], mass loss and stellar wind, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], X-RAY, Supernova remmants, X ray binaries, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SEYFERT 1 GALAXY, nuclear astrophysic
Abstract: Disponible preprint en: arXiv:1812.04023v1 [astro-ph.HE] [v1] Mon, 10 Dec 2018 19:00:52 UTC (4,376 KB), In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s.© 2018, Science China Press and Springer-Verlag GmbH Germany, part of Springer Nature., This work was supported by the Royal Society, ERC Starting (Grant No. 639217), the European Union Horizon 2020 Research and Innovation Programme under the Marie Sklodowska-Curie Global Fellowship (Grant No. 703916), the National Natural Science Foundation of China (Grant Nos. 11233001, 11773014, 11633007, 11403074, 11333005, 11503008, and 11590781), the National Basic Research Program of China (Grant No. 2015CB857100), NASA (Grant No. NNX13AD28A), an ARC Future Fellowship (Grant No. FT120100363), the National Science Foundation (Grant No. PHY-1430152), the Spanish MINECO (Grant No. AYA2016-76012-C3-1-P), the ICCUB (Unidad de Excelencia 'Maria de Maeztu') (Grant No. MDM-2014-0369), EU's Horizon Programme through a Marie Sklodowska-Curie Fellowship (Grant No. 702638), the Polish National Science Center (Grant Nos. 2015/17/B/ST9/03422, 2015/18/M/ST9/00541, 2013/10/M/ST9/00729, and 2015/18/A/ST9/00746), the Strategic Priority Research Program of the Chinese Academy of Sciences (Grant No. XDA15020100), and the NWO Veni Fellowship (Grant No. 639.041.647).
Published: 2019
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12. Confirmation of IGR J01363 plus 6610 as a Be X-Ray Binary with Very Low Quiescent X-Ray Luminosity

Author: Tomsick, John A, Heinke, Craig, Halpern, Jules, Kaaret, Philip, Chaty, Sylvain, Rodriguez, Jerome, and Bodaghee, Arash
Subjects: Astrophysics
Abstract: The field containing the candidate High Mass X-ray Binary IGR J01 363+6610 was observed by XMM-Newton on 2009 July 31 for 28 ks. A Be star was previously suggested as the possible counterpart of the INTEGRAL source, and although Chandra, during a 2007 observation, did not detect an X-ray source at the position of the Be star, we find a variable source (XMMU 101 3549.5+661243) with an average X-ray flux of 2 x 10(exp -13)ergs/sq cm/s (0.2-12 keV, unabsorbed) at this position with XMM-Newton. The spectrum of this source is consistent with a hard power law with a photon index of r = 1.4+/-0.3 and a column density of N(sub H) = (15(+0.7/-0.5)) x 10(exp 22)/sq cm (90% confidence errors). These results, along with our optical investigation of other X-ray sources in the field, make the association with the Be star very likely, and the 2 kpc distance estimate for the Be star indicates an X-ray luminosity of 9.1 x 10(exp 31) ergs/s. This is lower than typical for a Be X-ray binary, and the upper limit on the luminosity was even lower ( < 1.4 x 10(exp 3)ergs/s assuming the same spectral model) during the Chandra observation. We discuss possible implications of the very low quiescent luminosity for the physical properties of IGR 101363+6610.
Published: 2011
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13. The 2010 May Flaring Episode of Cygnus X-3 in Radio, X-Rays, and gamma-Rays

Author: Williams, Peter K. G, Tomsick, John A, Bodaghee, Arash, Bower, Geoffrey C, Pooley, Guy G, Pottschmidt, Katja, Rodriguez, Jerome, Wilms, Joern, Migliari, Simone, and Trushkin, Sergei A
Subjects: Astronomy
Abstract: In 2009, Cygnus X-3 (Cyg X-3) became the first microquasar to be detected in the GeV gamma-ray regime, via the satellites Fermi and AGILE. The addition of this new band to the observational toolbox holds promise for building a more detailed understanding of the relativistic jets of this and other systems. We present a rich dataset of radio, hard and soft X-ray, and gamma-ray observations of Cyg X-3 made during a flaring episode in 2010 May. We detect a approx.3-d softening and recovery of the X-ray emission, followed almost immediately by a approx.1-Jy radio flare at 15 GHz, followed by a 4.3sigma gamma-ray flare (E > 100 MeV) approx.1.5 d later. The radio sampling is sparse, but we use archival data to argue that it is unlikely the gamma-ray flare was followed by any significant unobserved radio flares. In this case, the sequencing of the observed events is difficult to explain in a model in which the gamma-ray emission is due to inverse Compton scattering of the companion star's radiation field. Our observations suggest that other mechanisms may also be responsible for gamma-ray emission from Cyg X-3.
Published: 2011

14. Accretion in strong field gravity with eXTP

Author: De Rosa, Alessandra, Uttley, Phil, Gou, Li Jun, Liu, Yuan, Bambi, Cosimo, Barret, Didier, Belloni, Tomaso, Berti, Emanuele, Bianchi, Stefano, Caiazzo, Ilaria, Casella, Piergiorgio, Feroci, Marco, Ferrari, Valeria, Gualtieri, Leonardo, Heyl, Jeremy, Ingram, Adam, Karas, Vladimir, Lu, Fang Jun, Luo, Bin, Matt, Giorgio, Motta, Sara, Neilsen, Joseph, Pani, Paolo, Santangelo, Andrea, Shu, Xin Wen, Wang, Jun Feng, Wang, Jian Min, Xue, Yong Quan, Xu, Yu Peng, Yuan, Wei Min, Yuan, Ye Fei, Zhang, Shuang Nan, Zhang, Shu, Agudo, Ivan, Amati, Lorenzo, Andersson, Nils, Baglio, Cristina, Bakala, Pavel, Baykal, Altan, Bhattacharyya, Sudip, Bombaci, Ignazio, Bucciantini, Niccoló, Capitanio, Fiamma, Ciolfi, Riccardo, Cui, Wei K., D’Ammando, Filippo, Dauser, Thomas, Del Santo, Melania, De Marco, Barbara, Di Salvo, Tiziana, Done, Chris, Dovčiak, Michal, Fabian, Andrew C., Falanga, Maurizio, Gambino, Angelo Francesco, Gendre, Bruce, Grinberg, Victoria, Heger, Alexander, Homan, Jeroen, Iaria, Rosario, Jiang, Jia Chen, Jin, Chi Chuan, Koerding, Elmar, Linares, Manu, Liu, Zhu, Maccarone, Thomas J., Malzac, Julien, Manousakis, Antonios, Marin, Frédéric, Marinucci, Andrea, Mehdipour, Missagh, Méndez, Mariano, Migliari, Simone, Miller, Cole, Miniutti, Giovanni, Nardini, Emanuele, O’Brien, Paul T., Osborne, Julian P., Petrucci, Pierre Olivier, Possenti, Andrea, Riggio, Alessandro, Rodriguez, Jerome, Sanna, Andrea, Shao, Li Jing, Sobolewska, Malgosia, Sramkova, Eva, Stevens, Abigail L., Stiele, Holger, Stratta, Giulia, Stuchlik, Zdenek, Svoboda, Jiri, Tamburini, Fabrizio, Tauris, Thomas M., Tombesi, Francesco, Torok, Gabriel, Urbanec, Martin, Vincent, Frederic, Wu, Qing Wen, Yuan, Feng, in’ t Zand, Jean J.M., Zdziarski, Andrzej A., and Zhou, Xin Lin
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: In this paper we describe the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to accretion flows in the strong field gravity regime around both stellar-mass and supermassive black-holes. eXTP has the unique capability of using advanced “spectral-timing-polarimetry” techniques to analyze the rapid variations with three orthogonal diagnostics of the flow and its geometry, yielding unprecedented insight into the inner accreting regions, the effects of strong field gravity on the material within them and the powerful outflows which are driven by the accretion process. X-spinmeasurements.
Published: 2019

15. Using Chandra Localizations and Gaia Distances and Proper Motions to Classify Hard X-Ray Sources Discovered by INTEGRAL.

Author: Tomsick, John A., Coughenour, Benjamin M., Hare, Jeremy, Krivonos, Roman, Bodaghee, Arash, Chaty, Sylvain, Clavel, Maďca, Fornasini, Francesca M., Rodriguez, Jerome, and Shaw, Aarran W.
Subjects: HARD X-rays, X-ray binaries, ACTIVE galactic nuclei, DISTANCES, ASTROPHYSICS
Abstract: Here, we report on X-ray observations of ten 17–60 keV sources discovered by the International Gamma-Ray Astrophysics Laboratory satellite. The primary new information is sub-arcsecond positions obtained by the Chandra X-ray Observatory. In six cases (IGR J17040-4305, IGR J18017-3542, IGR J18112-2641, IGR J18434-0508, IGR J19504+3318, and IGR J20084+3221), a unique Chandra counterpart is identified with a high degree of certainty, and for five of these sources (all but J19504), Gaia distances or proper motions indicate that they are Galactic sources. For four of these, the most likely classifications are that the sources are magnetic cataclysmic variables (CVs). J20084 could be either a magnetic CV or a high-mass X-ray binary. We classify the sixth source (J19504) as a likely active galactic nucleus (AGN). In addition, we find likely Chandra counterparts to IGR J18010-3045 and IGR J19577+3339, and the latter is a bright radio source and probable AGN. The other two sources, IGR J12529-6351 and IGR J18013-3222, do not have likely Chandra counterparts, indicating that they are transient, highly variable, or highly absorbed. [ABSTRACT FROM AUTHOR]
Published: 2021
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16. Feasibility of Observing Gamma-Ray Polarization from Cygnus X-1 Using a CubeSat.

Author: Yang, Chien-Ying, Chang, Yi-Chi, Liang, Hung-Hsiang, Chu, Che-Yen, Hsiang, Jr-Yue, Chiu, Jeng-Lun, Lin, Chih-Hsun, Laurent, Philippe, Rodriguez, Jerome, and Chang, Hsiang-Kuang
Published: 2020
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17. X-ray Spectral Analysis of the Steady States of Grs1915+105

Author: Peris , Charith, Remillard , Ronald, Steiner , James, Vrtilek , Saeqa, Varnière , Peggy, Rodriguez , Jerome, Pooley , Guy, 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 ), Laboratoire AIM, and Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay
Subjects: X-rays: binaries, binaries: close, accretion, Astrophysics::High Energy Astrophysical Phenomena, accretion disks, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], black hole physics, magnetic fields, X-rays: individual
Abstract: International audience; We report on the X-ray spectral behavior within the steady states of GRS1915+105. Our work is based on the full data set of the source obtained using the Proportional Counter Array (PCA) on the Rossi X-ray Timing Explorer (RXTE) and 15 GHz radio data obtained using the Ryle Telescope. The steady observations within the X-ray data set naturally separated into two regions in the color–color diagram and we refer to these regions as steady-soft and steady-hard. GRS1915+105 displays significant curvature in the coronal component in both the soft and hard data within the RXTE/PCA bandpass. A majority of the steady-soft observations displays a roughly constant inner disk radius (${R}_{{\rm{in}}}$), while the steady-hard observations display an evolving disk truncation which is correlated to the mass accretion rate through the disk. The disk flux and coronal flux are strongly correlated in steady-hard observations and very weakly correlated in the steady-soft observations. Within the steady-hard observations, we observe two particular circumstances when there are correlations between the coronal X-ray flux and the radio flux with log slopes $\eta \sim 0.68\pm 0.35$ and $\eta \sim 1.12\pm 0.13$. They are consistent with the upper and lower tracks of Gallo et al. (2012), respectively. A comparison of the model parameters to the state definitions shows that almost all of the steady-soft observations match the criteria of either a thermal or steep power-law state, while a large portion of the steady-hard observations match the hard-state criteria when the disk fraction constraint is neglected.
Published: 2016
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18. The On-Site Analysis of the Cherenkov Telescope Array

Author: Bulgarelli, Andrea, Fioretti, Valentina, Lombardi, Saverio, Tosti, Gino, Bergamaschi, Sonia, Beneventano, Domenico, Lamanna, Giovanni, Jacquemier, Jean, Kosack, Karl, Antonelli, Lucio Angelo, Boisson, Catherine, Borkowski, Jerzy, Zoli, Andrea, Buson, Sara, Carosi, Alessandro, Conforti, Vito, Colomé, Pep, de los Reyes, Raquel, Dumm, Jon, Evans, Phil, Fortson, Lucy, Fuessling, Matthias, Gotz, Diego, Aboudan, Alessio, Graciani, Ricardo, Gianotti, Fulvio, Grandi, Paola, Hinton, Jim, Humensky, Brian, Inoue, Susumu, Knödlseder, Jürgen, Flour, Thierry Le, Lindemann, Rico, Malaguti, Giuseppe, Rodríguez-Vázquez, Juan José, Markoff, Sera, Marisaldi, Martino, Neyroud, Nadine, Nicastro, Luciano, Ohm, Stefan, Osborne, Julian, Oya, Igor, Rodriguez, Jerome, Rosen, Simon, Ribo, Marc, De Cesare, Giovanni, Tacchini, Alessandro, Schüssler, Fabian, Stolarczyk, Thierry, Torresi, Eleonora, Testa, Vincenzo, Wegner, Peter, Consortium, Amanda Weinstein, Cherenkov Telescope Array Consortium, De Rosa, Adriano, Maier, Gernot, Lyard, Etienne, Bastieri, Denis, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), and CTA
Subjects: Cherenkov Telescope Array, Real-time computing, FOS: Physical sciences, Astrophysics, 01 natural sciences, 7. Clean energy, Real-Time Analysis, Software, Observatory, 0103 physical sciences, ddc:530, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Cherenkov radiation, Physics, 010308 nuclear & particles physics, business.industry, Bandwidth (signal processing), Site analysis, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], On-Site Analysis, high-energy gamma-ray observatories, Pipeline transport, 13. Climate action, Data quality, Astrophysics - Instrumentation and Methods for Astrophysics, business
Abstract: The Cherenkov Telescope Array (CTA) observatory will be one of the largest ground-based very high-energy gamma-ray observatories. The On-Site Analysis will be the first CTA scientific analysis of data acquired from the array of telescopes, in both northern and southern sites. The On-Site Analysis will have two pipelines: the Level-A pipeline (also known as Real-Time Analysis, RTA) and the level-B one. The RTA performs data quality monitoring and must be able to issue automated alerts on variable and transient astrophysical sources within 30 seconds from the last acquired Cherenkov event that contributes to the alert, with a sensitivity not worse than the one achieved by the final pipeline by more than a factor of 3. The Level-B Analysis has a better sensitivity (not be worse than the final one by a factor of 2) and the results should be available within 10 hours from the acquisition of the data: for this reason this analysis could be performed at the end of an observation or next morning. The latency (in particular for the RTA) and the sensitivity requirements are challenging because of the large data rate, a few GByte/s. The remote connection to the CTA candidate site with a rather limited network bandwidth makes the issue of the exported data size extremely critical and prevents any kind of processing in real-time of the data outside the site of the telescopes. For these reasons the analysis will be performed on-site with infrastructures co-located with the telescopes, with limited electrical power availability and with a reduced possibility of human intervention. This means, for example, that the on-site hardware infrastructure should have low-power consumption. A substantial effort towards the optimization of high-throughput computing service is envisioned to provide hardware and software solutions with high-throughput, low-power consumption at a low-cost., In Proceedings of the 34th International Cosmic Ray Conference (ICRC2015), The Hague, The Netherlands. All CTA contributions at arXiv:1508.05894
Published: 2015
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19. The Hot and Energetic Universe: A White Paper presenting the science theme motivating the Athena+ mission

Author: Nandra, Kirpal, Barret, Didier, Barcons, Xavier, Fabian, Andy, Den Herder, Jan-Willem, Piro, Luigi, Watson, Mike, Adami, Christophe, Aird, James, Afonso, Jose Manuel, Alexander, Dave, Argiroffi, Costanza, Amati, Lorenzo, Arnaud, Monique, Atteia, Jean-Luc, Audard, Marc, Badenes, Carles, Ballet, Jean, Ballo, Lucia, Bamba, Aya, Bhardwaj, Anil, Stefano Battistelli, Elia, Becker, Werner, Becker, Michaël, Behar, Ehud, Bianchi, Stefano, Biffi, Veronica, Bîrzan, Laura, Bocchino, Fabrizio, Bogdanov, Slavko, Boirin, Laurence, Boller, Thomas, Borgani, Stefano, Borm, Katharina, Bouché, Nicolas, Bourdin, Hervé, Bower, Richard, Braito, Valentina, Branchini, Enzo, Branduardi-Raymont, Graziella, Bregman, Joel, Brenneman, Laura, Brightman, Murray, Brüggen, Marcus, Buchner, Johannes, Bulbul, Esra, Brusa, Marcella, Bursa, Michal, Caccianiga, Alessandro, Cackett, Ed, Campana, Sergio, Cappelluti, Nico, Cappi, Massimo, Carrera, Francisco, Ceballos, Maite, Christensen, Finn, Chu, You-Hua, Churazov, Eugene, Clerc, Nicolas, Corbel, Stephane, Corral, Amalia, Comastri, Andrea, Costantini, Elisa, Croston, Judith, Dadina, Mauro, D Ai, Antonino, Decourchelle, Anne, Della Ceca, Roberto, Dennerl, Konrad, Dolag, Klaus, Done, Chris, Dovciak, Michal, Drake, Jeremy, Eckert, Dominique, Edge, Alastair, Ettori, Stefano, Ezoe, Yuichiro, Feigelson, Eric, Fender, Rob, Feruglio, Chiara, Finoguenov, Alexis, Fiore, Fabrizio, Galeazzi, Massimiliano, Gallagher, Sarah, Gandhi, Poshak, Gaspari, Massimo, Gastaldello, Fabio, Georgakakis, Antonis, Georgantopoulos, Ioannis, Gilfanov, Marat, Gitti, Myriam, Gladstone, Randy, Goosmann, Rene, Gosset, Eric, Grosso, Nicolas, Guedel, Manuel, Guerrero, Martin, Haberl, Frank, Hardcastle, Martin, Heinz, Sebastian, Alonso Herrero, Almudena, Hervé, Anthony, Holmstrom, Mats, Iwasawa, Kazushi, Jonker, Peter, Kaastra, Jelle, Kara, Erin, Karas, Vladimir, Kastner, Joel, King, Andrew, Kosenko, Daria, Koutroumpa, Dimita, Kraft, Ralph, Kreykenbohm, Ingo, Lallement, Rosine, Lanzuisi, Giorgio, Lee, J., Lemoine-Goumard, Marianne, Lobban, Andrew, Lodato, Giuseppe, Lovisari, Lorenzo, Lotti, Simone, Mccharthy, Ian, Mcnamara, Brian, Maggio, Antonio, Maiolino, Roberto, Marco, Barbara, Martino, Domitilla, Mateos, Silvia, Matt, Giorgio, Maughan, Ben, Mazzotta, Pasquale, Mendez, Mariano, Merloni, Andrea, Micela, Giuseppina, Miceli, Marco, Mignani, Robert, Miller, Jon, Miniutti, Giovanni, Molendi, Silvano, Montez, Rodolfo, Moretti, Alberto, Motch, Christian, Nazé, Yaël, Nevalainen, Jukka, Nicastro, Fabrizio, Nulsen, Paul, Ohashi, Takaya, O Brien, Paul, Osborne, Julian, Oskinova, Lida, Pacaud, Florian, Paerels, Frederik, Page, Mat, Papadakis, Iossif, Pareschi, Giovanni, Petre, Robert, Petrucci, Pierre-Olivier, Piconcelli, Enrico, Pillitteri, Ignazio, Pinto, C., Plaa, Jelle, Pointecouteau, Etienne, Ponman, Trevor, Ponti, Gabriele, Porquet, Delphine, Pounds, Ken, Pratt, Gabriel, Predehl, Peter, Proga, Daniel, Psaltis, Dimitrios, Rafferty, David, Ramos-Ceja, Miriam, Ranalli, Piero, Rasia, Elena, Rau, Arne, Rauw, Gregor, Rea, Nanda, Read, Andy, Reeves, James, Reiprich, Thomas, Renaud, Matthieu, Reynolds, Chris, Risaliti, Guido, Rodriguez, Jerome, Rodriguez Hidalgo, Paola, Roncarelli, Mauro, Rosario, David, Rossetti, Mariachiara, Rozanska, Agata, Rovilos, Emmanouil, Salvaterra, Ruben, Salvato, Mara, Di Salvo, Tiziana, Jeremy Sanders, Sanz-Forcada, Jorge, Schawinski, Kevin, Schaye, Joop, Schwope, Axel, Sciortino, Salvatore, Severgnini, Paola, Shankar, Francesco, Sijacki, Debora, Sim, Stuart, Schmid, Christian, Smith, Randall, Steiner, Andrew, Stelzer, Beate, Stewart, Gordon, Strohmayer, Tod, Strüder, Lothar, Sun, Ming, Takei, Yoh, Tatischeff, V., Tiengo, Andreas, Tombesi, Francesco, Trinchieri, Ginevra, Tsuru, T. G., Ud-Doula, Asif, Ursino, Eugenio, Valencic, Lynne, Vanzella, Eros, Vaughan, Simon, Vignali, Cristian, Vink, Jacco, Vito, Fabio, Volonteri, Marta, Wang, Daniel, Webb, Natalie, Willingale, Richard, Wilms, Joern, Wise, Michael, Worrall, Diana, Young, Andrew, Zampieri, Luca, In T Zand, Jean, Zane, Silvia, Zezas, Andreas, Zhang, Yuying, Zhuravleva, Irina, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), 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), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Dipartimento di Fisica e Chimica (DiFC), Università degli studi di Palermo - University of Palermo, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de recherche en astrophysique et planétologie (IRAP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Columbia Astrophysics Laboratory (CAL), Columbia University [New York], Department of Astrophysical Sciences [Princeton], Princeton University, Département d'Astrophysique (ex SAP) (DAP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), 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), Institute for Computational Cosmology (ICC), Durham University, Dipartimento de Fisica Roma Tre (DF-Roma3), Università degli Studi Roma Tre, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Technische Universität München [München] (TUM), National Space Institute [Lyngby] (DTU Space), Technical University of Denmark [Lyngby] (DTU), 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), SRON Netherlands Institute for Space Research (SRON), Max-Planck-Institut für Extraterrestrische Physik (MPE), Department of Physics [Durham University], Ecole Polytechnique Fédérale de Lausanne (EPFL), Tokyo Metropolitan University [Tokyo], Department of Astronomy and Astrophysics [PennState], Pennsylvania State University (Penn State), Penn State System-Penn State System, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Physics [Coral Gables], University of Miami [Coral Gables], Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Swedish Institute of Space Physics [Kiruna] (IRF), Astronomical Institute of the Czech Academy of Sciences, Czech Academy of Sciences [Prague] (ASCR), HEPPI - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), 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), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Cavendish Laboratory, University of Cambridge [UK] (CAM), Università degli Studi di Roma Tor Vergata [Roma], Max-Planck-Institut für Astrophysik (MPA), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, PSL Research University (PSL), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], School of Physics and Astronomy [Southampton], University of Southampton, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Department of Computer Science, Penn State System, Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Lawrence Livermore National Laboratory (LLNL), Max Plank Institute for Extraterrestial Life, 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), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Fisica e Chimica [Palermo] (DiFC), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi Roma Tre = Roma Tre University (ROMA TRE), Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), 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), Tokyo Metropolitan University [Tokyo] (TMU), 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), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), HELIOS - LATMOS, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), 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), Harvard University-Smithsonian Institution, Université Paris sciences et lettres (PSL), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universiteit Leiden, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Astronomy, Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-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), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Smithsonian Institution-Harvard University [Cambridge], Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Maiolino, Roberto [0000-0002-4985-3819], Reynolds, Christopher [0000-0002-1510-4860], Sijacki, Debora [0000-0002-3459-0438], Apollo - University of Cambridge Repository, 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)-Université Fédérale Toulouse Midi-Pyrénées-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), 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), and Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Earth and Planetary Astrophysics (astro-ph.EP), astro-ph.SR, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics - Cosmology and Extragalactic Astrophysics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], astro-ph.EP, astro-ph.CO, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), astro-ph.IM, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: This White Paper, submitted to the recent ESA call for science themes to define its future large missions, advocates the need for a transformational leap in our understanding of two key questions in astrophysics: 1) How does ordinary matter assemble into the large scale structures that we see today? 2) How do black holes grow and shape the Universe? Hot gas in clusters, groups and the intergalactic medium dominates the baryonic content of the local Universe. To understand the astrophysical processes responsible for the formation and assembly of these large structures, it is necessary to measure their physical properties and evolution. This requires spatially resolved X-ray spectroscopy with a factor 10 increase in both telescope throughput and spatial resolving power compared to currently planned facilities. Feedback from supermassive black holes is an essential ingredient in this process and in most galaxy evolution models, but it is not well understood. X-ray observations can uniquely reveal the mechanisms launching winds close to black holes and determine the coupling of the energy and matter flows on larger scales. Due to the effects of feedback, a complete understanding of galaxy evolution requires knowledge of the obscured growth of supermassive black holes through cosmic time, out to the redshifts where the first galaxies form. X-ray emission is the most reliable way to reveal accreting black holes, but deep survey speed must improve by a factor ~100 over current facilities to perform a full census into the early Universe. The Advanced Telescope for High Energy Astrophysics (Athena+) mission provides the necessary performance (e.g. angular resolution, spectral resolution, survey grasp) to address these questions and revolutionize our understanding of the Hot and Energetic Universe. These capabilities will also provide a powerful observatory to be used in all areas of astrophysics., Submitted in response to the call for White Papers for the definition of the L2 and L3 missions in the ESA Science program. More information: http://www.the-athena-x-ray-observatory.eu/. 19 pages, 12 figures, 4 tables
Published: 2013

20. Revealing the nature of high-mass X-ray binaries through multi-wavelength and statistical analyses

Author: Bodaghee, Arash, Tomsick, John A., and Rodriguez, Jerome
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We summarize the results of our long-running campaign to help understand the nature of high-mass X-ray binaries (HMXBs), emphasizing recent Suzaku observations of IGR J16207-5129 and IGR J17391-3021. Thanks to the expanding ranks of HMXBs in our Galaxy, we are able to perform more reliable statistical analyses on the three currently-known sub-classes of HMXB: those with supergiant companions (SGXBs); those with Be companions (BEXBs); and the enigmatic Supergiant Fast X-ray Transients (SFXTs). We discuss new diagnostic tools, akin to the "Corbet diagram," in which HMXBs tend to segregate based on their dominant accretion mechanism. We show how SFXTs span across the divided populations of BEXBs and SGXBs, bolstering the intriguing possibility that some SFXTs represent an evolutionary link. The use of HMXBs as tracers of recent massive star formation is revisited as we present the first ever spatial correlation function for HMXBs and OB star-forming complexes. Our results indicate that at distances less than a few kpc from a given HMXB, it is more likely to have neighbors that are known massive-star forming regions as opposed to objects drawn from random distributions. The characteristic scale of the correlation function holds valuable clues to HMXB evolutionary timescales., 6 pages, 5 figures, to appear in proceedings of the 4th International MAXI Workshop in Tokyo, "The First Year of MAXI: Monitoring Variable X-ray Sources"
Published: 2011

21. Is the plateau state in GRS 1915+105 equivalent to canonical hard states?

Author: van Oers, Pieter, Markoff, Sera, Maitra, Dipankar, Rahoui, Farid, Nowak, Michael, Wilms, Jörn, Castro-Tirado, Alberto J., Rodriguez, Jerome, Dhawan, Vivek, Harlaftis, Emilios, 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 (UMR_7158 / 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-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), High Energy Physics - Theory, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, black hole physics, galaxies: active, FOS: Physical sciences, radiation mechanisms: general, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: jets, accretion discs, General Relativity and Quantum Cosmology, X-rays: binaries, High Energy Physics - Theory (hep-th), accretion, [SDU]Sciences of the Universe [physics], Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: GRS1915+105 is a very peculiar black hole binary that exhibits accretion-related states that are not observed in any other stellar-mass black hole system. One of these states, however -- referred to as the plateau state -- may be related to the canonical hard state of black hole X-ray binaries. Both the plateau and hard state are associated with steady, relatively lower X-ray emission and flat/inverted radio emission, that is sometimes resolved into compact, self-absorbed jets. However, while generally black hole binaries quench their jets when the luminosity becomes too high, GRS1915+105 seems to sustain them despite the fact that it accretes at near- or super-Eddington rates. In order to investigate the relationship between the plateau and the hard state, we fit two multi-wavelength observations using a steady-state outflow-dominated model, developed for hard state black hole binaries. The data sets consist of quasi-simultaneous observations in radio, near-infrared and X-ray bands. Interestingly, we find both significant differences between the two plateau states, as well as between the best-fit model parameters and those representative of the hard state. We discuss our interpretation of these results, and the possible implications for GRS 1915+105's relationship to canonical black hole candidates., Comment: accepted for publication in MNRAS
Published: 2010
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22. Broad-Band Spectrum of The Black Hole Candidate IGR J17497-2821 Studied with Suzaku

Author: PAIZIS, Adamantia, EBISAWA, Ken, TAKAHASHI, Hiromitsu, DOTANI, Tadayasu, KOHMURA, Takayoshi, KOKUBUN, Motohide, RODRIGUEZ, Jerome, UEDA, Yoshihiro, WALTER, Roland, YAMADA, Shinya, YAMAOKA, Kazutaka, and YUASA, Takayuki
Subjects: Physics, accretion disks, Astrophysics::High Energy Astrophysical Phenomena, Spectral properties, Spectrum (functional analysis), black hole physics, stars: individual (IGR J17497-2821), Astrophysics (astro-ph), Astronomy, Broad band, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Black hole, Accretion disc, Space and Planetary Science, X-ray: binaries
Abstract: The broad-band 1-300 keV Suzaku spectrum of IGR J17497-2821, the X-ray transient discovered by INTEGRAL in September 2006, is presented. Suzaku observed IGR J17497-2821 on September 25, eight days after its discovery, for a net exposure of about 53 ksec. During the Suzaku observation, IGR J17497-2821 is very bright, 2 x 10^37 erg/s at 8 kpc in the 1-300 keV range, and shows a hard spectrum, typical of black hole candidates in the low-hard state. Despite the multi-mission X-ray monitoring of the source, only with Suzaku is it possible to obtain a broad-band spectrum in the 1-300 keV range with a very high signal to noise ratio. A sum of a multi-color disc (DISKBB) and a thermal Comptonization component (COMPPS) with mild reflection is a good representation of our IGR J17497-2821 Suzaku spectrum. The spectral properties of the accretion disc as well as the cut-off energy in the spectrum at about 150 keV are clearly detected and constrained. We discuss the implications on the physical model used to interpret the data and the comparison with previous results., 7 pages, 6 figures, Accepted for publication in PASJ, Suzaku Special Issue
Published: 2008

23. Identifications of five INTEGRAL sources through optical spectroscopy

Author: Butler, Suzanne C., Tomsick, John A., Chaty, Sylvain, Heras, Juan A. Z., Rodriguez, Jerome, Walter, Roland, Kaaret, Philip, Kalemci, Emrah, and Özbey, Mehtap
Subjects: QB799-903 Stars
Abstract: The International Gamma-Ray Astrophysics Laboratory (INTEGRAL) is discovering hundreds of new hard X-ray sources, many of which remain unidentified. We report on optical spectroscopy of five such sources for which X-ray observations at lower energies (0.5–10 keV) and higher angular resolutions than INTEGRAL have allowed for unique optical counterparts to be located. We find that IGR J16426+6536 and IGR J22292+6647 are Type 1 Seyfert active galactic nuclei (with IGR J16426+6536 further classified as a Seyfert 1.5) which have redshifts of z = 0.323 and z = 0.113, respectively. IGR J18308–1232 is identified as a cataclysmic variable (CV), and we confirm a previous identification of IGR J19267+1325 as a magnetic CV. By comparing the spectrum of IGR J18214–1318 to colors of various types of stars, we conclude that it is probably a high mass X-ray binary.
Published: 2008

24. Broad-band spectral changes of the microquasars Cygnus X-1 and SWIFT J1753.5-0127

Author: Bel, Marion Cadolle, Ribo, Marc, Rodriguez, Jerome, Chaty, Sylvain, Corbel, Stephane, Goldwurm, Andrea, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Universitat de Barcelona, Universitat de Barcelona (UB), in Como, Italy, Eds: T. Belloni et al. 2006 (Proceedings of Science website http://pos.sissa.it/), INTEGRAL, and RXTE
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We report high-energy results obtained with INTEGRAL and Rossi-XTE on two microquasars: the persistent high-mass system Cygnus X-1 and the transient low-mass binary SWIFT J1753.5-0127. INTEGRAL observed Cygnus X-1 from 2002 to 2004: the spectral (5-1000 keV) properties of the source, seen at least in three distinct spectral states, show disc and corona changes. In 2003 June, a high-energy tail at several hundred keV in excess of the thermal Comptonization model was observed, suggesting the presence of an additional non-thermal component. At that time, we detected an unusual correlation between radio data and high-energy hardness. We also report and compare the results obtained with simultaneous observations of the transient source SWIFT J1753.5-0127 performed with Rossi-XTE, INTEGRAL, VLA, REM and NTT on 2005 August 10-12 near its hard X-ray outburst. Broad-band spectra and fast time-variability properties are derived on this source (probably located in the galactic halo) together with radio, IR and optical data. We build a spectral energy distribution of the source and derive interesting multiwavelength constraints. Significantly detected up to 600 keV in a typical Low/Hard State, the transient does not seem to follow the usual radio/X-ray correlation., 5 figures, 2 in color
Published: 2006

25. Chandra identification of two AGN discovered by INTEGRAL.

Author: Tomsick, John A., Krivonos, Roman, Rahoui, Farid, Ajello, Marco, Rodriguez, Jerome, Barrière, Nicolas, Bodaghee, Arash, and Chaty, Sylvain
Subjects: ASTRONOMICAL observations, GALACTIC X-ray sources, ACTIVE galactic nuclei, SEYFERT galaxies, PHOTONS
Abstract: Here, we report on observations of two hard X-ray sources that were originally discovered with the INTEGRAL satellite: IGR J04059+5416 and IGR J08297-4250.We use the Chandra X-ray Observatory to localize the sources and then archival near-IR images to identify the counterparts. Both sources have counterparts in the catalogue of extended 2 Micron All-Sky Survey sources, and the counterpart to IGR J04059+5416 has been previously identified as a galaxy. Thus, we place IGR J04059+5416 in the class of active galactic nuclei (AGN), and we suggest that IGR J08297-4250 is also an AGN. If this identification is correct, the near-IR images suggest that the host galaxy of IGR J08297-4250 may be merging with a smaller nearby galaxy. For IGR J04059+5416, the 0.3-86 keV spectrum from Chandra and INTEGRAL is consistent with an absorbed power-law with a column density of NH = (3.1-1.5+2.0) x 1022 cm-2 and a photon index of Γ = 1.4 ± 0.7, and we suggest that it is a Seyfert galaxy. For IGR J08297-4250, the photon index is similar, Γ = 1.5 ± 0.8, but the source is highly absorbed (NH = (6.1-4.3+10.1) x 1023 cm-2). [ABSTRACT FROM AUTHOR]
Published: 2015
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26. IS THE CORONA THE SOURCE OF THE EJECTED MATERIAL IN MICROQUASARS?

Author: RODRIGUEZ, JEROME and PRAT, LIONEL
Subjects: *SOLAR corona, *QUASARS, *RADIO sources (Astronomy), *ASTRONOMY, *SPECTRUM analysis
Abstract: Microquasar outbursts are characterized by spectral state transitions. The transitions between states characterized by a hard spectrum and those characterized by a soft spectrum are of particular interest. Besides drastic spectral and timing changes, these transitions often show discrete ejections detectable in the radio domain. The mechanisms giving birth to the ejections, the links with accretion and the exact nature of the ejected material are still largely unknown. We present systematic X–ray spectral analysis prior to the ejection in several microquasars, and show that, in each case, the properties of the corona drastically evolve, while that of the disc remain roughly constant. We intepret this behavior as possibly due to an ejection of the corona at the spectral transition. [ABSTRACT FROM AUTHOR]
Published: 2010
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27. INVESTIGATING THE OPTICAL COUNTERPART CANDIDATES OF FOUR INTEGRAL SOURCES LOCALIZED WITH CHANDRA.

Author: Özbey Arabacı, Mehtap, Kalemci, Emrah, Tomsick, John A., Halpern, Jules, Bodaghee, Arash, Chaty, Sylvain, Rodriguez, Jerome, and Rahoui, Farid
Subjects: OPTICAL spectroscopy, SOLAR flares, SOLAR activity, SOLAR radiation, STARS
Abstract: We report on the optical spectroscopic follow-up observations of the candidate counterparts to four INTEGRAL sources: IGR J04069+5042, IGR J06552–1146, IGR J21188+4901, and IGR J22014+6034. The candidate counterparts were determined with Chandra, and the optical observations were performed with 1.5 m RTT-150 telescope (TÜBİTAK National Observatory, Antalya, Turkey) and 2.4 m Hiltner Telescope (MDM Observatory, Kitt Peak, Arizona). Our spectroscopic results show that one of the two candidates of IGR J04069+5042 and the one observed for IGR J06552–1146 could be active late-type stars in RS CVn systems. However, according to the likelihood analysis based on Chandra and INTEGRAL, two optically weaker sources in the INTEGRAL error circle of IGR J06552–1146 have higher probabilities to be the actual counterpart. The candidate counterparts of IGR J21188+4901 are classified as an active M-type star and a late-type star. Among the optical spectra of four candidates of IGR J22014+6034, two show Hα emission lines, one is a late-type star, and the other is an M type. The likelihood analysis favors a candidate with no distinguishing features in the optical spectrum. Two of the candidates classified as M-type dwarfs, are similar to some IGR candidates claimed to be symbiotic stars. However, some of the prominent features of symbiotic systems are missing in our spectra, and their NIR colors are not consistent with those expected for giants. We consider the IR colors of all IGR candidates claimed to be symbiotic systems and find that low-resolution optical spectrum may not be enough for conclusive identification. [ABSTRACT FROM AUTHOR]
Published: 2012
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28. LOCALIZING INTEGRAL SOURCES WITH CHANDRA: X-RAY AND MULTI-WAVELENGTH IDENTIFICATIONS AND ENERGY SPECTRA.

Author: Tomsick, John A., Bodaghee, Arash, Chaty, Sylvain, Rodriguez, Jerome, Rahoui, Farid, Halpern, Jules, Kalemci, Emrah, and Özbey Arabaci, Mehtap
Subjects: X-ray spectra, ACTIVE galaxies, WAVELENGTHS, ACTIVE galactic nuclei, NEAR infrared radiation
Abstract: We report on Chandra observations of 18 hard X-ray (>20 keV) sources discovered with the INTEGRAL satellite near the Galactic plane. For 14 of the INTEGRAL sources, we have uncovered one or two potential Chandra counterparts per source. These provide soft X-ray (0.3-10 keV) spectra and subarcsecond localizations, which we use to identify counterparts at other wavelengths, providing information about the nature of each source. Despite the fact that all of the sources are within 5° of the plane, four of the IGR sources are active galactic nuclei (AGNs; IGR J01545+6437, IGR J15391-5307, IGR J15415-5029, and IGR J21565+5948) and four others are likely AGNs (IGR J03103+5706, IGR J09189-4418, IGR J16413-4046, and IGR J16560-4958) based on each of them having a strong IR excess and/or extended optical or near-IR emission. We compare the X-ray and near-IR fluxes of this group of sources to those of AGNs selected by their 2-10 keV emission in previous studies and find that these IGR AGNs are in the range of typical values. There is evidence in favor of four of the sources being Galactic (IGR J12489-6243, IGR J15293-5609, IGR J16173-5023, and IGR J16206-5253), but only IGR J15293-5609 is confirmed as a Galactic source as it has a unique Chandra counterpart and a parallax measurement from previous optical observations that puts its distance at 1.56 ± 0.12 kpc. The 0.3-10 keV luminosity for this source is (1.4+1.0– 0.4) × 1032 erg s–1, and its optical/IR spectral energy distribution is well described by a blackbody with a temperature of 4200-7000 K and a radius of 12.0-16.4 R☼. These values suggest that IGR J15293-5609 is a symbiotic binary with an early K-type giant and a white dwarf accretor. We also obtained likely Chandra identifications for IGR J13402-6428 and IGR J15368-5102, but follow-up observations are required to constrain their source types. [ABSTRACT FROM AUTHOR]
Published: 2012
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29. CONFIRMATION OF IGR J01363+6610 AS A Be X-RAY BINARY WITH VERY LOW QUIESCENT X-RAY LUMINOSITY.

Author: Tomsick, John A., Heinke, Craig, Halpern, Jules, Kaaret, Philip, Chaty, Sylvain, Rodriguez, Jerome, and Bodaghee, Arash
Published: 2011
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30. CHANDRA LOCALIZATIONS AND SPECTRA OF INTEGRAL SOURCES IN THE GALACTIC PLANE: THE CYCLE 9 SAMPLE.

Author: Tomsick, John A., Chaty, Sylvain, Rodriguez, Jerome, Walter, Roland, and Kaaret, Philip
Published: 2009
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31. IDENTIFICATIONS OF FIVE INTEGRAL SOURCES VIA OPTICAL SPECTROSCOPY.

Author: Butler, Suzanne C., Tomsick, John A., Chaty, Sylvain, Heras, Juan A. Zurita, Rodriguez, Jerome, Walter, Roland, Kaaret, Philip, Kalemci, Emrah, and Özbey, Mehtap
Published: 2009
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32. QUASI-PERIODIC OSCILLATION FREQUENCY-COLOR RADIUS CONNECTION IN GRS 1915+105: A POSSIBLE TURNOVER SUPPORTING ACCRETION-EJECTION INSTABILITY PREDICTIONS.

Author: Mikles, Valerie J., Varniere, Peggy, Eikenberry, Stephen S., Rodriguez, Jerome, and Rothstein, Dave
Published: 2009
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33. Identifications of Four INTEGRAL Sources in the Galactic Plane via Chandra Localizations.

Author: Tomsick, John A., Chaty, Sylvain, Rodriguez, Jerome, Foschini, Luigi, Walter, Roland, and Kaaret, Philip
Published: 2006
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34. Psychology's Hidden Figures: Undergraduate Psychology Majors' (In)Ability to Recognize Our Diverse Pioneers.

Author: Cramblet Alvarez, Leslie D., Jones, K. Nicole, Walljasper-Schuyler, Chelsea, Trujillo, Marissa, Weiser, Mikayla A., Rodriguez, Jerome L., Ringler, Rachael L., and Leach, Jonah L.
Subjects: *HISTORY of psychology, *WOMEN of color, *PEOPLE of color, *PSYCHOLOGY, *UNDERGRADUATES, *ABILITY
Abstract: Psychology as a science professes a dedication to diversity in many forms including celebrating diverse perspectives and people. Nevertheless, women and people of color, both historically and currently, face barriers to their advancement in the field. Illustrative of one of the challenges that women and psychologists of color face, undergraduate students know very little about psychology's diverse historical roots including eminent pioneers who are women and people of color. Junior and senior psychology majors completed a name recognition task which included 42 pioneers in psychology, 21 of who were women, and 9 who were people of color. Participants recognized eminent women and people of color at significantly lower rates as compared to White, male pioneers (z = -12.95, p < .001, r = -.82; z = -10.62, p < .001, r = -.68, respectively). Having completed a History of Psychology course increased participants' ability to recognize pioneers (U = 738.00, z = -3.79, p < .001, r = -.38) but primarily benefited White, male pioneers. Because psychology majors, professionals, and practitioners are an increasingly diverse group, implications for the psychology curriculum and minoritized students are discussed. [ABSTRACT FROM AUTHOR]
Published: 2019
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35. GRS 1915+105 AS A GALACTIC ANALOG OF A FANAROFF-RILEY II QUASAR

Author: Rodriguez, Jerome [Laboratoire AIM, CEA/DSM-CNRS-Universite Paris Diderot, IRFU SAp, F-91191 Gif-sur-Yvette (France)]
Published: 2013
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36. THE RELATIONSHIP BETWEEN X-RAY LUMINOSITY AND MAJOR FLARE LAUNCHING IN GRS 1915+105

Author: Rodriguez, Jerome [Laboratoire AIM, CEA/DSM-CNRS-Universite Paris Diderot, IRFU SAp, F-91191 Gif-sur-Yvette (France)]
Published: 2013
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37. The enhanced X-ray Timing and Polarimetry mission—eXTP

Author: ShuangNan Zhang, Andrea Santangelo, Marco Feroci, YuPeng Xu, FangJun Lu, Yong Chen, Hua Feng, Shu Zhang, Søren Brandt, Margarita Hernanz, Luca Baldini, Enrico Bozzo, Riccardo Campana, Alessandra De Rosa, YongWei Dong, Yuri Evangelista, Vladimir Karas, Norbert Meidinger, Aline Meuris, Kirpal Nandra, Teng Pan, Giovanni Pareschi, Piotr Orleanski, QiuShi Huang, Stephane Schanne, Giorgia Sironi, Daniele Spiga, Jiri Svoboda, Gianpiero Tagliaferri, Christoph Tenzer, Andrea Vacchi, Silvia Zane, Dave Walton, ZhanShan Wang, Berend Winter, Xin Wu, Jean J. M. in’ t Zand, Mahdi Ahangarianabhari, Giovanni Ambrosi, Filippo Ambrosino, Marco Barbera, Stefano Basso, Jörg Bayer, Ronaldo Bellazzini, Pierluigi Bellutti, Bruna Bertucci, Giuseppe Bertuccio, Giacomo Borghi, XueLei Cao, Franck Cadoux, Francesco Ceraudo, TianXiang Chen, YuPeng Chen, Jerome Chevenez, Marta Civitani, Wei Cui, WeiWei Cui, Thomas Dauser, Ettore Del Monte, Sergio Di Cosimo, Sebastian Diebold, Victor Doroshenko, Michal Dovciak, YuanYuan Du, Lorenzo Ducci, QingMei Fan, Yannick Favre, Fabio Fuschino, José Luis Gálvez, Min Gao, MingYu Ge, Olivier Gevin, Marco Grassi, QuanYing Gu, YuDong Gu, DaWei Han, Bin Hong, Wei Hu, Long Ji, ShuMei Jia, WeiChun Jiang, Thomas Kennedy, Ingo Kreykenbohm, Irfan Kuvvetli, Claudio Labanti, Luca Latronico, Gang Li, MaoShun Li, Xian Li, Wei Li, ZhengWei Li, Olivier Limousin, HongWei Liu, XiaoJing Liu, Bo Lu, Tao Luo, Daniele Macera, Piero Malcovati, Adrian Martindale, Malgorzata Michalska, Bin Meng, Massimo Minuti, Alfredo Morbidini, Fabio Muleri, Stephane Paltani, Emanuele Perinati, Antonino Picciotto, Claudio Piemonte, JinLu Qu, Alexandre Rachevski, Irina Rashevskaya, Jerome Rodriguez, Thomas Schanz, ZhengXiang Shen, LiZhi Sheng, JiangBo Song, LiMing Song, Carmelo Sgro, Liang Sun, Ying Tan, Phil Uttley, Bo Wang, DianLong Wang, GuoFeng Wang, Juan Wang, LangPing Wang, YuSa Wang, Anna L. Watts, XiangYang Wen, Jörn Wilms, ShaoLin Xiong, JiaWei Yang, Sheng Yang, YanJi Yang, Nian Yu, WenDa Zhang, Gianluigi Zampa, Nicola Zampa, Andrzej A. Zdziarski, AiMei Zhang, ChengMo Zhang, Fan Zhang, Long Zhang, Tong Zhang, Yi Zhang, XiaoLi Zhang, ZiLiang Zhang, BaoSheng Zhao, ShiJie Zheng, YuPeng Zhou, Nicola Zorzi, J. Frans Zwart, ITA, GBR, FRA, DEU, ESP, DNK, POL, CZE, CHN, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, eXTP, Zhang, ShuangNan, Santangelo, Andrea, Feroci, Marco, Xu, YuPeng, Lu, FangJun, Chen, Yong, Feng, Hua, Zhang, Shu, Brandt, Søren, Hernanz, Margarita, Baldini, Luca, Bozzo, Enrico, Campana, Riccardo, De Rosa, Alessandra, Dong, YongWei, Evangelista, Yuri, Karas, Vladimir, Meidinger, Norbert, Meuris, Aline, Nandra, Kirpal, Pan, Teng, Pareschi, Giovanni, Orleanski, Piotr, Huang, QiuShi, Schanne, Stephane, Sironi, Giorgia, Spiga, Daniele, Svoboda, Jiri, Tagliaferri, Gianpiero, Tenzer, Christoph, Vacchi, Andrea, Zane, Silvia, Walton, Dave, Wang, ZhanShan, Winter, Berend, Wu, Xin, in’ t Zand, Jean J. M., Ahangarianabhari, Mahdi, Ambrosi, Giovanni, Ambrosino, Filippo, Barbera, Marco, Basso, Stefano, Bayer, Jörg, Bellazzini, Ronaldo, Bellutti, Pierluigi, Bertucci, Bruna, Bertuccio, Giuseppe, Borghi, Giacomo, Cao, XueLei, Cadoux, Franck, Ceraudo, Francesco, Chen, TianXiang, Chen, YuPeng, Chevenez, Jerome, Civitani, Marta, Cui, Wei, Cui, WeiWei, Dauser, Thoma, Del Monte, Ettore, Di Cosimo, Sergio, Diebold, Sebastian, Doroshenko, Victor, Dovciak, Michal, Du, YuanYuan, Ducci, Lorenzo, Fan, QingMei, Favre, Yannick, Fuschino, Fabio, Gálvez, José Lui, Gao, Min, Ge, MingYu, Gevin, Olivier, Grassi, Marco, Gu, QuanYing, Gu, YuDong, Han, DaWei, Hong, Bin, Hu, Wei, Ji, Long, Jia, ShuMei, Jiang, WeiChun, Kennedy, Thoma, Kreykenbohm, Ingo, Kuvvetli, Irfan, Labanti, Claudio, Latronico, Luca, Li, Gang, Li, MaoShun, Li, Xian, Li, Wei, Li, ZhengWei, Limousin, Olivier, Liu, HongWei, Liu, XiaoJing, Lu, Bo, Luo, Tao, Macera, Daniele, Malcovati, Piero, Martindale, Adrian, Michalska, Malgorzata, Meng, Bin, Minuti, Massimo, Morbidini, Alfredo, Muleri, Fabio, Paltani, Stephane, Perinati, Emanuele, Picciotto, Antonino, Piemonte, Claudio, Qu, JinLu, Rachevski, Alexandre, Rashevskaya, Irina, Rodriguez, Jerome, Schanz, Thoma, Shen, ZhengXiang, Sheng, LiZhi, Song, JiangBo, Song, LiMing, Sgro, Carmelo, Sun, Liang, Tan, Ying, Uttley, Phil, Wang, Bo, Wang, DianLong, Wang, GuoFeng, Wang, Juan, Wang, LangPing, Wang, YuSa, Watts, Anna L., Wen, XiangYang, Wilms, Jörn, Xiong, ShaoLin, Yang, JiaWei, Yang, Sheng, Yang, YanJi, Yu, Nian, Zhang, WenDa, Zampa, Gianluigi, Zampa, Nicola, Zdziarski, Andrzej A., Zhang, AiMei, Zhang, ChengMo, Zhang, Fan, Zhang, Long, Zhang, Tong, Zhang, Yi, Zhang, XiaoLi, Zhang, ZiLiang, Zhao, BaoSheng, Zheng, ShiJie, Zhou, YuPeng, Zorzi, Nicola, Zwart, J. Frans, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Gravity (chemistry), Computer science, space mission: eXTP, X-ray timing, Polarimetry, General Physics and Astronomy, FOS: Physical sciences, 01 natural sciences, 7. Clean energy, Physics and Astronomy (all), Settore FIS/05 - Astronomia E Astrofisica, Observatory, X-ray instrumentation, 0103 physical sciences, X-ray polarimetry, Ground segment, Aerospace engineering, 010306 general physics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), High Energy Astrophysical Phenomena (astro-ph.HE), Spacecraft, sezele, business.industry, Payload, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, Space Science, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: In this paper we present the enhanced X-ray Timing and Polarimetry mission - eXTP. eXTP is a space science mission designed to study fundamental physics under extreme conditions of density, gravity and magnetism. The mission aims at determining the equation of state of matter at supra-nuclear density, measuring effects of QED, and understanding the dynamics of matter in strong-field gravity. In addition to investigating fundamental physics, eXTP will be a very powerful observatory for astrophysics that will provide observations of unprecedented quality on a variety of galactic and extragalactic objects. In particular, its wide field monitoring capabilities will be highly instrumental to detect the electro-magnetic counterparts of gravitational wave sources. The paper provides a detailed description of: (1) the technological and technical aspects, and the expected performance of the instruments of the scientific payload; (2) the elements and functions of the mission, from the spacecraft to the ground segment., Accepted for publication on Sci. China Phys. Mech. Astron. (2019)
Published: 2019
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