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140 results on '"Rodriguez, Jerome"'

1. Drop in the hard pulsed fraction and a candidate cyclotron line in IGR J16320-4751 seen by NuSTAR

Author: Bodaghee, Arash, Chiu, Alan J. -L., Tomsick, John A., Bhalerao, Varun, Bottacini, Eugenio, Clavel, Maica, Cox, Cody, Fürst, Felix, Middleton, Matthew J., Rahoui, Farid, Rodriguez, Jerome, Romano, Pat, Wilms, Joern, Bodaghee, Arash, Chiu, Alan J. -L., Tomsick, John A., Bhalerao, Varun, Bottacini, Eugenio, Clavel, Maica, Cox, Cody, Fürst, Felix, Middleton, Matthew J., Rahoui, Farid, Rodriguez, Jerome, Romano, Pat, and Wilms, Joern
Abstract: We report on a timing and spectral analysis of a 50-ks NuSTAR observation of IGR J16320-4751 (= AX J1631.9-4752); a high-mass X-ray binary hosting a slowly-rotating neutron star. In this observation from 2015, the spin period was 1,308.8+/-0.4 s giving a period derivative dP/dt ~ 2E-8 s s-1 when compared with the period measured in 2004. In addition, the pulsed fraction decreased as a function of energy, as opposed to the constant trend that was seen previously. This suggests a change in the accretion geometry of the system during the intervening 11 years. The phase-averaged spectra were fit with the typical model for accreting pulsars: a power law with an exponential cutoff. This left positive residuals at 6.4 keV attributable to the known iron K-alpha line, as well as negative residuals around 14 keV from a candidate cyclotron line detected at a significance of 5-sigma. We found no significant differences in the spectral parameters across the spin period, other than the expected changes in flux and component normalizations. A flare lasting around 5 ks was captured during the first half of the observation where the X-ray emission hardened and the local column density decreased. Finally, the binary orbital period was refined to 8.9912+/-0.0078 d thanks to Swift/BAT monitoring data from 2005-2022., Comment: 17 pages, 11 figures, Referee-revised version accepted for publication in the Astrophysical Journal
Published: 2023
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2. Chasing the break: Tracing the full evolution of a black hole X-ray binary jet with multi-wavelength spectral modeling

Author: Echiburú-Trujillo, Constanza, Tetarenko, Alexandra J., Haggard, Daryl, Russell, Thomas D., Koljonen, Karri I. I., Bahramian, Arash, Wang, Jingyi, Bremer, Michael, Bright, Joe, Casella, Piergiorgio, Russell, David M., Altamirano, Diego, Baglio, M. Cristina, Belloni, Tomaso, Ceccobello, Chiara, Corbel, Stephane, Trigo, Maria Diaz, Maitra, Dipankar, Gabuya, Aldrin, Gallo, Elena, Heinz, Sebastian, Homan, Jeroen, Kara, Erin, Körding, Elmar, Lewis, Fraser, Lucchini, Matteo, Markoff, Sera, Migliari, Simone, Miller-Jones, James C. A., Rodriguez, Jerome, Saikia, Payaswini, Sarazin, Craig L., Shahbaz, Tariq, Sivakoff, Gregory, Soria, Roberto, Testa, Vincenzo, Tetarenko, Bailey E., Tudose, Valeriu, Echiburú-Trujillo, Constanza, Tetarenko, Alexandra J., Haggard, Daryl, Russell, Thomas D., Koljonen, Karri I. I., Bahramian, Arash, Wang, Jingyi, Bremer, Michael, Bright, Joe, Casella, Piergiorgio, Russell, David M., Altamirano, Diego, Baglio, M. Cristina, Belloni, Tomaso, Ceccobello, Chiara, Corbel, Stephane, Trigo, Maria Diaz, Maitra, Dipankar, Gabuya, Aldrin, Gallo, Elena, Heinz, Sebastian, Homan, Jeroen, Kara, Erin, Körding, Elmar, Lewis, Fraser, Lucchini, Matteo, Markoff, Sera, Migliari, Simone, Miller-Jones, James C. A., Rodriguez, Jerome, Saikia, Payaswini, Sarazin, Craig L., Shahbaz, Tariq, Sivakoff, Gregory, Soria, Roberto, Testa, Vincenzo, Tetarenko, Bailey E., and Tudose, Valeriu
Abstract: Black hole X-ray binaries (BH XRBs) are ideal targets to study the connection between accretion inflow and jet outflow. Here we present quasi-simultaneous, multi-wavelength observations of the Galactic black hole system MAXI J1820+070, throughout its 2018-2019 outburst. Our data set includes coverage from the radio through X-ray bands from 17 different instruments/telescopes, and encompasses 19 epochs over a 7 month time period, resulting in one of the most well-sampled multi-wavelength data sets of a BH XRB outburst to date. With our data, we compile and model the broad-band spectra of this source using a phenomenological model that includes emission from the jet, companion star, and accretion flow. This modeling allows us to track the evolution of the spectral break in the jet spectrum, a key observable that samples the jet launching region. We find that the spectral break location changes over at least $\approx3$ orders of magnitude in electromagnetic frequency over this period. Using these spectral break measurements, we link the full cycle of jet behavior, including the rising, quenching, and re-ignition, to the changing accretion flow properties as the source evolves through its different accretion states. Our analyses show a consistent jet behavior with other sources in similar phases of their outbursts, reinforcing that the jet quenching and recovery may be a global feature of BH XRB systems in outburst. Our results also provide valuable evidence supporting a close connection between the geometry of the inner accretion flow and the base of the jet., Comment: Accepted for publication in ApJ
Published: 2023
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3. Are Low-Frequency Quasi-Periodic Oscillations seen in accretion flows the disk response to a jet instability?

Author: Ferreira, Jonathan, Marcel, Gregoire, Petrucci, Pierre-Olivier, Rodriguez, Jerome, Malzac, Julien, Belmont, Renaud, Clavel, Maica, Henri, Gilles, Corbel, Stephane, Coriat, Mickael, Ferreira, Jonathan, Marcel, Gregoire, Petrucci, Pierre-Olivier, Rodriguez, Jerome, Malzac, Julien, Belmont, Renaud, Clavel, Maica, Henri, Gilles, Corbel, Stephane, and Coriat, Mickael
Abstract: Low Frequency Quasi-Periodic Oscillations or LF QPOs are ubiquitous in BH X-ray binaries and provide strong constraints on the accretion-ejection processes. Although several models have been proposed so far, none has been proven to reproduce all observational constraints and no consensus has emerged yet. We make the conjecture that disks are threaded by a large scale vertical magnetic field that splits it into two radial zones. In the inner Jet Emitting Disk (JED), a near equipartition field allows to drive powerful self-collimated jets, while beyond a transition radius, the disk magnetization is too low and a Standard Accretion Disk (SAD) is settled. In a series of papers, this hybrid JED-SAD disk configuration has been shown to successfully reproduce most multi-wavelength (radio and X-rays) observations, as well as the concurrence with the LFQPOs for the archetypal source GX 339-4. We first analyze the main QPO scenarios provided in the literature: 1) a specific process occurring at the transition radius, 2) the accretion-ejection instability and 3) the solid-body Lense-Thirring disk precession. We recall their main assumptions and shed light on some severe theoretical issues that question the capability to reproduce LF QPOs. We then argue that none of these models could be operating under the JED-SAD physical conditions. We finally propose an alternative scenario where LF QPOs would be the disk response to an instability triggered in the jets, near a magnetic recollimation zone. Such a situation could account for most Type-C QPO phenomenology and is consistent with the global behavior of black hole binaries. The calculation of this non-destructive jet instability remains however to be done. If the existence of this instability is numerically confirmed, then it could also naturally account for the jet wobbling phenomenology seen in various accreting sources., Comment: 11 pages, 1 figure, accepted for publication in Astronomy & Astrophysics
Published: 2022
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4. The enhanced X-ray Timing and Polarimetry mission – eXTP:an update on its scientific cases, mission profile and development status

Author: den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Zhang, Shuang Nan, Santangelo, Andrea, Xu, Yupeng, Feroci, Marco, Hernanz, Margarita, Lu, Fangjun, Chen, Yong, Feng, Hua, Nandra, Kirpal, Jiang, Weichun, Svoboda, Jiri, Brandt, Søren, Schanne, Stéphane, Zand, Jean, Michalska, Malgorzata, Bozzo, Enrico, Kalemci, Emrah, Agudo, Ivan, Ahangarianabhari, Mahdi, Aitink-Kroes, Gabby, Ambrosi, Giovanni, Ambrosino, Filippo, An, Zhenghua, Perez Torres, Miguel Angel, Antonelli, Matias, Argan, Andrea, Babinec, Viktor, Baldini, Luca, Barbera, Marco, van Baren, Coen, Baudin, David, Bayer, Jörg, Bellazzini, Ronaldo, Bellutti, Pierluigi, Bertucci, Bruna, Bertuccio, Giuseppe, Bi, Xingzi, Boezio, Mirko, Bonvicini, Valter, Bonvicini, Walter, Bordas, Pol, Borghese, Alice, Borghi, Giacomo, Bouyjou, Florent, Bozkurt, Ayhan, Brez, Alessandro, Brienza, Daniele, Cadoux, Franck, Campana, Riccardo, Cao, Jiewei, Cao, Xuelei, Casares, Jorge, Cavazzuti, Elisabetta, Ceraudo, Francesco, Chen, Tianxiang, Chen, Wen, Chen, Can, Chen, Yupeng, Chen, Xin, Chen, Yehai, Chenevez, Jerome, Cheng, Yaodong, Cirrincione, Daniela, Civitani, Marta, Cong, Min, Zelati, Francesco Coti, Cui, Weiwei, Cui, Tao, Cui, Wei, Dai, Boyu, Dauser, Thomas, De Angelis, Nicolas, De Marco, Barbara, De Rosa, Alessandra, Monte, Ettore Del, Cosimo, Sergio Di, Diebold, Sebastian, Dilillo, Giuseppe, Ding, Fei, Dohnal, Roman, Dong, Zefang, Donnarumma, Immacolata, Dovciak, Michal, Du, Yuanyuan, Ducci, Lorenzo, Evangelista, Yuri, Fan, Qingmei, Favre, Yannick, Ferrés, Patrícia, Fiandrini, Emanuele, Ficorella, Francesco, Fuschino, Fabio, Gálvez, José Luis, Gao, Na, Gao, Min, Ge, Yuqiang, Ge, Mingyu, Gevin, Olivier, Grassi, Marco, Gu, Yudong, Gu, Quanying, Guan, Ju, Guedel, Manuel, Han, Xingbo, Han, Dawei, He, Huilin, He, Junwang, Hedderman, Paul, den Herder, Jan Willem, Hong, Bin, Hormaetxe, Ander, Hou, Dongjie, Hu, Zexun, Hu, Hao, Hu, Qingbao, Hu, Yu, Huang, Yue, Huang, Jiangjiang, Huang, Qiushi, Huo, Jia, Hynek, Richard, Iwasawa, Kazumi, Izzo, Lucca, Ji, Long, Jia, Shumei, Jiang, Bowen, Jiang, Wei, Jiang, Jiechen, Jiang, Xiaowei, Jiao, Yang, Jin, Ge, Jin, Fan, Jose, Jordi, Karas, Vladimir, Kennedy, Thomas, Kirsch, Christian, Kole, Merlin, Komarek, Martin, Kreykenbohm, Ingo, Kuiper, Lucien, Kuvvetli, Irfan, Labanti, Claudio, Latronico, Luca, Laubert, Phillip, Li, Tao, Li, Longhui, Li, Hong, Li, Duo, Li, Wei, Li, Maoshun, Li, Gang, Li, Xiaobo, Li, Chengkui, Li, Bing, Li, Haibo, Liang, Hong, Liao, Qiuyan, Liao, Jinyuan, Limousin, Olivier, Lin, Yanjian, Linares, Manuel, Liu, Rui, Liu, Yichen, Liu, Zhihao, Liu, Hongwei, Liu, Xiaojing, Liu, Xiaohua, Cicero, Ugo Lo, Loehring, Jens, Lombardi, Giovanni, Lorenz, Maximilian, Lu, Bing, Lucchesi, Leonardo, Luo, Tao, Luo, Laidan, Ma, Jia, Ma, Xiang, Macera, Daniele, Malcovati, Piero, Manfreda, Alberto, Paredes, Josep Maria, Marinucci, Andrea, Martindale, Adrian, Meidinger, Norbert, Mele, Filippo, Mendes, Vasco, Meng, Bin, Merkl, Martin, Meuris, Aline, Miniutti, Giovanni, Minuti, Massimo, Morbidini, Alfredo, Morgante, Gianluca, Muleri, Fabio, Munini, Riccardo, Mussolin, Lorenzo, Negri, Barbara, Nie, Jianyin, Novák, Petr, Nowosielski, Witold, Nuti, Alessio, Onat, Ahmet, Orleanski, Piotr, Orsini, Leonardo, Ottensamer, Roland, Ou, Ge, Pacciani, Luigi, Paltani, Stephane, Pan, Teng, Pan, Kai, Pareschi, Giovanni, Patruno, Alessandro, Pepponi, Giancarlo, Perinati, Emanuele, Piazzolla, Raffaele, Picciotto, Antonino, Piemonte, Claudio, Pinchera, Michele, Pliego, Samuel, Poutanen, Juri, Qi, Liqiang, Qi, Fazhi, Qiang, Pengfei, Qiao, Fangjian, Qiao, Zheng, Qiu, Xiangbiao, Qiu, Chengbo, Qu, Jinlu, Rachevski, Alexandre, Rashevskaia, Irina, Rea, Nanda, Ribo, Marc, de la Rie, Rob, Rodriguez, Jerome, Gil, Pablo Rodríguez, Sala, Gloria, Schanz, Thomas, Serafinelli, Roberto, Sgro, Carmelo, Shen, Zhengxiang, Sheng, Lizhi, Shi, Jingyan, Sironi, Giorgia, Skup, Konrad, Song, Liming, Song, Zeyu, Song, Jiangbo, Spandre, Gloria, Spiga, Daniele, Su, Yongquan, Sun, Liang, Sungur, Müberra, Svéda, Libor, Tagliaferri, Gianpiero, Tan, Ying, Tao, Lian, Tcherniak, Denis, Tenzer, Chris, Todaro, Michela, Tolos, Laura, Torok, Gabriel, Torres, Diego F., Trois, Alessio, Turhan, Onur, Uttley, Phil, Vacchi, Andrea, Virgilli, Enrico, Vogel, Channah, Walton, Dave, Wang, Jian, Wang, Xianqi, Wang, Bo, Wang, Langping, Wang, Xiaofeng, Wang, Dianlong, Wang, Yusa, Wang, Juan, Wang, Hao, Wang, Ruijie, Wang, Ping, Wang, Lingjun, Wang, Wenshuai, Wang, Tian, Wang, Haoyu, Wang, Zhanshan, Watts, Anna L., Wen, Xiangyang, Wilms, Jörn, Winter, Berend, Wu, Xin, Wu, Chao, Wu, Zhenyu, Wu, Qiong, Wu, Kaiji, Xiong, Hao, Xiong, Shaolin, Xu, Wei, Xu, Zhao, Xu, Jingjing, Xu, Xiongwei, Xue, Jiadai, Yan, Yongqing, Yan, Xingtao, Yang, Xianghui, Yang, Yanji, Yang, Xiongtao, Yang, Sheng, Yang, Jiawei, Yang, Yingquan, Yi, Shuxu, Yu, Yonggao, Yu, Ke, Zampa, Ganluigi, Zampa, Nicola, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Long, Zhang, Shu, Zhang, Wenda, Zhang, Xiaoli, Zhang, Zhen, Zhang, Jiawei, Zhang, Fan, Zhang, Ziliang, Zhang, Dali, Zhang, Honglin, Zhang, Aimei, Zhang, Tong, Zhang, Hongmei, Zhang, Juan, Zhang, Liang, Zhang, Yueting, Zhao, Li, Zhao, Baosheng, Zhao, Zijian, Zhao, Xiaofan, Zhao, Haisheng, Zhao, Xiaoyun, Zheng, Shijie, Zhou, Yupeng, Zhou, Xiaohong, Zhu, Jiahuan, Zhu, Yuxuan, Zhu, Cheng, Zhu, Zhencai, Zorzi, Nicola, Zwart, Frans, den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Zhang, Shuang Nan, Santangelo, Andrea, Xu, Yupeng, Feroci, Marco, Hernanz, Margarita, Lu, Fangjun, Chen, Yong, Feng, Hua, Nandra, Kirpal, Jiang, Weichun, Svoboda, Jiri, Brandt, Søren, Schanne, Stéphane, Zand, Jean, Michalska, Malgorzata, Bozzo, Enrico, Kalemci, Emrah, Agudo, Ivan, Ahangarianabhari, Mahdi, Aitink-Kroes, Gabby, Ambrosi, Giovanni, Ambrosino, Filippo, An, Zhenghua, Perez Torres, Miguel Angel, Antonelli, Matias, Argan, Andrea, Babinec, Viktor, Baldini, Luca, Barbera, Marco, van Baren, Coen, Baudin, David, Bayer, Jörg, Bellazzini, Ronaldo, Bellutti, Pierluigi, Bertucci, Bruna, Bertuccio, Giuseppe, Bi, Xingzi, Boezio, Mirko, Bonvicini, Valter, Bonvicini, Walter, Bordas, Pol, Borghese, Alice, Borghi, Giacomo, Bouyjou, Florent, Bozkurt, Ayhan, Brez, Alessandro, Brienza, Daniele, Cadoux, Franck, Campana, Riccardo, Cao, Jiewei, Cao, Xuelei, Casares, Jorge, Cavazzuti, Elisabetta, Ceraudo, Francesco, Chen, Tianxiang, Chen, Wen, Chen, Can, Chen, Yupeng, Chen, Xin, Chen, Yehai, Chenevez, Jerome, Cheng, Yaodong, Cirrincione, Daniela, Civitani, Marta, Cong, Min, Zelati, Francesco Coti, Cui, Weiwei, Cui, Tao, Cui, Wei, Dai, Boyu, Dauser, Thomas, De Angelis, Nicolas, De Marco, Barbara, De Rosa, Alessandra, Monte, Ettore Del, Cosimo, Sergio Di, Diebold, Sebastian, Dilillo, Giuseppe, Ding, Fei, Dohnal, Roman, Dong, Zefang, Donnarumma, Immacolata, Dovciak, Michal, Du, Yuanyuan, Ducci, Lorenzo, Evangelista, Yuri, Fan, Qingmei, Favre, Yannick, Ferrés, Patrícia, Fiandrini, Emanuele, Ficorella, Francesco, Fuschino, Fabio, Gálvez, José Luis, Gao, Na, Gao, Min, Ge, Yuqiang, Ge, Mingyu, Gevin, Olivier, Grassi, Marco, Gu, Yudong, Gu, Quanying, Guan, Ju, Guedel, Manuel, Han, Xingbo, Han, Dawei, He, Huilin, He, Junwang, Hedderman, Paul, den Herder, Jan Willem, Hong, Bin, Hormaetxe, Ander, Hou, Dongjie, Hu, Zexun, Hu, Hao, Hu, Qingbao, Hu, Yu, Huang, Yue, Huang, Jiangjiang, Huang, Qiushi, Huo, Jia, Hynek, Richard, Iwasawa, Kazumi, Izzo, Lucca, Ji, Long, Jia, Shumei, Jiang, Bowen, Jiang, Wei, Jiang, Jiechen, Jiang, Xiaowei, Jiao, Yang, Jin, Ge, Jin, Fan, Jose, Jordi, Karas, Vladimir, Kennedy, Thomas, Kirsch, Christian, Kole, Merlin, Komarek, Martin, Kreykenbohm, Ingo, Kuiper, Lucien, Kuvvetli, Irfan, Labanti, Claudio, Latronico, Luca, Laubert, Phillip, Li, Tao, Li, Longhui, Li, Hong, Li, Duo, Li, Wei, Li, Maoshun, Li, Gang, Li, Xiaobo, Li, Chengkui, Li, Bing, Li, Haibo, Liang, Hong, Liao, Qiuyan, Liao, Jinyuan, Limousin, Olivier, Lin, Yanjian, Linares, Manuel, Liu, Rui, Liu, Yichen, Liu, Zhihao, Liu, Hongwei, Liu, Xiaojing, Liu, Xiaohua, Cicero, Ugo Lo, Loehring, Jens, Lombardi, Giovanni, Lorenz, Maximilian, Lu, Bing, Lucchesi, Leonardo, Luo, Tao, Luo, Laidan, Ma, Jia, Ma, Xiang, Macera, Daniele, Malcovati, Piero, Manfreda, Alberto, Paredes, Josep Maria, Marinucci, Andrea, Martindale, Adrian, Meidinger, Norbert, Mele, Filippo, Mendes, Vasco, Meng, Bin, Merkl, Martin, Meuris, Aline, Miniutti, Giovanni, Minuti, Massimo, Morbidini, Alfredo, Morgante, Gianluca, Muleri, Fabio, Munini, Riccardo, Mussolin, Lorenzo, Negri, Barbara, Nie, Jianyin, Novák, Petr, Nowosielski, Witold, Nuti, Alessio, Onat, Ahmet, Orleanski, Piotr, Orsini, Leonardo, Ottensamer, Roland, Ou, Ge, Pacciani, Luigi, Paltani, Stephane, Pan, Teng, Pan, Kai, Pareschi, Giovanni, Patruno, Alessandro, Pepponi, Giancarlo, Perinati, Emanuele, Piazzolla, Raffaele, Picciotto, Antonino, Piemonte, Claudio, Pinchera, Michele, Pliego, Samuel, Poutanen, Juri, Qi, Liqiang, Qi, Fazhi, Qiang, Pengfei, Qiao, Fangjian, Qiao, Zheng, Qiu, Xiangbiao, Qiu, Chengbo, Qu, Jinlu, Rachevski, Alexandre, Rashevskaia, Irina, Rea, Nanda, Ribo, Marc, de la Rie, Rob, Rodriguez, Jerome, Gil, Pablo Rodríguez, Sala, Gloria, Schanz, Thomas, Serafinelli, Roberto, Sgro, Carmelo, Shen, Zhengxiang, Sheng, Lizhi, Shi, Jingyan, Sironi, Giorgia, Skup, Konrad, Song, Liming, Song, Zeyu, Song, Jiangbo, Spandre, Gloria, Spiga, Daniele, Su, Yongquan, Sun, Liang, Sungur, Müberra, Svéda, Libor, Tagliaferri, Gianpiero, Tan, Ying, Tao, Lian, Tcherniak, Denis, Tenzer, Chris, Todaro, Michela, Tolos, Laura, Torok, Gabriel, Torres, Diego F., Trois, Alessio, Turhan, Onur, Uttley, Phil, Vacchi, Andrea, Virgilli, Enrico, Vogel, Channah, Walton, Dave, Wang, Jian, Wang, Xianqi, Wang, Bo, Wang, Langping, Wang, Xiaofeng, Wang, Dianlong, Wang, Yusa, Wang, Juan, Wang, Hao, Wang, Ruijie, Wang, Ping, Wang, Lingjun, Wang, Wenshuai, Wang, Tian, Wang, Haoyu, Wang, Zhanshan, Watts, Anna L., Wen, Xiangyang, Wilms, Jörn, Winter, Berend, Wu, Xin, Wu, Chao, Wu, Zhenyu, Wu, Qiong, Wu, Kaiji, Xiong, Hao, Xiong, Shaolin, Xu, Wei, Xu, Zhao, Xu, Jingjing, Xu, Xiongwei, Xue, Jiadai, Yan, Yongqing, Yan, Xingtao, Yang, Xianghui, Yang, Yanji, Yang, Xiongtao, Yang, Sheng, Yang, Jiawei, Yang, Yingquan, Yi, Shuxu, Yu, Yonggao, Yu, Ke, Zampa, Ganluigi, Zampa, Nicola, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Long, Zhang, Shu, Zhang, Wenda, Zhang, Xiaoli, Zhang, Zhen, Zhang, Jiawei, Zhang, Fan, Zhang, Ziliang, Zhang, Dali, Zhang, Honglin, Zhang, Aimei, Zhang, Tong, Zhang, Hongmei, Zhang, Juan, Zhang, Liang, Zhang, Yueting, Zhao, Li, Zhao, Baosheng, Zhao, Zijian, Zhao, Xiaofan, Zhao, Haisheng, Zhao, Xiaoyun, Zheng, Shijie, Zhou, Yupeng, Zhou, Xiaohong, Zhu, Jiahuan, Zhu, Yuxuan, Zhu, Cheng, Zhu, Zhencai, Zorzi, Nicola, and Zwart, Frans
Abstract: The enhanced X-ray Timing and Polarimetry mission (eXTP) is a flagship observatory for X-ray timing, spectroscopy and polarimetry developed by an International Consortium. Thanks to its very large collecting area, good spectral resolution and unprecedented polarimetry capabilities, eXTP will explore the properties of matter and the propagation of light in the most extreme conditions found in the Universe. eXTP will, in addition, be a powerful X-ray observatory. The mission will continuously monitor the X-ray sky, and will enable multiwavelength and multi-messenger studies. The mission is currently in phase B, which will be completed in the middle of 2022.
Published: 2022

5. 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, Parra, Maxime, 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
Abstract: In our self-similar, analytical, magneto-hydrodynamic (MHD) accretion-ejection solution, the density at the base of the outflow is explicitly dependent on the disk accretion rate - a unique property of this class of solutions. We had earlier found that the ejection index $p >\sim 0.1 (\dot{M}_{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 3 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 disk, $\rm{r_o|_{max}} = 10^5, \, 10^6 \,\, \rm{r_G}$, and the angle of the line of sight, $i \sim 10 - 25^{\circ}$. 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 ksec 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 $10^4 - 10^5$ even for the least favourable simulated cases., Comment: 18 pages, 13 figures in the main body and 3 figures in the appendix. Accepted for publication in MNRAS
Published: 2022
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6. A multi-wavelength study of GRS 1716-249 in outburst : constraints on its system parameters

Author: Saikia, Payaswini, Russell, David M., Baglio, M. C., Bramich, D. M., Casella, Piergiorgio, Trigo, M. Diaz, Gandhi, Poshak, Jiang, Jiachen, Maccarone, Thomas, Soria, Roberto, Noori, Hind Al, Yazeedi, Aisha Al, Alabarta, Kevin, Belloni, Tomaso, Bel, Marion Cadolle, Ceccobello, Chiara, Corbel, Stephane, 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., Saikia, Payaswini, Russell, David M., Baglio, M. C., Bramich, D. M., Casella, Piergiorgio, Trigo, M. Diaz, Gandhi, Poshak, Jiang, Jiachen, Maccarone, Thomas, Soria, Roberto, Noori, Hind Al, Yazeedi, Aisha Al, Alabarta, Kevin, Belloni, Tomaso, Bel, Marion Cadolle, Ceccobello, Chiara, Corbel, Stephane, 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, and Tetarenko, Alexandra J.
Abstract: 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 also report the long-term optical light curve of the source and find that the quiescent i-band magnitude is 21.39$\pm$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 dataset to those of other outbursting black hole X-ray binaries, we find that while GRS 1716-249 shows similar X-ray behaviour, 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 $\sim$4-8 kpc., Comment: Accepted for publication in The Astrophysical Journal
Published: 2022
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7. Are Low-Frequency Quasi-Periodic Oscillations seen in accretion flows the disk response to a jet instability?

Author: Ferreira, Jonathan, Marcel, Gregoire, Petrucci, Pierre-Olivier, Rodriguez, Jerome, Malzac, Julien, Belmont, Renaud, Clavel, Maica, Henri, Gilles, Corbel, Stephane, Coriat, Mickael, Ferreira, Jonathan, Marcel, Gregoire, Petrucci, Pierre-Olivier, Rodriguez, Jerome, Malzac, Julien, Belmont, Renaud, Clavel, Maica, Henri, Gilles, Corbel, Stephane, and Coriat, Mickael
Abstract: Low Frequency Quasi-Periodic Oscillations or LF QPOs are ubiquitous in BH X-ray binaries and provide strong constraints on the accretion-ejection processes. Although several models have been proposed so far, none has been proven to reproduce all observational constraints and no consensus has emerged yet. We make the conjecture that disks are threaded by a large scale vertical magnetic field that splits it into two radial zones. In the inner Jet Emitting Disk (JED), a near equipartition field allows to drive powerful self-collimated jets, while beyond a transition radius, the disk magnetization is too low and a Standard Accretion Disk (SAD) is settled. In a series of papers, this hybrid JED-SAD disk configuration has been shown to successfully reproduce most multi-wavelength (radio and X-rays) observations, as well as the concurrence with the LFQPOs for the archetypal source GX 339-4. We first analyze the main QPO scenarios provided in the literature: 1) a specific process occurring at the transition radius, 2) the accretion-ejection instability and 3) the solid-body Lense-Thirring disk precession. We recall their main assumptions and shed light on some severe theoretical issues that question the capability to reproduce LF QPOs. We then argue that none of these models could be operating under the JED-SAD physical conditions. We finally propose an alternative scenario where LF QPOs would be the disk response to an instability triggered in the jets, near a magnetic recollimation zone. Such a situation could account for most Type-C QPO phenomenology and is consistent with the global behavior of black hole binaries. The calculation of this non-destructive jet instability remains however to be done. If the existence of this instability is numerically confirmed, then it could also naturally account for the jet wobbling phenomenology seen in various accreting sources., Comment: 11 pages, 1 figure, accepted for publication in Astronomy & Astrophysics
Published: 2022
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8. Evidence for low kick velocities among high-mass X-ray binaries in the Small Magellanic Cloud from the spatial correlation function

Author: Bodaghee, Arash, Antoniou, Vallia, Zezas, Andreas, Tomsick, John A., Jordan, Zachary, Frechette, Eric, Jackson, Brenton, Agnew, Ryan, Hornschemeier, Ann E., Rodriguez, Jerome, Bodaghee, Arash, Antoniou, Vallia, Zezas, Andreas, Tomsick, John A., Jordan, Zachary, Frechette, Eric, Jackson, Brenton, Agnew, Ryan, Hornschemeier, Ann E., and Rodriguez, Jerome
Abstract: We present the two-point cross-correlation function between high-mass X-ray binaries (HMXBs) in the Small Magellanic Cloud (SMC) and their likely birthplaces (OB Associations: OBAs). This function compares the spatial correlation between the observed HMXB and OBA populations against mock catalogs in which the members are distributed randomly across the sky. A significant correlation (15 sigma) is found for the HMXB and OBA populations when compared with a randomized catalog in which the OBAs are distributed uniformly over the SMC. A less significant correlation (4 sigma) is found for a randomized catalog of OBAs built with a bootstrap method. However, no significant correlation is detected when the randomized catalogs assume the form of a Gaussian ellipsoid or a distribution that reflects the star-formation history from 40 Myr ago. Based on their observed distributions and assuming a range of migration timescales, we infer that the average value of the kick velocity inherited by an HMXB during the formation of its compact object is 2-34 km/s. This is considerably less than the value obtained for their counterparts in the Milky Way hinting that the galactic environment affecting stellar evolution plays a role in setting the average kick velocity of HMXBs., Comment: 10 pages, 7 figures, accepted for publication in the Astrophysical Journal
Published: 2021
Full Text: View/download PDF

9. INTEGRAL reloaded: spacecraft, instruments and ground system

Author: Kuulkers, Erik, Ferrigno, Carlo, Kretschmar, Peter, Alfonso-Garzon, Julia, Baab, Marius, Bazzano, Angela, Belanger, Guillaume, Benson, Ian, Bird, Anthony J., Bozzo, Enrico, Brandt, Soren, Coe, Elliott, Caballero, Isabel, Cangemi, Floriane, Chenevez, Jerome, 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, Gotz, Diego, Gouiffes, Christian, Grebenev, Sergei A., Greiner, Jochen, Gros, Aleksandra, Hanlon, Lorraine, Hermsen, Wim, Hernandez, Cristina, Hernanz, Margarita, Huebner, 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, Jerome, Roques, Jean-Pierre, Donate, Emilio Salazar, Salt, Dave, Sanchez-Fernandez, Celia, Sauvageon, Aymeric, Savchenko, Volodymyr, Sazonov, Sergey Yu., Scaglioni, Stefano, Schartel, Norbert, Siegert, Thomas, Southworth, Richard, Sunyaev, Rashid A., Toma, Liviu, Ubertini, Pietro, Heuvel, Ed P. J. van den, von Kienlin, Andreas, von Krusenstiern, Nikolai, Winkler, Christoph, Wojciech, Hajdas, Zannoni, Ugo, Kuulkers, Erik, Ferrigno, Carlo, Kretschmar, Peter, Alfonso-Garzon, Julia, Baab, Marius, Bazzano, Angela, Belanger, Guillaume, Benson, Ian, Bird, Anthony J., Bozzo, Enrico, Brandt, Soren, Coe, Elliott, Caballero, Isabel, Cangemi, Floriane, Chenevez, Jerome, 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, Gotz, Diego, Gouiffes, Christian, Grebenev, Sergei A., Greiner, Jochen, Gros, Aleksandra, Hanlon, Lorraine, Hermsen, Wim, Hernandez, Cristina, Hernanz, Margarita, Huebner, 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, Jerome, Roques, Jean-Pierre, Donate, Emilio Salazar, Salt, Dave, Sanchez-Fernandez, Celia, Sauvageon, Aymeric, Savchenko, Volodymyr, Sazonov, Sergey Yu., Scaglioni, Stefano, Schartel, Norbert, Siegert, Thomas, Southworth, Richard, Sunyaev, Rashid A., Toma, Liviu, Ubertini, Pietro, Heuvel, Ed P. J. van den, von Kienlin, Andreas, von Krusenstiern, Nikolai, Winkler, Christoph, Wojciech, Hajdas, and Zannoni, Ugo
Abstract: ESA's INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL) was launched on 17 Oct 2002 at 06:41 CEST. Since then, it has been providing long, uninterrupted observations (up to about 47 hr, or 170 ksec, per satellite orbit of 2.7 days) with a large field-of-view (fully coded: 100 deg^2), msec time resolution, keV energy resolution, polarization measurements, as well as additional coverage in the optical. This is realized by two main instruments in the 15 keV to 10 MeV range, the spectrometer SPI (spectral resolution 3 keV at 1.8 MeV) and the imager IBIS (angular resolution 12 arcmin FWHM), complemented by X-ray (JEM-X; 3-35 keV) and optical (OMC; Johnson V-band) monitors. All instruments are co-aligned to simultaneously observe the target region. A particle radiation monitor (IREM) measures charged particle fluxes near the spacecraft. The Anti-coincidence subsystems of the main instruments are also efficient all-sky gamma-ray detectors, which provide omni-directional monitoring above ~75 keV. INTEGRAL can also rapidly (within a couple of hours) re-point and conduct Target of Opportunity observations. INTEGRAL has build an impressive legacy: e.g. discovery of >600 new high-energy sources; first-ever direct detection of 56Ni and 56Co radio-active decay lines from a Type Ia supernova; new insights on positron annihilation in the Galactic bulge and disk; pioneering gamma-ray polarization studies. INTEGRAL is also a successful in multi-messenger astronomy: INTEGRAL found the first prompt electromagnetic radiation in coincidence with a binary neutron star merger. More than 1750 papers based on INTEGRAL data have been published in refereed journals. Here we give a comprehensive update of the satellite status after more than 18 years of operations in a harsh space environment, and an account of the successful Ground Segment., Comment: 29 pages, 20 figures, accepted for publication in special issue of New Astronomy Reviews
Published: 2021

10. INTEGRAL reloaded: spacecraft, instruments and ground system

Author: Kuulkers, Erik, Ferrigno, Carlo, Kretschmar, Peter, Alfonso-Garzon, Julia, Baab, Marius, Bazzano, Angela, Belanger, Guillaume, Benson, Ian, Bird, Anthony J., Bozzo, Enrico, Brandt, Soren, Coe, Elliott, Caballero, Isabel, Cangemi, Floriane, Chenevez, Jerome, 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, Gotz, Diego, Gouiffes, Christian, Grebenev, Sergei A., Greiner, Jochen, Gros, Aleksandra, Hanlon, Lorraine, Hermsen, Wim, Hernandez, Cristina, Hernanz, Margarita, Huebner, 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, Jerome, Roques, Jean-Pierre, Donate, Emilio Salazar, Salt, Dave, Sanchez-Fernandez, Celia, Sauvageon, Aymeric, Savchenko, Volodymyr, Sazonov, Sergey Yu., Scaglioni, Stefano, Schartel, Norbert, Siegert, Thomas, Southworth, Richard, Sunyaev, Rashid A., Toma, Liviu, Ubertini, Pietro, Heuvel, Ed P. J. van den, von Kienlin, Andreas, von Krusenstiern, Nikolai, Winkler, Christoph, Wojciech, Hajdas, Zannoni, Ugo, Kuulkers, Erik, Ferrigno, Carlo, Kretschmar, Peter, Alfonso-Garzon, Julia, Baab, Marius, Bazzano, Angela, Belanger, Guillaume, Benson, Ian, Bird, Anthony J., Bozzo, Enrico, Brandt, Soren, Coe, Elliott, Caballero, Isabel, Cangemi, Floriane, Chenevez, Jerome, 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, Gotz, Diego, Gouiffes, Christian, Grebenev, Sergei A., Greiner, Jochen, Gros, Aleksandra, Hanlon, Lorraine, Hermsen, Wim, Hernandez, Cristina, Hernanz, Margarita, Huebner, 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, Jerome, Roques, Jean-Pierre, Donate, Emilio Salazar, Salt, Dave, Sanchez-Fernandez, Celia, Sauvageon, Aymeric, Savchenko, Volodymyr, Sazonov, Sergey Yu., Scaglioni, Stefano, Schartel, Norbert, Siegert, Thomas, Southworth, Richard, Sunyaev, Rashid A., Toma, Liviu, Ubertini, Pietro, Heuvel, Ed P. J. van den, von Kienlin, Andreas, von Krusenstiern, Nikolai, Winkler, Christoph, Wojciech, Hajdas, and Zannoni, Ugo
Abstract: ESA's INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL) was launched on 17 Oct 2002 at 06:41 CEST. Since then, it has been providing long, uninterrupted observations (up to about 47 hr, or 170 ksec, per satellite orbit of 2.7 days) with a large field-of-view (fully coded: 100 deg^2), msec time resolution, keV energy resolution, polarization measurements, as well as additional coverage in the optical. This is realized by two main instruments in the 15 keV to 10 MeV range, the spectrometer SPI (spectral resolution 3 keV at 1.8 MeV) and the imager IBIS (angular resolution 12 arcmin FWHM), complemented by X-ray (JEM-X; 3-35 keV) and optical (OMC; Johnson V-band) monitors. All instruments are co-aligned to simultaneously observe the target region. A particle radiation monitor (IREM) measures charged particle fluxes near the spacecraft. The Anti-coincidence subsystems of the main instruments are also efficient all-sky gamma-ray detectors, which provide omni-directional monitoring above ~75 keV. INTEGRAL can also rapidly (within a couple of hours) re-point and conduct Target of Opportunity observations. INTEGRAL has build an impressive legacy: e.g. discovery of >600 new high-energy sources; first-ever direct detection of 56Ni and 56Co radio-active decay lines from a Type Ia supernova; new insights on positron annihilation in the Galactic bulge and disk; pioneering gamma-ray polarization studies. INTEGRAL is also a successful in multi-messenger astronomy: INTEGRAL found the first prompt electromagnetic radiation in coincidence with a binary neutron star merger. More than 1750 papers based on INTEGRAL data have been published in refereed journals. Here we give a comprehensive update of the satellite status after more than 18 years of operations in a harsh space environment, and an account of the successful Ground Segment., Comment: 29 pages, 20 figures, accepted for publication in special issue of New Astronomy Reviews
Published: 2021

11. INTEGRAL reloaded: spacecraft, instruments and ground system

Author: Kuulkers, Erik, Ferrigno, Carlo, Kretschmar, Peter, Alfonso-Garzon, Julia, Baab, Marius, Bazzano, Angela, Belanger, Guillaume, Benson, Ian, Bird, Anthony J., Bozzo, Enrico, Brandt, Soren, Coe, Elliott, Caballero, Isabel, Cangemi, Floriane, Chenevez, Jerome, 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, Gotz, Diego, Gouiffes, Christian, Grebenev, Sergei A., Greiner, Jochen, Gros, Aleksandra, Hanlon, Lorraine, Hermsen, Wim, Hernandez, Cristina, Hernanz, Margarita, Huebner, 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, Jerome, Roques, Jean-Pierre, Donate, Emilio Salazar, Salt, Dave, Sanchez-Fernandez, Celia, Sauvageon, Aymeric, Savchenko, Volodymyr, Sazonov, Sergey Yu., Scaglioni, Stefano, Schartel, Norbert, Siegert, Thomas, Southworth, Richard, Sunyaev, Rashid A., Toma, Liviu, Ubertini, Pietro, Heuvel, Ed P. J. van den, von Kienlin, Andreas, von Krusenstiern, Nikolai, Winkler, Christoph, Wojciech, Hajdas, Zannoni, Ugo, Kuulkers, Erik, Ferrigno, Carlo, Kretschmar, Peter, Alfonso-Garzon, Julia, Baab, Marius, Bazzano, Angela, Belanger, Guillaume, Benson, Ian, Bird, Anthony J., Bozzo, Enrico, Brandt, Soren, Coe, Elliott, Caballero, Isabel, Cangemi, Floriane, Chenevez, Jerome, 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, Gotz, Diego, Gouiffes, Christian, Grebenev, Sergei A., Greiner, Jochen, Gros, Aleksandra, Hanlon, Lorraine, Hermsen, Wim, Hernandez, Cristina, Hernanz, Margarita, Huebner, 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, Jerome, Roques, Jean-Pierre, Donate, Emilio Salazar, Salt, Dave, Sanchez-Fernandez, Celia, Sauvageon, Aymeric, Savchenko, Volodymyr, Sazonov, Sergey Yu., Scaglioni, Stefano, Schartel, Norbert, Siegert, Thomas, Southworth, Richard, Sunyaev, Rashid A., Toma, Liviu, Ubertini, Pietro, Heuvel, Ed P. J. van den, von Kienlin, Andreas, von Krusenstiern, Nikolai, Winkler, Christoph, Wojciech, Hajdas, and Zannoni, Ugo
Abstract: ESA's INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL) was launched on 17 Oct 2002 at 06:41 CEST. Since then, it has been providing long, uninterrupted observations (up to about 47 hr, or 170 ksec, per satellite orbit of 2.7 days) with a large field-of-view (fully coded: 100 deg^2), msec time resolution, keV energy resolution, polarization measurements, as well as additional coverage in the optical. This is realized by two main instruments in the 15 keV to 10 MeV range, the spectrometer SPI (spectral resolution 3 keV at 1.8 MeV) and the imager IBIS (angular resolution 12 arcmin FWHM), complemented by X-ray (JEM-X; 3-35 keV) and optical (OMC; Johnson V-band) monitors. All instruments are co-aligned to simultaneously observe the target region. A particle radiation monitor (IREM) measures charged particle fluxes near the spacecraft. The Anti-coincidence subsystems of the main instruments are also efficient all-sky gamma-ray detectors, which provide omni-directional monitoring above ~75 keV. INTEGRAL can also rapidly (within a couple of hours) re-point and conduct Target of Opportunity observations. INTEGRAL has build an impressive legacy: e.g. discovery of >600 new high-energy sources; first-ever direct detection of 56Ni and 56Co radio-active decay lines from a Type Ia supernova; new insights on positron annihilation in the Galactic bulge and disk; pioneering gamma-ray polarization studies. INTEGRAL is also a successful in multi-messenger astronomy: INTEGRAL found the first prompt electromagnetic radiation in coincidence with a binary neutron star merger. More than 1750 papers based on INTEGRAL data have been published in refereed journals. Here we give a comprehensive update of the satellite status after more than 18 years of operations in a harsh space environment, and an account of the successful Ground Segment., Comment: 29 pages, 20 figures, accepted for publication in special issue of New Astronomy Reviews
Published: 2021

12. Evidence for low kick velocities among high-mass X-ray binaries in the Small Magellanic Cloud from the spatial correlation function

Author: Bodaghee, Arash, Antoniou, Vallia, Zezas, Andreas, Tomsick, John A., Jordan, Zachary, Frechette, Eric, Jackson, Brenton, Agnew, Ryan, Hornschemeier, Ann E., Rodriguez, Jerome, Bodaghee, Arash, Antoniou, Vallia, Zezas, Andreas, Tomsick, John A., Jordan, Zachary, Frechette, Eric, Jackson, Brenton, Agnew, Ryan, Hornschemeier, Ann E., and Rodriguez, Jerome
Abstract: We present the two-point cross-correlation function between high-mass X-ray binaries (HMXBs) in the Small Magellanic Cloud (SMC) and their likely birthplaces (OB Associations: OBAs). This function compares the spatial correlation between the observed HMXB and OBA populations against mock catalogs in which the members are distributed randomly across the sky. A significant correlation (15 sigma) is found for the HMXB and OBA populations when compared with a randomized catalog in which the OBAs are distributed uniformly over the SMC. A less significant correlation (4 sigma) is found for a randomized catalog of OBAs built with a bootstrap method. However, no significant correlation is detected when the randomized catalogs assume the form of a Gaussian ellipsoid or a distribution that reflects the star-formation history from 40 Myr ago. Based on their observed distributions and assuming a range of migration timescales, we infer that the average value of the kick velocity inherited by an HMXB during the formation of its compact object is 2-34 km/s. This is considerably less than the value obtained for their counterparts in the Milky Way hinting that the galactic environment affecting stellar evolution plays a role in setting the average kick velocity of HMXBs., Comment: 10 pages, 7 figures, accepted for publication in the Astrophysical Journal
Published: 2021
Full Text: View/download PDF

13. INTEGRAL reloaded: spacecraft, instruments and ground system

Author: Kuulkers, Erik, Ferrigno, Carlo, Kretschmar, Peter, Alfonso-Garzon, Julia, Baab, Marius, Bazzano, Angela, Belanger, Guillaume, Benson, Ian, Bird, Anthony J., Bozzo, Enrico, Brandt, Soren, Coe, Elliott, Caballero, Isabel, Cangemi, Floriane, Chenevez, Jerome, 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, Gotz, Diego, Gouiffes, Christian, Grebenev, Sergei A., Greiner, Jochen, Gros, Aleksandra, Hanlon, Lorraine, Hermsen, Wim, Hernandez, Cristina, Hernanz, Margarita, Huebner, 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, Jerome, Roques, Jean-Pierre, Donate, Emilio Salazar, Salt, Dave, Sanchez-Fernandez, Celia, Sauvageon, Aymeric, Savchenko, Volodymyr, Sazonov, Sergey Yu., Scaglioni, Stefano, Schartel, Norbert, Siegert, Thomas, Southworth, Richard, Sunyaev, Rashid A., Toma, Liviu, Ubertini, Pietro, Heuvel, Ed P. J. van den, von Kienlin, Andreas, von Krusenstiern, Nikolai, Winkler, Christoph, Wojciech, Hajdas, Zannoni, Ugo, Kuulkers, Erik, Ferrigno, Carlo, Kretschmar, Peter, Alfonso-Garzon, Julia, Baab, Marius, Bazzano, Angela, Belanger, Guillaume, Benson, Ian, Bird, Anthony J., Bozzo, Enrico, Brandt, Soren, Coe, Elliott, Caballero, Isabel, Cangemi, Floriane, Chenevez, Jerome, 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, Gotz, Diego, Gouiffes, Christian, Grebenev, Sergei A., Greiner, Jochen, Gros, Aleksandra, Hanlon, Lorraine, Hermsen, Wim, Hernandez, Cristina, Hernanz, Margarita, Huebner, 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, Jerome, Roques, Jean-Pierre, Donate, Emilio Salazar, Salt, Dave, Sanchez-Fernandez, Celia, Sauvageon, Aymeric, Savchenko, Volodymyr, Sazonov, Sergey Yu., Scaglioni, Stefano, Schartel, Norbert, Siegert, Thomas, Southworth, Richard, Sunyaev, Rashid A., Toma, Liviu, Ubertini, Pietro, Heuvel, Ed P. J. van den, von Kienlin, Andreas, von Krusenstiern, Nikolai, Winkler, Christoph, Wojciech, Hajdas, and Zannoni, Ugo
Abstract: ESA's INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL) was launched on 17 Oct 2002 at 06:41 CEST. Since then, it has been providing long, uninterrupted observations (up to about 47 hr, or 170 ksec, per satellite orbit of 2.7 days) with a large field-of-view (fully coded: 100 deg^2), msec time resolution, keV energy resolution, polarization measurements, as well as additional coverage in the optical. This is realized by two main instruments in the 15 keV to 10 MeV range, the spectrometer SPI (spectral resolution 3 keV at 1.8 MeV) and the imager IBIS (angular resolution 12 arcmin FWHM), complemented by X-ray (JEM-X; 3-35 keV) and optical (OMC; Johnson V-band) monitors. All instruments are co-aligned to simultaneously observe the target region. A particle radiation monitor (IREM) measures charged particle fluxes near the spacecraft. The Anti-coincidence subsystems of the main instruments are also efficient all-sky gamma-ray detectors, which provide omni-directional monitoring above ~75 keV. INTEGRAL can also rapidly (within a couple of hours) re-point and conduct Target of Opportunity observations. INTEGRAL has build an impressive legacy: e.g. discovery of >600 new high-energy sources; first-ever direct detection of 56Ni and 56Co radio-active decay lines from a Type Ia supernova; new insights on positron annihilation in the Galactic bulge and disk; pioneering gamma-ray polarization studies. INTEGRAL is also a successful in multi-messenger astronomy: INTEGRAL found the first prompt electromagnetic radiation in coincidence with a binary neutron star merger. More than 1750 papers based on INTEGRAL data have been published in refereed journals. Here we give a comprehensive update of the satellite status after more than 18 years of operations in a harsh space environment, and an account of the successful Ground Segment., Comment: 29 pages, 20 figures, accepted for publication in special issue of New Astronomy Reviews
Published: 2021

14. 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, Maica, Fornasini, Francesca M., Rodriguez, Jerome, Shaw, Aarran W., Tomsick, John A., Coughenour, Benjamin M., Hare, Jeremy, Krivonos, Roman, Bodaghee, Arash, Chaty, Sylvain, Clavel, Maica, Fornasini, Francesca M., Rodriguez, Jerome, and Shaw, Aarran W.
Abstract: Here we report on X-ray observations of ten 17-60 keV sources discovered by the INTEGRAL 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., Comment: 17 pages, 9 tables, 4 figures, accepted by ApJ
Published: 2021
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15. Chandra Observations of High Energy X-ray Sources Discovered by INTEGRAL

Author: Tomsick, John A., Bodaghee, Arash, Chaty, Sylvain, Clavel, Maica, Fornasini, Francesca M., Hare, Jeremy, Krivonos, Roman, Rahoui, Farid, Rodriguez, Jerome, Tomsick, John A., Bodaghee, Arash, Chaty, Sylvain, Clavel, Maica, Fornasini, Francesca M., Hare, Jeremy, Krivonos, Roman, Rahoui, Farid, and Rodriguez, Jerome
Abstract: The International Gamma-Ray Astrophysics Laboratory (INTEGRAL) satellite has detected in excess of 1000 sources in the ~20-100 keV band during its surveys of the sky over the past 17 years. We obtained 5 ks observations of 15 unclassified IGR sources with the Chandra X-ray Observatory in order to localize them, to identify optical/IR counterparts, to measure their soft X-ray spectra, and to classify them. For 10 of the IGR sources, we detect Chandra sources that are likely (or in some cases certain) to be the counterparts. IGR J18007-4146 and IGR J15038-6021 both have Gaia parallax distances, placing them at 2.5+0.5-0.4 and 1.1+1.5-0.4 kpc, respectively. We tentatively classify both of them as intermediate polar-type Cataclysmic Variables. Also, IGR J17508-3219 is likely to be a Galactic source, but it is unclear if it is a Dwarf Nova or another type of transient. For IGR J17118-3155, we provide a Chandra localization, but it is unclear if the source is Galactic or extragalactic. Based on either near-IR/IR colors or the presence of extended near-IR emission, we classify four sources as Active Galactic Nuclei (IGR J16181-5407, IGR J16246-4556, IGR J17096-2527, and IGR J19294+1327), and IGR J20310+3835 and IGR J15541-5613 are AGN candidates. In addition, we identified an AGN in the INTEGRAL error circle of IGR J16120-3543 that is a possible counterpart., Comment: Accepted by ApJ
Published: 2019
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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, Chang, Hsiang-Kuang, 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
Abstract: Instruments flown on CubeSats are small. Meaningful applications of CubeSats in astronomical observations rely on the choice of a particular subject that is feasible for CubeSats. Here we report the result of a feasibility study for observing gamma-ray polarization from Cygnus X-1 using a small Compton polarimeter on board a 3U CubeSat. Silicon detectors and cerium bromide scintillators were employed in the instrument models that we discussed in this study. Through Monte Carlo simulations with Geant4-based MEGAlib package, we found that, with a 10-Ms on-axis, zenith-direction observation in a low inclination, low altitude earth orbit radiation background environment, the minimum detectable polarization degree can be down to about 10\% in 160 - 250 keV, 20\% in 250 - 400 keV, and 65\% in 400 - 2000 keV. A 3U CubeSat dedicated to observing Cygnus X-1 can therefore yield useful information on the polarization state of gamma-ray emissions from the brightest persistent X-ray black-hole binary in the sky., Comment: 11 pages, 7 figures, accepted on June 11, 2020, for publication in The Astronomical Journal
Published: 2019
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17. 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, Chang, Hsiang-Kuang, 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
Abstract: Instruments flown on CubeSats are small. Meaningful applications of CubeSats in astronomical observations rely on the choice of a particular subject that is feasible for CubeSats. Here we report the result of a feasibility study for observing gamma-ray polarization from Cygnus X-1 using a small Compton polarimeter on board a 3U CubeSat. Silicon detectors and cerium bromide scintillators were employed in the instrument models that we discussed in this study. Through Monte Carlo simulations with Geant4-based MEGAlib package, we found that, with a 10-Ms on-axis, zenith-direction observation in a low inclination, low altitude earth orbit radiation background environment, the minimum detectable polarization degree can be down to about 10\% in 160 - 250 keV, 20\% in 250 - 400 keV, and 65\% in 400 - 2000 keV. A 3U CubeSat dedicated to observing Cygnus X-1 can therefore yield useful information on the polarization state of gamma-ray emissions from the brightest persistent X-ray black-hole binary in the sky., Comment: 11 pages, 7 figures, accepted on June 11, 2020, for publication in The Astronomical Journal
Published: 2019
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18. Chandra Observations of High Energy X-ray Sources Discovered by INTEGRAL

Author: Tomsick, John A., Bodaghee, Arash, Chaty, Sylvain, Clavel, Maica, Fornasini, Francesca M., Hare, Jeremy, Krivonos, Roman, Rahoui, Farid, Rodriguez, Jerome, Tomsick, John A., Bodaghee, Arash, Chaty, Sylvain, Clavel, Maica, Fornasini, Francesca M., Hare, Jeremy, Krivonos, Roman, Rahoui, Farid, and Rodriguez, Jerome
Abstract: The International Gamma-Ray Astrophysics Laboratory (INTEGRAL) satellite has detected in excess of 1000 sources in the ~20-100 keV band during its surveys of the sky over the past 17 years. We obtained 5 ks observations of 15 unclassified IGR sources with the Chandra X-ray Observatory in order to localize them, to identify optical/IR counterparts, to measure their soft X-ray spectra, and to classify them. For 10 of the IGR sources, we detect Chandra sources that are likely (or in some cases certain) to be the counterparts. IGR J18007-4146 and IGR J15038-6021 both have Gaia parallax distances, placing them at 2.5+0.5-0.4 and 1.1+1.5-0.4 kpc, respectively. We tentatively classify both of them as intermediate polar-type Cataclysmic Variables. Also, IGR J17508-3219 is likely to be a Galactic source, but it is unclear if it is a Dwarf Nova or another type of transient. For IGR J17118-3155, we provide a Chandra localization, but it is unclear if the source is Galactic or extragalactic. Based on either near-IR/IR colors or the presence of extended near-IR emission, we classify four sources as Active Galactic Nuclei (IGR J16181-5407, IGR J16246-4556, IGR J17096-2527, and IGR J19294+1327), and IGR J20310+3835 and IGR J15541-5613 are AGN candidates. In addition, we identified an AGN in the INTEGRAL error circle of IGR J16120-3543 that is a possible counterpart., Comment: Accepted by ApJ
Published: 2019
Full Text: View/download PDF

19. 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, Chang, Hsiang-Kuang, 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
Abstract: Instruments flown on CubeSats are small. Meaningful applications of CubeSats in astronomical observations rely on the choice of a particular subject that is feasible for CubeSats. Here we report the result of a feasibility study for observing gamma-ray polarization from Cygnus X-1 using a small Compton polarimeter on board a 3U CubeSat. Silicon detectors and cerium bromide scintillators were employed in the instrument models that we discussed in this study. Through Monte Carlo simulations with Geant4-based MEGAlib package, we found that, with a 10-Ms on-axis, zenith-direction observation in a low inclination, low altitude earth orbit radiation background environment, the minimum detectable polarization degree can be down to about 10\% in 160 - 250 keV, 20\% in 250 - 400 keV, and 65\% in 400 - 2000 keV. A 3U CubeSat dedicated to observing Cygnus X-1 can therefore yield useful information on the polarization state of gamma-ray emissions from the brightest persistent X-ray black-hole binary in the sky., Comment: 11 pages, 7 figures, accepted on June 11, 2020, for publication in The Astronomical Journal
Published: 2019
Full Text: View/download PDF

20. 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, Zingale, Michael, 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
Abstract: 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.
Published: 2019

21. 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, Zand, Jean J. M. in 't, 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, 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, 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, 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, Zand, Jean J. M. in 't, 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, 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, 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
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., Comment: Accepted for publication on Sci. China Phys. Mech. Astron. (2019)
Published: 2018
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22. Accretion in Strong Field Gravity with eXTP

Author: De Rosa, Alessandra, 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, Nardin, 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, Tor, Gabriel, Urbanec, Martin, Vincent, Frederic, Wu, Qingwen, Yuan, Feng, Zand, Jean J. M. in 't, Zdziarski, Andrzej A., Zhou, Xinlin, De Rosa, Alessandra, 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, Nardin, 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, Tor, Gabriel, Urbanec, Martin, Vincent, Frederic, Wu, Qingwen, Yuan, Feng, Zand, Jean J. M. in 't, Zdziarski, Andrzej A., and Zhou, Xinlin
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., Comment: Accepted for publication on Sci. China Phys. Mech. Astron. (2019)
Published: 2018
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23. Observatory science with eXTP

Author: Zand, Jean J. M. in 't, 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, Chichuan, Jin, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D'Aı, 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, Torres, Miguel A. Pérez, Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodrıguez-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, Jirı, 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, Zand, Jean J. M. in 't, 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, Chichuan, Jin, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D'Aı, 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, Torres, Miguel A. Pérez, Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodrıguez-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, Jirı, 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
Abstract: 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., Comment: Accepted for publication on Sci. China Phys. Mech. Astron. (2019)
Published: 2018
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24. Modelling the compact jet in MAXI J1836-194 with disc-driven shocks

Author: Péault, Mathias, Malzac, Julien, Coriat, Mickael, Russell, Thomas D., Koljonen, Karri I. I., Belmont, Renaud, Corbel, Stéphane, Drappeau, Samia, Ferreira, Jonathan, Petrucci, Pierre-Olivier, Rodriguez, Jerome, Russell, Dave M., Péault, Mathias, Malzac, Julien, Coriat, Mickael, Russell, Thomas D., Koljonen, Karri I. I., Belmont, Renaud, Corbel, Stéphane, Drappeau, Samia, Ferreira, Jonathan, Petrucci, Pierre-Olivier, Rodriguez, Jerome, and Russell, Dave M.
Abstract: The black hole candidate MAXI J1836-194 was discovered in 2011 when it went into an outburst, and was the subject of numerous, quasi-simultaneous, multi-wavelength observations in the radio, infrared, optical and X-rays. In this paper, we model its multi-wavelength radio to optical spectral energy distributions (SEDs) with an internal shock jet model. The jet emission is modelled on five dates of the outburst, during which the source is in the hard and hard intermediate X-ray spectral states. The model assumes that fluctuations of the jet velocity are driven by the variability in the accretion flow which is traced by the observed X-ray timing properties of the source. While the global shape of the SED is well reproduced by this model for all the studied observations, the variations in bolometric flux and typical energies require at least two parameters to evolve during the outburst. Here we investigate variations of the jet power and mean Lorentz factor, which are both found to increase with the source luminosity. Our results are compatible with the evolution of the jet Lorentz factor reported in earlier studies of this source. However, due to the large degeneracy of the parameters of the ishem model, our proposed scenario is not unique., Comment: 13 pages, 8 figures
Published: 2018
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25. Looking for the elusive 3:2 ratio of high-frequency quasi-periodic oscillations in the microquasar XTE J1550-564

Author: Varniere, Peggy, Rodriguez, Jerome, Varniere, Peggy, and Rodriguez, Jerome
Abstract: Using the two main XTE J1550-564 outbursts (1998-99 and 2000) we gathered about 30 observations with confirmed detections of HFQPOs. While this is a small sample it is enough to start looking at the generic properties of these oscillations, especially focusing on their frequencies and their potential harmonic relationship. This then will provide us with a list of constraints, necessary for any attempt of modelling their origin. We defined five groups based on their similarities in the Fourier domain, namely the continuum of their power density spectra (PDS) and the HFQPO frequencies. We then combined the individual PDSs of each family to obtain a PDS with higher statistics to search for other potential, previously undetected, weaker peaks. While we have two $3\sigma$ potential detections of a pair of HFQPOs in our combined PDSs, none of them shows HFQPOs with frequencies in a previously claimed 3:2 ratio. Using the results presented here we propose an updated list of requirements for any model trying to explain the HFQPOs in microquasars., Comment: accepted by ApJ
Published: 2018
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26. Observatory science with eXTP

Author: Zand, Jean J. M. in 't, 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, Chichuan, Jin, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D'Aı, 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, Torres, Miguel A. Pérez, Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodrıguez-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, Jirı, 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, Zand, Jean J. M. in 't, 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, Chichuan, Jin, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D'Aı, 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, Torres, Miguel A. Pérez, Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodrıguez-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, Jirı, 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
Abstract: 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., Comment: Accepted for publication on Sci. China Phys. Mech. Astron. (2019)
Published: 2018
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27. Accretion in Strong Field Gravity with eXTP

Author: De Rosa, Alessandra, 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, Nardin, 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, Tor, Gabriel, Urbanec, Martin, Vincent, Frederic, Wu, Qingwen, Yuan, Feng, Zand, Jean J. M. in 't, Zdziarski, Andrzej A., Zhou, Xinlin, De Rosa, Alessandra, 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, Nardin, 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, Tor, Gabriel, Urbanec, Martin, Vincent, Frederic, Wu, Qingwen, Yuan, Feng, Zand, Jean J. M. in 't, Zdziarski, Andrzej A., and Zhou, Xinlin
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., Comment: Accepted for publication on Sci. China Phys. Mech. Astron. (2019)
Published: 2018
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28. 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, Zand, Jean J. M. in 't, 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, 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, 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, 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, Zand, Jean J. M. in 't, 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, 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, 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
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., Comment: Accepted for publication on Sci. China Phys. Mech. Astron. (2019)
Published: 2018
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29. Modelling the compact jet in MAXI J1836-194 with disc-driven shocks

Author: Péault, Mathias, Malzac, Julien, Coriat, Mickael, Russell, Thomas D., Koljonen, Karri I. I., Belmont, Renaud, Corbel, Stéphane, Drappeau, Samia, Ferreira, Jonathan, Petrucci, Pierre-Olivier, Rodriguez, Jerome, Russell, Dave M., Péault, Mathias, Malzac, Julien, Coriat, Mickael, Russell, Thomas D., Koljonen, Karri I. I., Belmont, Renaud, Corbel, Stéphane, Drappeau, Samia, Ferreira, Jonathan, Petrucci, Pierre-Olivier, Rodriguez, Jerome, and Russell, Dave M.
Abstract: The black hole candidate MAXI J1836-194 was discovered in 2011 when it went into an outburst, and was the subject of numerous, quasi-simultaneous, multi-wavelength observations in the radio, infrared, optical and X-rays. In this paper, we model its multi-wavelength radio to optical spectral energy distributions (SEDs) with an internal shock jet model. The jet emission is modelled on five dates of the outburst, during which the source is in the hard and hard intermediate X-ray spectral states. The model assumes that fluctuations of the jet velocity are driven by the variability in the accretion flow which is traced by the observed X-ray timing properties of the source. While the global shape of the SED is well reproduced by this model for all the studied observations, the variations in bolometric flux and typical energies require at least two parameters to evolve during the outburst. Here we investigate variations of the jet power and mean Lorentz factor, which are both found to increase with the source luminosity. Our results are compatible with the evolution of the jet Lorentz factor reported in earlier studies of this source. However, due to the large degeneracy of the parameters of the ishem model, our proposed scenario is not unique., Comment: 13 pages, 8 figures
Published: 2018
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30. Looking for the elusive 3:2 ratio of high-frequency quasi-periodic oscillations in the microquasar XTE J1550-564

Author: Varniere, Peggy, Rodriguez, Jerome, Varniere, Peggy, and Rodriguez, Jerome
Abstract: Using the two main XTE J1550-564 outbursts (1998-99 and 2000) we gathered about 30 observations with confirmed detections of HFQPOs. While this is a small sample it is enough to start looking at the generic properties of these oscillations, especially focusing on their frequencies and their potential harmonic relationship. This then will provide us with a list of constraints, necessary for any attempt of modelling their origin. We defined five groups based on their similarities in the Fourier domain, namely the continuum of their power density spectra (PDS) and the HFQPO frequencies. We then combined the individual PDSs of each family to obtain a PDS with higher statistics to search for other potential, previously undetected, weaker peaks. While we have two $3\sigma$ potential detections of a pair of HFQPOs in our combined PDSs, none of them shows HFQPOs with frequencies in a previously claimed 3:2 ratio. Using the results presented here we propose an updated list of requirements for any model trying to explain the HFQPOs in microquasars., Comment: accepted by ApJ
Published: 2018
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31. X-RAY SPECTRAL ANALYSIS OF THE STEADY STATES OF GRS1915+105

Author: MIT Kavli Institute for Astrophysics and Space Research, Remillard, Ronald A, Steiner, James F, Peris, Charith S., Vrtilek, Saeqa D., Varnière, Peggy, Rodriguez, Jerome, Pooley, Guy, MIT Kavli Institute for Astrophysics and Space Research, Remillard, Ronald A, Steiner, James F, Peris, Charith S., Vrtilek, Saeqa D., Varnière, Peggy, Rodriguez, Jerome, and Pooley, Guy
Abstract: United States. National Aeronautics and Space Administration (PF5-160144)
Published: 2017

32. The Accretion Flow - Discrete Ejection Connection in GRS 1915+105

Author: Punsly, Brian, Rodriguez, Jerome, Trushkin, Sergei A., Punsly, Brian, Rodriguez, Jerome, and Trushkin, Sergei A.
Abstract: The microquasar GRS~1915+105 is known for its spectacular discrete ejections. They occur unexpectedly, thus their inception escapes direct observation. It has been shown that the X-ray flux increases in the hours leading up to a major ejection. In this article, we consider the serendipitous interferometric monitoring of a modest version of a discrete ejection described in Reid et al. (2014) that would have otherwise escaped detection in daily radio light curves. The observation begins $\sim 1$ hour after the onset of the ejection, providing unprecedented accuracy on the estimate of the ejection time. The astrometric measurements allow us to determine the time of ejection as $\rm{MJD}\, 56436.274^{+0.016}_{-0.013}$, i.e., within a precision of 41 minutes (95\% confidence). Just like larger flares, we find that the X-ray luminosity increases in last 2 - 4 hours preceding ejection. Our finite temporal resolution indicates that this elevated X-ray flux persists within $21.8^{+22.6}_{-19.1}$ minutes of the ejection with 95\% confidence, the highest temporal precision of the X-ray - superluminal ejection connection to date. This observation provides direct evidence that the physics that launches major flares occurs on smaller scales as well (lower radio flux and shorter ejection episodes). The observation of a X-ray spike prior to a discrete ejection, although of very modest amplitude suggests that the process linking accretion behavior to ejection is general from the smallest scales to high luminosity major superluminal flares., Comment: To appear in ApJ
Published: 2016
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33. A Temporal Analysis Indicates a Mildly Relativistic Compact Jet in GRS~1915+105

Author: Punsly, Brian, Rodriguez, Jerome, Punsly, Brian, and Rodriguez, Jerome
Abstract: Most of our knowledge of the radio morphology and kinematics of X-ray binary partially synchrotron self-absorbed compact jets (hereafter compact jets) is based on the observations of GRS~1915+105 which has the most prominent compact jet. Yet, the compact jet bulk velocity, $v$, is poorly constrained in the literature, $0.07 < v/c < 0.98$. In spite of this uncertainty, compact jets are often unified with relativistic jets in active galactic nuclei. We have estimated $v$ as part of a temporal analysis of GRS~1915+105 jets in "high plateau states" (HPS). We define the HPS as a state showing a hard X-ray spectrum and low level of long-term ($>10$s) X-ray activity associated with 15 GHz flux density $>70$ mJy for $>7$ consecutive days. The radio emission is associated with compact jet emission. Two HPS were monitored at 15 GHz during their termination with e-folding times of 3.8 hrs and 8.6 hrs. We combine this time scale with the scale of spatial variation of the linear source of a VLBA image preceding the fade of one of these HPS in order to estimate the jet speed. Our assumption that the reduction in radio emissivity propagates as an approximate discontinuity down the HPS jet (leaving a weak jet in its wake) indicates $0.17
Published: 2016
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34. 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., Zhang, Xiaoling, 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
Abstract: Microquasars are stellar-mass black holes accreting matter from a companion star and ejecting plasma jets at almost the speed of light. They are analogues of quasars that contain supermassive black holes of $10^6$ to $10^{10}$ solar masses. Accretion in microquasars varies on much shorter timescales than in quasars and occasionally produces exceptionally bright X-ray flares. How the flares are produced is unclear, as is the mechanism for launching the relativistic jets and their composition. An emission line near 511 kiloelectronvolts has long been sought in the emission spectrum of microquasars as evidence for the expected electron-positron plasma. Transient high-energy spectral features have been reported in two objects, but their positron interpretation remains contentious. Here we report observations of $\gamma$-ray emission from the microquasar V404 Cygni during a recent period of strong flaring activity. The emission spectrum around 511 kiloelectronvolts shows clear signatures of variable positron annihilation, which implies a high rate of positron production. This supports the earlier conjecture that microquasars may be the main sources of the electron-positron plasma responsible for the bright diffuse emission of annihilation $\gamma$-rays in the bulge region of our Galaxy. Additionally, microquasars could be the origin of the observed megaelectronvolt continuum excess in the inner Galaxy., Comment: Accepted and published in Nature; 11 pages, 4 figures, 5 tables. Further information on data analysis added in version 2: 9 pages, 11 figures
Published: 2016
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35. The Accretion Flow - Discrete Ejection Connection in GRS 1915+105

Author: Punsly, Brian, Rodriguez, Jerome, Trushkin, Sergei A., Punsly, Brian, Rodriguez, Jerome, and Trushkin, Sergei A.
Abstract: The microquasar GRS~1915+105 is known for its spectacular discrete ejections. They occur unexpectedly, thus their inception escapes direct observation. It has been shown that the X-ray flux increases in the hours leading up to a major ejection. In this article, we consider the serendipitous interferometric monitoring of a modest version of a discrete ejection described in Reid et al. (2014) that would have otherwise escaped detection in daily radio light curves. The observation begins $\sim 1$ hour after the onset of the ejection, providing unprecedented accuracy on the estimate of the ejection time. The astrometric measurements allow us to determine the time of ejection as $\rm{MJD}\, 56436.274^{+0.016}_{-0.013}$, i.e., within a precision of 41 minutes (95\% confidence). Just like larger flares, we find that the X-ray luminosity increases in last 2 - 4 hours preceding ejection. Our finite temporal resolution indicates that this elevated X-ray flux persists within $21.8^{+22.6}_{-19.1}$ minutes of the ejection with 95\% confidence, the highest temporal precision of the X-ray - superluminal ejection connection to date. This observation provides direct evidence that the physics that launches major flares occurs on smaller scales as well (lower radio flux and shorter ejection episodes). The observation of a X-ray spike prior to a discrete ejection, although of very modest amplitude suggests that the process linking accretion behavior to ejection is general from the smallest scales to high luminosity major superluminal flares., Comment: To appear in ApJ
Published: 2016
Full Text: View/download PDF

36. A Temporal Analysis Indicates a Mildly Relativistic Compact Jet in GRS~1915+105

Author: Punsly, Brian, Rodriguez, Jerome, Punsly, Brian, and Rodriguez, Jerome
Abstract: Most of our knowledge of the radio morphology and kinematics of X-ray binary partially synchrotron self-absorbed compact jets (hereafter compact jets) is based on the observations of GRS~1915+105 which has the most prominent compact jet. Yet, the compact jet bulk velocity, $v$, is poorly constrained in the literature, $0.07 < v/c < 0.98$. In spite of this uncertainty, compact jets are often unified with relativistic jets in active galactic nuclei. We have estimated $v$ as part of a temporal analysis of GRS~1915+105 jets in "high plateau states" (HPS). We define the HPS as a state showing a hard X-ray spectrum and low level of long-term ($>10$s) X-ray activity associated with 15 GHz flux density $>70$ mJy for $>7$ consecutive days. The radio emission is associated with compact jet emission. Two HPS were monitored at 15 GHz during their termination with e-folding times of 3.8 hrs and 8.6 hrs. We combine this time scale with the scale of spatial variation of the linear source of a VLBA image preceding the fade of one of these HPS in order to estimate the jet speed. Our assumption that the reduction in radio emissivity propagates as an approximate discontinuity down the HPS jet (leaving a weak jet in its wake) indicates $0.17
Published: 2016
Full Text: View/download PDF

37. 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., Zhang, Xiaoling, 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
Abstract: Microquasars are stellar-mass black holes accreting matter from a companion star and ejecting plasma jets at almost the speed of light. They are analogues of quasars that contain supermassive black holes of $10^6$ to $10^{10}$ solar masses. Accretion in microquasars varies on much shorter timescales than in quasars and occasionally produces exceptionally bright X-ray flares. How the flares are produced is unclear, as is the mechanism for launching the relativistic jets and their composition. An emission line near 511 kiloelectronvolts has long been sought in the emission spectrum of microquasars as evidence for the expected electron-positron plasma. Transient high-energy spectral features have been reported in two objects, but their positron interpretation remains contentious. Here we report observations of $\gamma$-ray emission from the microquasar V404 Cygni during a recent period of strong flaring activity. The emission spectrum around 511 kiloelectronvolts shows clear signatures of variable positron annihilation, which implies a high rate of positron production. This supports the earlier conjecture that microquasars may be the main sources of the electron-positron plasma responsible for the bright diffuse emission of annihilation $\gamma$-rays in the bulge region of our Galaxy. Additionally, microquasars could be the origin of the observed megaelectronvolt continuum excess in the inner Galaxy., Comment: Accepted and published in Nature; 11 pages, 4 figures, 5 tables. Further information on data analysis added in version 2: 9 pages, 11 figures
Published: 2016
Full Text: View/download PDF

38. The On-Site Analysis of the Cherenkov Telescope Array

Author: Bulgarelli, Andrea, Fioretti, Valentina, Zoli, Andrea, Aboudan, Alessio, Rodríguez-Vázquez, Juan José, De Cesare, Giovanni, De Rosa, Adriano, Maier, Gernot, Lyard, Etienne, Bastieri, Denis, Lombardi, Saverio, Tosti, Gino, Bergamaschi, Sonia, Beneventano, Domenico, Lamanna, Giovanni, Jacquemier, Jean, Kosack, Karl, Antonelli, Lucio Angelo, Boisson, Catherine, Borkowski, Jerzy, Buson, Sara, Carosi, Alessandro, Conforti, Vito, Colomé, Pep, Reyes, Raquel de los, Dumm, Jon, Evans, Phil, Fortson, Lucy, Fuessling, Matthias, Gotz, Diego, Graciani, Ricardo, Gianotti, Fulvio, Grandi, Paola, Hinton, Jim, Humensky, Brian, Inoue, Susumu, Knödlseder, Jürgen, Flour, Thierry Le, Lindemann, Rico, Malaguti, Giuseppe, Markoff, Sera, Marisaldi, Martino, Neyroud, Nadine, Nicastro, Luciano, Ohm, Stefan, Osborne, Julian, Oya, Igor, Rodriguez, Jerome, Rosen, Simon, Ribo, Marc, Tacchini, Alessandro, Schüssler, Fabian, Stolarczyk, Thierry, Torresi, Eleonora, Testa, Vincenzo, Wegner, Peter, Weinstein, Amanda, Bulgarelli, Andrea, Fioretti, Valentina, Zoli, Andrea, Aboudan, Alessio, Rodríguez-Vázquez, Juan José, De Cesare, Giovanni, De Rosa, Adriano, Maier, Gernot, Lyard, Etienne, Bastieri, Denis, Lombardi, Saverio, Tosti, Gino, Bergamaschi, Sonia, Beneventano, Domenico, Lamanna, Giovanni, Jacquemier, Jean, Kosack, Karl, Antonelli, Lucio Angelo, Boisson, Catherine, Borkowski, Jerzy, Buson, Sara, Carosi, Alessandro, Conforti, Vito, Colomé, Pep, Reyes, Raquel de los, Dumm, Jon, Evans, Phil, Fortson, Lucy, Fuessling, Matthias, Gotz, Diego, Graciani, Ricardo, Gianotti, Fulvio, Grandi, Paola, Hinton, Jim, Humensky, Brian, Inoue, Susumu, Knödlseder, Jürgen, Flour, Thierry Le, Lindemann, Rico, Malaguti, Giuseppe, Markoff, Sera, Marisaldi, Martino, Neyroud, Nadine, Nicastro, Luciano, Ohm, Stefan, Osborne, Julian, Oya, Igor, Rodriguez, Jerome, Rosen, Simon, Ribo, Marc, Tacchini, Alessandro, Schüssler, Fabian, Stolarczyk, Thierry, Torresi, Eleonora, Testa, Vincenzo, Wegner, Peter, and Weinstein, Amanda
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., Comment: In Proceedings of the 34th International Cosmic Ray Conference (ICRC2015), The Hague, The Netherlands. All CTA contributions at arXiv:1508.05894
Published: 2015

39. Chandra Observations of Eight Sources Discovered by INTEGRAL

Author: Tomsick, John A., Krivonos, Roman, Wang, Qinan, Bodaghee, Arash, Chaty, Sylvain, Rahoui, Farid, Rodriguez, Jerome, Fornasini, Francesca M., Tomsick, John A., Krivonos, Roman, Wang, Qinan, Bodaghee, Arash, Chaty, Sylvain, Rahoui, Farid, Rodriguez, Jerome, and Fornasini, Francesca M.
Abstract: We report on 0.3-10 keV observations with the Chandra X-ray Observatory of eight hard X-ray sources discovered within 8 degrees of the Galactic plane by the INTEGRAL satellite. The short (5 ks) Chandra observations of the IGR source fields have yielded very likely identifications of X-ray counterparts for three of the IGR sources: IGR J14091-6108, IGR J18088-2741, and IGR J18381-0924. The first two have very hard spectra in the Chandra band that can be described by a power-law with photon indices of Gamma = 0.6+/-0.4 and -0.7(+0.4)(-0.3), respectively (90% confidence errors are given), and both have a unique near-IR counterpart consistent with the Chandra position. IGR J14091-6108 also displays a strong iron line and a relatively low X-ray luminosity, and we argue that the most likely source type is a Cataclysmic Variable (CV), although we do not completely rule out the possibility of a High Mass X-ray Binary. IGR J18088-2741 has an optical counterpart with a previously measured 6.84 hr periodicity, which may be the binary orbital period. We also detect five cycles of a possible 800-950 s period in the Chandra light curve, which may be the compact object spin period. We suggest that IGR J18088-2741 is also most likely a CV. For IGR J18381-0924, the spectrum is intrinsically softer with Gamma = 1.5(+0.5)(-0.4), and it is moderately absorbed, nH = (4+/-1)e22 cm-2. There are two near-IR sources consistent with the Chandra position, and they are both classified as galaxies, making it likely that IGR J18381-0924 is an Active Galactic Nucleus (AGN). For the other five IGR sources, we provide lists of nearby Chandra sources, which may be used along with further observations to identify the correct counterparts, and we discuss the implications of the low inferred Chandra count rates for these five sources., Comment: Accepted by ApJ, 14 pages
Published: 2015
Full Text: View/download PDF

40. X-ray Spectral Analysis of the Steady States of GRS 1915+105

Author: Peris, Charith S., Remillard, Ronald A., Steiner, James F., Vrtilek, Saeqa D., Varniere, Peggy, Rodriguez, Jerome, Pooley, Guy, Peris, Charith S., Remillard, Ronald A., Steiner, James F., Vrtilek, Saeqa D., Varniere, Peggy, Rodriguez, Jerome, and Pooley, Guy
Abstract: We report on the X-ray spectral behavior within the steady states of GRS 1915+105. Our work is based on the full data set on the source obtained using the Proportional Counter Array on the Rossi X-ray Timing Explorer 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 them as steady-soft and steady-hard. GRS 1915+105 displays significant curvature in the coronal component in both the soft and hard data within the {\it RXTE}/PCA bandpass. A majority of the steady-soft observations displays a roughly constant inner disk radius (R_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~0.68 +/- 0.35 and \eta ~ 1.12 +/- 0.13. They are consistent with the upper and lower tracks of Gallo et al. (2012), respectively. A comparison of model parameters to the state definitions show that almost all steady-soft observations match the criteria of either 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., Comment: 21 pages, 15 figures, 2 tables. Accepted for publication in ApJ
Published: 2015
Full Text: View/download PDF

41. Creating a high-resolution picture of Cygnus with the Cherenkov Telescope Array

Author: Weinstein, Amanda, Aliu, Ester, Casanova, Sabrina, Di Girolamo, Tristano, Dyrda, Michael, Hahn, Joachim, Majumdar, Pratik, Rodriguez, Jerome, Tibaldo, Luigi, Weinstein, Amanda, Aliu, Ester, Casanova, Sabrina, Di Girolamo, Tristano, Dyrda, Michael, Hahn, Joachim, Majumdar, Pratik, Rodriguez, Jerome, and Tibaldo, Luigi
Abstract: The Cygnus region hosts one of the most remarkable star-forming regions in the Milky Way. Indeed, the total mass in molecular gas of the Cygnus X complex exceeds 10 times the total mass of all other nearby star-forming regions. Surveys at all wavelengths, from radio to gamma-rays, reveal that Cygnus contains such a wealth and variety of sources---supernova remnants (SNRs), pulsars, pulsar wind nebulae (PWNe), H II regions, Wolf-Rayet binaries, OB associations, microquasars, dense molecular clouds and superbubbles---as to practically be a galaxy in microcosm. The gamma-ray observations along reveal a wealth of intriguing sources at energies between 1 GeV and tens of TeV. However, a complete understanding of the physical phenomena producing this gamma-ray emission first requires us to disentangle overlapping sources and reconcile discordant pictures at different energies. This task is made more challenging by the limited angular resolution of instruments such as the Fermi Large Area Telescope, ARGO-YBJ, and HAWC and the limited sensitivity and field of view of current imaging atmospheric Cherenkov telescopes (IACTs). The Cherenkov Telescope Array (CTA), with its improved angular resolution, large field of view, and order of magnitude gain in sensitivity over current IACTs, has the potential to finally create a coherent and well-resolved picture of the Cygnus region between a few tens of GeV and a hundred TeV. We describe a proposed strategy to study the Cygnus region using CTA data, which combines a survey of the whole region at $65^{\circ} < l < 85^{\circ}$ and $-3.5^{\circ} < b < 3.5^{\circ} $ with deeper observations of two sub-regions that host rich groups of known gamma-ray sources., Comment: In Proceedings of the 34th International Cosmic Ray Conference (ICRC2015), The Hague, The Netherlands. All CTA contributions at arXiv:1508.05894
Published: 2015

42. Chandra Identification of Two AGN Discovered by INTEGRAL

Author: Tomsick, John A., Krivonos, Roman, Rahoui, Farid, Ajello, Marco, Rodriguez, Jerome, Barriere, Nicolas, Bodaghee, Arash, Chaty, Sylvain, Tomsick, John A., Krivonos, Roman, Rahoui, Farid, Ajello, Marco, Rodriguez, Jerome, Barriere, Nicolas, Bodaghee, Arash, and Chaty, Sylvain
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 catalog 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 N_H = 3.1(+2.0)(-1.5)e22 cm-2 and a photon index of Gamma = 1.4+/-0.7, and we suggest that it is a Seyfert galaxy. For IGR J08297-4250, the photon index is similar, Gamma = 1.5+/-0.8, but the source is highly absorbed (N_H = 6.1(+10.1)(-4.3)e23 cm-2)., Comment: 10 pages, 5 figures, 5 tables
Published: 2015
Full Text: View/download PDF

43. Broad-Band Spectrum of the Black Hole Candidate IGR J17497-2821 Studied with Suzaku

Author: PAIZIS, Adamantia, 海老澤, 研, EBISAWA, Ken, 高橋, 弘充, TAKAHASHI, Hiromitsu, 堂谷, 忠靖, DOTANI, Tadayasu, 幸村, 孝由, KOHMURA, Takayoshi, 国分, 紀秀, KOKUBUN, Motohide, RODRIGUEZ, Jerome, 上田, 佳宏, UEDA, Yoshihiro, WALTER, Roland, 山田, 真也, YAMADA, Shinya, 山岡, 和貴, YAMAOKA, Kazutaka, 湯浅, 孝行, YUASA, Takayuki, PAIZIS, Adamantia, 海老澤, 研, EBISAWA, Ken, 高橋, 弘充, TAKAHASHI, Hiromitsu, 堂谷, 忠靖, DOTANI, Tadayasu, 幸村, 孝由, KOHMURA, Takayoshi, 国分, 紀秀, KOKUBUN, Motohide, RODRIGUEZ, Jerome, 上田, 佳宏, UEDA, Yoshihiro, WALTER, Roland, 山田, 真也, YAMADA, Shinya, 山岡, 和貴, YAMAOKA, Kazutaka, 湯浅, 孝行, and YUASA, Takayuki
Published: 2015

44. Chandra Observations of Eight Sources Discovered by INTEGRAL

Author: Tomsick, John A., Krivonos, Roman, Wang, Qinan, Bodaghee, Arash, Chaty, Sylvain, Rahoui, Farid, Rodriguez, Jerome, Fornasini, Francesca M., Tomsick, John A., Krivonos, Roman, Wang, Qinan, Bodaghee, Arash, Chaty, Sylvain, Rahoui, Farid, Rodriguez, Jerome, and Fornasini, Francesca M.
Abstract: We report on 0.3-10 keV observations with the Chandra X-ray Observatory of eight hard X-ray sources discovered within 8 degrees of the Galactic plane by the INTEGRAL satellite. The short (5 ks) Chandra observations of the IGR source fields have yielded very likely identifications of X-ray counterparts for three of the IGR sources: IGR J14091-6108, IGR J18088-2741, and IGR J18381-0924. The first two have very hard spectra in the Chandra band that can be described by a power-law with photon indices of Gamma = 0.6+/-0.4 and -0.7(+0.4)(-0.3), respectively (90% confidence errors are given), and both have a unique near-IR counterpart consistent with the Chandra position. IGR J14091-6108 also displays a strong iron line and a relatively low X-ray luminosity, and we argue that the most likely source type is a Cataclysmic Variable (CV), although we do not completely rule out the possibility of a High Mass X-ray Binary. IGR J18088-2741 has an optical counterpart with a previously measured 6.84 hr periodicity, which may be the binary orbital period. We also detect five cycles of a possible 800-950 s period in the Chandra light curve, which may be the compact object spin period. We suggest that IGR J18088-2741 is also most likely a CV. For IGR J18381-0924, the spectrum is intrinsically softer with Gamma = 1.5(+0.5)(-0.4), and it is moderately absorbed, nH = (4+/-1)e22 cm-2. There are two near-IR sources consistent with the Chandra position, and they are both classified as galaxies, making it likely that IGR J18381-0924 is an Active Galactic Nucleus (AGN). For the other five IGR sources, we provide lists of nearby Chandra sources, which may be used along with further observations to identify the correct counterparts, and we discuss the implications of the low inferred Chandra count rates for these five sources., Comment: Accepted by ApJ, 14 pages
Published: 2015
Full Text: View/download PDF

45. X-ray Spectral Analysis of the Steady States of GRS 1915+105

Author: Peris, Charith S., Remillard, Ronald A., Steiner, James F., Vrtilek, Saeqa D., Varniere, Peggy, Rodriguez, Jerome, Pooley, Guy, Peris, Charith S., Remillard, Ronald A., Steiner, James F., Vrtilek, Saeqa D., Varniere, Peggy, Rodriguez, Jerome, and Pooley, Guy
Abstract: We report on the X-ray spectral behavior within the steady states of GRS 1915+105. Our work is based on the full data set on the source obtained using the Proportional Counter Array on the Rossi X-ray Timing Explorer 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 them as steady-soft and steady-hard. GRS 1915+105 displays significant curvature in the coronal component in both the soft and hard data within the {\it RXTE}/PCA bandpass. A majority of the steady-soft observations displays a roughly constant inner disk radius (R_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~0.68 +/- 0.35 and \eta ~ 1.12 +/- 0.13. They are consistent with the upper and lower tracks of Gallo et al. (2012), respectively. A comparison of model parameters to the state definitions show that almost all steady-soft observations match the criteria of either 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., Comment: 21 pages, 15 figures, 2 tables. Accepted for publication in ApJ
Published: 2015
Full Text: View/download PDF

46. Creating a high-resolution picture of Cygnus with the Cherenkov Telescope Array

Author: Weinstein, Amanda, Aliu, Ester, Casanova, Sabrina, Di Girolamo, Tristano, Dyrda, Michael, Hahn, Joachim, Majumdar, Pratik, Rodriguez, Jerome, Tibaldo, Luigi, Weinstein, Amanda, Aliu, Ester, Casanova, Sabrina, Di Girolamo, Tristano, Dyrda, Michael, Hahn, Joachim, Majumdar, Pratik, Rodriguez, Jerome, and Tibaldo, Luigi
Abstract: The Cygnus region hosts one of the most remarkable star-forming regions in the Milky Way. Indeed, the total mass in molecular gas of the Cygnus X complex exceeds 10 times the total mass of all other nearby star-forming regions. Surveys at all wavelengths, from radio to gamma-rays, reveal that Cygnus contains such a wealth and variety of sources---supernova remnants (SNRs), pulsars, pulsar wind nebulae (PWNe), H II regions, Wolf-Rayet binaries, OB associations, microquasars, dense molecular clouds and superbubbles---as to practically be a galaxy in microcosm. The gamma-ray observations along reveal a wealth of intriguing sources at energies between 1 GeV and tens of TeV. However, a complete understanding of the physical phenomena producing this gamma-ray emission first requires us to disentangle overlapping sources and reconcile discordant pictures at different energies. This task is made more challenging by the limited angular resolution of instruments such as the Fermi Large Area Telescope, ARGO-YBJ, and HAWC and the limited sensitivity and field of view of current imaging atmospheric Cherenkov telescopes (IACTs). The Cherenkov Telescope Array (CTA), with its improved angular resolution, large field of view, and order of magnitude gain in sensitivity over current IACTs, has the potential to finally create a coherent and well-resolved picture of the Cygnus region between a few tens of GeV and a hundred TeV. We describe a proposed strategy to study the Cygnus region using CTA data, which combines a survey of the whole region at $65^{\circ} < l < 85^{\circ}$ and $-3.5^{\circ} < b < 3.5^{\circ} $ with deeper observations of two sub-regions that host rich groups of known gamma-ray sources., Comment: In Proceedings of the 34th International Cosmic Ray Conference (ICRC2015), The Hague, The Netherlands. All CTA contributions at arXiv:1508.05894
Published: 2015

47. The On-Site Analysis of the Cherenkov Telescope Array

Author: Bulgarelli, Andrea, Fioretti, Valentina, Zoli, Andrea, Aboudan, Alessio, Rodríguez-Vázquez, Juan José, De Cesare, Giovanni, De Rosa, Adriano, Maier, Gernot, Lyard, Etienne, Bastieri, Denis, Lombardi, Saverio, Tosti, Gino, Bergamaschi, Sonia, Beneventano, Domenico, Lamanna, Giovanni, Jacquemier, Jean, Kosack, Karl, Antonelli, Lucio Angelo, Boisson, Catherine, Borkowski, Jerzy, Buson, Sara, Carosi, Alessandro, Conforti, Vito, Colomé, Pep, Reyes, Raquel de los, Dumm, Jon, Evans, Phil, Fortson, Lucy, Fuessling, Matthias, Gotz, Diego, Graciani, Ricardo, Gianotti, Fulvio, Grandi, Paola, Hinton, Jim, Humensky, Brian, Inoue, Susumu, Knödlseder, Jürgen, Flour, Thierry Le, Lindemann, Rico, Malaguti, Giuseppe, Markoff, Sera, Marisaldi, Martino, Neyroud, Nadine, Nicastro, Luciano, Ohm, Stefan, Osborne, Julian, Oya, Igor, Rodriguez, Jerome, Rosen, Simon, Ribo, Marc, Tacchini, Alessandro, Schüssler, Fabian, Stolarczyk, Thierry, Torresi, Eleonora, Testa, Vincenzo, Wegner, Peter, Weinstein, Amanda, Bulgarelli, Andrea, Fioretti, Valentina, Zoli, Andrea, Aboudan, Alessio, Rodríguez-Vázquez, Juan José, De Cesare, Giovanni, De Rosa, Adriano, Maier, Gernot, Lyard, Etienne, Bastieri, Denis, Lombardi, Saverio, Tosti, Gino, Bergamaschi, Sonia, Beneventano, Domenico, Lamanna, Giovanni, Jacquemier, Jean, Kosack, Karl, Antonelli, Lucio Angelo, Boisson, Catherine, Borkowski, Jerzy, Buson, Sara, Carosi, Alessandro, Conforti, Vito, Colomé, Pep, Reyes, Raquel de los, Dumm, Jon, Evans, Phil, Fortson, Lucy, Fuessling, Matthias, Gotz, Diego, Graciani, Ricardo, Gianotti, Fulvio, Grandi, Paola, Hinton, Jim, Humensky, Brian, Inoue, Susumu, Knödlseder, Jürgen, Flour, Thierry Le, Lindemann, Rico, Malaguti, Giuseppe, Markoff, Sera, Marisaldi, Martino, Neyroud, Nadine, Nicastro, Luciano, Ohm, Stefan, Osborne, Julian, Oya, Igor, Rodriguez, Jerome, Rosen, Simon, Ribo, Marc, Tacchini, Alessandro, Schüssler, Fabian, Stolarczyk, Thierry, Torresi, Eleonora, Testa, Vincenzo, Wegner, Peter, and Weinstein, Amanda
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., Comment: In Proceedings of the 34th International Cosmic Ray Conference (ICRC2015), The Hague, The Netherlands. All CTA contributions at arXiv:1508.05894
Published: 2015

48. Chandra Identification of Two AGN Discovered by INTEGRAL

Author: Tomsick, John A., Krivonos, Roman, Rahoui, Farid, Ajello, Marco, Rodriguez, Jerome, Barriere, Nicolas, Bodaghee, Arash, Chaty, Sylvain, Tomsick, John A., Krivonos, Roman, Rahoui, Farid, Ajello, Marco, Rodriguez, Jerome, Barriere, Nicolas, Bodaghee, Arash, and Chaty, Sylvain
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 catalog 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 N_H = 3.1(+2.0)(-1.5)e22 cm-2 and a photon index of Gamma = 1.4+/-0.7, and we suggest that it is a Seyfert galaxy. For IGR J08297-4250, the photon index is similar, Gamma = 1.5+/-0.8, but the source is highly absorbed (N_H = 6.1(+10.1)(-4.3)e23 cm-2)., Comment: 10 pages, 5 figures, 5 tables
Published: 2015
Full Text: View/download PDF

49. SPECTRAL STATE DEPENDENCE OF THE 0.4–2 MEV POLARIZED EMISSION IN CYGNUS X-1 SEEN WITH INTEGRAL/IBIS, AND LINKS WITH THE AMI RADIO DATA

Author: MIT Kavli Institute for Astrophysics and Space Research, Grinberg, Victoria, Laurent, Philippe, Bel, Marion Cadolle, Pottschmidt, Katja, Pooley, Guy, Bodaghee, Arash, Rodriguez, Jerome, Wilms, Jorn, Gouiffes, Christian, MIT Kavli Institute for Astrophysics and Space Research, Grinberg, Victoria, Laurent, Philippe, Bel, Marion Cadolle, Pottschmidt, Katja, Pooley, Guy, Bodaghee, Arash, Rodriguez, Jerome, Wilms, Jorn, and Gouiffes, Christian
Abstract: Polarization of the [> over ~] 400 keV hard tail of the microquasar Cygnus X-1 has been independently reported by INTEGRAL/Imager on Board the INTEGRAL Satellite (IBIS), and INTEGRAL/SPectrometer on INTEGRAL and interpreted as emission from a compact jet. These conclusions were, however, based on the accumulation of all INTEGRAL data regardless of the spectral state. We utilize additional INTEGRAL exposure accumulated until 2012 December, and include the AMI/Ryle (15 GHz) radio data in our study. We separate the observations into hard, soft, and intermediate/transitional states and detect radio emission from a compact jet in hard and intermediate states (IS), but not in the soft. The 10–400 keV INTEGRAL (JEM-X and IBIS) state resolved spectra are well modeled with thermal Comptonization and reflection components. We detect a hard tail in the 0.4–2 MeV range for the hard state only. We extract the state dependent polarigrams of Cyg X-1, which are all compatible with no or an undetectable level of polarization except in the 400–2000 keV range in the hard state where the polarization fraction is 75% ± 32% and the polarization angle 40[° over .]0 ± 14[° over .]3. An upper limit on the 0.4–2 MeV soft state polarization fraction is 70%. Due to the short exposure, we obtain no meaningful constraint for the IS. The likely detection of a >400 keV polarized tail in the hard state, together with the simultaneous presence of a radio jet, reinforce the notion of a compact jet origin of the >400 keV emission.
Published: 2015

50. Evidence of Elevated X-Ray Absorption Before and During Major Flare Ejections in GRS 1915+105

Author: Punsly, Brian, Rodriguez, Jerome, Trushkin, Sergei A., Punsly, Brian, Rodriguez, Jerome, and Trushkin, Sergei A.
Abstract: We present time resolved X-ray spectroscopy of the microquasar GRS1915+105 with the MAXI observatory in order to study the accretion state just before and during the ejections associated with its major flares. Radio monitoring with the RATAN-600 radio telescope from 4.8 - 11.2 GHz has revealed two large steep spectrum major flares in the first eight months of 2013. Since, the RATAN receives one measurement per day, we cannot determine the jet forming time without more information. Fortunately, this is possible since a distinct X-ray light curve signature that occurs preceding and during major ejections has been determined in an earlier study. The X-ray luminosity spikes to very high levels in the hours before ejection then becomes variable (with a nearly equal X-ray luminosity when averaged over the duration of the ejection) during a brief 3 to 8 hour ejection process. By comparing this X-ray behavior to MAXI light curves, we can estimate the beginning and end of the ejection episode of the strong 2013 flares to within $\sim$3 hours. Using this estimate in conjunction with time resolved spectroscopy from the data in the MAXI archives allows us to deduce that the X-ray absorbing hydrogen column density increases significantly in the hours preceding the ejections and remains elevated during the ejections responsible for the major flares. This finding is consistent with an out-flowing wind or enhanced accretion at high latitudes., Comment: To appear in ApJ
Published: 2014
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