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18 results on '"Rodriguez, Jerome"'

1. INTEGRAL/IBIS polarization detection in the hard and soft intermediate states of Swift J1727.8-1613

Author

Bouchet, Tristan, Rodriguez, Jérôme, Cangemi, Floriane, Thalhammer, Philipp, Laurent, Philippe, Grinberg, Victoria, Wilms, Joern, and Pottschimdt, Katja

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Soft gamma-ray emission (100 keV -- 10 MeV) has previously been detected in the hard state of several microquasars. In some sources, this emission was found to be highly polarized and was suggested to be emitted at the base of the jet. Until now, no $\gamma$-ray polarization had been found in any other state. Using INTEGRAL/IBIS, we studied the soft gamma-ray spectral and polarization properties of Swift J1727.8-1613 throughout its outburst. We detect a highly polarized spectral component in both the hard intermediate state and the early stages of the soft intermediate state above 210 keV. In the hard intermediate state, the polarization angle significantly deviates from the compact jet angle projected onto the sky, whereas in the soft intermediate they are closely aligned. This constitutes the first detection of jet-aligned polarization in the soft gamma-ray for a microquasar. We attribute this polarized spectral component to synchrotron emission from the jet, which indicates that some of the jet might persist into the softer states., Comment: 7 pages, 4 figures. Accepted for publication in A&A Letters

Published
2024
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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., and Tudose, Valeriu

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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. 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, and Wilms, Joern

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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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4. Absorption lines from magnetically driven winds in X-ray binaries II: high resolution observational signatures expected from future X-ray observatories

Author

Chakravorty, Susmita, Petrucci, Pierre-Olivier, Datta, Sudeb Ranjan, Ferreira, Jonathan, Wilms, Joern, Jacquemin-Ide, Jonatan, Clavel, Maica, Marcel, Gregoire, Rodriguez, Jerome, Malzac, Julien, Belmont, Renaud, Corbel, Stephane, Coriat, Mickael, Henri, Gilles, and Parra, Maxime

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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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5. 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, and Tetarenko, Alexandra J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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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6. 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, and Coriat, Mickael

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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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7. Chasing the Break: Tracing the Full Evolution of a Black Hole X-Ray Binary Jet with Multiwavelength Spectral Modeling

Author

Echiburú-Trujillo, Constanza, primary, Tetarenko, Alexandra J., additional, Haggard, Daryl, additional, Russell, Thomas D., additional, Koljonen, Karri I. I., additional, Bahramian, Arash, additional, Wang, Jingyi, additional, Bremer, Michael, additional, Bright, Joe, additional, Casella, Piergiorgio, additional, Russell, David M., additional, Altamirano, Diego, additional, Baglio, M. Cristina, additional, Belloni, Tomaso, additional, Ceccobello, Chiara, additional, Corbel, Stephane, additional, Diaz Trigo, Maria, additional, Maitra, Dipankar, additional, Gabuya, Aldrin, additional, Gallo, Elena, additional, Heinz, Sebastian, additional, Homan, Jeroen, additional, Kara, Erin, additional, Körding, Elmar, additional, Lewis, Fraser, additional, Lucchini, Matteo, additional, Markoff, Sera, additional, Migliari, Simone, additional, Miller-Jones, James C. A., additional, Rodriguez, Jerome, additional, Saikia, Payaswini, additional, Sarazin, Craig L., additional, Shahbaz, Tariq, additional, Sivakoff, Gregory, additional, Soria, Roberto, additional, Testa, Vincenzo, additional, Tetarenko, Bailey E., additional, and Tudose, Valeriu, additional

Published
2024
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9. Absorption lines from magnetically driven winds in X-ray binaries – II. High resolution observational signatures expected from future X-ray observatories

Author

Chakravorty, Susmita, primary, Petrucci, Pierre-Olivier, additional, Datta, Sudeb Ranjan, additional, Ferreira, Jonathan, additional, Wilms, Joern, additional, Jacquemin-Ide, Jonatan, additional, Clavel, Maica, additional, Marcel, Gregoire, additional, Rodriguez, Jerome, additional, Malzac, Julien, additional, Belmont, Renaud, additional, Corbel, Stephane, additional, Coriat, Mickael, additional, Henri, Gilles, additional, and Parra, Maxime, additional

Published
2022
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10. The enhanced x-ray timing and polarimetry mission: eXTP: an update on its scientific cases, mission profile and development status

Author

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, Chinese Academy of Sciences, Agenzia Spaziale Italiana, Ministerio de Ciencia e Innovación (España), Federal Ministry of Economics and Technology (Germany), and Foundation for Polish Science

Subjects
Equation of state, Extreme gravity, Black hole, X-ray timing, X-ray polarimetry, Neutron star, Extreme magnetism, Extreme density
Abstract

Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray (2022), Montreal, Jul 17-22, 2022.--Proceedings of SPIE - The International Society for Optical Engineering vol. 12181 Article number 121811W.-- Full list of authors: Zhang, Shuang-Nan; Santangelo, Andrea; Xu, Yupeng; Feroci, Marco; Hernanz, Margarita; Lu, Fangjun; Chen, Yong; Feng, Hua; Nandra, Kirpal; Jiang, Weichun; Svoboda, Jiri; Brandt, Soren; Schanne, Stephane; in't 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, Joerg; 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; Coti Zelati, Francesco; Cui, Weiwei; Cui, Tao; Cui, Wei; Dai, Boyu; Dauser, Thomas; De Angelis, Nicolas; De Marco, Barbara; De Rosa, Alessandra; Del Monte, Ettore; Di Cosimo, Sergio; Diebold, Sebastian; Dilillo, Giuseppe; Ding, Fei; Dohnal, Roman; Dong, Zefang; Donnarumma, Immacolata; Dovciak, Michal; Du, Yuanyuan; Ducci, Lorenzo; Evangelista, Yuri; Fan, Qingmei; Favre, Yannick; Ferres, Patricia; Fiandrini, Emanuele; Ficorella, Francesco; Fuschino, Fabio; Luis Galvez, Jose; 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; Lo Cicero, Ugo; Loehring, Jens; Lombardi, Giovanni; Lorenz, Maximilian; Lu, Bing; Lucchesi, Leonardo; Luo, Tao; Luo, Laidan; Ma, Jia; Ma, Xiang; Macera, Daniele; Malcovati, Piero; Manfreda, Alberto; Maria Paredes, Josep; 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; Novak, 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; Rodriguez Gil, Pablo; 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, Muberra; Sveda, 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, Joern; 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, 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. © 2022 SPIE. All rights reserved., The Chinese team acknowledges support by the Chinese Academy of Sciences through the Strategic Priority Research Program, Grant No. XDA15020100. The Italian authors acknowledge funding support by the Italian Space Agency (under agreement n. 2020-3-HH.0 and ASI-INAF n.2017-14-H.O) and INFN (project XRO -X-ray Observatories). The Spanish authors acknowledge funding support from the MICIN/AEI grant PID2019-108709GB-I00. The German team acknowledges support from the Bundesministerium fur Wirtschaft und Technologie through the Deutsches Zentrum fur Luft-und Raumfahrt e.V. (DLR) under the grant number FKZ 50 OO 1902. The Polish team acknowledges FNP grant POIR.04.04.00-00-5C65/17. The Czech team acknowledges support from the GACR project 21-06825X. The Turkish team acknowledges support from the Turkish Space Agency., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709

Published
2022
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11. Data

Author

Cramblet Alvarez, Leslie, Lattif, Chelsea, Trujillo, Marissa, Leach, Jonah, Rodriguez, Jerome, Weiser, Mikayla, Ringler, Rachael, and Jones, Nikki

Published
2022
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13. Survey

Author

Cramblet Alvarez, Leslie, Lattif, Chelsea, Trujillo, Marissa, Leach, Jonah, Rodriguez, Jerome, Weiser, Mikayla, Ringler, Rachael, and Jones, Nikki

Published
2022
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14. Literature

Author

Cramblet Alvarez, Leslie, Lattif, Chelsea, Trujillo, Marissa, Leach, Jonah, Rodriguez, Jerome, Weiser, Mikayla, Ringler, Rachael, and Jones, Nikki

Published
2022
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15. A Multiwavelength Study of GRS 1716-249 in Outburst

Author

Saikia, Payaswini, Russell, David M., Baglio, M. C., Bramich, D. M., Casella, Piergiorgio, Trigo, Maria Diaz, Gandhi, Poshak, Jiang, Jiachen, Maccarone, Thomas, Soria, Roberto, Al Noori, Hind, Al Yazeedi, Aisha, Alabarta, Kevin, Belloni, Tomaso, Bel, Marion Cadolle, Ceccobello, Chiara, Corbel, Stéphane, Fender, Rob, Gallo, Elena, Homan, Jeroen, Koljonen, Karri, Lewis, Fraser, Markoff, Sera B., Miller-Jones, James C.A., Rodriguez, Jerome, Russell, Thomas D., Shahbaz, Tariq, Sivakoff, Gregory R., Testa, Vincenzo, Tetarenko, Alexandra J., New York University Abu Dhabi, Osservatorio Astronomico Roma, European Southern Observatory, University of Southampton, University of Cambridge, Texas Tech University, University of Chinese Academy of Sciences, University of California Santa Barbara, Osservatorio Astronomico di Brera, Chalmers University of Technology, IRFM-CEA, University of Oxford, University of Michigan, Ann Arbor, Eureka Scientific, Inc., Metsähovi Radio Observatory, Cardiff University, University of Amsterdam, Curtin University, National Institute for Astrophysics, Instituto de Astrofísica de Canarias, University of Alberta, Aalto-yliopisto, and Aalto University

Abstract

Funding Information: The authors thank the anonymous referee for useful comments and suggestions. The authors also thank Lian Tao for the revised black hole mass estimation using the updated distance. D.M.R. and D.M.B. acknowledge the support of the NYU Abu Dhabi Research Enhancement Fund under grant RE124. J.J. acknowledges the support of the Leverhulme Trust, the Isaac Newton Trust, and St. Edmund’s college, University of Cambridge. R.S. acknowledges grant No. 12073029 from the Natural National Science Foundation of China (NSFC). S.M. is thankful for support by Dutch Research Council (NWO) VICI award, grant Nr. 639.043.513. T.M.B. acknowledges financial contribution from the agreement ASI- INAF n.2017-14-H.0 and from PRIN-INAF 2019 N.15. T.D.R. acknowledges financial contribution from the agreement ASI-INAF n.2017-14-H.0. T.S. acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under grant PID2020-114822GB-I00. G.R.S. is supported by NSERC Discovery Grants RGPIN-2016-06569 and RGPIN-2021-0400. K.I.I.K. acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 101002352) and from the Academy of Finland projects 320045 and 320085. This work uses data from the Faulkes Telescope Project, which is an education partner of Las Cumbres Observatory (LCO). The Faulkes Telescopes are maintained and operated by LCO. This work also uses observations made with the REM Telescope, INAF Chile. It is also based on observations collected at the European Southern Observatory under ESO programmes 098.D-0893 and 099.D-0884 (PI: D. Russell). Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51494.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. This work also makes use of data supplied by the UK Swift Science Data Centre at the University of Leicester, and the MAXI data provided by RIKEN, JAXA, and the MAXI team. Publisher Copyright: © 2022. The Author(s). Published by the American Astronomical Society. We present a detailed study of the evolution of the Galactic black hole transient GRS 1716-249 during its 2016-2017 outburst at optical (Las Cumbres Observatory), mid-infrared (Very Large Telescope), near-infrared (Rapid Eye Mount telescope), and ultraviolet (the Neil Gehrels Swift Observatory Ultraviolet/Optical Telescope) wavelengths, along with archival radio and X-ray data. We show that the optical/near-infrared and UV emission of the source mainly originates from a multi-temperature accretion disk, while the mid-infrared and radio emission are dominated by synchrotron emission from a compact jet. The optical/UV flux density is correlated with the X-ray emission when the source is in the hard state, consistent with an X-ray irradiated accretion disk with an additional contribution from the viscous disk during the outburst fade. We find evidence for a weak, but highly variable jet component at mid-infrared wavelengths. We also report the long-term optical light curve of the source and find that the quiescent i′ -band magnitude is 21.39 ± 0.15 mag. Furthermore, we discuss how previous estimates of the system parameters of the source are based on various incorrect assumptions, and so are likely to be inaccurate. By comparing our GRS 1716-249 data set to those of other outbursting black hole X-ray binaries, we find that while GRS 1716-249 shows similar X-ray behavior, it is noticeably optically fainter, if the literature distance of 2.4 kpc is adopted. Using several lines of reasoning, we argue that the source distance is further than previously assumed in the literature, likely within 4-17 kpc, with a most likely range of ∼4-8 kpc.

Published
2022

16. A Multiwavelength Study of GRS 1716-249 in Outburst: Constraints on Its System Parameters

Author

Saikia, Payaswini, primary, Russell, David M., additional, Baglio, M. C., additional, Bramich, D. M., additional, Casella, Piergiorgio, additional, Trigo, Maria Diaz, additional, Gandhi, Poshak, additional, Jiang, Jiachen, additional, Maccarone, Thomas, additional, Soria, Roberto, additional, Al Noori, Hind, additional, Al Yazeedi, Aisha, additional, Alabarta, Kevin, additional, Belloni, Tomaso, additional, Bel, Marion Cadolle, additional, Ceccobello, Chiara, additional, Corbel, Stéphane, additional, Fender, Rob, additional, Gallo, Elena, additional, Homan, Jeroen, additional, Koljonen, Karri, additional, Lewis, Fraser, additional, Markoff, Sera B., additional, Miller-Jones, James C. A., additional, Rodriguez, Jerome, additional, Russell, Thomas D., additional, Shahbaz, Tariq, additional, Sivakoff, Gregory R., additional, Testa, Vincenzo, additional, and Tetarenko, Alexandra J., additional

Published
2022
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17. 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

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

Author

Chakravorty, Susmita, Petrucci, Pierre-Olivier, Datta, Sudeb Ranjan, Ferreira, Jonathan, Wilms, Joern, Jacquemin-Ide, Jonatan, Clavel, Maica, Marcel, Gregoire, Rodriguez, Jerome, Malzac, Julien, Belmont, Renaud, Corbel, Stephane, Coriat, Mickael, Henri, Gilles, and Parra, Maxime

Subjects
BINARY black holes, OBSERVATORIES, X-ray spectra, ACCRETION disks, ABSORPTION, X-ray astronomy
Abstract

In our self-similar, analytical, magnetohydrodynamic (MHD) accretion–ejection solution, the density at the base of the outflow is explicitly dependent on the disc accretion rate – a unique property of this class of solutions. We had earlier found that the ejection index |$p \gt \sim 0.1 (\dot{M}_{\rm{acc}} \propto r^p)$| is a key MHD parameter that decides if the flow can cause absorption lines in the high resolution X-ray spectra of black hole binaries. Here, we choose three dense warm solutions with p  = 0.1, 0.3, 0.45 and carefully develop a methodology to generate spectra which are convolved with the Athena and XRISM response functions to predict what they will observe seeing through such MHD outflows. In this paper two other external parameters were varied – extent of the disc, |$\rm {r_o|_{\rm{max}}} = 10^5, \, 10^6 \, \, \rm {r_G}$|⁠ , and the angle of the line of sight, i ∼ 10–25°. Resultant absorption lines (H and He-like Fe, Ca, Ar) change in strength and their profiles manifest varying degrees of asymmetry. We checked if (a) the lines and (ii) the line asymmetries are detected, in our suit of synthetic Athena and XRISM spectra. Our analysis shows that Athena should detect the lines and their asymmetries for a standard 100 ks observation of a 100 mCrab source – lines with equivalent width as low as a few eV should be detected if the 6–8 keV counts are larger than 104–105 even for the least favourable simulated cases. [ABSTRACT FROM AUTHOR]

Published
2023
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