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| Médium: | Preprint |
| Vydáno: |
2023
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| Témata: | |
| On-line přístup: | https://arxiv.org/abs/2312.04421 |
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| _version_ | 1866917677293895680 |
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| author | Churazov, Eugene Khabibullin, Ildar Barnouin, Thibault Bucciantini, Niccolò Costa, Enrico Di Gesu, Laura Di Marco, Alessandro Ferrazzoli, Riccardo Forman, William Kaaret, Philip Kim, Dawoon E. Kolodziejczak, Jeffery J. Kraft, Ralph Marin, Frédéric Matt, Giorgio Negro, Michela Romani, Roger W. Silvestri, Stefano Soffitta, Paolo Sunyaev, Rashid Svoboda, Jiri Vikhlinin, Alexey Weisskopf, Martin C. Xie, Fei Agudo, Iván Antonelli, Lucio A. Bachetti, Matteo Baldini, Luca Baumgartner, Wayne H. Bellazzini, Ronaldo Bianchi, Stefano Bongiorno, Stephen D. Bonino, Raffaella Brez, Alessandro Capitanio, Fiamma Castellano, Simone Cavazzuti, Elisabetta Chen, Chien-Ting Ciprini, Stefano De Rosa, Alessandra Del Monte, Ettore Di Lalla, Niccolò Donnarumma, Immacolata Doroshenko, Victor Dovčiak, Michal Ehlert, Steven R. Enoto, Teruaki Evangelista, Yuri Fabiani, Sergio García, Javier A. Gunji, Shuichi Hayashida, Kiyoshi Heyl, Jeremy Iwakiri, Wataru Jorstad, Svetlana G. Karas, Vladimir Kislat, Fabian Kitaguchi, Takao Krawczynski, Henric La Monaca, Fabio Latronico, Luca Liodakis, Ioannis Maldera, Simone Manfreda, Alberto Marinucci, Andrea Marscher, Alan P. Marshall, Herman L. Massaro, Francesco Mitsuishi, Ikuyuki Mizuno, Tsunefumi Muleri, Fabio Ng, Chi-Yung O'Dell, Stephen L. Omodei, Nicola Oppedisano, Chiara Papitto, Alessandro Pavlov, George G. Peirson, Abel L. Perri, Matteo Pesce-Rollins, Melissa Petrucci, Pierre-Olivier Pilia, Maura Possenti, Andrea Poutanen, Juri Puccetti, Simonetta Ramsey, Brian D. Rankin, John Ratheesh, Ajay Roberts, Oliver J. Sgrò, Carmelo Slane, Patrick Spandre, Gloria Swartz, Douglas A. Tamagawa, Toru Tavecchio, Fabrizio Taverna, Roberto Tawara, Yuzuru Tennant, Allyn F. Thomas, Nicholas E. Tombesi, Francesco Trois, Alessio Tsygankov, Sergey S. Turolla, Roberto Vink, Jacco Wu, Kinwah Zane, Silvia |
| author_facet | Churazov, Eugene Khabibullin, Ildar Barnouin, Thibault Bucciantini, Niccolò Costa, Enrico Di Gesu, Laura Di Marco, Alessandro Ferrazzoli, Riccardo Forman, William Kaaret, Philip Kim, Dawoon E. Kolodziejczak, Jeffery J. Kraft, Ralph Marin, Frédéric Matt, Giorgio Negro, Michela Romani, Roger W. Silvestri, Stefano Soffitta, Paolo Sunyaev, Rashid Svoboda, Jiri Vikhlinin, Alexey Weisskopf, Martin C. Xie, Fei Agudo, Iván Antonelli, Lucio A. Bachetti, Matteo Baldini, Luca Baumgartner, Wayne H. Bellazzini, Ronaldo Bianchi, Stefano Bongiorno, Stephen D. Bonino, Raffaella Brez, Alessandro Capitanio, Fiamma Castellano, Simone Cavazzuti, Elisabetta Chen, Chien-Ting Ciprini, Stefano De Rosa, Alessandra Del Monte, Ettore Di Lalla, Niccolò Donnarumma, Immacolata Doroshenko, Victor Dovčiak, Michal Ehlert, Steven R. Enoto, Teruaki Evangelista, Yuri Fabiani, Sergio García, Javier A. Gunji, Shuichi Hayashida, Kiyoshi Heyl, Jeremy Iwakiri, Wataru Jorstad, Svetlana G. Karas, Vladimir Kislat, Fabian Kitaguchi, Takao Krawczynski, Henric La Monaca, Fabio Latronico, Luca Liodakis, Ioannis Maldera, Simone Manfreda, Alberto Marinucci, Andrea Marscher, Alan P. Marshall, Herman L. Massaro, Francesco Mitsuishi, Ikuyuki Mizuno, Tsunefumi Muleri, Fabio Ng, Chi-Yung O'Dell, Stephen L. Omodei, Nicola Oppedisano, Chiara Papitto, Alessandro Pavlov, George G. Peirson, Abel L. Perri, Matteo Pesce-Rollins, Melissa Petrucci, Pierre-Olivier Pilia, Maura Possenti, Andrea Poutanen, Juri Puccetti, Simonetta Ramsey, Brian D. Rankin, John Ratheesh, Ajay Roberts, Oliver J. Sgrò, Carmelo Slane, Patrick Spandre, Gloria Swartz, Douglas A. Tamagawa, Toru Tavecchio, Fabrizio Taverna, Roberto Tawara, Yuzuru Tennant, Allyn F. Thomas, Nicholas E. Tombesi, Francesco Trois, Alessio Tsygankov, Sergey S. Turolla, Roberto Vink, Jacco Wu, Kinwah Zane, Silvia |
| contents | We report the discovery of X-ray polarization from the X-ray-bright filament. G0.13-0.11 in the Galactic center (GC) region. This filament features a bright, hard X-ray source that is most plausibly a pulsar wind nebula (PWN) and an extended and structured diffuse component. Combining the polarization signal from IXPE with the imaging/spectroscopic data from Chandra, we find that X-ray emission of G0.13-0.11 is highly polarized PD=$57(\pm18)$% in the 3-6 keV band, while the polarization angle is PA=$21^\circ(\pm9^\circ)$. This high degree of polarization proves the synchrotron origin of the X-ray emission from G0.13-0.11. In turn, the measured polarization angle implies that the X-ray emission is polarized approximately perpendicular to a sequence of nonthermal radio filaments that may be part of the GC Radio Arc. The magnetic field on the order of $100\,{\rmμG}$ appears to be preferentially ordered along the filaments. The above field strength is the fiducial value that makes our model self-consistent, while the other conclusions are largely model independent. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2312_04421 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Pulsar-wind-nebula-powered Galactic center X-ray filament G0.13-0.11: Proof of the synchrotron nature by IXPE Churazov, Eugene Khabibullin, Ildar Barnouin, Thibault Bucciantini, Niccolò Costa, Enrico Di Gesu, Laura Di Marco, Alessandro Ferrazzoli, Riccardo Forman, William Kaaret, Philip Kim, Dawoon E. Kolodziejczak, Jeffery J. Kraft, Ralph Marin, Frédéric Matt, Giorgio Negro, Michela Romani, Roger W. Silvestri, Stefano Soffitta, Paolo Sunyaev, Rashid Svoboda, Jiri Vikhlinin, Alexey Weisskopf, Martin C. Xie, Fei Agudo, Iván Antonelli, Lucio A. Bachetti, Matteo Baldini, Luca Baumgartner, Wayne H. Bellazzini, Ronaldo Bianchi, Stefano Bongiorno, Stephen D. Bonino, Raffaella Brez, Alessandro Capitanio, Fiamma Castellano, Simone Cavazzuti, Elisabetta Chen, Chien-Ting Ciprini, Stefano De Rosa, Alessandra Del Monte, Ettore Di Lalla, Niccolò Donnarumma, Immacolata Doroshenko, Victor Dovčiak, Michal Ehlert, Steven R. Enoto, Teruaki Evangelista, Yuri Fabiani, Sergio García, Javier A. Gunji, Shuichi Hayashida, Kiyoshi Heyl, Jeremy Iwakiri, Wataru Jorstad, Svetlana G. Karas, Vladimir Kislat, Fabian Kitaguchi, Takao Krawczynski, Henric La Monaca, Fabio Latronico, Luca Liodakis, Ioannis Maldera, Simone Manfreda, Alberto Marinucci, Andrea Marscher, Alan P. Marshall, Herman L. Massaro, Francesco Mitsuishi, Ikuyuki Mizuno, Tsunefumi Muleri, Fabio Ng, Chi-Yung O'Dell, Stephen L. Omodei, Nicola Oppedisano, Chiara Papitto, Alessandro Pavlov, George G. Peirson, Abel L. Perri, Matteo Pesce-Rollins, Melissa Petrucci, Pierre-Olivier Pilia, Maura Possenti, Andrea Poutanen, Juri Puccetti, Simonetta Ramsey, Brian D. Rankin, John Ratheesh, Ajay Roberts, Oliver J. Sgrò, Carmelo Slane, Patrick Spandre, Gloria Swartz, Douglas A. Tamagawa, Toru Tavecchio, Fabrizio Taverna, Roberto Tawara, Yuzuru Tennant, Allyn F. Thomas, Nicholas E. Tombesi, Francesco Trois, Alessio Tsygankov, Sergey S. Turolla, Roberto Vink, Jacco Wu, Kinwah Zane, Silvia High Energy Astrophysical Phenomena We report the discovery of X-ray polarization from the X-ray-bright filament. G0.13-0.11 in the Galactic center (GC) region. This filament features a bright, hard X-ray source that is most plausibly a pulsar wind nebula (PWN) and an extended and structured diffuse component. Combining the polarization signal from IXPE with the imaging/spectroscopic data from Chandra, we find that X-ray emission of G0.13-0.11 is highly polarized PD=$57(\pm18)$% in the 3-6 keV band, while the polarization angle is PA=$21^\circ(\pm9^\circ)$. This high degree of polarization proves the synchrotron origin of the X-ray emission from G0.13-0.11. In turn, the measured polarization angle implies that the X-ray emission is polarized approximately perpendicular to a sequence of nonthermal radio filaments that may be part of the GC Radio Arc. The magnetic field on the order of $100\,{\rmμG}$ appears to be preferentially ordered along the filaments. The above field strength is the fiducial value that makes our model self-consistent, while the other conclusions are largely model independent. |
| title | Pulsar-wind-nebula-powered Galactic center X-ray filament G0.13-0.11: Proof of the synchrotron nature by IXPE |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2312.04421 |