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| Auteurs principaux: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| Accès en ligne: | https://arxiv.org/abs/2503.22665 |
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| _version_ | 1866910963847921664 |
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| author | Ewing, Melissa Parra, Maxime Mastroserio, Guglielmo Veledina, Alexandra Ingram, Adam Dovčiak, Michal García, Javier A. Russell, Thomas D. Baglio, Maria C. Poutanen, Juri Adegoke, Oluwashina Bianchi, Stefano Capitanio, Fiamma Connors, Riley Del Santo, Melania De Marco, Barbara Trigo, María Díaz Gandhi, Poshak Gupta, Maitrayee Kang, Chulsoo Kammoun, Elias Loktev, Vladislav Marra, Lorenzo Matt, Giorgio Nathan, Edward Petrucci, Pierre-Olivier Shidatsu, Megumi Steiner, James F. Tombesi, Francesco |
| author_facet | Ewing, Melissa Parra, Maxime Mastroserio, Guglielmo Veledina, Alexandra Ingram, Adam Dovčiak, Michal García, Javier A. Russell, Thomas D. Baglio, Maria C. Poutanen, Juri Adegoke, Oluwashina Bianchi, Stefano Capitanio, Fiamma Connors, Riley Del Santo, Melania De Marco, Barbara Trigo, María Díaz Gandhi, Poshak Gupta, Maitrayee Kang, Chulsoo Kammoun, Elias Loktev, Vladislav Marra, Lorenzo Matt, Giorgio Nathan, Edward Petrucci, Pierre-Olivier Shidatsu, Megumi Steiner, James F. Tombesi, Francesco |
| contents | We report the first detection of the X-ray polarisation of the transient black hole X-ray binary IGRJ17091-3624 taken with the Imaging X-ray polarimetry Explorer (IXPE) in March 2025, and present the results of an X-ray spectro-polarimetric analysis. The polarisation was measured in the 2--8 keV band with 5.2$σ$ statistical confidence. We report a polarisation degree (PD) of $9.1\pm1.6$ per cent and a polarisation angle of $83^{\circ} \pm 5^{\circ}$ (errors are $1σ$ confidence). There is a hint of a positive correlation of PD with energy that is not statistically significant. We report that the source is in the corona-dominated hard state, which is confirmed by a hard power-law dominated spectrum with weak reflection features and the presence of a Type-C quasi-periodic oscillation at $\sim0.2$~Hz. The orientation of the emitted radio jet is not known, and so we are unable to compare it with the direction of X-ray polarization, but we predict the two to be parallel if the geometry is similar to that in Cygnus X-1 and Swift J1727.8-1613, the two hard state black hole binaries previously observed by IXPE. In the Comptonisation scenario, the high observed PD requires a very favourable geometry of the corona, a high inclination angle (supported by the presence of a dip in the light curve) and possibly a mildly relativistic outflow and/or scattering in an optically thick wind. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_22665 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The very high X-ray polarisation of accreting black hole IGRJ17091-3624 in the hard state Ewing, Melissa Parra, Maxime Mastroserio, Guglielmo Veledina, Alexandra Ingram, Adam Dovčiak, Michal García, Javier A. Russell, Thomas D. Baglio, Maria C. Poutanen, Juri Adegoke, Oluwashina Bianchi, Stefano Capitanio, Fiamma Connors, Riley Del Santo, Melania De Marco, Barbara Trigo, María Díaz Gandhi, Poshak Gupta, Maitrayee Kang, Chulsoo Kammoun, Elias Loktev, Vladislav Marra, Lorenzo Matt, Giorgio Nathan, Edward Petrucci, Pierre-Olivier Shidatsu, Megumi Steiner, James F. Tombesi, Francesco High Energy Astrophysical Phenomena We report the first detection of the X-ray polarisation of the transient black hole X-ray binary IGRJ17091-3624 taken with the Imaging X-ray polarimetry Explorer (IXPE) in March 2025, and present the results of an X-ray spectro-polarimetric analysis. The polarisation was measured in the 2--8 keV band with 5.2$σ$ statistical confidence. We report a polarisation degree (PD) of $9.1\pm1.6$ per cent and a polarisation angle of $83^{\circ} \pm 5^{\circ}$ (errors are $1σ$ confidence). There is a hint of a positive correlation of PD with energy that is not statistically significant. We report that the source is in the corona-dominated hard state, which is confirmed by a hard power-law dominated spectrum with weak reflection features and the presence of a Type-C quasi-periodic oscillation at $\sim0.2$~Hz. The orientation of the emitted radio jet is not known, and so we are unable to compare it with the direction of X-ray polarization, but we predict the two to be parallel if the geometry is similar to that in Cygnus X-1 and Swift J1727.8-1613, the two hard state black hole binaries previously observed by IXPE. In the Comptonisation scenario, the high observed PD requires a very favourable geometry of the corona, a high inclination angle (supported by the presence of a dip in the light curve) and possibly a mildly relativistic outflow and/or scattering in an optically thick wind. |
| title | The very high X-ray polarisation of accreting black hole IGRJ17091-3624 in the hard state |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2503.22665 |