The geometry of the hot corona in MCG-05-23-16 constrained by X-ray polarimetry

Tagliacozzo, D.; Marinucci, Andrea; Ursini, F.; Matt, Giorgio; Bianchi, S.; Baldini, Luca; Barnouin, Thibault; Rodriguez, N Cavero; Rosa, A. De; Gesu, Laura Di; Dovčiak, Michal; Harper, D; Ingram, Adam; Karas, Vladimír; Kim, Dawoon E.; Krawczynski, H.; Madejski, G.; Marin, Frédéric; Middei, R.; Marshall, Herman L.; Muleri, Fabio; Panagiotou, Christos; Petrucci, P.-O.; Podgorný, Jakub; Poutanen, Juri; Puccetti, S.; Soffitta, P.; Tombesi, Francesco; Veledina, Alexandra; Zhang, Wenda; Agudo, I.; Antonelli, L. A.; Bachetti, Matteo; Baumgartner, W. H.; Bellazzini, R.; Bongiorno, Stephen D.; Bonino, R.; Brez, A.; Bucciantini, N.; Capitanio, F.; Castellano, S; Cavazzuti, E.; Chen, Chun-Tao; Ciprini, S.; Costa, E.; Monte, E. Del; Lalla, N. Di; Marco, Alessandro Di; Donnarumma, I.; Doroshenko, V.; Ehlert, Steven R.; Enoto, Teruaki; Evangelista, Y.; Fabiani, Sergio; Ferrazzoli, Riccardo; García, Javier A.; Gunji, Shuichi; Heyl, Jeremy; Iwakiri, W.; Jorstad, Svetlana G.; Kaaret, Philip; Kislat, Fabian; Kitaguchi, Takao; Kolodziejczak, Jeffery J.; Monaca, Fabio La; Latronico, L.; Liodakis, Ioannis; Maldera, S.; Manfreda, Alberto; Marscher, A. P.; Massaro, F.; Mitsuishi, Ikuyuki; Mizuno, T.; Negro, Michela; Ng, C.‐Y.; O’Dell, Stephen L.; Omodei, N.; Oppedisano, C.; Papitto, A.; Pavlov, G. G.; Peirson, Abel L.; Perri, M.; Pesce-Rollins, Melissa; Pilia, M.; Possenti, A.; Ramsey, Brian D.; Rankin, John; Ratheesh, Ajay; Roberts, O. J.; Romani, Roger W.; Sgrò, C.; Slane, Patrick; Spandre, G.; Swartz, Douglas A.; Tamagawa, Toru; Tavecchio, F.; Taverna, Roberto; Tawara, Yuzuru; Tennant, Allyn F.; Thomas, Nicholas E.; Trois, A.; Tsygankov, Sergey S.; Turolla, R.; Vink, Jacco; Weisskopf, Martin C.; Wu, Kinwah; Xie, Fei; Zane, S.

doi:10.1093/mnras/stad2627

Cited by 21 publications

(4 citation statements)

References 58 publications

(64 reference statements)

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“…Analogs to these classes of sources can be found in active galactic nuclei, whose geometry studies are now also enabled by IXPE data. For the hardspectrum sources where the innermost parts of the accretion disk are visible, the X-ray polarization is found to be in a range of about a few percent (Cyg X-1, Krawczynski et al 2022;NGC 4151, Gianolli et al 2023;MCG-05-23-16, Marinucci et al 2022;Tagliacozzo et al 2023;IC 4329A, Ingram et al 2023) and aligned with the jet direction (wherever it is constrained). For the sources where the central engine is obscured, the observed spectrum is dominated by a reflection continuum, and high (PD >20%) polarization orthogonal to the jet direction (polarization aligned with the obscuring torus) has been found (Cyg X-3, Veledina et al 2023; Circinus galaxy, Ursini et al 2023).…”

Section: Discussionmentioning

confidence: 98%

Discovery of X-Ray Polarization from the Black Hole Transient Swift J1727.8−1613

Veledina,

Muleri,

Dovčiak

et al. 2023

ApJL

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We report the first detection of the X-ray polarization of the bright transient Swift J1727.8−1613 with the Imaging X-ray Polarimetry Explorer. The observation was performed at the beginning of the 2023 discovery outburst, when the source resided in the bright hard state. We find a time- and energy-averaged polarization degree of 4.1% ± 0.2% and a polarization angle of 2.°2 ± 1.°3 (errors at 68% confidence level; this translates to ∼20σ significance of the polarization detection). This finding suggests that the hot corona emitting the bulk of the detected X-rays is elongated, rather than spherical. The X-ray polarization angle is consistent with that found in submillimeter wavelengths. Since the submillimeter polarization was found to be aligned with the jet direction in other X-ray binaries, this indicates that the corona is elongated orthogonal to the jet.

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Section: Discussionmentioning

confidence: 98%

Discovery of X-Ray Polarization from the Black Hole Transient Swift J1727.8−1613

Veledina,

Muleri,

Dovčiak

et al. 2023

ApJL

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“…We stress, however, that the configuration of the corona remains unclear and difficult to distinguish from spectral analysis (e.g., Tortosa et al 2018). Further determination of coronal geometry usually requires additional information, for instance from X-ray reverberation mapping (e.g., Reynolds et al 1999;Fabian et al 2009;Kara et al 2016;Caballero-García et al 2020) or X-ray spectropolarimetry (e.g., Tagliacozzo et al 2023; but see Ingram et al 2023). Comparing well-understood theoretical emissivity profiles to the profile determined from the Fe line and applying constraints from reverberation lags can help establish the geometry (Wilkins & Fabian 2012), but this is beyond the scope of this work.…”

Section: Model Selectionmentioning

confidence: 99%

The Reliability of Accretion Disk Inclination Derived from X-Ray Spectroscopy of Active Galaxies

Du,

Ding,

et al. 2024

ApJ

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The inclination angle of substructures in active galaxies gives insights into physical components from scales of the vicinity of the central black hole to the entire host galaxy. We use the self-consistent reflection spectral model RELXILL to measure the inclination of the inner region of accretion disks with broadband (0.3–78 keV) X-ray observations, systematically studying the reliability of this methodology. To test the capability of the model to return statistically consistent results, we analyze multiepoch joint XMM-Newton and NuSTAR data of the narrow-line Seyfert 1 galaxy I Zwicky 1 and the broad-line radio galaxy 3C 382, which exhibit different degrees of spectral complexity and reflection features. As expected, we find that adding more data for analysis narrows the confidence interval and that multiepoch joint observations return optimal measurements; however, even single-epoch data can be well fitted if the reflection component is sufficiently dominant. Mock spectra are used to test the capability of RELXILL to recover input parameters from typical single-epoch joint observations. We find that inclination is well recovered at 90% confidence, with improved constraints at higher reflection fraction and higher inclination. Higher iron abundance and corona temperature tighten the constraints as well, but the effect is not as significant as a higher reflection fraction. The spin, however, has little effect in reflection-based inclination measurements. We conclude that broadband reflection spectroscopy can reliably measure inner accretion disk inclination.

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“…Since the beginning of IXPE operation, three unobscured radio-quiet Seyfert 1 galaxies have been observed (NGC 4151: [78], IC 4329A: [79], and MCG-05-23-16: [80,81]). The X-ray polarization analysis for RQAGN was conducted using both model-independent and spectropolarimetric analysis methods.…”

Section: Ixpe Observations Of Unobscured Radio-quiet Agnmentioning

confidence: 99%

Investigating the Properties of the Relativistic Jet and Hot Corona in AGN with X-ray Polarimetry

Kim,

Di Gesu,

Marin

et al. 2024

Galaxies

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X-ray polarimetry has been suggested as a prominent tool for investigating the geometrical and physical properties of the emissions from active galactic nuclei (AGN). The successful launch of the Imaging X-ray Polarimetry Explorer (IXPE) on 9 December 2021 has expanded the previously restricted scope of polarimetry into the X-ray domain, enabling X-ray polarimetric studies of AGN. Over a span of two years, IXPE has observed various AGN populations, including blazars and radio-quiet AGN. In this paper, we summarize the remarkable discoveries achieved thanks to the opening of the new window of X-ray polarimetry of AGN through IXPE observations. We will delve into two primary areas of interest: first, the magnetic field geometry and particle acceleration mechanisms in the jets of radio-loud AGN, such as blazars, where the relativistic acceleration process dominates the spectral energy distribution; and second, the geometry of the hot corona in radio-quiet AGN. Thus far, the IXPE results from blazars favor the energy-stratified shock acceleration model, and they provide evidence of helical magnetic fields inside the jet. Concerning the corona geometry, the IXPE results are consistent with a disk-originated slab-like or wedge-like shape, as could result from Comptonization around the accretion disk.

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The geometry of the hot corona in MCG-05-23-16 constrained by X-ray polarimetry

Cited by 21 publications

References 58 publications

Discovery of X-Ray Polarization from the Black Hole Transient Swift J1727.8−1613

Discovery of X-Ray Polarization from the Black Hole Transient Swift J1727.8−1613

The Reliability of Accretion Disk Inclination Derived from X-Ray Spectroscopy of Active Galaxies

Investigating the Properties of the Relativistic Jet and Hot Corona in AGN with X-ray Polarimetry

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