Constraining Disk-to-Corona Power Transfer Fraction, Soft X-ray Excess Origin, and Black Hole Spin Population of Type-1 AGN across Mass Scales
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| Autores principales: | , , , , , , , , |
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| Formato: | Preprint |
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2025
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| _version_ | 1866910801293475840 |
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| author | Mallick, Labani Pinto, Ciro Tomsick, John Markowitz, Alex Fabian, Andrew Safi-Harb, Samar Steiner, James Pacucci, Fabio Alston, William |
| author_facet | Mallick, Labani Pinto, Ciro Tomsick, John Markowitz, Alex Fabian, Andrew Safi-Harb, Samar Steiner, James Pacucci, Fabio Alston, William |
| contents | Understanding the nature of the accretion disk, its interplay with the X-ray corona, and assessing black hole spin demographics are some open challenges in astrophysics. In this work, we examine the predictions of the standard $α$-disk model, origin of the soft X-ray excess, and measure the black hole spin parameter by applying the updated high-density disk reflection model to the XMM-Newton/NuSTAR broadband (0.3$-$78 keV) X-ray spectra of a sample of Type-1 AGN. Our Bayesian analysis confirms that the high-density relativistic reflection model with a broken power-law emissivity profile can simultaneously fit the soft X-ray excess, broad iron K line, and Compton hump for $\sim$70% of the sample, while an additional warm Comptonization model is still required to describe the observed soft X-ray excess for the remaining sources. Our first-ever calculation of the disk-to-corona power transfer fraction reveals that the fraction of power released from the accretion disk into the hot corona can have diverse values, the sample median of which is $0.7_{-0.4}^{+0.2}$. We find that the transferred power from the accretion disk can potentially soften the X-ray spectrum of the hot corona. The median values of the hot coronal temperature and optical depth for the sample are estimated to be $63_{-11}^{+23}$ keV and $0.85_{-0.27}^{+0.12}$, respectively. Finally, through joint XMM-Newton+NuSTAR relativistic reflection spectroscopy, we systematically constrain the black hole spin parameter across the broad range of black hole masses, $\log(M_{\rm BH}/M_{\odot}) \sim 5.5-9.0$, and increase the available spin measurements in the AGN population by $\sim$20%. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2501_15380 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Constraining Disk-to-Corona Power Transfer Fraction, Soft X-ray Excess Origin, and Black Hole Spin Population of Type-1 AGN across Mass Scales Mallick, Labani Pinto, Ciro Tomsick, John Markowitz, Alex Fabian, Andrew Safi-Harb, Samar Steiner, James Pacucci, Fabio Alston, William High Energy Astrophysical Phenomena Astrophysics of Galaxies Space Physics Understanding the nature of the accretion disk, its interplay with the X-ray corona, and assessing black hole spin demographics are some open challenges in astrophysics. In this work, we examine the predictions of the standard $α$-disk model, origin of the soft X-ray excess, and measure the black hole spin parameter by applying the updated high-density disk reflection model to the XMM-Newton/NuSTAR broadband (0.3$-$78 keV) X-ray spectra of a sample of Type-1 AGN. Our Bayesian analysis confirms that the high-density relativistic reflection model with a broken power-law emissivity profile can simultaneously fit the soft X-ray excess, broad iron K line, and Compton hump for $\sim$70% of the sample, while an additional warm Comptonization model is still required to describe the observed soft X-ray excess for the remaining sources. Our first-ever calculation of the disk-to-corona power transfer fraction reveals that the fraction of power released from the accretion disk into the hot corona can have diverse values, the sample median of which is $0.7_{-0.4}^{+0.2}$. We find that the transferred power from the accretion disk can potentially soften the X-ray spectrum of the hot corona. The median values of the hot coronal temperature and optical depth for the sample are estimated to be $63_{-11}^{+23}$ keV and $0.85_{-0.27}^{+0.12}$, respectively. Finally, through joint XMM-Newton+NuSTAR relativistic reflection spectroscopy, we systematically constrain the black hole spin parameter across the broad range of black hole masses, $\log(M_{\rm BH}/M_{\odot}) \sim 5.5-9.0$, and increase the available spin measurements in the AGN population by $\sim$20%. |
| title | Constraining Disk-to-Corona Power Transfer Fraction, Soft X-ray Excess Origin, and Black Hole Spin Population of Type-1 AGN across Mass Scales |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies Space Physics |
| url | https://arxiv.org/abs/2501.15380 |