XRISM/Resolve Spectroscopy of the Central Engine in the Seyfert-1 AGN Mrk 279
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| Main Authors: | , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866915571521552384 |
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| author | Miller, Jon M. Xiang, Xin Byun, Doyee Behar, Ehud Brenneman, Laura Cackett, Edward Costantini, Elisa Gallo, Luigi Horne, Keith Kammoun, Elias Li, Chen Zoghbi, Abderahmen |
| author_facet | Miller, Jon M. Xiang, Xin Byun, Doyee Behar, Ehud Brenneman, Laura Cackett, Edward Costantini, Elisa Gallo, Luigi Horne, Keith Kammoun, Elias Li, Chen Zoghbi, Abderahmen |
| contents | High-resolution X-ray spectroscopy with XRISM gives an unprecedented view of the ``central engine'' in active galactic nuclei, providing unique insights into black hole accretion and feedback. We present an analysis of the first XRISM/Resolve spectrum of the Seyfert-1 galaxy Mrk 279, known for its complex line profiles and variability. The data reveal velocity components within the Fe K$_α$ emission line that can be associated with the inner face of the molecular torus ($r \geq 10^{4}~GM/c^{2})$, the broad line region (BLR; $r = 1650^{+5780}_{-1480}~GM/c^{2}$), and the inner accretion disk ($r = 81^{+280}_{-75}~GM/c^{2}$). We find evidence of low-velocity, highly ionized gas that contributes an H-like Fe XXVI emission line at 6.97 keV, confirming suggestions from prior low-resolution spectra. The data do not show slow winds in absorption, but two pairs of lines - consistent with He-like and H-like Fe shifted by $v\simeq 0.22c$ and $v\simeq 0.33c$ - improve the fit, and could represent an ultra-fast outflow (UFO). Their addition to the model only reduces the Akaike Information Criterion by 3.6 and 3.5, respectively, signaling modest support. Additional observations are needed to definitively test for the presence of fast X-ray winds in Mrk 279. We discuss these results in the context of the geometry of the central engine in AGN, emerging trends in XRISM studies of AGN, and the nature of the potential UFOs. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2510_20083 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | XRISM/Resolve Spectroscopy of the Central Engine in the Seyfert-1 AGN Mrk 279 Miller, Jon M. Xiang, Xin Byun, Doyee Behar, Ehud Brenneman, Laura Cackett, Edward Costantini, Elisa Gallo, Luigi Horne, Keith Kammoun, Elias Li, Chen Zoghbi, Abderahmen High Energy Astrophysical Phenomena Astrophysics of Galaxies High-resolution X-ray spectroscopy with XRISM gives an unprecedented view of the ``central engine'' in active galactic nuclei, providing unique insights into black hole accretion and feedback. We present an analysis of the first XRISM/Resolve spectrum of the Seyfert-1 galaxy Mrk 279, known for its complex line profiles and variability. The data reveal velocity components within the Fe K$_α$ emission line that can be associated with the inner face of the molecular torus ($r \geq 10^{4}~GM/c^{2})$, the broad line region (BLR; $r = 1650^{+5780}_{-1480}~GM/c^{2}$), and the inner accretion disk ($r = 81^{+280}_{-75}~GM/c^{2}$). We find evidence of low-velocity, highly ionized gas that contributes an H-like Fe XXVI emission line at 6.97 keV, confirming suggestions from prior low-resolution spectra. The data do not show slow winds in absorption, but two pairs of lines - consistent with He-like and H-like Fe shifted by $v\simeq 0.22c$ and $v\simeq 0.33c$ - improve the fit, and could represent an ultra-fast outflow (UFO). Their addition to the model only reduces the Akaike Information Criterion by 3.6 and 3.5, respectively, signaling modest support. Additional observations are needed to definitively test for the presence of fast X-ray winds in Mrk 279. We discuss these results in the context of the geometry of the central engine in AGN, emerging trends in XRISM studies of AGN, and the nature of the potential UFOs. |
| title | XRISM/Resolve Spectroscopy of the Central Engine in the Seyfert-1 AGN Mrk 279 |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2510.20083 |