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| Main Authors: | , , , , , , , , |
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| Format: | Preprint |
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2024
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2406.15901 |
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| _version_ | 1866929395722092544 |
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| author | Elías-Chávez, M. Longinotti, A. L. Krongold, Y. Rosa-González, D. Vignali, C. Mathur, S. Miyaji, T. Mayya, Y. D. Nicastro, F. |
| author_facet | Elías-Chávez, M. Longinotti, A. L. Krongold, Y. Rosa-González, D. Vignali, C. Mathur, S. Miyaji, T. Mayya, Y. D. Nicastro, F. |
| contents | In this work, we present the results of a detailed X-ray spectral analysis of the brightest AGNs detected in the XMM-Newton 1.75 Ms Ultra Narrow Deep Field. We analyzed 23 AGNs that have a luminosity range of $\sim 10^{42} - 10^{46}\, \rm{erg}\, \rm{s}^{-1}$ in the $2 - 10\, \rm{keV}$ energy band, redshifts up to 2.66, and $\sim 10,000$ X-ray photon counts in the $0.3 - 10\, \rm{keV}$ energy band. Our analysis confirms the Iwasawa-Taniguchi effect, an anti-correlation between the X-ray luminosity ($L_x$) and the Fe-k$α$ Equivalent Width ($EW_{Fe}$) possibly associated with the decreasing of the torus covering factor as the AGN luminosity increases. We investigated the relationship among black hole mass ($M_{BH}$), $L_x$, and X-ray variability, quantified by the Normalized Excess Variance ($σ^2_{rms}$). Our analysis suggest an anti-correlation in both $M_{BH} - σ^2_{rms}$ and $L_x- σ^2_{rms}$ relations. The first is described as $σ^2_{rms} \propto M^{-0.26 \pm 0.05}_{BH}$, while the second presents a similar trend with $σ^2_{rms} \propto L_{x}^{-0.31 \pm 0.04}$. These results support the idea that the luminosity-variability anti-correlation is a byproduct of an intrinsic relationship between the BH mass and the X-ray variability, through the size of the emitting region. Finally, we found a strong correlation among the Eddington ratio ($λ_{Edd}$), the hard X-ray photon index ($Γ$), and the illumination factor $\log(A)$, which is related to the ratio between the number of Compton scattered photons and the number of seed photons. The $\log(λ_{Edd})-Γ-\log(A)$ plane could arise naturally from the connection between the accretion flow and the hot corona. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2406_15901 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | XMM-Newton Ultra Narrow Deep Field survey II: X-ray spectral analysis of the brightest AGN population Elías-Chávez, M. Longinotti, A. L. Krongold, Y. Rosa-González, D. Vignali, C. Mathur, S. Miyaji, T. Mayya, Y. D. Nicastro, F. High Energy Astrophysical Phenomena In this work, we present the results of a detailed X-ray spectral analysis of the brightest AGNs detected in the XMM-Newton 1.75 Ms Ultra Narrow Deep Field. We analyzed 23 AGNs that have a luminosity range of $\sim 10^{42} - 10^{46}\, \rm{erg}\, \rm{s}^{-1}$ in the $2 - 10\, \rm{keV}$ energy band, redshifts up to 2.66, and $\sim 10,000$ X-ray photon counts in the $0.3 - 10\, \rm{keV}$ energy band. Our analysis confirms the Iwasawa-Taniguchi effect, an anti-correlation between the X-ray luminosity ($L_x$) and the Fe-k$α$ Equivalent Width ($EW_{Fe}$) possibly associated with the decreasing of the torus covering factor as the AGN luminosity increases. We investigated the relationship among black hole mass ($M_{BH}$), $L_x$, and X-ray variability, quantified by the Normalized Excess Variance ($σ^2_{rms}$). Our analysis suggest an anti-correlation in both $M_{BH} - σ^2_{rms}$ and $L_x- σ^2_{rms}$ relations. The first is described as $σ^2_{rms} \propto M^{-0.26 \pm 0.05}_{BH}$, while the second presents a similar trend with $σ^2_{rms} \propto L_{x}^{-0.31 \pm 0.04}$. These results support the idea that the luminosity-variability anti-correlation is a byproduct of an intrinsic relationship between the BH mass and the X-ray variability, through the size of the emitting region. Finally, we found a strong correlation among the Eddington ratio ($λ_{Edd}$), the hard X-ray photon index ($Γ$), and the illumination factor $\log(A)$, which is related to the ratio between the number of Compton scattered photons and the number of seed photons. The $\log(λ_{Edd})-Γ-\log(A)$ plane could arise naturally from the connection between the accretion flow and the hot corona. |
| title | XMM-Newton Ultra Narrow Deep Field survey II: X-ray spectral analysis of the brightest AGN population |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2406.15901 |