Complex Nuclear Structure in Seyfert 2 Galaxy NGC 4388 Revealed by XRISM Observation
Fuente:
arXiv
Salvato in:
| Autori principali: | , , , , , , , , , , , , , , , |
|---|---|
| Natura: | Preprint |
| Pubblicazione: |
2026
|
| Soggetti: | |
| Accesso online: | |
| Tags: |
Aggiungi Tag
Nessun Tag, puoi essere il primo ad aggiungerne!!
|
| _version_ | 1866910112052936704 |
|---|---|
| author | Fujiwara, Kanta Ueda, Yoshihiro Ogawa, Shoji Nakatani, Yuya Miller, Jon M. Okajima, Takashi Kawamuro, Taiki Boorman, Peter G. Gallo, Luigi Mizumoto, Misaki Mushotzky, Richard Noda, Hirofumi Terashima, Yuichi Tombesi, Francesco Meulen, Bert Vander Yamada, Satoshi |
| author_facet | Fujiwara, Kanta Ueda, Yoshihiro Ogawa, Shoji Nakatani, Yuya Miller, Jon M. Okajima, Takashi Kawamuro, Taiki Boorman, Peter G. Gallo, Luigi Mizumoto, Misaki Mushotzky, Richard Noda, Hirofumi Terashima, Yuichi Tombesi, Francesco Meulen, Bert Vander Yamada, Satoshi |
| contents | We report results from the simultaneous XRISM (183 ks) and NuSTAR (62 ks) observations of the Seyfert-2 galaxy NGC 4388. This AGN has the brightest Fe K$α$ line among Compton-thin, obscured sources. To model the reflection continuum and fluorescent lines, we employ an updated version of XCLUMPY and a broad line region model with a disk-like geometry. The profile of the neutral Fe-K fluorescent line is well described as the sum of three components convolved with Gaussians with FWHM values of $\sim 290\ \mathrm{km\ s^{-1}}$, $\sim 1470\ \mathrm{km\ s^{-1}}$, and $\sim 11100\ \mathrm{km\ s^{-1}}$. These line widths correspond to radii of 1.5 pc, 0.060 pc, and $1.0\times10^{-3}$ pc by assuming Keplerian motion, which we interpret as the dusty torus, its inner edge region, and the BLR, respectively. The data suggest that the Fe K$α$ BLR component is larger than that of H$α$ (FWHM of 4500 $\mathrm{km\ s^{-1}}$) in the polarized optical spectrum, implying that the velocity field of the BLR is dominated by that parallel to the equatorial plane. In addition, Fe XXVI Ly$α$ and Fe XXV absorption lines are detected, characterized by $\logξ \sim 3.50~\mathrm{erg\ cm\ s^{-1}}$, $\log{N_{\mathrm{H}}} \sim 22.1~\mathrm{cm^{-2}}$, $v_{\mathrm{out}} \sim 40\ \mathrm{km\ s^{-1}}$, and $σ_v \sim 160\ \mathrm{km\ s^{-1}}$. We infer that the absorber is gravitationally bound and is possibly associated with a failed wind, consistent with a radiation-driven fountain flow. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2604_06719 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Complex Nuclear Structure in Seyfert 2 Galaxy NGC 4388 Revealed by XRISM Observation Fujiwara, Kanta Ueda, Yoshihiro Ogawa, Shoji Nakatani, Yuya Miller, Jon M. Okajima, Takashi Kawamuro, Taiki Boorman, Peter G. Gallo, Luigi Mizumoto, Misaki Mushotzky, Richard Noda, Hirofumi Terashima, Yuichi Tombesi, Francesco Meulen, Bert Vander Yamada, Satoshi High Energy Astrophysical Phenomena Astrophysics of Galaxies We report results from the simultaneous XRISM (183 ks) and NuSTAR (62 ks) observations of the Seyfert-2 galaxy NGC 4388. This AGN has the brightest Fe K$α$ line among Compton-thin, obscured sources. To model the reflection continuum and fluorescent lines, we employ an updated version of XCLUMPY and a broad line region model with a disk-like geometry. The profile of the neutral Fe-K fluorescent line is well described as the sum of three components convolved with Gaussians with FWHM values of $\sim 290\ \mathrm{km\ s^{-1}}$, $\sim 1470\ \mathrm{km\ s^{-1}}$, and $\sim 11100\ \mathrm{km\ s^{-1}}$. These line widths correspond to radii of 1.5 pc, 0.060 pc, and $1.0\times10^{-3}$ pc by assuming Keplerian motion, which we interpret as the dusty torus, its inner edge region, and the BLR, respectively. The data suggest that the Fe K$α$ BLR component is larger than that of H$α$ (FWHM of 4500 $\mathrm{km\ s^{-1}}$) in the polarized optical spectrum, implying that the velocity field of the BLR is dominated by that parallel to the equatorial plane. In addition, Fe XXVI Ly$α$ and Fe XXV absorption lines are detected, characterized by $\logξ \sim 3.50~\mathrm{erg\ cm\ s^{-1}}$, $\log{N_{\mathrm{H}}} \sim 22.1~\mathrm{cm^{-2}}$, $v_{\mathrm{out}} \sim 40\ \mathrm{km\ s^{-1}}$, and $σ_v \sim 160\ \mathrm{km\ s^{-1}}$. We infer that the absorber is gravitationally bound and is possibly associated with a failed wind, consistent with a radiation-driven fountain flow. |
| title | Complex Nuclear Structure in Seyfert 2 Galaxy NGC 4388 Revealed by XRISM Observation |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2604.06719 |