AGN outflows and their properties in Mrk 766 as revealed by KOOLS-IFU on the Seimei Telescope
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2025
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| author | Oh, Kyuseok Ueda, Yoshihiro Yamada, Satoshi Toba, Yoshiki Isogai, Keisuke Tanimoto, Atsushi Ogawa, Shoji Uematsu, Ryosuke Nakatani, Yuya Fujiwara, Kanta Okada, Yuta Matsubayashi, Kazuya Setoguchi, Kenta |
| author_facet | Oh, Kyuseok Ueda, Yoshihiro Yamada, Satoshi Toba, Yoshiki Isogai, Keisuke Tanimoto, Atsushi Ogawa, Shoji Uematsu, Ryosuke Nakatani, Yuya Fujiwara, Kanta Okada, Yuta Matsubayashi, Kazuya Setoguchi, Kenta |
| contents | We present the emission-line flux distributions and their ratios, as well as the gas outflow features, of the innermost 2 kpc region of the type 1 Seyfert galaxy Mrk 766, using the Kyoto Okayama Optical Low-dispersion Spectrograph with an optical-fiber integral field unit on the Seimei Telescope. We find that the central region of Mrk 766 is kinematically disturbed, exhibiting asymmetric and radially distributed AGN-driven ionized gas outflows traced by \OIII\ with velocities exceeding 500 \kms. The mass of the ionized gas outflow is estimated to be $10^{4.65-5.95} M_{\odot}$, and the mass outflow rate is $0.14-2.73$ M${\odot}$ yr$^{-1}$. This corresponds to a kinetic power, $\dot{E}_{\rm K}$, of $4.31 \times 10^{40} \ {\rm erg} \ {\rm s^{-1}}< \dot{E}_{\rm K} < 8.62 \times 10^{41} \ {\rm erg} \ {\rm s^{-1}}$, which is equivalent to $0.08\%-1.53\%$ of the bolometric luminosity, $L_{\rm bol}$. This result is consistent with other observed properties of ionized gas outflows, although it is lower than the theoretical predictions in AGN feedback models ($\sim5\%$), implying that ionized gas outflows traced by \OIII\ represent only a minor fraction of the total outflows ejected from the host galaxy. Given the asymmetric and radially distributed outflow signatures observed across the host galaxy within the limited field of view, the maximum distance the outflowing gas has traveled remains an open question. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_02936 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | AGN outflows and their properties in Mrk 766 as revealed by KOOLS-IFU on the Seimei Telescope Oh, Kyuseok Ueda, Yoshihiro Yamada, Satoshi Toba, Yoshiki Isogai, Keisuke Tanimoto, Atsushi Ogawa, Shoji Uematsu, Ryosuke Nakatani, Yuya Fujiwara, Kanta Okada, Yuta Matsubayashi, Kazuya Setoguchi, Kenta Astrophysics of Galaxies We present the emission-line flux distributions and their ratios, as well as the gas outflow features, of the innermost 2 kpc region of the type 1 Seyfert galaxy Mrk 766, using the Kyoto Okayama Optical Low-dispersion Spectrograph with an optical-fiber integral field unit on the Seimei Telescope. We find that the central region of Mrk 766 is kinematically disturbed, exhibiting asymmetric and radially distributed AGN-driven ionized gas outflows traced by \OIII\ with velocities exceeding 500 \kms. The mass of the ionized gas outflow is estimated to be $10^{4.65-5.95} M_{\odot}$, and the mass outflow rate is $0.14-2.73$ M${\odot}$ yr$^{-1}$. This corresponds to a kinetic power, $\dot{E}_{\rm K}$, of $4.31 \times 10^{40} \ {\rm erg} \ {\rm s^{-1}}< \dot{E}_{\rm K} < 8.62 \times 10^{41} \ {\rm erg} \ {\rm s^{-1}}$, which is equivalent to $0.08\%-1.53\%$ of the bolometric luminosity, $L_{\rm bol}$. This result is consistent with other observed properties of ionized gas outflows, although it is lower than the theoretical predictions in AGN feedback models ($\sim5\%$), implying that ionized gas outflows traced by \OIII\ represent only a minor fraction of the total outflows ejected from the host galaxy. Given the asymmetric and radially distributed outflow signatures observed across the host galaxy within the limited field of view, the maximum distance the outflowing gas has traveled remains an open question. |
| title | AGN outflows and their properties in Mrk 766 as revealed by KOOLS-IFU on the Seimei Telescope |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2504.02936 |