2025/04/03 by Kyuseok Oh, Oh, Kyuseok, Yoshihiro Ueda +22
Engineering · Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Space Technology and Applications
paper · pdf · doi:10.48550/arxiv.2504.02936
openalex publication_date 2025/04/03 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
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 104.65-5.95 M\odot, and the mass outflow rate is 0.14-2.73 M\odot yr-1. This corresponds to a kinetic power, E\rm K, of 4.31 × 1040 \rm erg \rm s-1< E\rm K < 8.62 × 1041 \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 (∼5%), 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.