Feeding versus feedback in AGN from near-infrared Integral Field Spectroscopy X: NGC5929

TL;DR

This study uses near-infrared integral field spectroscopy to analyze the gas and stellar kinematics, emission-line distributions, and AGN feedback mechanisms in the Seyfert 2 galaxy NGC5929, revealing complex interactions between the jet, gas, and stars.

Contribution

First detailed near-infrared integral field spectroscopic analysis of NGC5929 revealing gas dynamics, excitation mechanisms, and AGN feedback effects at 20 pc resolution.

Findings

Gas in the galaxy shows rotation and outflows influenced by the AGN.

Radio jets induce shocks and turbulence in the surrounding gas.

Black hole mass estimated at 52 million solar masses.

Abstract

We present near-infrared emission-line flux distributions, excitation and kinematics, as well as stellar kinematics, of the inner 520x520 pc2$ of the Seyfert 2 galaxy NGC5929. The observations were performed with the Gemini's Near-Infrared Integral Field Spectrograph (NIFS) at a spatial resolution of 20 pc and spectral resolution of 40km/s in the J- and K-bands. The flux distributions of H2, [FeII], [PII] and recombination lines are extended over most of the field of view, with the highest intensity levels observed along PA=60/240deg, and well correlated with the radio emission. The H2 and [FeII] line emission are originated in thermal processes, mainly due to heating of the gas by X-rays from the central Active Galactic Nucleus (AGN). Contribution of shocks due to the radio jet is observed at locations co-spatial with the radio hotspots at 0.5" northeast and 0.6" southwest of the nucleus, as evidenced by the emission-line ratio and gas kinematics. The stellar kinematics shows rotation with an amplitude at 250pc from the nucleus of 200 km/s after corrected for the inferred inclination of 18.3deg. The stellar velocity dispersion obtained from the integrated K-band spectrum is sigma*=133+/-8 km/s, which implying on a mass for the supermassive black hole of M=5.2E7 Msun, using the M-sigma* relation. The gas kinematics present three components: (1) gas in the plane of the galaxy in counter-rotation relative to the stars; (2) an outflow perpendicular to the radio jet that seems to be due to an equatorial AGN outflow; (3) turbulence of the gas observed in association with the radio hot spots, supporting an interaction of the radio jet with the gas of the disk. We estimated the mass of ionized and warm molecular gas of ~1.3E6 Msun and ~470 Msun, respectively.