A nuclear ionized gas outflow in the Seyfert 2 galaxy UGC 2024

Abstract

As part of a high-resolution observational study of feeding and feedback processes occurring in the vicinity of the active galactic nucleus in 40 galaxies, we observed the inner 3${^{\prime\prime}_{.}}$5 × 5 arcsec of the nearby spiral and Seyfert 2 galaxy UGC 2024 with the integral field unit of the Gemini-South Telescope. The observations enabled a study of the stellar and gas kinematics in this region at a spatial resolution of 0${^{\prime\prime}_{.}}$5 (218 pc), and a spectral resolution of 36 km s−1 over the wavelength range 4100–7300 Å. For the strongest emission-lines (H β, [$\rm{O\,{\small III}}$] λ5007 Å, H α, [$\rm{N\,{\small II}}$] λ6584 Å, and [$\rm{S\,{\small II}}$] λλ6717,6731 Å) we derived maps of the flux, radial velocity, and velocity dispersion. The flux distribution and kinematics of the [$\rm{O\,{\small III}}$] emission line are roughly symmetric around the nucleus: the radial velocity is close to systemic over the full field of view. The kinematics of the other strong emission lines trace both this systemic velocity component, and ordered rotation (with kinematic centre 0${^{\prime\prime}_{.}}$2 north-west of the nucleus). The stellar continuum morphology and kinematics are, however, asymmetrical around the nucleus. We interpret these unusual kinematics as the superposition of a component of gas rotating in the galaxy disc plus a ‘halo’ component of highly ionized gas. This halo either traces a quasi-spherical fountain with average radial velocity 200 km s−1, in which case the total nuclear outflow mass and momentum are 2 × 105 M⊙ and 4 × 107 M⊙ km s−1, respectively, or a dispersion supported halo created by a past nuclear starburst.

AGNIFS survey of local AGN: GMOS-IFU data and outflows in 30 sources

“…In order to be able to resolve the inner kpc of moderately active galaxies, our group AGNIFS (AGN Integral Field Spectroscopy) has observed over the years several AGN hosts using Gemini IFS in the optical (e.g. Fathi et al 2006;Storchi-Bergmann et al 2007; Barbosa et al 2009;Schnorr-Müller et al 2014a;Lena et al 2015;Schnorr-Müller et al 2016, 2017aBrum et al 2017;Slater et al 2018;Freitas et al 2018;Humire et al 2018;Muñoz-Vergara et al 2019;Soto-Pinto et al 2019) and in the near-IR (Storchi-Bergmann et al 2009, 2010Riffel et al 2017Riffel et al , 2018Schönell et al 2019). While we have so far focused on individual galaxies, in this paper we present data for 30 objects observed in the optical using the Gemini Multi-Object Spectrograph Integral Field Unit (GMOS-IFU).…”

Ionised Gas Kinematics in MaNGA AGN. Extents of the Narrow Line and Kinematically Disturbed regions

“…The KDR extents and how they relate to the size of the NLR is less clear. So far, studies on individual objects and small samples find ionised gas outflows on scales from tens of parsecs to kiloparsec (Das et al 2005(Das et al , 2007Storchi-Bergmann et al 2010;Liu et al 2013aLiu et al , 2014Barbosa et al 2014;Davies et al 2014;Cresci et al 2015;Riffel et al 2013Riffel et al , 2018Fischer et al 2017;Revalski et al 2018;Fischer et al 2018;Diniz et al 2019;Muñoz Vergara et al 2019;Soto-Pinto et al 2019). Here, we measure both the extent of the KDR and the size of the NLR.…”

Ionized and hot molecular outflows in the inner 500 pc of NGC1275

“…We adopt N e = 500 cm −3 , a typical value of the electron density measured for AGN based on the [S ii] emission lines (e.g., Dors et al 2014) and L Paβ = 5.4 × 10 39 erg s −1 , by integrating the fluxes of the broad Paβ components. Following previous spatially resolved studies of outflows (Riffel et al 2013b;Diniz et al 2019;Shimizu et al 2019;Muñoz-Vergara et al 2019;Soto-Pinto et al 2019;Fischer et al 2019;Gnilka et al 2020), we use the measured centroid velocity of the broad components as the velocity of the outflow: v out = 200 km s −1 (see middle panels of Figs. 8, A1 and A2).…”