Outflowing gas in a compact ionization cone in the Seyfert 2 galaxy ESO 153-G20

Soto-Pinto, Pamela; Nagar, Neil M.; Finlez, C.; Muñoz-Vergara, Dania; Slater, R.; Humire, P. K.; Storchi‐Bergmann, Thaisa; Lena, Davide; Kraemer, S. B.; Fischer, Travis C.; Schmitt, H. R.; Riffel, Rogemar A.; Schnorr-Müller, A.; Robinson, Andrew; Crenshaw, D. Michael; Elvis, M.

doi:10.1093/mnras/stz2333

Cited by 11 publications

(6 citation statements)

References 74 publications

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“…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 one kiloparsec (Das et al 2005(Das et al , 2007Storchi-Bergmann et al 2010;Liu et al 2013bLiu et al , 2014Barbosa et al 2014;Davies et al 2014;Cresci et al 2015;Riffel et al 2013Riffel et al , 2018Fischer et al 2017Fischer et al , 2018Revalski et al 2018;Diniz et al 2019;Muñoz Vergara et al 2019;Soto-Pinto et al 2019). Here, we measured both the extent of the KDR and the size of the NLR.…”

Section: Estimates Of the Nlr And Kdr Extentsmentioning

confidence: 99%

Ionised gas kinematics in MaNGA AGN

Machado

Riffel

Ilha

et al. 2022

A&A

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Context. Feedback from active galactic nuclei (AGNs) in general seems to play an important role in the evolution of galaxies, although the impact of AGN winds on their host galaxies is still unknown in the absence of a detailed analysis. Aims. We aim to analyse the kinematics of a sample of 170 AGN host galaxies as compared to those of a matched control sample of non-active galaxies from the MaNGA survey in order to characterise and estimate the extents of the narrow-line region (NLR) and of the kinematically disturbed region (KDR) by the AGN. Methods. We defined the observed NLR radius (rNLR, o) as the farthest distance from the nucleus within which both [O III]/Hβ and [N II]/Hα ratios fall in the AGN region of the BPT diagram, and the Hα equivalent width was required to be larger than 3.0 Å. The extent of the KDR (rKDR, o) is defined as the distance from the nucleus within which the AGN host galaxies show a more disturbed gas kinematics than the control galaxies. Results. The AGN [O III]λ5007 luminosity ranges from 1039 to 1041 erg s−1, and the kinematics derived from the [O III] line profiles reveal that, on average, the most luminous AGNs (L[O III] > 3.8 × 1040 erg s−1) possess higher residual differences between the gaseous and stellar velocities and velocitie dispersions than their control galaxies in all the radial bins. Spatially resolved NLRs and KDRs were found in 55 and 46 AGN host galaxies, with corrected radii 0.2 < rKDR, c < 2.3 kpc and 0.4 < rNLR, c < 10.1 kpc and a relation between the two given by log rKDR, c = (0.53 ± 0.12) log rNLR, c + (1.07 ± 0.22), respectively. On average, the extension of the KDR corresponds to about 30% of that of the NLR. Assuming that the KDR is due to an AGN outflow, we have estimated ionised gas mass outflow rates that range between 10−5 and ∼1 M⊙ yr−1, and kinetic powers that range from 1034 to 1040 erg s−1. Conclusions. Comparing the power of the AGN ionised outflows with the AGN luminosities, they are always below the 0.05 LAGN model threshold for having an important feedback effect on their respective host galaxies. The mass outflow rates (and power) of our AGN sample correlate with their luminosities, populating the lowest AGN luminosity range of the correlations previously found for more powerful sources.

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Section: Estimates Of the Nlr And Kdr Extentsmentioning

confidence: 99%

Ionised gas kinematics in MaNGA AGN

Machado

Riffel

Ilha

et al. 2022

A&A

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“…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).…”

Section: Introductionmentioning

confidence: 99%

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

Ruschel-Dutra,

Storchi-Bergmann,

Schnorr-Müller

et al. 2021

Preprint

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We analyse optical datacubes of the inner kiloparsec of 30 local (z 0.02) active galactic nuclei (AGN) hosts that our research group, AGNIFS, has collected over the past decade via observations with the integral field units of the Gemini Multi-Object Spectrographs. Spatial resolutions range between 50 pc and 300 pc and spectral coverage is from 4800 Å or 5600 Å to 7000 Å, at velocity resolutions of ≈50 km s −1 . We derive maps of the gas excitation and kinematics, determine the AGN ionisation axis -which has random orientation relative to the galaxy, and the kinematic major axes of the emitting gas. We find that rotation dominates the gas kinematics in most cases, but is disturbed by the presence of inflows and outflows. Outflows have been found in 21 nuclei, usually along the ionisation axis. The gas velocity dispersion is traced by W 80 (velocity width encompassing 80 per cent of the line flux), adopted as a tracer of outflows. In 7 sources W 80 is enhanced perpendicularly to the ionisation axis, indicating lateral expansion of the outflow. We have estimated mass-outflow rates Ṁ and powers Ė, finding median values of log [ Ṁ /( M yr −1 )] = −2.1 +1.6 −1.0 and log [ Ė/( erg s −1 )] = 38.5 +1.8 −0.9 , respectively. Both quantities show a mild correlation with the AGN luminosity (L AGN ). Ė is of the order of 0.01 L AGN for 4 sources, but much lower for the majority (9) of the sources, with a median value of log [ Ė/L AGN ] = −5.34 +3.2 −0.9 indicating that typical outflows in the local Universe are unlikely to significantly impact their host galaxy evolution.

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“…We find that the FWHM of the secondary velocity component in the observed spectra at several locations in both galaxies exceed 500 − 600 km s −1 , a value which is quite high and is typically attributed to ionized gas outflows in numerous studies (Arribas et al 2014;Fischer et al 2017;Humire et al 2018;Couto et al 2017;Soto-Pinto et al 2019). The mock spectra extracted from the disk model for our target galaxies show an average enhancement of the velocity dispersion of about 40 − 50 km s −1 (or FWHM upto 100 km s −1 ) due to beam smearing effect, far below what we observe from data.…”

Section: Discussionmentioning

confidence: 52%

Evidence of wind signatures in the gas velocity profiles of Red Geysers

Roy,

Bundy,

Nevin

et al. 2021

Preprint

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Spatially resolved spectroscopy from SDSS-IV MaNGA survey has revealed a class of quiescent, relatively common early-type galaxies, termed "red geysers", that possibly host large scale active galactic nuclei driven winds. Given their potential importance in maintaining low level of star formation at late times, additional evidence confirming that winds are responsible for the red geyser phenomenon is critical. In this work, we present follow-up observations with the Echellette Spectrograph and Imager (ESI) at the Keck telescope of two red geysers (z<0.1) using multiple long slit positions to sample different regions of each galaxy. Our ESI data with a spectral resolution (R) ∼ 8000 improves upon MaNGA's resolution by a factor of four, allowing us to resolve the ionized gas velocity profiles along the putative wind cone with an instrumental resolution of σ = 16 km s −1 . The line profiles of Hα and [NII]λ6584 show asymmetric shapes that depend systematically on location − extended blue wings on the red-shifted side of the galaxy and red wings on the opposite side. We construct a simple wind model and show that our results are consistent with geometric projections through an outflowing conical wind oriented at an angle towards the line of sight. An alternative hypothesis that assigns the asymmetric pattern to "beam-smearing" of a rotating, ionized gas disk does a poor job matching the line asymmetry profiles. While our study features just two sources, it lends further support to the notion that red geysers are the result of galaxy-scale winds.

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Outflowing gas in a compact ionization cone in the Seyfert 2 galaxy ESO 153-G20

Cited by 11 publications

References 74 publications

Ionised gas kinematics in MaNGA AGN

Ionised gas kinematics in MaNGA AGN

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

Evidence of wind signatures in the gas velocity profiles of Red Geysers

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