Volume 614, June 2018
|Number of page(s)||16|
|Published online||20 June 2018|
An outflow in the Seyfert ESO 362-G18 revealed by Gemini-GMOS/IFU observations★
Departamento de Astronomía, Universidad de Concepción,
2 Departamento de Física y Astronomía, Universidad de La Serena, La Serena, Chile
3 Gemini Observatory, Southern Operations centre, La Serena, Chile
4 Dirección de Formacion General, Facultad de Educación y Cs. Sociales, Universidad Andres Bello, Sede Concepción, autopista Concepción-Talcahuano 7100, Talcahuano, Chile
5 SRON, Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
6 Department of Astrophysics/IMAPP, Radboud University, Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands
7 Universidade Federal de Santa Maria, Departamento de Física, Centro de Ciencias Naturais e Exatas, 97105-900 Santa Maria, RS, Brazil
8 Naval Research Laboratory, Washington, DC 20375, USA
9 Institute for Astrophysics and Computational Sciences, Department of Physics, The Catholic University of America, Washington, DC 20064, USA
10 Instituto de Física, CP 15015, Universidade Federal do Rio Grande do Sul, 91501-970, Porto Alegre, RS, Brazil
11 Astrophysics Science Division, Goddard Space Flight centre, Code 665, Greenbelt, MD 20771, USA
12 Department of Physics, Rochester Institute of Technology, 84 Lomb Memorial Drive, Rochester, NY 14623, USA
13 Department of Physics and Astronomy, Georgia State University, Astronomy Offices, 25 Park Place Suite 605, Atlanta, GA 30303, USA
14 Harvard-Smithsonian centre for Astrophysics 60 Garden St., ms.6, Cambridge MA 02138 USA
Accepted: 16 February 2018
We present two-dimensional stellar and gaseous kinematics of the inner 0.7 × 1.2 kpc2 of the Seyfert 1.5 galaxy ESO 362-G18, derived from optical (4092–7338 Å) spectra obtained with the GMOS integral field spectrograph on the Gemini South telescope at a spatial resolution of ≈170 pc and spectral resolution of 36 km s−1. ESO 362-G18 is a strongly perturbed galaxy of morphological type Sa or S0/a, with a minor merger approaching along the NE direction. Previous studies have shown that the [O III] emission shows a fan-shaped extension of ≈10′′ to the SE. We detect the [O III] doublet, [N II] and Hα emission lines throughout our field of view.
The stellar kinematics is dominated by circular motions in the galaxy plane, with a kinematic position angle of ≈137° and is centred approximately on the continuum peak. The gas kinematics is also dominated by rotation, with kinematic position angles ranging from 122° to 139°, projected velocity amplitudes of the order of 100 km s−1, and a mean velocity dispersion of 100 km s−1. A double-Gaussian fit to the [O III]λ5007 and Hα lines, which have the highest signal to noise ratios of the emission lines, reveal two kinematic components: (1) a component at lower radial velocities which we interpret as gas rotating in the galactic disk; and (2) a component with line of sight velocities 100–250 km s−1 higher than the systemic velocity, interpreted as originating in the outflowing gas within the AGN ionization cone. We estimate a mass outflow rate of 7.4 × 10−2 M⊙ yr−1 in the SE ionization cone (this rate doubles if we assume a biconical configuration), and a mass accretion rate on the supermassive black hole (SMBH) of 2.2 × 10−2 M⊙ yr−1. The total ionized gas mass within ~84 pc of the nucleus is 3.3 × 105 M⊙; infall velocities of ~34 km s−1 in this gas would be required to feed both the outflow and SMBH accretion.
Key words: galaxies: active / galaxies: individual: ESO 362-G18 / galaxies: Seyfert / galaxies: nuclei / galaxies: kinematics and dynamics
The reduced datacube (FITS file) is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/614/A94
© ESO 2018
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