An outflow in the Seyfert ESO 362-G18 revealed by Gemini-GMOS/IFU observations

Pedro K. Humire, Neil M. Nagar, Carolina Finlez, Verónica Firpo, Roy Slater, Davide Lena, Pamela Soto-Pinto, Dania Muñoz-Vergara, Rogemar A. Riffel, Henrique R. Schmitt, Steven B. Kraemer, Allan Schnorr-Müller, Travis C. Fischer, Andrew Robinson, Thaisa Storchi-Bergmann, Mike Crenshaw, Martin S. Elvis

Resultado de la investigación: Contribución a una revistaArtículorevisión exhaustiva

10 Citas (Scopus)

Resumen

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.

Idioma originalInglés
Número de artículoA94
PublicaciónAstronomy and Astrophysics
Volumen614
DOI
EstadoPublicada - 1 jun 2018
Publicado de forma externa

Áreas temáticas de ASJC Scopus

  • Astronomía y astrofísica
  • Ciencias planetarias y espacial

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