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

• Autor(a) principal: Soto-Pinto, Pamela
• Data de Publicação: 2019
• Outros Autores: Nagar, Neil M., Finlez, Carolina, Ramakrishnan, Venkatessh, Munõz-Vergara, Dania, Slater, Roy, Humire, Pedro K., Storchi-Bergmann, Thaisa, Lena, Davide, Kraemer, S. B., Fischer, Travis C., Schmitt, Henrique Roberto, Riffel, Rogemar André, Müller, Allan Schnorr, Robinson, Andrew, Crenshaw, Daniel Michael, Elvis, Martin
• Tipo de documento: Artigo
• Idioma: eng
• Título da fonte: Repositório Institucional da UFRGS
• Texto Completo: http://hdl.handle.net/10183/203749
• topic: Galaxias seyfert; Formacao de estrelas; Galáxias ativas; Galaxies: active; Galaxies: individual : ESO 153-G20; Galaxies: kinematics and dynamics; Galaxies: nuclei; Galaxies: Seyfert

We present two-dimensional ionized gas and stellar kinematics in the inner 1.4 × 1.9 kpc2 of the Seyfert 2 galaxy ESO 153-G20 obtained with the Gemini-South/Gemini multi-object spectrograph integral field unit (GMOS-IFU) at a spatial resolution of ~250 pc and spectral resolution of 36 km s−1. Strong [O iii], Hα, [N ii] and [S ii] emission lines are detected over the entire field of view. The stellar kinematics trace circular rotation with a projected velocity amplitude of ±96 km s−1, a kinematic major axis in position angle of 11°, and an average velocity dispersion of 123 km s−1. To analyse the gas kinematics, we used aperture spectra, position–velocity diagrams and single/double Gaussian fits to the emission lines. All lines show two clear kinematic components: a rotating component that follows the stellar kinematics, and a larger-dispersion component, close to the systemic velocity (from which most of the [O iii] emission comes), mainly detected to the south-west. We interpret this second component as gas outflowing at ~400 km s−1 in a compact (300 pc) ionization cone with a half-opening angle ≤40°. The counter-cone is probably obscured behind a dust lane. We estimate a mass outflow rate of 1.1 M⊙ yr−1, 200 times larger than the estimated accretion rate on to the supermassive black hole, and a kinetic to radiative power ratio of 1.7 × 10−3. Bar-induced perturbations probably explain the remaining disturbances observed in the velocity field of the rotating gas component.