1. Outflowing gas in a compact ionization cone in the Seyfert 2 galaxy ESO 153-G20.
- Author
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Soto-Pinto, Pamela, Nagar, Neil M, Finlez, Carolina, Ramakrishnan, Venkatessh, Muñoz-Vergara, Dania, Slater, Roy, Humire, Pedro K, Storchi-Bergmann, Thaisa, Lena, Davide, Kraemer, Steven B, Fischer, Travis C, Schmitt, Henrique R, Riffel, Rogemar A, Schnorr-Müller, Allan, Robinson, Andrew, Crenshaw, D Michael, and Elvis, Martin S
- Subjects
SEYFERT galaxies ,ELECTRON impact ionization ,SUPERMASSIVE black holes ,IONIZED gases ,KINEMATICS ,CONES ,GAS fields - Abstract
We present two-dimensional ionized gas and stellar kinematics in the inner 1.4 × 1.9 kpc
2 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|$\odot$| 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. [ABSTRACT FROM AUTHOR]- Published
- 2019
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