Ionized Gas Outflows and Shock-Heated Emission in the Highly Inclined Active Galaxy CGCG 012-070

Lucas Ramos Vieira; Rogemar A. Riffel; Rogério Riffel; Oli L. Dors; Marina Bianchin; Thaisa Storchi-Bergmann

doi:10.1093/mnras/staf1437

paper

Ionized Gas Outflows and Shock-Heated Emission in the Highly Inclined Active Galaxy CGCG 012-070

arXiv:2508.20286 · doi:10.1093/mnras/staf1437

Abstract

Active Galactic Nuclei (AGNs) exhibit excess mid-infrared H $_{2}$ emission compared to star-forming galaxies, likely driven by outflows and shocks inferred from integrated spectra. We present optical IFU observations of the central 2\,kpc of the AGN host CGCG 012-070, selected for its pronounced H $_{2}$ emission excess, to map stellar and gas kinematics. The stellar velocity field is well described by a rotating disc with a line of nodes at $10 3^{\circ} \pm 4^{\circ}$ , with the northwest side approaching and the southeast side receding. Gas kinematics, traced by strong emission lines, show two components: a narrow one ( $σ ≲ 200 km s^{- 1}$ ) in the disc plane following stellar motions, and a broad ( $σ ≳ 300 km s^{- 1}$ ) associated with outflows within the inner $\sim$ 1\,kpc. Disc gas emission is mainly driven by AGN photoionization, while the outflow also includes shock-heated gas, as indicated by flux ratio diagnostics. The outflows are radiatively driven, with a mass-outflow rate of $(0.067 \pm 0.026) M_{⊙} y r^{- 1}$ and a kinetic coupling efficiency of 0.07%, potentially redistributing gas and contributing to maintenance-mode feedback in CGCG 012-070. Our results provide further evidence that the warm H $_{2}$ emission excess in nearby AGN is associated with shocks produced by outflows. Observations of other gas phases, such as cold molecular gas, are necessary to gain a more comprehensive understanding of the impact of the outflows on the host galaxy.

Ionized Gas Outflows and Shock-Heated Emission in the Highly Inclined Active Galaxy CGCG 012-070

Abstract

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