A possible binary AGN in Mrk 622?. (28th November 2017)

• Record Type: Journal Article
• Authors: Benítez, E; Rodríguez-Espinosa, J M; Cruz-González, I; González-Martín, O; Negrete, C A; Ruschel-Dutra, D; Gutiérrez, L; Jiménez-Bailón, E
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 474:Number 1(2018:Feb.)
• Page Start: L56
• Page End: L60
• Publication Date: 2017-11-28
• Subjects: galaxies: nuclei -- quasars: emission lines -- quasars: individual: Mrk 622 -- galaxies: Seyfert; Astronomy -- Research -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnrasl/slx188
• Languages: English
• ISSNs: 1745-3933

Abstract

Abstract: Mrk 622 is a Compton thick active galactic nuclei (AGN) and a double-peaked narrow emission line galaxy, thus a dual AGN candidate. In this work, new optical long-slit spectroscopic observations clearly show that this object is rather a triple peaked narrow emission line galaxy, with both blue and red shifted narrow emission lines, as well as a much narrower emission line centred at the host galaxy systemic velocity. The average velocity offset between the blue and red shifted components is ∼500 km s −1, which is producing the apparent double-peaked emission lines. These two components are in the loci of AGN in the Baldwin, Phillips & Terlevich diagrams and are found to be spatially separated by ∼76 pc. Analysis of the optical spatially resolved spectroscopic observations presented in this work favours that Mrk 622 is a system consisting of a composite AGN amidst a binary AGN candidate, likely the result of a recent merger. This notwithstanding, outflows from a starburst, or single AGN could also explain the triple nature of the emission lines.