The AGNIFS survey: distribution and excitation of the hot molecular and ionized gas in the inner kpc of nearby AGN hosts. Issue 3 (10th April 2021)

• Record Type: Journal Article
• Authors: Riffel, R A; Storchi-Bergmann, T; Riffel, R; Bianchin, M; Zakamska, N L; Ruschel-Dutra, D; Schönell, A J; Rosario, D J; Rodriguez-Ardila, A; Fischer, T C; Davies, R I; Dametto, N Z; Dahmer-Hahn, L G; Crenshaw, D M; Burtscher, L; Bentz, M C
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 504:Issue 3(2021)
• Page Start: 3265
• Page End: 3283
• Publication Date: 2021-04-10
• Subjects: techniques: imaging spectroscopy -- galaxies: active -- galaxies: ISM -- galaxies: Seyfert; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stab998
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We use the Gemini NIFS instrument to map the H$_2\, 2.1218\, \mu$ m and Brγ flux distributions in the inner 0.04–2 kpc of a sample of 36 nearby active galaxies (0.001 ≲ z ≲ 0.056) at spatial resolutions from 4 to 250 pc. We find extended emission in 34 galaxies. In ∼55 per cent of them, the emission in both lines is most extended along the galaxy major axis, while in the other 45 per cent the extent follows a distinct orientation. The emission of H2 is less concentrated than that of Brγ, presenting a radius that contains half of the flux 60 per cent greater, on average. The H2 emission is driven by thermal processes – X-ray heating and shocks – at most locations for all galaxies, where $0.4\lt \rm H_2/Br\gamma \lt 6$ . For regions where H2 /Brγ > 6 (seen in 40 per cent of the galaxies), shocks are the main H2 excitation mechanism, while in regions with H2 /Brγ < 0.4 (25 per cent of the sample) the H2 emission is produced by fluorescence. The only difference we found between type 1 and type 2 active galactic nucleus (AGN) was in the nuclear emission-line equivalent widths that are smaller in type 1 than in type 2 due to a larger contribution to the continuum from the hot dusty torus in the former. The gas masses in the inner 125 pc radius are in the range 10 1 −10 4 M⊙ for the hot H2 and 10 3 −10 6 M⊙ for the ionized gas and would be enough to power the AGN in our sample for 10 5 −10 8 yr at their current accretion rates.