The first 62 AGN observed with SDSS-IV MaNGA – IV. Gas excitation and star formation rate distributions

Journal Article · Wed Apr 17 00:00:00 EDT 2019 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stz1083· OSTI ID:1512827

Nascimento, Janaína C. do ^[1]; Storchi-Bergmann, Thaisa ^[1]; Mallmann, Nícolas D.  ^[1]; Riffel, Rogério  ^[1]; Ilha, Gabriele S.  ^[2]; Riffel, Rogemar A.  ^[2]; Rembold, Sandro B. ^[2]; Schimoia, Jáderson ^[3]; da Costa, Luiz Nicolaci ^[4]; Maia, Marcio A. G. ^[4]; Machado, Alice D. ^[2]

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1. Departamento de Astronomia, IF, Universidade Federal do Rio Grande do Sul, CP 15051, 91501-970 Porto Alegre, RS, Brazil, Laboratório Interinstitucional de e-Astronomia - LIneA, Rua General José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil
2. Laboratório Interinstitucional de e-Astronomia - LIneA, Rua General José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil, Departamento de Física, CCNE, Universidade Federal de Santa Maria, 97105-900 Santa Maria, RS, Brazil
3. Laboratório Interinstitucional de e-Astronomia - LIneA, Rua General José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil, Departamento de Física, Universidade Federal de Santa Catarina, CP 88040-900, Florianópolis, SC, Brazil
4. Laboratório Interinstitucional de e-Astronomia - LIneA, Rua General José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil, Observatório Nacional, Rua General José Cristino, 77, Rio de Janeiro, RJ 20921-400, Brazil

Abstract We present maps of the ionized gas flux distributions, excitation, star formation rate (SFR), surface mass density ΣH+, and obtain total values of SFR and ionized gas masses M for 62 active galactic nuclei (AGN) observed with SDSS-IV MaNGA and compare them with those of a control sample of 112 non-active galaxies. The most luminous AGN – with $$L(\rm {[O\,{\small III}]}\lambda 5007) \ge 3.8\times 10^{40}\, \mbox{erg}\, \mbox{s}^{-1}$$, and those hosted by earlier type galaxies are dominated by Seyfert excitation within 0.2 effective radius Re from the nucleus, surrounded by LINER excitation or transition regions, while the less luminous and hosted by later-type galaxies show equally frequent LINER and Seyfert excitation within $$0.2\, R_\mathrm{ e}$$. The extent R of the region ionized by the AGN follows the relation $$R\propto \, L(\rm {[O\,{\small III}]})^{0.5}$$ – as in the case of the broad-line region. The SFR distribution over the region ionized by hot stars is similar for AGN and controls, while the integrated SFR – in the range 10−3–10 M⊙ yr−1 is also similar for the late-type subsample, but higher in the AGN for 75 per cent of the early-type subsample. We thus conclude that there is no signature of AGN quenching star formation in the body of the galaxy in our sample. We also find that 66 per cent of the AGN have higher ionized gas masses M than the controls – in the range 105–3 × 107 M⊙ – while 75 per cent of the AGN have higher ΣH+ within $$0.2\, R_\mathrm{ e}$$ than the control galaxies.

• Sponsoring Organization: USDOE
• OSTI ID: 1512827
• Journal Information: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Vol. 486 Journal Issue: 4; ISSN 0035-8711
• Publisher: Oxford University Press
• Country of Publication: United Kingdom
• Language: English