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

• Autor(a) principal: Nascimento, Janaina Correa do
• Data de Publicação: 2019
• Outros Autores: Storchi-Bergmann, Thaisa, Mallmann, Nícolas Dullius, Riffel, Rogério, Ilha, Gabriele da Silva, Riffel, Rogemar André, Rembold, Sandro Barboza, Schimoia, Jáderson da Silva, Costa, Luiz N. da, Maia, Marcio Antonio Geimba, Machado, Alice Deconto
• Tipo de documento: Artigo
• Idioma: eng
• Título da fonte: Repositório Institucional da UFRGS
• Texto Completo: http://hdl.handle.net/10183/198543
• topic: Formacao de estrelas; Nucleo galatico; Gas ionizado; Galáxias ativas; galaxies: active

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([OIII]λ5007)≥3.8×1040ergs−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 0.2Re. The extent R of the region ionized by the AGN follows the relation R∝L([OIII])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 0.2Re than the control galaxies