How do central and satellite galaxies quench? -- Insights from spatially resolved spectroscopy in the MaNGA survey

Asa F. L. Bluck; Roberto Maiolino; Joanna M. Piotrowska; James Trussler; Sara L. Ellison; Sebastian F. Sanchez; Mallory D. Thorp; Hossen Teimoorinia; Jorge Moreno; Christopher J. Conselice

doi:10.1093/mnras/staa2806

paper

How do central and satellite galaxies quench? -- Insights from spatially resolved spectroscopy in the MaNGA survey

arXiv:2009.05341 · doi:10.1093/mnras/staa2806

Abstract

We investigate how star formation quenching proceeds within central and satellite galaxies using spatially resolved spectroscopy from the SDSS-IV MaNGA DR15. We adopt a complete sample of star formation rate surface densities ( $Σ_{SFR}$ ), derived in Bluck et al. (2020), to compute the distance at which each spaxel resides from the resolved star forming main sequence ( $Σ_{SFR} - Σ_{*}$ relation): $Δ Σ_{SFR}$ . We study galaxy radial profiles in $Δ Σ_{SFR}$ , and luminosity weighted stellar age ( $Ag e_{L}$ ), split by a variety of intrinsic and environmental parameters. Via several statistical analyses, we establish that the quenching of central galaxies is governed by intrinsic parameters, with central velocity dispersion ( $σ_{c}$ ) being the most important single parameter. High mass satellites quench in a very similar manner to centrals. Conversely, low mass satellite quenching is governed primarily by environmental parameters, with local galaxy over-density ( $δ_{5}$ ) being the most important single parameter. Utilising the empirical $M_{B H}$ - $σ_{c}$ relation, we estimate that quenching via AGN feedback must occur at $M_{B H} \geq 1 0^{6.5 - 7.5} M_{⊙}$ , and is marked by steeply rising $Δ Σ_{SFR}$ radial profiles in the green valley, indicating `inside-out' quenching. On the other hand, environmental quenching occurs at over-densities of 10 - 30 times the average galaxy density at z $\sim$ 0.1, and is marked by steeply declining $Δ Σ_{SFR}$ profiles, indicating `outside-in' quenching. Finally, through an analysis of stellar metallicities, we conclude that both intrinsic and environmental quenching must incorporate significant starvation of gas supply.

arXiv commentAccepted for publication in MNRAS. 40 pages; 24 figures

How do central and satellite galaxies quench? -- Insights from spatially resolved spectroscopy in the MaNGA survey

Abstract

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