How do central and satellite galaxies quench? – Insights from spatially resolved spectroscopy in the MaNGA survey
| Autor: | Sara L. Ellison, Asa F. L. Bluck, Roberto Maiolino, Hossen Teimoorinia, Christopher J. Conselice, James Trussler, Joanna M Piotrowska, Sebastián F. Sánchez, Mallory D. Thorp, Jorge Moreno |
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| Přispěvatelé: | Bluck, Asa [0000-0001-6395-4504], Maiolino, Roberto [0000-0002-4985-3819], Piotrowska-Karpov, Joanna [0000-0003-1661-2338], Apollo - University of Cambridge Repository |
| Rok vydání: | 2020 |
| Předmět: |
Cosmology and Nongalactic Astrophysics (astro-ph.CO)
Galaxy: disc FOS: Physical sciences Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics 01 natural sciences Galaxy: bulge Luminosity Bulge 0103 physical sciences Satellite galaxy galaxies: formation 010303 astronomy & astrophysics galaxies: statistics Astrophysics::Galaxy Astrophysics Physics 010308 nuclear & particles physics Star formation Sigma Velocity dispersion Astronomy and Astrophysics Astrophysics - Astrophysics of Galaxies Galaxy 13. Climate action Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) galaxies: star formation galaxies: evolution Low Mass Astrophysics - Cosmology and Nongalactic Astrophysics |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 499:230-268 |
| ISSN: | 1365-2966 0035-8711 |
| DOI: | 10.1093/mnras/staa2806 |
| Popis: | 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 ($\Sigma_{\rm SFR}$), derived in Bluck et al. (2020), to compute the distance at which each spaxel resides from the resolved star forming main sequence ($\Sigma_{\rm SFR} - \Sigma_*$ relation): $\Delta \Sigma_{\rm SFR}$. We study galaxy radial profiles in $\Delta \Sigma_{\rm SFR}$, and luminosity weighted stellar age (${\rm Age_L}$), 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 ($\sigma_c$) 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 ($\delta_5$) being the most important single parameter. Utilising the empirical $M_{BH}$ - $\sigma_c$ relation, we estimate that quenching via AGN feedback must occur at $M_{BH} \geq 10^{6.5-7.5} M_{\odot}$, and is marked by steeply rising $\Delta \Sigma_{\rm SFR}$ 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 $\Delta \Sigma_{\rm SFR}$ 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. Comment: Accepted for publication in MNRAS. 40 pages; 24 figures |
| Databáze: | OpenAIRE |
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