SDSS-IV MaNGA: Inside-out versus Outside-in Quenching of Galaxies in Different Local Environments
| Autor: | Sebastián F. Sánchez, Bau-Ching Hsieh, Sandro Barboza Rembold, Yu Rong, Fang-Ting Yuan, Francesco Belfiore, Kate Rowlands, R. A. Riffel, Maria Argudo-Fernández, Niv Drory, Roberto Maiolino, Eric M. Wilcots, Ivan Lacerna, Dmitry Bizyaev, Lihwai Lin, Hsi-An Pan |
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| Přispěvatelé: | Lin, L [0000-0001-7218-7407], Hsieh, BC [0000-0001-5615-4904], Pan, HA [0000-0002-1370-6964], Bizyaev, D [0000-0002-3601-133X], Lacerna, I [0000-0002-7802-7356], Rong, Y [0000-0002-2204-6558], Drory, N [0000-0002-7339-3170], Apollo - University of Cambridge Repository |
| Rok vydání: | 2020 |
| Předmět: |
Physics
Quenching (fluorescence) biology High Energy Physics::Lattice Astronomy and Astrophysics general [Galaxies] Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics biology.organism_classification evolution [Galaxies] star formation [Galaxies] galaxies: general Galaxy Galaxias Space and Planetary Science galaxies: star formation Evolucao galatica Halo Halos Galáxias galaxies: evolution Astrophysics::Galaxy Astrophysics |
| Zdroj: | Repositório Institucional da UFRGS Universidade Federal do Rio Grande do Sul (UFRGS) instacron:UFRGS |
| DOI: | 10.17863/cam.51823 |
| Popis: | The large Integral Field Spectroscopy surveys have allowed the classification of ionizing sources of emission lines on sub-kiloparsec scales. In this work, we define two non-parametric parameters, quiescence (F q ) and its concentration (C q ), to quantify the strength and the spatial distribution of the quenched areas, respectively, traced by the LI(N)ER regions with low EW(Hα). With these two measurements, we classify MaNGA galaxies into inside-out and outside-in quenching types according to their locations on the F q versus C q plane and we measure the fraction of inside-out (outside-in) quenching galaxies as a function of halo mass. We find that the fraction of galaxies showing inside-out quenching increases with halo mass, irrespective of stellar mass or galaxy type (satellites versus centrals). In addition, high-stellar-mass galaxies exhibit a greater fraction of inside-out quenching compared to low-stellar-mass ones in all environments. In contrast, the fraction of outside-in quenching does not depend on halo mass. Our results suggest that morphological quenching may be responsible for the inside-out quenching seen in all environments. On the other hand, the flat dependence of the outside-in quenching on halo mass could be a mixed result of ram pressure stripping and galaxy mergers. Nevertheless, for a given environment and stellar mass, the fraction of inside-out quenching is systematically greater than that of outside-in quenching, suggesting that inside-out quenching is the dominant quenching mode in all environments. |
| Databáze: | OpenAIRE |
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