Filaments in VIPERS: galaxy quenching in the infalling regions of groups. (arXiv:1902.04624v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Salerno_J/0/1/0/all/0/1">Juan Manuel Salerno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martinez_H/0/1/0/all/0/1">Héctor J. Martínez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muriel_H/0/1/0/all/0/1">Hernán Muriel</a>
We study the quenching of galaxies in different environments and its
evolution in the redshift range $0.43 leq z leq 0.89$. For this purpose, we
identify galaxies inhabiting filaments, the isotropic infall region of groups,
the field, and groups in the VIMOS Public Extragalactic Redshift Survey
(VIPERS). We classify galaxies as quenched (passive), through their $NUV-r$
versus $r-K$ colours. We study the fraction of quenched galaxies ($F_{r}$) as a
function of stellar mass and environment at two redshift intervals. Our results
confirm that stellar mass is the dominant factor determining galaxy quenching
over the full redshift range explored. We find compelling evidence of evolution
in the quenching of intermediate mass galaxies $(9.3 leq log(M_{*}/M_{odot})
leq 10.5)$ for all environments. For this mass range, $F_{r}$ is largest for
galaxies in groups and smallest for galaxies in the field, while galaxies in
filaments and in the isotropic infall regions appear to have intermediate
values with the exception of the high redshift bin, where the latter show
similar fraction of quenched galaxies as in the field. Galaxies in filaments
are systematically more quenched than their counterparts infalling from other
directions, in agreement to similar results found at low redshift. The least
massive galaxies in our samples do not show evidence of internal or
environmental quenching.
We study the quenching of galaxies in different environments and its
evolution in the redshift range $0.43 leq z leq 0.89$. For this purpose, we
identify galaxies inhabiting filaments, the isotropic infall region of groups,
the field, and groups in the VIMOS Public Extragalactic Redshift Survey
(VIPERS). We classify galaxies as quenched (passive), through their $NUV-r$
versus $r-K$ colours. We study the fraction of quenched galaxies ($F_{r}$) as a
function of stellar mass and environment at two redshift intervals. Our results
confirm that stellar mass is the dominant factor determining galaxy quenching
over the full redshift range explored. We find compelling evidence of evolution
in the quenching of intermediate mass galaxies $(9.3 leq log(M_{*}/M_{odot})
leq 10.5)$ for all environments. For this mass range, $F_{r}$ is largest for
galaxies in groups and smallest for galaxies in the field, while galaxies in
filaments and in the isotropic infall regions appear to have intermediate
values with the exception of the high redshift bin, where the latter show
similar fraction of quenched galaxies as in the field. Galaxies in filaments
are systematically more quenched than their counterparts infalling from other
directions, in agreement to similar results found at low redshift. The least
massive galaxies in our samples do not show evidence of internal or
environmental quenching.
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