SDSS-IV MaNGA: Inside-out vs. outside-in quenching in different local environments. (arXiv:1901.05126v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lin_L/0/1/0/all/0/1">Lihwai Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hsieh_B/0/1/0/all/0/1">Bau-Ching Hsieh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pan_H/0/1/0/all/0/1">Hsi-An Pan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rembold_S/0/1/0/all/0/1">Sandro B. Rembold</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_S/0/1/0/all/0/1">Sebastián F. Sánchez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Argudo_Fernandez_M/0/1/0/all/0/1">Maria Argudo-Fernández</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rowlands_K/0/1/0/all/0/1">Kate Rowlands</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belfiore_F/0/1/0/all/0/1">Francesco Belfiore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bizyaev_D/0/1/0/all/0/1">Dmitry Bizyaev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lacerna_I/0/1/0/all/0/1">Ivan Lacerna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riffel_R/0/1/0/all/0/1">Rogréio Riffel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rong_Y/0/1/0/all/0/1">Yu Rong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yuan_F/0/1/0/all/0/1">Fangting Yuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drory_N/0/1/0/all/0/1">Niv Drory</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maiolino_R/0/1/0/all/0/1">Roberto Maiolino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilcots_E/0/1/0/all/0/1">Eric Wilcots</a>
The large Integral Field Spectroscopy (IFS) surveys have allowed the
classification of ionizing sources of emission lines on sub-kpc 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(H$alpha$). With these two measurements, we classify MaNGA galaxies into
inside-out and outside-in quenching types according to their locations on the
f$_{q}$ vs. 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 vs. 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, at 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.
The large Integral Field Spectroscopy (IFS) surveys have allowed the
classification of ionizing sources of emission lines on sub-kpc 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(H$alpha$). With these two measurements, we classify MaNGA galaxies into
inside-out and outside-in quenching types according to their locations on the
f$_{q}$ vs. 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 vs. 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, at 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.
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