TY - JOUR
T1 - SDSS-IV MaNGA
T2 - Inside-out versus Outside-in Quenching of Galaxies in Different Local Environments
AU - Lin, Lihwai
AU - Hsieh, Bau Ching
AU - Pan, Hsi An
AU - Rembold, Sandro B.
AU - Sánchez, Sebastián F.
AU - Argudo-Fernández, Maria
AU - Rowlands, Kate
AU - Belfiore, Francesco
AU - Bizyaev, Dmitry
AU - Lacerna, Ivan
AU - Riffel, Rogréio
AU - Rong, Yu
AU - Yuan, Fangting
AU - Drory, Niv
AU - Maiolino, Roberto
AU - Wilcots, Eric
N1 - Publisher Copyright:
© 2019. The American Astronomical Society. All rights reserved.
PY - 2019/2/10
Y1 - 2019/2/10
N2 - 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.
AB - 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.
KW - galaxies: evolution
KW - galaxies: general
KW - galaxies: star formation
UR - http://www.scopus.com/inward/record.url?scp=85062019498&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/aafa84
DO - 10.3847/1538-4357/aafa84
M3 - Article
AN - SCOPUS:85062019498
SN - 0004-637X
VL - 872
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - A50
ER -