Galaxy and Mass Assembly (GAMA): Impact of the Group Environment on Galaxy Star Formation

We explore how the group environment may affect the evolution of star-forming galaxies. We select 1197 Galaxy And Mass Assembly groups at 0.05 ≤ z ≤ 0.2 and analyze the projected phase space (PPS) diagram, i.e., the galaxy velocity as a function of projected group-centric radius, as a local environm...

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Bibliographic Details
Published in:The Astrophysical journal 2018-04, Vol.857 (1), p.71
Main Authors: Barsanti, S., Owers, M. S., Brough, S., Davies, L. J. M., Driver, S. P., Gunawardhana, M. L. P., Holwerda, B. W., Liske, J., Loveday, J., Pimbblet, K. A., Robotham, A. S. G., Taylor, E. N.
Format: Article
Language:English
Subjects:
Assembly
Astrophysics
Environmental impact
Galactic clusters
Galactic evolution
Galactic halos
Galaxies
galaxies: evolution
galaxies: groups: general
galaxies: kinematics and dynamics
galaxies: star formation
Halos
Star & galaxy formation
Star clusters
Star formation
Star formation rate
Stars & galaxies
Stellar evolution
Stellar mass
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Summary:We explore how the group environment may affect the evolution of star-forming galaxies. We select 1197 Galaxy And Mass Assembly groups at 0.05 ≤ z ≤ 0.2 and analyze the projected phase space (PPS) diagram, i.e., the galaxy velocity as a function of projected group-centric radius, as a local environmental metric in the low-mass halo regime 1012 ≤ (M200/M ) < 1014. We study the properties of star-forming group galaxies, exploring the correlation of star formation rate (SFR) with radial distance and stellar mass. We find that the fraction of star-forming group members is higher in the PPS regions dominated by recently accreted galaxies, whereas passive galaxies dominate the virialized regions. We observe a small decline in specific SFR of star-forming galaxies toward the group center by a factor ∼1.2 with respect to field galaxies. Similar to cluster studies, we conclude for low-mass halos that star-forming group galaxies represent an infalling population from the field to the halo and show suppressed star formation.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/aab61a