Galaxy and Mass Assembly (GAMA) : Impact of the Group Environment on Galaxy Star Formation
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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 ≤ (M 200/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.
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 2018 , ' Galaxy and Mass Assembly (GAMA) : Impact of the Group Environment on Galaxy Star Formation ' , Astrophysical Journal , vol. 857 , no. 1 , 71 . https://doi.org/10.3847/1538-4357/aab61a
© 2018. The American Astronomical Society. All rights reserved. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.3847/1538-4357/aab61a
DescriptionMSO acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140100255). SB acknowledges funding support from the Australian Research Council through a Future Fellowship (FT140101166).
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