Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 710, Issue 1, Pages L1-L6Publisher
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/710/1/L1
Keywords
galaxies: clusters: general; galaxies: evolution; galaxies: formation
Categories
Funding
- ASI [1/016/07/0]
- STFC [ST/F00298X/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/F00298X/1] Funding Source: researchfish
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Analyzing 24 mu m MIPS/Spitzer data and the [O II]3727 line of a sample of galaxies at 0.4 <= z <= 0.8 from the ESO Distant Cluster Survey, we investigate the ongoing star formation rate (SFR) and the specific star formation rate (SSFR) as a function of stellar mass in galaxy clusters and groups, and compare these with. results from field studies. As for the field, we find a decline in SFR with time, indicating that star formation (SF),vas more active in the past, and a decline in SSFR as galaxy stellar mass increases, showing that the current SF contributes more to the fractional growth of low-mass galaxies than high-mass galaxies. However, we find a lower median SFR (by a factor of similar to 1.5) in cluster star-forming galaxies than in the field. The difference is highly significant when all Spitzer and emission-line galaxies are considered, regardless of color. It remains significant at z > 0.6 after removing red emission-line galaxies, to avoid possible active galactic nucleus contamination. While there is overlap between the cluster and field SFR-mass relations, we find a population of cluster galaxies (10%-25%) wit I reduced SFR for their mass. These are likely to be in transition from star forming to passive. Separately comparing clusters and groups at z > 0.6, only cluster trends are significantly different from the field, and the average cluster SFR at a given mass is similar to two times lower than the field. We conclude that the average SFR in star-forming galaxies varies with galaxy environment at a fixed galaxy mass.
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