Galaxy Groups at 0.3 <= z <= 0.55. II. Evolution to z ~ 0

Details Galaxy Groups at 0.3 <= z <= 0.55. II. Evolution to z ~ 0 Galaxy Groups at 0.3 <= z <= 0.55. II. Evolution to z ~ 0

2005-01-11

arxiv.org/abs/astro-ph/0501183v1

Mon.Not.Roy.Astron.Soc. 358 (2005) 88-100

Astronomy and Astrophysics

Astrophysics

15 pages, 14 figures, accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2005.08745.x

We compare deep Magellan spectroscopy of 26 groups at 0.3 <= z <= 0.55, selected from the Canadian Network for Observational Cosmology 2 field survey (CNOC2), with a large sample of nearby groups from the 2PIGG catalogue (Eke et al., 2004). We find that the fraction of group galaxies with significant [OII] emission (>=5\AA) increases strongly with redshift, from ~29% in 2dFGRS to ~58% in CNOC2, for all galaxies brighter than ~ M*+1.75. This trend is parallel to the evolution of field galaxies, where the equivalent fraction of emission line galaxies increases from ~ 53% to ~ 75%. The fraction of emission-line galaxies in groups is lower than in the field, across the full redshift range, indicating that the history of star formation in groups is influenced by their environment. We show that the evolution required to explain the data is inconsistent with a quiescent model of galaxy evolution; instead, discrete events in which galaxies cease forming stars (truncation events) are required. We constrain the probability of truncation (P_trunc) and find that a high value is required in a simple evolutionary scenario neglecting galaxy mergers (P_trunc >~ 0.3 Gyr^{-1}). However, without assuming significant density evolution, P_trunc is not required to be larger in groups than in the field, suggesting that the environmental dependence of star formation was embedded at redshifts z >~ 0.45.

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