al. 2003; Baldry et al. 2004), Kauffmann et al. (2004) bins galaxies by mass and finds that star formation history (SFH) depends on the local density at any galaxy stellar mass.

The first evidence that the galaxy population in clusters may evolve with redshift was found by Butcher & Oemler (1978), who observed that galaxies in clusters beyond $z$$\sim$0.4 tend to be bluer than galaxies in nearby clusters. However, the Butcher & Oemler observations did not compare the cluster to the field populations at high redshift, while later observations showed that galaxies in all environments had higher SFRs in the past (Lilly et al. 1996; Madau et al. 1996; Wilson et al. 2002). Using large surveys able to probe a range of environments at high redshifts, recent observations have found that the SFR-density and color-density relations may be reversed at $z$$\sim$1 compared to those at $z$$\sim$0 (e.g. Cucciati et al. 2006; Elbaz et al. 2007; Cooper et al. 2008; Ideue et al. 2009; Salimbeni et al. 2009; Tran et al. 2010; Gr[ü]{}tzbauch et al. 2011; Popesso et al. 2011).

For example, Elbaz et al. (2007; E07) compare local star-forming SDSS galaxies to star-forming galaxies in the GOODS-S and GOODS-N fields 