We analyzed 17 galaxy clusters, and investigated, for the first time, the dependence of the SFR and sSFR as a function of projected distance (as a proxy for environment) and stellar mass for cluster galaxies in an intermediate-to-high redshift range (0.4 < z < 0.9). We used up to nine flux points (BVRIZYJHKs magnitudes), its errors and redshifts to compute Mstar, SFR and sSFR through spectral energy distribution fitting technique. We use a z-dependent sSFR value to distinguish star-forming (SF) from quiescent galaxies. To analyse the SFR and sSFR history we split our sample in two redshift bins: galaxies at 0.4 < z < 0.6 and 0.6 < z < 0.9. We separate the effects of environment and stellar mass on galaxies by comparing the properties of star- forming and quiescent galaxies at fixed environment (projected radius) and fixed stellar mass. For the selected spectroscopic sample of more than 500 galaxies, the well-known correlation between SFR and Mstar is already in place at z ∼ 0.9, for both SF and quenched galaxies. Our results are consistent with no evidence that SFinte intermediate-to- high redshift range, mass is the primary characteristic that drives SFR.
|Original language||English (US)|
|State||Published - May 30 2018|
- High redshift galaxy clusters
- Specific star formation rate
- Star-formation rate
ASJC Scopus subject areas