{ "id": "1805.12175", "version": "v1", "published": "2018-05-30T18:48:49.000Z", "updated": "2018-05-30T18:48:49.000Z", "title": "Star-formation rates of cluster galaxies: nature vs nurture", "authors": [ "Tatiana F. Lagana", "M. P. ulmer" ], "comment": "10 pages, 5 figures", "journal": "2018, MNRAS 475, 523", "doi": "10.1093/mnras/stx3210", "categories": [ "astro-ph.GA" ], "abstract": "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 M$_{\\rm{star}}$, 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 $M_{\\rm star}$ is already in place at $z \\sim 0.9$, for both SF and quenched galaxies. Our results are consistent with no evidence that SFR (or sSFR) depends on environment, suggesting that for cluster galaxies at an intermediate-to-high redshift range, mass is the primary characteristic that drives SFR.", "revisions": [ { "version": "v1", "updated": "2018-05-30T18:48:49.000Z" } ], "analyses": { "keywords": [ "cluster galaxies", "star-formation rates", "stellar mass", "intermediate-to-high redshift range", "quiescent galaxies" ], "tags": [ "journal article" ], "note": { "typesetting": "TeX", "pages": 10, "language": "en", "license": "arXiv", "status": "editable" } } }