The most massive galaxies in clusters are already fully grown at $z\sim 0.5$

Abstract

By constructing scaling relations for galaxies in the massive cluster MACSJ0717.5 at $z=0.545$ and comparing with those of Coma, we model the luminosity evolution of the stellar populations and the structural evolution of the galaxies. We calculate magnitudes, surface brightnesses and effective radii using HST/ACS images and velocity dispersions using Gemini/GMOS spectra, and present a catalogue of our measurements for 17 galaxies. We also generate photometric catalogues for $\sim 3000$ galaxies from the HST imaging. With these, we construct the colour-magnitude relation, the fundamental plane, the mass-to-light versus mass relation, the mass-size relation and the mass-velocity dispersion relation for both clusters. We present a new, coherent way of modelling these scaling relations simultaneously using a simple physical model in order to infer the evolution in luminosity, size and velocity dispersion as a function of redshift, and show that the data can be fully accounted for with this model. We find that (a) the evolution in size and velocity dispersion undergone by these galaxies between $z\sim 0.5$ and $z\sim 0$ is mild, with $R_e(z)\sim (1+z{)}^{-0.40\pm 0.32}$ and $\sigma (z)\sim (1+z{)}^{0.09\pm 0.27}$, and (b) the stellar populations are old, $\sim 10$ Gyr, with a $\sim 3$ Gyr dispersion in age, and are consistent with evolving purely passively since $z\sim 0.5$ with $\Delta \log M/L_B=-0.55_{-0.07}^{+0.15}z$. The implication is that these galaxies formed their stars early and subsequently grew dissipationlessly so as to have their mass already in place by $z\sim 0.5$, and suggests a dominant role for dry mergers, which may have accelerated the growth in these high-density cluster environments.

20 pages; accepted for publication in MNRAS

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Cited by in corpus (5)

• Galaxy structure from multiple tracers: III. Radial variations in M87's IMF
• The SAMI Galaxy Survey: stellar population and structural trends across the Fundamental Plane
• The KMOS Cluster Survey (KCS) III: fundamental plane of cluster galaxies at $z\simeq 1.80$ in JKCS 041
• Galaxy And Mass Assembly (GAMA): Stellar-to-Dynamical Mass Relation I. Constraining the Precision of Stellar Mass Estimates
• The Evolution of Bulge-Dominated Field Galaxies from z~1 to the Present