On the evolutionary status of early-type galaxies in clusters at z~0.2 - I. The Fundamental Plane

Details On the evolutionary status of early-type galaxies in clusters at z~0.2 - I. The Fundamental Plane On the evolutionary status of early-type galaxies in clusters at z~0.2 - I. The Fundamental Plane

2005-01-18

arxiv.org/abs/astro-ph/0501379v1

Mon.Not.Roy.Astron.Soc. 358 (2005) 233-255

Astronomy and Astrophysics

Astrophysics

25 pages, 12 figures (including 2 figures in the appendix), accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2005.08779.x

We investigate a spectroscopic sample of 48 early-type (E+S0) galaxies in the rich cluster Abell 2390 (z=0.23) and 48 E+S0 galaxies from a previously published survey of Abell 2218 (z=0.18). The A2390 spectra are based on Multi Object Spectroscopy with MOSCA at the Calar Alto 3.5-m, complemented by ground-based and HST F555W and F814W observations. Our investigation spans a broad range in luminosity (-20.5>M_r>-23.0) and a wide FOV of 1.5x1.5 Mpc^2. Since the A2218 and A2390 samples are very similar, we can combine them and analyse a total of 96 E+S0 galaxies at z~0.2. We construct the Faber-Jackson relation (FJR) for all E+S0s and detect a modest luminosity evolution. The average offset from the local FJR in Gunn r-band is (DeltaM_r)=0.32+-0.22^m. Less-massive galaxies show a trend for a larger evolution than more-massive galaxies. HST/WFPC2 surface brightness profile fits were used to derive structural parameters. For 34 E+S0 galaxies which enter the Fundamental Plane (FP) we deduce a mild evolution in Gunn r with a zero-point offset of 0.10+-0.06, corresponding to 0.31+-0.18^m. Elliptical and lenticular galaxies are uniformly distributed along the FP with a similar scatter of 0.1 dex. We find little evidence for differences between the populations of ellipticals and S0s. Lenticulars induce on average a larger evolution of 0.44+-0.18^m than ellipticals with 0.02+-0.21^m. The M/L ratios at z=0.2 are offset by (Deltalog(M/L_r))=-0.12+-0.06 dex compared to those of Coma. Our results can be reconciled with a passive evolution of the stellar populations and a high formation redshift for the bulk of the stars in E+S0 galaxies. However, our findings are also consistent with the hierarchical formation picture for rich clusters. [abridged]

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