Luminosity Evolution of Field Early-Type Galaxies to [CLC][ITAL]z[/ITAL][/CLC] = 0.55

Abstract

We study the Fundamental Plane of field early-type galaxies at intermediate redshift, using HST WFPC2 observations and deep Keck spectroscopy. Structural parameters and internal velocity dispersions are measured for eighteen galaxies at 0.15 < z < 0.55. Rest frame M/L_B ratios are determined from the Fundamental Plane and compared to those of cluster early-type galaxies at the same redshifts. The systematic offset between M/L ratios of field and cluster early-type galaxies at intermediate redshift is small, and not significant: (field) - (cluster) = -0.18 +- 0.11. The M/L ratios of field early-type galaxies evolve as \Delta (ln M/L_B) = (-1.35 +- 0.35) z, very similar to cluster early-type galaxies. After correcting for luminosity evolution, the FP of field early-type galaxies has a scatter 0.09 +- 0.02 in log r_e, similar to that in local clusters. The scatter appears to be driven by low mass S0 galaxies; for the elliptical galaxies alone we find 0.03 +- 0.03. There is a hint that the FP has a different slope than in clusters, but more data are needed to confirm this. The similarity of the M/L ratios of cluster and field early-type galaxies provides a constraint on the relative ages of their stars. At = 0.43, field early-type galaxies are younger than cluster early-type galaxies by only 21 +- 13 %, and we infer that the stars in field early-type galaxies probably formed at z >~ 1.5. Recent semi-analytical models for galaxy formation in a Lambda-CDM Universe predict a systematic difference between field and cluster galaxies of \Delta (ln M/L_B) ~ -0.6, much larger than the observed difference. This result is consistent with the hypothesis that field early-type galaxies formed earlier than predicted by these models.