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The existence of massive galaxies with strongly suppressed star formation atz~2.3, identified in a previous paper, suggests that a red sequence may alreadybe in place beyond z=2. In order to test this hypothesis, we study therest-frame U-B color distribution of massive galaxies at 2<z<3. The sample isdrawn from our near-infrared spectroscopic survey for massive galaxies. Thecolor distribution shows a statistically significant (>3 sigma) red sequence,which hosts ~60% of the stellar mass at the high-mass end. The red-sequencegalaxies have little or no ongoing star formation, as inferred from bothemission-line diagnostics and stellar continuum shapes. Their strong Balmerbreaks and their location in the rest-frame U-B, B-V plane indicate that theyare in a post-starburst phase, with typical ages of ~0.5-1.0 Gyr. In order tostudy the evolution of the red sequence, we compare our sample withspectroscopic massive galaxy samples at 0.02<z<0.045 and 0.6<z<1.0. Therest-frame U-B color reddens by ~0.25 mag from z~2.3 to the present at a givenmass. Over the same redshift interval, the number and stellar mass density onthe high-mass end (>10^11 Msol) of the red sequence grow by factors of ~8 and~6, respectively. We explore simple models to explain the observed evolution.Passive evolution models predict too strong d(U-B), and produce z~0 galaxiesthat are too red. More complicated models that include aging, galaxytransformations, and red mergers can explain both the number density and colorevolution of the massive end of the red sequence between z~2.3 and the present.

The Detection of a Red Sequence of Massive Field Galaxies at z~2.3 and its Evolution to z~0