A Substantial Population of Red Galaxies at z > 2: Modeling of the Spectral Energy Distributions of an Extended Sample

We investigate the nature of the substantial population of high-redshift galaxies with J sub(s) - K sub(s) . 2.3 colors recently discovered as part of our Faint Infrared Extragalactic Survey (FIRES). This color cut efficiently isolates galaxies at z > 2 with red rest-frame optical colors ("distant red galaxies" [DRGs]). We select J sub(s) - K sub(s) . 2.3 objects in both FIRES fields, the -2'.5 x 2'.5 Hubble Deep Field-South (HDF-S) and the -5' x 5' field around the MS 1054-03 cluster at z = 0.83; the surface densities at K sub(s,Vega) < 21 mag are 1.6 c 0.6 and 1.0 c 0.2 arcmin super(-2), respectively. We here discuss a subsample of 34 DRGs at 2 , z , 3.5: 11 at K sub(s,Vega) < 22.5 mag in HDF-S and 23 at K sub(s,Vega) < 21.7 mag in the MS 1054-03 field. This sample enables for the first time a robust assessment of the population properties of DRGs. We analyze the l = 0.3-2.2 km spectral energy distributions (SEDs) constructed from our very deep near-infrared (NIR) and optical imaging collected at the ESO Very Large Telescope and from the Hubble Space Telescope. We develop diagnostics involving the I sub(814) - J sub(s), J sub(s) - H, and H - K sub(s) colors to argue that the red NIR colors of our DRG sample cannot be attributed solely to interstellar dust extinction and require for many the presence of an evolved stellar population with a prominent Balmer/4000 AA break. In the rest frame, the optical colors of DRGs fall within the envelope of normal nearby galaxies and the ultraviolet colors suggest a wide range in star formation activity and/or extinction. This is in stark contrast with the much bluer and more uniform SEDs of Lyman break galaxies (LBGs). From evolutionary synthesis modeling assuming constant star formation (CSF), we derive for the DRGs old ages, large extinctions, and high stellar masses, mass-to-light ratios, and star formation rates (SFRs). For solar metallicity, a Salpeter initial mass function (IMF) between 0.1 and 100 M sub( ), and the Calzetti et al. extinction law, the median values for the HDF-S (MS 1054-03 field) sample are 1.7 (2.0) Gyr, A sub(V) = 2.7 (2.4) mag, M* = 0.8 (1.6) x 10 super(11) M sub( ), M*/L sub(V),* = 1.2 (2.3) M sub( )LV super(-1), , and SFR = 120 (170) M sub( )yr super(-1). Models assuming exponentially declining SFRs with e-folding timescales in the range from 10 Myr to 1 Gyr generally imply younger ages, lower extinction, and lower SFRs, but similar stellar masses within a factor of 2. Compared to LBGs at