The properties and evolution of a K-band selected sample of massive galaxies at z∼ 0.4-2 in the Palomar/DEEP2 survey

We present the results of a study on the properties and evolution of massive (M * > 10 11 M ) galaxies at z 0.4-2 utilizing Keck spectroscopy, near-infrared Palomar imaging, and Hubble, Chandra and Spitzer data covering fields targeted by the DEEP2 galaxy spectroscopic survey. Our sample is K-band selected and stellar mass limited, based on wide-area near-infrared imaging from the Palomar Observatory Wide-Field Infrared Survey, which covers 1.53 deg 2 to a 5 depth of K s,vega 20.5. Our primary goal is to obtain a broad census of massive galaxies through measuring how their number and mass densities, morphology, as well as their star formation and active galactic nucleus content evolve from z 0.4-2. Our major findings include: (i) statistically the mass and number densities of M * > 10 11 M galaxies show little evolution between z = 0 and 1 and from z 0 to 2 for M * > 10 11.5 M galaxies. We however find significant evolution within 1 10 11 M selected galaxies show a nearly constant elliptical fraction of 70-90 per cent at all redshifts. The remaining objects tend to be peculiars possibly undergoing mergers at z > 0.8, while spirals dominate the remainder at lower redshifts. A significant fraction (25 per cent) of these early-types contain minor structural anomalies. (iii) We find that only a fraction (60 per cent) of massive galaxies with M * > 10 11 M are on the red sequence at z 1.4, while nearly 100 per cent evolve on to it by z 0.4. (iv) By utilizing Spitzer MIPS imaging and O II line fluxes we argue that M * > 10 11.5 M galaxies have a steeply declining star formation rate (SFR) density (1 + z) 6 . By examining the contribution of star formation to the evolution of the mass function, as well as the merger history through the CAS parameters, we determine that M * > 10 11 M galaxies undergo on average 0.9 +0.7 -0.5 major mergers at 0.4 10 11 M galaxies are X-ray emitters. Roughly half of these are morphologically distorted ellipticals or peculiars. Finally, we compare our mass growth with semi-analytical models from the Millennium Simulation,