GALAXY STELLAR MASS ASSEMBLY BETWEEN 0.2 < z < 2 FROM THE S-COSMOS SURVEY

By O. Ilbert, Mara Salvato, É. Le Floc'h, H. Aussel, P. Capak, H. McCracken, B. Mobasher, J. Kartaltepe, N. Scoville, D. Sanders and 15 more. 2009

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We follow the galaxy stellar mass assembly by morphological and spectral type in the COSMOS 2 deg2 field. We derive the stellar mass functions and stellar mass densities from z = 2 to z = 0.2 using 196,000 galaxies selected at F3.6 μm > 1 μJy with accurate photometric redshifts ( at i+ < 22.5). Using a spectral classification, we find that z ∼ 1 is an epoch of transition in the stellar mass assembly of quiescent galaxies. Their stellar mass density increases by 1.1 dex between z = 1.5–2 and z = 0.8–1 (Δt ∼ 2.5 Gyr), but only by 0.3 dex between z = 0.8–1 and z ∼ 0.1 (Δt ∼ 6 Gyr). Then, we add the morphological information and find that 80%–90% of the massive quiescent galaxies have an elliptical morphology at z < 0.8. Therefore, a dominant mechanism links the shutdown of star formation and the acquisition of an elliptical morphology in massive galaxies. Still, a significant fraction of quiescent galaxies present a Spi/Irr morphology at low mass (40%–60% at ), but this fraction is smaller than predicted by semi-analytical models using a “halo quenching” recipe. We also analyze the evolution of star-forming galaxies and split them into “intermediate activity” and “high activity” galaxies. We find that the most massive “high activity” galaxies end their high star formation rate phase first. Finally, the space density of massive star-forming galaxies becomes lower than the space density of massive elliptical galaxies at z < 1. As a consequence, the rate of “wet mergers” involved in the formation of the most massive ellipticals must decline very rapidly at z < 1, which could explain the observed slow down in the assembly of these quiescent and massive sources.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e855f5012ad8b23ae9767040bb817e47650510cd

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