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The specific star formation rate and stellar mass fraction of low-mass central galaxies in cosmological simulations | | V. Avila-Reese
; P.Colín
; A. González-Samaniego
; O. Valenzuela
; C. Firmani
; H. Velázquez
; D. Ceverino
; | | Date: |
23 Mar 2011 | | Abstract: | By means of cosmological simulations of galaxies in the context of the LCDM
scenario we explore the specific star formation rates (SSFR=SFR/Ms, Ms is the
stellar mass) and stellar mass fractions (Fs=Ms/Mh, Mh is the halo mass) for
sub-M* field galaxies at different redshifts (0<z<1.5). Distinct low-mass halos
(2.5< Mh/10^10 Msun < 50 at z=0) were selected for the high-resolution
re-simulations. The Hydrodynamics ART code was used and some variations of the
sub-grid parameters were explored. Most of simulated galaxies, specially those
with the highest resolutions, have significant disk components and their
structural and dynamical properties are in reasonable agreement with
observations of sub-M* field galaxies. However, the SSFRs are 5-10 times
smaller than the averages of several (compiled and homogenized here)
observational determinations for field blue/star-forming galaxies at z<0.3 (at
low masses, most of observed field galaxies are actually blue/star-forming);
this inconsistency seems to remain even at z~1-1.5 though less drastic. The Fs
of simulated galaxies increases with Mh as semi-empirical inferences show, but
in absolute values the former are ~5-10 times larger than the latter at z= 0;
this difference increases probably to larger factors at z~1-1.5. The
inconsistencies reported here imply that simulated low-mass galaxies
(0.2<Ms/10^9 Msun <30 at z=0) assembled their stellar masses much earlier than
observations suggest, probably as a consequence of the early assembly of their
dark halos. Our results confirm the predictions found by means of LCDM-based
models of disk galaxy formation and evolution for isolated low-mass galaxies
(Firmani & Avila-Reese 2010). | | Source: | arXiv, 1103.4422 | | Services: | Forum | Review | PDF | Favorites | |
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