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Title: THE SPECIFIC STAR FORMATION RATE AND STELLAR MASS FRACTION OF LOW-MASS CENTRAL GALAXIES IN COSMOLOGICAL SIMULATIONS

Abstract

By means of cosmological N-body + hydrodynamics simulations of galaxies in the context of the {Lambda} cold dark matter ({Lambda}CDM) scenario we explore the specific star formation rates (SSFR = SFR/M{sub s} , M{sub s} is the stellar mass) and stellar mass fractions (F{sub s} {identical_to} M{sub s} /M{sub h} , M{sub h} is the halo mass) for sub-M* field galaxies at different redshifts (0 {approx}< z {approx}< 1.5). Distinct low-mass halos (2.5 {approx}< M{sub h} /10{sup 10} M{sub sun} {approx}< 50 at z = 0) were selected for the high-resolution re-simulations. The Hydrodynamics Adaptive Refinement Tree (ART) code was used and some variations of the sub-grid parameters were explored. Most 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 observed field galaxies are actually blue/star forming). This inconsistency seems to remain even at z {approx} 1-1.5, although it is less drastic. The F{sub s} of simulated galaxies increases with M{submore » h} as semi-empirical inferences show. However, the values of F{sub s} at z {approx} 0 are {approx}5-10 times larger in the simulations than in the inferences; these differences increases probably to larger factors at z {approx} 1-1.5. The inconsistencies reported here imply that simulated low-mass galaxies (0.2 {approx}< M{sub s} /10{sup 9} M{sub sun} {approx}< 30 at z = 0) assembled their stellar masses much earlier than observations suggest. Our results confirm the predictions found by means of {Lambda}CDM-based models of disk galaxy formation and evolution for isolated low-mass galaxies, and highlight that our understanding and implementation of astrophysics into simulations and models are still lacking vital ingredients.« less

Authors:
; ; ;  [1];  [2];  [3];  [4]
  1. Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, A. P. 70-264, 04510, Mexico, D. F. (Mexico)
  2. Centro de Radioastronomia y Astrofisica, Universidad Nacional Autonoma de Mexico, A. P. 72-3 (Xangari), Morelia, Michoacan 58089 (Mexico)
  3. Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, A. P. 877, Ensenada BC 22800 (Mexico)
  4. Racah Institute of Physics, The Hebrew University, Jerusalem 91904 (Israel)
Publication Date:
OSTI Identifier:
21578203
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 736; Journal Issue: 2; Other Information: DOI: 10.1088/0004-637X/736/2/134; Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; GALACTIC EVOLUTION; GALAXIES; HYDRODYNAMICS; MASS; NONLUMINOUS MATTER; SIMULATION; STARS; EVOLUTION; FLUID MECHANICS; MATTER; MECHANICS

Citation Formats

Avila-Reese, V., Gonzalez-Samaniego, A., Valenzuela, O., Firmani, C., ColIn, P., Velazquez, H., and Ceverino, D. THE SPECIFIC STAR FORMATION RATE AND STELLAR MASS FRACTION OF LOW-MASS CENTRAL GALAXIES IN COSMOLOGICAL SIMULATIONS. United States: N. p., 2011. Web. doi:10.1088/0004-637X/736/2/134.
Avila-Reese, V., Gonzalez-Samaniego, A., Valenzuela, O., Firmani, C., ColIn, P., Velazquez, H., & Ceverino, D. THE SPECIFIC STAR FORMATION RATE AND STELLAR MASS FRACTION OF LOW-MASS CENTRAL GALAXIES IN COSMOLOGICAL SIMULATIONS. United States. doi:10.1088/0004-637X/736/2/134.
Avila-Reese, V., Gonzalez-Samaniego, A., Valenzuela, O., Firmani, C., ColIn, P., Velazquez, H., and Ceverino, D. Mon . "THE SPECIFIC STAR FORMATION RATE AND STELLAR MASS FRACTION OF LOW-MASS CENTRAL GALAXIES IN COSMOLOGICAL SIMULATIONS". United States. doi:10.1088/0004-637X/736/2/134.
@article{osti_21578203,
title = {THE SPECIFIC STAR FORMATION RATE AND STELLAR MASS FRACTION OF LOW-MASS CENTRAL GALAXIES IN COSMOLOGICAL SIMULATIONS},
author = {Avila-Reese, V. and Gonzalez-Samaniego, A. and Valenzuela, O. and Firmani, C. and ColIn, P. and Velazquez, H. and Ceverino, D.},
abstractNote = {By means of cosmological N-body + hydrodynamics simulations of galaxies in the context of the {Lambda} cold dark matter ({Lambda}CDM) scenario we explore the specific star formation rates (SSFR = SFR/M{sub s} , M{sub s} is the stellar mass) and stellar mass fractions (F{sub s} {identical_to} M{sub s} /M{sub h} , M{sub h} is the halo mass) for sub-M* field galaxies at different redshifts (0 {approx}< z {approx}< 1.5). Distinct low-mass halos (2.5 {approx}< M{sub h} /10{sup 10} M{sub sun} {approx}< 50 at z = 0) were selected for the high-resolution re-simulations. The Hydrodynamics Adaptive Refinement Tree (ART) code was used and some variations of the sub-grid parameters were explored. Most 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 observed field galaxies are actually blue/star forming). This inconsistency seems to remain even at z {approx} 1-1.5, although it is less drastic. The F{sub s} of simulated galaxies increases with M{sub h} as semi-empirical inferences show. However, the values of F{sub s} at z {approx} 0 are {approx}5-10 times larger in the simulations than in the inferences; these differences increases probably to larger factors at z {approx} 1-1.5. The inconsistencies reported here imply that simulated low-mass galaxies (0.2 {approx}< M{sub s} /10{sup 9} M{sub sun} {approx}< 30 at z = 0) assembled their stellar masses much earlier than observations suggest. Our results confirm the predictions found by means of {Lambda}CDM-based models of disk galaxy formation and evolution for isolated low-mass galaxies, and highlight that our understanding and implementation of astrophysics into simulations and models are still lacking vital ingredients.},
doi = {10.1088/0004-637X/736/2/134},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 736,
place = {United States},
year = {2011},
month = {8}
}