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Cosmological simulations of low-mass galaxies: some potential issues

Published online by Cambridge University Press:  27 April 2011

Pedro Colín ,
Vladimir Avila-Reese  and
Octavio Valenzuela
Pedro Colín
Affiliation:
Centro de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, A.P. 72-3 (Xangari), Morelia, Michoacán 58089, México
Vladimir Avila-Reese
Affiliation:
Instituto de Astronomía, Universidad Nacional Autónoma de México, A.P. 70-264, 04510, México, D.F., México
Octavio Valenzuela
Affiliation:
Instituto de Astronomía, Universidad Nacional Autónoma de México, A.P. 70-264, 04510, México, D.F., México
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Abstract

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Cosmological Adaptive Mesh Refinement simulations are used to study the specific star formation rate (sSFR=SSF/Ms) history and the stellar mass fraction, fs=Ms/MT, of small galaxies, total masses MT between few × 1010 M⊙ to few ×1011 M⊙. Our results are compared with recent observational inferences that show the so-called “downsizing in sSFR” phenomenon: the less massive the galaxy, the higher on average is its sSFR, a trend seen at least since z ~ 1. The simulations are not able to reproduce this phenomenon, in particular the high inferred values of sSFR, as well as the low values of fs constrained from observations. The effects of resolution and sub-grid physics on the SFR and fs of galaxies are discussed.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 503 - 506
Copyright
Copyright © International Astronomical Union 2011

References

Colín, P., Avila-Reese, V., Vázquez-Semadeni, E., Valenzuela, O., & Ceverino, D. 2010, ApJ, 713, 535Google Scholar
Behroozi, P. S., Conroy, C., & Wechsler, R. H. 2010, ApJ, 717, 379Google Scholar
Firmani, C., Avila-Reese, V., & Rodríguez-Puebla, A. 2010, MNRAS, 404, 1100Google Scholar
Franco, J., & Cox, D. P. 1986, PASP, 98, 1076Google Scholar
Guo, Q, White, S., Li, Ch., & Boylan-Kolchin, M. 2010, MNRAS, 404, 1100Google Scholar
Kravtsov, A. V., Klypin, A. A., & Khokhlov, A.M., 1997, ApJS, 111, 73Google Scholar
Kravtsov, A. V. 2003, ApJ (Letters), 590, 1Google Scholar
Salim, S. et al. 2007, ApJS, 173, 267Google Scholar
Santini, P. et al. , 2009, A&A, 504, 751Google Scholar
van Dishoeck, E. F., & Black, J. H. 1988, ApJ, 334, 771CrossRefGoogle Scholar