The history of the baryon budget

Free access article

Issue		A&A Volume 445, Number 1, January I 2006


Page(s)		1 - 27
Section		Cosmology (including clusters of galaxies)
DOI		http://dx.doi.org/10.1051/0004-6361:20053116

A&A 445, 1-27 (2006)
DOI: 10.1051/0004-6361:20053116

Cosmic logistics in a hierarchical universe

Y. Rasera and R. Teyssier

DAPNIA, Service d'Astrophysique, Bâtiment 709, L'Orme des Merisiers, 91191 Gif-sur-Yvette Cedex, France
e-mail: romain.teyssier@cea.fr

(Received 22 March 2005 / Accepted 3 June 2005 )

Abstract
Using a series of high-resolution N-body hydrodynamical numerical simulations, we investigate several scenarios for the evolution of the baryon budget in galactic halos. We derive individual halo star formation history (SFH), as well as the global star formation rate in the universe. We develop a simple analytical model that allows us to compute surprisingly accurate predictions, when compared to our simulations, but also to other simulations presented in Springel & Hernquist (2003b, MNRAS, 339, 312). The model depends on two main parameters: the star formation time scale t_* and the wind efficiency $\eta_{\rm w}$ . We also compute, for halos of a given mass, the baryon fraction in each of the following phases: cold disc gas, hot halo gas, and stars. Here again, our analytical model predictions are in good agreement with simulation results, if one correctly takes finite resolution effect into account. We compare predictions of our analytical model to several observational constraints and conclude that a very narrow range of the model parameters is allowed. The important role played by galactic winds is outlined, as well as a possible "superwind" scenario in groups and clusters. The "anti-hierarchical" behavior of observed SFH is reproduced well by our best model with t_*=3 Gyr and $\eta_{\rm w}=1.5$ . We obtain in this case a present-day cosmic baryon budget of $\Omega_{*}\simeq 0.004$ , $\Omega_{\rm cold}\simeq 0.0004$ , $\Omega_{\rm hot}\simeq 0.01$ and $\Omega_{\rm back} \simeq 0.02$ (diffuse background).

Key words: galaxies: formation -- galaxies: stellar content -- cosmology: theory -- methods: analytical -- methods: numerical -- galaxies: evolution

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