The mass and temperature functions in a moving barrier model

Abstract

In this paper, I use the extension of the excursion set model of Sheth & Tormen (2002) and the barrier shape obtained in Del Popolo & Gambera (1998) to calculate the unconditional halo mass function, and the conditional mass function in several cosmological models. I show that the barrier obtained in Del Popolo & Gambera (1998), which takes account of tidal interaction between proto-haloes, is a better description of the mass functions than the spherical collapse and is in good agreement with numerical simulations (Tozzi & Governato 1998, and Governato et al. 1999). The results are also in good agreement with those obtained by Sheth & Tormen (2002), only slight differences are observed expecially at the low mass end. I moreover calculate, and compare with simulations, the temperature function obtained by means of the mass functions previously calculated and also using an improved version of the M-T relation, which accounts for the fact that massive clusters accrete matter quasi-continuously, and finally taking account of the tidal interaction with neighboring clusters. Even in this case the discrepancy between the Press-Schecter predictions and simulations is considerably reduced.

23 pages; 11 encapsulated figures. Accepted for publication in MNRAS

References in corpus (5)

• Concentrations of Dark Halos from their Assembly Histories
• An excursion set model of hierarchical clustering: Ellipsoidal collapse and the moving barrier
• Universal gas density and temperature profile
• Mass-Temperature Relation of Galaxy Clusters: A Theoretical Study
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• Small scale problems of the $\Lambda$CDM model: a short review
• Non-Baryonic Dark Matter in Cosmology
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• Neutrino Mass Limit from Galaxy Cluster Number Density Evolution
• Improvements in the M-T relation and mass function and the measured Omega_m through clusters evolution
• Measuring Omega_m using clusters evolution
• Barions and $\Lambda$CDM Model Problems
• Cosmological constraints from clustering properties of galaxy clusters