| Full text | |
| Author(s): |
Total Authors: 2
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| Affiliation: | [1] Inst Nacl Pesquisas Espaciais, Div Astrofis, BR-12227010 Sao Paulo, SP - Brazil
Total Affiliations: 1
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| Document type: | Journal article |
| Source: | NEW ASTRONOMY; v. 41, p. 48-52, NOV 2015. |
| Web of Science Citations: | 0 |
| Abstract | |
The cosmic star formation rate (CSFR) represents the fraction of gas that is converted into stars within a certain comoving volume and at a given time t. However the evolution of the dark matter haloes and its relationship with the CSFR is not yet clear. In this context, we have investigated the role of the dark halo mass function - DHMF - in the process of gas conversion into stars. We observed a strong dependence between the fraction of baryons in structures, f(b), and the specific mass function used for describing the dark matter haloes. In some cases, we have obtained f(b) greater than one at redshift z = 0. This result indicates that the evolution of dark matter, described by the specific DHMF, could not trace the baryonic matter without a bias parameter. We also observed that the characteristic time-scale for star formation, t, is strongly dependent on the considered DHMF, when the model is confronted against the observational data. Also, as part of this work it was released, under GNU general public license, a Python package called `pycosmicstar' to study the CSFR and its relationship with the DHMF. (C) 2015 Elsevier B.V. All rights reserved. (AU) | |
| FAPESP's process: | 12/21877-5 - Numerical simulation of Supermassive black holes population and its role into the universe reionization |
| Grantee: | Eduardo dos Santos Pereira |
| Support Opportunities: | Scholarships in Brazil - Post-Doctoral |