The evolution of the baryon fraction in halos as a cause of scatter in the galaxy stellar mass in the EAGLE simulation
| Autor: | Tom Theuns, Nelson Padilla, E. Paillas, Matthieu Schaller, Robert A. Crain, Joop Schaye, Andrea Kulier, Richard G. Bower |
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| Rok vydání: | 2019 |
| Předmět: |
Physics
Stellar population Stellar mass 010308 nuclear & particles physics Dark matter FOS: Physical sciences Astronomy and Astrophysics Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences Astrophysics - Astrophysics of Galaxies Galaxy Accretion (astrophysics) Redshift Baryon Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Halo 010303 astronomy & astrophysics QC Astrophysics::Galaxy Astrophysics QB |
| Zdroj: | Monthly notices of the Royal Astronomical Society, 2019, Vol.482(3), pp.3261-3273 [Peer Reviewed Journal] Monthly Notices of the RAS (0035-8711), 482(3), 3261-3273 |
| ISSN: | 0035-8711 |
| Popis: | The EAGLE simulation suite has previously been used to investigate the relationship between the stellar mass of galaxies, $M_{*}$, and the properties of dark matter halos, using the hydrodynamical reference simulation combined with a dark matter only (DMO) simulation having identical initial conditions. The stellar masses of central galaxies in halos with $M_{\mathrm{200c}} > 10^{11} \mathrm{M_{\odot}}$ were shown to correlate with the DMO halo maximum circular velocity, with $\approx 0.2$ dex of scatter that is uncorrelated with other DMO halo properties. Here we revisit the origin of the scatter in the $M_{*}-V_{\mathrm{max, DMO}}$ relation in EAGLE at $z = 0.1$. We find that the scatter in $M_{*}$ correlates with the mean age of the galaxy stellar population such that more massive galaxies at fixed $V_{\mathrm{max, DMO}}$ are younger. The scatter in the stellar mass and mean stellar population age results from variation in the baryonic mass, $M_{\mathrm{bary}} = M_{\mathrm{gas}} + M_{*}$, of the galaxies' progenitors at fixed halo mass and concentration. At the redshift of peak correlation ($z \approx 1$), the progenitor baryonic mass accounts for $75\%$ of the variance in the $z=0.1$ $M_{*}-V_{\mathrm{max, DMO}}$ relation. The scatter in the baryonic mass, in turn, is primarily set by differences in feedback strength and gas accretion over the course of the evolution of each halo. 15 pages, 9 figures. Version accepted to MNRAS |
| Databáze: | OpenAIRE |
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