Tracing the quenching history of cluster galaxies in the EAGLE simulation
| العنوان: | Tracing the quenching history of cluster galaxies in the EAGLE simulation |
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| المؤلفون: | Facundo A. Gómez, Nelson Padilla, P. Cerulo, S. Torres-Flores, D. Olave-Rojas, Diego Pallero, R. Demarco |
| المصدر: | Monthly Notices of the Royal Astronomical Society. 488:847-858 |
| بيانات النشر: | Oxford University Press (OUP), 2019. |
| سنة النشر: | 2019 |
| مصطلحات موضوعية: | Physics, Eagle, Quenching (fluorescence), biology, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Tracing, 01 natural sciences, Galaxy, Space and Planetary Science, biology.animal, 0103 physical sciences, Cluster (physics), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics |
| الوصف: | We use the Evolution and Assembly of GaLaxies and their Environments (EAGLE) hydrodynamical simulation to trace the quenching history of galaxies in its 10 most massive clusters. We use two criteria to identify moments when galaxies suffer significant changes in their star formation activity: (i) the instantaneous star formation rate (SFR) strongest drop, $\Gamma _{\rm SFR}^{\rm SD}$, and (ii) a ‘quenching’ criterion based on a minimum threshold for the specific SFR of ≲10$^{-11}\,\rm yr^{-1}$. We find that a large fraction of galaxies (${\gtrsim} 60\,{\rm per\,cent}$) suffer their $\Gamma _{\rm SFR}^{\rm SD}$ outside the cluster’s R200. This ‘pre-processed’ population is dominated by galaxies that are either low mass and centrals or inhabit low-mass hosts (1010.5 ≲ Mhost ≲ 1011.0 M⊙). The host mass distribution is bimodal, and galaxies that suffered their $\Gamma _{\rm SFR}^{\rm SD}$ in massive hosts ($10^{13.5} \lesssim M_{\rm host} \lesssim 10^{14.0}\, \mathrm{M}_{\odot }$) are mainly processed within the clusters. Pre-processing mainly limits the total stellar mass with which galaxies arrive in the clusters. Regarding quenching, galaxies preferentially reach this state in high-mass haloes ($10^{13.5} \lesssim M_{\rm host} \lesssim 10^{14.5}\, \mathrm{M}_{\odot }$). The small fraction of galaxies that reach the cluster already quenched have also been pre-processed, linking both criteria as different stages in the quenching process of those galaxies. For the z = 0 satellite populations, we find a sharp rise in the fraction of quenched satellites at the time of first infall, highlighting the role played by the dense cluster environment. Interestingly, the fraction of pre-quenched galaxies rise with final cluster mass. This is a direct consequence of the hierarchical cosmological model used in these simulations. |
| تدمد: | 1365-2966 0035-8711 |
| URL الوصول: | https://explore.openaire.eu/search/publication?articleId=doi_________::bd5e7445e7a20700d69401ae78c2e4c6 https://doi.org/10.1093/mnras/stz1745 |
| حقوق: | OPEN |
| رقم الأكسشن: | edsair.doi...........bd5e7445e7a20700d69401ae78c2e4c6 |
| قاعدة البيانات: | OpenAIRE |
| تدمد: | 13652966 00358711 |
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