2020
DOI: 10.1093/mnras/staa291
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Aging haloes: implications of the magnitude gap on conditional statistics of stellar and gas properties of massive haloes

Abstract: Cold dark matter model predicts that the large-scale structure grows hierarchically. Small dark matter halos form first. Then, they grow gradually via continuous merger and accretion. These halos host the majority of baryonic matter in the Universe in the form of hot gas and cold stellar phase. Determining how baryons are partitioned into these phases requires detailed modeling of galaxy formation and their assembly history. It is speculated that formation time of the same mass halos might be correlated with t… Show more

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Cited by 24 publications
(25 citation statements)
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References 94 publications
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“…We use the results being as close as possible to our median redshift and consider the redshift dependence of p(Z, z). The gas mass slopes of numerical simulations (Young et al 2011;Planelles et al 2013;Barnes et al 2017b;Wu et al 2015;Truong et al 2018;Farahi et al 2018a;Henden et al 2020;Farahi et al 2020) are higher than predicted by the self-similar model (β = 1). Some simulations are slightly steeper than the self-similar expectation (1 < βg < 1.1) while others have a clear higher slope (βg > ∼ 1.2).…”
Section: Scaling Relations and Mass-dependent Slopesmentioning
confidence: 64%
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“…We use the results being as close as possible to our median redshift and consider the redshift dependence of p(Z, z). The gas mass slopes of numerical simulations (Young et al 2011;Planelles et al 2013;Barnes et al 2017b;Wu et al 2015;Truong et al 2018;Farahi et al 2018a;Henden et al 2020;Farahi et al 2020) are higher than predicted by the self-similar model (β = 1). Some simulations are slightly steeper than the self-similar expectation (1 < βg < 1.1) while others have a clear higher slope (βg > ∼ 1.2).…”
Section: Scaling Relations and Mass-dependent Slopesmentioning
confidence: 64%
“…Recent cosmological hydrodynamic simulations (e.g. Young et al 2011;McCarthy et al 2011;Planelles et al 2013;Martizzi et al 2014;Le Brun et al 2014;Wu et al 2015;Sembolini et al 2016a;McCarthy et al 2017;Barnes et al 2017b;Farahi et al 2018a;Henden et al 2020;Farahi et al 2020) studied stellar mass and gas distributions in clusters and/or groups. The simulations include the effect of cooling, AGN feedback, star formation, and SN feedback and compare them with the results of non-radiative simulations.…”
Section: Comparison Of Numerical Simulationsmentioning
confidence: 99%
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“…Relying on simulations, richness, formation time and magnitude gap are related to each other. The number of satellite galaxies in a halo, which is closely related to the cluster richness, depending on the formation time (Farahi et al 2020), because satellites in early formed haloes had more time to merge and reduce their number. Moreover, the cannibalism of the central galaxy, grown by major mergers, produces the lack of bright satellite galaxies (Jones et al 2003;Giodini et al 2013) and consequently increases the magnitude gap between the first and the second BCG, which should therefore be indicative of the formation time.…”
Section: Discussionmentioning
confidence: 99%
“…A larger scatter in such relations produces larger errors in the cosmological parameters estimates (Lima & Hu 2005). The scatter can be due to the measurement errors of the involved quantities, but there is also ★ E-mail: emanuella.puddu@inaf.it an intrinsic component that reflects the variegated properties of the examined clusters sample (Andreon et al 2017); such properties are related to the formation and evolution scenarios (Hartley et al 2008;Fujita et al 2018) and to the underlying physical processes taking place into clusters (Farahi et al 2020). Understanding the nature of the intrinsic component could contribute having a more deep insight into these processes (for example AGN feedback, star formation, mergers, radiative cooling and other non-gravitational effects; e.g.…”
Section: Introductionmentioning
confidence: 99%