2015
DOI: 10.1093/mnras/stv1508
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Star formation in mergers with cosmologically motivated initial conditions

Abstract: We use semi-analytic models and cosmological merger trees to provide the initial conditions for multi-merger numerical hydrodynamic simulations, and exploit these simulations to explore the effect of galaxy interaction and merging on star formation (SF). We compute numerical realisations of twelve merger trees from z = 1.5 to z = 0. We include the effects of the large hot gaseous halo around all galaxies, following recent obervations and predictions of galaxy formation models. We find that including the hot ga… Show more

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Cited by 15 publications
(13 citation statements)
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References 123 publications
(189 reference statements)
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“…In our analysis, we introduce dry (major) mergers in the evolution of Φ pass,HD , assuming that two objects in the same bin of log M can merge without triggering relevant episodes of star formation (e.g. Di Matteo et al 2005;Karman et al 2015). We set the fraction of galaxies undergoing a 1:1 merger to be equal to f dry (z), with no dependence on the stellar mass of the initial pair (Xu et al 2012).…”
Section: An Empirical Approachmentioning
confidence: 99%
“…In our analysis, we introduce dry (major) mergers in the evolution of Φ pass,HD , assuming that two objects in the same bin of log M can merge without triggering relevant episodes of star formation (e.g. Di Matteo et al 2005;Karman et al 2015). We set the fraction of galaxies undergoing a 1:1 merger to be equal to f dry (z), with no dependence on the stellar mass of the initial pair (Xu et al 2012).…”
Section: An Empirical Approachmentioning
confidence: 99%
“…Our definition of the SF enhancement include stars formed in the satellite as well. A more sophisticated analysis of the merger driven star formation rates is presented in a complementary work (Karman et al 2015), but the general trends are investigated here.…”
Section: Sites Of Star Formationmentioning
confidence: 99%
“…In some models, producing an elliptical-like remnant with an old stellar population requires a powerful AGN to clear out the left-over gas Hopkins et al 2006;Sparre & Springel 2017). When pre-existing hot gaseous halos are included in merger simulations, infall from the halo helps sustain star formation, but the efficiency of star formation is decreased because of heating of halo gas by shocks and by the conversion of satellite orbital energy into heat (Sinha & Holley-Bockelmann 2009;Moster et al 2011;Karman et al 2015;Hwang & Park 2015). Model predictions depend upon the resolution of the simulation and the details of the calculations, with higher resolution models including multiphase interstellar gas producing more efficient star formation (Teyssier, Chapon, & Bournaud 2010;Hopkins et al 2013;Hayward et al 2014;Sparre & Springel 2016).…”
Section: Introductionmentioning
confidence: 99%