2002
DOI: 10.1086/339917
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First Stars, Very Massive Black Holes, and Metals

Abstract: Recent studies suggest that the initial mass function (IMF) of the first stars (Population III) is likely to have been extremely top-heavy, unlike what is observed at present. We propose a scenario to generate fragmentation to lower masses once the first massive stars have formed and derive constraints on the primordial IMF. We estimate the mass fraction of pair-unstable supernovae (SN ), shown to be the dominant sources of the first heavy elements. These metals enrich the surrounding gas up to %10 À4 Z , when… Show more

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Cited by 476 publications
(523 citation statements)
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References 71 publications
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“…The critical metallicity at which the transition in the IMF takes place is uncertain, but cosmological simulations suggest that Pop III supernovae quickly boost the local metallicity above the critical metallicity, so the onset of Pop II star formation does not depend sensitively on this choice (Maio et al 2010(Maio et al , 2011. We choose a critical metallicity of Zcrit = 10 −4 Z , with Z = 0.02, a value roughly consistent with both theory (Bromm et al 2001;Schneider et al 2002) and the inferred metallicities of metal-poor stars (Frebel et al 2007;Caffau et al 2011). …”
Section: Star Formationmentioning
confidence: 97%
“…The critical metallicity at which the transition in the IMF takes place is uncertain, but cosmological simulations suggest that Pop III supernovae quickly boost the local metallicity above the critical metallicity, so the onset of Pop II star formation does not depend sensitively on this choice (Maio et al 2010(Maio et al , 2011. We choose a critical metallicity of Zcrit = 10 −4 Z , with Z = 0.02, a value roughly consistent with both theory (Bromm et al 2001;Schneider et al 2002) and the inferred metallicities of metal-poor stars (Frebel et al 2007;Caffau et al 2011). …”
Section: Star Formationmentioning
confidence: 97%
“…One is remnant BHs of massive Population III (Pop III) stars with ∼ 100 M (Madau & Rees 2001;Haiman & Loeb 2001;Schneider et al 2002;Islam, Taylor & Silk 2003;Volonteri, Haardt & Madau 2003;Tanaka & Haiman 2009). Second, the socalled direct collapse model (Loeb & Rasio 1994;Oh & Haiman 2002;Bromm & Loeb 2003;Begelman, Volonteri & Rees 2006;Lodato & Natarajan 2006;Shang, Bryan & 2014).…”
Section: Introductionmentioning
confidence: 99%
“…Schneider et al 2002;Heger & Woosley 2002;Suda & Fujimoto 2010) and small (e.g. Clark et al 2011;Stacy & Bromm 2014).…”
Section: Introductionmentioning
confidence: 99%