The growth of the stellar seeds of supermassive black holes

Johnson, Jarrett L.; Agarwal, Bhaskar; Whalen, Daniel J.; Vecchia, Claudio Dalla; Fryer, Christopher L.; Khochfar, Sadegh; Li, Hui; Livio, Mario

doi:10.1063/1.4754374

Cited by 43 publications

(82 citation statements)

References 3 publications

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“…The primordial SFRD rises until z ∼ 20 and decreases afterwards (as Pop II star formation becomes the main mode). This evolution of the total SFRD is consistent with previous studies (e.g., Agarwal et al 2012;Johnson et al 2013), but our results show clearly the contribution of Pop III.2D stars. Significant Pop III.2D star formation occurs after Pop III.1 stars are formed and emit copious amounts of FUV photons.…”

Section: Mass Distribution Of Primordial Starssupporting

confidence: 83%

“…18a). In comparison to the background FUV field calculated by Agarwal et al (2012) and Johnson et al (2013), the local J21 is at the same levels for z 15 but starts to decline earlier for z 15. This earlier decline is because of our ignorance of Pop II stars for calculating the FUV radiation fields.…”

Section: Star Formation Rate Densitymentioning

confidence: 99%

“…Previous studies show that the FUV radiation from nearby Pop II stars dominates over the Pop III component at z 10 − 15 (e.g., Agarwal et al 2012;Johnson et al 2013). Thus, we stop our simulations at z = 10 (see also discussion in Sec.…”

Section: Sampling Star-forming Regions In Cosmological Simulationsmentioning

confidence: 99%

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Primordial star formation under the influence of far ultraviolet radiation: 1540 cosmological haloes and the stellar mass distribution

Hirano

Hosokawa

Yoshida

et al. 2015

Monthly Notices of the Royal Astronomical Society

333

313

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We perform a large set of cosmological simulations of early structure formation and follow the formation and evolution of 1540 star-forming gas clouds to derive the mass distribution of primordial stars. The star formation in our cosmological simulations is characterized by two distinct populations, the so-called Population III.1 stars and primordial stars formed under the influence of far-ultraviolet (FUV) radiation (Population III.2 D stars). In this work, we determine the stellar masses by using the dependences on the physical properties of star-forming cloud and/or the external photodissociating intensity from nearby primordial stars, which are derived from the results of 2D radiation hydrodynamic simulations of protostellar feedback. The characteristic mass of the Pop III stars is found to be a few hundred solar masses at z ∼ 25, and it gradually shifts to lower masses with decreasing redshift. At high redshifts z > 20, about half of the star-forming gas clouds are exposed to intense FUV radiation and thus give birth to massive Pop III.2 D stars. However, the local FUV radiation by nearby Pop III stars becomes weaker at lower redshifts, when typical Pop III stars have smaller masses and the mean physical separation between the stars becomes large owing to cosmic expansion. Therefore, at z < 20, a large fraction of the primordial gas clouds host Pop III.1 stars. At z 15, the Pop III.1 stars are formed in relatively cool gas clouds due to efficient radiative cooling by H 2 and HD molecules; such stars have masses of a few ×10 M ⊙ . Since the stellar evolution and the final fate are determined by the stellar mass, Pop III stars formed at different epochs play different roles in the early Universe.

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Section: Mass Distribution Of Primordial Starssupporting

confidence: 83%

Section: Star Formation Rate Densitymentioning

confidence: 99%

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Primordial star formation under the influence of far ultraviolet radiation: 1540 cosmological haloes and the stellar mass distribution

Hirano

Hosokawa

Yoshida

et al. 2015

Monthly Notices of the Royal Astronomical Society

333

313

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“…The exact redshift evolution of the Pop III SFR depends on the details of the treatment of reionization and metal enrichment (cf. Johnson et al 2013, for a comparison).…”

Section: Resultsmentioning

confidence: 99%

Gravitational waves from the remnants of the first stars

Hartwig

Volonteri

Bromm

et al. 2016

Monthly Notices of the Royal Astronomical Society: Letters

164

149

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Gravitational waves (GWs) provide a revolutionary tool to investigate yet unobserved astrophysical objects. Especially the first stars, which are believed to be more massive than present-day stars, might be indirectly observable via the merger of their compact remnants. We develop a self-consistent, cosmologically representative, semi-analytical model to simulate the formation of the first stars. By extrapolating binary stellarevolution models at 10 % solar metallicity to metal-free stars, we track the individual systems until the coalescence of the compact remnants. We estimate the contribution of primordial stars to the merger rate density and to the detection rate of the Advanced Laser Interferometer Gravitational-Wave Observatory (aLIGO). Owing to their higher masses, the remnants of primordial stars produce strong GW signals, even if their contribution in number is relatively small. We find a probability of 1% that the current detection GW150914 is of primordial origin. We estimate that aLIGO will detect roughly 1 primordial BH-BH merger per year for the final design sensitivity, although this rate depends sensitively on the primordial initial mass function (IMF). Turning this around, the detection of black hole mergers with a total binary mass of ∼ 300 M would enable us to constrain the primordial IMF.

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“…mechanisms, which suggest Pop III stars could have formed as early as z ∼ 20 − 30 and a small amount of them might still form until the end of reionization (Scannapieco et al 2003;Furlanetto & Loeb 2005;Trenti et al 2009;Johnson et al 2013). …”

Section: Population III Starsmentioning

confidence: 99%

Constraints on the star formation efficiency of galaxies during the epoch of reionization

Sun

Furlanetto

2016

Mon. Not. R. Astron. Soc.

183

157

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Reionization is thought to have occurred in the redshift range of 6 < z < 9, which is now being probed by both deep galaxy surveys and CMB observations. Using halo abundance matching over the redshift range 5 < z < 8 and assuming smooth, continuous gas accretion, we develop a model for the star formation efficiency f of dark matter halos at z > 6 that matches the measured galaxy luminosity functions at these redshifts. We find that f peaks at ∼ 30% at halo masses M ∼ 10 11 -10 12 M , in qualitative agreement with its behavior at lower redshifts. We then investigate the cosmic star formation histories and the corresponding models of reionization for a range of extrapolations to small halo masses. We use a variety of observations to further constrain the characteristics of the galaxy populations, including the escape fraction of UV photons. Our approach provides an empirically-calibrated, physically-motivated model for the properties of star-forming galaxies sourcing the epoch of reionization. In the case where star formation in low-mass halos is maximally efficient, an average escape fraction ∼ 0.1 can reproduce the optical depth reported by Planck, whereas inefficient star formation in these halos requires either about twice as many UV photons to escape, or an escape fraction that increases towards higher redshifts. Our models also predict how future observations with JWST can improve our understanding of these galaxy populations.

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The growth of the stellar seeds of supermassive black holes

Cited by 43 publications

References 3 publications

Primordial star formation under the influence of far ultraviolet radiation: 1540 cosmological haloes and the stellar mass distribution

Primordial star formation under the influence of far ultraviolet radiation: 1540 cosmological haloes and the stellar mass distribution

Gravitational waves from the remnants of the first stars

Constraints on the star formation efficiency of galaxies during the epoch of reionization

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