Exploring the nature of the Lyman-α emitter CR7

Hartwig, Tilman; Latif, Muhammad; Magg, Mattis; Bromm, Volker; Klessen, Ralf S.; Glover, Simon C. O.; Whalen, Daniel J.; Pellegrini, E.; Volonteri, Marta

doi:10.1093/mnras/stw1775

Cited by 48 publications

(68 citation statements)

References 180 publications

(251 reference statements)

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“…For this, we shift the functional form of the H17 OF by 1 dex in stellar mass, and modify the plateau at low mass with a linear extrapolation, down to OF=0 ("H17low1") or OF=0.01 ("H17low2"). We have compared the shifted scaling to the occupation fraction in two studies that model DCBHs, the simulation of Tremmel et al (2017), and the semi-analytical model by Hartwig et al (2016). Occupation fractions are unpublished, but the authors provided us with their values, and the results are similar to the rescaled/shifted valued we estimated.…”

Section: Luminosity Functions and Dependence On "Seed" Bh Propertiesmentioning

confidence: 77%

High-redshift Galaxies and Black Holes Detectable with the JWST: A Population Synthesis Model from Infrared to X-Rays

Volonteri

Reines

Atek

et al. 2017

ApJ

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The first billion years of the Universe has been a pivotal time: stars, black holes (BHs), and galaxies formed and assembled, sowing the seeds of galaxies as we know them today. Detecting, identifying, and understanding the first galaxies and BHs is one of the current observational and theoretical challenges in galaxy formation. In this paper we present a population synthesis model aimed at galaxies, BHs, and active galactic nuclei (AGNs) at high redshift. The model builds a population based on empirical relations. The spectral energy distribution of galaxies is determined by age and metallicity, and that of AGNs by BH mass and accretion rate. We validate the model against observations, and predict properties of galaxies and AGN in other wavelength and/or luminosity ranges, estimating the contamination of stellar populations (normal stars and high-mass X-ray binaries) for AGN searches from the infrared to X-rays, and vice versa for galaxy searches. For high-redshift galaxies with stellar ages 1 Gyr < , we find that disentangling stellar and AGN emission is challenging at restframe UV/optical wavelengths, while high-mass X-ray binaries become more important sources of confusion in X-rays. We propose a color-color selection in the James Webb Space Telescope bands to separate AGN versus star-dominated galaxies in photometric observations. We also estimate the AGN contribution, with respect to massive, hot, and metal-poor stars, at driving high-ionization lines, such as C IV and He II. Finally, we test the influence of the minimum BH mass and occupation fraction of BHs in low-mass galaxies on the restframe UV/near-IR and X-ray AGN luminosity function.

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Section: Luminosity Functions and Dependence On "Seed" Bh Propertiesmentioning

confidence: 77%

High-redshift Galaxies and Black Holes Detectable with the JWST: A Population Synthesis Model from Infrared to X-Rays

Volonteri

Reines

Atek

et al. 2017

ApJ

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“…Recent modeling efforts have demonstrated that a nearby galaxy may well have produced a high enough level of LW radiation to induce the formation of a DCBH in this galaxy and that the nebular emission could be explained by an accreting BH with a mass consistent with formation as a DCBH (e.g. Pallottini et al 2015;Agarwal et al 2016c;Hartwig et al 2016;Smidt et al 2016;Smith et al 2016;Dijkstra et al 2016a). 3 In suggesting that the critical LW flux may be lower than previously thought, our results lend support to DCBH scenario for the origin of CR7.…”

Section: Discussionmentioning

confidence: 99%

“…Sobral et al 2015;Visbal et al 2016; see also Johnson 2010), is dubious since it is unknown how a sufficiently high mass of Population III stars could be assembled rapidly enough to explain the observed extremely bright emission (e.g. Hartwig et al 2016;Yajima & Khochfar 2016;Xu et al 2016;Visbal et al 2017). …”

Section: Discussionmentioning

confidence: 99%

Enhanced direct collapse due to Lyman α feedback

Johnson

Dijkstra

2017

A&A

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We assess the impact of trapped Lyman α cooling radiation on the formation of direct collapse black holes (DCBHs). We apply a one-zone chemical and thermal evolution model, accounting for the photodetachment of H − ions, precursors to the key coolant H 2 , by Lyman α photons produced during the collapse of a cloud of primordial gas in an atomic cooling halo at high redshift. We find that photodetachment of H − by trapped Lyman α photons may lower the level of the H 2 -dissociating background radiation field required for DCBH formation substantially, dropping the critical flux by up to a factor of a few. This translates into a potentially large increase in the expected number density of DCBHs in the early Universe, and supports the view that DCBHs may be the seeds for the BHs residing in the centers of a significant fraction of galaxies today. We find that detachment of H − by Lyman α has the strongest impact on the critical flux for the relatively high background radiation temperatures expected to characterize the emission from young, hot stars in the early Universe. This lends support to the DCBH origin of the highest redshift quasars.

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“…Since the first detection of GW150914, several investigations have examined how double black hole binaries could have been produced from the evolution of massive stars, whether from classical isolated evolution in low-metallicity environments (Belczynski et al 2016a;Eldridge & Stanway 2016); via the aid of rapid rotation and hence homogeneous chemical evolution Woosley 2016); via Population III stars (Hartwig et al 2016;Inayoshi et al 2016;Dvorkin et al 2016); or from dynamical formation in interacting environments (Mapelli 2016;Rodriguez et al 2016). Other more exotic scenarios have been introduced and discussed in the context of GW150914; dark matter primordial BH-BH formation (Sasaki et al 2016;Eroshenko 2016), formation of a BH-BH merger from a divided core of a massive rapidly rotating single star (Loeb 2016), or formation of BH-BH mergers with disks around BHs formed from fallback material in weak supernova explosions (Perna et al 2016).…”

Section: Introductionmentioning

confidence: 99%

The effect of pair-instability mass loss on black-hole mergers

Belczyński

Heger

Gładysz

et al. 2016

A&A

438

426

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Context. Mergers of two stellar origin black holes are a prime source of gravitational waves and are under intensive investigation. One crucial ingredient in their modeling has been neglected: pair-instability pulsation supernovae with associated severe mass loss may suppress the formation of massive black holes, decreasing black hole merger rates for the highest black hole masses. Aims. We demonstrate the effects of pair-instability pulsation supernovae on merger rate and mass using populations of double black hole binaries formed through the isolated binary classical evolution channel. Methods. The mass loss from pair-instability pulsation supernova is estimated based on existing hydrodynamical calculations. This mass loss is incorporated into the StarTrack population synthesis code. StarTrack is used to generate double black hole populations with and without pair-instability pulsation supernova mass loss. Results. The mass loss associated with pair-instability pulsation supernovae limits the Population I/II stellar-origin black hole mass to 50 M ⊙ , in tension with earlier predictions that the maximum black hole mass could be as high as 100 M ⊙ . In our model, neutron stars form with mass 1-2 M ⊙ , then we encounter the first mass gap at 2-5 M ⊙ with an absence of compact objects due to rapid supernova explosions, followed by the formation of black holes with mass 5-50 M ⊙ , with a second mass gap at 50-135 M ⊙ created by pairinstability pulsation supernovae and by pair-instability supernovae. Finally, black holes having masses above 135 M ⊙ may potentially form to arbitrarily high mass limited only by the extent of the initial mass function and the strength of stellar winds. Suppression of double black hole merger rates by pair-instability pulsation supernovae is negligible for our evolutionary channel. Our standard evolutionary model with the inclusion of pair-instability pulsation supernovae and pair-instability supernovae is fully consistent with the LIGO observations of black hole mergers: GW150914, GW151226, and LVT151012. The LIGO results are inconsistent with high ( 400 km s −1 ) BH natal kicks. We predict the detection of several, and up to as many as ∼ 60, BH-BH mergers with a total mass of 10-150 M ⊙ (most likely range: 20-80 M ⊙ ) in the forthcoming ∼ 60 effective days of the LIGO O2 observations, assuming the detectors reach the optimistic target O2 sensitivity. Conclusions.

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Exploring the nature of the Lyman-α emitter CR7

Cited by 48 publications

References 180 publications

High-redshift Galaxies and Black Holes Detectable with the JWST: A Population Synthesis Model from Infrared to X-Rays

High-redshift Galaxies and Black Holes Detectable with the JWST: A Population Synthesis Model from Infrared to X-Rays

Enhanced direct collapse due to Lyman α feedback

The effect of pair-instability mass loss on black-hole mergers

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