On the number density of ‘direct collapse’ black hole seeds

Habouzit, Mélanie; Volonteri, Marta; Latif, Muhammad; Dubois, Yohan; Peirani, Sébastien

doi:10.1093/mnras/stw1924

Cited by 145 publications

(202 citation statements)

References 66 publications

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“…It is encouraging to note that our number densities only differ from previous works (Agarwal et al 2012;Dijkstra et al 2014;Habouzit et al 2016) by less than one order of magnitude for a chosen Jcrit value. This difference could arise from a number of assumptions made in this work including: only assuming the starting leaves of a given halo to be pristine and using simple analytic estimates to account for a clustering-induced enhancement of the LW background seen by a galaxy.…”

Section: Conclusion and Discussionsupporting

confidence: 54%

“…Agarwal et al 2012;Dijkstra et al 2014;Habouzit et al 2016). Given that the LW background produced by a galaxy dominates within the threshold radius, it might be expected that galaxies with a larger halo mass will have a higher probability of attaining P thres .…”

Section: Redshift-evolution Of the Lw Background And Implications Formentioning

confidence: 99%

“…First postulated as massive (10 5−6 M ) black hole seeds, to explain the presence of super-massive black holes (SMBH) at early cosmic epochs (e.g. Loeb & Rasio 1994;Bromm & Loeb 2003), DCBH formation scenarios have been continually refined and developed over the past years (e.g Begelman et al 2006;Regan & Haehnelt 2009;Shang et al 2010;Johnson et al 2012;Latif et al 2013;Agarwal et al 2014;Dijkstra et al 2014;Ferrara et al 2014;Habouzit et al 2016). This field has been lent impetus by the possible, albeit highly debated (Sobral et al 2015;Bowler et al 2017), detection of a DCBH (Agarwal et al 2016;Hartwig et al 2016;Smith et al 2016;Pacucci et al 2017) in the Lyman Alpha Emitting "CR7" galaxy at z ∼ 7.…”

Section: Introductionmentioning

confidence: 99%

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Warm dark matter constraints from high-z direct collapse black holes using the JWST

Dayal

Choudhury

Pacucci

2017

Monthly Notices of the Royal Astronomical Society

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We use a semi-analytic model, Delphi, that jointly tracks the dark matter and baryonic assembly of high-redshift (z 4−20) galaxies to gain insight on the number density of Direct Collapse Black Hole (DCBH) hosts in three different cosmologies: the standard Cold Dark Matter (CDM) model and two Warm Dark Matter (WDM) models with particle masses of 3.5 and 1.5 keV. Using the Lyman-Werner (LW) luminosity of each galaxy from Delphi we use a clustering bias analysis to identify all, pristine halos with a virial temperature T vir > ∼ 10 4 K that are irradiated by a LW background above a critical value as, DCBH hosts. In good agreement with previous studies, we find the DCBH number density rises from ∼ 10 −6.1 to ∼ 10 −3.5 cMpc −3 from z 17.5 to 8 in the CDM model using a critical LW background value of 30J 21 (where J 21 = 10 −21 erg s −1 Hz −1 cm −2 sr −1 ). We find that a combination of delayed structure formation and an accelerated assembly of galaxies results in a later metalenrichment and an accelerated build-up of the LW background in the 1.5 keV WDM model, resulting in DCBH hosts persisting down to much lower redshifts (z 5) as compared to CDM where DCBH hosts only exist down to z 8. We end by showing how the expected colours in three different bands of the Near Infrared Camera (NIRCam) onboard the forthcoming James Webb Space Telescope can be used to hunt for potential z 5 − 9 DCBHs, allowing hints on the WDM particle mass.

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Section: Conclusion and Discussionsupporting

confidence: 54%

Section: Redshift-evolution Of the Lw Background And Implications Formentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Warm dark matter constraints from high-z direct collapse black holes using the JWST

Dayal

Choudhury

Pacucci

2017

Monthly Notices of the Royal Astronomical Society

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“…At higher redshifts the Buchner et al (2015) region exceeds our results. Similarly, the simulated XLFs by Habouzit et al (2016) appear to over-predict the density of low-luminosity AGN. Giallongo et al (2015) applied a detection procedure based on searching for clustering of photons in energy, space, and time, at the pre-determined optical positions of CANDELS-detected galaxies (see also Fiore et al 2012), which allowed the authors to push the Chandra sensitivity beyond the limit reachable by blind detection methods (i.e., with no previous knowledge of the positions of galaxies).…”

Section: The Agn Xlf At High Redshiftmentioning

confidence: 88%

High-redshift AGN in the Chandra Deep Fields: the obscured fraction and space density of the sub-L* population

Vito

Brandt

Yang

et al. 2017

Monthly Notices of the Royal Astronomical Society

164

184

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We investigate the population of high-redshift (3 z < 6) AGN selected in the two deepest X-ray surveys, the 7 Ms Chandra Deep Field-South and 2 Ms Chandra Deep Field-North. Their outstanding sensitivity and spectral characterization of faint sources allow us to focus on the sub-L * regime (logL X 44), poorly sampled by previous works using shallower data, and the obscured population. Taking fully into account the individual photometric-redshift probability distribution functions, the final sample consists of ≈ 102 X-ray selected AGN at 3 z < 6. The fraction of AGN obscured by column densities logN H > 23 is ∼ 0.6 − 0.8, once incompleteness effects are taken into account, with no strong dependence on redshift or luminosity. We derived the high-redshift AGN number counts down to F 0.5−2 keV = 7 × 10 −18 erg cm −2 s −1 , extending previous results to fainter fluxes, especially at z > 4. We put the tightest constraints to date on the low-luminosity end of AGN luminosity function at high redshift. The space-density, in particular, declines at z > 3 at all luminosities, with only a marginally steeper slope for low-luminosity AGN. By comparing the evolution of the AGN and galaxy densities, we suggest that such a decline at high luminosities is mainly driven by the underlying galaxy population, while at low luminosities there are hints of an intrinsic evolution of the parameters driving nuclear activity. Also, the black-hole accretion rate density and star-formation rate density, which are usually found to evolve similarly at z 3, appear to diverge at higher redshifts.

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“…The gas is more metal-enriched, therefore the number of BHs that formed is reduced, and ends up being similar to the T simulation. The metal enrichment of the T and D simulations is discussed in Habouzit et al (2016a) (Fig. 2).…”

Section: The Influence Of Star Formation and Metallicity On Bh Formationmentioning

confidence: 99%

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

Habouzit

Volonteri²,

Dubois³

2017

Monthly Notices of the Royal Astronomical Society

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245

223

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Massive black holes (BHs) inhabit local galaxies, including the Milky Way and some dwarf galaxies. BH formation, occurring at early cosmic times, must account for the properties of BHs in today's galaxies, notably why some galaxies host a BH, and others do not. We investigate the formation, distribution and growth of BH 'seeds' by using the adaptive mesh refinement code Ramses. We develop an implementation of BH formation in dense, low-metallicity environments, as advocated by models invoking the collapse of the first generation of stars, or of dense nuclear star clusters. The seed masses are computed one-by-one on-the-fly, based on the star formation rate and the stellar initial mass function. This self-consistent method to seed BHs allows us to study the distribution of BHs in a cosmological context and their evolution over cosmic time. We find that all high-mass galaxies tend to host a BH, whereas low-mass counterparts have a lower probability of hosting a BH. After the end of the epoch of BH formation, this probability is modulated by the growth of the galaxy. The simulated BHs connect to low-redshift observational samples, and span a similar range in accretion properties as Lyman-Break Analogs. The growth of BHs in low-mass galaxies is stunted by strong supernova feedback. The properties of BHs in dwarf galaxies thus remain a testbed for BH formation. Simulations with strong supernova feedback, which is able to quench BH accretion in shallow potential wells, produce galaxies and BHs in better agreement with observational constraints.

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On the number density of ‘direct collapse’ black hole seeds

Cited by 145 publications

References 66 publications

Warm dark matter constraints from high-z direct collapse black holes using the JWST

Warm dark matter constraints from high-z direct collapse black holes using the JWST

High-redshift AGN in the Chandra Deep Fields: the obscured fraction and space density of the sub-L* population

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

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