The Early Growth of the First Black Holes

Johnson, Jarrett L.; Haardt, Francesco

doi:10.1017/pasa.2016.4

Cited by 62 publications

(51 citation statements)

References 190 publications

(312 reference statements)

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“…Different classes of theories have been proposed to explain the formation of the BH seeds that eventually became SMBH, the two most promising ones involving "light seeds" (M ∼ 10 2 M ), as remnants of the first Pop III stars, and "heavy seeds" (M ∼ 10 4−6 M ), perhaps formed during the direct collapse of giant pristine gas clouds (e.g. Haiman 2013;Johnson & Haardt 2016;Volonteri et al 2016b, and references therein). To match the masses of SMBH discovered at z > 6, all such models require continuous nearly Eddington-limited or even super-Eddington accretion phases during which the growing SMBH is plausibly buried in material with large column densities, even exceeding the Compton-thick level (e.g.…”

Section: Introductionmentioning

confidence: 99%

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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Section: Introductionmentioning

confidence: 99%

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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“…For instance, they are unique environments to study the interplay between stellar dynamics and stellar evolution, they host multiple stellar populations, they are nurseries of high frequency gravitationalwave sources (Benacquista & Downing 2013;Rodriguez et al 2018;Choksi et al 2018), and some of them may host an intermediate mass black hole (IMBH) at their centre (Miller & Hamilton 2002). IMBHs are the black holes with mass between 10 2 − 10 5 M , which are considered the missing link between the less massive stellar black holes and the supermassive black holes found in the centre of galaxies as they are often referred as seeds upon which super-massive black holes have grown (Volonteri 2010;Latif & Ferrara 2016;Johnson & Haardt 2016;Mezcua 2017 IMBHs has been matter of debate for a long time (Bahcall & Ostriker 1975). Dense stellar systems like GCs could be breeding grounds for the formation of IMBHs, via stellar collisions or gravitational encounters among stellar black holes followed by mergers (Miller & Hamilton 2002;Portegies Zwart & McMillan 2002;Gürkan et al 2004; Portegies Zwart et al 2004;Giersz et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Intermediate mass black holes in globular clusters: effects on jerks and jounces of millisecond pulsars

Abbate

Spera

Colpi

2019

Monthly Notices of the Royal Astronomical Society

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Globular clusters may host intermediate mass black holes (IMBHs) at their centres.Here we propose a new method for their identification using millisecond pulsars (MSPs) as probes. We show that measuring the first (jerk) and second (jounce) derivatives of the accelerations of an ensemble of MSPs will let us infer the presence of an IMBH in a globular cluster better than measuring the sole accelerations. We test this concept by simulating a set of star clusters with and without a central IMBH to extract the distributions of the stellar jerks and jounces. We then apply this technique to the ensemble of MSPs in the Galactic globular cluster 47 Tucanae. Current timing observations are insufficient to constrain the presence of an IMBH and can only be used to pose upper limits on its mass. But, with few more years of observations it will be possible to test for the presence of a central IMBH with mass smaller than ∼ 1000 M . We conclude that jerks and jounces help significantly in reducing the upper limit of the mass of IMBHs in Galactic globular clusters.

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“…This has important implications as the detection of a blazar implies the existence of 2Γ 2 such sources (where Γ∼10-15; e.g., Sikora et al 1997) with misaligned jets at the same redshift, hosting similarly massive black holes. Therefore a detailed study of MeV blazars, hosting extremely massive black holes, places useful constraints on the high end of the black hole mass function, which is essential for a full theoretical understanding of the growth and evolution of black holes over cosmic time (e.g., Johnson & Haardt 2016). This can be accomplished by adopting a multiwavelength approach and utilizing data from a variety of instruments.…”

Section: Introductionmentioning

confidence: 99%

High-redshift Blazars through NuSTAR Eyes

Marcotulli¹,

Paliya²,

Ajello³

et al. 2017

ApJ

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The most powerful sources among the blazar family are MeV blazars. Often detected at z>2, they usually display high X-and γ-ray luminosities, larger-than-average jet powers, and black hole masses 10 9 M ☉ . In the present work, we perform a multiwavelength study of three high-redshift blazars: 3FGL J0325.5+2223 (z = 2.06), 3FGL J0449.0+1121 (z = 2.15), and 3FGL J0453.2−2808 (z = 2.56), analyzing quasi-simultaneous data from GROND, Swift-UVOT and XRT, Nuclear Spectroscopic Telescope Array (NuSTAR), and Fermi-LAT. Our main focus is on the hard X-ray band recently unveiled by NuSTAR(3-79 keV) where these objects show a hard spectrum that enables us to constrain the inverse Compton (IC) peak and the jet power. We found that all three targets resemble the most powerful blazars, with the synchrotron peak located in the submillimeter range and the IC peak in the MeV range, and therefore belong to the MeV blazar class. Using a simple one-zone leptonic emission model to reproduce the spectral energy distributions, we conclude that a simple combination of synchrotron and accretion disk emission reproduces the infrared-optical spectra, while the X-ray to γ-ray part is well reproduced by the IC scattering of low-energy photons supplied by the broad-line region. The black hole masses for each of the three sources are calculated to be 4×10 8 M ☉ . The three studied sources have jet power at the level of, or beyond, the accretion luminosity.

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The Early Growth of the First Black Holes

Cited by 62 publications

References 190 publications

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

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

Intermediate mass black holes in globular clusters: effects on jerks and jounces of millisecond pulsars

High-redshift Blazars through NuSTAR Eyes

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