Extreme primordial black holes

Chongchitnan, Siri; Chantavat, Teeraparb; Zunder, Jenna

doi:10.1002/asna.202113826

Cited by 5 publications

(2 citation statements)

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“…This translates to a number count of 𝑁 10 3 objects in 10 < 𝑧 < 20. Such an abundance of massive Pop III stars is ideal for seeding massive black holes at high redshifts, in addition to black holes of primordial origin (Chongchitnan et al 2021).…”

Section: Extreme Pop III Starsmentioning

confidence: 99%

The most massive Population III stars

Chantavat

Chongchitnan

Silk

2023

Monthly Notices of the Royal Astronomical Society

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Recent data from the James Webb Space Telescope suggest that there are realistic prospects for detecting the earliest generation of stars at redshift ∼20. These metal-poor, gaseous Population III (Pop III) stars are likely in the mass range 10 − 103 M⊙. We develop a framework for calculating the abundances of Pop III stars as well as the distribution of the most massive Pop III stars based on an application of extreme-value statistics. Our calculations use the star formation rate density from a recent simulation to calibrate the star-formation efficiency from which the Pop III stellar abundances are derived. Our extreme-value modelling suggests that the most massive Pop III stars at redshifts 10 < z < 20 are likely to be ≳ 103 − 104 M⊙. Such extreme Pop III stars were sufficiently numerous to be the seeds of supermassive black holes at high redshifts and possibly source detectable gravitational waves. We conclude that the extreme-value formalism provides an effective way to constrain the stellar initial mass function.

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Section: Extreme Pop III Starsmentioning

confidence: 99%

The most massive Population III stars

Chantavat

Chongchitnan

Silk

2023

Monthly Notices of the Royal Astronomical Society

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“…Beyond the application to PBH spin discussed in this work, the POT formalism is applicable to other contexts wherever the rarity of extreme objects is to be quantified, e.g., extreme-mass clusters or extreme-radius cosmic voids. An alternative extreme-value technique (the "exact" formulation of extreme-value statistics) was applied to these problems in [41][42][43], but it would be interesting to see what the POT formalism could add to previous findings. The SAS transformation, in the case of massive clusters and voids, would also translate directly to primordial non-Gaussianities that affect the skewness and kurtosis of the pdf of primordial overdensities [44].…”

Section: B Further Astrophysical Applications Of Evsmentioning

confidence: 99%

Extreme-value statistics of the spin of primordial black holes

Chongchitnan

Silk

2021

Phys. Rev. D

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How rare are extreme-spin primordial black holes? We show how, from an underlying distribution of primordial black hole (PBH) spin, extreme-value statistics can be used to quantify the rarity of spinning PBHs with Kerr parameter close to 1. Using the peaks-over-threshold method, we show how the probability that a PBH forms with spin exceeding a sufficiently high threshold can be calculated using the generalized Pareto distribution. This allows us to estimate the average number of PBHs amongst which we can find a single PBH that formed with spin exceeding a high threshold. We found that the primordial spin distribution gives rise to exceedingly rare near-extremal spin PBHs at formation time: for typical parameter values, roughly up to one in a hundred million PBHs would be formed with spin exceeding the Thorne limit. We discuss conditions under which even more extreme-spin PBHs may be produced, including modifying the skewness and kurtosis of the spin distribution via a smooth transformation. We deduce from our calculations that, if indeed asteroid-mass PBHs above the current observational limit on evaporating PBHs of mass ∼10 17 g contribute significantly to the dark matter, it is very likely that some of them at somewhat lower masses could be long-lived near-extremal PBHs.

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Extreme-value modelling of the brightest galaxies at z ≳ 9

Heather,

Chantavat,

Chongchitnan

et al. 2024

Monthly Notices of the Royal Astronomical Society

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Data from the JWST have revealed an intriguing population of bright galaxies at high redshifts. In this work, we use extreme-value statistics to calculate the distribution [in ultraviolet (UV) magnitude] of the brightest galaxies in the redshift range $9 \lesssim z \lesssim 16$. We combine the generalized extreme-value approach with modelling of the galaxy luminosity function. We obtain predictions of the brightest galaxies for a suite of luminosity functions, including the Schechter and double power-law functions, as well as a model parametrized by the stellar formation efficiency $f_*$. We find that the JWST data are broadly consistent with $f_*$ of $5\!\!-\!\!10{{\ \rm per\, cent}}$, and that the brightest galaxy at $z\sim 16$ will have $M_{\rm UV}\approx -23.5^{0.8}_{0.4}$. If $f_*$ is dependent on halo mass, we predict $M_{\rm UV}\approx -22.5^{0.5}_{1.5}$ for such an object. We show that extreme-value statistics not only predict the magnitude of the brightest galaxies at high redshifts, but may also be able to distinguish between models of star formation in high-redshift galaxies.

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Extreme primordial black holes

Cited by 5 publications

References 50 publications

The most massive Population III stars

The most massive Population III stars

Extreme-value statistics of the spin of primordial black holes

Extreme-value modelling of the brightest galaxies at z ≳ 9

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