Supercritical growth pathway to overmassive black holes at cosmic dawn: coevolution with massive quasar hosts

Hu, Haojie; Inayoshi, Kohei; Haiman, Zoltán; Li, Wenxiu; Quataert, Eliot; Kuiper, Rolf

doi:10.48550/arxiv.2204.12513

Cited by 3 publications

(3 citation statements)

References 42 publications

(54 reference statements)

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“…be produced unless we enhance the maximum allowed accretion rate (by factors 10) within these extreme overdense regions by either increasing the Eddington factor or decreasing the radiative efficiency. Notably, this result is consistent with the recent work of (Hu et al 2022) which uses semi-analytic approach to produce z ∼ 6 quasars using super-Eddington accretion, from both light (10 M ) and heavy seeds (10 5 M ).…”

Section: Implications For Strongly Restrictive Seed Models In Produci...supporting

confidence: 91%

Probing the $z\gtrsim6$ quasars in a universe with IllustrisTNG physics: Impact of gas-based black hole seeding models

Bhowmick,

Blecha,

et al. 2022

Preprint

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We explore the implications of a range of black hole (BH) seeding prescriptions on the formation of the brightest z 6 quasars in cosmological hydrodynamic simulations. The underlying galaxy formation model is the same as in the IllustrisTNG simulations. Using initial conditions generated in constrained Gaussian realizations, we study the growth of BHs in rare overdense regions (forming 10 12 M /h halos by z = 7) using a (9 Mpc/h) 3 simulated volume. BH growth is maximal within halos that are compact and have a low tidal field. For these halos, we consider an array of gas-based seeding prescriptions wherein M seed = 10 4 − 10 6 M /h seeds are inserted in halos above critical thresholds for halo mass and dense, metal-poor gas mass (defined as Mh and Msf,mp , respectively, in units of M seed ). We find that a seed model with Msf,mp = 5 and Mh = 3000 successfully produces a z ∼ 6 quasar with ∼ 10 9 M mass and ∼ 10 47 ergs s −1 luminosity. BH mergers play a crucial role at z 9, causing an early boost in BH mass at a time when accretion-driven BH growth is negligible. When more stringent seeding conditions are applied (e.g., Msf,mp = 1000), the relative paucity of BH seeds results in a much lower merger rate. In this case, z 6 quasars can only be formed if we enhance the maximum allowed BH accretion rates (by factors 10) compared to the accretion model used in IllustrisTNG. This can be achieved either by allowing for super-Eddington accretion, or by reducing the radiative efficiency. Our results demonstrate that progenitors of z ∼ 6 quasars have distinct BH merger histories for different seeding models, which will be distinguishable with LISA observations.

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Section: Implications For Strongly Restrictive Seed Models In Produci...supporting

confidence: 91%

Probing the $z\gtrsim6$ quasars in a universe with IllustrisTNG physics: Impact of gas-based black hole seeding models

Bhowmick,

Blecha,

et al. 2022

Preprint

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“…In conclusion, the upcoming JWST observations, with the aid of physically motivated selection criteria, will be able to improve the detection efficiency of fast-growing seed BHs. The discovery of such unique objects will prove that seed BHs had experienced super-Eddington growth early on (Inayoshi et al 2022;Hu et al 2022), offering a path toward explaining the population of overmassive BHs seen in high-z quasars (e.g., Izumi et al 2021). Observations of such BHs and their host galaxies will be a milestone in revealing how coevolution between BHs and host galaxies has been established at cosmic dawn (Habouzit et al 2022).…”

Section: Discussionmentioning

confidence: 97%

The Age of Discovery with the James Webb Space Telescope: Excavating the Spectral Signatures of the First Massive Black Holes

Inayoshi

Onoue

Sugahara

et al. 2022

ApJL

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The James Webb Space Telescope (JWST) will open a new window into the most distant universe and unveil the early growth of supermassive black holes (BHs) in the first galaxies. In preparation for deep JWST imaging surveys, it is crucial to understand the color selection of high-redshift accreting seed BHs. We model the spectral energy distribution of super-Eddington accreting BHs with millions of solar masses in metal-poor galaxies at z ≳ 8, applying postprocess line transfer calculations to radiation hydrodynamical simulation results. Exposures of 10 ks with the NIRCam and MIRI broadband filters are sufficient to detect the radiation flux from the seed BHs with bolometric luminosities of L bol ≃ 1045 erg s−1. While the continuum colors are similar to those of typical low-z quasars, strong Hα line emission with a rest-frame equivalent width EWrest ≃ 1300 Å is so prominent that the line flux affects the broadband colors significantly. The unique colors, for instance, F356W − F560W ≳ 1 at 7 < z < 8 and F444W − F770W ≳ 1 at 9 < z < 12, provide robust criteria for photometric selection of rapidly growing seed BHs. Moreover, NIRSpec observations of low-ionization emission lines can test whether the BH is fed via a dense accretion disk at super-Eddington rates.

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“…We have so far assumed Eddington-limited black hole growth, though mass inflow rates could permit super-Eddington accretion. Hu et al (2022a) and Hu et al (2022b) have recently explored BH accretion when the large-scale feeding rate is substantially higher than 𝑀 Edd [≡ 𝐿 Edd /(𝜖 𝑐 2 )] in radiation-hydrodynamics simulations. They find, consistent with earlier results (Jiang et al 2014;Sądowski et al 2014;Inayoshi et al 2016;Toyouchi et al 2021), that when the external gas supply rate 𝑀 0 exceeds the Eddington rate, photons trapped in the dense flow produce strong outflows which then decrease the mass inflow rate with distance 𝑟 from the black hole as ∝ 𝑟 𝑝 with 𝑝 ∼ 0.5 -0.7.…”

Section: An Alternative Model For Bh Growthmentioning

confidence: 99%

How long do high-redshift massive black hole seeds remain outliers in black hole vs. host galaxy relations?

Scoggins¹,

Haiman²,

Wise³

2022

Preprint

Self Cite

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The existence of 10 9 M supermassive black holes (SMBHs) within the first billion years of the universe remains a puzzle in our conventional understanding of black hole formation and growth. The so-called direct-collapse scenario suggests that the formation of supermassive stars (SMSs) can yield the massive seeds of early SMBHs. This scenario leads to an overly massive BH galaxy (OMBG), whose nuclear black hole's mass is comparable to or even greater than the surrounding stellar mass: a 10 4 − 10 6 M seed black hole is born in a dark matter halo with a mass as low as 10 7 − 10 8 M . The black hole to stellar mass ratio is 𝑀 bh /𝑀 * 10 −3 , well in excess of the typical values at lower redshift. We investigate how long these newborn BHs remain outliers in the 𝑀 bh − 𝑀 * relation, by exploring the subsequent evolution of two OMBGs previously identified in the Renaissance simulations. We find that both OMBGs have 𝑀 bh /𝑀 * > 1 during their entire life, from their birth at 𝑧 ≈ 15 until they merge with much more massive haloes at 𝑧 ≈ 8. We find that the OMBGs are spatially resolvable from their more massive, 10 11 M , neighboring haloes until their mergers are complete at 𝑧 ≈ 8. This affords a window for future observations with JWST and sensitive X-ray telescopes to diagnose the direct-collapse scenario, by detecting similar OMBGs and establishing their uniquely high black hole-to-stellar mass ratio.

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Supercritical growth pathway to overmassive black holes at cosmic dawn: coevolution with massive quasar hosts

Cited by 3 publications

References 42 publications

Probing the $z\gtrsim6$ quasars in a universe with IllustrisTNG physics: Impact of gas-based black hole seeding models

Probing the $z\gtrsim6$ quasars in a universe with IllustrisTNG physics: Impact of gas-based black hole seeding models

The Age of Discovery with the James Webb Space Telescope: Excavating the Spectral Signatures of the First Massive Black Holes

How long do high-redshift massive black hole seeds remain outliers in black hole vs. host galaxy relations?

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