The Emergence of the First Star-free Atomic Cooling Haloes in the Universe

Abstract

Using the Renaissance suite of simulations we examine the emergence of pristine atomic cooling haloes that are both metal-free and star-free in the early Universe. The absence of metals prevents catastrophic cooling, suppresses fragmentation, and may allow for the formation of massive black hole seeds. Here we report on the abundance of pristine atomic cooling haloes found and on the specific physical conditions that allow for the formation of these direct-collapse-black-hole (DCBH) haloes. In total in our simulations we find that 79 DCBH haloes form before a redshift of 11.6. We find that the formation of pristine atomic haloes is driven by the rapid assembly of the atomic cooling haloes with mergers, both minor and/or major, prior to reaching the atomic cooling limit a requirement. However, the ability of assembling haloes to remain free of (external) metal enrichment is equally important and underlines the necessity of following the transport of metals in such simulations. The candidate DCBH hosting haloes we find, have been exposed to mean Lyman-Werner radiation fields of J${}_{LW}$ $\sim$ 1 J${}_{21}$ and typically lie at least 10 kpc (physical) from the nearest massive galaxy. Growth rates of the haloes reach values of greater than 10${}^7$ M${}_{\odot }$ per unit redshift, leading to significant dynamical heating and the suppression of efficient cooling until the halo crosses the atomic cooling threshold. Finally, we also find five synchronised halo candidates where pairs of pristine atomic cooling haloes emerge that are both spatially and temporally synchronised.

Minor updates after acceptance by MNRAS

References in corpus (33)

• A luminous quasar at a redshift of z = 7.085
• Formation of Supermassive Black Holes by Direct Collapse in Pregalactic Halos
• Observational constraints on Cosmic Reionization
• An ultra-luminous quasar with a twelve-billion-solar-mass black hole at redshift 6.30
• Formation of the first nuclear clusters and massive black holes at high redshift
• Accretion onto the First Stellar Mass Black Holes
• Fluctuations in the High-Redshift Lyman-Werner Background: Close Halo Pairs as the Origin of Supermassive Black Holes
• Population III star formation in a Lambda CDM universe, II: Effects of a photodissociating background
• Formation of massive black holes in rapidly growing pre-galactic gas clouds
• Resolving the Formation of Protogalaxies. II. Central Gravitational Collapse
• Rapid growth of seed black holes in the early universe by supra-exponential accretion
• Quasistars: Accreting black holes inside massive envelopes
• The Evolution of Supermassive Population III Stars
• Feedback-regulated Super Massive Black Hole Seed Formation
• The critical radiation intensity for direct collapse black hole formation: dependence on the radiation spectral shape
• Constraining the high redshift formation of black hole seeds in nuclear star clusters with gas inflows
• Accretion onto Intermediate-Mass Black Holes in Dense Protogalactic Clouds
• Direct collapse black hole formation from synchronized pairs of atomic cooling halos
• Formation of an embryonic supermassive star in the first galaxy
• The formation of compact massive self-gravitating discs in metal-free haloes with virial temperatures of ~ 13000-30000 K
• How realistic UV spectra and X-rays suppress the abundance of direct collapse black holes
• A UV flux constraint on the formation of direct collapse black holes
• The Direct Collapse of a Massive Black Hole Seed Under the Influence of an Anisotropic Lyman-Werner Source
• Conditions for Optimal Growth of Black Hole Seeds
• The Santa Fe Light Cone Simulation Project: I. Confusion and the WHIM in Upcoming Sunyaev-Zel'dovich Effect Surveys
• Revised rate coefficients for H${}_2$ and H${}^{-}$ destruction by realistic stellar spectra
• The suppression of direct collapse black hole formation by soft X-ray irradiation
• On the Rotation of Supermassive Stars
• A No-Go Theorem for Direct Collapse Black Holes Without a Strong Ultraviolet Background
• Scaling Relations for Galaxies Prior to Reionization
• Spatially Extended 21 cm Signal from Strongly Clustered UV and X-Ray Sources in the Early Universe
• Fragmentation inside atomic cooling haloes exposed to Lyman-Werner radiation
• The effect of dark matter resolution on the collapse of baryons in high redshift numerical simulations

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• Gravitational waves from Population III binary black holes formed by dynamical capture
• Light, medium-weight or heavy? The nature of the first supermassive black hole seeds
• Formation of supermassive black hole seeds in nuclear star clusters via gas accretion and runaway collisions
• Finding Direct-Collapse Black Holes at Birth
• Effect of mass loss due to stellar winds on the formation of supermassive black hole seeds in dense nuclear star clusters
• Direct-collapse black hole formation induced by internal radiation of host halos
• Conditions for direct black hole seed collapse near a radio-loud quasar 1 Gyr after the Big Bang
• Some First Stars Were Red: Detecting Signatures of Massive Population III Formation Through Long-Term Stochastic Color Variations
• Rotating Supermassive Pop III Stars On The Main Sequence
• Astrophysics with the Laser Interferometer Space Antenna
• Can supermassive stars form in protogalaxies due to internal Lyman-Werner feedback?
• Halo Mergers Enhance the Growth of Massive Black Hole Seeds
• Impact of primordial black holes on the formation of the first stars and galaxies
• Triggered Population III star formation: the effect of H${}_2$ self-shielding
• Population III Star Formation in an X-ray background: II. Protostellar Discs, Multiplicity and Mass Function of the Stars
• Direct Collapse Black Hole Candidates from Decaying Dark Matter
• Population III Star Formation in an X-ray background: I. Critical Halo Mass of Formation and Total Mass in Stars
• Rapid sinking and efficient mergers of supermassive black holes in compact high-redshift galaxies
• Radiative feedback on supermassive star formation: the massive end of the Population III initial mass function