Black hole formation in the context of dissipative dark matter

Latif, Muhammad; Lupi, Alessandro; Schleicher, Dominik R. G.; D’Amico, Guido; Panci, Paolo; Bovino, S.

doi:10.1093/mnras/stz608

Cited by 27 publications

(26 citation statements)

References 52 publications

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“…To do so, we use the Rec-FAST++ software and the interaction-rate coefficients re-scaled by the methods derived in Ryan et al (2021a). Previous work in the mirror matter model (equivalent to atomic dark matter with r α = r m = r M = 1 for our purposes) (Latif et al 2019;D'Amico et al 2018) assumed the ratio x e /x H2 ≈ 10 2 carried over from the Standard Model, independent of the dark matter parameters. Here, we calculate the primordial molecular abundance directly and find that this assumption often fails, because the primordial molecular abundance depends not only on the primordial ionization fraction but also on the dark-particle number density at the time of molecule formation.…”

Section: Discussionmentioning

confidence: 99%

Molecular Chemistry for Dark Matter II: Recombination, Molecule Formation, and Halo Mass Function in Atomic Dark Matter

Gurian,

Jeong,

Ryan

et al. 2021

Preprint

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Dissipative dark matter predicts rich observable phenomena that can be tested with future large-scale structure surveys. As a specific example, we study atomic dark matter, consisting of a heavy particle and a light particle charged under a dark electromagnetism. In particular, we calculate the cosmological evolution of atomic dark matter focusing on dark recombination and dark-molecule formation. We have obtained the relevant interaction-rate coefficients by re-scaling the rates for normal hydrogen, and evolved the abundances for ionized, atomic, and molecular states using a modified version of RecFAST++. We also provide an analytical approximation for the final abundances. We then calculate the effects of the atomic dark matter on the linear power spectrum, which enter through a darkphoton diffusion and dark acoustic oscillations. At the formation time, the atomic dark matter model suppresses halo abundances on scales smaller than the diffusion scale, just like the warm dark matter models suppress the abundance below the free-streaming scale. The subsequent evolution with radiative cooling, however, will alter the halo mass function further.

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Section: Discussionmentioning

confidence: 99%

Molecular Chemistry for Dark Matter II: Recombination, Molecule Formation, and Halo Mass Function in Atomic Dark Matter

Gurian,

Jeong,

Ryan

et al. 2021

Preprint

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“…Another possible solution is the formation of intermediatemass BHs with masses of about 10 4 M in mildly metal-enriched nuclear stellar clusters, either via collisions between stars (Portegies Zwart & McMillan 2002;Gürkan et al 2004;Omukai et al 2008;Devecchi & Volonteri 2009;Devecchi et al 2010Devecchi et al , 2012Katz et al 2015;Boekholt et al 2018;Reinoso et al 2018;Das et al 2020;Tagawa et al 2020) or the runaway merger of stellar-mass BHs (Davies et al 2011;Miller & Davies 2012;Lupi et al 2014;Tagawa et al 2015). This range of masses is also obtained in models invoking physics beyond the standard model, for instance from the collapse of self-interacting (Balberg et al 2002;Pollack et al 2015) or other forms of dissipative dark matter (D'Amico et al 2018;Latif et al 2019). However, because of the relatively low initial mass of these seeds, it is not clear yet whether they can represent the seeds of the MBHs in high-redshift quasars.…”

Section: Introductionmentioning

confidence: 92%

Forming massive seed black holes in high-redshift quasar host progenitors

Lupi,

Haiman,

Volonteri

2021

Preprint

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The presence of massive black holes (BHs) with masses of order 10 9 M , powering bright quasars when the Universe was less than 1 Gyr old, poses strong constraints on their formation mechanism. Several scenarios have been proposed to date to explain massive BH formation, from the low-mass seed BH remnants of the first generation of stars to the massive seed BHs resulting from the rapid collapse of massive gas clouds. However, the plausibility of some of these scenarios to occur within the progenitors of high-z quasars has not yet been thoroughly explored. In this work, we investigate, by combining dark-matter only N-body simulations with a semi-analytic framework, whether the conditions for the formation of massive seed BHs from synchronised atomic-cooling halo pairs and/or dynamically-heated mini-haloes are fulfilled in the overdense regions where the progenitors of a typical high-redshift quasar host form and evolve. Our analysis shows that the peculiar conditions in such regions, i.e. strong halo clustering and high star formation rates, are crucial to produce a non-negligible number of massive seed BH host candidates: we find ≈ 1400 dynamically heated metal-free mini-haloes, including one of these which evolves to a synchronised pair and ends up in the massive quasarhost halo by 𝑧 = 6. This demonstrates that the progenitors of high-redshift quasar host haloes can harbour early massive seed BHs. Our results further suggest that multiple massive seed BHs may form in or near the quasar host's progenitors, potentially merging at lower redshifts and yielding gravitational wave events.

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“…Finally, these subroutines can be embedded as a library in any hydrodynamics code. It has been successfully employed to study a variety of problems (environments and processes) as: black holes (Latif et al 2019), SF activity (Lupi et al 2018;Lupi & Bovino 2020), metal and molecular chemistry in galaxies and filaments (Bovino et al 2016;Capelo et al 2018;Seifried et al 2017), first-stars (Latif & Schleicher 2015;Sharda et al 2019), etc.…”

Section: Main Characteristics Of the Chemistry Package Kromementioning

confidence: 99%

Modelling H$_2$ and its effects on star formation using a joint implementation of GADGET-3 and KROME

Sillero,

Tissera,

Lambas

et al. 2021

Preprint

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We present P-GADGET3-K, an updated version of GADGET3, that incorporates the chemistry package KROME. P-GADGET3-K follows the hydrodynamical and chemical evolution of cosmic structures, incorporating the chemistry and cooling of H 2 and metal cooling in non-equilibrium. We performed different runs of the same ICs to assess the impact of various physical parameters and prescriptions, namely gas metallicity, molecular hydrogen formation on dust, star formation recipes including or not H 2 dependence, and the effects of numerical resolution. We find that the characteristics of the simulated systems, both globally and at kpc-scales, are in good agreement with several observable properties of molecular gas in star-forming galaxies. The surface density profiles of SFR and H 2 are found to vary with the clumping factor and resolution. In agreement with previous results, the chemical enrichment of the gas component is found to be a key ingredient to model the formation and distribution of H 2 as a function of gas density and temperature. A SF algorithm that takes into account the H 2 fraction together with a treatment for the local stellar radiation field improves the agreement with observed H 2 abundances over a wide range of gas densities and with the molecular Kennicutt-Schmidt law, implying a more realistic modelling of the star formation process.

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Black hole formation in the context of dissipative dark matter

Cited by 27 publications

References 52 publications

Molecular Chemistry for Dark Matter II: Recombination, Molecule Formation, and Halo Mass Function in Atomic Dark Matter

Molecular Chemistry for Dark Matter II: Recombination, Molecule Formation, and Halo Mass Function in Atomic Dark Matter

Forming massive seed black holes in high-redshift quasar host progenitors

Modelling H$_2$ and its effects on star formation using a joint implementation of GADGET-3 and KROME

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