Early formation of supermassive black holes via dark matter self-interactions

Choquette, Jeremie; Cline, James M.; Cornell, Jonathan M.

doi:10.1088/1475-7516/2019/07/036

Cited by 66 publications

(67 citation statements)

References 64 publications

(153 reference statements)

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“…Such processes can efficiently remove energy from the centres of halos and lead to halo core collapse in less than a Hubble time (Essig et al 2019;Huo et al 2020) leaving testable signatures in dwarf galaxies. They could also contribute to the formation of supermassive black holes already at high redshift (Choquette et al 2019). Note, however, that dissipative dark matter interactions are constrained by the non-detection of DM acoustic oscillations (Cyr-Racine et al 2014), and absence of a significant thin 'dark disk' in the Milky Way (Schutz et al 2018).…”

Section: Self-interacting Dark Matter (Sidm) Decaying and Dissipative...mentioning

confidence: 99%

Large-scale dark matter simulations

Angulo

Hahn

2022

Living Rev Comput Astrophys

111

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We review the field of collisionless numerical simulations for the large-scale structure of the Universe. We start by providing the main set of equations solved by these simulations and their connection with General Relativity. We then recap the relevant numerical approaches: discretization of the phase-space distribution (focusing on N-body but including alternatives, e.g., Lagrangian submanifold and Schrödinger–Poisson) and the respective techniques for their time evolution and force calculation (direct summation, mesh techniques, and hierarchical tree methods). We pay attention to the creation of initial conditions and the connection with Lagrangian Perturbation Theory. We then discuss the possible alternatives in terms of the micro-physical properties of dark matter (e.g., neutralinos, warm dark matter, QCD axions, Bose–Einstein condensates, and primordial black holes), and extensions to account for multiple fluids (baryons and neutrinos), primordial non-Gaussianity and modified gravity. We continue by discussing challenges involved in achieving highly accurate predictions. A key aspect of cosmological simulations is the connection to cosmological observables, we discuss various techniques in this regard: structure finding, galaxy formation and baryonic modelling, the creation of emulators and light-cones, and the role of machine learning. We finalise with a recount of state-of-the-art large-scale simulations and conclude with an outlook for the next decade.

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Section: Self-interacting Dark Matter (Sidm) Decaying and Dissipative...mentioning

confidence: 99%

Large-scale dark matter simulations

Angulo

Hahn

2022

Living Rev Comput Astrophys

111

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“…Given the approximate nature of our cooling estimates, one might envisage the possibility that the central black hole was formed from a mirror matter halo that collapsed relatively slowly and adiabatically within about a billion years or so, without significant mirror star formation or loss of pressure support. (A subdominant dissipative DM component that could seed central black hole production via gravithermal collapse has previously been considered, for example in [94,[136][137][138].) However, it is far beyond the scope of this paper to carefully examine this possibility.…”

Section: Jhep11(2021)198mentioning

confidence: 99%

Direct detection of mirror matter in Twin Higgs models

Chacko

Curtin

Geller

et al. 2021

J. High Energ. Phys.

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We explore the possibility of discovering the mirror baryons and electrons of the Mirror Twin Higgs model in direct detection experiments, in a scenario in which these particles constitute a subcomponent of the observed DM. We consider a framework in which the mirror fermions are sub-nano-charged, as a consequence of kinetic mixing between the photon and its mirror counterpart. We consider both nuclear recoil and electron recoil experiments. The event rates depend on the fraction of mirror DM that is ionized, and also on its distribution in the galaxy. Since mirror DM is dissipative, at the location of the Earth it may be in the form of a halo or may have collapsed into a disk, depending on the cooling rate. For a given mirror DM abundance we determine the expected event rates in direct detection experiments for the limiting cases of an ionized halo, an ionized disk, an atomic halo and an atomic disk. We find that by taking advantage of the complementarity of the different experiments, it may be possible to establish not just the multi-component nature of mirror dark matter, but also its distribution in the galaxy. In addition, a study of the recoil energies may be able to determine the masses and charges of the constituents of the mirror sector. By showing that the mass and charge of mirror helium are integer multiples of those of mirror hydrogen, these experiments have the potential to distinguish the mirror nature of the theory. We also carefully consider mirror plasma screening effects, showing that the capture of mirror dark matter particles in the Earth has at most a modest effect on direct detection signals.

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“…If the self-interaction is totally inelastic (hit-and-stick), the collapse timescale can be two orders of magnitude shorter than the prediction in elastic SIDM [45,47,48]. Therefore, totally dissipative self-interacting dark matter (tdSIDM) can greatly accelerate the catastrophic collapse of halos, which leads to the formation of SMBHs in the early universe.…”

Section: Introductionmentioning

confidence: 99%

“…However, such elastic selfinteracting dark matter (eSIDM) requires a cross-section σ/m = 5 cm 2 /g to seed SMBHs with masses 10 6 M at z ∼ 10 [33], which is now ruled out by observations of galaxy cluster collisions [44]. To avoid the constraints on the cross-section, hybrid dark matter models were proposed where the bulk of dark matter does not have any self-interaction, but a small fraction is SIDM with a large cross-section [34,45]. Alternatively, the presence of baryons in protogalaxies has also been shown to accelerate the gravothemal collapse of eSIDM halos [46] with a smaller cross-section.…”

Section: Introductionmentioning

confidence: 99%

“…Though the timescale of seeding SMBHs in an isolated tdSIDM halo was well-studied numerically using Nbody simulations [45,47], the cosmological abundance of SMBHs in the early Universe has never been calculated. For the first time, we compute the cosmological abundance of SMBHs seeded from tdSIDM halos and show this seeding mechanism can be consistent with both high redshift and low redshift observations of SMBHs.…”

Section: Introductionmentioning

confidence: 99%

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SMBH seeds from dissipative dark matter

Xiao

Shen

Hopkins

et al. 2021

J. Cosmol. Astropart. Phys.

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The existence of supermassive black holes (SMBHs) with masses greater than ∼ 10 9 M at high redshift (z 7) is difficult to be accommodated in standard astrophysical scenarios. We study the possibility that (nearly) totally dissipative self-interacting dark matter (tdSIDM)-in rare, high density dark matter fluctuations in the early Universe-produces SMBH seeds through catastrophic collapse. We use a semi-analytic model, tested and calibrated by a series of N-body simulations of isolated dark matter halos, to compute the collapse criteria and timescale of tdSIDM halos, where dark matter loses nearly all of its kinetic energy in a single collision in the center-of-momentum frame. Applying this model to halo merger trees, we empirically assign SMBH seeds to halos and trace the formation and evolution history of SMBHs. We make predictions for the quasar luminosity function, the MBH-σ * v relation, and cosmic SMBH mass density at high redshift and compare them to observations. We find that a dissipative dark matter interaction cross-section of σ/m ∼ 0.05 cm 2 /g is sufficient to produce the SMBHs observed in the early Universe while remaining consistent with ordinary SMBHs in the late Universe.

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Early formation of supermassive black holes via dark matter self-interactions

Cited by 66 publications

References 64 publications

Large-scale dark matter simulations

Large-scale dark matter simulations

Direct detection of mirror matter in Twin Higgs models

SMBH seeds from dissipative dark matter

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