SMBH seeds from dissipative dark matter

Xiao, Huangyu; Shen, Xuejian; Hopkins, Philip F.; Zurek, Kathryn M.

doi:10.1088/1475-7516/2021/07/039

Cited by 21 publications

(14 citation statements)

References 161 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Refs. [180][181][182][183][184][185] further show that SIDM could explain the origin of supermassive black holes via the mechanism of gravothermal collapse.…”

Section: Self-interacting Dark Mattermentioning

confidence: 82%

Snowmass2021 Cosmic Frontier White Paper: Dark Matter Physics from Halo Measurements

Bechtol¹,

Birrer²,

Cyr-Racine³

et al. 2022

Preprint

View full text Add to dashboard Cite

The non-linear process of cosmic structure formation produces gravitationally bound overdensities of dark matter known as halos. The abundances, density profiles, ellipticities, and spins of these halos can be tied to the underlying fundamental particle physics that governs dark matter at microscopic scales. Thus, macroscopic measurements of dark matter halos offer a unique opportunity to determine the underlying properties of dark matter across the vast landscape of dark matter theories. This white paper summarizes the ongoing rapid development of theoretical and experimental methods, as well as new opportunities, to use dark matter halo measurements as a pillar of dark matter physics.

show abstract

“…Refs. [180][181][182][183][184][185] further show that SIDM could explain the origin of supermassive black holes via the mechanism of gravothermal collapse.…”

Section: Self-interacting Dark Mattermentioning

confidence: 82%

Snowmass2021 Cosmic Frontier White Paper: Dark Matter Physics from Halo Measurements

Bechtol¹,

Birrer²,

Cyr-Racine³

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…Balberg et al 2002;Koda & Shapiro 2011) and cored dark matter subhaloes for the larger dwarfs. Moreover, exotic scenarios involving exothermic or endothermic (dissipative) processes from inelastic scattering have been considered to evaporate the Milky Way satellites (Vogelsberger et al 2019) or seed supermassive black holes at high redshift (e.g., Choquette et al 2019;Xiao et al 2021).…”

Section: Introductionmentioning

confidence: 99%

X-ray morphology of cluster-mass haloes in self-interacting dark matter

Shen¹,

Brinckmann²,

Rapetti³

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

We perform cosmological zoom-in simulations of 19 relaxed cluster-mass haloes with the inclusion of adiabatic gas within the cold dark matter (CDM) and self-interacting dark matter (SIDM) models. These clusters are selected as dynamically relaxed clusters from a parent simulation and have typical masses of 𝑀 200 1 -3 × 10 15 M . We find that both the dark matter and the intracluster gas distributions in SIDM are more spherical than their CDM counterparts, although the difference is smaller for the gas. Mock X-ray images are generated based on the simulations and are compared to the real X-ray images of 84 relaxed clusters selected from the Chandra and ROSAT archives. We perform ellipse fitting for the isophotes of mock and real X-ray images and obtain the ellipticities at cluster-centric radii of 𝑟 0.1 -0.2 𝑅 200 . The X-ray isophotes in SIDM models with increasing cross-sections are rounder than their CDM counterparts, which manifests as a systematic shift in the distribution function of ellipticities. Unexpectedly, the X-ray morphology of the observed "non-peaky" (non-cool-core) clusters agrees better with SIDM models with cross-section per unit mass (𝜎/𝑚) = 0.5 -1 cm 2 g −1 than CDM and SIDM with (𝜎/𝑚) = 0.1 cm 2 g −1 . Our statistical analysis indicates that the latter two models are disfavored at least at the 68% confidence level. This conclusion is not altered by shifting the radial range of measurements or applying temperature selection criterion. However, the primary uncertainty originates from the lack of baryonic physics in the adiabatic model, such as gas cooling, star formation and feedback effects, which have the potential to reconcile CDM simulations with observations.

show abstract

“…For instance, this is the only model that successfully accounts for the natural formation of early BH seeds; the existence of a correlation between properties of the central SMBH and the host galaxy and underlying dark matter halo and explains the CXB-CIB cross-correlation and its excess, while being consistent with all the multi-wavelength observations at z < 6. Other alternate DM models, like those that include dissipative DM with self-interactions that lead to core-collapse (SIDM variants) are amongst non-CDM proposals for BH seed formation (see for instance, recent proposal by Xiao et al 2021). In the absence of any detection of the putative DM particle after several decades of direct and indirect experimental searches, PBH-DM offers an economical scenario that is well motivated by physics and is one that couples early-Universe physics with phenomena on cosmological scales in the late Universe.…”

Section: Discussionmentioning

confidence: 99%

Exploring the high-redshift PBH-$Λ$CDM Universe: early black hole seeding, the first stars and cosmic radiation backgrounds

Cappelluti,

Hasinger,

Natarajan

2021

Preprint

View full text Add to dashboard Cite

We explore the observational implications of a model in which primordial black holes (PBHs) with a broad birth mass function ranging in mass from a fraction of a solar mass to ∼10 6 M , consistent with current observational limits, constitute the dark matter component in the Universe. The formation and evolution of dark matter and baryonic matter in this PBH-ΛCDM Universe are presented. In this picture, PBH DM mini-halos collapse earlier than in standard ΛCDM, baryons cool to form stars at z ∼ 15 − 20, and growing PBHs at these early epochs start to accrete through Bondi capture. The volume emissivity of these sources peaks at z ∼ 20 and rapidly fades at lower redshifts. As a consequence, PBH DM could also provide a channel to make early black hole seeds and naturally account for the origin of an underlying dark matter halo -host galaxy and central black hole connection that manifests as the M bh − σ correlation. To estimate the luminosity function and contribution to integrated emission power spectrum from these high-redshift PBH DM halos, we develop a Halo Occupation Distribution (HOD) model. In addition to tracing the star formation and reionizaton history, it permits us to evaluate the Cosmic Infrared and X-ray Backgrounds (CIB and CXB). We find that accretion onto PBHs/AGN successfully accounts for the detected backgrounds and their crosscorrelation, with the inclusion of an additional IR stellar emission component. Detection of the deep IR source count distribution by the JWST could reveal the existence of this population of high-redshift star-forming and accreting PBH DM.

show abstract

SMBH seeds from dissipative dark matter

Cited by 21 publications

References 161 publications

Snowmass2021 Cosmic Frontier White Paper: Dark Matter Physics from Halo Measurements

Snowmass2021 Cosmic Frontier White Paper: Dark Matter Physics from Halo Measurements

X-ray morphology of cluster-mass haloes in self-interacting dark matter

Exploring the high-redshift PBH-$Λ$CDM Universe: early black hole seeding, the first stars and cosmic radiation backgrounds

Contact Info

Product

Resources

About