Constraining dark-matter ensembles with supernova data

Desai, Alisha; Thomas, Brooks

doi:10.1103/physrevd.101.035031

Cited by 20 publications

(14 citation statements)

References 98 publications

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“…In particular, we have focused on the regime in which the lifetimes of all unstable dark-sector states are sufficiently short that all of their energy density has been transferred to the lightest species by the beginning of the BBN epoch. We have made this assumption since the decays of unstable particles at subsequent times-even decays solely to other, lighter states within the dark sector-are constrained by their impact of the cosmic expansion rate and its effect on various observables [55][56][57][58]. These observables include the spatial distribution of CMB anisotropies, baryon-acousticoscillation data, and the relationship between the redshifts and luminosity distances of Type Ia supernovae.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Deciphering the archaeological record: Cosmological imprints of nonminimal dark sectors

Huang

Kost

et al. 2020

Phys. Rev. D

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Many proposals for physics beyond the Standard Model give rise to a dark sector containing many degrees of freedom. In this work, we explore the cosmological implications of the nontrivial dynamics which may arise within such dark sectors, focusing on decay processes which take place entirely among the dark constituents. First, we demonstrate that such decays can leave dramatic imprints on the resulting dark-matter phase-space distribution. In particular, this distribution need not be thermal-it can even be multimodal, exhibiting a nontrivial pattern of peaks and troughs as a function of momentum. We then proceed to show how these features can induce modifications to the matter power spectrum. Finally, we assess the extent to which one can approach the archaeological "inverse" problem of deciphering the properties of an underlying dark sector from the matter power spectrum. Indeed, one of the main results of this paper is a remarkably simple conjectured analytic expression which permits the reconstruction of many of the important features of the dark-matter phase-space distribution directly from the matter power spectrum. Our results therefore provide an interesting toolbox of methods for learning about, and potentially constraining, the features of nonminimal dark sectors and their dynamics in the early universe.

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Section: Conclusion and Discussionmentioning

confidence: 99%

Deciphering the archaeological record: Cosmological imprints of nonminimal dark sectors

Huang

Kost

et al. 2020

Phys. Rev. D

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“…[458] discuss a scenario in which the observed DM comprises a vast array of interacting fields, each with different values of their masses, couplings, and abundances. Within such a "dynamical" dark matter model, a generalization of the decaying dark matter scenario, it is possible to address the Hubble tension issue, providing a self-sustaining framework to unify short-lived and long-lived decaying dark matter models [459].…”

Section: Dynamical Dark Mattermentioning

confidence: 99%

In the Realm of the Hubble tension $-$ a Review of Solutions

Di Valentino,

Mena,

Pan

et al. 2021

Preprint

178

252

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The simplest ΛCDM model provides a good fit to a large span of cosmological data but harbors large areas of phenomenology and ignorance. With the improvement of the number and the accuracy of observations, discrepancies among key cosmological parameters of the model have emerged. The most statistically significant tension is the 4σ to 6σ disagreement between predictions of the Hubble constant, H 0 , made by the early time probes in concert with the "vanilla" ΛCDM Cosmological model, and a number of late time, model-independent determinations of H 0 from local measurements of distances and redshifts. The high precision and consistency of the data at both ends present strong challenges to the possible solution space and demands a hypothesis with enough rigor to explain multiple observations-whether these invoke new physics, unexpected large-scale structures or multiple, unrelated errors. A thorough review of the problem including a discussion of recent Hubble constant estimates and a summary of the proposed theoretical solutions is presented here. We include more than 850 references, indicating that the interest in this area has grown considerably just during the last few years. We classify the many proposals to resolve the tension in these categories: Early Dark Energy, Late Dark Energy, Dark energy models with 6 degrees of freedom and their extensions, Models with extra relativistic degrees of freedom, Models with Extra Interactions, Unified cosmologies, Modified gravity, Inflationary models, Modified recombination history, Physics of the critical Phenomena, and Alternative proposals. Some are formally successful, improving the fit to the data in light of their additional degrees of freedom, restoring agreement within 1 − 2σ between Planck 2018, using the Cosmic Microwave Background power spectra data, Baryon Acoustic Oscillations, Pantheon SN data, and R20, the latest SH0ES Team [2] measurement of the Hubble constant (H 0 = 73.2 ± 1.3 km s −1 Mpc −1 at 68% confidence level). However, there are many more unsuccessful models which leave the discrepancy well above the 3σ disagreement level. In many cases, reduced tension comes not simply from a change in the value of H 0 but also due to an increase in its uncertainty due to degeneracy with additional physics, complicating the picture and pointing to the need for additional probes. While no specific proposal makes a strong case for being highly likely or far better than all others, solutions involving early or dynamical dark energy, neutrino interactions, interacting cosmologies, primordial magnetic fields, and modified gravity provide the best options until a better alternative comes along.

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“…(N) Modified Gravity models [166] in which gravity changes with redshift, such that the H 0 estimate from CMB can have larger values [167][168][169][170][171][172][223][224][225][226] . (N) Decaying dark matter [179][180][181][182][183][184][185][186][187][188] or interacting neutrinos [45,86,197] .…”

Section: State-of-the-art -mentioning

confidence: 99%