Erratum: IceCube neutrinos, decaying dark matter, and the Hubble constant [Phys. Rev. D<b>92</b>, 061301(R) (2015)]

Anchordoqui, Luis A.; Barger, Vernon; Goldberg, Haim; Huang, X. T.; Marfatia, Danny; Silva, Luiz H. M. da; Weiler, T.

doi:10.1103/physrevd.94.069901

Cited by 42 publications

(35 citation statements)

References 20 publications

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“…For example, a statistically significant tension currently exists between the value of H now obtained from local probes of the cosmic expansion rate (including not only Type Ia supernova data [35][36][37], but also lensing time-delay experiments [38,39]) and the value inferred from CMB data in the context of a ΛCDM cosmology [40][41][42][43]. Dark-matter decays between t LS and t now have been posited as one possible [44][45][46][47][48] way of alleviating these tensions. While it has not been our aim in this paper to address this tension, it is likely that the DDM framework can serve to alleviate these tensions in new and interesting ways.…”

Section: Discussionmentioning

confidence: 99%

Constraining dark-matter ensembles with supernova data

Desai

Thomas

2020

Phys. Rev. D

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The constraints on non-minimal dark sectors involving ensembles of unstable dark-matter species are well established and quite stringent in cases in which these species decay to visible-sector particles. However, in cases in which these ensembles decay exclusively to other, lighter dark-sector states, the corresponding constraints are less well established. In this paper, we investigate how information about the expansion rate of the universe at low redshifts gleaned from observations of Type Ia supernovae can be used to constrain ensembles of unstable particles which decay primarily into dark radiation. arXiv:1909.07981v1 [astro-ph.CO]

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Section: Discussionmentioning

confidence: 99%

Constraining dark-matter ensembles with supernova data

Desai

Thomas

2020

Phys. Rev. D

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“…Many scenarios to resolve the Hubble tension have been proposed, including modified dark energy [19][20][21] and decaying dark matter particles [22][23][24][25][26][27][28]. In this note, we argue that Hubble tension may be a result of extrapolating the CMB data from the time of recombination (z = 1089) to the present time (z = 0) using the CDM cosmology, which assumes pressureless dark matter.…”

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confidence: 90%

Non-particle dark matter from Hubble parameter

Popławski

2019

Eur. Phys. J. C

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The measurements of the Hubble parameter using the cosmic microwave background radiation appear to be inconsistent with the measurements of this parameter using Cepheid variable stars. This inconsistency may be a result of using the CDM cosmology, which assumes pressureless dark matter, in extrapolating the data from the recombination time to the present time. We show that both measurements are consistent if dark matter satisfies an equation of state in which the pressure p and the energy density are related by p = w with a negative value of w. The data give w ≈ −0.01. The negative value of w indicates that dark matter would not be formed by particles, which is consistent with the lack of experimental evidence for them.The observations of the temperature angular power spectrum of the cosmic microwave background (CMB) radiation provide the information about the composition of the universe [1]. The measurements of the position of the first acoustic peak show that the universe is nearly flat, with the density parameter ≈ 1. The measurements of the amplitudes of the peaks determine the values of b h 2 and c h 2 , where b is the density parameter for baryonic matter, c is the density parameter for dark matter, and the present-day Hubble parameter H 0 = 100h km/s/Mpc. Combining these values with the measured h = 0.674 ± 0.005 gives (omitting errors) b = 0.049 and c = 0.265, as obtained by the Planck satellite [2,3]. Consequently, the density parameter for total matter is m = 0.314.Before the Planck measurements, most measured values of h also clustered around 0.68, including the data from high-redshift type Ia supernovae (SN Ia) [4,5], Wilkinson Microwave Anisotropy Probe CMB data [6], baryon acoustic oscillations (BAO) [7], SN Ia and BAO data [8], measurements of the Hubble parameter at intermediate redshifts [9], and large-scale-structure data [10]. Assuming a flat universe, = 1 − m = 0.686 for dark energy (cosmological constant). The resulting age of the universe is t univ = a e-mail: NPoplawski@newhaven.edu da/(a H) =

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“…While extended cosmological models with more parameters [34][35][36][37][38][39][40][41][42][43][44] may be able to accommodate these tensions, specific solutions from particle physics have also been proposed recently in Refs. [45][46][47][48] for decaying DM and in Refs. [24-27, 49, 50] for interacting DM and DR where either gauge bosons or fermions are the DR so that their lightness is protected by gauge symmetry or chiral symmetry.…”

Section: Introductionmentioning

confidence: 99%

Hidden charged dark matter and chiral dark radiation

Nagata

Tang

2017

Physics Letters B

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In the light of recent possible tensions in the Hubble constant H 0 and the structure growth rate σ 8 between the Planck and other measurements, we investigate a hidden-charged dark matter (DM) model where DM interacts with hidden chiral fermions, which are charged under the hidden SU(N ) and U(1) gauge interactions. The symmetries in this model assure these fermions to be massless. The DM in this model, which is a Dirac fermion and singlet under the hidden SU(N ), is also assumed to be charged under the U(1) gauge symmetry, through which it can interact with the chiral fermions. Below the confinement scale of SU(N ), the hidden quark condensate spontaneously breaks the U(1) gauge symmetry such that there remains a discrete symmetry, which accounts for the stability of DM. This condensate also breaks a flavor symmetry in this model and Nambu-Goldstone bosons associated with this flavor symmetry appear below the confinement scale. The hidden U(1) gauge boson and hidden quarks/Nambu-Goldstone bosons are components of dark radiation (DR) above/below the confinement scale. These light fields increase the effective number of neutrinos by δN eff 0.59 above the confinement scale for N = 2, resolving the tension in the measurements of the Hubble constant by Planck and Hubble Space Telescope if the confinement scale is 1 eV. DM and DR continuously scatter with each other via the hidden U(1) gauge interaction, which suppresses the matter power spectrum and results in a smaller structure growth rate. The DM sector couples to the Standard Model sector through the exchange of a real singlet scalar mixing with the Higgs boson, which makes it possible to probe our model in DM direct detection experiments. Variants of this model are also discussed, which may offer alternative ways to investigate this scenario.

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Erratum: IceCube neutrinos, decaying dark matter, and the Hubble constant [Phys. Rev. D92, 061301(R) (2015)]

Cited by 42 publications

References 20 publications

Constraining dark-matter ensembles with supernova data

Constraining dark-matter ensembles with supernova data

Non-particle dark matter from Hubble parameter

Hidden charged dark matter and chiral dark radiation

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