Impacts of dark matter particle annihilation on recombination and the anisotropies of the cosmic microwave background

Zhang, Le; Chen, Xuelei; Lei, Yian; Si, Zong-Guo

doi:10.1103/physrevd.74.103519

Cited by 111 publications

(133 citation statements)

References 59 publications

(71 reference statements)

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“…Energy injection from dark matter (DM) annihilation can change the recombination history and affect the shape of the angular CMB spectra (Chen & Kamionkowski 2004;Padmanabhan & Finkbeiner 2005;Zhang et al 2006;Mapelli et al 2006). As recently shown in several papers (see e.g., Galli et al 2009Galli et al , 2011Giesen et al 2012;Hutsi et al 2011;Natarajan 2012;Evoli et al 2013) CMB anisotropies offer an opportunity to constrain DM annihilation models.…”

Section: Dark Matter Annihilationmentioning

confidence: 99%

Planck2013 results. XVI. Cosmological parameters

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

5,008

163

2,253

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This paper presents the first cosmological results based on Planck measurements of the cosmic microwave background (CMB) temperature and lensing-potential power spectra. We find that the Planck spectra at high multipoles ( > ∼ 40) are extremely well described by the standard spatiallyflat six-parameter ΛCDM cosmology with a power-law spectrum of adiabatic scalar perturbations. Within the context of this cosmology, the Planck data determine the cosmological parameters to high precision: the angular size of the sound horizon at recombination, the physical densities of baryons and cold dark matter, and the scalar spectral index are estimated to be θ * = (1.04147 ± 0.00062) × 10 −2 , Ω b h 2 = 0.02205 ± 0.00028, Ω c h 2 = 0.1199 ± 0.0027, and n s = 0.9603 ± 0.0073, respectively (note that in this abstract we quote 68% errors on measured parameters and 95% upper limits on other parameters). For this cosmology, we find a low value of the Hubble constant, H 0 = (67.3 ± 1.2) km s −1 Mpc −1 , and a high value of the matter density parameter, Ω m = 0.315 ± 0.017. These values are in tension with recent direct measurements of H 0 and the magnituderedshift relation for Type Ia supernovae, but are in excellent agreement with geometrical constraints from baryon acoustic oscillation (BAO) surveys. Including curvature, we find that the Universe is consistent with spatial flatness to percent level precision using Planck CMB data alone. We use high-resolution CMB data together with Planck to provide greater control on extragalactic foreground components in an investigation of extensions to the six-parameter ΛCDM model. We present selected results from a large grid of cosmological models, using a range of additional astrophysical data sets in addition to Planck and high-resolution CMB data. None of these models are favoured over the standard six-parameter ΛCDM cosmology. The deviation of the scalar spectral index from unity is insensitive to the addition of tensor modes and to changes in the matter content of the Universe. We find an upper limit of r 0.002 < 0.11 on the tensor-to-scalar ratio. There is no evidence for additional neutrino-like relativistic particles beyond the three families of neutrinos in the standard model. Using BAO and CMB data, we find N eff = 3.30 ± 0.27 for the effective number of relativistic degrees of freedom, and an upper limit of 0.23 eV for the sum of neutrino masses. Our results are in excellent agreement with big bang nucleosynthesis and the standard value of N eff = 3.046. We find no evidence for dynamical dark energy; using BAO and CMB data, the dark energy equation of state parameter is constrained to be w = −1.13 +0.13 −0.10 . We also use the Planck data to set limits on a possible variation of the fine-structure constant, dark matter annihilation and primordial magnetic fields. Despite the success of the six-parameter ΛCDM model in describing the Planck data at high multipoles, we note that this cosmology does not provide a good fit to the temperature power spectrum at low multipoles. T...

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Section: Dark Matter Annihilationmentioning

confidence: 99%

Planck2013 results. XVI. Cosmological parameters

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

5,008

163

2,253

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“…A widely considered process is the decay or annihilation of massive particles [20,32,33,34,35,36,37,38]. The decay channel depends on the nature of the particles, and could, for example, include charged and neutral leptons, quarks or gauge bosons.…”

Section: A Modified Ionization Historymentioning

confidence: 99%

Cosmological constraints in the presence of ionizing and resonance radiation at recombination

Bean

Melchiorri²,

Silk

2007

Phys. Rev. D

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With the recent measurement of full sky cosmic microwave background polarization from WMAP, key cosmological degeneracies have been broken, allowing tighter constraints to be placed on cosmological parameters inferred assuming a standard recombination scenario. Here we consider the effect on cosmological constraints if additional ionizing and resonance radiation sources are present at recombination. We find that the new CMB data significantly improve the constraints on the additional radiation sources, with log 10 [ǫα] < −0.5 and log 10 [ǫi] < −2.4 at 95% c.l. for resonance and ionizing sources respectively. Including the generalized recombination scenario, however, we find that the constraints on the scalar spectral index ns are weakened to ns = 0.98 ± 0.03, with the ns = 1 case now well inside the 95% c.l.. The relaxation of constraints on tensor modes, scale invariance, dark energy and neutrino masses are also discussed.

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“…To estimate the fraction of the deposited energy ending up in ionizing and heating the medium we use the approximation motivated by the original work of Shull & van Steenberg (1985) and used in several subsequent papers (Chen & Kamionkowski 2004;Padmanabhan & Finkbeiner 2005;Mapelli et al 2006;Zhang et al 2006;Natarajan & Schwarz 2008): ∼(1 − x e )/3 goes into ionization and ∼(1 + 2x e )/3 into heating. Here x e is the ionization fraction.…”

Section: Radiative Transfer Extragalactic Gamma Background Reionizamentioning

confidence: 99%

“…Padmanabhan & Finkbeiner (2005), Mapelli et al (2006), Zhang et al (2006), Natarajan & Schwarz (2008), Belikov & Hooper (2009a), Galli et al (2009. Prior to the calculations done in Natarajan & Schwarz (2008), Belikov & Hooper (2009a) all the authors have only included the homogeneous DM component, i.e.…”

Section: Introductionmentioning

confidence: 99%

Constraints on leptonically annihilating dark matter from reionization and extragalactic gamma background

Hütsi

Hektor

Raidal

2009

A&A

106

134

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Context. The PAMELA, Fermi and HESS experiments (PFH) have shown anomalous excesses in the cosmic positron and electron fluxes. A very exciting possibility is that those excesses are due to annihilating dark matter (DM). Aims. In this paper we calculate constraints on leptonically annihilating DM using observational data on diffuse extragalactic γ-ray background and measurements of the optical depth to the last-scattering surface, and compare those with the PFH favored region in the m DM − σ A υ plane. Methods. Having specified the detailed form of the energy input with PYTHIA Monte Carlo tools we solve the radiative transfer equation which allows us to determine the amount of energy being absorbed by the cosmic medium and also the amount left over for the diffuse gamma background. Results. We find that the constraints from the optical depth measurements are able to rule out the PFH favored region fully for the τ − + τ + annihilation channel and almost fully for the μ − + μ + annihilation channel. It turns out that those constraints are quite robust with almost no dependence on low redshift clustering boost. The constraints from the γ-ray background are sensitive to the assumed halo concentration model and, for the power law model, rule out the PFH favored region for all leptonic annihilation channels. We also find that it is possible to have models that fully ionize the Universe at low redshifts. However, those models produce too large free electron fractions at z 100 and are in conflict with the optical depth measurements. Also, the magnitude of the annihilation cross-section in those cases is larger than suggested by the PFH data.

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Impacts of dark matter particle annihilation on recombination and the anisotropies of the cosmic microwave background

Cited by 111 publications

References 59 publications

Planck2013 results. XVI. Cosmological parameters

Planck2013 results. XVI. Cosmological parameters

Cosmological constraints in the presence of ionizing and resonance radiation at recombination

Constraints on leptonically annihilating dark matter from reionization and extragalactic gamma background

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