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The effective energy deposition fractions for the smooth DM background component, as a function of the DM mass, in GeV. Blue (upper) and red (lower) curves denote the e + e − and µ + µ − annihilation channels explored in this study. Red (lower) curve stop at the muon mass, the threshold DM mass for muon production via annihilation.
Source publication
We compute the bounds on the dark matter (DM) annihilation cross section
using the most recent Cosmic Microwave Background measurements from WMAP9,
SPT'11 and ACT'10. We consider DM with mass in the MeV-TeV range annihilating
100% into either an e+e- or a mu+mu- pair. We consider a realistic energy
deposition model, which includes the dependence on...
Contexts in source publication
Context 1
... 50, before reionization starts and the upper limit is chosen to be z max = 1100, when the effect of DM annihilations starts to delay recombination 5 . We have verified that the results obtained with the effective deposition efficiency f eff (m χ ) differ by less than a few percent from those obtained with the full redshift-dependent f (z, m χ ). Fig. 1 shows f eff (m χ ) for DM annihilations into e + e − and µ + µ − , as a function of the DM mass. We note that the effective f eff (m χ ) deposition efficiency is much lower for the χχ → µ + µ − channel due the large fraction of final-state neutrinos, which do not heat the IGM nor contribute to ionization. As noted in Section II, f (z, ...
Context 2
... the energy deposited equals the energy injected (f (z, m χ ) = 1) using WMAP9+SPT'11+HST+BAO data sets. Notice that, when including the effective efficiency f eff (m χ ), the χχ → e + e − bounds become less stringent as the DM mass increases compared to those when assuming perfect efficiency (f (z, m χ ) = 1), as expected from the left panel of Fig. 1. Finally, the upper dashed black line illustrates the 95% CL bounds for the µ + µ − channel, with the corresponding f eff (m χ ) function, and using WMAP9+SPT'11+HST+BAO data sets. In this case, the bounds are weaker since ∼ 2/3 of the energy is lost in the form of ...
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Citations
... However, as a first approximation, the fðzÞ dependence on redshift z can be neglected, which implies the absorption of total injected energy by the galactic medium with a typical efficiency fðzÞ ≃ f eff [3,91,93]. In addition, for the parameter space of interest one can put f eff ≃ 1 [94]. We notice again that this constraint is valid only for scalar DM annihilation in the s-wave [95]. ...
We discuss the thermal target curves of Majorana, Dirac, scalar, and vector light dark matter (DM) that are associated with the freeze-out mechanism via the annihilation into the e+e− pair through the electron-specific spin-0 mediator of dark matter. We also discuss the mechanism to produce the regarded DM mediator in the electron (positron) fixed-target experiments such as NA64e and LDMX. We derive the corresponding experimental reaches of NA64e and LDMX that are complementary to the DM thermal target parameter space.
... In the second subsection, we discuss the modeling of an extra-galactic signal. We adopt the signal flux simulation described in [13,[26][27][28]. ...
... (B.3). Here, we use the one described in [27]. We give a brief discussion of the different approximations in appendix B and appendix C along with a few intermediate results of our calculations. ...
... In this calculation, we set M min = 10 −3 M ⊙ as a conservative lower limit [58,59]. [60] and [27] have been compared here. The deviation is hard in the low halo mass region, whereas in the higher mass region, both approximations converge. ...
We present a new search for weakly interacting massive particles utilizing ten years of public IceCube data, setting more stringent bounds than previous IceCube analysis on massive dark matter to neutrino annihilation. We also predict the future potential of the new neutrino observatory, P-ONE, showing that it may even exceed the sensitivities of Fermi-LAT gamma-ray searches by about 1–2 orders of magnitude in 1–10 TeV regions. This analysis considers the diffuse dark matter self-annihilation to neutrinos via direct and indirect channels, from the galactic dark matter halo and extra-galactic sources. We also predict that P-ONE will be capable of pushing these bounds further than IceCube, even reaching the thermal relic abundance utilizing a galactic center search for extended run-time.
... Jordan Koechler injection [20][21][22], the two latter ones as dotted lines, and finally FSR from decaying DM using 16 years of I data [23] as a thin dot-dashed line. LeoT gas heati ng V o ya g e r1 ...
... The CMB is especially useful at constraining DM annihilation or decay into SM particles, see e.g., [3][4][5][6][7][8][9][10][11][12][13]. Both scenarios result in an exotic injection of energy into the intergalactic medium (IGM). ...
... Finally, in section 5, we discuss these results and conclude. In this work, we use a ΛCDM cosmology with parameters (Ω m , Ω b , Ω Λ , h, σ 8 ...
... 9 7 In practice (e.g., for a Bayesian inference), because of the broad range of associated uncertainties, f II ⋆,10 , f III ⋆,7 , f II esc,10 , f III esc,7 priors are often implemented in logarithmic space with a flat prior between e.g., 10 −3 and 10 0 . 8 In this work, the Sheth, Mo and Tormen (SMT) HMF [53] is adopted. 9 Upon the completion of this work, the authors of [57] have performed an initial study of the impact of DM energy injection on the H2 content of first galaxies. ...
The redshifted 21cm signal from the Cosmic Dawn is expected to provide unprecedented insights into early Universe astrophysics and cosmology. Here we explore how dark matter can heat the intergalactic medium before the first galaxies, leaving a distinctive imprint in the 21cm power spectrum. We provide the first dedicated Fisher matrix forecasts on the sensitivity of the Hydrogen Epoch of Reionization Array (HERA) telescope to dark matter decays. We show that with 1000 hours of observation, HERA has the potential to improve current cosmological constraints on the dark matter decay lifetime by up to three orders of magnitude. Even in extreme scenarios with strong X-ray emission from early-forming, metal-free galaxies, the bounds on the decay lifetime would be improved by up to two orders of magnitude. Overall, HERA shall improve on existing limits for dark matter masses below 2 GeV/c ² for decays into e⁺e⁻ and below few MeV/c ² for decays into photons.
... The CMB is especially useful at constraining DM annihilation or decay into SM particles, see e.g. [3][4][5][6][7][8][9][10][11][12][13]. Both scenarios result in an exotic injection of energy into the intergalactic medium (IGM). ...
... In addition to this, as molecular hydrogen can be easily dissociated by photons within the Lyman-Werner (LW) energy range (11.2 − 13.6 eV), star formation 7 In practice (e.g. for a Bayesian inference), because of the broad range of associated uncertainties, f II ⋆,10 , f III ⋆,7 , f II esc,10 , f III esc,7 priors are often implemented in logarithmic space with a flat prior between e.g. 10 −3 and 10 0 . 8 In this work, the Sheth, Mo and Tormen (SMT) HMF [52] is adopted. ...
... In addition, the DM annihilation signature in the 21cm signal is expected to strongly depend on the late time boost arising from structure formation (see e.g. [17,18]), contrary to CMB bounds [8,10]. We therefore leave the study of DM annihilation for future work. ...
The redshifted 21cm signal from the Cosmic Dawn is expected to provide unprecedented insights into early Universe astrophysics and cosmology. Here we explore how dark matter can heat the intergalactic medium before the first galaxies, leaving a distinctive imprint in the 21cm power spectrum. We provide the first dedicated Fisher matrix forecasts on the sensitivity of the Hydrogen Epoch of Reionization Array (HERA) telescope to dark matter decays. We show that with 1000 hours of observation, HERA has the potential to improve current cosmological constraints on the dark matter decay lifetime by up to three orders of magnitude. Even in extreme scenarios with strong X-ray emission from early-forming, metal-free galaxies, the bounds on the decay lifetime would be improved by up to two orders of magnitude. Overall, HERA shall improve on existing limits for dark matter masses below $2$ GeV$/c^2$ for decays into $e^+e^-$ and below few MeV$/c^2$ for decays into photons.
... Final combined results for annihilating DM from this work (Xmm-Newton), compared with existing bounds. We report the bounds from Essig et al. [47], obtained using a compilation of X-ray and soft γ-ray data (dot-dashed green line marked 'diffuse γ-rays'); the bounds from Boudaud et al. [48] derived using data from Voyager 1 (dashed green and blue lines, corresponding to the e + e − and µ + µ − annihilation channels, respectively); the CMB bounds from Slatyer [49] and Lopez-Honorez et al. [50] (dotted green and blue lines, for the e + e − and µ + µ − channels); the bounds from gas heating in Leo T, obtained by Wadekar and Wang [51] (also dotted, since the physics mechanism of energy injection is similar to the CMB one). cm 3 /s in the range m DM 1 − 20 MeV, the region where the dominant contribution of the ICS component is too low in energy to be constrained by the data. ...
... Using the impact on the CMB anisotropies of the e + e − injection by DM annihilation events, Slatyer [49] and Lopez-Honorez et al. [50] derived the constraints represented by the dotted lines in figure 7. Our Xmm-Newton bounds reach deeper than these CMB constraints, in the portion of large mass where the ICS effect is important (m DM 180 MeV and m DM 400 MeV, respectively for the e + e − and µ + µ − , π + π − channels). The CMB constraints are still more stringent elsewhere. ...
Sub-GeV dark matter particles can annihilate or decay producing e ± pairs which upscatter the low-energy photon fields in the Galaxy and generate an X-ray emission (via the Inverse Compton effect). Using X -ray data from Xmm-Newton , Integral , NuStar and Suzaku , we derive new constraints on this class of dark matter (DM). In the annihilation case, our new bounds are the strongest available for DM masses above 180 MeV, reaching 〈 σv 〉 ≲ 10 ⁻²⁸ cm ³ /s for m DM ≃ 1 GeV. In the decay case, our bounds are the strongest to date over a large fraction of the considered mass range, constraining τ ≳ 10 ²⁸ s for m DM ≃ 1 GeV and improving by up to 3 orders of magnitude upon existing limits.
... At low redshifts, typically at z z max A , star formation and active galactic nuclei are expected to inject extra sources of energy in the IGM and to drive reionization at z = z reio < z max A , see e.g. the discussion in refs. [23,24]. Here, we will consider two different approaches to reionization. ...
... [10,22,29,30], that can lead to strong constraints on beyond the Standard Model scenarios, see e.g. [11,12,17,23,[31][32][33]. The energy injection efficiencies and the different reionization histories, discussed in sections 2.2 and 2.3, are two crucial inputs for our CMB analysis. ...
... It would however be interesting to review these constraints in the light of next-generation measurements of 21 cm emission/absorption that is expected to become a very sensitive probe of the IGM JCAP06(2023)060 temperature at low redshifts, see e.g. [44], and potentially surpass the CMB constraint for DM decay, see also [23,[45][46][47]. ...
Dark matter energy injection in the early universe modifies both the ionization history and the temperature of the intergalactic medium. In this work, we improve the CMB bounds on sub-keV dark matter and extend previous bounds from Lyman-α observations to the same mass range, resulting in new and competitive constraints on axion-like particles (ALPs) decaying into two photons. The limits depend on the underlying reionization history, here accounted self-consistently by our modified version of the publicly available DarkHistory and CLASS codes. Future measurements such as the ones from the CMB-S4 experiment may play a crucial, leading role in the search for this type of light dark matter candidates.
... At low redshifts, typically at z z max A , star formation and active galactic nuclei are expected to inject extra sources of energy in the IGM and to drive reionization at z = z reio < z max A , see e.g. the discussion in Refs. [22,23]. Here, we will consider two different approaches to reionization. ...
... [9,21,28,29], that can lead to strong constraints on beyond the Standard Model scenarios, see e.g. [10,11,16,22,[30][31][32]. The energy injection efficiencies and the different reionization histories, discussed in Secs 2.2 and 2.3, are two crucial inputs for our CMB analysis. ...
... It appears that, given the methodology followed here, the Lyman-α bounds are up to one order of magnitude weaker than the CMB bounds obtained in Sec. 3. It would however be interesting to review these constraints in the light of next-generation measurements of 21 cm emission/absorption that is expected to become a very sensitive probe of the IGM temperature at low redshifts, see e.g. [40], and potentially surpass the CMB constraint for DM decay, see also [22,[41][42][43]. ...
Dark matter energy injection in the early universe modifies both the ionization history and the temperature of the intergalactic medium. In this work, we improve the CMB bounds on sub-keV dark matter and extend previous bounds from Lyman-$\alpha$ observations to the same mass range, resulting in new and competitive constraints on axion-like particles (ALPs) decaying into two photons. The limits depend on the underlying reionization history, here accounted self-consistently by our modified version of the publicly available {\tt DarkHistory} and {\tt CLASS} codes. Future measurements such as the ones from the CMB-S4 experiment may play a crucial, leading role in the search for this type of light dark matter candidates
... Boudaud el al. [470] have derived their constraints on the e + e − and µ + µ − channels using the low energy measurements of the local cosmic-ray flux, carried out by the VOYAGER 1 spacecraft The CMB constraints derived in Ref. [471] are the most stringent across the whole mass range of interest. They are given in Ref. [471] for the e + e − channel and in the earlier study of Ref. [472] for the µ + µ − channel. However, they hold under the assumption that the DM annihilation cross-section is speed-independent (s-wave). ...
In this thesis, we examined the possibilities offered by multi-messenger astronomy in the context of indirect dark matter detection. We have applied a multi-wavelength strategy by studying different signals across the electromagnetic spectrum (gamma-rays, X-rays, radio waves) produced at different scales of the Universe (galactic, extragalactic, cosmic web filaments). In Part I, we obtained the first-ever prediction of the cross-correlation signal between the extragalactic gamma-ray flux and the 21cm line emitted by hydrogen atoms in dark matter halos. We showed that the neutral hydrogen distribution is a highly competitive probe for dark matter searches, especially in view of the next-generation radio telescope Square Kilometre Array. In Part II, we obtained the limits on the annihilation cross-section of dark matter particles by comparing the X-ray flux measured by INTEGRAL with the theoretical signal expected in the case of particles with a mass between 1 MeV and 5 GeV. We derived the most stringent constraints in the literature on such particles with a mass between 150 MeV and 1.5 GeV. The originality of this work resides in including the contribution from the scattering between the low-energy photons in the Milky Way with the electrons and positrons, produced by dark matter particles. In Part III, we focused on an exotic radio signal, emerging from the GLEAM survey, which seems compatible with a filament of the cosmic web and provides direct evidence for one of the pillars of our understanding of structure formation in the Universe. This radio emission can be explained by dark matter candidates with a mass in the range of 5-10 GeV, decaying into pairs of electrons and positrons. This thesis contributes to a broad spectrum of research for particle dark matter on different levels, since we considered different types of signals, multiple targets and different mass scales.
... The factor ∆ 2 (z), which accounts for the enhancement to the annihilation rate due to the DM clustering in halos, is defined in table 1, where the values of f 0 for the NFW, Moore, and Kravtsov profiles are 5 × 10 4 , 5 × 10 5 , and 2 × 10 4 , respectively. The halo boost factor G(z) in this table, given in ref. [30], is calculated by summing the contribution of all halos, i.e., a single halo contribution is weighted by the halo mass function (HMF), dn/dM : ...
... [36], using the HMF in refs. [32], [33] and [34,35], respectively to calculate the boost factor G(z) [30]. ...
... The solid magenta line is the calculation of [29], and the solid blue line that of [37]. The orange, green, and blue shaded regions correspond to the calculation of the boost factor G(z) [30] in ref. [36] using the halo mass function of refs. [32], [33] and [34,35] respectively. ...
The Hyper-Kamiokande (HyperK) experiment is expected to precisely measure the Diffuse Supernova Neutrino Background (DSNB). This requires that the backgrounds in the relevant energy range are well understood. One possible background that has not been considered thus far is the annihilation of low-mass dark matter (DM) to neutrinos. We conduct simulations of the DSNB signal and backgrounds in HyperK, and quantify the extent to which DM annihilation products can pollute the DSNB signal. We find that the presence of DM could affect the determination of the correct values of parameters of interest for DSNB physics, such as effective neutrino temperatures and star formation rates. While this opens the possibility of simultaneously characterising the DNSB and discovering dark matter via indirect detection, we argue that it would be hard to disentangle the two contributions due to the lack of angular information available at low energies.
