Probing dark matter annihilation in the Galaxy with antiprotons and gamma rays

Cuoco, A.; Heisig, Jan; Korsmeier, Michael; Krämer, M.

doi:10.1088/1475-7516/2017/10/053

Cited by 77 publications

(114 citation statements)

References 84 publications

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“…As this is clearly not a large effect, and to be most conservative, we choose to use the most recent full data set which gives a weaker limit due to these excesses. (Note this low significance excess can be meaningfully combined with the AMS antiproton excess [74][75][76][77][78]. )…”

Section: Fermimentioning

confidence: 99%

GeV-scale thermal WIMPs: Not even slightly ruled out

et al. 2018

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Weakly interacting massive particles (WIMPs) have long reigned as one of the leading classes of dark matter candidates. The observed dark matter abundance can be naturally obtained by freezeout of weakscale dark matter annihilations in the early Universe. This "thermal WIMP" scenario makes direct predictions for the total annihilation cross section that can be tested in present-day experiments. While the dark matter mass constraint can be as high as m χ ≳ 100 GeV for particular annihilation channels, the constraint on the total cross section has not been determined. We construct the first model-independent limit on the WIMP total annihilation cross section, showing that allowed combinations of the annihilationchannel branching ratios considerably weaken the sensitivity. For thermal WIMPs with s-wave 2 → 2 annihilation to visible final states, we find the dark matter mass is only known to be m χ ≳ 20 GeV. This is the strongest largely model-independent lower limit on the mass of thermal-relic WIMPs; together with the upper limit on the mass from the unitarity bound (m χ ≲ 100 TeV), it defines what we call the "WIMP window." To probe the remaining mass range, we outline ways forward.

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Section: Fermimentioning

confidence: 99%

GeV-scale thermal WIMPs: Not even slightly ruled out

et al. 2018

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“…For instance, just above its threshold, the photon spectrum for χχ → HH → bbbb has the same shape as the one for χχ → bb but is shifted by a factor of 2 towards smaller energies. This is also reflected in the fact that the three observations can be fitted by DM annihilation into a SM-like Higgs for masses around the threshold [103], i.e., roughly a factor of two larger than the DM mass providing the best fit for χχ → bb.…”

Section: Indirect Detectionmentioning

confidence: 99%

“…For pNG DM annihilation via a resonant h or H exchange in the s-channel, the composition of final states is the same as for the (singlet scalar) Higgs portal model, unless m χ > m h, H . For this case, explicit fits to the gamma-ray galactic centre excess [106] and the CR antiproton excess [103] have been performed. The latter analysis also provides a joint fit of both observations and the above-mentioned excess in the LSST+Fermi -LAT (proj.)…”

Section: Indirect Detectionmentioning

confidence: 99%

Global fit of pseudo-Nambu-Goldstone Dark Matter

Arina

Beniwal

Degrande

et al. 2020

J. High Energ. Phys.

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We perform a global fit within the pseudo-Nambu-Goldstone dark matter (DM) model emerging from an additional complex scalar singlet with a softly broken global U (1) symmetry. Leading to a momentum-suppressed DM-nucleon cross section at tree level, the model provides a natural explanation for the null results from direct detection experiments. Our global fit combines constraints from perturbative unitarity, DM relic abundance, Higgs invisible decay, electroweak precision observables and latest Higgs searches at colliders. The results are presented in both frequentist and Bayesian statistical frameworks. Furthermore, post-processing our samples, we include the likelihood from gamma-ray observations of Fermi-LAT dwarf spheroidal galaxies and compute the one-loop DM-nucleon cross section. We find two favoured regions characterised by their dominant annihilation channel: the Higgs funnel and annihilation into Higgs pairs. Both are compatible with current Fermi-LAT observations, and furthermore, can fit the slight excess observed in four dwarfs in a mass range between about 30-300 GeV. While the former region is hard to probe experimentally, the latter can partly be tested by current observations of cosmic-ray antiprotons as well as future gamma-ray observations. [15,16]. More commonly, however, particle DM models with a pseudoscalar mediator [17][18][19][20][21][22] leads to a momentum-suppressed DM-nucleon cross section. Thus, this class of models can naturally evade the strong limits from direct detection experiments.A popular example in this regards is the pseudo-Nambu-Goldstone (pNG) DM. It is realised by adding a complex scalar singlet with a softly broken global U (1) symmetry [23-25] to the Standard Model (SM) particle content. Due to the soft symmetry breaking, the resulting Goldstone becomes massive, i.e., a pNG boson. An additional CP symmetry ensures the stability of the pNG boson, which serves as a viable DM candidate. The Goldstone nature of the DM particle implies that the pNG DM-nucleon cross section is momentum-suppressed at tree-level. 1 Thus, a pNG DM model offers a natural way of evading the strong direct detection limits. A leading-order contribution to the pNG DM-nucleon cross section in the zero-momentum limit appears at the one-loop level [27,28]. For typical DM velocities in our galaxy, v χ ∼ 10 −3 , it can easily dominate over the tree-level contribution. The one-loop cross section can vary by several orders of magnitude in the allowed model parameter space. It has been shown that for parameter points which satisfy the relic density constraint, the one-loop cross section is typically below ∼ 10 −50 cm 2 [27] and thus beyond the expected reach of future direct detection experiments, e.g., LUX-ZEPLIN (LZ) [29] and DARWIN [30].More recently, the pNG DM model was confronted against the constraints from perturbative unitarity, DM relic density, Higgs invisible decay, XENON1T, Fermi-LAT dwarf spheroidal (dSph) galaxies [31] and LHC searches at √ s = 13 TeV [25,[32][33][34]. Projected limits from DA...

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“…Moreover, an excess of GeV-scale gamma-rays from the Inner Galaxy has now been firmly confirmed [13][14][15][16][17][18][19]. Although these two signals are sensitive to very different systematic uncertainties and backgrounds, it is intriguing that they could both be explained by a ∼60 GeV dark matter particle with an annihilation cross section near that predicted for a generic thermal relic [17,[20][21][22][23]. The concordance between these two signals is suggestive and provides considerable motivation for additional indirect searches for dark matter (see e.g.…”

Section: Introductionmentioning

confidence: 99%

A robust excess in the cosmic-ray antiproton spectrum: Implications for annihilating dark matter

2019

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An excess of ∼10-20 GeV cosmic-ray antiprotons has been identified in the spectrum reported by the AMS-02 Collaboration. The systematic uncertainties associated with this signal, however, have made it difficult to interpret these results. In this paper, we revisit the uncertainties associated with the time, charge and energy-dependent effects of solar modulation, the antiproton production cross section, and interstellar cosmic-ray propagation. After accounting for these uncertainties, we confirm the presence of a 4.7σ antiproton excess, consistent with that arising from a mχ ≈ 64 − 88 GeV dark matter particle annihilating to bb with a cross section of σv (0.8 − 5.2) × 10 −26 cm 3 /s. If we allow for the stochastic acceleration of secondary antiprotons in supernova remnants, the data continues to favor a similar range of dark matter models (mχ ≈ 46−94 GeV, σv ≈ (0.7−3.8)×10 −26 cm 3 /s) with a significance of 3.3σ. The same range of dark matter models that are favored to explain the antiproton excess can also accommodate the excess of GeV-scale gamma rays observed from the Galactic Center.

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Probing dark matter annihilation in the Galaxy with antiprotons and gamma rays

Cited by 77 publications

References 84 publications

GeV-scale thermal WIMPs: Not even slightly ruled out

GeV-scale thermal WIMPs: Not even slightly ruled out

Global fit of pseudo-Nambu-Goldstone Dark Matter

A robust excess in the cosmic-ray antiproton spectrum: Implications for annihilating dark matter

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