Complex scalar dark matter<i>vis-à-vis</i>CoGeNT, DAMA/LIBRA, and XENON100

Barger, Vernon; McCaskey, Mathew; Shaughnessy, Gabe

doi:10.1103/physrevd.82.035019

Cited by 97 publications

(61 citation statements)

References 105 publications

(126 reference statements)

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“…Except for a typical assumption of S-wave annihilation our results are largely model-independent, so all the particle-physics scenarios motivated by DAMA/LIBRA and CoGeNT results Andreas et al 2010;Chang et al 2010;Foot 2010;Barger et al 2010b;Hooper et al 2010;Essig et al 2010;Barger et al 2010a;Cline et al 2011;Buckley et al 2011) including theoretically wellmotivated particle physics models that predict light DM, such as the MSSM (Feldman et al 2010;Kuflik et al 2010;Fornengo et al 2011;Bottino et al 2010) and the NMSSM (Kang et al 2011;Belikov et al 2011;Gunion et al 2010;Draper et al 2011), are stringently tested by WMAP and Planck.…”

Section: Cmb Constraintsmentioning

confidence: 99%

WMAP7 and future CMB constraints on annihilating dark matter: implications for GeV-scale WIMPs

Hütsi

Chluba

Hektor

et al. 2011

A&A

120

154

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Aims. We calculate constraints from current and future cosmic microwave background (CMB) measurements on annihilating dark matter (DM) with masses below the electroweak scale: m DM = 5−100 GeV. In particular, we assume the S-wave annihilation mode to be dominant, and focus our attention on the lower end of this mass range, as DM particles with masses m DM ∼ 10 GeV have recently been claimed to be consistent with the CoGeNT and DAMA/LIBRA results, while also providing viable DM candidates to explain the measurements of Fermi and WMAP haze. We study the model (in)dependence of the CMB power spectra on particle physics DM models, large-scale structure formation and cosmological uncertainties. We attempt to find a simple and practical recipe for estimating current and future CMB bounds on a broad class of DM annihilation models. Methods. We use a model-independent description for DM annihilation into a wide set of Standard Model particles simulated by PYTHIA Monte Carlo. Our Markov chain Monte Carlo calculations used for finding model constraints involve realistic CMB likelihoods and assume a standard 6-parameter ΛCDM background cosmological model, which is extended by two additional DM annihilation parameters: m DM and σ A υ /m DM . Results. We show that in the studied DM mass range the CMB signal of DM annihilations is independent of the details of large-scale structure formation, distribution, and profile of DM halos and other cosmological uncertainties. All particle physics models of DM annihilation can be described with only one parameter, the fraction of energy carried away by neutrinos in DM annihilation. As the main result we provide a simple and rather generic fitting formula for calculating CMB constraints on the annihilation cross section of light WIMPs. We show that thermal relic DM in the CoGeNT, DAMA/LIBRA favored mass range is in a serious conflict with present CMB data for the annihilation channels with few neutrinos, and will definitely be tested by the Planck mission for all possible DM annihilation channels. Also, our findings strongly disfavor the claim that thermal relic DM annihilations with m DM ∼ 10 GeV and σ A υ ∼ 9 × 10 −25 cm 3 s −1 could be a cause of Fermi and WMAP haze.

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Section: Cmb Constraintsmentioning

confidence: 99%

WMAP7 and future CMB constraints on annihilating dark matter: implications for GeV-scale WIMPs

Hütsi

Chluba

Hektor

et al. 2011

A&A

120

154

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“…Once the constraint from DM relic abundance is imposed, the number of independent model parameters is reduced to one. Since previous experimental data has excluded a fermionic DM (except for the pseudo-scalar coupling) [3], we focus on either a real or complex scalar DM, on which early studies can be found in [4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19][20] and [21][22][23][24][25][26][27] , respectively. 1 In the light of the direct detection arising from the LUX 2016 data, the indirect detection arising from the Higgs invisible decay at LHC [29], and the indirect detection arising from gamma ray spectrum induced by DM annihilation at Fermi-LAT [30,31] and HESS [32], the DM mass regions are updated as follows.…”

Section: Introductionmentioning

confidence: 99%

Scalar dark matter: real vs complex

Zheng

2017

J. High Energ. Phys.

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We update the parameter spaces for both a real and complex scalar dark matter via the Higgs portal. In the light of constraints arising from the LUX 2016 data, the latest Higgs invisible decay and the gamma ray spectrum, the dark matter resonant mass region is further restricted to a narrow window between 54.9−62.3 GeV in both cases, and its large mass region is excluded until 834 GeV and 3473 GeV for the real and complex scalar, respectively.

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“…: SUSY particles (as neutralino [21] or sneutrino in various scenarios [22]), inelastic Dark Matter in various scenarios [23,24], electron interacting dark matter (including WIMP scenarios) [10], a heavy neutrino of the 4-th family, sterile neutrino [11], Kaluza-Klein particles, self-interacting dark matter, axion-like (light pseudoscalar and scalar candidate) [6], mirror dark matter in various scenarios [25], Resonant Dark Matter [26], DM from exotic 4th generation quarks [27], Elementary Black holes, Planckian objects, Daemons, Composite DM [28], Light scalar WIMP through Higgs portal [29], Complex Scalar Dark Matter [30], specific two Higgs doublet models, exothermic DM [31], Secluded WIMPs [32], Asymmetric DM [33], Isospin-Violating Dark Matter [34], Singlet DM [35], Specific GU [36], SuperWIMPs [37], WIMPzilla [38], etc. [39].…”

Section: Introductionmentioning

confidence: 99%

Dark Matter Annual Modulation Results by DAMA/LIBRA

Bernabei

Belli

Cappella

et al. 2013

Springer Proceedings in Physics

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Abstract. The DAMA/LIBRA experiment, running at the Gran Sasso National Laboratory of the I.N.F.N. in Italy, has a sensitive mass of about 250 kg highly radiopure NaI(Tl). It is mainly devoted to the investigation of Dark Matter (DM) particles in the Galactic halo by exploiting the model independent DM annual modulation signature. The present DAMA/LIBRA experiment and the former DAMA/NaI one (the first generation experiment having an exposed mass of about 100 kg) have released so far results corresponding to a total exposure of 1.17 ton × yr over 13 annual cycles. They provide a model independent evidence of the presence of DM particles in the galactic halo at 8.9 σ C.L. on the basis of the investigated DM signature. The data of another annual cycle in the same DAMA/LIBRA running conditions are at hand. After the replacement at the end of 2012 of all the photomultipliers (PMTs) with new ones, having higher quantum efficiency, DAMA/LIBRA has entered to its phase 2; such a replacements allowed the lowering of the software energy threshold of the experiment in the present data taking. A short summary of the obtained results is presented and future perspectives of the experiment mentioned.

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Complex scalar dark mattervis-à-visCoGeNT, DAMA/LIBRA, and XENON100

Cited by 97 publications

References 105 publications

WMAP7 and future CMB constraints on annihilating dark matter: implications for GeV-scale WIMPs

WMAP7 and future CMB constraints on annihilating dark matter: implications for GeV-scale WIMPs

Scalar dark matter: real vs complex

Dark Matter Annual Modulation Results by DAMA/LIBRA

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