Imprint of multicomponent dark matter on AMS-02

Geng, Chao–Qiang; Huang, Da; Tsai, Lu‐Hsing

doi:10.1103/physrevd.89.055021

Cited by 27 publications

(23 citation statements)

References 125 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This result triggered significant interest as it seems consistent with a long-sought-for signal from dark matter decay , annihilation [11,35,48], de-excitation [11,[49][50][51][52][53][54][55][56][57][58] or conversion in the magnetic field [59][60][61]. Many particle physics models that predict such properties for the dark matter particle, have been put forward, including sterile neutrino, axion, axino, gravitino and many others, see for reviews e.g.…”

mentioning

confidence: 99%

Checking the Dark Matter Origin of a 3.53 keV Line with the Milky Way Center

et al. 2015

View full text Add to dashboard Cite

We detect a line at 3.539 ± 0.011 keV in the deep exposure dataset of the Galactic Center region, observed with the XMM-Newton. The dark matter interpretation of the signal observed in the Perseus galaxy cluster, the Andromeda galaxy [1] and in the stacked spectra of galaxy clusters [2], together with non-observation of the line in blank sky data, put both lower and upper limits on the possible intensity of the line in the Galactic Center data. Our result is consistent with these constraints for a class of Milky Way mass models, presented previously by observers, and would correspond to radiative decay dark matter lifetime τDM ∼ 6 − 8 × 10 27 sec. Although it is hard to exclude an astrophysical origin of this line based the Galactic Center data alone, this is an important consistency check of the hypothesis that encourages to check it with more observational data that are expected by the end of 2015.Recently, two independent groups [1, 2] reported a detection of an unidentified X-ray line at energy 3.53 keV in the long-exposure X-ray observations of a number of dark matterdominated objects. The authors of [2] have observed this line in a stacked XMM spectrum of 73 galaxy clusters spanning a redshift range 0.01 − 0.35 and separately in subsamples of nearby and remote clusters. Ref. [1] have found this line in the outskirts of the Perseus cluster and in the central 14 ′ of the Andromeda galaxy. The global significance of detection of the same line in the datasets of Ref.[1] is 4.3σ (taking into account the trial factors); the signal in [2] has significance above 4σ based on completely independent data.The position of the line is correctly redshifted between galaxy clusters [2] and between the Perseus cluster and the Andromeda galaxy [1]. In a very long exposure blank sky observation (15.7 Msec of cleaned data) the feature is absent [1]. This makes it unlikely that an instrumental effect is at the origin of this feature (e.g. an unmodeled wiggle in the effective area).To identify this spectral feature with an atomic line in galaxy clusters, one should assume a strongly super-solar abundance of potassium or some anomalous argon transition [2]. Moreover, according to the results of [1] this should be true not only in the center of the Perseus cluster considered in [2], but also (i) in its outer parts up to at least 1/2 of its virial radius and (ii) in the Andromeda galaxy.This result triggered significant interest as it seems consistent with a long-sought-for signal from dark matter decay , annihilation [11, 35, 48], de-excitation [11, 49-58] or conversion in the magnetic field [59][60][61]. Many particle physics models that predict such properties for the dark matter particle, have been put forward, including sterile neutrino, axion, axino, gravitino and many others, see for reviews e.g. [37,62] and references therein. If the interaction of dark matter particles is weak enough (e.g. much weaker than that of the Standard Model neutrino), they need not to be stable as their lifetime can exceed the age of the Universe...

show abstract

mentioning

confidence: 99%

Checking the Dark Matter Origin of a 3.53 keV Line with the Milky Way Center

et al. 2015

View full text Add to dashboard Cite

show abstract

“…Since direct and indirect detection (considering annihilations only, for stable DM) rates of DM are directly proportional to the DM density and DM density squared respectively, multi-component DM models can find larger allowed region of parameter space by appropriate tuning of their relative abundance. In addition to that, such multi-component DM scenarios often give rise to very interesting signatures at direct and indirect detection experiments [23,32,37,[52][53][54][55][56][57][58][59][60][61][62][63][64][65][66][67][68][69].…”

Section: Introductionmentioning

confidence: 99%

Type III seesaw for neutrino masses in U(1)B−L model with multi-component dark matter

Biswas

Borah

Nanda

2019

J. High Energ. Phys.

View full text Add to dashboard Cite

We propose a B − L gauged extension of the Standard Model where light neutrino masses arise from type III seesaw mechanism. Unlike the minimal B −L model with three right handed neutrinos having unit lepton number each, the model with three fermion triplets is however not anomaly free. We show that the leftover triangle anomalies can be cancelled by two neutral Dirac fermions having fractional B − L charges, both of which are naturally stable by virtue of a remnant Z 2 × Z 2 symmetry, naturally leading to a two component dark matter scenario without any ad-hoc symmetries. We constrain the model from all relevant phenomenological constraints including dark matter properties. Light neutrino mass and collider prospects are also discussed briefly. Due to additional neutral gauge bosons, the fermion triplets in type III seesaw can have enhanced production cross section in collider experiment.

show abstract

“…Furthermore, multicomponent DM can provide an alternative solution to the small scale structure problems that are a result of the discrepancy between collisionless cold dark matter and observational data [5]. In addition, studies with multiple dark matter particles have illustrated very interesting phenomenology as well as the potential of providing "smoking gun" signatures in both particle and astrophysical experiments [3,[6][7][8][9][10][11][12][13][14][15][16][17][18][19][20][21][22][23].…”

Section: Introductionmentioning

confidence: 99%

Multi-component dark matter through a radiative Higgs portal

DiFranzo

Mohlabeng

2017

J. High Energ. Phys.

View full text Add to dashboard Cite

Abstract:We study a multi-component dark matter model where interactions with the Standard Model are primarily via the Higgs boson. The model contains vector-like fermions charged under SU(2) W × U(1) Y and under the dark gauge group, U(1) . This results in two dark matter candidates. A spin-1 and a spin-1 2 candidate, which have loop and tree-level couplings to the Higgs, respectively. We explore the resulting effect on the dark matter relic abundance, while also evaluating constraints on the Higgs invisible width and from direct detection experiments. Generally, we find that this model is highly constrained when the fermionic candidate is the predominant fraction of the dark matter relic abundance.

show abstract

Imprint of multicomponent dark matter on AMS-02

Cited by 27 publications

References 125 publications

Checking the Dark Matter Origin of a 3.53 keV Line with the Milky Way Center

Checking the Dark Matter Origin of a 3.53 keV Line with the Milky Way Center

Type III seesaw for neutrino masses in U(1)B−L model with multi-component dark matter

Multi-component dark matter through a radiative Higgs portal

Contact Info

Product

Resources

About