Searching for a U-boson with a positron beam

Wojtsekhowski, B.; Elouadrhiri, L.; Grames, Jospeh; Melnitchouk, Wally; Voutier, E.; Forest, Tony A.

doi:10.1063/1.3232023

Cited by 32 publications

(28 citation statements)

References 11 publications

(16 reference statements)

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“…Belle-II could explore the remaining m >GeV portion of this target if mono-photon triggers are implemented [22]. Beyond dark matter physics, the approach we advocate will play an important role in improving sensitivity to kinetically mixed dark photons that decay invisibly, nicely complementing the ongoing program of searches for visible decays [33,34,[41][42][43][44][45][46][47][48][49][50][51][52][53][54][55][56][57][58][59][60]. Indeed, while the window identified six years ago for visibly decaying dark photons to explain the muon g − 2 anomaly has recently been closed [61], the corresponding parameter space for invisibly decaying dark-photons has not been fully explored.…”

Section: Introductionmentioning

confidence: 99%

Testing GeV-scale dark matter with fixed-target missing momentum experiments

et al. 2015

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We describe an approach to detect dark matter and other invisible particles with mass below a GeV, exploiting missing energy-momentum measurements and other kinematic features of fixedtarget production. In the case of an invisibly decaying MeV-GeV-scale dark photon, this approach can improve on present constraints by 2-6 orders of magnitude over the entire mass range, reaching sensitivity as low as 2 ∼ 10 −14 . Moreover, the approach can explore essentially all of the viable parameter space for thermal or asymmetric dark matter annihilating through the vector portal.

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Section: Introductionmentioning

confidence: 99%

Testing GeV-scale dark matter with fixed-target missing momentum experiments

et al. 2015

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“…Of these, collider searches [20][21][22][23] can cover the widest range of gauge boson masses, while fixed-target experiments are sensitive to the widest range of couplings, but at lower masses [22,24,25]. Most fixed-target results [26][27][28][29][30][31][32][33] and recent proposals [34][35][36][37][38][39] have the greatest reach at masses below ∼ 200 MeV, the region where substructure effects can be most dramatic. Understanding the role of substructure is essential to clarify what regions of parameter space have astrophysical motivation.…”

Section: Introductionmentioning

confidence: 99%

Sommerfeld-enhanced annihilation in dark matter substructure: Consequences for constraints on cosmic-ray excesses

2012

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In models of dark matter with Sommerfeld-enhanced annihilation, where the annihilation rate scales as the inverse velocity, N -body simulations of dark matter structure formation suggest that the local annihilation signal may be dominated by small, dense, cold subhalos. This contrasts with the usual assumption of a signal originating from the smooth dark matter halo, with much higher velocity dispersion. Accounting for local substructure modifies the parameter space for which Sommerfeld-enhanced annihilating DM can explain the PAMELA and Fermi excesses. Limits from the inner galaxy and the CMB are weakened, without introducing new tension with substructuredependent limits, such as from dwarf galaxies or isotropic gamma-ray studies. With substructure, previously excluded parameter regions with mediators of mass ∼ 1-200 MeV are now easily allowed. For O(MeV) mediators, subhalos in a specific range of host halo masses may be evaporated, further suppressing diffuse signals without affecting substructure in the Milky Way.PACS numbers: 95.35.+d

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“…As shown in [36,37], dark matter annihilating via a light mediator can fit these data well for an approximately thermal cross section. Thus, the combination of these signals (X-ray and gamma-ray) motivate additional low energy searches for the mediator φ [38][39][40][41], such as those at APEX [40,42], MAMI [43], HPS [44] and DarkLight [45], searches at low energye + e − colliders [46][47][48][49][50] as well LHC searches [51,52] for the associated lepton jets signal [53,54]. (For a review, see [55].…”

Section: B Galactic Centermentioning

confidence: 99%

X-ray line from exciting dark matter

Finkbeiner

Weiner

2016

Phys. Rev. D

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The eXciting Dark Matter (XDM) model was proposed as a mechanism to efficiently convert the kinetic energy (in sufficiently hot environments) of dark matter into e+e-pairs. The standard scenario invokes a doublet of nearly degenerate DM states, and a dark force to mediate a large upscattering cross section between the two. For heavy (∼ TeV) DM, the kinetic energy of WIMPs in large (galaxy-sized or larger) halos is capable of producing low-energy positrons. For lighter dark matter, this is kinematically impossible, and the unique observable signature becomes an X-ray line, arising from χχ → χ * χ * , followed by χ * → χγ. This variant of XDM is distinctive from other DM X-ray scenarios in that its signatures tend to be most present in more massive, hotter environments, such as clusters, rather than nearby dwarfs, and has different dependencies from decaying models.We find that it is capable of explaining the recently reported X-ray line at 3.56 keV. For very long lifetimes of the excited state, primordial decays can explain the signal without the presence of upscattering. Thermal models freeze-out as in the normal XDM setup, via annihilations to the light boson φ. For suitable masses the annihilation χχ → φφ followed by φ → SM can explain the reported gamma-ray signature from the galactic center. Direct detection is discussed, including the possibility of explaining DAMA via the "Luminous" dark matter approach. Quite generally, the proximity of the 3.56 keV line to the energy scale of DAMA motivates a reexamination of electromagnetic explanations. Other signals, including lepton jets and the modification of cores of dwarf galaxies are also considered.PACS numbers: 95.35.+d

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Searching for a U-boson with a positron beam

Cited by 32 publications

References 11 publications

Testing GeV-scale dark matter with fixed-target missing momentum experiments

Testing GeV-scale dark matter with fixed-target missing momentum experiments

Sommerfeld-enhanced annihilation in dark matter substructure: Consequences for constraints on cosmic-ray excesses

X-ray line from exciting dark matter

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