Search for Boosted Dark Matter Interacting with Electrons in Super-Kamiokande

Kachulis, C.; Abe, K.; Bronner, C.; Hayato, Y.; Ikeda, M.; Iyogi, K.; Kameda, J.; Kato, Y.; Kishimoto, Y.; Marti, Ll.; Miura, M.; Moriyama, S.; Nakahata, M.; Nakano, Y.; Nakayama, S.; Okajima, Y.; Orii, A.; Pronost, G.; Sekiya, H.; Shiozawa, M.; Sonoda, Y.; Takeda, Atsushi; Takenaka, A.; Tasaka, S.; Tomura, T.; Akutsu, R.; Kajita, T.; Kaneyuki, K.; Nishimura, Y.; Okumura, K.; Tsui, K. M.; Labarga, L.; Fernández, P.; Blaszczyk, F. d. M.; Gustafson, J.; Kearns, E.; Raaf, J. L.; Stone, J. L.; Sulak, L.; Berkman, S.; Tobayama, S.; Goldhaber, M.; Elnimr, M.; Kropp, W. R.; Mine, S.; Locke, S.; Weatherly, P.; Smy, M. B.; Sobel, H. W.; Takhistov, Volodymyr; Ganezer, K. S.; Hill, J.; Kim, J Y; Lim, I. T.; Park, R G; Himmel, A.; Li, Z; O’Sullivan, Erin; Scholberg, K.; Walter, C. W.; Ishizuka, T.; Nakamura, T.; Jang, J. S.; Choi, K.; Learned, J. G.; Matsuno, S.; Smith, S. N.; Amey, Jake Lewis; Litchfield, R. P.; Y, W; Uchida, Y.; Wascko, M. O.; Cao, S.; Friend, M.; Hasegawa, T.; Ishida, Toru; Ishii, T.; Kobayashi, T.; Nakadaira, T.; Nakamura, Kenzo; Oyama, Y.; Sakashita, K.; Sekiguchi, T.; Tsukamoto, T.; Abe, K.; Hasegawa, M.; Suzuki, A.; Takeuchi, Y.; Yano, T.; Hayashino, T.; Hiraki, T.; Hirota, S.; Huang, K.; Jiang, M.; Nakamura, K.; Nakaya, T.; Quilain, B.; Patel, N. D.; Wendell, R.; Anthony, L. H. V.; McCauley, N.; Pritchard, A.; Fukuda, Y.; Itow, Y.; Murase, M.; Muto, Fumihito; Mijakowski, P.; Frankiewicz, K.; Jung, C. K.; Li, X; Palomino, J. L.; Santucci, G.; Vilela, C.; Wilking, M. J.; Yanagisawa, C.; Ito, S.; Fukuda, Daisuke; Ishino, H.; Kibayashi, A.; Koshio, Y.; Nagata, Hiroshi; Sakuda, M.; Xu, Chenyuan; Kuno, Y.; Wark, D.; Lodovico, F. Di; Richards, B.; Tacik, R.; Kim, S B; Cole, A. A.; Thompson, L. F.; Okazawa, H.; Choi, Y.; Ito, K.; Nishijima, K.; Koshiba, M.; Totsuka, Y.; Suda, Y.; Yokoyama, M.; Calland, R. G.; Hartz, M.; Martens, K.; Simpson, C.; Suzuki, Yoshihiro; Vagins, M. R.; Hamabe, D.; Kuze, M.; Yoshida, Tadashi; Ishitsuka, M.; Martin, J. F.; Nantais, C.; Tanaka, Hirohisa; Konaka, A.; Chen, S; Wan, L.; Zhang, Y; Wilkes, R. J.; Minamino, A.

doi:10.1103/physrevlett.120.221301

Cited by 60 publications

(82 citation statements)

References 50 publications

(58 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…If the speed of these recoiling electrons is > 0.75c, they emit detectable Cherenkov light. Such events are detected by Super-Kamiokande for deposition energies above the threshold of 100 MeV [62]. The main target of the search is dark matter coming from the center of the galaxy, and constraints are put on events within a cone with a certain opening angle measured from the center of the galaxy.…”

Section: Relativistic Electron Recoil and Subsequent Cherenkov Lightmentioning

confidence: 99%

“…Below the dashed line, the maximum momentum of accelerated CHAMPs is below the threshold, m 100 MeV/m e . For q > 0.1, photomultiplier tubes (PMTs) in the outer detector typically receive more than one photon from the Cherenkov radiation of CHAMPs, giving events that are vetoed in the analysis of [62]. The integrated flux of atmospheric muons 2 km below the Antarctic ice is Φ µ /4π ≈ 10 −7 cm −2 s −1 sr −1 [64] and contributes 3% [63] of the background rate.…”

Section: Relativistic Electron Recoil and Subsequent Cherenkov Lightmentioning

confidence: 99%

See 1 more Smart Citation

CHAMP cosmic rays

Dunsky

Hall

Harigaya

2019

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

We study interactions of cosmological relics, X, of mass m and electric charge qe in the galaxy, including thermalization with the interstellar medium, diffusion through inhomogeneous magnetic fields and Fermi acceleration by supernova shock waves. We find that for m < ∼ 10 10 q GeV, there is a large flux of accelerated X in the disk today, with a momentum distribution ∝ 1/p 2.5 extending to (βp) max ∼ 5 × 10 4 q GeV. Even though acceleration in supernova shocks is efficient, ejecting X from the galaxy, X are continually replenished by diffusion into the disk from the halo or confinement region. For m > ∼ 10 10 q GeV, X cannot be accelerated above the escape velocity within the lifetime of the shock. The accelerated X form a component of cosmic rays that can easily reach underground detectors, as well as deposit energies above thresholds, enhancing signals in various experiments. We find that nuclear/electron recoil experiments place very stringent bounds on X at low q; for example, X as dark matter is excluded for q > 10 −9 and m < 10 5 GeV. For larger q or m, stringent bounds on the fraction of dark matter that can be X are set by Cherenkov and ionization detectors. Nevertheless, very small q is highly motivated by the kinetic mixing portal, and we identify regions of (m, q) that can be probed by future experiments.

show abstract

Section: Relativistic Electron Recoil and Subsequent Cherenkov Lightmentioning

confidence: 99%

Section: Relativistic Electron Recoil and Subsequent Cherenkov Lightmentioning

confidence: 99%

CHAMP cosmic rays

Dunsky

Hall

Harigaya

2019

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

show abstract

“…For the dark-strahlung channel, we assume the all-sky survey (i.e., θ C = 180 • ) and negligible background, whereas for the leading-order, we consider two more search cones, θ C = 10 • (dot-dashed lines) and θ C = 40 • (dashed lines) as per suggestions in Refs. [1,4], in addition to the all-sky survey (solid lines). The number of neutrino-induced background events for the leading-order process is calculated with Eqs.…”

Section: Experimental Sensitivities Of Dunementioning

confidence: 99%

“…The models of boosted dark matter (BDM) are receiving rising attention [1,2] as an alternative scenario to reconcile the paradigm of thermal dark-matter with the null observation of dark-matter-induced signatures via non-gravitational interactions [3,4]. Many of them predict that some (subdominant) dark-matter components can be substantially boosted in the present universe and manifest themselves by relativistic scattering signatures in terrestrial detectors.…”

Section: Introductionmentioning

confidence: 99%

Searching for boosted dark matter via dark-photon bremsstrahlung

2019

View full text Add to dashboard Cite

We propose a new search channel for boosted dark matter (BDM) signals coming from the present universe, which are distinct from simple neutrino signals including those coming from the decay or pair-annihilation of dark matter. The signal process is initiated by the scattering of high-energetic BDM off either an electron or a nucleon. If the dark matter is dark-sector U(1)-charged, the scattered BDM may radiate a dark gauge boson (called "dark-strahlung") which subsequently decays to a Standard Model fermion pair. We point out that the existence of this channel may allow for the interpretation that the associated signal stems from BDM, not from the dark-matter-origin neutrinos. Although the dark-strahlung process is generally subleading compared to the lowestorder simple elastic scattering of BDM, we find that the BDM with a significant boost factor may induce an O(10 − 20%) event rate in the parameter regions unreachable by typical beam-produced dark-matter. We further find that the dark-strahlung channel may even outperform the leadingorder channel in the search for BDM, especially when the latter is plagued by substantial background contamination. We argue that cosmogenic BDM searches readily fall in such a case, hence taking full advantage of dark-strahlung. As a practical application, experimental sensitivities expected in the leading-order and dark-strahlung channels are contrasted in dark gauge boson parameter space, under the environment of DUNE far-detectors, revealing usefulness of dark-strahlung.

show abstract

“…In this paper, we demonstrate that large underground neutrino detectors as well as large directional dark matter detectors can provide a new method to probe inelastic dark matter. Other proposed searches for dark matter that could yield a signal in neutrino detectors include dark matter that destroys target baryons [25][26][27][28], dark matter that yields annihilation or decay products detectable in these experiments [29][30][31][32][33][34][35][36][37][38][39], self-destructing dark matter [40], dark matter produced at high-intensity accelerators or radioactive sources [41], or dark matter bounced off energetic cosmic rays [41,42]. Consider a dark matter particle with mass of order a TeV traversing through the Earth.…”

Section: Introductionmentioning

confidence: 99%

Luminous signals of inelastic dark matter in large detectors

Eby

Fox

Harnik

et al. 2019

J. High Energ. Phys.

View full text Add to dashboard Cite

We study luminous dark matter signals in models with inelastic scattering. Dark matter χ 1 that scatters inelastically off elements in the Earth is kicked into an excited state χ 2 that can subsequently decay into a monoenergetic photon inside a detector. The photon signal exhibits large sidereal-daily modulation due to the daily rotation of the Earth and anisotropies in the problem: the dark matter wind comes from the direction of Cygnus due to the Sun's motion relative to the galaxy, and the rock overburden is anisotropic, as is the dark matter scattering angle. This allows outstanding separation of signal from backgrounds. We investigate the sensitivity of two classes of large underground detectors to this modulating photon line signal: large liquid scintillator neutrino experiments, including Borexino and JUNO, and the proposed large gaseous scintillator directional detection experiment CYGNUS. Borexino's (JUNO's) sensitivity exceeds the bounds from xenon experiments on inelastic nuclear recoil for mass splittings δ > ∼ 240(180) keV, and is the only probe of inelastic dark matter for 350 keV < ∼ δ < ∼ 600 keV. CYGNUS's sensitivity is at least comparable to xenon experiments with ∼ 10 m 3 volume detector for δ < ∼ 150 keV, and could be substantially better with larger volumes and improved background rejection. Such improvements lead to the unusual situation that the inelastic signal becomes the superior way to search for dark matter even if the elastic and inelastic scattering cross sections are comparable.

show abstract

Search for Boosted Dark Matter Interacting with Electrons in Super-Kamiokande

Cited by 60 publications

References 50 publications

CHAMP cosmic rays

CHAMP cosmic rays

Searching for boosted dark matter via dark-photon bremsstrahlung

Luminous signals of inelastic dark matter in large detectors

Contact Info

Product

Resources

About