Indirect search for dark matter from the Galactic Center and halo with the Super-Kamiokande detector

Bronner, C.; Haga, Y.; Hayato, Y.; Ikeda, M.; Imaizumi, S.; Itô, Hiroshi; Iyogi, K.; Kameda, J.; Kataoka, Y.; Kato, Y.; Kishimoto, Y.; Marti, Ll.; Miura, Makoto; Moriyama, S.; Mochizuki, T.; Nagao, Y.; Nakahata, M.; Nakajima, Yoshikazu; Nakajima, Tetsuo; Nakayama, S.; Okada, Taku; Orii, A.; Pronost, G.; Sekiya, H.; Shiozawa, M.; Sonoda, Y.; Takeda, Atsushi; Takenaka, A.; Tasaka, S.; Tomura, T.; Ueno, K.; Yano, T.; Yokozawa, T.; Akutsu, R.; Han, S.; Irvine, T. J.; Kajita, T.; Kametani, I.; Lee, K. P.; Mclachlan, T. C.; Okumura, K.; Richard, E.; Tashiro, T.; Wang, R.; Xia, J. K.; Bravo-Berguño, D.; Labarga, L.; Fernández, P.; Blaszczyk, F. d. M.; Gustafson, J.; Kachulis, C.; Kearns, E.; Raaf, J. L.; Stone, J. L.; Sulak, L.; Sussman, S.; Wan, L.; Wester, T.; Berkman, S.; Tobayama, S.; Bian, J. G.; Carminati, G.; Elnimr, M.; Griskevich, N. J.; Kropp, W. R.; Locke, S.; Mine, S.; Renshaw, A.; Smy, M. B.; Sobel, H. W.; Takhistov, Volodymyr; Weatherly, P.; Hartfiel, B. L.; Hill, J.; Keig, W. E.; Hồng, Nguyễn Thị; Kim, J. Y.; Lim, I. T.; Park, R. G.; Akiri, T.; Bodur, B.; Himmel, A.; Li, Z.; O’Sullivan, Erin; Scholberg, K.; Walter, Christopher W.; Wongjirad, T.; Coffani, A.; Drapier, O.; Hedri, Sonia El; Giampaolo, A.; Gonin, M.; Imber, J.; Mueller, T.; Paganini, P.; Quilain, B.; Ishizuka, T.; Nakamura, T.; Jang, J. S.; Choi, K.; Learned, J. G.; Matsuno, S.; Smith, S. N.; Amey, Jake Lewis; Anthony, L. H. V.; Litchfield, R. P.; Y., W.; Sztuc, A. A.; Uchida, Y.; Wascko, M. O.; Berardi, V.; Catanesi, Maria Gabriella; Intonti, R. A.; Radicioni, E.; Calabria, N. F.; Machado, L. N.; Rosa, G. De; Collazuol, G.; Iacob, F.; Lamoureux, Mathieu; Ospina, N.; Ludovici, L.; Boschi, T.; Lodovico, F. Di; Sedgwick, S. Molina; Zsoldos, S.; Nishimura, Y.; Cao, S.; Friend, M.; Hasegawa, T.; Ishida, Toru; Ishii, T.; Kobayashi, T.; Nakadaira, T.; Nakamura, K.; Oyama, Y.; Sakashita, K.; Sekiguchi, T.; Tsukamoto, T.; Abe, K.; Hasegawa, M.; Isobe, Yuki; Miyabe, H.; Nakano, Y.; Shiozawa, T.; Sugimoto, Takashi; Suzuki, A.; Takeuchi, Y.; Yamamoto, Shuji; Ali, Ahmed Farag; Ashida, Yosuke; Hayashino, T.; Hiraki, T.; Hirota, S.; Huang, K.; Ieki, K.; Jiang, M.; Kikawa, T.; Mori, Masao; Murakami, Akira; Nakamura, K.; Nakaya, T.; Patel, N. D.; Suzuki, Kenta; Takahashi, Sentaro; Tateishi, K.; Wendell, R.; McCauley, N.; Mehta, Poonam; Pritchard, A.; Tsui, K. M.; Fukuda, Y.; Itow, Y.; Menjo, H.; Mitsuka, G.; Murase, M.; Muto, Fumihito; Niwa, T.; Sato, K.; Suzuki, T.; Taani, M.; Tsukada, M.; Mijakowski, P.; Frankiewicz, K.; Hignight, J.; Jung, C. K.; Li, X.; Palomino, J. L.; Santucci, G.; Vilela, C.; Wilking, M. J.; Yanagisawa, C.; Fukuda, Daisuke; Hagiwara, Kaoru; Harada, Masayuki; Horai, T.; Ishino, H.; Ito, S.; Kayano, T.; Kibayashi, A.; Koshio, Y.; Ma, W.; Mori, Takaaki; Nagata, Hiroshi; Piplani, N.; Sakuda, M.; Seiya, S.; Takahira, Y.; Xu, Chenyuan; Yamaguchi, R.; Kuno, Y.; Barr, G.; Barrow, D.; Cook, L.; Simpson, C.; Wark, D.; Nova, F.; Tacik, R.; Yang, J.; Cole, A. A.; Jenkins, S. J.; McElwee, J.; Thiesse, M.; Thompson, L. F.; Okazawa, H.; Kim, S. B.; Choi, Y.; Ito, K.; Nishijima, K.; Iwamoto, K.; Koshiba, M.; Suda, Y.; Yokoyama, M.; Calland, R. G.; Goldsack, A.; Martens, K.; Murdoch, M.; Suzuki, Yoshihiro; Vagins, M.; Hamabe, D.; Kuze, M.; Okajima, Y.; Tanaka, Masayuki; Yoshida, T.; Inomoto, M.; Ishitsuka, M.; Matsumoto, R.; Ohta, Kouji; Shinoki, M.; Martin, J. F.; Nantais, C.; Tanaka, Hirohisa; Towstego, T.; Hartz, M.; Konaka, A.; Perio, P. de; Prouse, N. W.; Chen, S.; Xu, B. D.; Zhang, Y.; Richards, B.; Connolly, K.; Wilkes, R. J.; Jamieson, B.; Walker, John M.; Giorgio, P.; Minamino, A.; Okamoto, Ken‐ichi; Pintaudi, G.

doi:10.1103/physrevd.102.072002

Cited by 35 publications

(42 citation statements)

References 48 publications

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“…The dark matter annihilating into neutrinos have also been probed by various experiments, the lowerright subfigure shows the experimental limits on cross section of ν LνL final states and the corresponding predictions in our model, both equations (4.4) and (4.6) could contribute to the annihilation. Current bounds from Super-K [98], IceCube [99], and ANTARES [100] are at most able to exclude σv ∼ 10 −24 cm 3 s −1 , which are far beyond the thermal annihilation cross section, hence cannot exclude any parameters in our model.…”

Section: Indirect Detectionmentioning

confidence: 96%

Observable signatures of scotogenic Dirac model

Guo

Han

2020

J. High Energ. Phys.

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In this work, we make a detailed discussion on the phenomenology of the scotogenic Dirac model, which could accommodate the Dirac neutrino mass and dark matter. We have studied the lepton-flavor-violating (LFV) processes in this model, which are mediated by the charged scalar ϕ± and heavy Dirac fermions Ni. The experimental bounds, especially given by decays μ → eγ and μ → 3e, have put severe constraints on the Yukawa couplings yΦ and masses mN1, mϕ. We select the heavy Dirac fermion N1 as dark matter candidate and find the correct relic density will be reached basically by annihilating through another Yukawa coupling yχ. After satisfying LFV and dark matter relic density constraints, we consider the indirect detections of dark matter annihilating into leptons. But the constraints are relatively loose, only the τ+τ− channel can impose a mild excluding capability. Then we make a detailed discussion on the dark matter direct detections. Although two Yukawa couplings can both contribute to the direct detection processes, more attention has been paid on the yΦ-related processes as the yχ-related process is bounded loosely. The current and future direct detection experiments have been used to set constraints on the Yukawa couplings and masses. The current direct detections bounds are relatively loose and can barely exclude more parameter region beyond the LFV. For the future direct detection experiments, the excluding capacities can be improved due to larger exposures. The detecting capabilities in the large mass region have not been weakened as the existence of mass enhancement from the magnetic dipole operator $$ {\mathcal{O}}_{\mathrm{mag}.} $$ O mag . . At last, we have briefly discussed the collider signal searching in this model, the most promising signature is pair produced ϕ+ϕ− and decay into the signal of ℓ+ℓ− + ɆT. The exclusion limits from collider on mN1 and mϕ have provided a complementary detecting capability compared to the LFV and dark matter detections.

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Section: Indirect Detectionmentioning

confidence: 96%

Observable signatures of scotogenic Dirac model

Guo

Han

2020

J. High Energ. Phys.

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“…< 0.11 (0.19), (5.5) as well as on the elastic and inelastic scattering cross section from direct searches with XENON1T [57], XENON100 [58,59] and PandaX-II [60]. The possible signal from DAMA/LIBRA [20,21], its ongoing verification [61][62][63], previous limits on indirect detection from DM annihilation into neutrinos in the Sun [43,64,65] and the Galactic Center [66][67][68][69], and expected event rates for neutrinos from the Sun in the current IceCube configuration with 86 strings (IC86) are also discussed in the following.…”

Section: Numerical Scanmentioning

confidence: 98%

Indirect detection constraints on the scotogenic dark matter model

Boer¹,

Busse²,

Kappes³

et al. 2021

Preprint

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Radiative seesaw models have the attractive property of providing dark matter candidates in addition to the generation of neutrino masses. Here we present a study of neutrino signals from the annihilation of dark matter particles that have been gravitationally captured in the Sun in the framework of the scotogenic model. We compute expected event rates in the IceCube detector in its 86-string configuration. As fermionic dark matter does not scatter off nucleons due to its singlet nature and therefore does not accumulate in the Sun, we study the case of scalar dark matter with a scan over the parameter space. Due to a naturally small mass splitting between the two neutral scalar components, inelastic scattering processes with nucleons can occur. We find that for most of the parameter space, i.e. for mass splittings below 500 keV, inelastic scattering in the Sun yields IceCube event rates above 10 events per year, whereas direct detection on Earth is sensitive only to 250 keV. Consequently, a detailed analysis with IceCube could lead to a lower limit on the scalar coupling λ 5 1.6 • 10 −5 • m DM /TeV. For larger mass splittings, only elastic scattering occurs in the Sun. In this case, XENON1T limits only allow for models with expected event rates of up to O(0.1) per year. Some of these models, in particular those with large DM mass and fermion coannihilation, could also be tested with a dedicated IceCube analysis of DM annihilation in the Galactic Center.

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“…Since the start of data taking on 1st April 1996, the Super-Kamiokande experiment has spent the last quarter century conducting ground-breaking studies of neutrinos from the Earth's atmosphere [26], the Sun [27,28], and long-baseline accelerator-generated beams from KEK [29] and J-PARC [30], while also searching for nucleon decay [31][32][33][34], dark matter [35,36], and both galactic [37,38] and diffuse supernova neutrinos [12,[39][40][41]. The discovery of neutrino oscillations in SK's atmospheric neutrino data resulted in a share of the 2015 Nobel Prize in physics, while those results plus SK's solar and long-baseline neutrino measurements led to a share of two 2016 Breakthrough Prizes.…”

Section: Super-kamiokande With Gadolinium-doping (Sk-gd) 31 a Brief H...mentioning

confidence: 99%

Prospects for the Detection of the Diffuse Supernova Neutrino Background with the Experiments SK-Gd and JUNO

Vagins

Wurm

2022

Universe

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The advent of gadolinium-loaded Super-Kamiokande (SK-Gd) and of the soon-to-start JUNO liquid scintillator detector marks a substantial improvement in global sensitivity for the Diffuse Supernova Neutrino Background (DSNB). The present article reviews the detector properties most relevant for the DSNB searches in both experiments and estimates the expected signal and background levels. Based on these inputs, we evaluate the sensitivity of both experiments individually and combined. Using a simplified statistical approach, we find that both SK-Gd and JUNO have the potential to reach >3σ evidence of the DSNB signal within 10 years of measurement. Combination of their results is likely to enable a 5σ discovery of the DSNB signal within the next decade.

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Indirect search for dark matter from the Galactic Center and halo with the Super-Kamiokande detector

Abstract: We present a search for an excess of neutrino interactions due to dark matter in the form of weakly interacting massive particles (WIMPs) annihilating in the Galactic center or halo based on the data set of

Cited by 35 publications

References 48 publications

Observable signatures of scotogenic Dirac model

Observable signatures of scotogenic Dirac model

Indirect detection constraints on the scotogenic dark matter model

Prospects for the Detection of the Diffuse Supernova Neutrino Background with the Experiments SK-Gd and JUNO

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