Search for neutrinos from dark matter self-annihilations in the center of the Milky Way with 3 years of IceCube/DeepCore

Aartsen, M. G.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Samarai, I. Al; Altmann, D.; Andeen, K.; Anderson, W. G.; Ansseau, I.; Anton, Gisela; Argüelles, C.; Auffenberg, J.; Axani, Spencer; Bagherpour, H.; Bai, X.; Barron, J. P.; Barwick, S. W.; Baum, V.; Bay, R.; Beatty, J. J.; Tjus, J. Becker; Becker, K. H.; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, Summer; Böhm, C.; Börner, M.; Bos, F.; Bose, D.; Böser, S.; Botner, O.; Bourbeau, J.; Bradascio, Federica; Braun, J.; Brayeur, L.; Brenzke, M.; Bretz, H.-P.; Bron, S.; Burgman, A.; Carver, T.; Casey, J.; Casier, M.; Cheung, E.; Chirkin, D.; Christov, A.; Clark, K.; Classen, L.; Coenders, S.; Collin, Gabriel; Conrad, J. M.; Cowen, D. F.; Cross, R.; Day, M.; André, J. P. A. M. de; Clercq, C. De; DeLaunay, James; Dembinski, H.-P.; Ridder, S. De; Desiati, P.; Vries, Krijn de; Wasseige, G. de; DeYoung, T.; Díaz-Vélez, J. C.; Lorenzo, V. di; Dujmović, Hrvoje; Dumm, J. P.; Dunkman, M.; Eberhardt, B.; Ehrhardt, Thomas; Eichmann, B.; Eller, P.; Evenson, P. A.; Fahey, S.; Fazely, A. R.; Felde, J.; Filimonov, K.; Finley, C.; Flis, S.; Franckowiak, A.; Friedman, E.; Fuchs, T.; Gaisser, T. K.; Gallagher, John S.; Gerhardt, L.; Ghorbani, K.; Giang, W.; Glauch, Theo; Glüsenkamp, T.; Goldschmidt, A.; González, J. G.; Grant, D.; Griffith, Z.; Haack, Christian; Hallgren, A.; Halzen, F.; Hanson, K.; Hebecker, D.; Heereman, D.; Helbing, K.; Hellauer, R.; Hickford, S.; Hignight, J.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, Matthías; Hultqvist, K.; In, S.; Ishihara, A.; Jacobi, E.; Japaridze, G. S.; Jeong, Minjin; Jero, K.; Jones, B. J. P.; Kalacynski, P.; Kang, Woosik; Kappes, A.; Karg, T.; Karle, A.; Katz, U.; Kauer, M.; Keivani, A.; Kelley, J. L.; Kheirandish, Ali; Kim, J.; Kim, M.; Kintscher, T.; Kiryluk, J.; Kittler, T.; Klein, S. R.; Kohnen, G.; Koirala, R.; Kolanoski, H.; Köpke, L.; Kopper, C.; Kopper, S.; Koschinsky, J. P.; Koskinen, D. J.; Kowalski, M.; Krings, K.; Kroll, M.; Krückl, G.; Kunnen, J.; Kunwar, S.; Kurahashi, N.; Kuwabara, T.; Kyriacou, A.; Labare, M.; Lanfranchi, J. L.; Larson, M. J.; Lauber, Frederik Hermann; Lennarz, D.; Lesiak-Bzdak, M.; Leuermann, M.; Liu, Q. R.; Lu, Lu; Lünemann, J.; Luszczak, William; Madsen, J.; Maggi, G.; Mahn, Kendall; Mancina, Sarah; Maruyama, R.; Mase, K.; Maunu, R.; McNally, F.; Meagher, K.; Medici, M.; Meier, Maximilian; Menne, T.; Merino, G.; Meures, T.; Miarecki, S.; Micallef, Jessie; Momenté, G.; Montaruli, T.; Moore, R. W.; Moulai, Marjon; Nahnhauer, R.; Nakarmi, P.; Naumann, Uwe; Neer, G.; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Pollmann, A. Obertacke; Olivas, A.; O’Murchadha, A.; Palczewski, T.; Pandya, Hershal; Pankova, D. V.; Peiffer, P.; Pepper, J. A.; Heros, C. Pérez de los; Pieloth, D.; Pinat, E.; Plum, M.; Price, P. B.; Przybylski, G. T.; Raab, Christoph; Rädel, L.; Rameez, M.; Rawlins, K.; Reimann, R.; Relethford, B.; Relich, M.; Resconi, E.; Rhode, W.; Richman, M.; Riedel, Benedikt; Robertson, Sally; Rongen, Martin; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk, D.; Sälzer, T.; Herrera, S. E. Sanchez; Sandrock, A.; Sandroos, J.; Sarkar, S.; Satalecka, K.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schoenen, S.; Schöneberg, S.; Schumacher, Lisa Johanna; Seckel, D.; Seunarine, S.; Soldin, D.; Song, M.; Spiczak, G. M.; Spiering, C.; Stachurska, J.; Stanev, T.; Stasik, A.; Stettner, J.; Steuer, A.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Strotjohann, N. L.; Sullivan, G. W.; Sutherland, M.; Taboada, I.; Tatar, J.; Tenholt, F.; Ter–Antonyan, S.; Terliuk, A.; Tešić, G.; Tilav, S.; Toale, P. A.; Tobin, M. N.; Toscano, S.; Tosi, D.; Tselengidou, M.; Tung, Chun Fai; Turcati, A.; Turley, C. F.; Ty, Bunheng; Unger, E.; Usner, M.; Vandenbroucke, J.; Driessche, W. Van; Eijndhoven, N. van; Vanheule, S.; Santen, J. V.; Vehring, M.; Vogel, E.; Vraeghe, M.; Walck, C.; Wallace, A.; Wallraff, M.; Wandler, F. D.; Wandkowsky, N.; Waza, A.; Weaver, Ch.; Weiss, Matthew J.; Wendt, C.; Westerhoff, S.; Whelan, B. J.; Wickmann, S.; Wiebe, K.; Wiebusch, C. H.; Wille, L.; Williams, Daniel; Wills, L.; Wolf, M.; Wood, J.; Wood, T. R.; Woolsey, E.; Woschnagg, K.; Xu, D. L.; Xu, X. W.; Xu, Yunlin; Yañez, J. P.; Yodh, G.; Yoshida, Shigeru; Yuan, Tianlu; Zoll, M.

doi:10.1140/epjc/s10052-017-5213-y

Cited by 104 publications

(129 citation statements)

References 44 publications

(41 reference statements)

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“…data on the annihilation χχ → V V → 2(e + e − ) [52,53], the Fermi-LAT data in the direction of the dwarf spheroidal galaxies [54], the Planck CMB data which is sensitive to energy injection to the CMB from DM annihilations [55,56], and the IceCube data on DM annihilation into neutrinos [57]. It also survives the upper bounds from XENON-10 and XENON-100 experiments on the DM scattering off electron [58].…”

Section: Iv-collidermentioning

confidence: 59%

Explaining the DAMPE data with scalar dark matter and gauged $$U(1)_{L_e-L_\mu }$$ U ( 1 ) L e

Cao¹,

Liu²,

Guo³

et al. 2018

Eur. Phys. J. C

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Inspired by the peak structure observed by recent DAMPE experiment in e + e − cosmic-ray spectrum, we consider a scalar dark matter (DM) model with gauged U (1) L e −L μ symmetry, which is the most economical anomaly-free theory to potentially explain the peak by DM annihilation in nearby subhalo. We utilize the process χχ → Z Z → lll l , where χ , Z , l ( ) denote the scalar DM, the new gauge boson and l ( ) = e, μ, respectively, to generate the e + e − spectrum. By fitting the predicted spectrum to the experimental data, we obtain the favored DM mass range m χ 3060 +80−100 GeV and m ≡ m χ − m Z 14 GeV at 68% Confidence Level (C.L.). Furthermore, we determine the parameter space of the model which can explain the peak and meanwhile satisfy the constraints from DM relic abundance, DM direct detection and the collider bounds. We conclude that the model we consider can account for the peak, although there exists a tension with the constraints from the LEP-II bound on m Z arising from the cross section measurement of e + e − → Z * → e + e − .

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Section: Iv-collidermentioning

confidence: 59%

Explaining the DAMPE data with scalar dark matter and gauged $$U(1)_{L_e-L_\mu }$$ U ( 1 ) L e

Cao¹,

Liu²,

Guo³

et al. 2018

Eur. Phys. J. C

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show abstract

“…[65,78] for a detailed discussion), such as the H.E.S.S. data on the annihilation χχ → S Ã S → 4e [97,113], the Fermi-LAT data in the direction of the dwarf spheroidal galaxies [114], the Planck cosmic microwave background (CMB) data which is sensitive to energy injection in the CMB from DM annihilations [115,116], and the IceCube data on DM annihilation into neutrinos [117]. Dark matter in our scenario also survives the upper bounds from the XENON-10 and XENON-100 experiments on DM-electron scattering [118].…”

Section: Dampe Explanation With Scalar Dmmentioning

confidence: 99%

Scalar dark matter explanation of the DAMPE data in the minimal left-right symmetric model

et al. 2018

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The left-right symmetric model (LRSM) is an attractive extension of the Standard Model (SM) that can address the origin of parity violation in the SM electroweak interactions, generate tiny neutrino masses, accommodate dark matter (DM) candidates, and provide a natural framework for baryogenesis through leptogenesis. In this work, we utilize the minimal LRSM to study the recently reported DAMPE results of the cosmic e þ e − spectrum, which exhibits a tentative peak around 1.4 TeV, while satisfying the current neutrino data. We propose to explain the DAMPE peak with a complex scalar DM χ in two scenarios: (1) χχ Ã → H þþ

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“…Almost universally in the parameter space of the MSSM the bounds on the spindependent cross section of the neutralino scattering off the proton or neutron cannot compete with the corresponding DD bounds on the spin-independent cross section. The current bounds on σ SD p for m χ of our interest come from the searches by the IceCube Collaboration for neutrinos coming from the center of the Milky Way [94], the Earth [95], and the Sun [96]. Since they are less constraining than the aforementioned DD bounds, and also the indirect detection bounds described below, we do not consider them here.…”

Section: P9mssm Scanning Setup and Constraintsmentioning

confidence: 99%

Testing dark matter with Cherenkov light — prospects of H.E.S.S. and CTA for exploring minimal supersymmetry

Hryczuk

Jodłowski

Moulin

et al. 2019

J. High Energ. Phys.

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We provide an updated and improved study of the prospects of the H.E.S.S. and Cherenkov Telescope Array (CTA) experiments in testing neutralino dark matter in the Minimal Supersymmetric Standard Model with nine free parameters (p9MSSM). We include all relevant experimental constraints and theoretical developments, in particular a calculation of the Sommerfeld enhancement for both present-day annihilations and the relic abundance. We perform a state-of-the-art analysis of the CTA sensitivity with a loglikelihood test ratio statistics and apply it to a numerical scan of the p9MSSM parameter space focusing on a TeV scale dark matter. We find that, assuming Einasto profile of dark matter halo in the Milky Way, H.E.S.S. has already been able to nearly reach the so-called thermal WIMP value, while CTA will go below it by providing a further improvement of at least an order of magnitude. Both H.E.S.S. and CTA are sensitive to several cases for which direct detection cross section will be below the so-called neutrino floor, with H.E.S.S. being sensitive to most of the wino region, while CTA also covering a large fraction of the ∼ 1 TeV higgsino region. We show that CTA sensitivity will be further improved in the monochromatic photon search mode for both single-component and underabundant dark matter.

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Search for neutrinos from dark matter self-annihilations in the center of the Milky Way with 3 years of IceCube/DeepCore

Cited by 104 publications

References 44 publications

Explaining the DAMPE data with scalar dark matter and gauged $$U(1)_{L_e-L_\mu }$$ U ( 1 ) L e

Explaining the DAMPE data with scalar dark matter and gauged $$U(1)_{L_e-L_\mu }$$ U ( 1 ) L e

Scalar dark matter explanation of the DAMPE data in the minimal left-right symmetric model

Testing dark matter with Cherenkov light — prospects of H.E.S.S. and CTA for exploring minimal supersymmetry

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