Search for dark matter towards the Galactic Centre with 11 years of ANTARES data

Albert, A.; André, M.; Anghinolfi, M.; Anton, G.; Ardid, M.; Aubert, J.J.; Aublin, J.; Baret, B.; Basa, S.; Belhorma, B.; Bertín, V.; Biagi, S.; Bissinger, M.; Boumaaza, J.; Bourret, S.; Bouta, M.; Bouwhuis, M. C.; Brânzaş, H.; Bruijn, R.; Brünner, J.; Busto, J.; Capone, A.; Caramete, L.; Carr, J.; Celli, S.; Chabab, M.; Chau, Thien Nhan; Moursli, R. Cherkaoui El; Chiarusi, T.; Circella, M.; Coleiro, A.; Colomer, M.; Coniglione, R.; Costantini, H.; Coyle, P.; Creusot, A.; Díaz, Antonio; Wasseige, Gwenhaël de; Deschamps, A.; Distefano, C.; Palma, I. Di; Domi, Alba; Donzaud, C.; Dornic, D.; Drouhin, D.; Eberl, T.; Bojaddaini, I. El; Khayati, N. El; Elsässer, Dominik; Enzenhöfer, A.; Ettahiri, A.; Fassi, F.; Fermani, P.; Ferrara, G.; Filippini, F.; Fusco, L.; Gay, P.; Glotin, Hervé; Gozzini, S. R.; Ruiz, R. Gracia; Graf, Κ.; Guidi, C.; Hallmann, S.; Haren, Hans van; Heijboer, A.; Hello, Y.; Hernández-Rey, J. J.; Hößl, J.; Hofestädt, J.; Illuminati, G.; James, C. W.; Jong, M. de; Jong, P. de; Jongen, M.; Kadler, M.; Kalekin, O.; Katz, U.; Khan-Chowdhury, N. R.; Kouchner, A.; Kreter, M.; Kreykenbohm, I.; Kulikovskiy, V.; Lahmann, R.; Breton, R. Le; Lefèvre, D.; Leonora, E.; Levi, G.; Lincetto, Massimiliano; Lopez-Coto, D.; Loucatos, S.; Maggi, G.; Mańczak, J.; Marcelin, M.; Margiotta, A.; Marinelli, A.; Martínez-Mora, J. A.; Mele, R.; Melis, K.; Migliozzi, P.; Möser, Michael; Moussa, A.; Müller, R.; Nauta, L.; Navas, S.; Nezri, E.; Nielsen, C.; Núñez-Castiñeyra, A.; O’Fearraigh, B.; Organokov, M.; Păvălaş, G. E.; Pellegrino, C.; Perrin-Terrin, M.; Piattelli, P.; Poirè, C.; Popa, V.; Pradier, T.; Quinn, L.; Randazzo, N.; Riccobene, G.; Sánchez-Losa, A.; Salah-Eddine, A.; Samtleben, D. F. E.; Sanguineti, M.; Sapienza, P.; Schüßler, F.; Spurio, M.; Stolarczyk, Th.; Strandberg, B.; Taiuti, M.; Tayalati, Y.; Thakore, T.; Tingay, S. J.; Trovato, A.; Vallage, B.; Elewyck, V. Van; Versari, F.; Viola, S.; Vivolo, D.; Wilms, J.; Zaborov, D.; Zegarelli, A.; Zornoza, J. D.; Zúñiga, J.

doi:10.1016/j.physletb.2020.135439

Cited by 44 publications

(65 citation statements)

References 27 publications

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“…At the location of the SK detector, the GC is below the horizon for ∼64% of the year, while for IceCube it is always above the horizon and can only be directly probed with downward-going events which typically suffer from more backgrounds from cosmic-ray muons. ANTARES is operating in the same hemisphere as SK and its limits [45] are stronger than the ones obtained here for M χ > 50-500 GeV (depending on the annihilation mode) due to the larger effective area of its detector. Weaker constraints from ANTARES observed for M χ < 500 GeV for bb and for M χ < 100-150 GeV for W þ W − =μ þ μ − annihilation channels are due to the different detection thresholds between ANTARES and SK.…”

Section: Results Of Combined Fit Analysismentioning

confidence: 63%

“…on the hσ A Vi versus WIMP mass (the region above the lines is excluded), for dark matter annihilating through νν, bb, W þ W − , and μ þ μ − into neutrinos, assuming the NFW halo profile. SK limits, obtained in the combined fit and corresponding to a total livetime of 5325.8 (5629.1) live-days for FC and PC (UP-μ) events, are compared with published results from IceCube (1005 live-days) [44] and ANTARES (3170 live-days) [45]. the signal is expected to come from the on-source region centered around the GC (266°RA, −29°DEC) while an independent background estimation is obtained from the off-source region, which is offset 180°in right ascension but at the same declination.…”

Section: On-source/off-source Analysismentioning

confidence: 99%

See 1 more Smart Citation

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

Bronner¹,

Haga²,

Hayato³

et al. 2020

Phys. Rev. D

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Section: Results Of Combined Fit Analysismentioning

confidence: 63%

Section: On-source/off-source Analysismentioning

confidence: 99%

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

Bronner¹,

Haga²,

Hayato³

et al. 2020

Phys. Rev. D

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show abstract

“…Indirect searches for dark matter have indeed been performed by gamma-ray telescopes (MAGIC, e.g., [84][85][86], H.E.S.S., e.g., [87][88][89][90], VERITAS [91,92]), X-ray telescopes (XMM-Newton, e.g., [93][94][95][96], NuSTAR, e.g., [97][98][99], Suzaku, e.g., [100][101][102][103]), cosmic-ray detectors (HAWC [104][105][106]), detectors in space (Fermi-LAT, e.g., [107][108][109], DAMPE, e.g., [110], CALET [111], AMS [112]) and neutrino telescopes (IceCube, e.g., [113][114][115], ANTARES, e.g., [116][117][118], Baikal, e.g., [119][120][121], Baksan [122] or Super-Kamiokande, e.g., [123][124][125]). Many of these detectors have upgrade programs underway, in different stages of R&D or implementation (CTA [126], IceCube-Gen2 [127], KM3NET [128]<...>…”

Section: Dark Matter Signatures From the Cosmosmentioning

confidence: 99%

Status, Challenges and Directions in Indirect Dark Matter Searches

Heros

2020

Symmetry

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Indirect searches for dark matter are based on detecting an anomalous flux of photons, neutrinos or cosmic-rays produced in annihilations or decays of dark matter candidates gravitationally accumulated in heavy cosmological objects, like galaxies, the Sun or the Earth. Additionally, evidence for dark matter that can also be understood as indirect can be obtained from early universe probes, like fluctuations of the cosmic microwave background temperature, the primordial abundance of light elements or the Hydrogen 21-cm line. The techniques needed to detect these different signatures require very different types of detectors: Air shower arrays, gamma- and X-ray telescopes, neutrino telescopes, radio telescopes or particle detectors in balloons or satellites. While many of these detectors were not originally intended to search for dark matter, they have proven to be unique complementary tools for direct search efforts. In this review we summarize the current status of indirect searches for dark matter, mentioning also the challenges and limitations that these techniques encounter.

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“…Limit on the annihilation cross section as a function of m X , compared to limits for e AE and μ AE channels from γ-ray observation of dwarf galaxies with Fermi-LAT from the supplemental material of Ref. [10] multiplied with three to account for the branching fraction, as well as the limit on neutrino emission from the galactic center by ANTARES [35], and respective sensitivity of KM3NeT [36], multiplied with four to account for the branching fraction and oscillation effect. The purple area shows the variation of the limit among all cases with nuisance parameters Φ and E cut d changed between 300 MV, 500 MV, 700 MV and 2 TeV, 4 TeV, 10 TeV respectively.…”

Section: Fit Of the Background Model To Calet And Ams-02 Datamentioning

confidence: 99%

“…This kind of DM would be a favorable target to search in electronpositron cosmic rays while being less detectable by γ-ray search. The partial direct annihilation to neutrinos also makes it a promising target for indirect dark matter search with neutrino telescopes looking for a monoenergetic line signature [35,36]. After establishing the particle physics model defining the properties of the DM, we discuss its cosmic-ray signatures and implications from available CALET and AMS-02 data.…”

Section: Introductionmentioning

confidence: 99%

Cosmic-ray signatures of dark matter from a flavor dependent gauge symmetry model with neutrino mass mechanism

et al. 2020

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We propose an extension to the Standard Model accommodating two families of Dirac neutral fermions and Majorana fermions under additional Uð1Þ e−μ × Z 3 × Z 2 symmetries where Uð1Þ e−μ is a flavor dependent gauge symmetry related to the first and second family of the lepton sector, which features a twoloop induced neutrino mass model. The two families are favored by minimally reproducing the current neutrino oscillation data and two mass difference squares and canceling the gauge anomalies at the same time. As a result, we have a prediction for neutrino masses. The lightest Dirac neutral fermion is a dark matter candidate with tree-level interaction restricted to electron, muon and neutrinos, which makes it difficult to detect in direct dark matter search as well as indirect search focusing on the τ-channel, such as through γ-rays. It may however be probed by search for dark matter signatures in electron and positron cosmic rays, and allows interpretation of a structure appearing in the CALET electron þ positron spectrum around 350-400 GeV as its signature, with a boost factor ∼40 Breit-Wigner enhancement of the annihilation cross section.

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Search for dark matter towards the Galactic Centre with 11 years of ANTARES data

Cited by 44 publications

References 27 publications

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

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

Status, Challenges and Directions in Indirect Dark Matter Searches

Cosmic-ray signatures of dark matter from a flavor dependent gauge symmetry model with neutrino mass mechanism

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