A search for Secluded Dark Matter in the Sun with the ANTARES neutrino telescope

Adrián-Martínez, S.; Albert, A.; André, M.; Anton, G.; Ardid, M.; Aubert, J.J.; Avgitas, T.; Baret, B.; Barrios-Martí, J.; Basa, S.; Bertín, V.; Biagi, S.; Bormuth, R.; Bou-Cabo, M.; Bouwhuis, M. C.; Bruijn, R.; Brünner, J.; Busto, J.; Capone, A.; Caramete, L.; Carr, J.; Celli, S.; Chiarusi, T.; Circella, M.; Coleiro, A.; Coniglione, R.; Costantini, H.; Coyle, P.; Creusot, A.; Deschamps, A.; Bonis, G. De; Distefano, C.; Donzaud, C.; Dornic, D.; Drouhin, D.; Eberl, T.; Bojaddaini, I. El; Elsässer, Dominik; Enzenhöfer, A.; Fehn, K.; Fusco, L.; Galatà, S.; Geißelsöder, S.; Geyer, K.; Giordano, V.; Gleixner, A.; Glotin, Hervé; Gracia-Ruiz, R.; Graf, Κ.; Hallmann, S.; Haren, Hans van; Heijboer, A.; Hello, Y.; Hernández-Rey, J. J.; Hößl, J.; Hofestädt, J.; Hugon, C.; Illuminati, G.; James, C. W.; Jong, M. de; Kadler, M.; Kalekin, O.; Katz, U.; Kießling, D.; Kouchner, A.; Kreter, M.; Kreykenbohm, I.; Kulikovskiy, V.; Lachaud, C.; Lahmann, R.; Lefèvre, D.; Leonora, E.; Loucatos, S.; Marcelin, M.; Margiotta, A.; Marinelli, A.; Martínez-Mora, J. A.; Mathieu, A.; Michael, T.; Migliozzi, P.; Moussa, A.; Mueller, C. L.; Nezri, E.; Păvălaş, G. E.; Pellegrino, C.; Perrina, C.; Piattelli, P.; Popa, V.; Pradier, T.; Racca, C.; Riccobene, G.; Roensch, K.; Saldaña, M.; Samtleben, D. F. E.; Sanguineti, M.; Sapienza, P.; Schnabel, J.; Schüßler, F.; Seitz, T.; Sieger, C.; Spurio, M.; Stolarczyk, Th.; Sánchez-Losa, A.; Taiuti, M.; Trovato, A.; Tselengidou, M.; Turpin, D.; Tönnis, Christoph; Vallage, B.; Vallée, C.; Elewyck, V. Van; Vivolo, D.; Wagner, S. J.; Wilms, J.; Zornoza, J.D.; Zúñiga, J.

doi:10.1088/1475-7516/2016/05/016

Cited by 49 publications

(70 citation statements)

References 42 publications

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“…The indirect limits from IceCube and SuperK assume annihilation to τ leptons (dashed) and b quarks (dotted). Additional limits, not shown for clarity, are set by LUX [51] and XENON1T [53] (comparable to PandaX-II) and by ANTARES [54,55] (comparable to IceCube). IA100118) and Consejo Nacional de Ciencia y Tecnología (CONACyT, México, Grant No.…”

Section: Acknowledgementsmentioning

confidence: 99%

Dark matter search results from the complete exposure of the PICO-60 C3F8 bubble chamber

Amole¹,

Ardid²,

Arnquist³

et al. 2019

Phys. Rev. D

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Final results are reported from operation of the PICO-60 C3F8 dark matter detector, a bubble chamber filled with 52 kg of C3F8 located in the SNOLAB underground laboratory. The chamber was operated at thermodynamic thresholds as low as 1.2 keV without loss of stability. A new blind 1404-kg-day exposure at 2.45 keV threshold was acquired with approximately the same expected total background rate as the previous 1167-kg-day exposure at 3.3 keV. This increased exposure is enabled in part by a new optical tracking analysis to better identify events near detector walls, permitting a larger fiducial volume. These results set the most stringent direct-detection constraint to date on the WIMP-proton spin-dependent cross section at 2.5 × 10 −41 cm 2 for a 25 GeV WIMP, and improve on previous PICO results for 3-5 GeV WIMPs by an order of magnitude.

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Section: Acknowledgementsmentioning

confidence: 99%

Dark matter search results from the complete exposure of the PICO-60 C3F8 bubble chamber

Amole¹,

Ardid²,

Arnquist³

et al. 2019

Phys. Rev. D

Self Cite

250

232

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“…For the muonic decay channel, one can also search for the muon tracks from mediators decaying in or near the detector, rather than searching for tracks induced by neutrino scattering events. We do not consider this possibility here but note that in some parts of the parameter space, this type of search results in slightly stronger limits than neutrino searches from muon decays [34]. 0.01 0.1 1 10 100 1000 10 4 10 5 10 6 Figure 13.…”

Section: The Muon Channelmentioning

confidence: 99%

Neutrinos and gamma rays from long-lived mediator decays in the Sun

Niblaeus

Beniwal

Edsjö

2019

J. Cosmol. Astropart. Phys.

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We investigate a scenario where dark matter (DM) particles can be captured and accumulate in the Sun, and subsequently annihilate into a pair of long-lived mediators. These mediators can decay further out in the Sun or outside of the Sun. Compared to the standard scenario where DM particles annihilate directly into Standard Model particles close to the solar core, here we also obtain fluxes of gamma rays and charged cosmic rays. We simulate this scenario using a full three-dimensional model of the Sun, and include interactions and neutrino oscillations. In particular, we perform a model-independent study of the complementarity between neutrino and gamma ray fluxes by comparing the recent searches from IceCube, Super-Kamiokande, Fermi-LAT, ARGO and HAWC.We find that the resulting neutrino fluxes are significantly higher at high energy when the mediators decay further out in the Sun. We also find that gamma ray searches place stronger constraints than neutrino searches on these models even in cases where the mediators decay mainly inside the Sun, except in the approximately inner 10% of the Sun where neutrino searches are more powerful. We present our results in a model-independent manner and release a new version of the WimpSim code that can be used to simulate this scenario for arbitrary mediator models.

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“…Over time, this leads to an accumulation of dark matter in the core of the star, which can have observable consequences. For example, the accumulation and subsequent annihilation of dark matter particles in the Sun can produce highly energetic fluxes of neutrinos that could potentially be seen by neutrino telescopes, providing an important means of dark matter indirect detection [8][9][10][11][12]. Alternatively, the annihilation of captured dark matter to long-lived dark mediators can lead to spectacular signals [13][14][15][16][17].…”

Section: Introductionmentioning

confidence: 99%

Capture of leptophilic dark matter in neutron stars

Bell

Busoni

Robles

2019

J. Cosmol. Astropart. Phys.

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Dark matter particles will be captured in neutron stars if they undergo scattering interactions with nucleons or leptons. These collisions transfer the dark matter kinetic energy to the star, resulting in appreciable heating that is potentially observable by forthcoming infrared telescopes. While previous work considered scattering only on nucleons, neutron stars contain small abundances of other particle species, including electrons and muons. We perform a detailed analysis of the neutron star kinetic heating constraints on leptophilic dark matter. We also estimate the size of loop induced couplings to quarks, arising from the exchange of photons and Z bosons. Despite having relatively small lepton abundances, we find that an observation of an old, cold, neutron star would provide very strong limits on dark matter interactions with leptons, with the greatest reach arising from scattering off muons. The projected sensitivity is orders of magnitude more powerful than current dark matter-electron scattering bounds from terrestrial direct detection experiments.Neutron stars provide particularly powerful DM constraints, because their high density leads to efficient capture. Indeed, for DM-nucleon cross sections above a threshold value of order 10 −45 cm 2 , the capture probably saturates at the geometric limit, σ ∼ πR 2 * m n /M * , such that all dark matter incident on the star is captured. This conclusion holds irrespective of whether DM scattering interactions are spin independent (SI) or spin dependent (SD). Given that conventional direct detection experiments currently have sensitivity to DM-nucleon cross sections below 10 −45 cm 2 only in a limited DM mass range, and only for SI interactions, NS techniques are clearly very useful. Moreover, velocity or momentum dependent interactions are completely inaccessible to terrestrial direct detection experiments, being severely suppressed in the non-relativistic regime applicable for scattering on Earth. In comparison, DM particles are accelerated to quasi-relativistic velocities upon NS infall, effectively erasing such kinematic suppression.When dark matter is gravitationally captured by a NS, the kinetic energy transferred in the collisions heat up the star. The captured dark matter will then undergo a series of further collisions, eventually transferring almost all of its initial kinetic energy, to reach a state of thermal equilibrium with the star. As shown in Refs. [18,19] this can heat neutron stars up to 1700K. 1 Because old isolated neutron stars can cool to temperatures below 1000K, such heating (or its absence) can be used to place limits on the strength of dark matter interactions. 2 Importantly, this kinetic heating may be within reach of forthcoming infrared telescopes [18,19]. Provided NSs are nearby, faint and sufficiently isolated, they are likely to be discovered by existing radio telescopes such as the Fivehundred-meter Aperture Spherical radio Telescope (FAST) [37], or the future Square Kilometer Array (SKA) [38]. Their thermal emission can then be m...

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A search for Secluded Dark Matter in the Sun with the ANTARES neutrino telescope

Cited by 49 publications

References 42 publications

Dark matter search results from the complete exposure of the PICO-60 C3F8 bubble chamber

Dark matter search results from the complete exposure of the PICO-60 C3F8 bubble chamber

Neutrinos and gamma rays from long-lived mediator decays in the Sun

Capture of leptophilic dark matter in neutron stars

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