Search for dark matter particle interactions with electron final states with DarkSide-50

Agnes, P.; Albuquerque, I. F. M.; Alexander, T.; Alton, A. K.; Ave, M.; Back, H. O.; Batignani, G.; Biery, K.; Bocci, V.; Bonivento, W. M.; Bottino, B.; Bussino, S.; Cadeddu, M.; Cadoni, M.; Calaprice, F.; Caminata, A.; Campos, M. D.; Canci, N.; Caravati, M.; Cariello, M.; Carlini, M.; Carpinelli, M.; Cataudella, V.; Cavalcante, P.; Cavuoti, S.; Chashin, S.; Chepurnov, A.; Cicalò, C.; Covone, G.; D'Angelo, D.; Davini, S.; De Candia, A.; De Cecco, S.; De Filippis, G.; De Rosa, G.; Derbin, A. V.; Devoto, A.; D'Incecco, M.; Dionisi, C.; Dordei, F.; Downing, M.; D'Urso, D.; Fiorillo, G.; Franco, D.; Gabriele, F.; Galbiati, C.; Ghiano, C.; Giganti, C.; Giovanetti, G. K.; Goretti, A. M.; di Cortona, G. Grilli; Grobov, A.; Gromov, M.; Guan, M.; Gulino, M.; Hackett, B. R.; Herner, K.; Hessel, T.; Hosseini, B.; Hubaut, F.; Hungerford, E. V.; Ianni, An.; Ippolito, V.; Keeter, K.; Kendziora, C. L.; Kimura, M.; Kochanek, I.; Korablev, D.; Korga, G.; Kubankin, A.; Kuss, M.; La Commara, M.; Lai, M.; Li, X.; Lissia, M.; Longo, G.; Lychagina, O.; Machulin, I. N.; Mapelli, L. P.; Mari, S. M.; Maricic, J.; Martoff, C. J.; Messina, A.; Milincic, R.; Monroe, J.; Morrocchi, M.; Mougeot, X.; Muratova, V. N.; Musico, P.; Nozdrina, A. O.; Oleinik, A.; Ortica, F.; Pagani, L.; Pallavicini, M.; Pandola, L.; Pantic, E.; Paoloni, E.; Pelczar, K.; Pelliccia, N.; Piacentini, S.; Piacentini, S.; Picciau, E.; Pocar, A.; Poehlmann, D. M.; Pordes, S.; Poudel, S. S.; Pralavorio, P.; Price, D. D.; Ragusa, F.; Razeti, M.; Razeto, A.; Renshaw, A. L.; Rescigno, M.; Rode, J.; Romani, A.; Sablone, D.; Samoylov, O.; Sands, W.; Sanfilippo, S.; Sanford, E.; Savarese, C.; Schlitzer, B.; Semenov, D. A.; Shchagin, A.; Sheshukov, A.; Skorokhvatov, M. D.; Smirnov, O.; Sotnikov, A.; Stracka, S.; Suvorov, Y.; Tartaglia, R.; Testera, G.; Tonazzo, A.; Unzhakov, E. V.; Vishneva, A.; Vogelaar, R. B.; Wada, M.; Wang, H.; Wang, Y.; Westerdale, S.; Wojcik, M. M.; Xiao, X.; Yang, C.; Zuzel, G.

doi:10.48550/arxiv.2207.11968

Cited by 5 publications

(6 citation statements)

References 41 publications

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“…The reason for this can be understood from Figs. 3 and 4, where we see that the BBDM flux for DM energies relevant to recoil Bin 3 of Super-K differs by ∼ O (10) for the two operators, The direct detection bounds from Xenon10, Xenon100, SENSEI [53][54][55] and DarkSide-50 [56] are also plotted. The bound arising due to DM attenuation is also given for heavy mediator scenario (plotted in grey).…”

Section: B Vector Mediatormentioning

confidence: 99%

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Blazar boosted Dark Matter -- direct detection constraints on $σ_{eχ}$ : Role of energy dependent cross sections

Bhowmick¹,

Ghosh²,

Sachdeva³

2023

Preprint

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Elastic collisions with relativistic electrons from the blazar's jet can accelerate dark matter (DM) particles in the DM spike surrounding the supermassive black hole at its center. This can allow one to set stringent limits on the DM-electron scattering cross section (σeχ) for DM masses less than 100 MeV. We consider DM particles boosted by energetic electrons in the jets of the blazars TXS 0506+056 and BL Lacertae. Both vector and scalar mediators for the scattering of electron and electrophilic fermionic DM are studied. We highlight that the ensuing energy dependency of the S-matrix for the corresponding Lorentz structure of the vertex significantly modifies the constraints. We find that the revised exclusion limits are orders of magnitude stronger than the equivalent results for the simple constant cross section assumption. Our limits are also assessed for the less cuspy spike.

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Section: B Vector Mediatormentioning

confidence: 99%

“…The various DM density profiles considered are Profile 1 (in red) and Profile 2 (in blue). The direct detection bounds from Xenon10, Xenon100, SENSEI [53][54][55] and DarkSide-50 [56] are also plotted. The bound arising due to DM attenuation is also given for heavy mediator scenario (plotted in grey).…”

Section: B Vector Mediatormentioning

confidence: 99%

Blazar boosted Dark Matter -- direct detection constraints on $σ_{eχ}$ : Role of energy dependent cross sections

Bhowmick¹,

Ghosh²,

Sachdeva³

2023

Preprint

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“…This indicates that a sub-GeV DM can ionize an electron from an atomic shell or facilitate an electron's transition from the valance band to the conduction band. Many experiments like XENON [63], SuperCDMS [64], DarkSide-50 [65,66], DAMIC [67], EDELWEISS [68], SENSEI [69,70], PandaX-II [71] etc. are searching for the signatures of such a phenomenon.…”

Section: Jhep02(2023)200mentioning

confidence: 99%

Dark matter substructures affect dark matter-electron scattering in xenon-based direct detection experiments

Maity

Laha

2023

J. High Energ. Phys.

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Recent sky surveys have discovered a large number of stellar substructures. It is highly likely that there are dark matter (DM) counterparts to these stellar substructures. We examine the implications of DM substructures for electron recoil (ER) direct detection (DD) rates in dual phase xenon experiments. We have utilized the results of the LAMOST survey and considered a few benchmark substructures in our analysis. Assuming that these substructures constitute 10% of the local DM density, we study the discovery limits of DM-electron scattering cross sections considering one kg-year exposure and 1, 2, and 3 electron thresholds. With this exposure and threshold, it is possible to observe the effect of the considered DM substructure for the currently allowed parameter space. We also explore the sensitivity of these experiments in resolving the DM substructure fraction. For all the considered cases, we observe that DM having mass $$ \mathcal{O}(10) $$ O 10 MeV has a better prospect in resolving substructure fraction as compared to $$ \mathcal{O}(100) $$ O 100 MeV scale DM. We also find that within the currently allowed DM-electron scattering cross-section; these experiments can resolve the substructure fraction (provided it has a non-negligible contribution to the local DM density) with good accuracy for $$ \mathcal{O}(10) $$ O 10 MeV DM mass with one electron threshold.

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“…Only the least (BM3, BM3 ) and most restrictive (BM1, BM1 ) new limits are shown. The ν-DM scattering bounds are the same as those in the left panel, while for e-DM scattering they are labelled with and are: (slate blue) solar reflection [75], (brown) Super-K for DM boosted by cosmic-ray electrons, (turquoise) blazar BL Lacertae for BM3 model [40], (gray) direct detection for light DM interacting with electrons [76][77][78][79].…”

Section: Constraints On Neutrino-dark Matter Scatteringmentioning

confidence: 99%

NGC 1068 constraints on neutrino-dark matter scattering

Cline¹,

Puel²

2023

Preprint

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The IceCube collaboration has observed the first steady-state point source of high-energy neutrinos, coming from the active galaxy NGC 1068. If neutrinos interacted strongly enough with dark matter, the emitted neutrinos would have been impeded by the dense spike of dark matter surrounding the supermassive black hole at the galactic center, which powers the emission. We derive a stringent upper limit on the scattering cross section between neutrinos and dark matter based on the observed events and theoretical models of the dark matter spike. The bound can be stronger than that obtained by the single IceCube neutrino event from the blazar TXS 0506+056 for some spike models.

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Search for dark matter particle interactions with electron final states with DarkSide-50

Cited by 5 publications

References 41 publications

Blazar boosted Dark Matter -- direct detection constraints on $σ_{eχ}$ : Role of energy dependent cross sections

Blazar boosted Dark Matter -- direct detection constraints on $σ_{eχ}$ : Role of energy dependent cross sections

Dark matter substructures affect dark matter-electron scattering in xenon-based direct detection experiments

NGC 1068 constraints on neutrino-dark matter scattering

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