Search for low-mass dark matter WIMPs with 12 ton-day exposure of DarkSide-50

Agnes, P.; Albuquerque, I. F. M.; Alexander, T.; Alton, A.; Ave, M.; Back, H. O.; Batignani, G.; Biery, K.; Bocci, V.; Bonivento, W.; Bottino, B.; Bussino, S.; Cadeddu, M.; Cadoni, Mariano; Calaprice, F.; Caminata, A.; Canci, N.; Caravati, M.; Cargioli, N.; Cariello, M.; Carlini, M.; Cataudella, V.; Cavalcante, P.; Cavuoti, S.; Chashin, S.; Chepurnov, A.; Cicalò, C.; Covone, G.; D’Angelo, D.; Davini, S.; Candia, A. de; Cecco, S. De; Filippis, G. De; Rosa, G. De; Derbin, A.; 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.; Cortona, Giovanni Grilli di; Grobov, A.; Gromov, M.; Guan, Mengyun; Gulino, M.; Hackett, B. R.; Herner, K.; Hessel, T.; Hosseini, B.; Hubaut, F.; Hungerford, E.; Ianni, An.; Ippolito, V.; Keeter, K. J.; Kendziora, C. L.; Kimura, Masato; Kochanek, I.; Korablëv, D.; Korga, G.; Kubankin, A. S.; Kuss, M.; Commara, M. La; Laí, M.; Li, X.; Lissia, M.; Longo, Giuseppe; Lychagina, O.; Machulin, I.; Mapelli, L.; Mari, Stefano Maria; Maricic, J.; Messina, A.; Milinčić, R.; Monroe, J.; Morrocchi, M.; Mougeot, X.; Muratova, V.; Musico, P.; Nozdrina, A.; Oleinik, A.; Ortica, F.; Pagani, L.; Pallavicini, M.; Pandola, L.; Pantic, E.; Paoloni, E.; Pelczar, K.; Pelliccia, N.; Piacentini, Stefano; Pocar, A.; M., Poehlmann, D.; Pordes, S.; Poudel, S. S.; Pralavorio, P.; Price, D.; Ragusa, F.; Razeti, M.; Razeto, A.; Renshaw, A.; Rescigno, M.; Rode, J.; Romani, A.; Sablone, D.; Samoylov, O.; Sands, W.; Sanfilippo, Simone; Sandford, Emily; Savarese, C.; Schlitzer, B.; Semenov, D.; Shchagin, A. V.; Sheshukov, A.; Skorokhvatov, M.; Smirnov, O.; Sotnikov, A.; Stracka, S.; Suvorov, Y.; Tartaglia, R.; Testera, G.; Tonazzo, A.; Unzhakov, E.; Vishneva, A.; Vogelaar, R. B.; Wada, M.; Wang, H.; Wang, Y.; Westerdale, S.; Wojcik, Mariusz; Xiao, Xiang; Yang, Changgen; Zuzel, G.

doi:10.1103/physrevd.107.063001

Cited by 33 publications

(29 citation statements)

References 50 publications

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“…For spin-independent WIMP-nucleus coherent elastic scattering with standard galactic halo parameters [16], the excess corresponds to a WIMP with mass ∼2.5 GeV/c 2 and a WIMP-nucleon scattering cross section ∼3 × 10 −40 cm 2 . This interpretation is nominally excluded by results from CDMSlite [17] and DarkSide-50 [18]. Attempts to find a consistent interpretation between these experiments by systematically varying detector response (e.g., nuclear-recoil ionization efficiencies), WIMP speed distribution, as well as alternate particle interaction models (e.g., Ref.…”

mentioning

confidence: 99%

Characterization of the background spectrum in DAMIC at SNOLAB

Aguilar-Arevalo¹,

Amidei²,

Arnquist³

et al. 2022

Phys. Rev. D

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We present results from a 3.1 kg-day target exposure of two charge-coupled devices (CCDs), each with 24 megapixels and skipper readout, deployed in the DAMIC (DArk Matter In CCDs) setup at SNOLAB. With a reduction in pixel readout noise of a factor of 10 relative to the previous detector, we investigate the excess population of low-energy bulk events previously observed above expected backgrounds. We address the dominant systematic uncertainty of the previous analysis through a depth fiducialization designed to reject surface backgrounds on the CCDs. The measured bulk ionization spectrum confirms with higher significance the presence of an excess population of low-energy events in the CCD target with characteristic rate of ∼7 events per kg-day and electronequivalent energies of ∼80 eV, whose origin remains unknown.

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mentioning

confidence: 99%

Characterization of the background spectrum in DAMIC at SNOLAB

Aguilar-Arevalo¹,

Amidei²,

Arnquist³

et al. 2022

Phys. Rev. D

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“…which is many orders of magnitude below the current sensitivity of the DarkSide 50 experiment [42] and of any foreseeable dark matter direct detection experiment. We also do not expect to have detectable signals of dark matter scatterings from neutron stars.…”

Section: Jcap01(2024)028mentioning

confidence: 76%

“…where µ = m N m χ /(m N + m χ ) is the dark matter-nucleon reduced mass, and f N ≈ 0.3 encodes the quark and gluon content of a nucleon. For dark matter in the GeV mass range, the best current sensitivity is provided by the DarkSide 50 experiment [42], which excludes cross sections larger than 2×10 −43 cm 2 for a dark matter mass of 3.4 GeV. This limit translates into λ χH ≲ 10 −2 , comparable to the constraint from the invisible Higgs decay.…”

Section: Dark Matter Signals Via the Higgs Portalmentioning

confidence: 99%

Matter-antimatter asymmetry and dark matter stability from baryon number conservation

Císcar-Monsalvatje,

Ibarra,

Vandecasteele

2024

J. Cosmol. Astropart. Phys.

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There is currently no evidence for a baryon asymmetry in our universe. Instead, cosmological observations have only demonstrated the existence of a quark-antiquark asymmetry, which does not necessarily imply a baryon asymmetric Universe, since the baryon number of the dark sector particles is unknown. In this paper we discuss a framework where the total baryon number of the Universe is equal to zero, and where the observed quark-antiquark asymmetry arises from neutron portal interactions with a dark sector fermion N that carries baryon number. In order to render a baryon symmetric universe throughout the whole cosmological history, we introduce a complex scalar χ, with opposite baryon number and with the same initial abundance as N. Notably, due to the baryon number conservation, χ is absolutely stable and could have an abundance today equal to the observed dark matter abundance. Therefore, in this simple framework, the existence of a quark-antiquark asymmetry is intimately related to the existence (and the stability) of dark matter.

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“…[1,2,7]). The required large DM-nucleon cross sections are, however, already excluded by the null results of the current DD experiments for DM particle mass above GeV scale [8][9][10][11]. For the case of halo DM-electron scatterings, in order to observe the sizable diurnal modulation, the DM-electron scattering cross section σ χe also needs to be large enough.…”

Section: Jcap11(2023)079mentioning

confidence: 98%

Diurnal modulation of electron recoils from DM-nucleon scattering through the Migdal effect

Qiao,

Xia,

Zhou

2023

J. Cosmol. Astropart. Phys.

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Halo dark matter (DM) particles could lose energy due to the scattering off nuclei within the Earth before reaching the underground detectors of DM direct detection experiments. This Earth shielding effect can result in diurnal modulation of the DM-induced recoil event rates observed underground due to the self-rotation of the Earth. For electron recoil signals from DM-electron scatterings, the current experimental constraints are very stringent such that the diurnal modulation cannot be observed for halo DM. We propose a novel type of diurnal modulation effect: diurnal modulation in electron recoil signals induced by DM-nucleon scattering via the Migdal effect. We set so far the most stringent constraints on DM-nucleon scattering cross section via the Migdal effect for sub-GeV DM using the S2-only data of PandaX-II and PandaX-4T with improved simulations of the Earth shielding effect. Based on the updated constraints, we show that the Migdal effect induced diurnal modulation of electron events can still be significant in the low energy region, and can be probed by experiments such as PandaX-4T in the near future.

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Search for low-mass dark matter WIMPs with 12 ton-day exposure of DarkSide-50

Cited by 33 publications

References 50 publications

Characterization of the background spectrum in DAMIC at SNOLAB

Characterization of the background spectrum in DAMIC at SNOLAB

Matter-antimatter asymmetry and dark matter stability from baryon number conservation

Diurnal modulation of electron recoils from DM-nucleon scattering through the Migdal effect

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