Home > Publications database > Velocity Independent Constraints on Spin-Dependent DM-Nucleon Interactions from IceCube and PICO > print

001     434788
005     20211110155926.0
024 7 _ |a Amole:2019coq
|2 INSPIRETeX
024 7 _ |a inspire:1746683
|2 inspire
024 7 _ |a arXiv:1907.12509
|2 arXiv
024 7 _ |a 10.3204/PUBDB-2020-00331
|2 datacite_doi
037 _ _ |a PUBDB-2020-00331
041 _ _ |a English
088 1 _ |a arXiv:1907.12509
088 _ _ |a arXiv:1907.12509
|2 arXiv
100 1 _ |a Aartsen, M. G.
|b 0
245 _ _ |a Velocity Independent Constraints on Spin-Dependent DM-Nucleon Interactions from IceCube and PICO
260 _ _ |c 2019
336 7 _ |a Preprint
|b preprint
|m preprint
|0 PUB:(DE-HGF)25
|s 1579521554_15393
|2 PUB:(DE-HGF)
336 7 _ |a WORKING_PAPER
|2 ORCID
336 7 _ |a Electronic Article
|0 28
|2 EndNote
336 7 _ |a preprint
|2 DRIVER
336 7 _ |a Report
|0 PUB:(DE-HGF)29
|2 PUB:(DE-HGF)
|m report
336 7 _ |a ARTICLE
|2 BibTeX
336 7 _ |a Output Types/Working Paper
|2 DataCite
500 _ _ |a
520 _ _ |a Adopting the Standard Halo Model (SHM) of an isotropic Maxwellian velocity distribution for dark matter (DM) particles in the Galaxy, the most stringent current constraints on their spin-dependent scattering cross-section with nucleons come from the IceCube neutrino observatory and the PICO-60 C$_3$F$_8$ superheated bubble chamber experiments. The former is sensitive to high energy neutrinos from the self-annihilation of DM particles captured in the Sun, while the latter looks for nuclear recoil events from DM scattering off nucleons. Although slower DM particles are more likely to be captured by the Sun, the faster ones are more likely to be detected by PICO. Recent N-body simulations suggest significant deviations from the SHM for the smooth halo component of the DM, while observations hint at a dominant fraction of the local DM being in substructures. We use the method of Ferrer et al. (2015) to exploit the complementarity between the two approaches and derive conservative constraints on DM-nucleon scattering. Our results constrain $\sigma_{\mathrm{SD}} \lesssim 10^{-39} \mathrm{cm}^2$ ($10^{-38} \mathrm{cm}^2$) at $\gtrsim 90\%$ C.L. for a DM particle of mass 1~TeV annihilating into $\tau^+ \tau^-$ ($b\bar{b}$) with a local density of $\rho_{\mathrm{DM}} = 0.3~\mathrm{ GeV/cm}^3$. The constraints scale inversely with $\rho_{\mathrm{DM}}$ and are independent of the DM velocity distribution.
536 _ _ |a 613 - Matter and Radiation from the Universe (POF3-613)
|0 G:(DE-HGF)POF3-613
|c POF3-613
|f POF III
|x 0
588 _ _ |a Dataset connected to INSPIRE
693 _ _ |0 EXP:(DE-H253)IceCube-20150101
|5 EXP:(DE-H253)IceCube-20150101
|e IceCube South Pole Neutrino Observatory
|x 0
700 1 _ |a Ackermann, Markus
|0 P:(DE-H253)PIP1014130
|b 1
|u desy
700 1 _ |a Adams, J.
|b 2
700 1 _ |a Aguilar, J. A.
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700 1 _ |a Ahlers, M.
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|b 5
700 1 _ |a Alispach, C.
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700 1 _ |a Andeen, K.
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700 1 _ |a Ansseau, I.
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700 1 _ |a Bai, X.
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700 1 _ |a Barwick, S. W.
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