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dc.contributor.authorAartsen, M. G
dc.contributor.authorAckermann, M.
dc.contributor.authorAdams, J.
dc.contributor.authorAguilar, J. A
dc.contributor.authorAhlers, M.
dc.contributor.authorAhrens, M.
dc.contributor.authorAlispach, C.
dc.contributor.authorAndeen, K.
dc.contributor.authorAnderson, T.
dc.contributor.authorAnsseau, I.
dc.contributor.authorAnton, G.
dc.contributor.authorArgüelles, C.
dc.contributor.authorAuffenberg, J.
dc.contributor.authorAxani, S.
dc.contributor.authorBackes, P.
dc.contributor.authorBagherpour, H.
dc.contributor.authorBai, X.
dc.contributor.authorBalagopal V., A.
dc.contributor.authorBarbano, A.
dc.contributor.authorBarwick, S. W
dc.date.accessioned2021-09-17T18:01:47Z
dc.date.available2021-09-17T18:01:47Z
dc.date.issued2020-09-04
dc.identifier.urihttps://hdl.handle.net/1721.1/131292
dc.description.abstractAbstract 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 $$\hbox {C}_3\hbox {F}_8$$ 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. (JCAP 1509: 052, 2015) to exploit the complementarity between the two approaches and derive conservative constraints on DM-nucleon scattering. Our results constrain $$\sigma _{\mathrm{SD}} \lesssim 3 \times 10^{-39} \mathrm {cm}^2$$ σ SD ≲ 3 × 10 - 39 cm 2 ( $$6 \times 10^{-38} \mathrm {cm}^2$$ 6 × 10 - 38 cm 2 ) at $$\gtrsim 90\%$$ ≳ 90 % C.L. for a DM particle of mass 1 TeV annihilating into $$\tau ^+ \tau ^-$$ τ + τ - ( $$b\bar{b}$$ b b ¯ ) with a local density of $$\rho _{\mathrm{DM}} = 0.3~\mathrm {GeV/cm}^3$$ ρ DM = 0.3 GeV / cm 3 . The constraints scale inversely with $$\rho _{\mathrm{DM}}$$ ρ DM and are independent of the DM velocity distribution.en_US
dc.publisherSpringer Berlin Heidelbergen_US
dc.relation.isversionofhttps://doi.org/10.1140/epjc/s10052-020-8069-5en_US
dc.rightsCreative Commons Attributionen_US
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/en_US
dc.sourceSpringer Berlin Heidelbergen_US
dc.titleVelocity independent constraints on spin-dependent DM-nucleon interactions from IceCube and PICOen_US
dc.typeArticleen_US
dc.identifier.citationThe European Physical Journal C. 2020 Sep 04;80(9):819en_US
dc.contributor.departmentMassachusetts Institute of Technology. Department of Physics
dc.identifier.mitlicensePUBLISHER_CC
dc.eprint.versionFinal published versionen_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dc.date.updated2020-09-05T03:32:38Z
dc.language.rfc3066en
dc.rights.holderThe Author(s)
dspace.embargo.termsN
dspace.date.submission2020-09-05T03:32:38Z
mit.licensePUBLISHER_CC
mit.metadata.statusAuthority Work and Publication Information Needed


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