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000483309 0247_ $$2inspire$$ainspire:922090
000483309 0247_ $$2datacite_doi$$a10.3204/PUBDB-2022-05237
000483309 0247_ $$2arXiv$$aarXiv:1108.0664
000483309 037__ $$aPUBDB-2022-05237
000483309 041__ $$aEnglish
000483309 082__ $$a530
000483309 088__ $$2arXiv$$aarXiv:1108.0664
000483309 088__ $$2DESY$$aDESY-11-135
000483309 1001_ $$aEvoli, C.$$b0
000483309 245__ $$aAntiprotons from dark matter annihilation in the Galaxy: Astrophysical uncertainties
000483309 260__ $$c2012
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000483309 3367_ $$2BibTeX$$aARTICLE
000483309 3367_ $$2DataCite$$aOutput Types/Working Paper
000483309 500__ $$aISSN 1550-2368 not unique: **2 hits**.29 pages, 18 figures, 2 tables. Match to the published version in PRD. References updated/ Physical Review D, vol. 85, Issue 12, 2012
000483309 520__ $$aThe latest years have seen steady progresses in WIMP dark matter (DM) searches, with hints of possible signals suggested by both direct and indirect detection experiments. Antiprotons can play a key role validating those interpretations since they are copiously produced by WIMP annihilations in the Galactic halo, and the secondary antiproton background produced by Cosmic Ray (CR) interactions is predicted with fair accuracy and matches the observed spectrum very well. Using the publicly available numerical DRAGON code, we reconsider antiprotons as a tool to constrain DM models discussing its power and limitations. We provide updated constraints on a wide class of annihilating DM models by comparing our predictions against the most up-to-date ap measurements, taking also into account the latest spectral information on the p, He and other CR nuclei fluxes. Doing that, we probe carefully the uncertainties associated to both secondary and DM originated antiprotons, by using a variety of distinctively different assumptions for the propagation of CRs and for the DM distribution in the Galaxy. We find that the impact of the astrophysical uncertainties on constraining the DM properties can be much stronger, up to a factor of ~50, than the one due to uncertainties on the DM distribution (~2-6). Remarkably, even reducing the uncertainties on the propagation parameters derived by local observables, non-local effects can still change DM model constraints even by 50%. Nevertheless, current ap data place tight constraints on DM models, excluding some of those suggested in connection with indirect and direct searches. Finally we discuss the power of upcoming CR spectral data from the AMS-02 observatory to drastically reduce the uncertainties discussed in this paper and estimate the expected sensitivity of this instrument to some sets of DM models.
000483309 536__ $$0G:(DE-HGF)POF2-51x$$a51x - Programm Elementarteilchenphysik - Topic unbekannt (POF2-51x)$$cPOF2-51x$$fPOF II$$x0
000483309 588__ $$aDataset connected to CrossRef, INSPIRE, Journals: bib-pubdb1.desy.de
000483309 650_7 $$2INSPIRE$$adark matter: annihilation
000483309 650_7 $$2INSPIRE$$aWIMP: dark matter
000483309 650_7 $$2INSPIRE$$adark matter: galaxy: halo
000483309 650_7 $$2INSPIRE$$aanti-p: cosmic radiation
000483309 650_7 $$2INSPIRE$$aAMS
000483309 650_7 $$2INSPIRE$$aanti-p: energy spectrum
000483309 650_7 $$2INSPIRE$$acosmic radiation: flux
000483309 650_7 $$2INSPIRE$$acosmic radiation: propagation
000483309 650_7 $$2INSPIRE$$acosmic radiation: energy spectrum
000483309 650_7 $$2INSPIRE$$aWIMP: mass
000483309 650_7 $$2INSPIRE$$adark matter: density
000483309 650_7 $$2INSPIRE$$across section: annihilation
000483309 650_7 $$2INSPIRE$$ap: flux
000483309 650_7 $$2INSPIRE$$aanti-p: flux
000483309 650_7 $$2INSPIRE$$aWino: dark matter
000483309 650_7 $$2INSPIRE$$aPAMELA
000483309 650_7 $$2INSPIRE$$adark matter: mass
000483309 650_7 $$2autogen$$a95.35.+d
000483309 650_7 $$2autogen$$acosmic rays
000483309 650_7 $$2autogen$$aelementary particles
000483309 650_7 $$2autogen$$adark matter
000483309 650_7 $$2autogen$$aantiprotons
000483309 693__ $$0EXP:(DE-MLZ)NOSPEC-20140101$$5EXP:(DE-MLZ)NOSPEC-20140101$$eNo specific instrument$$x0
000483309 7001_ $$aCholis, I.$$b1
000483309 7001_ $$aGrasso, D.$$b2
000483309 7001_ $$aMaccione, L.$$b3
000483309 7001_ $$aUllio, P.$$b4
000483309 7870_ $$0PHPPUBDB-21690$$aEvoli, C. et.al.$$d[S.l.] : Soc., 2012$$iIsParent$$tAntiprotons from dark matter annihilation in the Galaxy: Astrophysical uncertainties
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000483309 9132_ $$0G:(DE-HGF)POF3-611$$1G:(DE-HGF)POF3-610$$2G:(DE-HGF)POF3-600$$aDE-HGF$$bForschungsbereich Materie$$lMaterie und Universum$$vFundamental Particles and Forces$$x0
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