000077223 001__ 77223
000077223 005__ 20200716101523.0
000077223 0247_ $$2doi$$a10.1103/PhysRevD.99.023012
000077223 0248_ $$2sideral$$a110544
000077223 037__ $$aART-2019-110544
000077223 041__ $$aeng
000077223 100__ $$aEvans, N.W.
000077223 245__ $$aRefinement of the standard halo model for dark matter searches in light of the Gaia Sausage
000077223 260__ $$c2019
000077223 5060_ $$aAccess copy available to the general public$$fUnrestricted
000077223 5203_ $$aPredicting signals in experiments to directly detect dark matter (DM) requires a form for the local DM velocity distribution. Hitherto, the standard halo model (SHM), in which velocities are isotropic and follow a truncated Gaussian law, has performed this job. New data, however, suggest that a substantial fraction of our stellar halo lies in a strongly radially anisotropic population, the "Gaia sausage." Inspired by this recent discovery, we introduce an updated DM halo model, the SHM++, which includes a "sausage" component, thus better describing the known features of our Galaxy. The SHM++ is a simple analytic model with five parameters: the circular speed, local escape speed, and local DM density, which we update to be consistent with the latest data, and two new parameters: the anisotropy and the density of DM in the sausage. The impact of the SHM++ on signal models for weakly interacting massive particles (WIMPs) and axions is rather modest since the multiple changes and updates have competing effects. In particular, this means that the older exclusion limits derived for WIMPS are still reasonably accurate. However, changes do occur for directional detectors, which have sensitivity to the full three-dimensional velocity distribution.
000077223 536__ $$9info:eu-repo/grantAgreement/ES/MINECO/FPA2015-65745-P
000077223 540__ $$9info:eu-repo/semantics/openAccess$$aAll rights reserved$$uhttp://www.europeana.eu/rights/rr-f/
000077223 590__ $$a4.833$$b2019
000077223 591__ $$aPHYSICS, PARTICLES & FIELDS$$b6 / 29 = 0.207$$c2019$$dQ1$$eT1
000077223 591__ $$aASTRONOMY & ASTROPHYSICS$$b16 / 68 = 0.235$$c2019$$dQ1$$eT1
000077223 592__ $$a1.664$$b2019
000077223 593__ $$aPhysics and Astronomy (miscellaneous)$$c2019$$dQ1
000077223 655_4 $$ainfo:eu-repo/semantics/article$$vinfo:eu-repo/semantics/publishedVersion
000077223 700__ $$0(orcid)0000-0003-3803-9384$$aO'Hare, C.A.J.$$uUniversidad de Zaragoza
000077223 700__ $$aMcCabe, C.
000077223 7102_ $$12004$$2405$$aUniversidad de Zaragoza$$bDpto. Física Teórica$$cÁrea Física Teórica
000077223 773__ $$g99, 2 (2019), 023012 [18 pp]$$pPhys. rev. D$$tPhysical Review D$$x2470-0010
000077223 8564_ $$s1354846$$uhttps://zaguan.unizar.es/record/77223/files/texto_completo.pdf$$yVersión publicada
000077223 8564_ $$s112006$$uhttps://zaguan.unizar.es/record/77223/files/texto_completo.jpg?subformat=icon$$xicon$$yVersión publicada
000077223 909CO $$ooai:zaguan.unizar.es:77223$$particulos$$pdriver
000077223 951__ $$a2020-07-16-09:28:20
000077223 980__ $$aARTICLE