Skip to content

Constraints on Dark Matter Properties from Observations of Milky Way Satellite Galaxies

Authors

Nadler, E. O.;
Drlica-Wagner, A.;
Bechtol, K.;
Mau, S.;
Wechsler, R. H.;
Gluscevic, V.;
Boddy, K.;
Pace, A. B.;
Li, T. S.;
McNanna, M.;
Riley, A. H.;
García-Bellido, J.;
Mao, Y.-Y.;
Green, G.;
Burke, D. L.;
Peter, A.;
Jain, B.;
Abbott, T. M. C.;
Aguena, M.;
Allam, S.;
Annis, J.;
Avila, S.;
Brooks, D.;
Carrasco Kind, M.;
Carretero, J.;
Costanzi, M.;
da Costa, L. N.;
De Vicente, J.;
Desai, S.;
Diehl, H. T.;
Doel, P.;
Everett, S.;
Evrard, A. E.;
Flaugher, B.;
Frieman, J.;
Gerdes, D. W.;
Gruen, D.;
Gruendl, R. A.;
Gschwend, J.;
Gutierrez, G.;
Hinton, S. R.;
Honscheid, K.;
Huterer, D.;
James, D. J.;
Krause, E.;
Kuehn, K.;
Kuropatkin, N.;
Lahav, O.;
Maia, M. A. G.;
Marshall, J. L.
RefereedArticle

Abstract

We perform a comprehensive study of Milky Way (MW) satellite galaxies to constrain the fundamental properties of dark matter (DM). This analysis fully incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and marginalizes over uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk. Our results are consistent with the cold, collisionless DM paradigm and yield the strongest cosmological constraints to date on particle models of warm, interacting, and fuzzy dark matter. At 95% confidence, we report limits on (i) the mass of thermal relic warm DM, mWDM>6.5 keV (free-streaming length, λfs≲10 h-1 kpc ), (ii) the velocity-independent DM-proton scattering cross section, σ0<8.8 ×10-29 cm2 for a 100 MeV DM particle mass [DM-proton coupling, cp≲(0.3 GeV )-2], and (iii) the mass of fuzzy DM, mϕ>2.9 ×10-21 eV (de Broglie wavelength, λdB≲0.5 kpc ). These constraints are complementary to other observational and laboratory constraints on DM properties.

Details

© The SAO Astrophysics Data System

help[at]scixplorer.org

SciX is a project created by the Astrophysics Data System (ADS), which is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement 80NSSC21M0056.

Version: v0.26.0

Smithsonian InstitutionCenter for AstrophysicsNASA

*The material contained in this document is based upon work supported by a National Aeronautics and Space Administration (NASA) grant or cooperative agreement. Any opinions, findings, conclusions or recommendations expressed in this material are those of the author and do not necessarily reflect the views of NASA.

RESOURCES

About SciXGive FeedbackSciX HelpSystem StatusCareers@SciXAccessibility Conformance ReportWeb Accessibility PolicyNASA Science Discovery Engine

SOCIAL

@scixcommunitySciX Blog

PROJECT

Privacy PolicyTerms of UseSmithsonian Astrophysical ObservatorySmithsonian InstitutionNASA