期刊
ASTROPHYSICAL JOURNAL
卷 932, 期 2, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/1538-4357/ac6e65
关键词
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资金
- National Science Foundation (NSF) [NSF DGE-1656518]
- U.S. Department of Energy [DE-AC02-76SF00515]
- NASA through the NASA Hubble Fellowship - Space Telescope Science Institute [HST-HF2-51441.001]
- NASA [NAS5-26555]
- U.S. Department of Energy Office
- U.S. National Science Foundation
- Ministry of Science and Education of Spain
- Science and Technology Facilities Council of the United Kingdom
- Higher Education Funding Council for England
- National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign
- Kavli Institute of Cosmological Physics at the University of Chicago
- Center for Cosmology and Astro-Particle Physics at the Ohio State University
- Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University
- Financiadora de Estudos e Projetos
- Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro
- Conselho Nacional de Desenvolvimento Cientifico e Tecnologico
- Ministerio da Ciencia, Tecnologia e Inovacao
- Deutsche Forschungsgemeinschaft
- Argonne National Laboratory
- University of California at Santa Cruz
- University of Cambridge
- Centro de Investigaciones Energeticas
- Medioambientales y Tecnologicas-Madrid
- University of Chicago
- University College London
- DES-Brazil Consortium
- University of Edinburgh
- Eidgenossische Technische Hochschule (ETH) Zurich
- Fermi National Accelerator Laboratory
- University of Illinois at UrbanaChampaign
- Institut de Ciencies de l'Espai (IEEC/CSIC)
- Institut de Fisica d'Altes Energies
- Lawrence Berkeley National Laboratory
- Ludwig-Maximilians Universitat Munchen
- associated Excellence Cluster Universe
- University of Michigan
- NSF's NOIRLab
- University of Nottingham
- Ohio State University
- University of Pennsylvania
- University of Portsmouth
- SLAC National Accelerator Laboratory
- Stanford University
- University of Sussex
- Texas AM University
- OzDES Membership Consortium
- National Science Foundation [AST-1138766, AST-1536171]
- MICINN [ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV2016-0588, SEV-2016-0597, MDM-2015-0509]
- ERDF funds from the European Union
- CERCA program of the Generalitat de Catalunya
- European Research Council under the European Union's Seventh Framework Program (FP7/20072013) including ERC grant [240672, 291329, 306478]
- Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) do e-Universo (CNPq grant) [465376/2014-2]
- U.S. Department of Energy, Office of Science, Office of High Energy Physics [DE-AC02-07CH11359]
We used the latest census data of satellite galaxies in the Milky Way to study the lifetime of particle dark matter (DM). By considering two-body decaying dark matter (DDM), we found that the decay of heavy DM particles significantly depletes the DM content of low-mass subhalos, making them more susceptible to tidal disruption. Using high-resolution simulations and comparing to observations, we excluded certain DDM models and provided strong constraints on the DM particle lifetime.
We use a recent census of the Milky Way (MW) satellite galaxy population to constrain the lifetime of particle dark matter (DM). We consider two-body decaying dark matter (DDM) in which a heavy DM particle decays with lifetime tau comparable to the age of the universe to a lighter DM particle (with mass splitting epsilon) and to a dark radiation species. These decays impart a characteristic kick velocity, V (kick) = epsilon c, on the DM daughter particles, significantly depleting the DM content of low-mass subhalos and making them more susceptible to tidal disruption. We fit the suppression of the present-day DDM subhalo mass function (SHMF) as a function of tau and V (kick) using a suite of high-resolution zoom-in simulations of MW-mass halos, and we validate this model on new DDM simulations of systems specifically chosen to resemble the MW. We implement our DDM SHMF predictions in a forward model that incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk using an empirical model for the galaxy-halo connection. By comparing to the observed MW satellite population, we conservatively exclude DDM models with tau < 18 Gyr (29 Gyr) for V (kick) = 20 kms(-1) (40 kms(-1)) at 95% confidence. These constraints are among the most stringent and robust small-scale structure limits on the DM particle lifetime and strongly disfavor DDM models that have been proposed to alleviate the Hubble and S (8) tensions.
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