4.7 Article

Milky Way Satellite Census. IV. Constraints on Decaying Dark Matter from Observations of Milky Way Satellite Galaxies

期刊

ASTROPHYSICAL JOURNAL
卷 932, 期 2, 页码 -

出版社

IOP Publishing Ltd
DOI: 10.3847/1538-4357/ac6e65

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资金

  1. National Science Foundation (NSF) [NSF DGE-1656518]
  2. U.S. Department of Energy [DE-AC02-76SF00515]
  3. NASA through the NASA Hubble Fellowship - Space Telescope Science Institute [HST-HF2-51441.001]
  4. NASA [NAS5-26555]
  5. U.S. Department of Energy Office
  6. U.S. National Science Foundation
  7. Ministry of Science and Education of Spain
  8. Science and Technology Facilities Council of the United Kingdom
  9. Higher Education Funding Council for England
  10. National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign
  11. Kavli Institute of Cosmological Physics at the University of Chicago
  12. Center for Cosmology and Astro-Particle Physics at the Ohio State University
  13. Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University
  14. Financiadora de Estudos e Projetos
  15. Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro
  16. Conselho Nacional de Desenvolvimento Cientifico e Tecnologico
  17. Ministerio da Ciencia, Tecnologia e Inovacao
  18. Deutsche Forschungsgemeinschaft
  19. Argonne National Laboratory
  20. University of California at Santa Cruz
  21. University of Cambridge
  22. Centro de Investigaciones Energeticas
  23. Medioambientales y Tecnologicas-Madrid
  24. University of Chicago
  25. University College London
  26. DES-Brazil Consortium
  27. University of Edinburgh
  28. Eidgenossische Technische Hochschule (ETH) Zurich
  29. Fermi National Accelerator Laboratory
  30. University of Illinois at UrbanaChampaign
  31. Institut de Ciencies de l'Espai (IEEC/CSIC)
  32. Institut de Fisica d'Altes Energies
  33. Lawrence Berkeley National Laboratory
  34. Ludwig-Maximilians Universitat Munchen
  35. associated Excellence Cluster Universe
  36. University of Michigan
  37. NSF's NOIRLab
  38. University of Nottingham
  39. Ohio State University
  40. University of Pennsylvania
  41. University of Portsmouth
  42. SLAC National Accelerator Laboratory
  43. Stanford University
  44. University of Sussex
  45. Texas AM University
  46. OzDES Membership Consortium
  47. National Science Foundation [AST-1138766, AST-1536171]
  48. MICINN [ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV2016-0588, SEV-2016-0597, MDM-2015-0509]
  49. ERDF funds from the European Union
  50. CERCA program of the Generalitat de Catalunya
  51. European Research Council under the European Union's Seventh Framework Program (FP7/20072013) including ERC grant [240672, 291329, 306478]
  52. Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) do e-Universo (CNPq grant) [465376/2014-2]
  53. U.S. Department of Energy, Office of Science, Office of High Energy Physics [DE-AC02-07CH11359]

向作者/读者索取更多资源

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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