Dark Matter Halo Properties of the Galactic Dwarf Satellites: Implication for Chemo-dynamical Evolution of the Satellites and a Challenge to Lambda Cold Dark Matter
Elucidating dark matter density profiles in Galactic dwarf satellites is essential to understanding not only the quintessence of dark matter, but also the evolution of the satellites themselves. In this work, we present the current constraints on dark matter densities in Galactic ultrafaint dwarf (U...
| Main Authors: | , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ace33e |
| _version_ | 1797694453694070784 |
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| author | Kohei Hayashi Yutaka Hirai Masashi Chiba Tomoaki Ishiyama |
| author_facet | Kohei Hayashi Yutaka Hirai Masashi Chiba Tomoaki Ishiyama |
| author_sort | Kohei Hayashi |
| collection | DOAJ |
| description | Elucidating dark matter density profiles in Galactic dwarf satellites is essential to understanding not only the quintessence of dark matter, but also the evolution of the satellites themselves. In this work, we present the current constraints on dark matter densities in Galactic ultrafaint dwarf (UFD) and diffuse galaxies. Applying our constructed nonspherical mass models to the currently available kinematic data of the 25 UFDs and two diffuse satellites, we find that whereas most of the galaxies have huge uncertainties on the inferred dark matter density profiles, Eridanus II, Segue I, and Willman 1 favor cuspy central profiles even when considering effects of a prior bias. We compare our results with the simulated subhalos on the plane between the dark matter density at 150 pc and the pericenter distance. We find that the most observed satellites and the simulated subhalos are similarly distributed on this plane, except for Antlia 2, Crater 2, and Tucana 3, which are less than one-tenth of the density. Despite considerable tidal effects, the subhalos detected by commonly used subhalo finders have difficulty explaining such a huge deviation. We also estimate the dynamical mass-to-light ratios of the satellites and confirm the ratio is linked to stellar mass and metallicity. Tucana 3 deviates largely from these relations, while it follows the mass–metallicity relation. This indicates that Tucana 3 has a cored dark matter halo, despite a significant uncertainty in its ratios. |
| first_indexed | 2024-03-12T02:58:12Z |
| format | Article |
| id | doaj.art-8eae361df8094c3f9fa1fb00b2175888 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T02:58:12Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-8eae361df8094c3f9fa1fb00b21758882023-09-03T15:07:30ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01953218510.3847/1538-4357/ace33eDark Matter Halo Properties of the Galactic Dwarf Satellites: Implication for Chemo-dynamical Evolution of the Satellites and a Challenge to Lambda Cold Dark MatterKohei Hayashi0https://orcid.org/0000-0002-8758-8139Yutaka Hirai1https://orcid.org/0000-0002-5661-033XMasashi Chiba2https://orcid.org/0000-0002-9053-860XTomoaki Ishiyama3https://orcid.org/0000-0002-5316-9171National Institute of Technology , Sendai College 48 Nodayama, Medeshima-Shiote, Natori, Miyagi 981-1239, Japan ; khayashi@sendai-nct.ac.jp; Astronomical Institute, Tohoku University , 6-3 Aoba, Aramaki, Aoba-ku, Sendai, Miyagi 980-8578, Japan; Institute for Cosmic Ray Research, The University of Tokyo, Chiba 277-8582, JapanAstronomical Institute, Tohoku University , 6-3 Aoba, Aramaki, Aoba-ku, Sendai, Miyagi 980-8578, Japan; Department of Physics and Astronomy, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556, USA; Joint Institute for Nuclear Astrophysics , Center for the Evolution of the Elements (JINA-CEE), East Lansing, MI 48824, USAAstronomical Institute, Tohoku University , 6-3 Aoba, Aramaki, Aoba-ku, Sendai, Miyagi 980-8578, JapanDigital Transformation Enhancement Council, Chiba University , 1-33, Yayoi-cho, Inage-ku, Chiba 263-8522, JapanElucidating dark matter density profiles in Galactic dwarf satellites is essential to understanding not only the quintessence of dark matter, but also the evolution of the satellites themselves. In this work, we present the current constraints on dark matter densities in Galactic ultrafaint dwarf (UFD) and diffuse galaxies. Applying our constructed nonspherical mass models to the currently available kinematic data of the 25 UFDs and two diffuse satellites, we find that whereas most of the galaxies have huge uncertainties on the inferred dark matter density profiles, Eridanus II, Segue I, and Willman 1 favor cuspy central profiles even when considering effects of a prior bias. We compare our results with the simulated subhalos on the plane between the dark matter density at 150 pc and the pericenter distance. We find that the most observed satellites and the simulated subhalos are similarly distributed on this plane, except for Antlia 2, Crater 2, and Tucana 3, which are less than one-tenth of the density. Despite considerable tidal effects, the subhalos detected by commonly used subhalo finders have difficulty explaining such a huge deviation. We also estimate the dynamical mass-to-light ratios of the satellites and confirm the ratio is linked to stellar mass and metallicity. Tucana 3 deviates largely from these relations, while it follows the mass–metallicity relation. This indicates that Tucana 3 has a cored dark matter halo, despite a significant uncertainty in its ratios.https://doi.org/10.3847/1538-4357/ace33eDark matterGalaxy kinematicsDwarf spheroidal galaxiesGalaxy dynamicsGalaxy structureLocal Group |
| spellingShingle | Kohei Hayashi Yutaka Hirai Masashi Chiba Tomoaki Ishiyama Dark Matter Halo Properties of the Galactic Dwarf Satellites: Implication for Chemo-dynamical Evolution of the Satellites and a Challenge to Lambda Cold Dark Matter The Astrophysical Journal Dark matter Galaxy kinematics Dwarf spheroidal galaxies Galaxy dynamics Galaxy structure Local Group |
| title | Dark Matter Halo Properties of the Galactic Dwarf Satellites: Implication for Chemo-dynamical Evolution of the Satellites and a Challenge to Lambda Cold Dark Matter |
| title_full | Dark Matter Halo Properties of the Galactic Dwarf Satellites: Implication for Chemo-dynamical Evolution of the Satellites and a Challenge to Lambda Cold Dark Matter |
| title_fullStr | Dark Matter Halo Properties of the Galactic Dwarf Satellites: Implication for Chemo-dynamical Evolution of the Satellites and a Challenge to Lambda Cold Dark Matter |
| title_full_unstemmed | Dark Matter Halo Properties of the Galactic Dwarf Satellites: Implication for Chemo-dynamical Evolution of the Satellites and a Challenge to Lambda Cold Dark Matter |
| title_short | Dark Matter Halo Properties of the Galactic Dwarf Satellites: Implication for Chemo-dynamical Evolution of the Satellites and a Challenge to Lambda Cold Dark Matter |
| title_sort | dark matter halo properties of the galactic dwarf satellites implication for chemo dynamical evolution of the satellites and a challenge to lambda cold dark matter |
| topic | Dark matter Galaxy kinematics Dwarf spheroidal galaxies Galaxy dynamics Galaxy structure Local Group |
| url | https://doi.org/10.3847/1538-4357/ace33e |
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