Milky Way Dark Matter Distribution or MOND Test from Vertical Stellar Kinematics with Gaia DR3
Vertical stellar kinematics+density can be used to trace the dark matter distribution (or the equivalent phantom mass in a Modified Newtonian Dynamics (MOND) scenario) through the Jeans equations. In this paper, we want to improve this type of analysis by making use of the recent data of the 6D info...
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad94f5 |
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| author | Martín López-Corredoira |
| author_facet | Martín López-Corredoira |
| author_sort | Martín López-Corredoira |
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| description | Vertical stellar kinematics+density can be used to trace the dark matter distribution (or the equivalent phantom mass in a Modified Newtonian Dynamics (MOND) scenario) through the Jeans equations. In this paper, we want to improve this type of analysis by making use of the recent data of the 6D information from the Gaia DR3 survey in the anticenter and the Galactic poles to obtain the dynamical mass distribution near plane regions, including extended kinematics over a wide region of 8 kpc < R < 22 kpc, ∣ z ∣ < 3 kpc. Our conclusions are as follows: (i) the model of the spherical dark matter halos and the MOND model are compatible with the data; (ii) the model of the disky matter (with density proportional to the gas density) is excluded; (iii) the total lack of dark matter (there is only visible matter) within Newtonian gravity is compatible with the data; for instance, at solar Galactocentric radius, we obtained Σ = 39 ± 18 M _⊙ pc ^−2 for z = 1.05 kpc, compatible with the expected value for visible matter alone of 44 M _⊙ pc ^−2 , thus allowing zero dark matter. Similarly, for R > R _⊙ , z = 1.05 kpc, Σ = 28.7 ± 9.6, 23.0 ± 5.7, 16.9 ± 5.8, and 11.4 ± 6.6 M _⊙ pc ^−2 , respectively, for R = 10, 13, 16, and 19 kpc, compatible with visible matter alone. Larger error bars in comparison with previous works are not due to worse data or a more awkward technique but to a stricter modeling of the stellar distribution. |
| format | Article |
| id | doaj-art-73f27e75ee8246c19dda0d4c5c333e21 |
| institution | OA Journals |
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| language | English |
| publishDate | 2024-01-01 |
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| series | The Astrophysical Journal |
| spelling | doaj-art-73f27e75ee8246c19dda0d4c5c333e212025-08-20T02:35:30ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-0197814510.3847/1538-4357/ad94f5Milky Way Dark Matter Distribution or MOND Test from Vertical Stellar Kinematics with Gaia DR3Martín López-Corredoira0https://orcid.org/0000-0001-6128-6274Instituto de Astrofísica de Canarias , E-38205 La Laguna, Tenerife, Spain ; martin@lopez-corredoira.com; PIFI-Visiting Scientist 2023 of Chinese Academy of Sciences at Purple Mountain Observatory , Nanjing 210023, and National Astronomical Observatories, Beijing 100012, People's Republic of China ; Departamento de Astrofisica, Universidad de La Laguna , E-38206 La Laguna, Tenerife, SpainVertical stellar kinematics+density can be used to trace the dark matter distribution (or the equivalent phantom mass in a Modified Newtonian Dynamics (MOND) scenario) through the Jeans equations. In this paper, we want to improve this type of analysis by making use of the recent data of the 6D information from the Gaia DR3 survey in the anticenter and the Galactic poles to obtain the dynamical mass distribution near plane regions, including extended kinematics over a wide region of 8 kpc < R < 22 kpc, ∣ z ∣ < 3 kpc. Our conclusions are as follows: (i) the model of the spherical dark matter halos and the MOND model are compatible with the data; (ii) the model of the disky matter (with density proportional to the gas density) is excluded; (iii) the total lack of dark matter (there is only visible matter) within Newtonian gravity is compatible with the data; for instance, at solar Galactocentric radius, we obtained Σ = 39 ± 18 M _⊙ pc ^−2 for z = 1.05 kpc, compatible with the expected value for visible matter alone of 44 M _⊙ pc ^−2 , thus allowing zero dark matter. Similarly, for R > R _⊙ , z = 1.05 kpc, Σ = 28.7 ± 9.6, 23.0 ± 5.7, 16.9 ± 5.8, and 11.4 ± 6.6 M _⊙ pc ^−2 , respectively, for R = 10, 13, 16, and 19 kpc, compatible with visible matter alone. Larger error bars in comparison with previous works are not due to worse data or a more awkward technique but to a stricter modeling of the stellar distribution.https://doi.org/10.3847/1538-4357/ad94f5Stellar kinematicsGalaxy dynamicsDark matterMilky Way disk |
| spellingShingle | Martín López-Corredoira Milky Way Dark Matter Distribution or MOND Test from Vertical Stellar Kinematics with Gaia DR3 The Astrophysical Journal Stellar kinematics Galaxy dynamics Dark matter Milky Way disk |
| title | Milky Way Dark Matter Distribution or MOND Test from Vertical Stellar Kinematics with Gaia DR3 |
| title_full | Milky Way Dark Matter Distribution or MOND Test from Vertical Stellar Kinematics with Gaia DR3 |
| title_fullStr | Milky Way Dark Matter Distribution or MOND Test from Vertical Stellar Kinematics with Gaia DR3 |
| title_full_unstemmed | Milky Way Dark Matter Distribution or MOND Test from Vertical Stellar Kinematics with Gaia DR3 |
| title_short | Milky Way Dark Matter Distribution or MOND Test from Vertical Stellar Kinematics with Gaia DR3 |
| title_sort | milky way dark matter distribution or mond test from vertical stellar kinematics with gaia dr3 |
| topic | Stellar kinematics Galaxy dynamics Dark matter Milky Way disk |
| url | https://doi.org/10.3847/1538-4357/ad94f5 |
| work_keys_str_mv | AT martinlopezcorredoira milkywaydarkmatterdistributionormondtestfromverticalstellarkinematicswithgaiadr3 |