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  Dynamical analysis of the dark matter and central black hole mass in the dwarf spheroidal Leo I

Bustamante-Rosell, M. J., Noyola, E., Gebhardt, K., Fabricius, M. H., Mazzalay, X., Thomas, J., et al. (2021). Dynamical analysis of the dark matter and central black hole mass in the dwarf spheroidal Leo I. The Astrophysical Journal, 921(2): 107. doi:10.3847/1538-4357/ac0c79.

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Bustamante-Rosell, M. J., Author
Noyola, Eva, Author
Gebhardt, Karl, Author
Fabricius, Maximilian H.1, Author              
Mazzalay, Ximena2, Author              
Thomas, Jens1, Author              
Zeimann, Greg, Author
Affiliations:
1Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society, ou_159895              
2High Energy Astrophysics, MPI for Extraterrestrial Physics, Max Planck Society, ou_159890              

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 Abstract: We measure the central kinematics for the dwarf spheroidal galaxy Leo I using integrated-light measurements and previously published data. We find a steady rise in the velocity dispersion from 300'' into the center. The integrated-light kinematics provide a velocity dispersion of 11.76 ± 0.66 km s−1 inside 75''. After applying appropriate corrections to crowding in the central regions, we achieve consistent velocity dispersion values using velocities from individual stars. Crowding corrections need to be applied when targeting individual stars in high-density stellar environments. From integrated light, we measure the surface brightness profile and find a shallow cusp toward the center. Axisymmetric, orbit-based models measure the stellar mass-to-light ratio, black hole mass, and parameters for a dark matter halo. At large radii it is important to consider possible tidal effects from the Milky Way, so we include a variety of assumptions regarding the tidal radius. For every set of assumptions, models require a central black hole consistent with a mass (3.3 ± 2) × 106 M. The no-black-hole case for any of our assumptions is excluded at over 95% significance, with 6.4 < Δχ2 < 14. A black hole of this mass would have significant effects on dwarf galaxy formation and evolution. The dark halo parameters are heavily affected by the assumptions for the tidal radii, with the circular velocity only constrained to be above 30 km s−1. Reasonable assumptions for the tidal radius result in stellar orbits consistent with an isotropic distribution in the velocities. These more realistic models have little need for a dark matter halo.

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 Dates: 2021-11-05
 Publication Status: Published online
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 Identifiers: DOI: 10.3847/1538-4357/ac0c79
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Title: The Astrophysical Journal
Source Genre: Journal
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Publ. Info: Bristol; Vienna : IOP Publishing; IAEA
Pages: - Volume / Issue: 921 (2) Sequence Number: 107 Start / End Page: - Identifier: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215_3