| Name: | K ADITYA |
| Affiliation: | INDIAN INSTITUTE OF ASTROPHYSICS |
| Conference ID : | ASI2024_509 |
| Title : | Black holes at the center of dwarf spheroidal galaxies: Is there room for more mass at the center ? |
| Authors : | K ADITYA \& ARUN MANGALAM |
| Authors Affiliation: | Indian Institute of Astrophysics, Koramangala, Bengaluru 560 034, INDIA |
| Mode of Presentation: | Poster |
| Abstract Category : | Galaxies and Cosmology |
| Abstract : | In this study, we present the mass models of the Milky Way dwarf spheroidal galaxies using the kinematic and photometric data available in the literature. We model these galaxies as a three-component system consisting of the star, dark matter halo, and a central black hole. Our analysis shows that mass models with a cuspy dark matter halos prefer a central black holes with masses equal to $10^3 M_{\odot}$. In contrast, in the case of cored dark matter models, the central black
hole masses fall within the range of $10^4 M_{\odot}$ to $10^6 M_{\odot}$. We note that the presence of a central black hole may be obscured in the case of cuspy dark matter models since the models with and without a central black hole predict a comparable stellar dispersion. Whereas we find that the cored dark matter model tends to favor the presence of a supermassive black hole at the center. Interestingly, we find that mass models for Leo 2 predict a black hole mass equal to $10^{6}M_{\odot}$ for both cored and cuspy dark matter models. Finally, we note that the dwarf spheroidal galaxies deviate from the $M_{BH}-\sigma_{*}$relation, with cored models consistent with the galaxy assembly-based origins $(M_{BH}\propto\sigma^{2}_{*})$ and cuspy models with a feedback-based scenario $(M_{BH}\propto\sigma^{4}_{*})$. |
