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Stellar-to-Halo Mass Ratio and Dark Matter Profiles

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Abstract

This paper seeks to verify if the inner halo density profile depends on the ratio between stellar and halo mass. The work follows the previous one by Del Popolo and Pace (2016), in which we studied the quoted problem in the case of Di Cintio et al. (2014) simulations, verifying if supernova feedback scenario is able to describe the inner structure of galaxies, employing more sophisticated statistical tools, namely Bayesian statistics, than those indicated in the quoted paper. The present paper extends the previous results of Del Popolo (2020) to new hydrodynamical simulations (Tollet et al. 2016, Macciò et al. 2020, Lazar et al. 2020). Similarly to Del Popolo (2020), the present paper and its analysis show that the simulations are still not in agreement with the data used. In summary, the quoted simulations, in which supernovae feedback flattens the inner profile of galaxies, cannot correctly explain the structure of the observed galaxies.

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  1. Dipartimento di Fisica e Astronomia, University of Catania, 95125, Catania, Italy

    A. Del Popolo

  2. Institute of Astronomy, Russian Academy of Sciences, 119017, Moscow, Russia

    A. Del Popolo

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Del Popolo, A. Stellar-to-Halo Mass Ratio and Dark Matter Profiles. Astron. Rep. 65, 529–542 (2021). https://doi.org/10.1134/S1063772921070039

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  • DOI: https://doi.org/10.1134/S1063772921070039

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