2018/11/27 by Juan Barranco, Barranco, J., Argelia Bernal +3 · 1 citation
Physics and Astronomy · #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #High Energy Astrophysical Phenomena (astro-ph.HE) #High Energy Physics - Phenomenology (hep-ph)
paper · pdf · doi:10.48550/arxiv.1811.11125
openalex publication_date 2018/11/27 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The equation of state for a degenerate gas of fermions at zero temperature in the non-relativistic case is a polytrope, i.e. p ∼ρ5/3/mF8/3. If dark matter is modeled by such a non-interacting fermion, this dependence in the mass of the fermion mF explains why if dark matter is very heavy the effective pressure of dark matter is negligible. Nevertheless, if the mass of the dark matter is very small, the effective pressure can be very large, and thus a system of self-gravitating fermions can be formed. In this work we model the dark matter halo of the Milky-Way by solving the Tolman-Oppenheimer-Volkoff equations, with the equation of state for a partially degenerate ultralight non-interacting fermion. We found that to fit the rotational velocity curve of the Milky-Way, the mass of the fermion should be in the range 31.5 ~eV < mF < 35~eV at 90% C.L. Moreover, the central density is restricted to be in the range of 1.2 < ρ0<1.7 GeV/cm3 at 90% C.L. The fermionic dark matter halo has a very different profile as compared with the standard Navarro-Frenk-White profile, thus, the possible indirect signals for annihilating dark matter may change by orders of magnitude. We found bounds for the annihilation cross section in this case by using the Saggitarius A* spectral energy distribution.