Modelling the Milky Way through adiabatic compression of cold dark matter halo

Abstract

We use the adiabatic compression theory to build a physically well - motivated Milky Way mass model in agreement with the observational data. The visible mass of the Galaxy is distributed in a spheroidal bulge and a multi - components disc parametrized by three galactic parameters, the Sun distance to the galactic centre, R_0, the total bulge mass, M_{bulge}, and the local disc surface density, Σ_{\odot}. To model the dark matter component, we adiabatically compress a Navarro, Frenk and White (NFW) halo (with concentration $c$ and total mass M_{vir}) for fixed values of the spin parameter, λ, the fraction of the mass in baryons, $m_b$, and the thin disc contribution to total angular momentum, j_d. An iterative selection procedure is used to explore in very detail the wide space of parameters only selecting those combinations of {R_0, M_{bulge}, Σ_{\odot}, λ, m_b, j_b, c, M_{vir}} that give rise to a Milky Way model in agreement with the observational constraints. This analysis leads us to conclude that only models with R_0 = 8.5 kpc, $0.8x10^{10}{M}_{\odot }<M_{bulge}<1.6x10^{10}{M}_{\odot }$ and $49M_{\odot }p{c}^{-2}\le {\Sigma }_{\odot }\le 56M_{\odot }p{c}^{-2}$ can be reconciled with the set of observational constraints. As regard the parameters entering the adiabatic compression, we find $0.03\le \lambda \le 0.10$ and $0.04\le m_b\le 0.10$, while the final estimates of the parameters describing the initial halo profile turn out to be $5\stackrel{<}{\sim }c\stackrel{<}{\sim }12$ and $7x10^{11}{M}_{\odot }\stackrel{<}{\sim }{M}_{\mathrm{vir}}\stackrel{<}{\sim }17x10^{11}{M}_{\odot }$ (all at 95.7% CL).

13 pages, 10 figures, accepted for publication on Astronomy & Astrophysics

References in corpus (1)

• Response of dark matter halos to condensation of baryons: cosmological simulations and improved adiabatic contraction model

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