The Dark Matter Profiles in the Milky Way. (arXiv:1906.08419v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lin_H/0/1/0/all/0/1">Hai-Nan Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_X/0/1/0/all/0/1">Xin Li</a>
We investigate the dark matter profile of the Milky Way using the observed
rotation curve data out to 100 kpc. The baryonic matter of the Milky Way is
divided into bulge, disk and gas components, and each component is modelled
using various possible mass profiles available in literature. The arbitrary
combination of seven bulge profiles, four disk profiles and two gas profiles
results in fifty-six baryon models. These baryon models are combined with one
of the four dark matter profiles: Burkert profile, core-modified profile,
pseudo-isothermal profile and NFW profile, to fit the observed rotation curve
data. Results show that in general the NFW profile fits the data better than
the Burkert profile, while the core-modified profile and the pseudo-isothermal
profile are essentially ruled out. The best-fitting NFW model has the scale
length $r_0=8.1pm 0.7$ kpc, and the corresponding local density of dark matter
is $rho_{rm dm}(R=R_odot)=0.51pm0.09~{rm GeV}/{rm cm}^3$.
We investigate the dark matter profile of the Milky Way using the observed
rotation curve data out to 100 kpc. The baryonic matter of the Milky Way is
divided into bulge, disk and gas components, and each component is modelled
using various possible mass profiles available in literature. The arbitrary
combination of seven bulge profiles, four disk profiles and two gas profiles
results in fifty-six baryon models. These baryon models are combined with one
of the four dark matter profiles: Burkert profile, core-modified profile,
pseudo-isothermal profile and NFW profile, to fit the observed rotation curve
data. Results show that in general the NFW profile fits the data better than
the Burkert profile, while the core-modified profile and the pseudo-isothermal
profile are essentially ruled out. The best-fitting NFW model has the scale
length $r_0=8.1pm 0.7$ kpc, and the corresponding local density of dark matter
is $rho_{rm dm}(R=R_odot)=0.51pm0.09~{rm GeV}/{rm cm}^3$.
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