The local dark matter density

作者：Read J I^*

来源：Journal of Physics G: Nuclear and Particle Physics , 2014, 41(6): 063101.

DOI：10.1088/0954-3899/41/6/063101

• dark matter
• local dark matter density
• mass modelling
• Milky Way
• direct dark matter detection

I review current efforts to measure the mean density of dark matter near the Sun. This encodes valuable dynamical information about our Galaxy and is also of great importance for %26apos;direct detection%26apos; dark matter experiments. I discuss theoretical expectations in our current cosmology; the theory behind mass modelling of the Galaxy; and I show how combining local and global measures probes the shape of the Milky Way dark matter halo and the possible presence of a %26apos;dark disc%26apos;. I stress the strengths and weaknesses of different methodologies and highlight the continuing need for detailed tests on mock data-particularly in the light of recently discovered evidence for disequilibria in the Milky Way disc. I collate the latest measurements of rho(dm) and show that, once the baryonic surface density contribution Sigma(b) is normalized across different groups, there is remarkably good agreement. Compiling data from the literature, I estimate Sigma(b) = 54.2 +/- 4.9 M(circle dot)pc(-2), where the dominant source of uncertainty is in the H I gas contribution. Assuming this contribution from the baryons, I highlight several recent measurements of rho(dm) in order of increasing data complexity and prior, and, correspondingly, decreasing formal error bars. Comparing these measurements with spherical extrapolations from the Milky Way%26apos;s rotation curve, I show that the Milky Way is consistent with having a spherical dark matter halo at R-0 similar to 8 kpc. The very latest measures of rho(dm) based on similar to 10 000 stars from the Sloan Digital Sky Survey appear to favour little halo flattening at R-0, suggesting that the Galaxy has a rather weak dark matter disc, with a correspondingly quiescent merger history. I caution, however, that this result hinges on there being no large systematics that remain to be uncovered in the SDSS data, and on the local baryonic surface density being Sigma(b) similar to 55 M(circle dot)pc(-2). I conclude by discussing how the new Gaia satellite will be transformative. We will obtain much tighter constraints on both Sigma(b) and rho(dm) by having accurate 6D phase space data for millions of stars near the Sun. These data will drive us towards fully three dimensional models of our Galactic potential, moving us into the realm of precision measurements of rho(dm).

• 出版日期2014-6