The Local Dark Matter Density from SDSS-SEGUE G-dwarfs
  We derive the local dark matter density by applying the integrated Jeans
equation method from Silverwood et al. (2016) to SDSS-SEGUE G-dwarf data
processed and presented by B\"udenbender et al. (2015). We use the MultiNest
Bayesian nested sampling software to fit a model for the baryon distribution,
dark matter and tracer stars, including a model for the 'tilt term' that
couples the vertical and radial motions, to the data. The $\alpha$-young
population from B\"udenbender et al. (2015) yields the most reliable result of
$\rho_{\rm DM} = 0.46^{+0.07}_{-0.09}\, {{\rm GeV\, cm}^{-3}} =
0.012^{+0.001}_{-0.002}\, {{\rm M}_\odot \, {\rm pc}^{-3}}$. Our analyses yield
inconsistent results for the $\alpha$-young and $\alpha$-old data, pointing to
problems in the tilt term and its modelling, the data itself, the assumption of
a flat rotation curve, or the effects of disequilibria.
