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We use stellar kinematics from the latest Gaia data release (DR2) to measurethe local dark matter density $\rho_{\rm DM}$ in a heliocentric cylinder ofradius $R= 150 \ {\rm pc}$ and half-height $z= 200 \ {\rm pc}$. We also explorethe prospect of using our analysis to estimate the DM density in localsubstructure by setting constraints on the surface density and scale height ofa thin dark disk aligned with the baryonic disk and formed due to dark matterself-interaction. Performing the statistical analysis within a Bayesianframework for three types of tracers, we obtain ${\rho_{\rm DM}= 0.016 \pm0.010}$ M$_\odot$/pc$^3$ for A stars; early G stars give a similar result,while F stars yield a significantly higher value. For a thin dark disk, A starsset the strongest constraint: excluding surface densities (5-12)M$_\odot$/pc$^2$ for scale heights below 100 pc with 95% confidence. Comparingour results with those derived using Tycho-Gaia Astrometric Solution (TGAS)data, we find that the uncertainty in our measurements of the local DM contentis dominated by systematic errors that arise from assumptions of our kinematicanalysis in the low $z$ region. Furthermore, there will only be a marginalreduction in these uncertainties with more data in the Gaia era. We comment onthe robustness of our method and discuss potential improvements for futurework.

Using Gaia DR2 to Constrain Local Dark Matter Density and Thin Dark Disk