SIMBAD references

We revisit systematics in determining the local dark matter density ρ_dm from the vertical motion of stars in the solar neighbourhood. Using a simulation of a Milky Way like galaxy, we determine the data quality required to detect ρ_dm at its expected local value. We introduce a new method for recovering ρ_dm that uses moments of the Jeans equations, combined with a Markov chain Monte Carlo technique, to marginalize over the unknown parameters. Given sufficiently good data, we show that our method can recover the correct local dark matter density even in the face of disc inhomogeneities, non-isothermal tracers and a non-separable distribution function. We illustrate the power of our technique by applying it to Hipparcos data. We first make the assumption that the A- and F-star tracer populations are isothermal. This recovers ρ_dm= 0.003^+0.009_- 0.007_M☉_/pc3 (ρ_dm= 0.11^+0.34_- 0.27_ GeV/cm3, with 90 per cent confidence), consistent with previous determinations. However, the vertical dispersion profile of these tracers is poorly known. If we assume instead a non-isothermal profile similar to that of the blue disc stars from SDSS DR-7 recently measured, we obtain a fit with a very similar χ² value, but with ρ_dm= 0.033^+0.008_- 0.009_M☉_/pc3 (ρ_dm= 1.25^+0.30_- 0.34_ GeV/cm3 with 90 per cent confidence). This highlights that it is vital to measure the vertical dispersion profile of the tracers to recover an unbiased estimate of ρ_dm. Confirmation of the VeLLO L1148-IRS: star formation at very low (column) density