GALACTIC MASERS AND THE MILKY WAY CIRCULAR VELOCITY

Masers found in massive star-forming regions can be located precisely in six-dimensional phase space and therefore serve as a tool for studying Milky Way dynamics. The non-random orbital phases at which the masers are found and the sparseness of current samples require modeling. Here, we model the phase-space distribution function of 18 precisely measured Galactic masers, permitting a mean velocity offset and a general velocity dispersion tensor relative to their local standards of rest, and accounting for different pieces of prior information. With priors only on the Sun's distance from the Galactic Center and on its motion with respect to the local standard of rest, the maser data provide a weak constraint on the circular velocity at the Sun of V(c) = 246 +/- 30 km s(-1). Including prior information on the proper motion of Sgr A* leads to V(c) = 244 +/- 13 km s(-1). We do not confirm the value of V(c) approximate to 254 km s(-1) found in more restrictive models. This analysis shows that there is no conflict between recent determinations of V(c) from Galactic Center analyses, orbital fitting of the GD-1 stellar stream, and the kinematics of Galactic masers; a combined estimate is V(c) = 236 +/- 11 km s(-1). Apart from the dynamical parameters, we find that masers tend to occur at post-apocenter, circular-velocity-lagging phases of their orbits.