Globular Cluster Streams as Galactic High-Precision Scales - The Poster
  Child Palomar 5
  Using the example of the tidal stream of the Milky Way globular cluster
Palomar 5 (Pal 5), we demonstrate how observational data on streams can be
efficiently reduced in dimensionality and modeled in a Bayesian framework. Our
approach combines detection of stream overdensities by a
Difference-of-Gaussians process with fast streakline models, a continuous
likelihood function built from these models, and inference with MCMC. By
generating $\approx10^7$ model streams, we show that the geometry of the Pal 5
debris yields powerful constraints on the solar position and motion, the Milky
Way and Pal 5 itself. All 10 model parameters were allowed to vary over large
ranges without additional prior information. Using only SDSS data and a few
radial velocities from the literature, we find that the distance of the Sun
from the Galactic Center is $8.30\pm0.25$ kpc, and the transverse velocity is
$253\pm16$ km/s. Both estimates are in excellent agreement with independent
measurements of these quantities. Assuming a standard disk and bulge model, we
determine the Galactic mass within Pal 5's apogalactic radius of 19 kpc to be
$(2.1\pm0.4)\times10^{11}$ M$_\odot$. Moreover, we find the potential of the
dark halo with a flattening of $q_z = 0.95^{+0.16}_{-0.12}$ to be essentially
spherical within the radial range that is effectively probed by Pal 5. We also
determine Pal 5's mass, distance and proper motion independently from other
methods, which enables us to perform vital cross-checks. We conclude that with
more observational data and by using additional prior information, the
precision of this method can be significantly increased.
