Searching for Tidal Tails in the Open Cluster M35

During star cluster dissolution, stars slowly leaving the cluster populate tidal tails that spread along the cluster orbit about the Galactic center. Tidal tails of open clusters can provide insights into both internal cluster dynamics and the structure of the Galaxy. However, they are notoriously hard to find, given their large spatial extents on the sky and low stellar densities. Using N-body simulations, we model the development of tidal tails in the young (~200 Myr) open cluster M35. We then project this model onto the sky to aid our identification of potential members of M35's real tidal tails using Gaia data. We download Gaia, Pan-STARRS and 2MASS photometry for these potential tidal tail members as input for the statistical software suite Bayesian Analysis for Stellar Evolution with Nine parameters (BASE-9). We use PARSEC stellar evolution models within BASE-9 to derive posterior distributions in global cluster properties and star-by-star posterior distributions in mass and mass-ratio (for binaries). Using these data, we investigate for differences between the stars and binaries in the central cluster and the tidal tails.