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We search for mass segregation in the intermediate-aged open cluster NGC 6819within a carefully identified sample of likely cluster members. Usingphotometry from the Gaia, 2MASS, and Pan-STARRS surveys as inputs for aBayesian statistics software suite, BASE-9, we identify a rich population of(photometric) binaries and derive posterior distributions for the cluster age,distance, metallicity and reddening as well as star-by-star photometricmembership probabilities, masses and mass ratios (for binaries). Within ourentire sample, we find 2781 likely cluster members and 831 binaries. We selecta main-sequence 'primary sample' with 14.85 < G < 19.5 containing 1515 likelycluster members and 256 binaries with mass ratios q > 0.5, to investigate formass segregation. Within this primary sample, we find the binary radialdistribution is significantly shifted toward the cluster center as compared tothe single stars, resulting in a binary fraction that increases significantlytoward the cluster core. Furthermore, we find that within the binary sample,more massive binaries have more centrally concentrated radial distributionsthan less massive binaries. The same is true for the single stars. As thecluster has persisted through several half-mass relaxation times, and theexpected mass-segregation timescale for stars in our primary sample is alsosignificantly shorter than the cluster age, we interpret these results asstrong evidence for mass segregation in the cluster. Importantly, this is thefirst study to investigate mass segregation of the binaries in the open clusterNGC 6819.

Investigating Mass Segregation of the Binary Stars in the Open Cluster NGC 6819