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We report the identification of a numerous binary star population in therecently discovered ~3 Gyr old open cluster UBC 274. It becomes visible oncethe cluster color-magnitude diagram is corrected by differential reddening andspans mass ratios (q) values from 0.5 up to 1.0. Its stellar density radialprofile and cumulative distribution as a function of the distance from thecluster's center reveal that it extends out to the observed boundaries of thecluster's tidal tails (~ 6 times the cluster's radius) following a spatialdistribution indistinguishable from that of cluster Main Sequence (MS) stars.Furthermore, binary stars with q values smaller or larger than 0.75 do not showany spatial distribution difference either. From Gaia DR2 astrometric andkinematics data we computed Galactic coordinates and space velocities withrespect to the cluster's center and mean cluster space velocity, respectively.We found that, cluster members located all along the tidal tails, irrespectiveof being a single or binary star, move relatively fast. The projection of theirmotions on the Galactic plane resembles that of a rotating solid body, whilethose along the radial direction from the Galactic center and perpendicular tothe Galactic plane suggest that the cluster is being disrupted. The similarityof the spatial distributions and kinematic patterns of cluster MS and binarystars reveals that UBC 274 is facing an intense process of disruption that hasapparently swept out any signature of internal dynamic evolution like masssegregation driven by two-body relaxation.

A binary star sequence in the outskirts of the disrupting Galactic open cluster UBC 274