Accurate measurements of the internal dynamics of young stellar clusters can be used to extract crucial information about their formation process. With Gaia, we are now able to trace stellar motions and study the dynamics of star clusters with unprecedented precision. A fundamental requirement for this analysis is a well-defined and reliable list of probable members. We examine d a region with a radius of a 2{deg} in Cepheus OB4, centered on the young cluster Berkeley 59, to build a reliable candidate member list. Our catalog enables the determination of structural and kinematic parameters of the cluster, as well as other properties of its stellar population. We compiled a catalog of optical and near-infrared photometry, along with precise positions and proper motions from Gaia DR3, for sources in the Cepheus OB4 field. Membership probabilities were determined using a probabilistic random forest algorithm and further refined by requiring HR diagram positions consistent with a young age. From a list of 1030 probable members, we estimate a distance of 1009+/-12pc to Berkeley 59. Masses, extinction, and ages were derived by fitting the spectral energy distributions to atmospheric and evolutionary models, while internal dynamics was analyzed using proper motions relative to the cluster's mean motion. Berkeley 59 exhibits an asymmetric expansion pattern with velocity increasing outward and a preferred motion toward the north. The IMF between 0.4 and 7M_{sun} follows a single power law (dN/dM{prop.to}M^-alpha^), with the slope alpha=2.3+/-0.3, consistent with Salpeter's slope and previous studies in the region. The region's median age, estimated from the HR diagram, is 2.9Myr. The velocity dispersion of Berkeley 59 exceeds the virial velocity dispersion derived from its total mass (650+/-30M{sun}_) and half-mass radius (1.71+/-0.13pc). The 2D motions of a stellar group located ~1{deg} north of Berkeley 59 provide further support for the previously proposed triggered star formation scenario.
Cone search capability for table J/A+A/703/A193/table3 (Members selected in this work, along with the Teff and AV from the SED fitting)
