Comprehensive Analysis of NGC 6134: Structure, Dynamics, and Blue Straggler Star Candidates

Open clusters play a critical role in the study of both stellar and Galactic evolution. We present a comprehensive analysis of the open cluster NGC 6134 using Gaia DR3 astrometric and photometric data, supplemented with multiwavelength observations from the Two Micron All Sky Survey, Wide-field Infrared Survey Explorer, NEOWISE, and Transiting Exoplanet Survey Satellite (TESS). A total of 714 high-probability members were identified using the Hierarchical Density-based Spatial Clustering of Applications with Noise algorithm. The cluster parameters were derived by Bayesian isochrone fitting with BASE-9, resulting in log (age/yr) = 9.1683 ± 0.019, [Fe/H] = 0.0911 ± 0.04, and A V = 1.2095 ± 0.015 mag. The cluster is dynamically relaxed ( t rh = 16.59 ± 0.25, ≪age) with significant mass segregation (Λ MSR = 1.71 ± 0.26). Galactic orbital integration using galpy indicates that the cluster resides in the thin disk on a slightly eccentric orbit. We identified three candidates of blue straggler stars (BSSs). The first candidate was modeled as an EA-type semidetached eclipsing binary using TESS photometry and Markov Chain Monte Carlo fitting, and Candidate 2 was fitted with a spectral energy distribution (SED) using the Virtual Observatory SED Analyzer tool, providing estimates of its temperature, surface gravity, and metallicity based on the SED-fitting results. However, the third candidate lacks sufficient observational data, which prevents further analysis. These results highlight binary mass transfer as a dominant channel of BSS candidates in NGC 6134, providing observational evidence for the formation mechanism of blue stragglers.