Comprehensive Analysis of Middle-Aged Open Cluster NGC 6793 in Vulpecula via Gaia DR3 Data

We conducted an in-depth analysis of NGC 6793 open cluster via Gaia DR3 data, including astrometric, spectroscopic, and photometric measurements. A selection of 147 stars, which show membership probabilities 𝑃 ≥ 0.5 were classified as likely members. The mean trigonometric parallaxes and proper-motion components of the cluster were found to be 𝜛 = 1.674 ± 0.045 mas and (𝜇𝛼 cos 𝛿, 𝜇𝛿) =(3.814 ± 0.031, 3.547 ± 0.034) mas yr−1 . The fundamental astrophysical parameters of NGC 6793 are derived simultaneously as 𝑡 = 650 ± 50 Myr, 𝜇 = 9.508 ± 0.070 mag and 𝐸(𝐺BP − 𝐺RP) = 0.361 ± 0.035 mag. The cluster’s luminosity function shows the 𝐺-absolute magnitude limit of its main stars, indicating a clear stellar population. The cluster’s total mass, from the mass function with 𝑃 ≥ 0.5 stars, is estimated as 139 ± 12 𝑀/𝑀⊙. The slope of the MF was found to be Γ = 1.40±0.26, a result consistent with the Salpeter value. The kinematic analyses present velocity ellipsoid parameters as well as the convergent point (𝐴o, 𝐷o) = (85◦ .85 ± 0 ◦ .11, 3 ◦ .12 ± 0 ◦ .57). Analyses show that it is moving in a box-shaped orbit beyond the Sun’s galactic radius and belongs to the thin disk population of the Milky Way. The calculated relaxation time suggests that NGC 6793 has reached a dynamically relaxed state with the dynamical evolution parameter 𝜏 significantly exceeds one. These results show the cluster’s stability and link to the thin disc population.