2025/03/24 by Taşdemir, Seval, Çınar, Deniz Cennet, Canbay, Remziye +3 · 1 citation
#Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences
paper · doi:10.48550/arxiv.2503.19015
We conducted an in-depth analysis of NGC 6793 open cluster via Gaia DR3 data, including astrometric, spectroscopic, and photometric measurements. 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 \varpi = 1.674 ±0.045 mas and (μαcos δ,~μδ) =(3.814±0.031,~3.547±0.034) mas yr-1. Fundamental astrophysical parameters of NGC 6793 are derived simultaneously as t = 650 ± 50 Myr, μ = 9.508±0.070 mag, and E(G\rm BP-G\rm RP) = 0.361 ± 0.035 mag. Additionally, the cluster's luminosity function analysis reveals the G-absolute magnitude limit of the most likely stars, indicating a well-defined stellar population. The total mass of the cluster, determined through the mass function (MF) and considering stars with membership probabilities P ≥ 0.5, was estimated as 139 ± 12 M/M\odot. 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 (A\rm o,~D\rm o) = (85∘.85 ± 0∘.11,~3∘.12 ± 0∘.57). Analyses have shown 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, where the dynamical evolution parameter τ significantly exceeds one. These results highlight both the cluster's internal stability and its connection to the thin disc population.