A study of detached eclipsing binary systems towards the open cluster NGC 7209

This work presents a detailed analysis of five detached eclipsing binary systems located towards the NGC 7209 cluster, using data from the TESS mission and ground-based photometry. Two of these systems are newly discovered and show light curves consistent with those of Algol-type eclipsing variables. We derived fundamental parameters for both components of these binaries, including their masses and radii. The parameters of these binaries were calculated using the PHOEBE and EXOPLANET softwares. The orbital periods of these systems range from ∼ 0.88 to ∼ 7.92 days. The primary components of binaries have masses ranging from ∼ 0.82 to ∼ 1.20 solar masses, classifying four as Sun-type stars and one as an intermediate-mass star. Their membership in NGC 7209 was assessed using HDBSCAN, which determined that all five systems are non-members of the cluster. We also investigated the evolutionary status of these binary stars from their positions on the H-R diagram, suggesting that all five are main-sequence binaries.

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