Photometric analysis of the eclipsing binary 2MASS 19090585+4911585
St. Raetz (1), M. Vanko (1), M. Mugrauer (1), T. O. B. Schmidt (1), T., Roell (1), T. Eisenbeiss (1), M. M. Hohle (1,3), A. Koeltzsch (1), Ch. Ginski, (1), C. Marka (1), M. Moualla (1), N. Tetzlaff (1), Ch. Broeg (2), R., Neuh\"auser (1) ((1) Astrophysikalisches Institut und
TL;DR
This study clarifies the true source of variability in a nearby star, confirming 2MASS 19090585+4911585 as an overcontact W UMa type binary with a 0.2884-day period through photometric analysis.
Contribution
The paper corrects a misclassification by identifying the true eclipsing binary and provides detailed photometric analysis of its light curves.
Findings
2MASS 19090585+4911585 is the true variable source.
The system is an overcontact W UMa type binary.
Orbital period is approximately 0.2884 days.
Abstract
We report on observations of the eclipsing binary 2MASS 19090585+4911585 with the 25 cm auxiliary telescope of the University Observatory Jena. We show that a nearby brighter star (2MASS 19090783+4912085) was previously misclassified as the eclipsing binary and find 2MASS 19090585+4911585 to be the true source of variation. We present photometric analysis of VRI light curves. The system is an overcontact binary of W UMa type with an orbital period of (0.288374 +/- 0.000010) d.
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