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    CCD UBV and Gaia DR3 based analysis of NGC 189, NGC 1758 and NGC 7762 open clusters
    (Elsevier Sci Ltd, 2023) Yontan, Talar; Bilir, Selcuk; Cakmak, Hikmet; Raul, Michel; Banks, Timothy; Soydugan, Esin; Canbay, Remziye
    This paper presents photometric, astrometric, and kinematic analyses of the open clusters NGC 189, NGC 1758 and NGC 7762 based on CCD UBV photometric and Gaia Data Release 3 (DR3) data. According to membership analyses, we identified 32, 57 and 106 most probable member stars with membership probabilities P >= 0:5 in NGC 189, NGC 1758 and NGC 7762, respectively. The color excesses and photometric metallicities of each cluster were determined separately using UBV two-color diagrams. The color excess E(B - V) is 0: 590 +/- 0:023 mag for NGC 189, 0:310 +/- 0:022 mag for NGC 1758 and 0:640 +/- 0:017 mag for NGC 7762. The photometric metallicity [Fe/H] is -0:08 +/- 0:03 dex for both NGC 189 and NGC 1758, and -0:12 +/- 0:02 dex for NGC 7762. Distance moduli and ages of the clusters were obtained by comparing PARSEC isochrones with the color-magnitude diagrams constructed from UBV and Gaia photometric data. During this process, we kept as constant color excess and metallicity for each cluster. The estimated isochrone distance is 1201 +/- 53 pc for NGC 189, 902 +/- 33 pc for NGC 1758 and 911 +/- 31 pc for NGC 7762. These are compatible with the values obtained from trigonometric parallax. Ages of the clusters are 500 +/- 50 Myr, 650 +/- 50 Myr and 2000 +/- 200 Myr for NGC 189, NGC 1758 and NGC 7762, respectively. Galactic orbit integration of the clusters showed that NGC 1758 completely orbits outside the solar circle, while NGC 189 and NGC 7762 enter the solar circle during their orbits. (c) 2023 COSPAR. Published by Elsevier B.V. All rights reserved.
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    Updated absolute parameters and kinematics of IS CMa
    (Wiley-V C H Verlag Gmbh, 2024) Evcil, Serkan; Adalali, Simge; Alan, Neslihan; Canbay, Remziye; Bilir, Selcuk
    Eclipsing binary systems are significant objects for astrophysics in that direct observations can determine the fundamental parameters of stars. In this study, we precisely determined the fundamental parameters of the binary component stars obtained by simultaneous analysis of radial velocities and the TESS light curve using the Wilson and Devinney code. Following the analysis, the masses and radii of the primary and secondary components were determined as M1 = 1.58 +/- 0.01M(circle dot), M-2 = 0.48 +/- 0.02M(circle dot), and R-1 = 1.93 +/- 0.01R(circle dot), R-2 = 1.14 +/- 0.01R(circle dot), respectively. Furthermore, the distance of IS CMa is calculated as 92.7 +/- 6.5$$ 92.7\pm 6.5 $$ pc. On the basis of the analysis of the mid-eclipse times, it was found that the variation in the orbital period is represented by an upward parabola. It has an increasing rate of dP/dt = 1.09 x 10(-7). Using PARSEC stellar evolutionary tracks and isochrones with solar metallicity estimated the age of IS CMa as 1.3 +/- 0.1 Gyr. Kinematic and Galactic orbital parameters of IS CMa were obtained from the astrometric and spectroscopic data of the system. The Galactic orbit analysis reveals that IS CMa formed inside the solar circle and it is a member of the young thin-disc population.