Evcil, SerkanAdalali, SimgeAlan, NeslihanCanbay, RemziyeBilir, Selcuk2025-01-272025-01-2720240004-63371521-3994https://doi.org/10.1002/asna.20240038https://hdl.handle.net/20.500.12428/21836Eclipsing 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.eninfo:eu-repo/semantics/closedAccessStar: binaries: eclipsingfundamental parametersindividual (IS CMa)Galaxy: kinematics and dynamicsArticle3456-710.1002/asna.20240038N/AWOS:0012526767000012-s2.0-85196628633Q3