First photometric investigation of V517 Cam combined with ground-based and TESS data

TL;DR

This study presents the first detailed photometric analysis of the V517 Cam eclipsing binary system, combining space-based TESS data with ground-based observations to precisely determine stellar parameters and evolutionary status.

Contribution

It is the first to combine TESS and ground-based photometry for V517 Cam, providing detailed stellar parameters and evolutionary insights.

Findings

Masses and radii of both stars were precisely determined.

Distance to V517 Cam is estimated at 284±20 pc.

Primary star is near the main-sequence, secondary is pre-main-sequence.

Abstract

The observations of eclipsing binary systems are of great importance in astrophysics, as they allow direct measurements of fundamental stellar parameters. By analysing high-quality space-based observations with ground-based photometric data, it becomes possible to detect these fundamental parameters with greater precision using multicolour photometry. Here, we report the first photometric analysis results of the V517 Cam eclipsing binary system by combining the Transiting Exoplanet Survey Satellite (TESS) light curve and new CCD observations in BVRI filters, obtained with a 60 cm robotic telescope (T60) at the T\"UB\.ITAK National Observatory. By means of photometric analyses, the masses and radii of the primary and secondary stars were carefully determined to be $M_{1}= 1.47\pm 0.06\,M_\odot$, $M_{2}= 0.79\pm0.05\,M_\odot$, and $R_{1}=1.43\pm 0.03\,R_\odot$, $R_{2}= 0.75\pm 0.04\,R_\odot$, respectively. Furthermore, the distance to V517 Cam was calculated to be $284\pm20$ pc. The overall age of the system is estimated to be around $63\pm15$ Myr. At this age, the primary component stands near the onset of its main-sequence evolution, near the ZAMS, whereas the secondary component remains in the pre-main-sequence evolutionary phase. To better understand the evolutionary status and nature of V517 Cam, the mass ratio and temperature values, obtained with relatively low sensitivity by photometric measurements, need to be confirmed by spectral analysis.