| Authors: | T. Yontan 1, R. Canbay 2 |
| Affiliations: | (1) Istanbul University, Faculty of Science, Department of Astronomy and Space Sciences, Istanbul, Turkey; (2) Istanbul University, Institute of Graduate Studies in Science, Programme of Astronomy and Space Sciences, Istanbul, Turkey |
| Accepted by: | Physics and Astronomy Reports |
| URL: | https://ui.adsabs.harvard.edu/abs/2023arXiv231013582Y/abstract |
In this study, we have used the Gaia Third Data Release (Gaia DR3) to investigate an intermediate-age open cluster Collinder 74. Taking into account the stars with membership probabilities over 0.5 and inside the limiting radius of the cluster, we identified 102 most likely cluster members. The mean proper-motion components of Collinder 74 are estimated as ($\mu_{\alpha}\cos \delta, \mu_{\delta})=(0.960 \pm 0.005, -1.526 \pm 0.004$) mas yr$^{-1}$. We detected previously confirmed four blue straggler stars which show flat radial distribution. Colour excess, distance, and age of the cluster were estimated simultaneously by fitting PARSEC isochrones to the observational data on Gaia based colour magnitude diagram. These values were derived as $E(G_{\rm BP}-G_{\rm RP})=0.425\pm 0.046$ mag, $d=2831 \pm118$ pc and $t=1800 \pm 200$ Myr, respectively. The mass function slope was estimated as $\Gamma = 1.34 \pm 0.21$ within the mass range $0.65\leq M/ M_{\odot}\leq 1.58$ which is well matched with that of Salpeter. Stellar mass distribution indicated that the massive and most likely stars are concentrated around the cluster center. The total mass of the cluster was found to be 365 $M/M_{\odot}$ for the stars with probabilities $P>0$. Galactic orbit integration shows that the Collinder 74 follows a boxy pattern outside the solar circle and is a member of the thin-disc component of the Galaxy.
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