Unresolved Binaries and Multiples in the Intermediate Mass Range in open clusters: Pleiades, Alpha Per, Praesepe, and NGC 1039

Abstract

In this study, we continue our project to search for unresolved binary and multiple systems in open clusters exploiting the photometric diagram (H-W2)-W1 vs W2-(BP-K) firstly introduced in \citet{Malofeeva+2022}. In particular, here we estimate the binary and multiple star ratios and the distribution of the component mass ratio $q$ in the Galactic clusters Alpha Persei, Praesepe, and NGC 1039. We have modified the procedure outlined in our first study \citep{Malofeeva+2022} making star counts automatic and by introducing bootstrapping for error estimation. Basing on this, we re-investigated the Pleiades star cluster in the same mass range as in our previous work and corrected an inaccuracy in the mass ratio $q$ distribution. The binary and multiple star ratio in the four clusters is then found to lie between 0.45$\pm$0.03 and 0.73$\pm$0.03. On the other hand, the ratio of systems with multiplicity more than 2 is between 0.06$\pm$0.01 and 0.09$\pm$0.02. The distribution of the component mass ratio $q$ is well fitted with a Gaussian having the mode between 0.22$\pm$0.04 and 0.52$\pm$0.01 and the dispersion between 0.10$\pm$0.02 and 0.35$\pm$0.07. All clusters show a large number of the very low-mass secondary components in the binary systems with primary components below 0.5 $M_{\odot }$.

16 pages, 12 figures, accepted for publication in the Astronomical Journal

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• TESS observations of the Pleiades cluster: a nursery for delta Scuti stars
• Young nearby open clusters and their luminosity functions
• Photometric Determination of Unresolved Main-sequence Binaries in the Pleiades: Binary Fraction and Mass Ratio Distribution
• Stellar masses and mass ratios for Gaia open cluster members
• Photometric Identification of Unresolved Binary Stars in Nearby Open Star Clusters
• Precision speckle interferometry with CMOS detector
• Looking for Signs of Unresolved Binarity in the Continuum of LAMOST Stellar Spectra