Abstract This paper introduces a new method to search for unresolved binary stars in open star clusters. The work aims at improving the approach introduced previously, which employs the (H − W2) − W1 versus W2 − (BP − K) photometric diagram. This diagram, in tandem with the Gaia color–magnitude diagram and using theoretical isochrones as reference sequences, is used to estimate the binary star fraction and the distribution of the component mass ratio q in eight nearby open star clusters, including Pleiades, Alpha Per, and Praesepe, which we investigated in previous studies. In this study, to alleviate the uncertainties associated with the use of theoretical isochrones, we propose an empirical isochrone approach. We show that this is an effective approach to exploring a wider primary-mass interval, in particular for the region of low-mass sources. Box-and-whisker plots are used to present the distribution of the component mass ratio q . The mode of distribution turns out to be in the range of 0.43–0.83 and 0.38–0.63 for Gaia and infrared-visible photometry, respectively. In addition, we update the algorithm to obtain the binary fraction, whose estimate lies in the range of 0.16–0.36 and 0.21–0.44, depending on the method adopted, and show that in previous studies the binary fraction has been overestimated. We do not find evidence that the variable spatial resolution of the employed catalogs (Gaia, Two Micron All Sky Survey, and Wide-field Infrared Survey Explorer) affects the precision of the binary fraction estimate.
Mikhnevich et al. (Wed,) studied this question.
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