Updated properties of the old open cluster Melotte 66: Searching for multiple stellar populations

TL;DR

This study investigates the old open cluster Melotte 66 to determine if it hosts multiple stellar populations, using new photometric and spectroscopic data, and concludes that observed features are explained by binaries and differential reddening.

Contribution

The paper provides the first detailed analysis ruling out multiple stellar populations in Melotte 66, attributing observed features to binaries and reddening, and refines the cluster's fundamental parameters.

Findings

Main sequence width explained by binaries and reddening

Binary fraction estimated at 30% with mass ratios 0.6-1.0

Cluster parameters refined: age 3.4 Gyr, distance 4.7 kpc

Abstract

Multiple generations of stars are routinely encountered in globular clusters but no convincing evidence has been found in Galactic open clusters to date. In this paper we use new photometric and spectroscopic data to search for multiple stellar population signatures in the old, massive open cluster, Melotte~66. The cluster is known to have a red giant branch wide in color, which could be an indication of metallicity spread. Also the main sequence is wider than what is expected from photometric errors only. This evidence might be associated with either differential reddening or binaries. Both hypothesis have, however, to be evaluated in detail before recurring to the presence of multiple stellar populations. New, high-quality, CCD UBVI photometry have been acquired to this aim with high-resolution spectroscopy of seven clump stars, that are complemented with literature data. Our photometric study confirms that the width of the main sequence close to the turn off point is entirely accounted for by binary stars and differential reddening, with no need to advocate more sofisticated scenarios, such as metallicity spread or multiple main sequences. By constructing synthetic color-magnitude diagrams, we infer that the binary fraction has to be as large as 30$%$ and their mass ratio in the range 0.6-1.0. As a by-product of our simulations, we provide new estimates of the cluster fundamental parameters. We measure a reddening E(B-V)=0.15$\pm$0.02, and confirm the presence of a marginal differential reddening. The distance to the cluster is $4.7^{+0.2}_{-0.1} $kpc and the age is 3.4$\pm$0.3 Gyr, which is somewhat younger and better constrained than previous estimates. Our detailed abundance analysis reveals that, overall, Melotte~66 looks like a typical object of the old thin disk population.