WOCS 40007: A Detached Eclipsing Binary near the Turnoff of the Open Cluster NGC 6819

TL;DR

This study precisely measures the masses and radii of a binary star system in NGC 6819, using these data to estimate the cluster's age and explore stellar evolution near the turnoff point.

Contribution

The paper provides the first precise mass and radius measurements for the binary components in NGC 6819, and uses these to derive a new age estimate for the cluster based on the mass-radius relation.

Findings

Binary components have ~1.6% mass and ~0.5% radius uncertainties.

Cluster age estimated at approximately 2.4 to 3.1 Gyr, depending on method.

Discovery of a third star orbiting the binary with a period over 3000 days.

Abstract

We analyze extensive BVR_cI_c time-series photometry and radial-velocity measurements for WOCS 40007 (Auner 259; KIC 5113053), a double-lined detached eclipsing binary and a member of the open cluster NGC 6819. Utilizing photometric observations from the 1-meter telescope at Mount Laguna Observatory and spectra from the WIYN 3.5-meter telescope, we measure precise and accurate masses (~1.6% uncertainty) and radii (~0.5%) for the binary components. In addition, we discover a third star orbiting the binary with a period greater than 3000 days using radial velocities and Kepler eclipse timings. Because the stars in the eclipsing binary are near the cluster turnoff, they are evolving rapidly in size and are sensitive to age. With a metallicity of [Fe/H]=+0.09+/-0.03, we find the age of NGC 6819 to be about 2.4 Gyr from CMD isochrone fitting and 3.1+/-0.4 Gyr by analyzing the mass-radius (M-R) data for this binary. The M-R age is above previous determinations for this cluster, but consistent within 1 sigma uncertainties. When the M-R data for the primary star of the additional cluster binary WOCS 23009 is included, the weighted age estimate drops to 2.5+/-0.2 Gyr, with a systematic uncertainty of at least 0.2 Gyr. The age difference between our CMD and M-R findings may be the result of systematic error in the metallicity or helium abundance used in models, or due to slight radius inflation of one or both stars in the WOCS 40007 binary.