We present the analysis of an eccentric , partially eclipsing long-period ( P = 19.23 d ) binary system KIC 9777062 that contains main sequence stars near the turnoff of the intermediate age open cluster NGC 6811 .
The primary is a metal-lined Am star with a possible convective blueshift to its radial velocities , and one star ( probably the secondary ) is likely to be a \gamma Dor pulsator .
The component masses are 1.603 \pm 0.006 ( stat . ) \pm 0.016 ( sys . )
and 1.419 \pm 0.003 \pm 0.008 M _ { \odot } , and the radii are 1.744 \pm 0.004 \pm 0.002 and 1.544 \pm 0.002 \pm 0.002 R _ { \odot } .
The isochrone ages of the stars are mildly inconsistent : the age from the mass-radius combination for the primary ( 1.05 \pm 0.05 \pm 0.09 Gyr , where the last quote was systematic uncertainty from models and metallicity ) is smaller than that from the secondary ( 1.21 \pm 0.05 \pm 0.15 Gyr ) and is consistent with the inference from the color-magnitude diagram ( 1.00 \pm 0.05 Gyr ) .

We have improved the measurements of the asteroseismic parameters \Delta \nu and \nu _ { max } for helium-burning stars in the cluster .
The masses of the stars appear to be larger ( or alternately , the radii appear to be smaller ) than predicted from isochrones using the ages derived from the eclipsing stars .

The majority of stars near the cluster turnoff are pulsating stars : we identify a sample of 28 \delta Sct , 15 \gamma Dor , and 5 hybrid types .
We used the period-luminosity relation for high-amplitude \delta Sct stars to fit the ensemble of the strongest frequencies for the cluster members , finding ( m - M ) _ { V } = 10.37 \pm 0.03 .
This is larger than most previous determinations , but smaller than values derived from the eclipsing binary ( 10.47 \pm 0.05 ) .