Optical and infrared interferometers definitively established that the photometric standard Vega ( = \alpha Lyrae ) is a rapidly rotating star viewed nearly pole-on .
Recent independent spectroscopic analyses could not reconcile the inferred inclination angle with the observed line profiles , preferring a larger inclination .
In order to resolve this controversy , we observed Vega using the six-beam Michigan Infrared Combiner ( MIRC6 ) on the Center for High Angular Resolution Astronomy ( CHARA ) Array .
With our greater angular resolution and dense ( u , v ) -coverage , we find Vega is rotating less rapidly and with a smaller gravity darkening coefficient than previous interferometric results .
Our models are compatible with low photospheric macroturbulence and also consistent with the possible rotational period of \sim 0.71 days recently reported based on magnetic field observations .
Our updated evolutionary analysis explicitly incorporates rapid rotation , finding Vega to have a mass of 2.15 ^ { +0.10 } _ { -0.15 } M _ { \odot } and an age 700 ^ { -75 } _ { +150 } Myrs , substantially older than previous estimates with errors dominated by lingering metallicity uncertainties ( Z = 0.006 ^ { +0.003 } _ { -0.002 } ) .