Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 761, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/761/1/L3
Keywords
infrared: stars; stars: individual (Vega); stars: rotation; techniques: interferometric
Categories
Funding
- National Science Foundation [AST-1211929, AST-0352723, AST-0707927, AST-1108963]
- Georgia State University
- University of Michigan
- NASA [NNH09AK731]
- Science and Technology Facilities Council [ST/J001651/1] Funding Source: researchfish
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1211929] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1108963] Funding Source: National Science Foundation
- STFC [ST/J001651/1] Funding Source: UKRI
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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 on the Center for High Angular Resolution Astronomy Array. With our greater angular resolution and dense (u, v)-coverage, we find that 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 are also consistent with the possible rotational period of similar to 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(-0.15) (+0.10) M-circle dot and an age 700(+150) (-75) Myr, substantially older than previous estimates with errors dominated by lingering metallicity uncertainties (Z = 0.006(-0.002) (+ 0.003)).
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