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The rotation-mass-age relationship offers a promising avenue for measuringthe ages of field stars, assuming the attendant uncertainties to this techniquecan be well characterized. We model stellar angular momentum evolution startingwith a rotation distribution from open cluster M37. Our predictedrotation-mass-age relationship shows significant zero-point offsets compared toan alternative angular momentum loss law and published gyrochronologyrelations. Systematic errors at the 30 percent level are permitted by currentdata, highlighting the need for empirical guidance. We identify two fundamentalsources of uncertainty that limit the precision of rotation-based ages andquantify their impact. Stars are born with a range of rotation rates, whichleads to an age range at fixed rotation period. We find that the inherentambiguity from the initial conditions is important for all young stars, andremains large for old stars below 0.6 solar masses. Latitudinal surfacedifferential rotation also introduces a minimum uncertainty into rotationperiod measurements and, by extension, rotation-based ages. Both models and thedata from binary star systems 61 Cyg and alpha Cen demonstrate that latitudinaldifferential rotation is the limiting factor for rotation-based age precisionamong old field stars, inducing uncertainties at the ~2 Gyr level. We alsoexamine the relationship between variability amplitude, rotation period, andage. Existing ground-based surveys can detect field populations with ages asold as 1-2 Gyr, while space missions can detect stars as old as the Galacticdisk. In comparison with other techniques for measuring the ages of lower mainsequence stars, including geometric parallax and asteroseismology,rotation-based ages have the potential to be the most precise chronometer for0.6-1.0 solar mass stars.

How Good a Clock is Rotation? The Stellar Rotation-Mass-Age Relationship for Old Field Stars