The Hyades , Praesepe , and Pleiades are well studied stellar clusters that anchor important secondary stellar age indicators .
Recent studies have shown that main sequence turn off-based ages for these clusters may depend on the degree of rotation in the underlying stellar models .
Rotation induces structural instabilities that can enhance the chemical mixing of a star , extending its fuel supply .
In addition , rotation introduces a modulation of the star ’ s observed magnitude and color due to the effects of gravity darkening .
We aim to investigate the extent to which stellar rotation affects the age determination of star clusters .
We utilize the MESA stellar evolution code to create models that cover a range of rotation rates corresponding to \Omega / \Omega _ { c } = 0.0 to 0.6 in 0.1 dex steps , allowing the assessment of variations in this dimension .
The statistical analysis package , MATCH , is employed to derive ages and metallicities by fitting our MESA models to Tycho B _ { T } , V _ { T } and 2MASS J , K _ { s } color-magnitude diagrams .
We find that the derived ages are relatively insensitive to the effects of rotation .
For the Hyades , Praesepe , and Pleiades , we derive ages based on synthetic populations that model a distribution of rotation rates or a fixed rate .
Across each case , derived ages tend to agree roughly within errors , near 680 , 590 , and 110 - 160 Myr for the Hyades , Praesepe , and Pleiades , respectively .
These ages are in agreement with Li depletion boundary-based ages and previous analyses that used non-rotating isochrones .
Our methods do not provide a strong constraint on the metallicities of these clusters .