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Precise measurements of eclipsing binary parameters and statistical studiesof young clusters have suggested that some magnetically active low-mass dwarfspossess radii inflated by $\sim$5-15% relative to theoretical expectations. Iftrue, this effect should be pronounced in young open clusters, due to the rapidrotation and strong magnetic activity of their most extreme members. We explorethis possibility by determining empirical radii for 83 members of the nearbyPleiades open cluster, using spectral energy distribution fitting to establish$\mathcal{F}_{bol}$ with a typical accuracy of $\approx$3\% together with colorand spectro-photometric indices to determine $T_{\rm eff}$. We find severalPleiades members with radii inflated above radius-$T_{\rm eff}$ models fromstate-of-the-art calculations, and apparent dispersions in radii for theK-dwarfs of the cluster. Moreover, we demonstrate that this putative radiusinflation correlates strongly with rotation rate, consistent with inflation ofyoung stars by magnetic activity and/or starspots. We argue that this signal isnot a consequence of starspot-induced color anomalies, binarity, or deptheffects in the cluster, employing Gaia DR1 distances as a check. Finally, weconsider the lithium abundances of these stars, demonstrating a triplecorrelation between rotation rate, radius inflation, and enhanced lithiumabundance. Our result---already significant to $\sim$99.99%confidence---provides strong support for a magnetic origin of the inflatedradii and lithium dispersion observed in young, low-mass stars.

A Measurement of Radius Inflation in the Pleiades and its Relation to Rotation and Lithium Depletion