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We identify a small group of low mass ultra fast rotating (UFR) stars which have rotation periods less than 0.3 days and show low levels of flaring activity in their TESS lightcurves. Given the rotation-activity relation, faster rotating stars should display higher levels of activity. We do not find any evidence that the lack of activity is related to age or rotational velocities and conclude it is most likely to be a result of the magnetic configurations of the star. In this talk, we willdoi:10.5281/zenodo.5128900 fatcat:qk4ppj3rgfa5ve3s4bbv4f4bz4