In [ Kawahara et al .
( 2018 ) ] and [ Masuda et al .
( 2019 ) ] , we reported the discovery of four self-lensing binaries consisting of F/G-type stars and ( most likely ) white dwarfs whose masses range from 0.2 to 0.6 solar masses .
Here we present their updated system parameters based on new radial velocity data from the Tillinghast Reflector Echelle Spectrograph at the Fred Lawrence Whipple Observatory , and the Gaia parallaxes and spectroscopic parameters of the primary stars .
We also briefly discuss the astrophysical implications of these findings .