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Light escaping from a gravitational potential suffers a redshift withmagnitude proportional to the depth of the potential. This "gravitationalredshift" is easily measurable in dense stars such as white dwarfs, but is muchweaker and has evaded unambiguous detection in main-sequence stars. I show thatthe effect is directly measurable in the Gaia DR3 radial velocities (RVs) ofthe components of wide binary stars. In a sample of $\sim$500 wide binariescontaining a solar-type main-sequence star and a red giant or red clumpcompanion, the apparent RV of the giant is on average $0.49 \pm 0.02 \,\, \rmkm\,s^{-1}$ lower than that of the main-sequence star. This owes primarily tothe giants' weaker gravitational fields and is in reasonably good agreementwith the value expected from general relativity.

The gravitational redshift of solar-type stars from Gaia DR3 wide binaries