How do mass measurements from eclipsing binaries compare in error certainty to Mass-Luminosity estimates?

Eclipsing systems yield errors as low as a few percent, versus 15 to 20 percent or more for M-L.

When comparing the precision of stellar mass determination techniques, the difference between gravity-based dynamical measurements and empirical correlation methods is stark. Measurements derived from binary star systems, particularly those classified as eclipsing binaries where orbital inclination is known precisely, are considered the gold standard; these measurements can often achieve remarkably low uncertainties, sometimes only a few percent error. In contrast, masses estimated for single stars using the Mass-Luminosity Relation are inherently less precise. This relationship, being an approximation based on a curve with scatter around the average, often results in mass estimates carrying an uncertainty of 15 to 20 percent or even higher, even for well-studied main-sequence stars. The precise binary results act as the essential anchor points used to calibrate the less certain indirect methods.