Image Details
Caption: Figure 4.
A contour plot of the percent error in T eff as a function of the percent errors in R * and F bol, derived from Equation (11). We see that the dependence on M * is much weaker, and with a typical ﹩{\sigma }_{{R}_{* }}﹩ of 3% and a systematic floor of L * ∼ 2.4%, the resulting constraint on T eff can be ∼1.5%—well below the systematic floor from evolutionary models, SED models, or spectra. In the best cases, we can measure R * to ∼1.7% and T eff uncertainties of just under 1%.
© 2023. The Author(s). Published by the American Astronomical Society.