Image Details
Caption: Figure 2.
A contour plot of the percent error in R * as a function of the percent errors in ρ * and M *, derived in Equation (9). We see that the dependence on M * is much weaker, and with a typical ﹩{\sigma }_{\,{\rho }_{* }}﹩ of 10%, the resulting constraint on R * can be well below the systematic floor from evolutionary models. In the best cases, we can measure ρ * to ∼1%, resulting in R * uncertainties of ∼1.7%—almost entirely dominated by the systematic floor in M *.
© 2023. The Author(s). Published by the American Astronomical Society.