gr8stars. II.

We furthermore use isochrone fitting to determine mass, radius, and age for all 585 stars, using input from all results. We use the radii determined by SED (Spectral Energy Distribution) fitting in the first gr8stars paper as a comparison to our isochronal radii from this work, in addition to comparing the isochronal logg to spectroscopic logg. The scatter in mass and radius from the use of different spectroscopic methods is investigated and propagated to exoplanetary parameters.

The induced fractional uncertainties in planetary radius (<~3 per cent) and mass (<~5 per cent) are found to be below those typically found in the literature. We estimate a lower limit on planetary equilibrium temperature fractional uncertainty of ~4 per cent, a noise floor that is currently not sufficiently represented in the literature.