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We present the spatially resolved absolute brightness of the Fe X, Fe XI andFe XIV visible coronal emission lines from 1.08 to 3.4 $R_\odot$, observedduring the 2019 July 2 total solar eclipse (TSE). The morphology of the coronawas typical of solar minimum, with a dipole field dominance showcased by largepolar coronal holes and a broad equatorial streamer belt. The Fe XI line isfound to be the brightest, followed by Fe X and Fe XIV (in disk $B_\odot$units). All lines had brightness variations between streamers and coronalholes, where Fe XIV exhibited the largest variation. However, Fe X remainedsurprisingly uniform with latitude. The Fe line brightnesses are used to inferthe relative ionic abundances and line of sight averaged electron temperature($T_e$) throughout the corona, yielding values from 1.25 - 1.4 MK in coronalholes up to 1.65 MK in the core of streamers. The line brightnesses andinferred $T_e$ values are then quantitatively compared to the PSIMagnetohydrodynamic model prediction for this TSE. The MHD model predicted theFe lines rather well in general, while the forward modeled line ratios slightlyunderestimated the observationally inferred $T_e$ within 5 to 10 % averagedover the entire corona. Larger discrepancies in the polar coronal holes maypoint to insufficient heating and/or other limitations in the approach. Thesecomparisons highlight the importance of TSE observations for constrainingmodels of the corona and solar wind formation.

The Solar Minimum Eclipse of 2019 July 2: II. The First Absolute Brightness Measurements and MHD Model Predictions of Fe X, XI and XIV out to 3.4 Rs