ERRATUM: "STELLAR DIAMETERS AND TEMPERATURES. III. MAIN SEQUENCE A, F, G, AND K STARS: ADDITIONAL HIGH-PRECISION MEASUREMENTS AND EMPIRICAL RELATIONS" (2013, ApJ, 771, 40)

We correct erroneous JHK magnitudes for stars that appear in Table 7 of the published article. These photometric values were improperly transformed from Two Micron All Sky Survey (2MASS) JHK to Johnson JHK photometric systems due to improper reads of data columns. The method used to perform the photometric transformations described in Section 3 of the published article remains correct.

This erratum presents a new version of the entire Table 7, with the corrections incorporated (values marked with a footnote "c"). We also identify a handful of stars that Table 7 did not have, but should have had; footnotes printed in Table 7 are indicative of transformed 2MASS photometry. The stars with missing footnotes apply to only the H magnitudes (with the exception of HD 11964), as published JK magnitudes in the Johnson system were available for the majority of the stars. These H magnitudes, which were also transformed improperly, are also corrected within this erratum (values marked with a footnote "d"). Last, we correct an error in the Johnson H magnitude of HD 186408, where both the transformation and the original input value were incorrect in the previously published Table 7 (value marked with a footnote "e"). Corrected values are also highlighted in bold type so the reader may easily identify the changes made.

Several versions of color–T_eff relations are presented in the paper (Table 8). The resulting coefficients to the color–T_eff relations without 2MASS colors are not affected by these conversion errors (those marked in Table 8 with a footnote "d"). This holds true even concerning the stars with missing markers in Table 7 (see above), as it was only a transcribing error in making Table 7, and they were properly removed in the analysis. There is no statistically significant change in the results for color–T_eff relations that include the transformed JHK magnitudes (V − J, V − H, V − K, R_J − J, R_J − H, R_J − K, R_C − J, R_C − H, R_C − K, R_K − J, R_K − H, R_K − K, g − J, g − H, and  g − K), and the scatter of these solutions remain much larger than the solutions derived omitting stars with 2MASS JHK magnitudes (those marked in Table 8 with a footnote "d").

We thank Cameron Bell for bringing the error in the photometric conversions to our attention and Eric Mamajek for enlightening discussions with respect to the results.