Table A6 'Zsoldos-early-colour-vsn-4' describes correlations for colours and temperatures done by one of us (EZ) using the same technique as used for Zsoldos (1986Obs...106..156Z, fig,1) for finding V. The found B-V and Teff equivalents and estimated accuracies for HR8752 are used as early-colour data in Section 3 of the main paper. For the period around 1900 the following few colour estimates are available for HR 8752. 1900 Jul 27 (2415228) G 1901 Jul 16 (2415582) WG+ 1902 Sep 1 (2415994) WG 1902 Sep 2 (2415995) WG Here G is yellow, WG is white-yellow. The source is G. Mueller \& P. Kempf (1903, Potsdam Publ., Band 14). Using the same technique as in Zsoldos (1986Obs...106..156Z, in constructing his Fig.1), we tried to convert these letter into (B-V) using the list of bright stars , for which J. Wilsing calculated temperatures (1919, Potsdam Publ., Band 24, No. 74, p. 25, Table 3). The Table has 27 stars with colour WG, 13 with G and 6 with WG+. Averaging the temperatures gives WG -> Teff = 5050 +/- 1900 K One star among the WG's has a rather discordant temperature, omitting it gives WG -> Teff = 4700 +/- 800 K WG+ -> Teff = 4800 +/- 300 K G -> Teff = 4100 +/- 700 K Collecting the B-V values of the stars in the four groups from the Bright Star Catalogue, omitting known variables (but keeping suspected variables), and averaging the (B-V)s gives WG -> (B-V) = 0.85 +/- 0.30 (n=26) WG+ -> (B-V) = 1.02 +/- 0.09 (n=6) G -> (B-V) = 1.17 +/- 0.26 (n=13) The stars used for the conversions were mostly giants, so some correction might be necessary. It seems that one hundred years after 1900, the star looked almost the same as around 1900, both in B-V and in V (cf. Fig.10 in the main paper) with V=5.1-5.2, roughly equal to the value of the Reference mean=5.1 in our Fig.13. Could this be an indication of a possible recurrence of an 'event' with a time of about 100 years? There is one more colour estimate, made by H. Osthoff (1916, Specola Astronomica Vaticana, Volume VIII), but he didn't give the date, only said the observations were made between 1894 and 1897. From three observations he estimated the colour (on his own scale) to be 6.2. Mueller & Kempf (1907, Potsdam Publ., Band 17) correlated their and Osthoff's scales, so 6.2 corresponds roughly to G-. Using the same process as above, G- implies a temperature of about 4200+/-700 (from 25 stars), or B-V=1.16+/-0.26 (from 21 stars). However, since there is no exact date, this one does not help much. The following table gives these 'Early-colour-1900' estimates of (B-V) and Teff. The data are given as observations with code "C" for (B-V) in Fig.6, and for Teff in Fig.5, both figures in the main paper. The data for (B-V) have to be corrected for the influence of interstellar reddening. Assuming the observations are compatible with the Johnson (B-V) system, we use the procedure outlined in section 3 of the main paper to find the 'unreddened'(B-V), from which we find Teff using the calibrations outlined in Section 3. The Teff values found from the 'unreddened'(B-V) are displayed in Fig.5 as upward printing triangles. The observational direct data for Teff are given in Fig.5 of the main paper as circles. They have not been 'dereddened' and are lower than the respective Teff from the 'unreddened' (B-V) data. Table of 'Zsoldos-early-colour' estimates ------------------------------------------------------------------------------ JD Date colour (B-V) e_(B-V) Teff e_Teff logT e_logT Reference ------------------------------------------------------------------------------ 2413560 1896_Jan_1 G- +1.16 .26 | 4200 700 3.623 0.072 1916, Specola Astronomica Vaticana, Volume VIII 2415228 1900_Jul_27 G +1.17 .26 | 4100 700 3.613 0.074 1903, Potsdam Publ., Band 14 2415582 1901_Jul_16 WG+ +1.02 .09 | 4800 300 3.681 0.027 1903, Potsdam Publ., Band 14 2415994 1902_Sep_1 WG +0.85 .30 | 4700 800 3.672 0.074 1903, Potsdam Publ., Band 14 2415995 1902_Sep_2 WG +0.85 .30 | 4700 800 3.672 0.074 1903, Potsdam Publ., Band 14 -------------------------------------------------------------------------------- (End)