at 4019Å. The linelist from Johnson & Bolte (2001) was used, except our [$gf$-value]{} for the line was revised up by 0.05 dex to reflect the recent laboratory measurement of the oscillator strength by Nilsson [et al.]{} (2002). The line noted by Sneden [et al.]{} (1996), which in our previous work was an unimportant contributor to the absorption, is much more important in this s-process-rich star. Our fit to the left of the Th line was improved if we shifted the line by 0.02Å to the red from its position in Johnson & Bolte (2001) and its [$gf$-value]{} decreased by 0.1 dex. This was a cosmetic change and does not affect the Th abundance determination. In an attempt to test the goodness of the fit of our synthesis spectra with different Th abundances, we did a $\chi^2$ test of the wavelength region of 4019.08–4019.25Å. The errors in our data points were assumed to be solely due to the Poisson noise in the counts, The smoothing of the synthesis was set by other lines in the region and not allowed to vary. The C abundance was set to match the [$^{12}$CH]{} lines at 4020Å (\[C/Fe\]=1.82), and a [$^{12}$CH]{}/[$^{13}$CH]{} value of 12 