Comparison of synthetic profiles of H and He lines calculated from our models (, log g = 5.46) with our UVES observation (for clarity smoothed with a low-pass filter, Savitzky & Golay 1964). Left panel: abundances from Table 1, and Sc, Ti, V, Cr, Mn, and Co with solar abundances (Scott et al. 2015a). Right panel: similar model in the left panel, except the Sc, Ti, V, Cr, Mn, and Co abundances are artifically increased by a factor of 700. The vertical bar indicates 10% of the continuum flux.