the excitation equilibrium of lines. Deriving [T$_{\rm eff}$]{} from colors in carbon-rich stars can be problematic because the presence of a large number of molecular lines affects the observed colors. However Hill [et al.]{} (2000) found that their excitation equilibrium temperature was consistent with temperatures derived from colors when they included the effects of the molecular lines on the atmospheres and on the colors. Our gravity comes from ionization equilibrium of /. The validity of this assumption in view of possible NLTE effects on lines has been the subject of much recent discussion (see e.g., Lucatello [et al.]{} 2003; Johnson 2002), but the abundances of most of the heavy elements are affected in the same manner by a change in log $g$. The microturbulent velocity ($\xi$) was determined by requiring lines of different equivalent widths (EWs) to give the same \[Fe/H\]. Our final atmospheric parameters are [T$_{\rm eff}$]{}=5500K, log $g$=2.70, $\xi$=1.3 km/s and \[Fe/H\]$_{mod}=-$2.30. These agree well with the parameters adopted by A02 for this same star ([T$_{\rm eff}$]{}=5600K, log $g$=3.00 and $\xi$=1.3 km/s). This implies too low a luminosity for this star to be an AGB star. We also checked for the presence of Tc lines at 4049Å and 