most of the data reduction, extraction of the Magellan data must account for the “tilted” slits, i.e., the lines are tilted with respect to the orders and the tilt varies across the CCD. While this is a feature of all cross-dispersed echelle spectrographs, for MIKE data the tilt is severe. We used the [mtools]{}[^3] set of tasks written by Jack Baldwin to correct for the tilt. Failure to make this correction would result in degradation of the spectral resolution as shown in Figure \[fig:tilt\]. (The magnitude of this effect depends upon the aperture size applied to the order being extracted. For the stellar spectra, the decrease in spectral resolution would be smaller than for the Th-Ar comparison spectra by roughly a factor of 2.)

Analysis {#sec:analysis}
========

Stellar parameters and the iron abundance {#sec:param}
-----------------------------------------

The first step in the analysis was to determine the stellar parameters: the effective temperature ([$T_{\rm eff}$]{}), the surface gravity (log $g$), and the microturbulent velocity ($\xi_t$). Equivalent widths (EWs) were measured for a set of Fe[i]{} and Fe[ii]{} lines using routines in IRAF. We used the same set of Fe lines presented in Y03. In Figure \[fig:ew\_compm\], we compare the measured EWs for Fe[i]{} 