order to better probe the disk/halo interface of the Milky Way. SEGUE is also obtaining $R$ $\simeq$ 2000 spectroscopy over the wavelength range 3800 $-$ 9200[Å]{} for some 250,000 stars in 200 selected areas over the sky available from Apache Point, New Mexico.

The SEGUE Stellar Parameter Pipeline (hereafter, SSPP) processes the wavelength- and flux-calibrated spectra generated by the standard SDSS spectroscopic reduction pipeline (Stoughton et al. 2002), obtains equivalent widths and/or line indices for 77 atomic or molecular absorption lines, and estimates $T_{\rm
eff}$, log $g$, and \[Fe/H\] through the application of a number of approaches. The current techniques employed by the SSPP include a minimum distance method (Allende Prieto et al. 2006), neural network analysis (Bailer-Jones 2000; Willemsen et al. 2005; Re Fiorentin et al. 2007), auto-correlation analysis (Beers et al. 1999), and a variety of line index calculations based on previous calibrations with respect to known standard stars (Beers et al. 1999; Cenarro et al. 2001a,b; Morrison et al. 2003). The SSPP employs five different methods for estimation of $T_{\rm eff}$, eight for estimation of log $g$, and nine for estimation of \[Fe/H\]. Details of the methods used are discussed in detail by Lee et al. (2007a, 