the lines from our sources of [$gf$-values]{}. We then predicted their EWs using MOOG. For lines with EWs $> 5$mÅ (slightly more for the lower S/N regions), we synthesized the region. Our starting point was the Kurucz & Bell (1995) (KUR95) line lists, which contained many rare earth lines that are the true contaminants in this situation, but were unimportant in the Sun and not included in Moore [et al.]{}. For lines we wanted to use for abundance analysis, we checked for blends from other lines and only used a line if it were essentially unblended or if the other line contributing to the blend had a recent, laboratory-based [$gf$-value]{}. We also synthesized the regions in three metal-poor stars: HD 122563 (neutron-capture and C-poor) (e.g., Westin [et al.]{} 2000), CS 22183-015 (neutron-capture and C-rich) (Johnson & Bolte 2002), and CS 22957-027 (neutron-capture-poor and C-rich) (e.g., Norris, Ryan, & Beers 1997) to check that our linelists adequately accounted for contamination from atomic and molecular lines. Our EWs and atomic parameters are in Table 1. We compared our EWs to those of A02 for the 22 lines we had in common. We found an average offset of $-0.8$mÅ with an r.m.s. scatter 