We have obtained new detailed abundances of the Fe-group elements Sc through Zn ( Z = 21 - 30 ) in three very metal-poor ( [ Fe/H ] \approx - 3 ) stars : BD + 03 ^ { o } 740 , BD - 13 ^ { o } 3442 , and CD - 33 ^ { o } 1173 .
High-resolution ultraviolet HST /STIS spectra in the wavelength range 2300 - 3050 Å were gathered , and complemented by an assortment of optical echelle spectra .
The analysis featured recent laboratory atomic data for number of neutral and ionized species for all Fe-group elements except Cu and Zn .
A detailed examination of scandium , titanium , and vanadium abundances in large-sample spectroscopic surveys indicates that they are positively correlated in stars with [ Fe/H ] < - 2 .
The abundances of these elements in BD + 03 ^ { o } 740 , BD - 13 ^ { o } 3442 , CD - 33 ^ { o } 1173 , and HD 84937 ( studied in a previous paper of this series ) are in accord with these trends and lie at the high end of the correlations .
Six elements have detectable neutral and ionized features , and generally their abundances are in reasonable agreement .
For Cr we find only minimal abundance disagreement between the neutral ( mean of [ Cr i /Fe ] = +0.01 ) and ionized species ( mean of [ Cr ii /Fe ] = +0.08 ) , unlike most studies in the past .
The prominent exception is Co , for which the neutral species indicates a significant overabundance ( mean of [ Co i /H ] = -2.53 ) , while no such enhancement is seen for the ionized species ( mean of [ Co ii /H ] = -2.93 ) .
These new stellar abundances , especially the correlations among Sc , Ti , and V , suggest that models of element production in early high-mass metal-poor stars should be revisited .