profile fit to the narrow emission lines. The rms noise in the continuum was taken to be the average of the rms on each side of an emission line. For weak lines, whose uncertainty is dominated by error from the continuum subtraction, the rms term determines the approximate uncertainty. For the lines with flux measurements much stronger than the rms noise of the continuum, (usually the H$\alpha$ lines and often the \[\] $\lambda\lambda$4959,5007 doublet) the error is dominated by flux calibration and de-reddening uncertainties. In this case, a minimum uncertainty of 2% was assumed, and the right hand term above dominates the uncertainty estimate. 31 of the 44 galaxies in our sample were measured to have \[\] $\lambda$4363 line strengths $> 4\sigma$. The measured \[\] $\lambda4959$/$\lambda5007$ ratios match theoretical expectations within the errors, supporting our error estimates and the assumption that the continuum subtraction dominates the uncertainties for the weak lines. For all the objects in the present sample, flux line strengths and corresponding errors are listed in Table \[tbl3\]. We concentrate the rest of our analysis on the objects for which direct electron temperature and chemical abundance determinations can be made. An analysis of the remaining spectra using strong-line 