  We place empirical constraints on the yields from zero- and low-metallicity
core collapse supernovae (CCSNe) using abundances measured in very metal-poor
(VMP; [Fe/H] $\leq$ $-2$) Damped Lyman Alpha Absorbers (DLAs). For some
abundance ratios ([N,Al,S/Fe]), VMP DLAs constrain the metal yields of the
first SNe more reliably than VMP stars. We compile a large sample of high-S/N
VMP DLAs from over 30 years of literature, most with high resolution spectral
measurements. We infer the IMF-averaged CCSNe yield from the median values from
the DLA abundance ratios of C, N, O, Al, Si, S, and Fe (over Fe and O). We
assume that the DLAs are metal-poor enough that they represent galaxies in
their earliest stages of evolution, when CCSNe are the only nucleosynthetic
sources of the metals we analyze. We compare five sets of zero- and
low-metallicity theoretical yields to the empirical yields derived in this
work. We find that the five models agree with the DLA yields for ratios
containing Si and S. Only one model, Heger & Woosley (2010, hereafter HW10),
reproduced the DLA values for N, and one other model, Limongi & Chieffi (2018,
hereafter LC18), reproduced [N/O]. We found little change in the theoretical
yields with the adoption of a SN explosion landscape (where certain progenitor
masses collapse into black holes, contributing no yields) onto HW10, but fixing
explosion energy to progenitor mass results in wide disagreements between the
predictions and DLA abundances. We investigate the adoption of a simple,
observationally motivated Initial Distribution of Rotational Velocities for
LC18 and find a slight improvement.
