  This work focuses on the gas chemical composition of CGCG007-025. This
compact dwarf is undergoing a galaxy wide star forming burst, whose spatial
behaviour has been observed by VLT/MUSE. We present a new line measurement
library to treat almost 7800 voxels. The direct method chemical analysis is
limited to 484 voxels with good detection of the
$[SIII]$6312$\mathring{\mathrm{A}}$ temperature diagnostic line. The
recombination fluxes are corrected for stellar absorption via a population
synthesis. Additionally, we discuss a new algorithm to fit photoionization
models via neural networks. The 8 ionic abundances analyzed show a spatial
normal distribution with a $\sigma\sim0.1\,dex$, where only half this value can
be explained by the uncertainty in the measurements. The oxygen abundance
distribution is $12+log(O/H)=7.88\pm0.11$. The $T_{e}[SIII]$ and $ne[SII]$ are
also normally distributed. However, in the central and brightest region, the
$ne[SII]$ is almost thrice the mean galaxy value. This is also reflected in the
extinction measurements. The ionization parameter has a distribution of $log(U)
= -2.52^{0.17}_{0.19}$. The parameter spatial behaviour agrees with the
$S^{2+}/S^{+}$ map. Finally, the discrepancies between the direct method and
the photoionization model fitting are discussed. In the latter technique, we
find that mixing lines with uneven uncertainty magnitudes can impact the
accuracy of the results. In these fittings, we recommend overestimating the
minimum flux uncertainty one order below the maximum line flux uncertainty.
This provides a better match with the direct method.
