  (Abridged) The abundance discrepancy problem in planetary nebulae (PNe) has
long puzzled astronomers. NGC6153, with its high Abundance Discrepancy Factor
(ADF~10), provides an opportunity to understand the chemical structure and
ionisation processes by constructing detailed emission line maps and examining
variations in electron temperature and density. We used the MUSE spectrograph
to acquire IFU data covering the wavelength range 4600-9300 \AA\ with a spatial
sampling of 0.2 arcsec and spectral resolutions ranging from R = 1600-3500. We
created emission line maps for 60 lines and two continuum regions. We developed
a tailored methodology for the analysis of the data, including correction for
recombination contributions to auroral lines and the contributions of different
plasma phases. Our analysis confirmed the presence of a low-temperature plasma
component in NGC6153. We find that electron temperatures derived from
recombination line and continuum diagnostics are significantly lower than those
derived from collisionally excited line diagnostics. Ionic chemical abundance
maps were constructed, considering the weight of the cold plasma phase in the
HI emission. Adopting this approach, we found ionic abundances that could be up
to 0.2 dex lower for those derived from CELs and up to 1.1 dex higher for those
derived from RLs than in the case of an homogeneous HI emission. The abundance
contrast factor (ACF) between both plasma components was defined, with values,
on average, 0.9 dex higher than the ADF. Different methods for calculating
ionisation correction factors (ICFs) yielded consistent results. Our findings
emphasise that accurate chemical abundance determinations in high-ADF PNe must
account for multiple plasma phases.
