  We present new $\lambda_{\rm rest}=77$ $\mu$m dust continuum observations
from the ALMA of HZ10 (CRISTAL-22), a dusty main-sequence galaxy at $z$=5.66 as
part of the [CII] Resolved Ism in STar-forming Alma Large program, CRISTAL. The
high angular resolution of the ALMA Band 7 and new Band 9 data($\sim{0}''.4$)
reveals the complex structure of HZ10, which comprises two main components
(HZ10-C and HZ10-W) and a bridge-like dusty emission between them (the Bridge).
We model the dust spectral energy distribution (SED) to constrain the physical
conditions of the interstellar medium (ISM) and its variations among the
different components identified in HZ10. We find that HZ10-W (the more
UV-obscured component) has an SED dust temperature of $T_{\rm
SED}$$\sim$51.2$\pm13.1$ K; this is $\sim$5 K higher (although still
consistent) than that of the central component and previous global estimations
for HZ10. Our new ALMA data allow us to reduce by a factor of $\sim$2.3 the
uncertainties of global $T_{\rm SED}$ measurements compared to previous
studies. Interestingly, HZ10-W shows a lower [CII]/FIR ratio compared to the
other two components (although still within the uncertainties), suggesting a
harder radiation field destroying polycyclic aromatic hydrocarbon associated
with [CII] emission (e.g., active galactic nuclei or young stellar
populations). While HZ10-C appears to follow the tight IRX-$\beta_{\rm UV}$
relation seen in local UV-selected starburst galaxies and high-$z$ star-forming
galaxies, we find that both HZ10-W and the Bridge depart from this relation and
are well described by dust-screen models with holes in front of a hard UV
radiation field. This suggests that the UV emission (likely from young stellar
populations) is strongly attenuated in the more dusty components of the HZ10
system.
