  (abridged) We study and compare the warm (>100 K) and cold (<100 K) material
toward the high-mass star-forming region IRAS 23385+6053 (IRAS 23385 hereafter)
combining high angular resolution observations in the mid-infrared (MIR) with
the JWST Observations of Young protoStars (JOYS) project and with the NOEMA at
mm wavelengths at angular resolutions of 0.2"-1".
  The spatial morphology of atomic and molecular species is investigated by
line integrated intensity maps. The temperature and column density of different
gas components is estimated using H2 transitions (warm and hot component) and a
series of CH3CN transitions as well as 3 mm continuum emission (cold
component).
  Toward the central dense core in IRAS 23385 the material consists of
relatively cold gas and dust (~50 K), while multiple outflows create heated
and/or shocked H2 and show enhanced temperatures (~400 K) along the outflow
structures. An energetic outflow with enhanced emission knots of [Fe II] and
[Ni II] hints at J-type shocks, while two other outflows have enhanced emission
of only H2 and [S I] caused by C-type shocks. The latter two outflows are also
more prominent in molecular line emission at mm wavelengths (e.g., SiO, SO,
H2CO, and CH3OH). Even higher angular resolution data are needed to
unambiguously identify the outflow driving sources given the clustered nature
of IRAS 23385. While most of the forbidden fine structure transitions are
blueshifted, [Ne II] and [Ne III] peak at the source velocity toward the MIR
source A/mmA2 suggesting that the emission is originating from closer to the
protostar.
