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

JOYS: Disentangling the warm and cold material in the high-mass IRAS 23385+6053 cluster