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The spectral energy distribution (SED) in the millimetre (mm) to centimetre(cm) range is a useful tool for characterising the dust in protostellarenvelopes as well as free-free emission from the protostar and outflow. Whilemany studies have been carried out towards low- and high-mass protostars,little exists so far about solar-type protostars in high-mass star-formingregions, which are likely to be representatives of the conditions where theSolar System was born. We focus here on the OMC-2/3 solar-type protostars,which are bounded by nearby HII regions and which are, therefore, potentiallyaffected by the high-UV illumination. We aim to understand whether thesmall-scale structure ($\leq$1000 au) and the evolutionary status of thesesolar-type protostars are affected by the nearby HII regions, as is the casefor the large-scale ($\leq$10$^4$ au) gas chemical composition. We used ALMA inthe 1.3 mm band (246.2 GHz) to image the continuum of 16 OMC-2/3 solar-typeprotostars, with an angular resolution of 0.25$''$ (100 au). We completed ourdata with archival data from the VANDAM survey of Orion Protostars at 333 and32.9 GHz, respectively, to construct the dust SED, extract several dustparameters and to assess whether free-free emission is contaminating their dustSED in the cm range. From the mm to cm range dust SED, we found low dustemissivity spectral indexes ($\beta < 1$) for the majority of our source sampleand free-free emission towards only 5 of the 16 sample sources. We were alsoable to confirm or correct the evolutionary status of the source sample.Finally, we did not find any dependence of the source dust parameters on theirlocation in the OMC-2/3 filament. Our results show that the small-scale dustproperties of the OMC-2/3 protostars are not affected by the high- UVillumination from the nearby HII regions.

ORion Alma New GEneration Survey (ORANGES) I. Dust continuum and free-free emission of OMC-2/3 filament protostars