ORion Alma New GEneration Survey (ORANGES)

Context. The spectral energy distribution (SED) in the millimetre to centimetre range is an extremely useful tool for characterising dust protostellar envelopes as well free-free emission from protostar and outflow. Actually, evolutionary status of solar-type protostars often based on their SED near-infrared range. In addition, presence or absence can be considered indicator source stage (Class 0/I versus Class II/III). While many studies have been carried out towards low- high-mass protostars, little exists so far about star-forming regions, which are likely representatives conditions where Solar System was born. Aims. this work, we focus embedded Orion Molecular Cloud (OMC) 2 3 filaments, bounded by nearby HII regions are, therefore, potentially affected high-UV illumination OB stars. We use various parameters understand whether small-scale structure (≤1000 au) these case large-scale (≤10 4 gas chemical composition. Methods. used Atacama Large (sub-)Millimeter Array (ALMA) 1.3 mm band (246.2 GHz) image continuum 16 young 0/I) OMC-2/3 with angular resolution 0.25″ (100 au). completed our data archival ALMA VLA VANDAM survey Protostars at 333 32.9 GHz, respectively, construct extract temperature, emissivity index, envelope plus disk mass sources assess contaminating Results. From SED, found low indexes ( β < 1) majority sample only 5 sources. were also able confirm correct reported literature. Finally, did not find any dependence location filament. Conclusions. Our results show that properties formation takes place simultaneously throughout