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Context: Solar-like protostars are known to be chemically rich, but it is notyet clear how much their chemical composition can vary and why. So far, twochemically distinct types of Solar-like protostars have been identified: hotcorinos, which are enriched in interstellar Complex Organic Molecules (iCOMs),such as methanol (CH$_3$OH) or dimethyl ether (CH$_3$OCH$_3$), and Warm CarbonChain Chemistry (WCCC) objects, which are enriched in carbon chain molecules,such as butadiynyl (C$_4$H) or ethynyl radical (CCH). However, none of thesehave been studied so far in environments similar to that in which our Sun wasborn, that is, one that is close to massive stars. Aims: In this work, wesearch for hot corinos and WCCC objects in the closest analogue to the Sun'sbirth environment, the Orion Molecular Cloud 2/3 (OMC-2/3) filament located inthe Orion A molecular cloud. Methods: We obtained single-dish observations ofCCH and CH$_3$OH line emission towards nine Solar-like protostars in thisregion. As in other, similar studies of late, we used the [CCH]/[CH$_3$OH]abundance ratio in order to determine the chemical nature of our protostarsample. Results: Unexpectedly, we found that the observed methanol and ethynylradical emission (over a few thousands au scale) does not seem to originatefrom the protostars but rather from the parental cloud and itsphoto-dissociation region, illuminated by the OB stars of the region.Conclusions: Our results strongly suggest that caution should be taken beforeusing [CCH]/[CH$_3$OH] from single-dish observations as an indicator of theprotostellar chemical nature and that there is a need for other tracers or highangular resolution observations for probing the inner protostellar layers.

Hunting for hot corinos and WCCC sources in the OMC-2/3 filament