The chemical nature of Orion protostars: Are ORANGES different from
  PEACHES? ORANGES II
  Understanding the chemical past of our Sun and how life appeared on Earth is
no mean feat. The best strategy we can adopt is to study newborn stars located
in an environment similar to the one in which our Sun was born and assess their
chemical content. In particular, hot corinos are prime targets since recent
studies showed correlations between interstellar Complex Organic Molecules
(iCOMs) abundances from hot corinos and comets. The ORion ALMA New GEneration
Survey (ORANGES) aims to assess the number of hot corinos in the closest and
best analogue to our Sun's birth environment, the OMC-2/3 filament. In this
context, we investigated the chemical nature of 19 solar-mass protostars and
found that 26\% of our sample sources shows warm methanol emission indicative
of hot corinos. Compared to the Perseus low-mass star-forming region, where the
PErseus ALMA CHEmistry Survey (PEACHES) detected $\sim 60$\% of hot corinos,
the latter seem to be relatively scarce in the OMC-2/3 filament. While this
suggests that the chemical nature of protostars in Orion and Perseus is
different, improved statistics are needed in order to consolidate this result.
If the two regions are truly different, this would indicate that the
environment is likely playing a role in shaping the chemical composition of
protostars.
