| Abstract
| - We investigate the chemical segregation of complex O-bearing species (including the largest and most complex ones detected to date in space) towards Orion KL, the closest high-mass star-forming region. The molecular line images obtained using the ALMA science verification data reveal a clear segregation of chemically related species depending on their different functional groups. We map the emission of 13CH 3OH, HCOOCH 3, CH 3OCH 3, CH 2OCH 2, CH 3COOCH 3, HCOOCH 2CH 3, CH 3CH 2OCH 3, HCOOH, OHCH 2CH 2OH, CH 3COOH, CH 3CH 2OH, CH 3OCH 2OH, OHCH 2CHO, and CH 3COCH 3 with ∼1.5″ angular resolution and provide molecular abundances of these species toward different gas components of this region. We disentangle the emission of these species in the different Orion components by carefully selecting lines free of blending and opacity effects. Possible effects in the molecular spatial distribution due to residual blendings and different excitation conditions are also addressed. We find that while species containing the C−O−C group, i.e. an ether group, exhibit their peak emission and higher abundance towards the compact ridge, the hot core south is the component where species containing a hydroxyl group (−OH) bound to a carbon atom (C−O−H) present their emission peak and higher abundance. This finding allows us to propose methoxy (CH 3O−) and hydroxymethyl (−CH 2OH) radicals as the major drivers of the chemistry in the compact ridge and the hot core south, respectively, as well as different evolutionary stages and prevailing physical processes in the different Orion components.
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