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The formation pathways of different types of organic molecules inprotostellar envelopes and other regions of star formation are subjects ofintense current interest. We here present observations of C$_4$H and CH$_3$OH,tracing two distinct groups of interstellar organic molecules, toward 16protostars in the Ophiuchus and Corona Australis molecular clouds. Togetherwith observations in the literature, we present C$_4$H and CH$_3$OH data fromsingle-dish observations of 40 embedded protostars. We find no correlationbetween the C$_4$H and CH$_3$OH column densities in this large sample. Based onthis lack of correlation, a difference in line profiles between C$_4$H andCH$_3$OH, and previous interferometric observations of similar sources, wepropose that the emission from these two molecules is spatially separated, withthe CH$_3$OH tracing gas that has been transiently heated to high ($\sim$70-100K) temperatures, and the C$_4$H tracing the cooler large-scale envelope whereCH$_4$ molecules have been liberated from ices. These results provide insightin the differentiation between hot corino and warm carbon-chain chemistry inembedded protostars.

On the origin of C$_4$H and CH$_3$OH in protostellar envelopes