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The Curious Chemistry of Hot Core G35.20-0.74N
Wednesday, June 22, 2016 - 3:30pm PDT
University of Groningen
N232, Room 227
Hot molecular cores are an early stage of high mass star formation where high abundances of complex organic molecules can be observed in compact (<0.05 pc), hot (>100 K), dense (>107 cm-3) sources. These objects are empirically defined, so it is unclear whether the molecular emission arises from a disk, the inner envelope, or outflow cavity walls. We have analyzed ALMA Cycle 0 observations of G35.20-0.74N, a high mass star forming region containing two hot cores, one of which shows strong evidence of a Keplerian disk (Sanchez-Monge et al 2013). In my talk I'll describe how, after further analysis, this disk candidate shows chemical segregation on the smallest scale yet observed with most Nitrogen bearing species found only to the south-eastern side of the disk. This region also shows a greatly increased deuteration fraction and a higher kinetic temperature (375 K vs 125 K) than that of the north-western side. I'll also explore the possible reasons for such chemical variation in this intriguing region.