Deuterated methanol on Solar System scale around the HH212 protostar
E. Bianchi, C. Codella, C. Ceccarelli, V. Taquet, S. Cabrit, F., Bacciotti, R. Bachiller, E. Chapillon, F. Gueth, A. Gusdorf, B. Lefloch, S., Leurini, L. Podio, K. L. J. Rygl, B. Tabone, M. Tafalla

TL;DR
This study used ALMA to map deuterated methanol around the HH212 protostar, revealing a lower D/H ratio than in other regions, and providing insights into methanol formation during star formation.
Contribution
First high-resolution ALMA observations of deuterated methanol in the HH212 protostar, measuring D/H ratio and analyzing its origin in the planet formation region.
Findings
Detected multiple lines of deuterated methanol and $^{13}$CH$_3$OH.
Derived a D/H ratio of approximately 2.4%, lower than in Perseus.
Mapped emission suggests a rotating structure possibly related to the accretion disk.
Abstract
Context: Methanol is thought to be mainly formed during the prestellar phase and its deuterated form keeps memory of the conditions at that epoch. Thanks to the unique combination of high angular resolution and sensitivity provided by ALMA, we wish to measure methanol deuteration in the planet formation region around a Class 0 protostar and to understand its origin. Aims: We mapped both the CHOH and CHDOH distribution in the inner regions (100 au) of the HH212 system in Orion B. To this end, we used ALMA Cycle 1 and Cycle 4 observations in Band 7 with angular resolution down to 0.15. Results: We detected 6 lines of CHOH and 13 lines of CHDOH with upper level energies up to 438 K in temperature units. We derived a rotational temperature of (171 52) K and column densities of 710 cm (CHOH) and…
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