Methanol deuteration in high-mass protostars

Astronomy and Astrophysics, vol. 667, pp. A136

Abstract

Context. The deuteration of molecules forming in the ices such as methanol (CH3OH) is sensitive to the physical conditions during their formation in dense cold clouds and can be probed through observations of deuterated methanol in hot cores. Aims. The aim is to determine the D/H ratio of methanol for a large sample of 99 high-mass protostars and to link this to the physical conditions during the formation of methanol in the prestellar phases. Methods. Observations with the Atacama Large Millimeter/submillimeter Array (ALMA) containing transitions of CH3OH, CH2DOH, CHD2OH, 13CH3OH, and CH318OH are investigated. The column densities of CH2DOH, CHD2OH, and CH3OH are determined for all sources, where the column density of CH3OH is derived from optically thin 13C and 18O isotopologues. Consequently, the D/H ratio of methanol is derived taking statistical effects into account. Results. Singly deuterated methanol (CH2DOH) is detected at the 3σ level toward 25 of the 99 sources in our sample of the high-mass protostars. Including upper limits, the (D/H)CH3OH ratio inferred from NCH2DOH/NCH3OH was derived for 38 of the 99 sources and varies between ~10−3-10−2. Including other high-mass hot cores from the literature, the mean methanol D/H ratio is 1.1 ± 0.7 × 10−3. This is more than one order of magnitude lower than what is seen for low-mass protostellar systems (2.2 ± 1.2 × 10−2). Doubly deuterated methanol (CHD2OH) is detected at the 3σ level toward 11 of the 99 sources. Including upper limits for 15 sources, the (D/H)CH2DOH ratios derived from NCHD2OH/NCH2DOH are more than two orders of magnitude higher than (D/H)CH3OH with an average of 2.0 ± 0.8 × 10−1 which is similar to what is found for low-mass sources. Comparison with literature GRAINOBLE models suggests that the high-mass prestellar phases are either warm (>20 K) or live shorter than the free-fall timescale. In contrast, for low-mass protostars, both a low temperature of <15 K and a prestellar phase timescale longer than the free-fall timescale are necessary. Conclusions. The (D/H)CH3OH ratio drops by more than an order of magnitude between low-mass and high-mass protostars due to either a higher temperature during the prestellar phases or shorter prestellar phases. However, successive deuteration toward CHD2OH seems equally effective between low-mass and high-mass systems.

Authors 9

1. M. L. van Gelder Aachen Leiden Observatory

   Leiden University · Leiden Observatory

   Affiliation as printed

   Leiden Observatory, Leiden University, PO Box 9513, 2300RA Leiden, The Netherlands

2. J. Jaspers Aachen Leiden Observatory

   Leiden University · Leiden Observatory

   Affiliation as printed

   Leiden Observatory, Leiden University, PO Box 9513, 2300RA Leiden, The Netherlands

3. Pooneh Nazari Aachen Leiden Observatory

   Leiden University · Leiden Observatory

   Affiliation as printed

   Leiden Observatory, Leiden University, PO Box 9513, 2300RA Leiden, The Netherlands

4. Aida Ahmadi Aachen Leiden Observatory

   Leiden University · Leiden Observatory

   Affiliation as printed

   Leiden Observatory, Leiden University, PO Box 9513, 2300RA Leiden, The Netherlands

5. Ewine F. van Dishoeck Aachen Leiden Observatory

   Leiden University · Max Planck Institute for Extraterrestrial Physics · Leiden Observatory

   Affiliation as printed

   Leiden Observatory, Leiden University, PO Box 9513, 2300RA Leiden, The Netherlands

   Max Planck Institut für Extraterrestrische Physik (MPE), Giessenbachstrasse 1, 85748 Garching, Germany

6. M. T. Beltrán

   Arcetri Astrophysical Observatory · National Institute for Astrophysics

   Affiliation as printed

   INAF-Osservatorio Astrofísico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy

7. G. A. Fuller

   University of Cologne · University of Manchester

   Affiliation as printed

   I. Physikalisches Institut, Universität zu Köln, Zülpicher Str.77, 50937 Köln, Germany

   Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK

8. Á. Sánchez-Monge

   University of Cologne

   Affiliation as printed

   I. Physikalisches Institut, Universität zu Köln, Zülpicher Str.77, 50937 Köln, Germany

9. P. Schilke

   University of Cologne

   Affiliation as printed

   I. Physikalisches Institut, Universität zu Köln, Zülpicher Str.77, 50937 Köln, Germany