Harju, Jorma ORCID: 0000-0002-1189-9790, Sipiae, Olli, Brunken, Sandra ORCID: 0000-0001-7175-4828, Schlemmer, Stephan ORCID: 0000-0002-1421-7281, Caselli, Paola, Juvela, Mika ORCID: 0000-0002-5809-4834, Menten, Karl M., Stutzki, Juergen, Asvany, Oskar, Kaminski, Tomasz ORCID: 0000-0001-8541-8024, Okada, Yoko ORCID: 0000-0002-6838-6435 and Higgins, Ronan (2017). Detection of Interstellar Ortho-D2H+ with SOFIA. Astrophys. J., 840 (2). BRISTOL: IOP PUBLISHING LTD. ISSN 1538-4357

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Abstract

We report on the detection of the ground-state rotational line of ortho-D2H+ at 1.477 THz (203 mu m) using the German REceiver for Astronomy at Terahertz frequencies (GREAT) on. board the Stratospheric Observatory For Infrared Astronomy (SOFIA). The line is seen in absorption against. far-infrared continuum from the protostellar binary IRAS 16293-2422 in Ophiuchus. The para-D2H+ line at 691.7 GHz was not detected with the APEX telescope toward this position. These D2H+ observations complement our previous detections of para-H2D+ and ortho-H2D+ using SOFIA and APEX. By modeling chemistry and radiative transfer in the dense core surrounding the protostars, we find that the ortho-D2H+ and para-H2D+ absorption features mainly originate in the cool (T < 18 K) outer envelope of the core. In contrast, the ortho-H2D+ emission from the core is significantly absorbed by the ambient molecular cloud. Analyses of the combined D2H+ and H2D+ data result in an age estimate of similar to 5. x. 10(5) yr for the core, with an uncertainty of similar to 2. x. 10(5) yr. The core material has probably been pre-processed for another 5. x. 10(5) years in conditions corresponding to those in the ambient molecular cloud. The inferred timescale is more than 10 times the age of the embedded protobinary. The D2H+ and H2D+ ions have large and nearly equal total (ortho+ para) fractional abundances of similar to 10(-9) in the outer envelope. This confirms the central role of H-3 + in the deuterium chemistry in cool, dense gas, and adds support to the prediction of chemistry models that also D-3(+) should be abundant in these conditions.

Item Type: Journal Article
Creators:
CreatorsEmailORCIDORCID Put Code
Harju, JormaUNSPECIFIEDorcid.org/0000-0002-1189-9790UNSPECIFIED
Sipiae, OlliUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Brunken, SandraUNSPECIFIEDorcid.org/0000-0001-7175-4828UNSPECIFIED
Schlemmer, StephanUNSPECIFIEDorcid.org/0000-0002-1421-7281UNSPECIFIED
Caselli, PaolaUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Juvela, MikaUNSPECIFIEDorcid.org/0000-0002-5809-4834UNSPECIFIED
Menten, Karl M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Stutzki, JuergenUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Asvany, OskarUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Kaminski, TomaszUNSPECIFIEDorcid.org/0000-0001-8541-8024UNSPECIFIED
Okada, YokoUNSPECIFIEDorcid.org/0000-0002-6838-6435UNSPECIFIED
Higgins, RonanUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
URN: urn:nbn:de:hbz:38-231230
DOI: 10.3847/1538-4357/aa6c69
Journal or Publication Title: Astrophys. J.
Volume: 840
Number: 2
Date: 2017
Publisher: IOP PUBLISHING LTD
Place of Publication: BRISTOL
ISSN: 1538-4357
Language: English
Faculty: Unspecified
Divisions: Unspecified
Subjects: no entry
Uncontrolled Keywords:
KeywordsLanguage
LOW-MASS PROTOSTAR; GOULD BELT SURVEY; TO-PARA RATIO; PRESTELLAR CORES; IRAS 16293-2422; DEUTERIUM FRACTIONATION; RADIATIVE-TRANSFER; DEUTERATED H-3(+); MOLECULAR CLOUDS; STAR-FORMATIONMultiple languages
Astronomy & AstrophysicsMultiple languages
Refereed: Yes
URI: http://kups.ub.uni-koeln.de/id/eprint/23123

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