Abstract-Detection of interstellar ortho-D2H+ with SOFIA

Jorma Harju (1,2), Olli Sipilä (1), Sandra Brünken (3), Stephan Schlemmer (3), Paola Caselli (1), Mika Juvela (2), Karl M. Menten (4), Jürgen Stutzki (3), Oskar Asvany (3), Tomasz Kaminski (5), Yoko Okada (3), Ronan Higgins (3) ((1) Max-Planck-Institut für extraterrestrische Physik, Garching, Germany, (2) Department of Physics, University of Helsinki, Finland, (3) I. Physikalisches Institut, Universität zu Köln, Germany, (4) Max-Planck-Institut für Radioastronomie, Bonn, Germany, (5) Harvard-Smithsonian Center for Astrophysics, Cambridge MA, USA)

(Submitted on 8 Apr 2017)

https://arxiv.org/abs/1704.02526

We report on the detection of the ground-state rotational line of ortho-D2H+ at 1.477 THz (203 micron) using the German REceiver for Astronomy at Terahertz frequencies (GREAT) onboard 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 ~500 000 yr for the core, with an uncertainty of ~200 000 yr. The core material has probably been pre-processed for another 500 000 years in conditions corresponding to those in the ambient molecular cloud. The inferred time scale is more than ten times the age of the embedded protobinary. The D2H+ and H2D+ ions have large and nearly equal total (ortho+para) fractional abundances of ~10−9 in the outer envelope. This confirms the central role of H3+ in the deuterium chemistry in cool, dense gas, and adds support to the prediction of chemistry models that also D3+ should be abundant in these conditions.