Linking interstellar and cometary O2: A deep search for 16O18O in the solar-Type protostar IRAS 16293b-2422
Artikel i vetenskaplig tidskrift, 2018

Recent measurements carried out at comet 67P/Churyumov-Gerasimenko (67P) with the Rosetta probe revealed that molecular oxygen, O2, is the fourth most abundant molecule in comets. Models show that O2 is likely of primordial nature, coming from the interstellar cloud from which our solar system was formed. However, gaseous O2 is an elusive molecule in the interstellar medium with only one detection towards quiescent molecular clouds, in the ρ Oph A core. We perform a deep search for molecular oxygen, through the 21-01 rotational transition at 234 GHz of its 16O18O isotopologue, towards the warm compact gas surrounding the nearby Class 0 protostar IRAS 16293-2422 B with the ALMA interferometer. We also look for the chemical daughters of O2, HO2, and H2O2. Unfortunately, the H2O2 rotational transition is dominated by ethylene oxide c-C2H4O while HO2 is not detected. The targeted 16O18O transition is surrounded by two brighter transitions at ± 1 km s-1 relative to the expected 16O18O transition frequency. After subtraction of these two transitions, residual emission at a 3σ level remains, but with a velocity offset of 0.3-0.5 km s-1 relative to the source velocity, rendering the detection "tentative". We derive the O2 column density for two excitation temperatures Tex of 125 and 300 K, as indicated by other molecules, in order to compare the O2 abundance between IRAS 16293 and comet 67P. Assuming that 16O18O is not detected and using methanol CH3OH as a reference species, we obtain a [O2]/[CH3OH] abundance ratio lower than 2-5, depending on the assumed Tex, a three to four times lower abundance than the [O2]/[CH3OH] ratio of 5-15 found in comet 67P. Such a low O2 abundance could be explained by the lower temperature of the dense cloud precursor of IRAS 16293 with respect to the one at the origin of our solar system that prevented efficient formation of O2 in interstellar ices.

Stars: formation

ISM: Abundances

ISM: molecules

Molecular processes

Astrochemistry

ISM: individual objects: IRAS 16293-2422

Författare

V. Taquet

Universiteit Leiden

Osservatorio Astrofisico di Arcetri

E. F. van Dishoeck

Universiteit Leiden

Max Planck-institutet

M. Swayne

Universiteit Leiden

D. Harsono

Universiteit Leiden

Jes K. Jørgensen

Köbenhavns Universitet

Luke T. Maud

Universiteit Leiden

N. F W Ligterink

Universiteit Leiden

H. S.P. Müller

Universität zu Köln

C. Codella

Osservatorio Astrofisico di Arcetri

Kathrin Altwegg

Universität Bern

A. Bieler

University of Michigan

A. Coutens

Laboratoire d'Astrophysique de Bordeaux

M. N. Drozdovskaya

Universität Bern

Kenji Furuya

University of Tsukuba

Magnus V. Persson

Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik, Galaktisk astrofysik

Merel L.R. Van'T Hoff

Universiteit Leiden

C. Walsh

University of Leeds

S. F. Wampfler

Universität Bern

Astronomy and Astrophysics

0004-6361 (ISSN) 1432-0746 (eISSN)

Vol. 618 A11

Ämneskategorier

Astronomi, astrofysik och kosmologi

Atom- och molekylfysik och optik

Teoretisk kemi

DOI

10.1051/0004-6361/201833175

Mer information

Senast uppdaterat

2018-11-05