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LIBRIS Formathandbok  (Information om MARC21)
FältnamnIndikatorerMetadata
00005585naa a2200637 4500
001oai:research.chalmers.se:4c3f2e95-c2c2-4af9-88e3-70ac70e8f8df
003SwePub
008181031s2018 | |||||||||||000 ||eng|
0247 a https://research.chalmers.se/publication/5057672 URI
0247 a https://research.chalmers.se/publication/5064372 URI
0247 a https://doi.org/10.1051/0004-6361/2018331752 DOI
040 a (SwePub)cth
041 a engb eng
042 9 SwePub
072 7a art2 swepub-publicationtype
072 7a ref2 swepub-contenttype
1001 a Taquet, V.u Universiteit Leiden (UL),Leiden University (UL),Osservatorio Astrofisico di Arcetri,Arcetri Astrophysical Observatory4 aut
2451 0a Linking interstellar and cometary O2: A deep search for 16O18O in the solar-Type protostar IRAS 16293b-2422
264 c 2018-10-03
264 1b EDP Sciences,c 2018
520 a 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.
650 7a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
650 7a NATURVETENSKAPx Fysikx Atom- och molekylfysik och optik0 (SwePub)103022 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Atom and Molecular Physics and Optics0 (SwePub)103022 hsv//eng
650 7a NATURVETENSKAPx Kemix Teoretisk kemi0 (SwePub)104072 hsv//swe
650 7a NATURAL SCIENCESx Chemical Sciencesx Theoretical Chemistry0 (SwePub)104072 hsv//eng
653 a ISM: individual objects: IRAS 16293-2422
653 a ISM: Abundances
653 a Molecular processes
653 a ISM: molecules
653 a Stars: formation
653 a Astrochemistry
7001 a van Dishoeck, E. F.u Universiteit Leiden (UL),Leiden University (UL),Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)4 aut
7001 a Swayne, M.u Universiteit Leiden (UL),Leiden University (UL)4 aut
7001 a Harsono, D.u Universiteit Leiden (UL),Leiden University (UL)4 aut
7001 a Jørgensen, Jes K.u Köpenhamns universitet,University of Copenhagen4 aut
7001 a Maud, Luke T.u Universiteit Leiden (UL),Leiden University (UL)4 aut
7001 a Ligterink, N. F Wu Universiteit Leiden (UL),Leiden University (UL)4 aut
7001 a Müller, H. S.P.u Universität zu Köln,University of Cologne4 aut
7001 a Codella, C.u Osservatorio Astrofisico di Arcetri,Arcetri Astrophysical Observatory4 aut
7001 a Altwegg, Kathrinu Universität Bern,University of Bern4 aut
7001 a Bieler, A.u University of Michigan4 aut
7001 a Coutens, A.u Laboratoire d'Astrophysique de Bordeaux4 aut
7001 a Drozdovskaya, M. N.u Universität Bern,University of Bern4 aut
7001 a Furuya, Kenjiu University of Tsukuba4 aut
7001 a Persson, Magnus V.,d 1983u Chalmers tekniska högskola,Chalmers University of Technology4 aut0 (Swepub:cth)magnpe
7001 a Van'T Hoff, Merel L.R.u Universiteit Leiden (UL),Leiden University (UL)4 aut
7001 a Walsh, C.u University of Leeds4 aut
7001 a Wampfler, S. F.u Universität Bern,University of Bern4 aut
7102 a Universiteit Leiden (UL)b Osservatorio Astrofisico di Arcetri4 org
7730 t Astronomy and Astrophysicsd : EDP Sciencesg 618q 618x 0004-6361x 1432-0746
8564 u https://www.aanda.org/articles/aa/pdf/2018/10/aa33175-18.pdf
8564 8u https://research.chalmers.se/publication/505767
8564 8u https://research.chalmers.se/publication/506437
8564 8u https://doi.org/10.1051/0004-6361/201833175

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