This article has an erratum: [erratum]
Volume 629, September 2019
|Number of page(s)||34|
|Section||Atomic, molecular, and nuclear data|
|Published online||06 September 2019|
Laboratory rotational spectroscopy of isotopic acetone, CH313C(O)CH3 and 13CH3C(O)CH3, and astronomical search in Sagittarius B2(N2)⋆
I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany
2 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
3 Departments of Chemistry and Astronomy, University of Virginia, Charlottesville, VA 22904, USA
Accepted: 13 June 2019
Context. Spectral lines of minor isotopic species of molecules that are abundant in space may also be detectable. Their respective isotopic ratios may provide clues about the formation of these molecules. Emission lines of acetone in the hot molecular core Sagittarius B2(N2) are strong enough to warrant a search for its singly substituted 13C isotopologs.
Aims. We want to study the rotational spectra of CH313C(O)CH3 and 13CH3C(O)CH3 and search for them in Sagittarius B2(N2).
Methods. We investigated the laboratory rotational spectrum of isotopically enriched CH313C(O)CH3 between 40 GHz and 910 GHz and of acetone between 36 GHz and 910 GHz in order to study 13CH3C(O)CH3 in natural isotopic composition. In addition, we searched for emission lines produced by these species in a molecular line survey of Sagittarius B2(N) carried out with the Atacama Large Millimeter/submillimeter Array (ALMA). Discrepancies between predictions of the main isotopic species and the ALMA spectrum prompted us to revisit the rotational spectrum of this isotopolog.
Results. We assigned 9711 new transitions of CH313C(O)CH3 and 63 new transitions of 13CH3C(O)CH3 in the laboratory spectra. More than 1000 additional transitions were assigned for the main isotopic species. We modeled the ground state data of all three isotopologs satisfactorily with the ERHAM program. We find that models of the torsionally excited states v12 = 1 and v17 = 1 of CH3C(O)CH3 improve only marginally. No transitrrrion of CH313C(O)CH3 is clearly detected toward the hot molecular core Sgr B2(N2). However, we report a tentative detection of 13CH3C(O)CH3 with a 12C/13C isotopic ratio of 27 that is consistent with the ratio previously measured for alcohols in this source. Several dozens of transitions of both torsional states of the main isotopolog are detected as well.
Conclusion. Our predictions of CH313C(O)CH3 and CH3C(O)CH3 are reliable into the terahertz region. The spectrum of 13CH3C(O)CH3 should be revisited in the laboratory with an enriched sample. The torsionally excited states v12 = 1 and v17 = 1 of CH3C(O)CH3 were not reproduced satisfactorily in our models. Nevertheless, transitions pertaining to both states could be identified unambiguously in Sagittarius B2(N2).
Key words: molecular data / methods: laboratory: molecular / techniques: spectroscopic / radio lines: ISM / ISM: molecules / ISM: individual objects: Sagittarius B2(N)
The experimental line lists are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/629/A72
© ESO 2019
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.