The Ground State Rotational Spectra of HDCO and D2CO

Bocquet, Rachel; Demaison, J.; Cosléou, J.; Friedrich, Alexander; Margulès, L.; Macholl, Sven; Mäder, H.; Beaky, M. M.; Winnewisser, G.

doi:10.1006/jmsp.1999.7836

Cited by 36 publications

(42 citation statements)

References 39 publications

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“…(11); the Hamiltonian matrix involved both A-and BCoriolis-type operators in the v-off diagonal blocks, and classical A-reduction Watson operators written in I r representation for the v-diagonal blocks. On the other hand, the ground state energy levels were computed using the parameters which were obtained in a recent microwave study (24).…”

Section: Discussionmentioning

confidence: 99%

“…Then the ground state energy levels were calculated (24) and added to the newly observed line positions to get a list of experimental upper state energy levels. These upper state levels were then introduced together with the available microwave data (12,13) in a least-squares fit to get an improved set of parameters for the upper interacting states {5 1 , 6 1 }.…”

Section: Discussionmentioning

confidence: 99%

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Evidence of Vibrational-Induced Rotational Axis Switching for HD12C16O: New High-Resolution Analysis of the ν5 and ν6 Bands and First Analysis of the ν4 Band (10-μm Region)

Perrin

Flaud

Smirnov

et al. 2000

Journal of Molecular Spectroscopy

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Evidence of Vibrational-Induced Rotational Axis Switching for HD12C16O: New High-Resolution Analysis of the ν5 and ν6 Bands and First Analysis of the ν4 Band (10-μm Region)

Perrin

Flaud

Smirnov

et al. 2000

Journal of Molecular Spectroscopy

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“…(3) For each species, the spectroscopic references given here are the most recent cited in the CDMS and JPL databases. All of them should be read as reference and references therein: (aa) Winnewisser et al (1997); (ab) Cazzoli et al (2004); (ac) Klapper et al (2001); (ad) Klapper et al (2003); (ae) Bogey et al (1997); (a f ) Klaus et al (1996); (ag) Müller et al (2000d); (ah) Bocquet et al (1999); (ai) Müller et al (2000c); (a j) Lohilahti & Horneman (2004); (ak) Müller et al (2000b); (al) Müller et al (2000a); (am) Belov et al (1998); (an) Müller et al (2004); ( Kim & Yamamoto (2003); (aw) Thorwirth et al (2003); (ax) ; (ay) Brünken et al (2004); (az) ; (ba) Kleiner et al (1996); (bb) Müller et al (2009);(bc) Clouthier et al (1994); (bd) Brown et al (1987); (be) Minowa et al (1997); (b f ) Golubiatnikov et al (2005); (bg) Lovas & Suenram (1987); (bh) Maeda et al (2008); (bi) Cho & Saito (1998); (b j) Thorwirth et al (2000a); (bk) Brünken et al (2006); (bl) Thorwirth et al (2000b); (bm) Spahn et al (2008); (bn) Belov (1995); (bo) Camy-Peyret et al (1985); (bp) …”

Section: Line Parametersmentioning

confidence: 99%

TIMASSS: the IRAS 16293-2422 millimeter and submillimeter spectral survey

Caux

Kahane

Castets

et al. 2011

A&A

164

220

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Context. Unbiased spectral surveys are powerful tools to study the chemistry and the physics of star forming regions, because they can provide a complete census of the molecular content and the observed lines probe the physical structure of the source. Aims. While unbiased surveys at the millimeter and sub-millimeter wavelengths observable from ground-based telescopes have previously been performed towards several high mass protostars, very little exists on low mass protostars, which are believed to resemble our own Sun's progenitor. To help fill up this gap in our understanding, we carried out a complete spectral survey of the bands at 3, 2, 1, and 0.9 mm towards the solar type protostar IRAS 16293-2422. Methods. The observations covered a range of about 200 GHz and were obtained with the IRAM-30 m and JCMT-15 m telescopes during about 300 h of observations. Particular attention was devoted to the inter-calibration of the acquired spectra with previous observations. All the lines detected with more than 3σ confidence-interval certainty and free from obvious blending effects were fitted with Gaussians to estimate their basic kinematic properties. Results. More than 4000 lines were detected (with σ ≥ 3) and identified, yielding a line density of approximatively 20 lines per GHz, comparable to previous surveys in massive hot cores. The vast majority (about two-thirds) of the lines are weak and produced by complex organic molecules. The analysis of the profiles of more than 1000 lines belonging to 70 species firmly establishes the presence of two distinct velocity components associated with the two objects, A and B, forming the IRAS 16293-2422 binary system. In the source A, the line widths of several species increase with the upper level energy of the transition, a behavior compatible with gas infalling towards a ∼1 M object. The source B, which does not show this effect, might have a much lower central mass of ∼0.1 M . The difference in the rest velocities of both objects is consistent with the hypothesis that the source B rotates around the source A. Conclusions. This spectral survey, although obtained with single-dish telescopes at a low spatial resolution, allows us to separate the emission from two different components, thanks to the large number of lines detected. The data of the survey are public and can be retrieved on the TIMASSS web site .

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“…(6) for a review). As a consequence, because of its astrophysical importance, the ground state rotational spectrum of HDCO was investigated in detail (6,7, and references therein). On the other hand, the existing microwave data involving the excited vibrational states of HDCO were rather limited since only some transitions in the 5 1 and 6 1 excited states were identified in the regions 9-980 MHz and 10-270 GHz by double resonance radiofrequency measurements inside a CO 2 laser cavity (8) and by microwave technique (9) respectively.…”

Section: Introductionmentioning

confidence: 99%

“…From this analysis, the experimental {5 1 , 6 1 , 4 1 } infrared energy levels were derived by adding the observed ν 5 , ν 6 , and ν 4 line positions to the ground state energy levels calculated using the parameters quoted in Ref. (7). These infrared energy levels, together with the existing ν 5 and ν 6 microwave measurements, were least squares fitted to get the upper state parameters.…”

Section: Introductionmentioning

confidence: 99%