FTFIR-spectrum of the ground state of D2CO

Lohilahti, Jarmo; Horneman, V.‐M.

doi:10.1016/j.jms.2004.06.010

Cited by 13 publications

(15 citation statements)

References 11 publications

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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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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

View full text Add to dashboard Cite

show abstract

“…Therefore, the values of the sextic and octic centrifugal distortion coefficients of all three states under consideration, (v 3 = 1), (v 4 = 1), and (v 6 = 1), were constrained to their ground state values from [26]. For the convenience of the reader, .0 a n tr is the number of assigned transitions.…”

Section: Analysis and Resultsmentioning

confidence: 99%

“…The ground state energies were calculated with the parameters from [26]. As a result of the analysis, we were able to assign 10 150 transitions in the recorded spectrum.…”

Section: Description Of the Spectrum And Assignment Of Transitionsmentioning

confidence: 99%

See 1 more Smart Citation

The fundamental bands ν3, ν4, and ν6 of

Lohilahti

Ulenikov

Bekhtereva

et al. 2005

Journal of Molecular Spectroscopy

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“…The Hamiltonian was fit to the data of the v 2 = 1 and v 4 = 2 states using the least-squares procedure. The ground-state constants of D 2 13 CO were taken from [27]. The resulting values of the v 2 = 1 and v 4 = 2 states of the D 2 13 CO molecule are presented in Table 2 together with the ground-state constants and v 2 = 1 state constants of D 2 CO for comparison.…”

Section: Discussionmentioning

confidence: 99%