A High Spectral Resolution Atlas of Comet 122P/de Vico

Cochran, A. L.; Cochran, William D.

doi:10.1006/icar.2002.6850

Cited by 92 publications

(80 citation statements)

References 26 publications

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“…To better appreciate which lines are the most useful, the brightest domains of the spectra of the three species (Cochran & Cochran 2002) shows several of these isotopic lines among the unidentified features.…”

Section: Observationsmentioning

confidence: 99%

The CN isotopic ratios in comets

Manfroid

Jehin

Hutsemékers

et al. 2009

A&A

110

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Our aim is to determine the isotopic ratios 12 C/ 13 C and 14 N/ 15 N in a variety of comets and link these measurements to the formation and evolution of the solar system. The 12 C/ 13 C and 14 N/ 15 N isotopic ratios are measured for the CN radical by means of high-resolution optical spectra of the R branch of the B-X (0, 0) violet band. 23 comets from different dynamical classes have been observed, sometimes at various heliocentric and nucleocentric distances, in order to estimate possible variations of the isotopic ratios in parent molecules. The 12 C/ 13 C and 14 N/ 15 N isotopic ratios in CN are remarkably constant (average values of, respectively, 91.0 ± 3.6 and 147.8 ± 5.7) within our measurement errors, for all comets whatever their origin or heliocentric distance. While the carbon isotopic ratio does agree with the terrestrial value (89), the nitrogen ratio is a factor of two lower than the terrestrial value (272), indicating a fractionation in the early solar system, or in the protosolar nebula, common to all the comets of our sample. This points towards a common origin of the comets independently of their birthplaces, and a relationship between HCN and CN.

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Section: Observationsmentioning

confidence: 99%

The CN isotopic ratios in comets

Manfroid

Jehin

Hutsemékers

et al. 2009

A&A

110

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“…In the visible, many features are noted (e.g., Brown et al 1996;Cochran & Cochran 2002), presumably due to radicals. Others were recently revealed in the infrared with the Keck/NIRSPEC instrument (Mumma et al 2001a,b), that could be due to parent molecules.…”

Section: Future Prospectsmentioning

confidence: 99%

The composition of ices in comet C/1995 O1 (Hale-Bopp) from radio spectroscopy

Crovisier

Bockelée‐Morvan²,

Colom³

et al. 2004

A&A

211

159

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Abstract. From radio spectroscopic observations of comets, more than 22 molecules, radicals and ions, plus several isotopologues, were detected, the majority of them being recently revealed in comets C/1996 B2 (Hyakutake) and C/1995 O1 (Hale-Bopp). Among them, 6 molecules were detected for the first time (Bockelée-Morvan et al. 2000) in the course of a spectral survey conducted at radio wavelengths in comet Hale-Bopp with the CSO, the IRAM 30-m telescope and Plateau de Bure interferometer. In addition, many species were searched for unsuccessfully, some of them with stringent upper limits. We present here a review of these observations and further analysis of their results. This include: (i) confirmed detection of acetaldehyde (CH 3 CHO); (ii) limits on small molecules such as ketene (H 2 CCO) or methanimine (CH 2 NH); (iii) limits on the abundance ratios in homologous series such as HC 5 N/HC 3 N, ethanol/methanol, acetic acid/formic acid; (iv) searches for precursors of key cometary species such as atomic Na and HNC; (v) constraints on more exotic species ranging from water dimer (H 2 O) 2 to glycine; (vi) detection of the H 34 2 S isotopic species and independent observations of HDO and DCN; (vii) limits on several other deuterated species; (viii) limits on several radicals and ions and a tentative detection of the C 2 H radical; (ix) the presence of unidentified lines. Typical abundance upper limits of 2-5 ×10 −4 relative to water are achieved for many species. Better upper limits are obtained for some linear molecules with high dipole moments. But more complex molecules such as dimethyl ether or glycine are poorly constrained. These results should give important clues to the chemical composition of cometary ices, to the formation mechanisms of cometary material, and to the chemical processes which occur in the inner coma.

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“…The quality of data is very good and thousands of lines are visible. We are presently listing and identifying all these lines by comparison with existing catalogs (Cochran & Cochran 2002;Brown et al 1996;Zhang et al 2001). The cometary atomic oxygen green line and the red doublet are clearly visible in the orders 24 of the blue part and 2 and 3 of the red part, respectively (see Figs.…”

Section: Introductionmentioning

confidence: 99%

O($^{\mathsf 1}$S) and O($^{\mathsf 1}$D) emission lines in the spectrum of 153P/2002 C1 (Ikeya-Zhang)

Capria¹,

Cremonese

Bhardwaj

et al. 2005

A&A

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High resolution spectroscopy observation of comet 153P/2002 C1 Ikeya-Zhang was performed on April 20, 2002 with the echelle spectrograph SARG on the 3.5 m Telescopio Nazionale Galileo in La Palma. The atomic O emission lines at 5577, 6360 and 6363 Å are clearly visible in the spectrum. We determined the intensity ratio of the green line to the sum of the red lines. In order to verify the hypothesis that water is the main parent species of these emissions, the result was compared with the value obtained from a coupled chemistry-transport model. The measured value for the green to red ratio, 0.12 ± 0.1, agrees quite well with the value obtained from the model. This led us to conclude that during the observation water was the parent species of atomic O lines.

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A High Spectral Resolution Atlas of Comet 122P/de Vico

Cited by 92 publications

References 26 publications

The CN isotopic ratios in comets

The CN isotopic ratios in comets

The composition of ices in comet C/1995 O1 (Hale-Bopp) from radio spectroscopy

O($^{\mathsf 1}$S) and O($^{\mathsf 1}$D) emission lines in the spectrum of 153P/2002 C1 (Ikeya-Zhang)

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