Microwave Detection of Interstellar Vinyl Alcohol, CH[TINF]2[/TINF][dbond]CHOH

Turner, B. E.; Apponi, A. J.

doi:10.1086/324762

Cited by 142 publications

(154 citation statements)

References 16 publications

Supporting

Mentioning

142

Contrasting

Unclassified

Order By: Relevance

“…With a beam filling factor of unity, a linewidth of 9 km s −1 , and a temperature of 11.6 K, we derive an upper limit of 2 × 10 14 cm −2 for the anti conformer, which is less constraining than the detection reported by Turner & Apponi (2001). Our upper limit is mainly set by the non-detection of the transition at 84.83 GHz.…”

Section: Vinyl Alcohol Ch 2 Chohmentioning

confidence: 71%

“…They are based on the measurements performed by Saito (1976) and Rodler (1983) for the former, and Rodler (1985) for the latter. Turner & Apponi (2001) report the detection of vinyl alcohol toward Sgr B2(N) with the Kitt Peak 12 m telescope at 3 and 2 mm. They claim the detection of five transitions of the anti conformer and two transitions of the syn conformer, with linewidths (FWHM) in the range 8-16 km s −1 .…”

Section: Vinyl Alcohol Ch 2 Chohmentioning

confidence: 98%

See 1 more Smart Citation

Complex organic molecules in the interstellar medium: IRAM 30 m line survey of Sagittarius B2(N) and (M)

Беллоче

Müller

Menten

et al. 2013

A&A

385

523

View full text Add to dashboard Cite

Context. The discovery of amino acids in meteorites fallen to Earth and the detection of glycine, the simplest of them, in samples returned from a comet to Earth strongly suggest that the chemistry of the interstellar medium is capable of producing such complex organic molecules and that they may be widespread in our Galaxy. Aims. Our goal is to investigate the degree of chemical complexity that can be reached in the interstellar medium, in particular in dense star-forming regions. Methods. We performed an unbiased, spectral line survey toward Sgr B2(N) and (M), two regions where high-mass stars are formed, with the IRAM 30 m telescope in the 3 mm atmospheric transmission window. Partial surveys at 2 and 1.3 mm were performed in parallel. The spectra were analyzed with a simple radiative transfer model that assumes local thermodynamic equilibrium but takes optical depth effects into account. Results. About 3675 and 945 spectral lines with a peak signal-to-noise ratio higher than 4 are detected at 3 mm toward Sgr B2(N) and (M), i.e. about 102 and 26 lines per GHz, respectively. This represents an increase by about a factor of two over previous surveys of Sgr B2. About 70% and 47% of the lines detected toward Sgr B2(N) and (M) are identified and assigned to 56 and 46 distinct molecules as well as to 66 and 54 less abundant isotopologues of these molecules, respectively. In addition, we report the detection of transitions from 59 and 24 catalog entries corresponding to vibrationally or torsionally excited states of some of these molecules, respectively, up to a vibration energy of 1400 cm −1 (2000 K). Excitation temperatures and column densities were derived for each species but should be used with caution. The rotation temperatures of the detected complex molecules typically range from ∼50 to 200 K. Among the detected molecules, aminoacetonitrile, n-propyl cyanide, and ethyl formate were reported for the first time in space based on this survey, as were five rare isotopologues of vinyl cyanide, cyanoacetylene, and hydrogen cyanide. We also report the detection of transitions from within twelve new vibrationally or torsionally excited states of known molecules. Absorption features produced by diffuse clouds along the line of sight are detected in transitions with low rotation quantum numbers of many simple molecules and are modeled with ∼30-40 velocity components with typical linewidths of ∼3-5 km s −1 . Conclusions. Although the large number of unidentified lines may still allow future identification of new molecules, we expect most of these lines to belong to vibrationally or torsionally excited states or to rare isotopologues of known molecules for which spectroscopic predictions are currently missing. Significant progress in extending the inventory of complex organic molecules in Sgr B2(N) and deriving tighter constraints on their location, origin, and abundance is expected in the near future thanks to an ongoing spectral line survey at 3 mm with ALMA in its cycles 0 and 1. The present single-dish surve...

show abstract

Section: Vinyl Alcohol Ch 2 Chohmentioning

confidence: 71%

Section: Vinyl Alcohol Ch 2 Chohmentioning

confidence: 98%

Complex organic molecules in the interstellar medium: IRAM 30 m line survey of Sagittarius B2(N) and (M)

Беллоче

Müller

Menten

et al. 2013

A&A

385

523

View full text Add to dashboard Cite

show abstract

“…Methylene amidogen has previously been found in the cold core TMC-1 (Ohishi et al 1994) and methyl formate and vinyl alcohol have previously been detected in hot cores (Fontani et al 2007;Turner & Apponi 2001). Using criterion (iii) from Section 4 we can rule out methylene amidogen as there are several expected transitions in the frequency range of our observations that are not seen.…”

Section: Moleculementioning

confidence: 72%

“…Using criterion (iii) from Section 4 we can rule out methylene amidogen as there are several expected transitions in the frequency range of our observations that are not seen. Vinyl alcohol can also be ruled out because the 112,10-110,11 transition has a low line intensity (Sµ 2 = 0.03), which leads to a column density of 2.7×10 20 cm −2 , six orders of magnitude higher than the vinyl alcohol column density in Sagittarius B2(N) (Turner & Apponi 2001) and much larger than those of more commonly-observed molecules. We therefore identify line A with the 188,10-178,9E transition of methyl formate, but the 242,23-241,24E, and 242,23-240,24E transitions also contribute to the line A emission.…”

Section: Moleculementioning

confidence: 99%

A high-resolution study of complex organic molecules in hot cores

Calcutt

Viti

Codella

et al. 2014

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present the results of a line identification analysis using data from the IRAM Plateau de Bure Inferferometer, focusing on six massive star-forming hot cores: G31.41+0.31, G29.96-0.02, G19.61-0.23, G10.62-0.38, G24.78+0.08A1 and G24.78+0.08A2. We identify several transitions of vibrationally excited methyl formate (HCOOCH 3 ) for the first time in these objects as well as transitions of other complex molecules, including ethyl cyanide (C 2 H 5 CN), and isocyanic acid (HNCO). We also postulate a detection of one transition of glycolaldehyde (CH 2 (OH)CHO) in two new hot cores. We find G29.96-0.02, G19.61-0.23, G24.78+0.08A1 and G24.78+0.08A2 to be chemically very similar. G31.41+0.31, however, is chemically different: it manifests a larger chemical inventory and has significantly larger column densities. We suggest that it may represent a different evolutionary stage to the other hot cores in the sample, or it may surround a star with a higher mass. We derive column densities for methyl formate in G31.41+0.31, using the rotation diagram method, of 4×10 17 cm −2 and a T rot of ∼170 K. For G29.96-0.02, G24.78+0.08A1 and G24.78+0.08A2, glycolaldehyde, methyl formate and methyl cyanide all seem to trace the same material and peak at roughly the same position towards the dust emission peak. For G31.41+0.31, however, glycolaldehyde shows a different distribution to methyl formate and methyl cyanide and seems to trace the densest, most compact inner part of hot cores.

show abstract

“…Two energetically less stable isomers of HNCO have recently been detected in the interstellar medium: cyanic acid (HOCN) tentatively towards Sgr B2 (OH) following its laboratory identification (Brünken et al 2009a), and fulminic acid (HCNO) towards three starless dark clouds and one lowmass star-forming region (Marcelino et al 2009) with abundance ratios relative to HNCO of 0.5% and 1−5%, respectively. The relative abundances of members of an isomeric family reflect their different formation and destruction processes, and observations of isomers of small systems like HCN/HNC (e.g., Schilke et al 1992) as well as complex organic species (Hollis et al 2000;Turner & Apponi 2001) have been previously Based on observations with the IRAM 30-m telescope. IRAM is supported by CNRS/INSU (France), the MPG (Germany) and the IGN (Spain).…”

Section: Introductionmentioning

confidence: 99%

Interstellar HOCN in the Galactic center region

Brünken¹,

Беллоче

Martín

et al. 2010

A&A

View full text Add to dashboard Cite

Aims. Our aim is to confirm the interstellar detection of cyanic acid, HOCN, in the Galactic center clouds. It has previously been tentatively detected only in Sgr B2(OH). Methods. We used a complete line survey of the hot cores Sgr B2(N) and (M) in the 3 mm range, complemented by additional observations carried out with the IRAM 30 m telescope at selected frequencies in the 2 mm band and towards four additional positions in the Sgr B2 cloud complex in the 2 and 3 mm bands. The spectral survey was analysed in the local thermodynamical equilibrium approximation (LTE) by modeling the emission of all identified molecules simultaneously. This allowed us to distinguish weak features of HOCN from the rich line spectrum observed in Sgr B2(N) and (M). Lines of the more stable (by 1.1 eV) isomer isocyanic acid, HNCO, in these sources, as well as those of HOCN and HNCO towards the other positions, were analysed in the LTE approximation as well. Results. Four transitions of HOCN were detected in a quiescent molecular cloud in the Galactic center at a position offset in (RA, Dec) by (20 , 100 ) from the hot core source Sgr B2(M), confirming its previous tentative interstellar detection. Up to four transitions were detected toward five other positions in the Sgr B2 complex, including the hot cores Sgr B2(M), (S), and (N). A fairly constant abundance ratio of ∼0.3−0.8% for HOCN relative to HNCO was derived for the extended gas components, suggesting a common formation process of these isomers.

show abstract

Microwave Detection of Interstellar Vinyl Alcohol, CH[TINF]2[/TINF][dbond]CHOH

Cited by 142 publications

References 16 publications

Complex organic molecules in the interstellar medium: IRAM 30 m line survey of Sagittarius B2(N) and (M)

Complex organic molecules in the interstellar medium: IRAM 30 m line survey of Sagittarius B2(N) and (M)

A high-resolution study of complex organic molecules in hot cores

Interstellar HOCN in the Galactic center region

Contact Info

Product

Resources

About