Millimeter-wave spectra of HCCCN

Mbosei, L; Fayt, André; Dréan, Pascal; Cosléou, J.

doi:10.1016/s0022-2860(99)00258-6

Cited by 27 publications

(30 citation statements)

References 11 publications

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“…The resonant interactions between 7 = 4 and 5 = 7 = 1 have been approached by the measurements of Yamada & Creswell (1986) and Mbosei et al (2000), but not reached. Therefore, predicted transition frequencies involving these resonances may differ from the actual frequencies by amounts exceeding three times the predicted uncertainties.…”

Section: Cyanoacetylene Hc 3 Nmentioning

confidence: 96%

“…The 13 C entries, including the doubly substituted ones, are based on Thorwirth et al (2001), and those of HC 3 15 N on Fayt et al (2004). Additional measurements in the range of our survey were taken from Creswell et al (1977) for the ground vibrational states of the main as well as singly substituted 13 C and 15 N entries, from Yamada et al (1995) for = 0 of the main species, Yamada & Creswell (1986) and Mbosei et al (2000) for several excited states of the main isotopologue, and Thorwirth et al (2001) for the HC 3 15 N entries.…”

Section: Cyanoacetylene Hc 3 Nmentioning

confidence: 99%

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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

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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...

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Section: Cyanoacetylene Hc 3 Nmentioning

confidence: 96%

Section: Cyanoacetylene Hc 3 Nmentioning

confidence: 99%

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

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“…From line profiles at mm frequencies, we see that the line intensity increases with the rotational quantum number J, whereas in the HIFI lines the opposite occurs (see Table A.1 where spectroscopic parameters for HC 3 N and its vibrational modes 2 are shown). The intensity 2 Spectroscopic parameters for HC 3 N (dipole moment µ = 3.73 D) were obtained from DeLeon et al (1985), de Zafra (1971, Mbosei (2000), Creswell et al (1977), Chen et al (1991), Yamada (2005), and Thorwirth et al (2000). For 13 C isotopologues the parameters were obtained from Creswell et al (1977), Mallinson & de Zafra (1978), and Thorwirth et al (2001).…”

Section: Line Profilesmentioning

confidence: 99%

“…For 13 C isotopologues the parameters were obtained from Creswell et al (1977), Mallinson & de Zafra (1978), and Thorwirth et al (2001). For the vibratonal mode ν 7 and its 13 C isotopologues, the parameters were obtained from Thorwirth et al (2000) and Thorwirth et al (2001), while the spectroscopic parameters for the rest of the vibrational modes were obtained from Yamada & Creswell (1986), Thorwirth et al (2000), and Mbosei (2000). of each line depends (among other paremeters) on the energy of the level and mainly on the frequency, but the covered frequency range for a given transition range is broader for HIFI than in IRAM-30-m.…”

Section: Line Profilesmentioning

confidence: 99%

Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC₃N

Esplugues

Cernicharo

Viti

et al. 2013

A&A

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Context. We present a study of cyanoacetylene (HC 3 N) and cyanodiacetylene (HC 5 N) in Orion KL using observations from two line surveys performed with the IRAM 30-m telescope and the HIFI instrument onboard the Herschel telescope. The frequency ranges covered are 80−280 GHz and 480−1906 GHz. Aims. This study (divided by families of molecules) is part of a global analysis of the physical conditions of Orion KL and the molecular abundances in the different components of this cloud. Methods. We modeled the observed lines of HC 3 N, HC 5 N, their isotopologues (including DC 3 N), and vibrational modes using a non-local thermodynamic equilibrium (non-LTE) radiative transfer code. In addition, to investigate the chemical origin of HC 3 N and DC 3 N in Orion KL, we used a time-dependent chemical model. Results. We detect 40 lines of the ground vibrational state of HC 3 N and 68 lines of its 13 C isotopologues. We also detect 297 lines of six vibrational modes of this molecule (ν 7 , 2ν 7 , 3ν 7 , ν 6 , ν 5 , and ν 6 +ν 7 ) and 35 rotational lines of the ground vibrational state of HC 5 N. We report the first tentative detection of DC 3 N in a giant molecular cloud. We have obtained a DC 3 N/HC 3 N abundance ratio of 0.015 ± 0.009, similar to typical D/H ratios of cold dark clouds. We provide column densities for all species and derived isotopic and molecular abundances. We also made a 2 × 2 map around Orion IRc2 and present maps of the HC 3 N lines with energies from 34 to 154 K and of the HC 3 N vibrational modes ν 6 and ν 7 with energies between 354 and 872 K. In addition, a comparison of our results for HC 3 N with those in other clouds has allowed us to derive correlations between the column density, the FWHM, the mass, and the luminosity of the clouds. Conclusions. The high column densities of HC 3 N obtained in the hot core, in particular of the ground vibrational state and the vibrational mode ν 7 , make this molecule an excellent tracer of hot and dense gas. In addition, the wide frequency range covered reveals the need to consider a temperature and density gradient in the hot core to obtain better line fits. The high D/H ratio (similar to that obtained in cold clouds) that we derive suggests a deuterium enrichment. Our chemical models indicate that the possible deuterated HC 3 N in Orion KL is formed during the gas-phase. This fact provides new hints concerning the processes leading to deuteration.

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“…Adopting the most recent molecular constants of HC 3 N and CH 3 CN published by Mbosei et al (2000) and Pearson & Muller (1996), respectively, as well as the standard formalism for rotational transitions in the ground vibrational state (see for instance Brown et al (1988), for CH 3 CN), we computed the rotational frequencies of both compounds. We discovered that our computed frequencies were affected by smaller errors and differred slightly from those of the line catalogs.…”

Section: Absolute Frequency Evaluationmentioning

confidence: 99%

Interferometric measurements of zonal winds on Titan

Moreno

Marten

Hidayat³

2005

A&A

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Abstract.We report millimetre observations of Titan performed with the IRAM Plateau de Bure Interferometer at the rotational frequencies of HC 3 N(25-24) and CH 3 CN(12-11). The most extended configuration of the array yielded disk-resolved emission spectra of Titan with an angular resolution of 0.6 . Data were acquired in February-March 2003 and February 2004 near the greatest eastern and western elongations of Titan at high spectral resolution (λ/∆λ = 5.5 × 10 6 ). Doppler lineshift measurements enable us to establish that the zonal wind flow is prograde in the upper atmosphere. Two different altitude regions are probed. Beam-integrated equatorial wind velocities of 160 (±60) m/s and 60 (±20) m/s are determined at respective altitudes of 300 (±150) km (upper stratosphere) and 450 (±100) km (lower mesosphere). The latter is the first direct determination of mesospheric wind speed on Titan.

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Millimeter-wave spectra of HCCCN

Cited by 27 publications

References 11 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)

Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC₃N

Interferometric measurements of zonal winds on Titan

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Millimeter-wave spectra of HCCCN

Cited by 27 publications

References 11 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)

Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC3N

Interferometric measurements of zonal winds on Titan

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Product

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Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC₃N