Sub-Doppler and Doppler spectroscopy of DCN isotopomers in the terahertz region: ground and first excited bending states (v1v2v3)=(0 1,0)

Brünken, Sandra; Fuchs, U.; Lewen, Frank; Urban, Štěpán; Giesen, Thomas; Winnewisser, G.

doi:10.1016/j.jms.2004.02.021

Cited by 23 publications

(14 citation statements)

References 44 publications

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“…The H 13 CN entries are mostly based on Fuchs et al (2004) and for 2 = 1 and 2 = 0, respectively. The entries for the ground vibrational states of HC 15 N, H 13 C 15 N, and DCN were based largely on , Fuchs et al (2004), and Brünken et al (2004), respectively. Sgr B2(N): the parameters of all entries related to hydrogen cyanide are listed in Table 40.…”

Section: Hydrogen Cyanide Hcnmentioning

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

390

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: Hydrogen Cyanide Hcnmentioning

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

390

523

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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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“…Recently, Lattanzi et al (2007) have addressed this issue for the formyl ion, HCO , probably the most abundant molecular ϩ ion in dense sources (see Herbst 2005 Brünken et al 2004). This was a clue to some inaccuracy in the data or in their treatment, and led us to reinvestigate the rotational spectrum of the formyl ion in its ground state up to nearly 900 GHz, in order to compare to the data of Lattanzi et al (2007) and to derive accurate spectroscopic constants.…”

mentioning

confidence: 99%

Improved Rest Frequencies of HCO ⁺ at 1 THz

Tinti

Bizzocchi

Esposti

et al. 2007

ApJ

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The ground-state rotational spectrum of HCO , produced in a negative-glow discharge cell, has been recorded ϩ up to 892 GHz. The sources of systematic error have been carefully accounted for, thus obtaining accurate rotational and centrifugal distortion constants. The present measurements have allowed us to determine a value of the sextic distortion constant, , which, unlike the recent determination of Lattanzi et al., is consistent with H J the values determined for DCO and for the isoelectronic molecule HCN. The new set of spectroscopic constants ϩ allows us to predict the rotational spectrum of the formyl ion with an accuracy of 1 part in 10 8 near 1 THz. Such an accuracy is important for kinematic studies of dense cores in molecular clouds and for future far-infrared observations.

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Sub-Doppler and Doppler spectroscopy of DCN isotopomers in the terahertz region: ground and first excited bending states (v1v2v3)=(0 1,0)

Cited by 23 publications

References 44 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)

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

Improved Rest Frequencies of HCO ⁺ at 1 THz

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Sub-Doppler and Doppler spectroscopy of DCN isotopomers in the terahertz region: ground and first excited bending states (v1v2v3)=(0 1,0)

Cited by 23 publications

References 44 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)

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

Improved Rest Frequencies of HCO + at 1 THz

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Product

Resources

About

Improved Rest Frequencies of HCO ⁺ at 1 THz