The Cologne Database for Molecular Spectroscopy, CDMS: a useful tool for astronomers and spectroscopists

Müller, H. S. P.; Schlöder, F.; Stützki, J.; Winnewisser, G.

doi:10.1016/j.molstruc.2005.01.027

Cited by 1,934 publications

(1,754 citation statements)

References 47 publications

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“…We note a 0.1 km s −1 discrepancy between the velocities of the 13 CN and C 15 N lines towards L1498, which could not be ascribed to any obvious technical issue. We note, however, that the uncertainty on the rest frequency reported in the Cologne Database for Molecular Spectroscopy (Müller et al 2005) is 0.1 MHz, or 0.25 km s −1 , which could account for the observed shift. New observation of the 13 CN(1-0) towards L1498 should be performed to check this discrepancy.…”

Section: Resultsmentioning

confidence: 66%

The CN/C¹⁵N isotopic ratio towards dark clouds

Hily-Blant

Forêts

Fauré

et al. 2013

A&A

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Understanding the origin of the composition of solar system cosmomaterials is a central question, not only in the cosmochemistry and astrochemistry fields, and requires various approaches to be combined. Measurements of isotopic ratios in cometary materials provide strong constraints on the content of the protosolar nebula. Their relation with the composition of the parental dark clouds is, however, still very elusive. In this paper, we bring new constraints based on the isotopic composition of nitrogen in dark clouds, with the aim of understanding the chemical processes that are responsible for the observed isotopic ratios. We have observed and detected the fundamental rotational transition of C 15 N towards two starless dark clouds, L1544 and L1498. We were able to derive the column density ratio of C 15 N over 13 CN towards the same clouds, and obtain the CN/C 15 N isotopic ratios, which were found to be 500 ± 75 for both L1544 and L1498. These values are therefore marginally consistent with the protosolar value of 441. Moreover, this ratio is larger than the isotopic ratio of nitrogen measured in HCN. In addition, we present model calculations of the chemical fractionation of nitrogen in dark clouds, which make it possible to understand how CN can be deprived of 15 N and HCN can simultaneously be enriched in heavy nitrogen. The non-fractionation of N 2 H + , however, remains an open issue and we propose some chemical way of alleviating the discrepancy between model predictions and the observed ratios.

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Section: Resultsmentioning

confidence: 66%

The CN/C¹⁵N isotopic ratio towards dark clouds

Hily-Blant

Forêts

Fauré

et al. 2013

A&A

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“…1). They are easily identified and disentangled from absorption intrinsic to the source, since they occur at the same frequency in both SW and NE spectra, see Spectroscopic data of ArH + transitions were taken from the CDMS (Müller et al 2001(Müller et al , 2005 and are summarized in Table 1. An isotopic invariant fit of diverse rotational and rovibrational data was carried out, similar to Odashima et al (1999), to determine spectroscopic parameters of the molecule and to derive rest frequencies of rotational transitions of argonium isotopologs.…”

Section: Observations and Spectroscopic Datamentioning

confidence: 99%

Detection of extragalactic argonium, ArH⁺, toward PKS 1830−211

Müller

Schilke

et al. 2015

A&A

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Context. Argonium has recently been detected as a ubiquitous molecule in our Galaxy. Model calculations indicate that its abundance peaks at molecular fractions in the range of 10 −4 to 10 −3 and that the observed column densities require high values of the cosmic ray ionization rate. Therefore, this molecular cation may serve as an excellent tracer of the very diffuse interstellar medium (ISM), as well as an indicator of the cosmic ray ionization rate. Aims. We attempted to detect ArH + in extragalactic sources to evaluate its diagnostic power as a tracer of the almost purely atomic ISM in distant galaxies. Methods. We obtained ALMA observations of a foreground galaxy at z = 0.89 in the direction of the lensed blazar PKS 1830−211. Results. Two isotopologs of argonium, 36 ArH + and 38 ArH + , were detected in absorption along two different lines of sight toward PKS 1830−211, known as the SW and NE images of the background blazar. The argonium absorption is clearly enhanced on the more diffuse line of sight (NE) compared to other molecular species. The isotopic ratio 36 Ar/ 38 Ar is 3.46 ± 0.16 toward the SW image, i.e., significantly lower than the solar value of 5.5.Conclusions. Our results demonstrate the suitability of argonium as a tracer of the almost purely atomic, diffuse ISM in high-redshift sources. The evolution of the isotopic ratio with redshift may help to constrain nucleosynthetic scenarios in the early Universe.

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“…Techniques range from classical absorption set-ups to the use of cavity ringdown spectroscopy to increase the sensitivity by orders of magnitude 24 . Transition frequencies and strengths of (sub)mm transitions are summarized in the Jet Propulsion Laboratory catalog (JPL) 25 and the Cologne Database for Molecular Spectroscopy (CDMS) 26,27 ¶ . Databases for vibrational transitions at infrared wavelengths include the HI-TRAN database 28 and the EXOMOL line lists .…”

Section: Laboratory Experimentsmentioning

confidence: 99%

Astrochemistry of dust, ice and gas: introduction and overview

Dishoeck

Ewine²

2014

Faraday Discuss.

138

102

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A brief introduction and overview of the astrochemistry of dust, ice and gas and their interplay is presented, aimed at non-specialists. The importance of basic chemical physics studies of critical reactions is illustrated through a number of recent examples. Such studies have also triggered new insight into chemistry, illustrating how astronomy and chemistry can enhance each other. Much of the chemistry in star- and planet-forming regions is now thought to be driven by gas-grain chemistry rather than pure gas-phase chemistry, and a critical discussion of the state of such models is given. Recent developments in studies of diffuse clouds and PDRs, cold dense clouds, hot cores, protoplanetary disks and exoplanetary atmospheres are summarized, both for simple and more complex molecules, with links to papers presented in this volume. In spite of many lingering uncertainties, the future of astrochemistry is bright: new observational facilities promise major advances in our understanding of the journey of gas, ice and dust from clouds to planets.Comment: Introductory paper for Faraday Discussions 168 conference, April 201

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The Cologne Database for Molecular Spectroscopy, CDMS: a useful tool for astronomers and spectroscopists

Cited by 1,934 publications

References 47 publications

The CN/C¹⁵N isotopic ratio towards dark clouds

The CN/C¹⁵N isotopic ratio towards dark clouds

Detection of extragalactic argonium, ArH⁺, toward PKS 1830−211

Astrochemistry of dust, ice and gas: introduction and overview

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The Cologne Database for Molecular Spectroscopy, CDMS: a useful tool for astronomers and spectroscopists

Cited by 1,934 publications

References 47 publications

The CN/C15N isotopic ratio towards dark clouds

The CN/C15N isotopic ratio towards dark clouds

Detection of extragalactic argonium, ArH+, toward PKS 1830−211

Astrochemistry of dust, ice and gas: introduction and overview

Contact Info

Product

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The CN/C¹⁵N isotopic ratio towards dark clouds

The CN/C¹⁵N isotopic ratio towards dark clouds

Detection of extragalactic argonium, ArH⁺, toward PKS 1830−211