THE COLOGNE DATABASE FOR MOLECULAR SPECTROSCOPY, CDMS

By H. S. P. Müller, F. Schlöder, S. Thorwirth, G. Winnewisser. 2001

957 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/369e98d934881e9cfd464a73e56011cb807ab104

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Citations in the corpus

Exploring Molecular Complexity with ALMA (EMoCA): Deuterated complex organic molecules in Sagittarius B2(N2) (2015, methodology): “Predictions for the three singly-deuterated species of ethyl cyanide were taken from the catalog of the Cologne Database for Molecular Spectroscopy (CDMS4, Müller et al. 2001, 2005) (tags 56509, 56510, and 56511, all version 1).”
Erratum: Detection of amino acetonitrile in Sgr B2(N) (2008, methodology): “In the course of the present investigation an amino acetonitrile entry (tag: 56507) has been prepared for the catalog of the Cologne Database for Molecular Spectroscopy (CDMS, see Müller et al. 2001, 2005).”
The composition of ices in comet C/1995 O1 (Hale-Bopp) from radio spectroscopy (2004, methodology): “As in our previous studies (Crovisier et al. 1993; Lis et al. 1997) we made an extensive use of the PAPSYNTHE software and of JPL and Cologne molecular databases (Pickett et al. 1998; Müller et al. 2001).”
On the internal structure of starless cores II. A molecular survey of L1498 and L1517B (2006, methodology): “For our calculations, we have used the H2CO parameters from the on-line Cologne Database for Molecular Spectroscopy (CDMS, Müller et al. 2001), together with the 10 K H2CO-He collision rates of Green (1991).”
A COLD COMPLEX CHEMISTRY TOWARD THE LOW-MASS PROTOSTAR B1-b: EVIDENCE FOR COMPLEX MOLECULE PRODUCTION IN ICES (2010, methodology): “The targeted lines are listed in Table 3 and the frequencies are taken from the JPL molecular database and the Cologne Database for Molecular Spectroscopy (Müller et al. 2001).”
The Galactic Center: The Largest Oxygen-bearing Organic Molecule Repository (2007, methodology): “They were obtained from the Cologne Database for Molecular Spectroscopy (Müller et al. 2001, 2005), the Jet Propulsion Laboratory catalog (Pickett et al. 1998), and Hollis et al. (2004b).”
A computer program for fast non-LTE analysis of interstellar line spectra With diagnostic plots to interpret observed line intensity ratios (2007, methodology): “Frequencies from this database are generally of line catalogs such as CDMS (Müller et al. 2001)12 should be consulted.”
Complex organic molecules in the interstellar medium: IRAM 30 m line survey of Sagittarius B2(N) and (M) (2013, background): “…are taken from our line catalog which contains all entri s from the catalog of the Cologne Database for Molecular Spectroscopy (CDMS4, see Müller et al. 2001, 2005) and most entries from the molecular spectroscopic database of the Jet Propulsi n Laboratory (JPL5, see Pickett et al.…”
Molecules with ALMA at Planet-forming Scales (MAPS). I. Program Overview and Highlights (2021, neutral): “…F=3–2 265.886434 −3.1292 7.0 25.5 CDMS Y Y Y Y Y J=3–2, F=3–3 265.884891 −4.0322 7.0 25.5 CDMS Y Y Y Y Y J=3–2, F=2–2 265.888522 −3.8861 5.0 25.5 CDMS Y Y Y Y Y 1 Spectroscopic data are compiled from the CDMS (Müller et al. 2001, 2005; Endres et al. 2016); JPL (Pickett et al. 1998); and LAMBDA…”
Increased complexity in interstellar chemistry: detection and chemical modeling of ethyl formate and n-propyl cyanide in Sagittarius B2(N) (2009, methodology): “The predictions used for the current analysis will be made available in the CDMS (Müller et al. 2001, 2005, see footnote 4).”
Discovery of Interstellar Propylene (CH2CHCH3): Missing Links in Interstellar Gas-Phase Chemistry (2007, background): “These lines appear neither in the JPL nor in the CDMS catalogs (Pickett et al. 1998; Müller et al. 2001, 2005).”
ALMA OBSERVATIONS OF CIRCUMSTELLAR DISKS IN THE UPPER SCORPIUS OB ASSOCIATION (2016, background): “Aul is the Einstein A coefficient and Eu is the energy of the upper level of the transition (Aul = 2.497× 10−6 s−1 and Euk = 33.19 K for 12CO J = 3−2, Müller et al. 2001, 2005).”