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11 results on '"Stephan Schlemmer"'

1. Pure Rotational Spectrum of CCl+

Author

Stephan Schlemmer, Kaori Kobayashi, Keigo Nagamori, J. Furuta, Sven Thorwirth, Charles R. Markus, Hiroshi Kohguchi, and Oskar Asvany

Subjects
Physics, Astrochemistry, Space and Planetary Science, TheoryofComputation_ANALYSISOFALGORITHMSANDPROBLEMCOMPLEXITY, Rotational spectrum, Astronomy and Astrophysics, Molecular spectroscopy, Atomic physics
Abstract

The pure rotational spectrum of the CCl+ (X 1Σ+) cation has been observed for the first time using a cryogenic ion trap apparatus and applying an action spectroscopy scheme. The major isotopic species 12C35Cl+ was observed up to the J = 4 ← 3 transition around 191 GHz and 12C37Cl+ was observed up to J = 3 ← 2. All transitions exhibit (partially) resolved hyperfine structure from the presence of the chlorine nuclei (both I = 3/2). This study provides the data needed for future sensitive radio astronomical searches for CCl+ in space.

Published
2021

2. The First Laboratory Detection of Vibration-rotation Transitions of 12CH+ and 13CH+ and Improved Measurement of Their Rotational Transition Frequencies

Author

Stephan Schlemmer, José Luis Doménech, Pavol Jusko, Oskar Asvany, Ministerio de Economía y Competitividad (España), European Research Council, and German Research Foundation

Subjects
Rest (physics), Physics, 010304 chemical physics, Methods: laboratory: molecular, Molecular data, laboratory: molecular [Methods], Rotational transition, Astronomy and Astrophysics, Rotational–vibrational spectroscopy, Rotation, 01 natural sciences, ISM: molecules, 3. Good health, Ion, Vibration, Interstellar medium, Space and Planetary Science, 0103 physical sciences, Atomic physics, 010303 astronomy & astrophysics, molecules [ISM]
Abstract

5 pags., 2 figs., 5 tabs., C-H stretches of the fundamental ions CH and CH, which have long been searched for, have been observed for the first time in the laboratory. The state-dependent attachment of He atoms to these ions at cryogenic temperatures has been exploited to obtain high-resolution rovibrational data. In addition, the lowest rotational transitions of CH, CH and CD have been revisited and their rest frequency values have improved substantially., This work (including the research visit of J.L.D. to Köln) has been supported by the Deutsche Forschungsgemeinschaft (DFG) via SFB 956 project B2 and the Gerätezentrum “Cologne Center for Terahertz Spectroscopy.” J.L.D. acknowledges partial support from the Spanish MINECO through grant FIS2016-77726-C3-1-P and from the European Research Council through grant agreement ERC-2013-SyG-610256 NANOCOSMOS.

Published
2018

3. ROTATIONAL SPECTROSCOPY OF THE CO-PARA-H2MOLECULAR COMPLEX

Author

Wolfgang Jäger, Stephan Schlemmer, A. V. Potapov, Leonid A Surin, Boris S. Dumesh, Paul L. Raston, V. A. Panfilov, and Thomas F. Giesen

Subjects
Physics, Jet (fluid), Astronomy and Astrophysics, Potential energy, Spectral line, symbols.namesake, Fourier transform, Space and Planetary Science, symbols, Rotational spectroscopy, Atomic physics, van der Waals force, Spectroscopy, Microwave
Abstract

The rotational spectrum of the CO-para-H2 van der Waals complex, produced using a molecular jet expansion, was observed with two different techniques: OROTRON intracavity millimeter-wave spectroscopy and pulsed Fourier transform microwave spectroscopy. Thirteen transitions in the frequency range from 80 to 130 GHz and two transitions in the 14 GHz region were measured and assigned, allowing for a precise determination of the corresponding energy level positions of CO-para-H2. The data obtained enable further radio astronomical searches for this molecular complex and provide a sensitive test of the currently best available intermolecular potential energy surface for the CO-H2 system.

Published
2009

4. High‐Frequency Rotational Spectrum of Thioformaldehyde, H2CS, in the Ground Vibrational State

Author

Eric Herbst, Frank C. De Lucia, Stephan Schlemmer, Atsuko Maeda, Holger S. P. Müller, Ivan R. Medvedev, Monika Koerber, Christian P. Endres, and Manfred Winnewisser

Subjects
Physics, Thioformaldehyde, Terahertz radiation, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, symbols.namesake, chemistry.chemical_compound, Nuclear magnetic resonance, chemistry, Space and Planetary Science, symbols, Rotational spectrum, Isotopologue, Atomic physics, Hamiltonian (quantum mechanics), Ground state, Astrophysics::Galaxy Astrophysics, Microwave, Dimensionless quantity
Abstract

Pure rotational transitions have been measured for the normal isotopologue of thioformaldehyde, -->H212C32S , in the ground vibrational state in the 110-370 GHz, 570-670 GHz, and 850-930 GHz frequency ranges. A global data set has been constructed consisting of prior microwave and millimeter-wave transitions, the submillimeter-wave and terahertz (THz) transitions reported here, and far-infrared data and ground state combination differences. The 783 different transition frequencies in the data set were fit to Watson's S-reduced Hamiltonian with 20 parameters, resulting in a dimensionless weighted root-mean-square deviation of 0.78. New frequency predictions have been made for astronomical observations based on the molecular parameters obtained in the present study.

Published
2008

5. Photodesorption of CO Ice

Author

Karin I. Öberg, Ewine F. van Dishoeck, Harold Linnartz, Stephan Schlemmer, Guido W. Fuchs, Helen J. Fraser, and Zainab Awad

Subjects
QC717, Physics, Photon, Astrochemistry, Abundance (chemistry), Ultra-high vacuum, Thermal desorption, Astronomy and Astrophysics, Space and Planetary Science, Chemical physics, Desorption, Molecule, Millimeter, Atomic physics, QC
Abstract

At the high densities and low temperatures found in star forming regions, all molecules other than H2 should stick on dust grains on timescales shorter than the cloud lifetimes. Yet these clouds are detected in the millimeter lines of gaseous CO. At these temperatures, thermal desorption is negligible and hence a non-thermal desorption mechanism is necessary to maintain molecules in the gas phase. Here, the first laboratory study of the photodesorption of pure CO ice under ultra high vacuum is presented, which gives a desorption rate of 3 × 10 3 CO molecules per UV (7–10.5 eV) photon at 15 K. This rate is factors of 10 2 -10 5 larger than previously estimated and is comparable to estimates of other non-thermal desorption rates. The experiments constrains the mechanism to a single photon desorption process of ice surface molecules. The measured efficiency of this process shows that the role of CO photodesorption in preventing total removal of molecules in the gas has been underestimated. Subject headings: Molecular data — Molecular processes — ISM: abundances — Physical Data and Processes: astrochemistry — ISM: molecules

Published
2007

6. The 2014 KIDA network for interstellar chemistry

Author

E. Herbst, Valentine Wakelam, Ian R. Sims, S. D. Le Picard, Pascal Honvault, Astrid Bergeat, Dieter Gerlich, Stephan Schlemmer, Stephen J. Klippenstein, B. Pavone, Gunnar Nyman, Kevin M. Hickson, Alexandre Faure, M. Ruaud, Daniele Galli, K. Béroff, Jean-Christophe Loison, Roland Wester, Wolf D. Geppert, Nanase Harada, Jonathan Tennyson, Pierre Gratier, D. Talbi, Marin Chabot, AMOR 2015, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut des Sciences Moléculaires (ISM), Centre National de la Recherche Scientifique (CNRS)-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Université Sciences et Technologies - Bordeaux 1-Université Montesquieu - Bordeaux 4-Institut de Chimie du CNRS (INC), Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université Grenoble Alpes - UFR Pharmacie (UGA UFRP), Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Stockholm Universtiy, Chemistry Division, Argonne National Laboratory [Lemont] (ANL), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), I. Physikalisches Institut [Köln], Universität zu Köln, Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Department of Physics and Astronomy [UCL London], University College of London [London] (UCL), Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut des Sciences Moléculaires ( ISM ), Université Montesquieu - Bordeaux 4-Université Sciences et Technologies - Bordeaux 1-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Centre National de la Recherche Scientifique ( CNRS ), Institut des Sciences Moléculaires d'Orsay ( ISMO ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Physique Nucléaire d'Orsay ( IPNO ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Université Grenoble Alpes - UFR Pharmacie ( UGA UFRP ), Université Grenoble Alpes ( UGA ), Institut de Physique de Rennes ( IPR ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ) -Centre National de la Recherche Scientifique ( CNRS ), Argonne National Laboratory [Lemont] ( ANL ), Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany, Univ Cologne, Inst Phys 1, Laboratoire Univers et Particules de Montpellier ( LUPM ), Université Montpellier 2 - Sciences et Techniques ( UM2 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université de Montpellier ( UM ) -Centre National de la Recherche Scientifique ( CNRS ), University College of London [London] ( UCL ), Université Montesquieu - Bordeaux 4-Université Sciences et Technologies - Bordeaux 1 (UB)-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln = University of Cologne, and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, [PHYS]Physics [physics], [ PHYS ] Physics [physics], Chemical models, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Chemical reaction, Astrophysics - Astrophysics of Galaxies, Interstellar medium, 13. Climate action, Space and Planetary Science, Chemical physics, [ SDU.ASTR.CO ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics of Galaxies (astro-ph.GA), Molecule, Chemical composition, ComputingMilieux_MISCELLANEOUS
Abstract

Chemical models used to study the chemical composition of the gas and the ices in the interstellar medium are based on a network of chemical reactions and associated rate coefficients. These reactions and rate coefficients are partially compiled from data in the literature, when available. We present in this paper kida.uva.2014, a new updated version of the kida.uva public gas-phase network first released in 2012. In addition to a description of the many specific updates, we illustrate changes in the predicted abundances of molecules for cold dense cloud conditions as compared with the results of the previous version of our network, kida.uva.2011., Accepted for publication in ApJS on February 26th, 2015

Published
2015

7. Low‐Temperature Experiments on the Formation of Deuterated C3H+3

Author

Dieter Gerlich, I. Savić, and Stephan Schlemmer

Subjects
Physics, Direct production, Deuterium, Isotope, Space and Planetary Science, Carbon chemistry, Interstellar cloud, Analytical chemistry, Astronomy and Astrophysics, Atomic physics, Dissociative recombination
Abstract

Manydeuteratedmoleculeshavebeendiscoveredininter-andcircumstellarregions.Insomecases,theobserved abundances can be explained with simple thermodynamic models; often, however, isotope enrichment is more complicated. This has been seen recently in detailed low-temperature experiments performed for the fundamental systemsH þ =H2D þ andCH þ =CHn� 1D þ .An unsolvedproblem is toexplainthelarge abundanceofC3H2andlarger hydrocarbons and their deuterated variants observed in cold, dark interstellar clouds. In this work a variabletemperature22poletrapisutilizedforcloselyscrutinizingvariousion-moleculereactionsthatmaycontributetothe formation of C3H2D þ or C3HD þ and, via dissociative recombination, C3HD. The experimental study of the promising candidate C3H þ þ HD ! C3H2D þ þ H2, which has already been excluded by theory, corroborates that this exothermic H-D exchange does not occur at all. A careful analysis of the data reveals that the 15 K rate coefficient is smaller than 4 ; 10 � 16 cm 3 s � 1 . In contrast, quite efficient routes have been found in the lowtemperature experiments, starting with C þ and proceeding via deuterated C3H þ to C3H þ and C3H þ . Formation of C3D þ in C þ þ HD collisions is 6 times faster than assumed in astrochemical models (k ¼ 9:3 ; 10 � 10 cm 3 s � 1 ). Surprisingly, direct production of C3HD þ via radiative association has also been observed (kr ¼ 6:0 ; 10 � 11 cm 3 s � 1 ).ReactionsofpartlyorfullydeuteratedC3H þ þ H2 collisionsystemarestronglydependentontemperatureand thehydrogenorthotopararatio.Inaddition,itshowsverycomplicatedisotopeeffects.Forexample,inC3H þ þ HD collisions the formation of C3HD þ (k ¼ 4:6 ;10 � 10 cm 3 s � 1 ) dominates over the H-D exchange (k ¼ 5:6 ; 10 � 11 cm 3 s � 1 ) and radiative association C3H2D þ (kr ¼ 3:2 ;10 � 11 cm 3 s � 1 ). The reactions of C3H þ þ H2 are very slow for all isotope combinations. Although several questions remain open and more low-temperature experiments are needed, it is recommended that the new values are included in astrochemical databases, since they are fundamental to the correct description of the carbon chemistry in interstellar clouds.

Published
2005

8. Deuteration of \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $\mathrm{CH}\,^{+}_{n}$ \end{document} (n= 3–5) in Collisions with HD Measured in a Low‐Temperature Ion Trap

Author

Dieter Gerlich, Stephan Schlemmer, and Oskar Asvany

Subjects
chemistry.chemical_classification, Physics, Astrochemistry, Hydrogen, Analytical chemistry, chemistry.chemical_element, Astronomy and Astrophysics, Chemical reaction, Ion, Reaction rate constant, Hydrocarbon, chemistry, Deuterium, Space and Planetary Science, Ion trap, Atomic physics
Abstract

Deuteration of small hydrocarbon ions CH via H-D exchange (n = 3-5) has been studied in a 22 pole ion trap at a nominal temperature of 15 K. Sequential deuteration from CH to CD is very fast if one uses pure HD as the target gas. Rate coefficients have been measured to be 1.65 × 10-9, 1.59 × 10-9, and 1.50 × 10-9 cm3 s-1. If, however, CH is relaxed in p-H2 containing traces of HD, the rate coefficient for isotope enrichment is significantly smaller, (4 ± 2) × 10-10 cm3 s-1. This important result is most probably due to symmetry selection rules influencing this reaction. The ions CH and CH are not observed, within the experimental uncertainties, to exchange H atoms for D atoms at all. Upper limits for the rate coefficients for forming CH3D+ and CH4D+ are 1 × 10-12 and 5 × 10-18 cm3 s-1, respectively. Hydrogen or deuterium abstraction in collisions of CH with HD occurs with a sum rate coefficient of 4.5 × 10-10 cm3 s-1. Surprisingly, the more exoenergetic and statistically favored product CH4D+ is formed only in 1/3 of the reactive collisions, while CH dominates with 2/3. The results are discussed on the basis of the formation of long-lived collision intermediates, open- and closed-shell ions, and barriers along the reaction path. All experimental data clearly indicate that conservation of total nuclear spin plays an important role in these low-temperature chemical reactions involving identical nuclei. Implications of this laboratory work to isotopic fractionation in astrophysical environments are discussed.

Published
2004

9. HOC[TSUP]+[/TSUP] + H[TINF]2[/TINF] Isomerization Rate at 25 K: Implications for the Observed [HCO[TSUP]+[/TSUP]]/[HOC[TSUP]+[/TSUP]] Ratios in the Interstellar Medium

Author

J. von Richthofen, M. Smith, Stephan Schlemmer, and Dieter Gerlich

Subjects
Physics, Interstellar medium, Range (particle radiation), Astrochemistry, Chemical models, Space and Planetary Science, Abundance (chemistry), Metastability, Analytical chemistry, Astronomy and Astrophysics, Atomic physics, Adiabatic process, Isomerization
Abstract

The recent detection of the metastable HOC+ isomer toward a wide range of interstellar environments has demonstrated abundances that cannot be explained within current chemical models. The abundance of HOC+ in these models relies heavily on the rate of the isomerization of HOC+ by H2 to the lowest energy isomer, HCO+. A variable temperature 22-pole ion-trap apparatus is employed to study the isomerization of HOC+ by H2 at 25 K. The observed rate coefficient for isomerization is (3.8 ± 0.5) × 10-10 cm3 s-1. This indicates that there is probably no temperature dependence in this reaction below 300 K, suggesting the absence of any significant energetic barrier on the lowest adiabatic H3CO+ potential surface. This result argues that in regions where abundant HOC+ is observed, the production of this isomer must be strongly favored or that there is a concomitant rapid physicochemical loss for the isomer HCO+. Some results for forming DCO+ are briefly mentioned.

Published
2002

10. A KInetic Database for Astrochemistry (KIDA)

Author

N. G. Adams, Gunnar Nyman, Kevin M. Hickson, Astrid Bergeat, Jürgen Troe, Eric Hébrard, Daniele Galli, Franck Selsis, Ian R. Sims, Pascal Pernot, Eric Herbst, Roland Wester, Stephen J. Klippenstein, D. Talbi, Jean-Christophe Loison, Alain Faure, Franck Hersant, Marin Chabot, Wolf D. Geppert, K. Béroff, Valentine Wakelam, Alexander Dalgarno, Ian W. M. Smith, S. D. Le Picard, Veronica M. Bierbaum, Stephan Schlemmer, Laurent Wiesenfeld, Dieter Gerlich, Jonathan Tennyson, Marie-Christine Bacchus-Montabonel, B. Pavone, E. F. van Dishoeck, Pascal Honvault, Vijayanand Chandrasekaran, AMOR 2012, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Ohio State Univ, Dept Phys, Columbus, OH 43210 USA, Ohio State University [Columbus] (OSU), Ohio State Univ, Dept Astron & Chem, Columbus, OH 43210 USA, Institut des Sciences Moléculaires (ISM), Université Montesquieu - Bordeaux 4-Université Sciences et Technologies - Bordeaux 1 (UB)-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Max-Planck-Institut für Extraterrestrische Physik (MPE), Leiden Observatory [Leiden], Universiteit Leiden, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), SSE 2012, FORMATION STELLAIRE 2012, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Chimie Physique D'Orsay (LCPO), Université Paris-Sud - Paris 11 (UP11)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), I. Physikalisches Institut [Köln], Universität zu Köln = University of Cologne, Groupe de Recherche en Astronomie et Astrophysique du Languedoc (GRAAL), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute of Physical Chemistry, Georg-August-University = Georg-August-Universität Göttingen, Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université Montesquieu - Bordeaux 4-Université Sciences et Technologies - Bordeaux 1-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Smithsonian Institution-Harvard University [Cambridge], Universiteit Leiden [Leiden], Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln, and Georg-August-University [Göttingen]

Subjects
Astrochemistry, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Interstellar cloud, FOS: Physical sciences, Astrophysics, Kinetic energy, computer.software_genre, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, miscellaneous [astrochemistry, astronomical databases], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010304 chemical physics, Database, Kinetic information, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Interstellar medium, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), computer, Chemical database, Galaxy Astrophysics
Abstract

We present a novel chemical database for gas-phase astrochemistry. Named the KInetic Database for Astrochemistry (KIDA), this database consists of gas-phase reactions with rate coefficients and uncertainties that will be vetted to the greatest extent possible. Submissions of measured and calculated rate coefficients are welcome, and will be studied by experts before inclusion into the database. Besides providing kinetic information for the interstellar medium, KIDA is planned to contain such data for planetary atmospheres and for circumstellar envelopes. Each year, a subset of the reactions in the database (kida.uva) will be provided as a network for the simulation of the chemistry of dense interstellar clouds with temperatures between 10 K and 300 K. We also provide a code, named Nahoon, to study the time-dependent gas-phase chemistry of 0D and 1D interstellar sources., Comment: Accepted for publication in ApJS

Published
2012

11. LABORATORY ROTATIONAL SPECTRUM OF l -C 3 H + AND CONFIRMATION OF ITS ASTRONOMICAL DETECTION

Author

Stephan Schlemmer, Alexander Stoffels, Oskar Asvany, Lars Kluge, and Sandra Brünken

Subjects
Physics, Astrochemistry, Space and Planetary Science, Photodissociation, Astronomy and Astrophysics, Ion trap, Photodissociation region, Carbocation, Atomic physics, Spectroscopy, Mass spectrometry, Astrophysics::Galaxy Astrophysics, Dissociation (chemistry)
Abstract

The rotational spectrum of l-C3H+ has been measured in the millimeter-wave band in a 4 K cryogenic ion trap apparatus employing a novel mass-selective action spectroscopy method based on light induced reactions (LIR). Line positions of four rotational transitions (J = 1-2 up to J = 4-5) were observed with a relative precision of 3 × 10–7. The experimental transition frequencies and derived spectroscopic constants agree with those from recent astronomical observations, and unambiguously confirm the detection of this astrochemically relevant carbocation in the Horsehead photodissociation region and toward Sgr B2(N).

Published
2014

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