DOCSLIB.ORG

Microwave Spectroscopy Information Letter Vol. Lxii

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Microwave Spectroscopy Information Letter Vol. Lxii MICROWAVE SPECTROSCOPY INFORMATION LETTER VOL. LXII April 15, 2019 Compiled By: Garry S. Grubbs II Missouri University of Science and Technology 400 W. 11th St. Rolla, MO, 65409 MICROWAVE SPECTROSCOPY NEWSLETTER LXI List of Contributors / Table of Contents Contributor Institution Lab, Page No. Alonso, J. L. Universidad de Valladolid 1, 1 Arunan, E. India Institute of Science, Bangalore 2, 4 Bird, R. University of Pittsburgh, Johnstown 3, 5 Bizzocchi, L. Max Planck Institute for Extraterrestrial Physics 6, 10 Blanco, S. Universidad de Valladolid 31, 94 Bohn, R. K. University of Connecticut 4, 6 Brown, G. South Carolina Governor’s School for Science and Mathematics 5, 8 Caselli, P. Max Planck Institute for Extraterrestrial Physics 6, 10 Cocinero, E. Universidad del País Vasco 7, 12 Cooke, S. A. Purchase College SUNY 8, 15 Dore, L. Università di Bologna 40, 122 Douglass, K. O. National Institute of Standards and Technolo gy 32, 98 Drouin, B. Jet Propulsion Laboratory, Pasadena 9, 18 Durig, J. R. University of Missouri, Kansas City 14, 43 Evangelisti, L. Università di Bologna 10, 20 Favero, L. B. Università di Bologna 10, 20 Feng, G. Chongqing University 12, 29 Fujitake, M. Kanazawa University 11, 26 Gou, Qian Chongqing University 12, 29 Grabow, J.-U. Gottfried-Wilhelm-Leibniz-Universität, Institut für Physikalische Chemie & Elektrochemie Hannover 13, 34 Groner, P. University of Missouri-Kansas City 14, 43 Grubbs, G. Missouri University of Science & Technolog y 15, 44 Harada, K. Kyushu University 16, 49 Hirota, E. Grad. Univ. for Advanced Studies, Kanagawa 17, 53 Ilyushin, V. Institute of Radio Astronomy NASU, Kharkiv 18, 57 Jäger, W. University of Alberta 19, 60 Kang, L. Kennesaw State University 20, 63 Kawashima, Y. Kanagawa Institute of Technology 21, 64 Kisiel, Z. Polish Academy of Sciences 22, 68 Kleiner, I. LISA, Univ. of Paris-Est Creteil, U. Paris Diderot 35, 106 Kobayashi, K. Toyama University 23, 71 Kukolich, S. G. University of Arizona 24, 73 Kuze, N. Sophia University 25, 75 Legon, A. C. University of Bristol 26, 77 Leopold, K. R. University of Minnesota 27, 79 Lesarri, A. Universidad de Valladolid 28, 82 Leung, H. O. Amherst College 29, 87 Lin, W. University of Texas Rio Grande Valley 30, 92 Lopez, J. C. Universidad de Vallodolid 31, 94 Lovas, F. J. National Institute of Standards and Technology 32, 98 Maris, A. Università di Bologna 10, 20 Marshall, M. D. Amherst College 29, 87 Melandri, S. Università di Bologna 10, 20 Minei, A. College of Mount St. Vincent 8, 15 Müller, H. S. P. I. Physikalisches Institute, Köln 34, 102 Nemchick, D. J. Jet Propulsion Laboratory, Pasadena 9, 18 Nguyen, L. LISA, Univ, of Paris-Est Creteil, U. Paris Diderot 35, 106 Novick, S. Wesleyan University 36, 109 Okabayashi, T. Shizuoka University 37, 113 Ozeki, H. Toho University 38, 115 Pearson, J. C. Jet Propulsion Laboratory, Pasadena 9, 18 Peebles, R. A. Eastern Illinois University 39, 117 Peebles, S. Eastern Illinois University 39, 117 Plusquellic, D. National Institute of Standards and Technology 32, 98 Pratt, D. University of Vermont 3, 5 Pringle, W. C. Wesleyan University 36, 109 Puzzarini, C. Università di Bologna 40, 122 Sanz, M. E. King’s College, London 41, 126 Schlemmer, S. I. Physikalisches Institute, Köln 34, 102 Schnell,M. Deutsches Elektronen-Synchrotron (DESY), Hamburg, Germany and Institute for Physical Chemistry, Christian-Albrechts-Universität zu Kiel 42, 129 Sedo, G. University of Virginia-Wise 33, 101 Shipman, S. New College Florida 43, 139 Stahl, W. Institut für Physikalische Chemie, Aachen 44, 140 Tanaka, K. Kyushu University 16, 49 Tubergen, M. Kent State University 45, 142 van Wijngaarden, J. University of Manitoba 46, 143 Walker, N. J. Newcastle University 47, 145 Walters, A. Université de Toulouse 48, 148 Widicus Weaver, S. Emory University 49, 149 Wlodarczak, G. Université de Lille 50, 150 Xu, Y. University of Alberta 51, 154 Yu, S. Jet Propulsion Laboratory, Pasadena 9, 18 Ziurys, L. University of Arizona 52, 158 Formula Index After Lab 52, i In Memoriam After Index Jon T. Hougen (Written by Angela Hight Walker) Walt Lafferty (Written by Wallace “Pete” Pringle and Bill Kirchhoff) Li-Hong Xu (Written by Yunjie Xu, Jens-Uwe Grabow, and Shui-Ming Hu) Interesting and Informative Websites Maintained by Our Colleagues and Funding Acknowledgement 1. The J. P. L. Submillimeter, Millimeter, and Microwave Spectral Line Catalog is accessible via anonymous ftp at spec.jpl.nasa.gov or via our home page at http://spec.jpl.nasa.gov Jet Propulsion Laboratory, Lab 9. 2. A database “Programs for ROtational SPEctroscopy (PROSPE)” is available at: http://info.ifpan.edu.pl/~kisiel/prospe.htm A new database on "History of Rotational Spectroscopy" is being constructed at: http://info.ifpan.edu.pl/~kisiel/rothist/rothist.html A subpage on this Newsletter is at: http://info.ifpan.edu.pl/~kisiel/rothist/newsletter.html This database depends critically on contributions, which are solicited and accepted at (preferably): [email protected], Lab 22 3. Recommended Rest Frequency Table. F. J. Lovas, J. Phys. Chem. Ref. Data, 1-181 (2004). See: http://physics.nist.gov/PhysRefData/micro/html/contents.html For diatomics, triatomics, and hydrocarbons, see: http://physics.nist.gov/PhysRefData/MolSpec/index.html A graphic, interactive fitting program, jb95, is available at http://physics.nist.gov/Divisions/Div844/facilities/uvs/jb95userguide.htm An application and description of the program is found in D. F. Plusquellic et al., J. Chem. Phys., 115 (2001) 3057. National Institute of Standards and Technology, Lab 32. 4. A bibliography of high resolution studies of weakly bound complexes is maintained on the Web at http://www.Wesleyan.edu/chem/faculty/novick/vdw.html Wesleyan University, Lab 36. 5. The Cologne Database for Molecular Spectroscopy is available online at http://www.astro.uni-koeln.de/cdms/ I. Physikalisches Institut, Köln, Lab 34. 6. The Hannover FTMW spectrometer control & analysis software is available at http://www.pci.uni-hannover.de/~lgpca/spectroscopy/ftmw Institut für Physikalische Chemie, Hannover, Lab 13. Garry Grubbs II would like to thank the Missouri University of Science and Technology Chemistry Department and College of Arts, Sciences, and Business for covering the cost of all printing and shipping of this volume of the Microwave Spectroscopy Information Letter. Lab 1 Name to whom queries should be addressed: Jose L. Alonso Mailing address Grupo Espectroscopia Molecular GEM. Centro de Investigación Quifima. Laboratorios de Espectroscopia y Bioespectroscopia. Parque Científico Uva. Unidad Asociada C.S.I.C. Universidad de Valladolid. Valladolid 47011 Spain Telephone: 34-983-186348/45/49 E- mail: [email protected] Website: www.gem.uva.es NAME OF NAME OF PRESENT STAGE FORMULA COMPOUND INVESTIGATOR OF PROGRESS b,d C2H6N2O Glycinamide ApJ 861:70 (7pp), 2018 a,b,d C2H3NO Methyl isocyanate mmw-sub wave spectrum C2H4O2 Vinyl Alcohol mmw-sub wave spectrum C2H3NO Propynal mmw-sub wave spectrum d C3H3NO Propiolamide mmw-sub wave spectrum C3H3NO2 Cyanoacetic acid spectrum assigned a C3H5NO Ethylisocyanide A&A 616, A173 (2018) a C3H6O2 Metoxyacetaldehyde A&A 619, A67 (2018) C3H6O2 Lactaldehyde ms. in preparation C3H3NO3 2,5-oxazolidinedione JPCL,10,1325(2019) C3H6N2O3 Hydantoic Acid JPCL,10,1325(2019) C3H7N3O2 Glycociamine LA-MBFT spectrum C3H9NO2 N-methyl alanine PCCP 20, 29159 (2018) C4H2O4 Squaric acid ms. in preparation C4H4O6 Malic acid ms. In preparation C4H6O6 Tartaric Acid ms. in preparation 1 Lab 1 NAME OF NAME OF PRESENT STAGE FORMULA COMPOUND INVESTIGATOR OF PROGRESS e,f C4H7N3O Creatinine ms. in preparation C4H7N3O3 Cytosine-water ms. in preparation C4H9NO2 Aminoisobutyric Acid Chem. E.J., 25, 2288 (2019) C4H9NO2 3-Aminobutyric Acid PCCP 20,15574 (2018) C4H9NO2S Homocysteine ms. in preparation C4H9NO3 Homoserine LA-CPFT/LA-MBFT spectrum C4H10O4 Erythritol LA-CPFT spectrum C5H10N2O2 Glutamine ms. in preparation C5H10O5 Arabinose ms. in preparation C5H10O5 Lixose ms. in preparation C5H10N2O3 Alanine-Glycine LA-CPFT spectrum C5H11NO Norvaline LA-CPFT spectrum C5H11NO2 Isovaline ms. in preparation C5H11NO2S Methionine ms. in preparation c C5H12O5 Ribitol Chem. Eur.J., 25,2288 (2019) C5H12O5 Arabitol LA-CPFT spectrum C5H12O5 Xylitol LA-CPFT spectrum C6H10NO2 Pipecolic Acid PCCP 21, 4155 (2019) C6H12O6 Mannose ms. in preparation C6H14O6 Dulcitol ChemPhysChem 2018,19,3334 C6H12O6 Sorbitol ChemPhysChem 2018,19,3334 C6H12O6 Manitol LA-CPFT spectrum 2 Lab 1 NAME OF NAME OF PRESENT STAGE FORMULA COMPOUND INVESTIGATOR OF PROGRESS C6H12O6 Inositol LA-CPFT spectrum C6H12N2O3 Alanyl alanine LA-CPFT spectrum C7H5NO3S Saccharin JPCA (2019) C7H12N2O3 Prolylglycine LA-CPFT spectrum C7H12N2O3 Glycylproline Comm. Chemistry (2019) C8H8O3 Mandelic acid LA-CPFT spectrum C8H8O4 Dopac LA-CPFT spectrum C8H9NO3 Pyridoxal (Vit. B6) ms. In preparation C8H11NO3 Pyridoxine (Vit. B6) ms. In preparation C8H11NO3 Noradrenaline LA-MB-FTMW spectrum C9H12N2O2 Dulcine LA-CPFT spectrum C9H12N2O5 Deoxyuridine LA-MB-FTMW spectrum C9H13NO3 Adrenaline ms. In preparation C12H16N2 N,N-Dimethyltryptamine LA-CPFT spectrum C12H22O11 Sucrose LA-CPFT spectrum C12H22O11 Lactose LA-CPFT spectrum C19H28O2 Testosterone LA-CPFT spectrum ________________________________________ In collaboration with: a J. Cernicharo. CSIC.Madrid b Z. Kisiel. Warszawa c M.E.Sanz. King´s College d J-C Guillemin. Rennes e Barone Pisa f Puzzarini. Bologna 3 Lab 2 Name to whom queries should be addressed: Prof. E. Arunan Mailing Address Department of Inorganic and Physical Chemistry Indian Institute of Science Bangalore. 560012 INDIA Telephone:+91-80-2293-2828 FAX:+91-80-2360-0282 E-Mail: [email protected] Website:http://ipc.iisc.ac.in/arunan.php NAME OF NAME OF PRESENT STAGE FORMULA COMPOUND INVESTIGATOR OF PROGRESS CH5FO Methylfluoride-H2O Sharon Priya Gnanasekar Assigned transitions for Manuel Goubet, Robert hydrogen bond structure. Georges Carbon bonded structure? CH3ArF Argon-methylfluoride Sharon Priya Gnanasekar Assigned transitions for Manuel Goubet, Robert a T-shaped structure. Georges Several unassigned lines C--Ar and F--Ar structures? H4S2 H2S dimer Arijit Das, Chris Medcarft Angew.
Load more

Recommended publications
  • Ubiquitous Argonium \(Arh+\) in the Diffuse Interstellar Medium: A
    A&A 566, A29 (2014) Astronomy DOI: 10.1051/0004-6361/201423727 & c ESO 2014 Astrophysics Ubiquitous argonium (ArH+) in the diffuse interstellar medium: A molecular tracer of almost purely atomic gas P. Schilke1, D. A. Neufeld2, H. S. P. Müller1, C. Comito1, E. A. Bergin3, D. C. Lis4;5, M. Gerin6, J. H. Black7, M. Wolfire8, N. Indriolo2, J. C. Pearson9, K. M. Menten10, B. Winkel10, Á. Sánchez-Monge1, T. Möller1, B. Godard6, and E. Falgarone6 1 I. Physikalisches Institut der Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany e-mail: [email protected] 2 The Johns Hopkins University, Baltimore, MD 21218, USA 3 Department of Astronomy, The University of Michigan, 500 Church Street, Ann Arbor, MI 48109-1042, USA 4 California Institute of Technology, Pasadena, CA 91125, USA 5 Sorbonne Universités, Université Pierre et Marie Curie, Paris 6, CNRS, Observatoire de Paris, UMR 8112 LERMA, Paris, France 6 LERMA, CNRS UMR 8112, Observatoire de Paris & École Normale Supérieure, 24 rue Lhomond, 75005 Paris, France 7 Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden 8 Astronomy Department, University of Maryland, College Park, MD 20742, USA 9 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA 10 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany Received 28 February 2014 / Accepted 29 March 2014 ABSTRACT Aims. We describe the assignment of a previously unidentified interstellar absorption line to ArH+ and discuss its relevance in the + context of hydride absorption in diffuse gas with a low H2 fraction.
    [Show full text]
  • The Preparation and Reactions of Certain Quarternary Ammonium And
    THE PREPARATION AND REACTIONS OF CERTAIN QUATERNARY AMMONIUM AND RELATED COMPOUNDS By CARL L MICHAELIS A DISSERTATION PRESENTED TO THE GRADUATE COUNCIL OF THE UNIVERSITY OF FLORIDA IN PARTIAL FULFILMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY UNIVERSITY OF FLORIDA August, 1953 ACKNOWLEDGMENTS The author wishes to express his sincere appreci- ation for the valuable assistance and inspiring direction of Dr. George B. Butler. Special thanks are due Dr. and Mrs. Armin Gropp for the help and encouragement in carrying out this investi- gation. The author also wishes to express his appreciation for the assistance and advice so readily given him by his fellow students, graduate and undergraduate alike. \ ii TABLE OF CONTENTS Page ACKNOWLEDGMENTS ii TABLE OF CONTENTS iii INTRODUCTION 1 A. Review of Literature and Statement of Problem 1 EXPERIMENTAL 14 A. General Discussion 14 B. Procedure 18 DISCUSSION . 51 SUMMARY 62 BIBLIOGRAPHY 64 BIOGRAPHICAL ITEMS 66 COMMITTEE REPORT 67 iii INTRODUCTION The need for compounds of good adrenergic blooking activity has been the object of extensive investigation in recent years. In order to get a better idea of the nature of adrenergic blocking activity, it might be best to under- stand first how an adrenergic compound functions. Certain compounds like epinephrine or adrenaline, are powerful agents in stimulating the sympathetic nervous system, that part of the nervous system springing from the thoracic lumbar cord. The substance epinephrine is much like, if not identical to, the substance called sympathin, which is produced at the ending of a nerve in the smooth muscle or gland when a nerve is stimulated.
    [Show full text]
  • Ubiquitous Argonium, Arh+, in the Diffuse Interstellar Medium
    Ubiquitous Argonium, ArH+, in the Interstellar Medium P. Schilke, Holger S. P. Müller, C. Comito, Á. Sánchez-Monge, D. A. Neufeld, N. Indriolo, E. A. Bergin, D. C. Lis, M. Gerin, J. H. Black, M. G. Wolfire, J. C. Pearson, K. M. Menten, B. Winkel V.6, 13th International HITRAN Conference, CfA, Cambridge, MA, USA, June 23–25, 2014 What is Argonium? ArH+, 1Σ+, isoelectronic to HCl + + Formation: Ar + H2 → ArH + H + + Destruction (e.g.): ArH + H2 → Ar + H3 Isotopic ratio: 36Ar : 38Ar : 40Ar terrestrial: 84.2 : 15.8 : 25018.8 (from decay of 40K) solar/ISM: ~84.6 : ~15.4 : 0.025 36ArH+ toward Crab Nebula SNR: J = 1 – 0 & 2 – 1 in emission (w. OH+ N = 1 – 0); SPIRE/Herschel M. J. Barlow et al., Science 342 (2013) 1343 On the Spectroscopy of ArH+ 40ArH+; rotational spectroscopy: K. B. Laughlin et al., PRL 58 (1987) 996: J" = 0 J. M. Brown et al., JMSp 128 (1988) 587: J" = 1 – 6 D. J. Liu et al., JCP 87 (1987) 2442: J" = 20 – 24; v ≤ 4 (MIR) 40ArD+; rotational spectroscopy: W. C. Bowman et al., JCP 79 (1983) 2093: J" = 0 (+ 36ArD+ & 38ArD+ H. Odashima et al., JMSp 195 (1999) 356: J" = 2 – 14 rovibrational spectroscopy: J. W. Brault & S. P. Davis, Phys. Sript. 25 (1982) 268: 40ArH+ J. W. C. Johns, JMSp 106 (1984) 124: 40ArH+, 40ArD+ R. R. Filueira & C. E. Blom, JMSp 127 (1988) 279: 36ArH+, 38ArH+ M. Cueto et al., ApJ 783 (2014) L5: 36ArH+, 38ArH+ ArH+ toward Sagittarius B2(M) – HIFI Line Survey Absorption toward Sgr B2(M) massive star-forming regions as background sources with approximate origins Sagittarius B2(M) Interstellar Chemistry of ArH+ I + + + + Ar + H2 → ArH + H exothermic (endo.
    [Show full text]
  • Detection of Extragalactic Argonium, Arh+, Toward PKS 1830−211⋆
    A&A 582, L4 (2015) Astronomy DOI: 10.1051/0004-6361/201527254 & c ESO 2015 Astrophysics Letter to the Editor Detection of extragalactic argonium, ArH+, toward PKS 1830−211 Holger S. P. Müller1, Sébastien Muller2, Peter Schilke1, Edwin A. Bergin3, John H. Black2, Maryvonne Gerin4, Dariusz C. Lis5,6, David A. Neufeld7, and Sümeyye Suri1 1 I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany e-mail: [email protected] 2 Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 43992 Onsala, Sweden 3 Department of Astronomy, The University of Michigan, 500 Church Street, Ann Arbor, MI 48109-1042, USA 4 LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, École normale supérieure, 75005 Paris, France 5 LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, 75014 Paris, France 6 Cahill Center for Astronomy and Astrophysics 301-17, California Institute of Technology, Pasadena, CA 91125, USA 7 Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA Received 26 August 2015 / Accepted 22 September 2015 ABSTRACT 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.
    [Show full text]
  • Primordially Hydridic Earth Viacheslav Zgonnik, Hervé Toulhoat, Vladimir Larin, Nikolay Larin
    Primordially hydridic Earth Viacheslav Zgonnik, Hervé Toulhoat, Vladimir Larin, Nikolay Larin Abundances of elements on Earth’s crust relative to Sun’s photosphere and Si plotted versus first ionization potential (IP) • Clearly shows separation of elements by their IP • Outliers are due to use of only Earth’s crust composition • Tested with success for other planets, Moon and asteroids • Described by a Boltzmann distribution depending on the distance to the protosun • Predicts high initial content of hydrogen • Earth currently has about 4% by weight of hydrogen. • It is mainly combined as hydrides and partly dissolved into other phases http://arxiv.org/abs/1208.2909v2 Non-Ionizing UV (< 7 eV) Photochemistry of Cosmic Ice Analogs of Ammonia Radiolysis involves electron Photochemistry involves electron excitation due to particle radiation excitation without ionization in addition to all ionization – reactions initiated by cations – production of low-energy electron cascade – non-uniform distribution of reaction intermediates, non-selective chemistry leading to multiple reaction products We see production of N2 and N3 species with high- energy electrons and < 8 eV photons, but not with < 6 eV photons Islem Bouhali Soumaya Bezzaouia Mourad Telmini Theoretical study of Rydberg states of HeH+ ion using the Halfium model Christian Jungen Presented by: Islem Bouhali 2 HeH+ molecular ion in Born-Oppenheimer approximation e2 r12 Max(extern region e1 r2a GMQDT r r 1a 2b r1b Max(reaction surface R MATCHING ++ + He H Max( : reaction volume R-MATRIX Combination of the Variational R-matrix method and of the Generalized Multichannel Quantum Defect Theory Telmini and Jungen, Phys. Rev. A 68 062704 (2003).
    [Show full text]
  • The Prospects for Petroleum Exploration in the Eastern Sector of Southern Baltic As Revealed by Sea Bottom Geochemical Survey Correlated with Seismic Data
    Przegl¹d Geologiczny, vol. 52, no. 8/2, 2004 The prospects for petroleum exploration in the eastern sector of Southern Baltic as revealed by sea bottom geochemical survey correlated with seismic data Jerzy Dom¿alski*, Wojciech Górecki**, Andrzej Mazurek*, Andrzej Myœko**, Wojciech Strzetelski**, Krzysztof Szama³ek*** A b s t r a c t . In the Polish offshore £eba (B) tectonic block in the southeastern part of the Baltic Sea the oil and gas fields are accumu- lated in Middle Cambrian quartzose sandstone, often fractured and diagenetically sealed at depth by advanced silification developed in reservoir around the petroleum deposit. Petroleum traps are mainly of structure-tectonic type, i.e., anticlines closed with strike-slip faults. At least four gas-condensate and four oil deposits of total reserves more than 10 Gm3 gas and 30 Mt oil were discovered by the “Petrobaltic” Co. in the Polish Baltic sector. The subsurface petroleum deposits in the Cambrian reservoir are the source of secondary vertical hydrocarbon migration to the surface which produces surface microseepages and hydrocarbon anomalies. Geochemical survey of the sea bottom sediments and waters run along seismic profiles was completed in 1999–2002 within a joint project of “Petrobaltic” Co. Gdañsk and the Fossil Fuels Dept., AGH University of Science and Technology, Kraków, approved by the Ministry of Environmental Protection, Natural Resources and Forestry. It was found that seafloor hydrocarbon anomalies are closely related to subsurface geologic structure and location of petroleum deposits. Particularly the faults as principal venues for vertical hydrocarbon migration are reflected in high-magnitude seafloor anomalies. Above petroleum field there occurs a “halo” effect of high-magnitude anomalies contouring the deposit with damping related to productive zone situated inbetween.
    [Show full text]
  • Microwave Spectroscopy Information Letter Vol
    MICROWAVE SPECTROSCOPY INFORMATION LETTER VOL. LXI April 15, 2018 Compiled By: Garry S. Grubbs II Asst. Professor of Chemistry Department of Chemistry Missouri Univ. of Science & Technology 400 W. 11th St. Rolla, MO, 65409 [email protected] MICROWAVE SPECTROSCOPY NEWSLETTER LXI List of Contributors / Table of Contents Contributor Institution Lab, Page No. Alonso, J. L. Universidad de Valladolid 1, 5 Arunan, E. India Institute of Science, Bangalore 2, 7 Bird, R. University of Pittsburgh, Johnstown 3, 8 Bizzocchi, L. Max Planck Inst. for Extraterrestrial Physics 33, 103 Blanco, S. Universidad de Valladolid 31, 94 Bohn, R. K. University of Connecticut 4, 9 Brown, G. Coker College 5, 11 Caselli, P. Max Planck Inst. for Extraterrestrial Physics 33, 103 Christen, D. Institut für Physikalische Chemie, Tübingen 6, 13 Cocinero, E. Universidad del País Vasco 7, 14 Cooke, S. A. Purchase College SUNY 8, 17 Dore, L. Università di Bologna 40, 124 Douglass, K. O. National Institute of Standards and Technology 32, 98 Drouin, B. Jet Propulsion Laboratory, Pasadena 9, 21 Durig, J. R. University of Missouri, Kansas City 14, 44 Esposti, C. D. Università di Bologna 10, 23 Evangelisti, L. Università di Bologna 10, 23 Favero, L. B. Università di Bologna 10, 23 Feng, G. Chongqing University 12, 33 Fujitake, M. Kanazawa University 11, 30 Gou, Qian Chongqing University 12, 33 Grabow, J.-U. Institut für Physikalische Chemie, Hannover 13, 36 Groner, P. University of Missouri, Kansas City 14, 44 Grubbs, G. Missouri University of Science & Technology 15, 45 Harada, K. Kyushu University 16, 49 Hirota, E. Grad. Univ. for Advanced Studies, Kanagawa 17, 53 Ilyushin, V.
    [Show full text]
  • Important Features of the Potential Energy Surface of the Methylamine Plus O(1D) Reaction
    Physical Chemistry Chemical Physics Important Features of the Potential Energy Surface of the Methylamine Plus O(1D) Reaction Journal: Physical Chemistry Chemical Physics Manuscript ID CP-ART-09-2019-005039.R1 Article Type: Paper Date Submitted by the 17-Oct-2019 Author: Complete List of Authors: Wolf, Mark; University of Georgia , Center for Computational Quantum Chemsitry; Hoobler, Preston; Covenant College, Chemistry; University of Georgia Franklin College of Arts and Sciences, Center for Computational Quantum Chemistry Turney, Justin; University of Georgia, Center for Computational Chemistry Schaefer, Henry; University of Georgia, Computational Chemistry Page 1 of 13 Physical Chemistry Chemical Physics Journal Name Important Features of the Potential Energy Surface of the Methy- lamine Plus O(1D) Reaction † Mark E. Wolf, Preston R. Hoobler, Justin M. Turney, and Henry F. Schaefer III∗ This research presents an ab initio characterization of the potential energy surface for the methy- lamine plus 1D oxygen atom reaction, which may be relevant to interstellar chemistry. Ge- ometries and harmonic vibrational frequencies were determined for all stationary points at the CCSD(T)/aug-cc-pVTZ level of theory. The focal point method along with several additive correc- tions was used to obtain reliable CCSDT(Q)/CBS potential energy surface features. Extensive conformational analysis and intrinsic reaction coordinate computations were performed to ensure accurate chemical connectivity of the stationary points. Five minima were determined to be pos- sible products of this reaction and three novel transition states were found that were previously unreported or mislabeled in the literature. The pathways we present can be used to guide further searches for NH2 containing species in the interstellar medium.
    [Show full text]
  • Is the Reaction Between Formic Acid and Protonated Aminomethanol a Possible Source of Glycine Precursors in the Interstellar Medium?
    A&A 579, A125 (2015) Astronomy DOI: 10.1051/0004-6361/201526548 & c ESO 2015 Astrophysics Is the reaction between formic acid and protonated aminomethanol a possible source of glycine precursors in the interstellar medium? Pilar Redondo, Antonio Largo, and Carmen Barrientos Computational Chemistry Group, Departamento de Química Física y Química Inorgánica, Facultad de Ciencias, Universidad de Valladolid, 47011 Valladolid, Spain e-mail: [predondo;alargo;cbb]@qf.uva.es Received 18 May 2015 / Accepted 28 May 2015 ABSTRACT Context. One of the most interesting questions in interstellar chemistry concerns whether we can detect the basic building blocks of proteins in astronomical sources. In ascertaining whether amino acids could be possible interstellar molecules, a crucial point is how they could be synthesized in the interstellar medium. Aims. We do a theoretical study of the ion-molecule reaction involving protonated aminomethanol and formic acid to establish its viability in space. This ion-molecule reaction has been proposed by other authors as a possible way to produce glycine in the interstellar medium. Methods. The relevant stationary points on the potential energy surface of the reaction between protonated aminomethanol and formic acid have been theoretically studied by using ab initio methods. The second-order Moller-Plesset level was employed, in conjunction with the correlation-consistent polarized valence triple-zeta (cc-pVTZ) basis set. In addition, the electronic energies were refined by means of single-point calculations at the CCSD(T) level (coupled cluster single and double excitation model augmented with a non-iterative treatment of triple excitations) on the MP2/cc-pVTZ geometries with the aug-cc-pVTZ basis set.
    [Show full text]
  • Lis Full CV 2019
    Curriculum Vitae Dariusz C. (Darek) Lis Educa7on 1985 – 1989 University of MassachuseEs at Amherst, Department of Physics and Astronomy, Ph. D. 1981 – 1985 University of Warsaw, Department of Physics. Professional Experience 2019 – Scien7st, Jet Propulsion Laboratory, California Ins7tute of Technology. 2014 – 2019 Professor (Professeur des universités 1ère classe), Sorbonne University. Director, Laboratory for Studies of Radia7on and MaEer in Astrophysics and Atmospheres (UMR8112 — CNRS, Paris Observatory/PSL University, Sorbonne University, École normale supérieure, University of Cergy-Pontoise). 2009 – 2014 Deputy Director, Caltech Submillimeter Observatory. 1998 – 2015 Senior Research Associate in Physics (now Research Professor), California Ins7tute of Technology. 1992 – 1998 Senior Research Fellow in Physics (now Research Assistant Professor), California Ins7tute of Technology. 1989 – 1992 Research Fellow in Physics, California Ins7tute of Technology. 1985 – 1989 Research Assistant, University of MassachuseEs, Five College Radio Astronomy Observatory. Visi7ng Appointments 2015 – Visi7ng Associate in Physics, California Ins7tute of Technology. 2013 Visi7ng Professor (Professeur des universités 1ère classe invité), École normale supérieure. 2011 Visi7ng Associate Professor (Maître de conférences invité), University of bordeaux 1. 2007 Visi7ng Senior Astronomer (Astronome invité), Paris Observatory. 2003 Visi7ng Scien7st, Max Planck Ins7tut for Radio Astronomy. 1992 – 1994 Lecturer, University of California, Los Angeles. 1989 – 1991 Consultant (Postdoctoral Research Associate), Rensselaer Polytechnic Ins7tute. Awards 2014 NASA Group Achievement Award, U.S. Herschel HIFI Instrument Team. 2010 NASA Group Achievement Award, Herschel HIFI Hardware Development Team. 1985 Minister of Science and Higher Learning Fellowship, Poland. Research Astrophysics and astrochemistry of the interstellar medium, star forma7on. Evolu7on of molecular complexity in astrophysical environments. Vola7le composi7on of comets and the origin of Earth’s oceans.
    [Show full text]
  • Reaction of Several Aminopyrimidines with Formaldehyde Gerald L
    JOURNAL OF RESEARCH of the National Bureau of Standards—A. Physics and Chemistry Vol. 66A, No. 1, January-February 1962 Reaction of Several Aminopyrimidines With Formaldehyde Gerald L. McLeod x (August 29, 1961) Formaldehyde has been shown to react with 2-aminopyrimidine (II) and 2-(methyl- amino)pyrimidine (V) at room temperature to give the corresponding methylol derivatives or the corresponding methylenebis(aminopyrimidines). The reaction of formaldehyde with 2-amino-4,6-dichloro-5-methylpyrimidine (VII) and also its failure to react with 2-(dimethylamino)pyrimidine (IX) are cited as evidence that the pyrimidine ring is not involved in the reaction. 1. Introduction methylol structure is supported by infrared analysis. The spectrum of 2-aminopyrimidine has two absorp- A number of investigations have been made on the tion bands near 3,320 and 3,170 cm"11 whichih are melamine-formaldehyde reaction, and several mech- 2 attributed to N—H asymmetric and symmetriy c anisms [1-5] have been suggested. The complex stretching modes [9]; the methylol compoundd, IIIIII, structures of the triamino-l,3,5-triazines made it shows one fairly broad band at 3,225 cm"1. The desirable to study simpler model compounds. A occurrence of both inter- and intra-molecular hydro- logical model compound, 2-amino-l,3,5~triazine (la), gen bonding in III could cause a lowering of the OH has been reported [6-8] not to give the usual amine stretching frequency, allowing it to overlap the reactions because it tautomerizes to the iminoid N—H stretching band. Treatment of the methylol structure (Ib).
    [Show full text]
  • OH and NH Stretching Vibrational Relaxation of Liquid Ethanolamine
    Z. Phys. Chem. 225 (2011) 913–926 / DOI 10.1524/zpch.2011.0125 © by Oldenbourg Wissenschaftsverlag, München OH and NH Stretching Vibrational Relaxation of Liquid Ethanolamine ∗ By Stephan Knop, Jörg Lindner, and Peter Vöhringer Lehrstuhl für Molekulare Physikalische Chemie, Institut für Physikalische und Theoretische Chemie, Rheinische Friedrich-Wilhelms-Universität Bonn, Wegelerstraße 12, 53115 Bonn, Germany Dedicated to Prof. Horst Hippler on the occasion of his 65th birthday (Received April 12, 2011; accepted in revised form May 30, 2011) Vibrational Relaxation / Liquid Dynamics / Hydrogen-Bonding / Ultrafast Spectroscopy Femtosecond mid-infrared pump-probe spectroscopy was carried out to obtain information about the dynamics of vibrational energy relaxation in liquid ethanolamine at room temperature and ambient pressure. Through partial deuteration it was possible to disentangle the dynamics resulting from the OH and the NH stretching modes that proceed independently and simultaneously in the hydrogen-bonded liquid following an ultrafast vibrational excitation by a resonant mid-infrared pulse. The OH-stretching vibrational lifetime was determined to be 450 fs while the NH-stretching lifetime was found to be 1.2 ps. This large difference in lifetimes highlights the importance of the hydrogen-donating and the hydrogen-accepting character of the vibrating groups that are engaged in hydrogen-bonding. 1. Introduction Vibrational energy relaxation (VER) in molecular liquids has attracted considerable attention of researchers devoted to exploring condensed phase chemical dynamics. As- sociated molecular liquids have been particularly attractive research targets because the influence of hydrogen bonding (H-bonding) on the timescales and molecular mechan- isms of the various vibrational dynamical phenomena remains until today only partially understood [1–3].
    [Show full text]