Supplement of Measurement Report: Important Contributions of Oxygenated Compounds to Emissions and Chemistry of Volatile Organic Compounds in Urban Air

Total Page:16

File Type:pdf, Size:1020Kb

Supplement of Measurement Report: Important Contributions of Oxygenated Compounds to Emissions and Chemistry of Volatile Organic Compounds in Urban Air Supplement of Atmos. Chem. Phys., 20, 14769–14785, 2020 https://doi.org/10.5194/acp-20-14769-2020-supplement © Author(s) 2020. This work is distributed under the Creative Commons Attribution 4.0 License. Supplement of Measurement report: Important contributions of oxygenated compounds to emissions and chemistry of volatile organic compounds in urban air Caihong Wu et al. Correspondence to: Bin Yuan ([email protected]) and Min Shao ([email protected]) The copyright of individual parts of the supplement might differ from the CC BY 4.0 License. 24 1. Sensitivity of VOCs in PTR-MS 25 Proton-transfer-reaction time-of-flight mass spectrometry (PTR-TOF-MS) allows 26 the detection of a large number of VOCs in air through proton-transfer reaction with 27 H3O+ reagent ions and detection by a mass spectrometer. Measurement sensitivities can 28 be experimentally determined using calibration gases, but only the sensitivity of few 29 species can be obtained. For other species, the sensitivity can be calculated using the 30 rate constant for the proton-transfer reaction. 31 In PTR-ToF-MS, VOCs that have higher proton affinity than water will be ionized + 32 via proton transfer with H3O to produce the product ions. + + 33 VOC+H3O → VOC·H +H2O 34 According to the reaction rate equation, the concentration of VOC•H can be 35 calculated as follows: + 36 VOC·H=H3O 0(1-exp(-[VOC]∆)) + + 37 Where k is the reaction rate constant, [H3O ]0 is the signal of H3O ions before 38 reaction, [VOC] is the number concentration of the VOC in the drift tube, and Δt is the + 39 reaction time for H3O traversing the drift tube. + 40 It is assumed that only a small amount of H3O has proton transfer reaction with 41 VOCs, the concentration of VOC•H can be calculated as follows: + 42 VOC·HH3O [VOC]∆ + + 43 Where [H3O ] is the signal of H3O ions after the end of the drift tube. 44 Considering the possibility of fragmentation for the protonated ions, a term + + 45 VOC∙H can be introduced to represent the fraction of product ions detected as VOC•H + 46 ions (0 ≤VOC∙H ≤1). The concentration of VOC·H becomes + + 47 VOC·HH3O [VOC]∆VOC∙H + 48 The fraction of H3O that is converted into VOC·H+ ions can be expressed as: VOC·H + 49 + [VOC]∆VOC∙H H3O 50 The signal of VOC·H is related to the transmission efficiency: 51 VOC·H+ VOC·H×VOC·H+ 52 The factors VOC·H+ is the transmission efficiencies for VOC·H . These are 2 53 determined by (i) the extraction efficiency of ions from the drift tube into the mass 54 analyzer, (ii) the transmission efficiency of the analyzer, and (iii) the detection 55 efficiency of the detector for each mass (Sekimoto et al., 2017). 56 The measured sensitivity in PTR-TOF-MS is defined as the ion intensity of 57 VOC·H obtained at a volume-mixing ratio of 1 ppbv (parts per billion by volume; 58 10−9): + + VOC·H + VOC·H + 59 Sensitivity 10 ∆H3O VOC∙H VOC + 10 H3O 60 For a certain VOC, the sensitivity is linearly related to the reaction rate constant. 61 Eq.3 suggests that if the measured sensitivity is corrected for fragmentation and 62 transmission efficiencies, the resulting sensitivity is linearly dependent on the reaction 63 rate constant k. This means that sensitivity can be calculated from the rate constants. + 64 Corrected Sensitivity Sensitivity⁄ /VOC∙H 65 The transmission efficiency of ions is quantified by laboratory experiments. A 66 large variety of high concentrations of VOCs, including methanol, acetonitrile, 67 ethylamine, formic acid, acetone, pyrrole, furan, isoprene, MACR, DMF, 68 hydroxyacetone, phenol, furfural, styrene, benzaldehyde, cresol, guaiacol, naphthalene, 69 pinene, bromobenzene, iodobenzene, octamethylcyclotetrasiloxane (D4), 1,3- 70 diiodobenzene, decamethylcyclopentasiloxane (D5), are selected for introduction into 71 the PTR-ToF-MS, reagent ions are obviously consumed. The transmission efficiency 72 can be obtained according to the decrease of reagent ions and the increase of product 73 ions. Figure S7 shows the transmission efficiency curves based on laboratory 74 experiments. 75 The fragment ratio was obtained by using the relative proportions relationship 76 between the signal intensity of VOC and the fragment ions generated by its fracture at 77 the same time during the transmission efficiency experiment. The fragment ratio of 78 different VOCs are shown in Table S2. 79 2 Calculation of initial isoprene concentration 80 Isoprene is extremely reactive and therefore its concentration is poor to indicate 81 direct biogenic emissions. To correct this atmospheric photochemical loss, we 3 82 extrapolated the isoprene concentration back to the source using measurements of 83 isoprene and its photo-oxidized products, methyl vinyl ketone (MVK) and methacrolein 84 (MACR) (Karl et al., 2009). The reaction process of isoprene being oxidized by OH 85 radicals in the atmosphere is: 86 isoprene OH → 0.32MVK 0.23MACR 87 110 88 MVK OH → Products 1.910 89 MACR OH → Products 3.310 . 90 1 ∆ 1 ∆ (1) 91 From the measured ratio between MVK + MACR and isoprene, the OH exposure 92 since emission can be determined, and the observed isoprene concentration can be 93 extrapolated back to the source(Figure S8c). 94 ∆ (2) 95 Here, we used the measured concentrations from online GC-MS/FID for isoprene, 96 as there are substantial interferences for PTR-TOF measurements of isoprene in urban 97 air (Yuan et al., 2017). MVK+MACR was only measured by PTR-ToF-MS. We 98 observed significant elevation of MVK+MACR concentrations in the evening when the 99 primary emissions are highest, indicating MVK+MACR concentrations measured by 100 PTR-ToF-MS are influenced by primary anthropogenic emissions (e.g. traffic), either 101 due to direct emissions of MVK or MACR from vehicles, or potential interferences 102 from other compounds that are emitted by vehicles. The data during the night time (20: 103 00-6: 00) was selected to determine the emission ratio of MVK + MACR relative to CO 104 (Figure S8a). MVK+MACR concentrations that are solely from biogenic sources can 105 be estimated by the following Eq. 3: 106 (3) 107 Where and are the concentration of MVK+MACR and 108 CO, respectively. is the tropospheric background of CO (100 ppb). -4 109 is the emission ratio of MVK+MACR versus CO (6.0×10 ppb [ppb 110 CO]-1). 4 111 3 Calculation of photolysis rates 112 To estimate photolysis rates for OVOCs, we follow the method in de Gouw et al. 113 (2018). It is assumed that the photolysis rates for all OVOCs are reduced relative to 114 their clear-sky rates by the same factor as for jNO2 and use the following equation: 115 (4) 、 116 Where are clear-sky photolysis rates of OVOC 117 and NO2, respectively. Clear-sky photolysis rates for different compounds are 118 calculated in this study from the parameterization used in the Master Chemical 119 Mechanism v3.3.1 (Saunders et al., 2003): 120 lcos sec (5) 121 Where χ is the solar zenith angle and l, m, and n are parameters listed for different 122 photolysis rates. The photolysis rates of NO2, H2O2, and HCHO were measured on-site 123 using a PFS-100 Photolysis Spectrometer (Focused Photonics Inc.) during the 124 campaign. The above methods were used to calculate the photolysis rates of H2O2 and 125 HCHO, and compared with the measurements. It is found that the calculated values 126 show good agreement with the measurements for the two compounds (Figure S9). 127 Based on this, the photolysis frequencies of other OVOCs were calculated and then the 128 corrections to the rate constants of OH reaction for these OVOCs were estimated based 129 on Eq. 3 in the main text. 130 5 131 Table S1. Sensitivities of PTR-ToF-MS for various VOC species calibrated with 132 standard gas and Liquid Calibration Unit (LCU). VOC species Ion formula Sensitivity, cps/ppb Species calibrated with gas standard + Formaldehyde CH2OH 1042 + Methanol CH4OH 629.3 + Acetonitrile C2H3NH 3374 + Acetaldehyde C2H4OH 2767 + Ethanol C2H6OH 99.23 + Acrolein C3H4OH 4107 + Acetone C3H6OH 4299 + Furan C4H4OH 2544 + Isoprene C5H8H 1888 + MVK C4H6OH 3868 + MEK C4H8OH 4467 + Benzene C6H6H 3151 + 2-Pentanone C5H10OH 4510 + Toluene C7H8H 3978 + Phenol C6H6OH 4076 + Furfural C5H4O2H 7460 + Methyl Isobutyl Ketone C6H12OH 3988 + Styrene C8H8H 4289 + O-xylene C8H10H 4241 + m-Cresol C7H8OH 4299 + 1,2,4-Teimethylbenzene C9H12H 4413 + Naphthalene C10H8H 5117 + a-Pinene C10H16H 2332 Species calibrated with the Liquid Calibration Unit (LCU). + Formic acid CH2O2H 856.6 + Acetic acid C2H4O2H 1711 6 + Propionic acid C3H6O2H 2072 + Butyric acid C4H8O2H 2358 + Pyrrole C4H5NH 2842 + Formamide CH3NOH 2871 + Acetamide C2H5NOH 3992 133 134 7 135 Table S2. The fraction of product ions detected as VOC•H+ ions for different VOCs. + VOC species Ion formula VOC∙H + Formaldehyde CH2OH 1 + Methanol CH4OH 1 + Acetonitrile C2H3NH 1 + Acetaldehyde C2H4OH 1 + Ethanol C2H6OH 1 + Acrolein C3H4OH 1 + Acetone C3H6OH 0.97 + Furan C4H4OH 1 + Isoprene C5H8H 0.87 + MVK C4H6OH 0.62 + MEK C4H8OH 0.87 + Benzene C6H6H 1 + 2-Pentanone C5H10OH 0.94 + Toluene C7H8H 1 + Phenol C6H6OH 1 + Furfural C5H4O2H 1 + Styrene C8H8H 1 + O-xylene C8H10H 1 + m-Cresol C7H8OH 1 + 1,2,4-Teimethylbenzene C9H12H 1 + Naphthalene C10H8H 1 + a-Pinene C10H16H 0.62 136 137 8 138 Table S3. Rate constants of OVOCs representing the combined loss to OH oxidation 139 and photolysis. ∗ jOVOC/[OH] f Species 10−12 cm3 molecule-1 s-1 Formaldehyde 9.4 7.86±0.120 17.26 1.84 Acetaldehyde 15 0.426±0.006 15.42 1.03 Propionaldehyde 20 1.89±0.026 21.89 1.09 n-butyraldehyde 24 3.26±0.046 27.26 1.14 i-butyraldehyde 24 5.64±0.080 29.64 1.24 MACR 29 1.99±0.030 30.99 1.07 Acetone 0.17 0.051±0.0007 0.22 1.29 MEK 1.22 0.368±0.005 1.59 1.30 MVK 20 3.22±0.049 23.22 1.16 Glyoxal 11 3.02±0.044 14.02 1.27 Methyl peroxide 5.5 0.628±0.009 6.13 1.11 Methyl nitrate 0.023 0.107±0.001 0.13 5.65 Ethyl nitrate 0.18 0.122±0.002 0.30 1.67 n-Propyl nitrate 0.58 0.163±0.002 0.74 1.28 i-Propyl nitrate 0.29 0.28±0.004 0.57 1.97 t-butyl nitrate 1.6 0.818±0.011 2.42 1.51 140 f represents the ratio of the rate constant representing the combined losses of reaction ∗ 141 with OH radical and photolysis () and the OH rate constant ().
Recommended publications
  • Interstellar Ices and Radiation-Induced Oxidations of Alcohols
    The Astrophysical Journal, 857:89 (8pp), 2018 April 20 https://doi.org/10.3847/1538-4357/aab708 © 2018. The American Astronomical Society. All rights reserved. Interstellar Ices and Radiation-induced Oxidations of Alcohols R. L. Hudson and M. H. Moore Astrochemistry Laboratory, NASA Goddard Space Flight Center, Greenbelt, Maryland, 20771, USA; [email protected] Received 2017 May 2; revised 2018 March 8; accepted 2018 March 9; published 2018 April 18 Abstract Infrared spectra of ices containing alcohols that are known or potential interstellar molecules are examined before and after irradiation with 1 MeV protons at ∼20 K. The low-temperature oxidation (hydrogen loss) of six alcohols is followed, and conclusions are drawn based on the results. The formation of reaction products is discussed in terms of the literature on the radiation chemistry of alcohols and a systematic variation in their structures. The results from these new laboratory measurements are then applied to a recent study of propargyl alcohol. Connections are drawn between known interstellar molecules, and several new reaction products in interstellar ices are predicted. Key words: astrochemistry – infrared: ISM – ISM: molecules – molecular data – molecular processes 1. Introduction 668 cm−1 was produced in solid propargyl alcohol’sIR spectrum after the compound was irradiated with 2 keV Interstellar ices are now recognized as an important comp- electrons (Sivaraman et al. 2015, hereafter SMSB from the onent of the interstellar medium (ISM). The results of multiple coauthors final initials). That IR peak was assigned to benzene infrared (IR) surveys have led to over a dozen assignments of (C H ), which was said “to be the major product from spectral features to molecular ices, with the more abundant 6 6 propargyl alcohol irradiation.” However, a full mid-IR interstellar ices being H O, CO, and CO (Boogert et al.
    [Show full text]
  • Accurate Enthalpies of Formation of Astromolecules: Energy, Stability and Abundance
    Accurate Enthalpies of Formation of Astromolecules: Energy, Stability and Abundance Emmanuel E. Etim and Elangannan Arunan* Inorganic and Physical Chemistry Department, Indian Institute of Science Bangalore, India-560012 *email: [email protected] ABSTRACT: Accurate enthalpies of formation are reported for known and potential astromolecules using high level ab initio quantum chemical calculations. A total of 130 molecules comprising of 31 isomeric groups and 24 cyanide/isocyanide pairs with atoms ranging from 3 to 12 have been considered. The results show an interesting, surprisingly not well explored, relationship between energy, stability and abundance (ESA) existing among these molecules. Among the isomeric species, isomers with lower enthalpies of formation are more easily observed in the interstellar medium compared to their counterparts with higher enthalpies of formation. Available data in literature confirm the high abundance of the most stable isomer over other isomers in the different groups considered. Potential for interstellar hydrogen bonding accounts for the few exceptions observed. Thus, in general, it suffices to say that the interstellar abundances of related species are directly proportional to their stabilities. The immediate consequences of this relationship in addressing some of the whys and wherefores among astromolecules and in predicting some possible candidates for future astronomical observations are discussed. Our comprehensive results on 130 molecules indicate that the available experimental enthalpy
    [Show full text]
  • Exhaustive Product Analysis of Three Benzene Discharges by Microwave Spectroscopy Michael C
    pubs.acs.org/JPCA Article Exhaustive Product Analysis of Three Benzene Discharges by Microwave Spectroscopy Michael C. McCarthy,* Kin Long Kelvin Lee, P. Brandon Carroll, Jessica P. Porterfield, P. Bryan Changala, James H. Thorpe, and John F. Stanton Cite This: J. Phys. Chem. A 2020, 124, 5170−5181 Read Online ACCESS Metrics & More Article Recommendations *sı Supporting Information ABSTRACT: Using chirped and cavity microwave spectroscopies, automated double resonance, new high-speed fitting and deep learning algorithms, and large databases of computed structures, the discharge products of benzene alone, or in combination with molecular oxygen or nitrogen, have been exhaustively characterized between 6.5 and 26 GHz. In total, more than 3300 spectral features were observed; 89% of these, accounting for 97% of the total intensity, have now been assigned to 152 distinct chemical species and 60 of their variants (i.e., isotopic species and vibrationally excited states). Roughly 50 of the products are entirely new or poorly characterized at high resolution, including many heavier by mass than the precursor benzene. These findings provide direct evidence for a rich architecture of two- and three-dimensional carbon and indicate that benzene growth, particularly the formation of ring−chain molecules, occurs facilely under our experimental conditions. The present analysis also illustrates the utility of microwave spectroscopy as a precision tool for complex mixture analysis, irrespective of whether the rotational spectrum of a product species is known a priori or not. From this large quantity of data, for example, it is possible to determine with confidence the relative abundances of different product masses, but more importantly the relative abundances of different isomers with the same mass.
    [Show full text]
  • One-Step Synthesis of Pyridines and Dihydro- Pyridines in a Continuous Flow Microwave Reactor
    One-step synthesis of pyridines and dihydro- pyridines in a continuous flow microwave reactor Mark C. Bagley*1, Vincenzo Fusillo2, Robert L. Jenkins2, M. Caterina Lubinu2 and Christopher Mason3 Full Research Paper Open Access Address: Beilstein J. Org. Chem. 2013, 9, 1957–1968. 1Department of Chemistry, School of Life Sciences, University of doi:10.3762/bjoc.9.232 Sussex, Falmer, Brighton, East Sussex, BN1 9QJ, UK, 2School of Chemistry, Main Building, Cardiff University, Park Place, Cardiff, Received: 05 July 2013 CF10 3AT, UK and 3CEM Microwave Technology Ltd, 2 Middle Slade, Accepted: 11 September 2013 Buckingham, MK18 1WA, UK Published: 30 September 2013 Email: This article is part of the Thematic Series "Chemistry in flow systems III". Mark C. Bagley* - [email protected] Guest Editor: A. Kirschning * Corresponding author © 2013 Bagley et al; licensee Beilstein-Institut. Keywords: License and terms: see end of document. Bohlmann–Rahtz; continuous flow processing; ethynyl ketones; flow chemistry; Hantzsch dihydropyridine synthesis; heterocycles; microwave synthesis; multicomponent reactions; pyridine synthesis Abstract The Bohlmann–Rahtz pyridine synthesis and the Hantzsch dihydropyridine synthesis can be carried out in a microwave flow reactor or using a conductive heating flow platform for the continuous processing of material. In the Bohlmann–Rahtz reaction, the use of a Brønsted acid catalyst allows Michael addition and cyclodehydration to be carried out in a single step without isolation of intermediates to give the corresponding trisubstituted pyridine as a single regioisomer in good yield. Furthermore, 3-substituted propargyl aldehydes undergo Hantzsch dihydropyridine synthesis in preference to Bohlmann–Rahtz reaction in a very high yielding process that is readily transferred to continuous flow processing.
    [Show full text]
  • The Interactions and Reactions of Atoms and Molecules on the Surfaces of Model Interstellar Dust Grains
    The Interactions and Reactions of Atoms and Molecules on the Surfaces of Model Interstellar Dust Grains A thesis submitted for the degree of Doctor of Philosophy Helen Jessica Kimber Department of Chemistry University College London 2016 -I, Helen Jessica Kimber, confirm that the work presented in this thesis is my own. Where information has been derived from other sources, I confirm that this has been indicated in the thesis. Signed, i Abstract The elemental composition of the known universe comprises almost exclusively light atoms (~99.9% hydrogen and helium). However, to date, close to 200 different molecules have been detected in the interstellar medium (ISM) where their distribution is far from uniform. The vast majority of these molecules are contained within vast clouds of gas and dust referred to as interstellar clouds. Within these interstellar clouds, many of the molecules present are formed via gas-phase ion-neutral reactions. However, there are several molecules for which known gas-phase kinetics cannot account for observed gas-phase abundances. As a result, reactions occurring on the surface of interstellar dust grains are invoked to account for the observed abundances of some of these molecules. This thesis presents results of experimental investigations into the interaction and reactions of atoms and molecules on the surface of model interstellar dust grains. Chapters three and four present results for the reaction of (3P)O on molecular ices. Specifically, the reaction of (3P)O and propyne or acrylonitrile. After a one hour dosing period, temperature programmed desorption (TPD), coupled with time-of-flight mass spectrometry (TOFMS), are used to identify (3P)O addition products.
    [Show full text]
  • Reduced Pressure Oxidation of Propargyl Alcohol to Aldehyde; Propynal
    Reduced pressure oxidation of propargyl alcohol to aldehyde; Propynal Nov 15, 2013 John MacMillan ([email protected]) Chemicals Used Propargyl alcohol, 99%, Aldrich, P5,080-3, redistilled Chromium (VI) oxide, 99+%, Aldrich, 20,782-9 Sodium Chloride, 99%*%, A.C.S. reagent, Aldrich, 22,351-4 Sulfuric acid, 95-98%, A.C.S. Reagent, Aldrich, 25.810-5 Procedure This material was prepared by a modification of the Organic Synthesis procedure. See lead reference. To a 2 liter three neck flask, equipped with a mechanical stirrer, and ice/salt bath was charged 120 g ((2.14 mole) redistilled propargyl alcohol and 240 ml of water. To this mixture was then added a cooled solution of 135 ml concentrated sulfuric acid in 150 ml of water. A "Y" tube was inserted in one neck of the flask and a pressure equalized dropping funnel was placed in one neck of the "Y" tube. The other neck of the "Y" tube lead to two traps, in series, which in turn were connected to a McLeod pressure gage and vacuum pump. The third neck of the flask was connected to a fine capillary which served as a nitrogen inlet. A cooled solution of 210 g chromium trioxide, 200 ml of water and 100 ml concentrated sulfuric acid was then added to the dropping funnel. One trap was cooled to ~ - 10° with an ice/salt mixture and the second trap was cooled with a dry ice/acetone bath to ~ -78°C. The exterior of the 2 liter flask was cooled to ~ - 10°C with ice/salt.
    [Show full text]
  • Signature Redacted Signature of the Author - Mark N
    PHOTOPHYSICS OF INFRARED MULTIPHOTON ABSORPTION BY THIOPHOSGENE by MARK NELSON SPENCER B.A., University of Pennsylvania (1978) SUBMITTED TO THE DEPARTMENT OF CHEMISTRY IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY at the MASSACHUSETTS INSTITUTE OF TECHNOLOGY DECEMBER 1982 c Massachusetts Institute of Technology Signature redacted Signature of the Author - Mark N. Spencer Signature redacted Department of Chemistry Certified by Jeffrey I. Steinfeld Thesis Supervisor Signature redacted Accepted by Glenn A. Berchtold Chairman, Depa rtmental Committee ArchJWjg MASSACFWCTTS INSTITUR OF CNOLO9y MAR 3 1 1983 LIBRARIES This doctoral thesis has been examined by a Committee of the Department of Chemistry as follows: redacted Professor Robert J. Silbey ,Signature Chairman Professor Jeffrey I. Steinfeld __ ___ __ __ ___ __ __ Signature redactedF-Thesis Supervisor Signature redacted Professor Robert W. Field, 2 PHOTOPHYSICS OF INFRARED MULTIPHOTON ABSORPTION BY THIOPHOSGENE by MARK NELSON SPENCER Submitted to the Department of Chemistry on December , 1982 in partial fulfillment of the requirements for the Degree of Doctor of Philosophy in Chemistry ABSTRACT Infrared-visible double resonance experiments were done on thiophosgene under collisionless conditions and in a bulb to determine the dynamics of infrared multiphoton absorption in its sparse density of states region. In the absence of collisions thiophosgene absorbs at all excitation frequencies. Measurements of the ground state depletion as a function of C0 2 laser frequency do not correlate at all with the conventional infrared absorption spectrum. At excitation frequencies coincident with the v 4 overtone, no population build-up is observed in excited states of the 2v 4 manifold.
    [Show full text]
  • 27 May 2021 Given by Tercero Et Al
    Astronomy & Astrophysics manuscript no. aa41297 ©ESO 2021 May 28, 2021 Letter to the Editor The sulphur saga in TMC-1: Discovery of HCSCN and HCSCCH ? J. Cernicharo1, C. Cabezas1, Y. Endo2, M. Agúndez1, B. Tercero3; 4, J. R. Pardo1, N. Marcelino1, P. de Vicente3 1 Grupo de Astrofísica Molecular, Instituto de Física Fundamental (IFF-CSIC), C/ Serrano 121, 28006 Madrid, Spain e-mail: [email protected],[email protected] 2 Department of Applied Chemistry, Science Building II, National Yang Ming Chiao Tung University, 1001 Ta-Hsueh Rd., Hsinchu 30010, Taiwan 3 Centro de Desarrollos Tecnológicos, Observatorio de Yebes (IGN), 19141 Yebes, Guadalajara, Spain 4 Observatorio Astronómico Nacional (IGN), C/Alfonso XII, 3, 28014, Madrid, Spain Received; accepted ABSTRACT We report the detection, for the first time in space, of cyano thioformaldehyde (HCSCN) and propynethial (HCSCCH) towards the starless core TMC-1. Cyano thioformaldehyde presents a series of prominent a- and b-type lines, which are the strongest previously unassigned features in our Q-band line survey of TMC-1. Remarkably, HCSCN is four times more abundant than cyano formaldehyde (HCOCN). On the other hand, HCSCCH is five times less abundant than propynal (HCOCCH). Surprisingly, we find an abundance ratio HCSCCH/HCSCN of ∼ 0.25, in contrast with most other ethynyl-cyanide pairs of molecules for which the CCH-bearing species is more abundant than the CN-bearing one. We discuss the formation of these molecules in terms of neutral-neutral reactions of S atoms with CH2CCH and CH2CN radicals as well as of CCH and CN radicals with H2CS.
    [Show full text]
  • 31295005227565.Pdf (11.48Mb)
    VIBRATIONAL ANALYSIS AND AB INITIO STUDIES OF PROPIOLIC ACID by EDMUND MOSES NSO NDIP, B.S., M.S. A DISSERTATION IN CHEMISTRY Submitted to the Graduate Faculty of Texas Tech University in Partial Fulfillment of the Requirements for the Degree of DOCTOR OF PHILOSOPHY Approved August, 1987 ACKNOWLEDGEMENTS My educational experiences at Texas Tech University have been very rewarding and along the way, I have had the good fortune of being associated with a lot of people. Consequently, I am indebted to them and wish to express my sincere gratitude for their help. First of all, I wish to thank Professor R. L Redington, my research mentor, for his ever enduring support, guidance and patience throughout the course of my study. My special thanks also go to Professor R. E. Wilde, Jr. for his friendship throughout the years. To the members of my committee, I say thank you for your patience. My thanks also go to Dr. J. L Mills, Dr. R. D. Larsen, and Dr. Jim Liang and his associates at the University of Utah, Chemistry Department. I do recognize here the goodwill of Prof. Josef MichI of the University of Texas at Austin (formerly of the University of Utah). Financial support was received from Texas Tech University and the Robert Welch Foundation. I must thank the government and people of Cameroon for the scholarships given me throughout the many years of my education. To my kids, Edmund, Jr. and Laura, I say thanks for the smiles throughout the difficult moments that we all shared. I especially thank my wife, Grace Manyi Ndip, for the sacrifices she has made over the years and for her help in preparing parts of this dissertation.
    [Show full text]
  • The Interstellar Chemistry of H2C3O Isomers
    The interstellar chemistry of H2C3O isomers. Jean-Christophe Loison1,2*, Marcelino Agúndez3, Núria Marcelino4, Valentine Wakelam5,6, Kevin M. Hickson1,2, José Cernicharo3, Maryvonne Gerin7, Evelyne Roueff8, Michel Guélin9 *Corresponding author: [email protected] 1 Univ. Bordeaux, ISM, UMR 5255, F-33400 Talence, France 2 CNRS, ISM, UMR 5255, F-33400 Talence, France 3 Instituto de Ciencia de Materiales de Madrid, CSIC, C\ Sor Juana Inés de la Cruz 3, 28049 Cantoblanco, Spain 4 INAF, Osservatorio di Radioastronomia, via P. Gobetti 101, 40129 Bologna, Italy 5 Univ. Bordeaux, LAB, UMR 5804, F-33270, Floirac, France. 6 CNRS, LAB, UMR 5804, F-33270, Floirac, France 7 LERMA, Observatoire de Paris, École Normale Supérieure, PSL Research University, CNRS, UMR8112, F-75014, Paris, France 8 LERMA, Observatoire de Paris, PSL Research University, CNRS, UMR8112, Place Jules Janssen, 92190 Meudon, France 9 Institut de Radioastronomie Millimétrique, 300 rue de la Piscine, 38046, St. Martin d’Heres, France We present the detection of two H2C3O isomers, propynal and cyclopropenone, toward various starless cores and molecular clouds, together with upper limits for the third isomer propadienone. We review the processes controlling the abundances of H2C3O isomers in interstellar media showing that the reactions involved are gas-phase ones. We show that the abundances of these species are controlled by kinetic rather than thermodynamic effects. 1 Introduction The formation of Complex Organic Molecules (COMs) in interstellar media, particularly in dense molecular clouds, is a challenging issue. Until recently, the paradigm has been that COMs were formed on grains through surface chemistry (Tielens & Hagen 1982) and then released into the gas-phase in warm environments through thermal desorption (Herbst & Van Dishoeck 2009).
    [Show full text]
  • Nomination Background: Propargyl Alcohol (CASRN: 107-19-7)
    SUMMARY OF DATA FOR CHEMICAL SELECTION PROPARGYL ALCOHOL CAS No. 107-19-7 BASIS OF NOMINATION TO THE CSWG The nomination of propargyl alcohol to the CSWG is based on high production volume, exposure potential, and suspicion of potential carcinogenicity. Dr. Elizabeth Weisburger, a member of the American Conference of Governmental Industrial Hygienists (ACGIH) TLV Committee as well as the Chemical Selection Working Group (CSWG), provided a list of 281 chemical substances with ACGIH recommended TLVs for which there were no long-term studies cited in the supporting data and no designations with respect to carcinogenicity. She presented the list to the Chemical Selection Planning Group (CSPG) for evaluation as chemicals which may warrant chronic testing; it was affirmed at the CSPG meeting held on August 9, 1994, that the 281 "TLV Chemicals" be reviewed as a Class Study. As a result of the class study review, propargyl alcohol is presented as a candidate for testing by the National Toxicology Program because of: • potential for occupational exposures based on moderately high production volume • evidence of occupational exposures based on TLV and other literature documentation • potential for human exposures based on hazardous waste occurrences in environmental media • suspicion of carcinogenicity based on mixed results in available short-term assays for genetic toxicity and liver and kidney changes in subchronic mammalian toxicity studies • lack of chronic toxicity data. Sources of human exposure to propargyl alcohol are mainly occupational; and the exposure potential is considered moderate based on an estimated U.S. annual production volume range of 0.5 to 2.8 million pounds, an estimate of 54,358 worker exposures (19,933 female) reported in the NOES database, and characterization of propargyl alcohol as a moderately volatile liquid identified in air, water, and soil.
    [Show full text]
  • The Complex Chemistry of Outflow Cavity Walls Exposed: the Case Of
    Mon. Not. R. Astron. Soc. 000, 1–21 (2015) Printed 18 June 2018 (MN LATEX style file v2.2) The complex chemistry of outflow cavity walls exposed: the case of low-mass protostars Maria N. Drozdovskaya1⋆, Catherine Walsh1, Ruud Visser2, Daniel Harsono1,3 and Ewine F. van Dishoeck1,4 1 Leiden Observatory, P.O. Box 9513, 2300 RA, Leiden, The Netherlands 2 European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany 3 SRON Netherlands Institute for Space Research, P.O. Box 800, 9700 AV Groningen, The Netherlands 4 Max-Planck-Institut f¨ur Extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany Accepted 2015 May 20. Received 2015 May 7; in original form 2015 March 18 ABSTRACT Complex organic molecules are ubiquitous companions of young low-mass protostars. Recent observations suggest that their emission stems, not only from the traditional hot corino, but also from offset positions. In this work, 2D physicochemical modelling of an envelope-cavity system is carried out. Wavelength-dependent radiative transfer calculations are performed and a comprehensive gas-grain chemical network is used to simulate the physical and chemical structure. The morphology of the system delineates three distinct regions: the cavity wall layer with time-dependent and species-variant enhancements; a torus rich in complex organic ices, but not reflected in gas-phase abundances; and the remaining outer envelope abundant in simpler solid and gaseous molecules. Strongly irradiated regions, such as the cavity wall layer, are subject to frequent photodissociation in the solid phase. Subsequent recombination of the photoproducts leads to frequent reactive desorption, causing gas-phase enhancements of several orders of magnitude.
    [Show full text]