Wet-Dry Cycles Enable the Parallel Origin of Canonical and Non-Canonical Nucleosides by Continuous Synthesis

Total Page:16

File Type:pdf, Size:1020Kb

Wet-Dry Cycles Enable the Parallel Origin of Canonical and Non-Canonical Nucleosides by Continuous Synthesis ARTICLE DOI: 10.1038/s41467-017-02639-1 OPEN Wet-dry cycles enable the parallel origin of canonical and non-canonical nucleosides by continuous synthesis Sidney Becker 1, Christina Schneider 1, Hidenori Okamura1, Antony Crisp 1, Tynchtyk Amatov 1, Milan Dejmek2 & Thomas Carell 1 1234567890():,; The molecules of life were created by a continuous physicochemical process on an early Earth. In this hadean environment, chemical transformations were driven by fluctuations of the naturally given physical parameters established for example by wet–dry cycles. These conditions might have allowed for the formation of (self)-replicating RNA as the fundamental biopolymer during chemical evolution. The question of how a complex multistep chemical synthesis of RNA building blocks was possible in such an environment remains unanswered. Here we report that geothermal fields could provide the right setup for establishing wet–dry cycles that allow for the synthesis of RNA nucleosides by continuous synthesis. Our model provides both the canonical and many ubiquitous non-canonical purine nucleosides in parallel by simple changes of physical parameters such as temperature, pH and concentration. The data show that modified nucleosides were potentially formed as competitor molecules. They could in this sense be considered as molecular fossils. 1 Center for Integrated Protein Science Munich CiPSM at the Department of Chemistry, Ludwig-Maximilians-Universität München, 81377 Munich, Germany. 2 Institute of Organic Chemistry and Biochemistry ASCR, 16610 Prague 6, Czech Republic. Correspondence and requests for materials should be addressedto T.C. (email: [email protected]) NATURE COMMUNICATIONS | (2018) 9:163 | DOI: 10.1038/s41467-017-02639-1 | www.nature.com/naturecommunications 1 ARTICLE NATURE COMMUNICATIONS | DOI: 10.1038/s41467-017-02639-1 he molecules of life originated around 4 billion years ago Herein, we report a robust synthetic pathway, which is purely under conditions governed by the composition of the based on fluctuations of physicochemical parameters such as pH, T ’ 1, 2 – Earth s crust and atmosphere at that time . Molecules concentration, and temperature, driven by wet dry cycles. These such as nucleic acids and amino acids must have formed by a fluctuations enable the direct enrichment or purification of all continuous physicochemical process, in which greater structural reaction intermediates that are directly used for the next synthetic complexity was generated based on fluctuations of the naturally steps. As such, a continuous synthesis is established. Our results given physical parameters3. Geothermal fields, for example, could show that RNA building blocks can indeed be formed in a pre- have established such fluctuations by wet–dry cycles that may biotically plausible geochemical environment without sophisti- have driven chemical transformations, which ultimately allowed cated isolation and purification procedures. The chemical – the emergence of life4 8. The appearance of (self)-replicating scenario presented here supports the hypothesis that life may RNA was certainly of central importance for the transition from have originated in a hydrothermal milieu on land rather than in a – an abiotic world to biology9 11. We need to consider, however, deep sea environment. The key assembly step in our pathway is that an early genetic polymer might have been structurally dif- the formation of variously substituted 5-nitroso-pyrimidines ferent from contemporary RNA. This involves differences (nitrosoPys) that can be converted into formamidopyrimidines regarding the sugar configuration (e.g., pyranosyl RNA) or the (FaPys) in the presence of formic acid and elementary metals (Ni presence of other nucleobases12, 13. Selection pressure led in this or Fe). When combined with ribose, the FaPy compounds react to scenario to the chemical evolution of RNA. Contemporary RNA give a set of purine nucleosides. This chemical pathway delivers molecules contain four canonical nucleosides (A, G, C, U), which not only the canonical purine nucleosides but concomitantly establish the sequence information. In addition, >120 non- many of the ubiquitously present non-canonical relatives, sug- canonical nucleosides are present, which govern a diverse set of gesting their origin as prebiotic competitor nucleosides (A, ms2A, 14 2 2 2 1 properties such as correct folding, e.g., to enable catalysis .In m A, DA, G, m G, m 2G, m G). Since chemical evolution fact, the genetic system of all known life is dependent on modified depended on those molecules that were available on early Earth, nucleosides. Many of these non-canonical nucleosides are found these non-canonical nucleosides may be considered to be mole- today in all three domains of life, which indicates that they were cular fossils, which maintained their essential life-supporting present early on during the development of life. For the ubiqui- character until the present day. tous non-canonical nucleosides we may assume that they were already formed as competitors in parallel with the canonical ones on the early Earth15. So far, however, a geochemical scenario that Results would allow for the parallel formation of canonical and non- Selective crystallization of an organic salt. The chemical sce- canonical RNA building blocks by a continuous process is not nario that leads to a continuous synthesis of RNA building blocks known. All reported multistep chemical models so far rely on by just fluctuations of physical parameters is shown in Figs. 1 and tightly controlled laboratory conditions and the isolation and 2a. The scenario starts with an aqueous solution of malononitrile purification of central reaction intermediates by sophisticated – 1 and different amidinium salts 2a-d (HCl or H2SO4 salts, 400 methods1, 16 19. mM), both recognized prebiotic compounds18. In addition, River landscape in a geothermal environment OH O CO2 + H2O O O Sugar HO OH formation H H OH OH R1 Ribose H O R2 CO 2 N N 2 O Hydrolysis O CH4 N N R3 H2N H HO H N2 Ribose H2O 1 H R N N NH 2 6a-h Atmosphere CO O N R 2 N2 + CH4 HCN N 1 Pool of RNA H2S H2N R N2 3 building blocks NH H2N N R 3 H2N N 2a-d 5a-h Malononitrile and Formamido- Reduction amidine derivatives pyrimidine (FaPy) 0.5 N2 + CO2 1 O NH OR HNO 2 Day-night Wet 2 N N R2 in H2O NaNO2 or seasonal N Dry HNO / NaNO H NR CO NO 3 3 2 cycles N N 2a-d H N N R3 NaNO2 3 2 4a-i Organic salt Nitrosopyrimidine (nitrosoPy) Fig. 1 RNA nucleoside formation pathway. A geothermal environment provides the right set up for the depicted transformations by establishing wet–dry cycles. The prebiotic starting materials are produced from a prebiotic atmosphere and washed into an aqueous environment (e.g. by rain). Major atmospheric components are written in larger letters, whereas minor components are written in smaller letters. Transformations are taking place in different environments, illustrated by various rivers (in light blue). Each environment provides the right setup for different chemistries, leading to several different chemical transformations. This geochemical setup leads to a set of canonical and non-canonical RNA building blocks by continuous synthesis (6a, 1 1 2 3 2 1 2 3 1 2 3 2 1 2 3 2 1 m G: R = O, R = Me, R = NH2; 6b,ms A: R = NH, R = H, R = SMe; 6c,A:R = NH, R = H, R = H; 6d,m G: R = O, R = H, R = NHMe; 6e,m 2G: R = 2 3 1 2 3 1 2 3 2 1 2 3 O, R = H, R = N(Me)2; 6f,G:R = O, R = H, R = NH2; 6g, DA: R = NH, R = H, R = NH2; 6h,mA: R = NH, R = H, R = Me) 2 NATURE COMMUNICATIONS | (2018) 9:163 | DOI: 10.1038/s41467-017-02639-1 | www.nature.com/naturecommunications NATURE COMMUNICATIONS | DOI: 10.1038/s41467-017-02639-1 ARTICLE a Temperature pH Crystalized Crystalized 4g-i Mixture of Organic salt Selective One-pot prebiotic formation hydrolysis of R3 conversion molecules O NH Aminolysis to FaPys N R2 of R1 = SMe, N R3 3 2 Hot R = O R Basic 1 N H2N N R N R3 R1 4a-d O N N N R2 N O 70 °C O 3 pH 7 1 R OH 3 H2N N R O R 2 NH2 2 HN R OH OH O– N R N N N H2N R 1 1 H2N N R 2a-d H2N N R N N 5a-h O 4b-f Cold 3 N N – Acidic S O 4b-d, 4f Nucleoside Na+ NO – O 2 OH Solid state formation O Cl– NH nitroso-pyrimidine upon ribose OH formation condensation H2N R Complexity b Physical enrichment I pH ~ 4 T = 45 °C pH ~ 4 T = 8 °C – NH NO2 O 2b, R = SMe H2N R OH 2a-d 2a, R = NHMe Na+ N N 1 Dry O– N Cl– O 2c, R = NH O– 2 S N N NH2 O OH 3 H2N R 2a-d Dilute prebiotic mixture Crystal formation 2d, R = Me Fig. 2 Chemical complexity created by physical fluctuations. a Relative changes of temperature (in blue) and pH (in red) are shown for each synthetic step for the continuous synthesis of purine RNA building blocks from small organic and inorganic molecules. Several wet–dry cycles establish fluctuations of the depicted physical parameters that enable the physical enrichment of intermediates. Gray backgrounds denote compounds that are enriched by crystallization from an aqueous solution. b Formation of an organic salt consisting of amidine derivatives 2a-d and (hydroxyimino)malononitrile 3. The salt is selectively crystalized by concentrating a dilute mixture of organic and inorganic compounds by slow evaporation. The crystal structures of the four crystalized organic salts are depicted (Supplementary Tables 1–4) sodium nitrite and acetic acid are present to establish a slightly The robustness and ease of crystallization establishes a first acidic pH of around 4.
Recommended publications
  • Laboratory Studies for Planetary Sciences
    Laboratory Studies for Planetary Sciences A Planetary Decadal Survey White Paper Prepared by the American Astronomical Society (AAS) Working Group on Laboratory Astrophysics (WGLA) http://www.aas.org/labastro Targeted Panels: Terrestrial Planets; Outer Solar System Satellites; Small Bodies Lead Author: Murthy S. Gudipati Ice Spectroscopy Lab, Science Division, Mail Stop 183-301, Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109. [email protected], 818-354-2637 Co-Authors: Michael A'Hearn - University of Maryland [email protected], 301-405-6076 Nancy Brickhouse - Harvard-Smithsonian Center for Astrophysics [email protected], 617-495-7438 John Cowan - University of Oklahoma [email protected], 405-325-3961 Paul Drake - University of Michigan [email protected], 734-763-4072 Steven Federman - University of Toledo [email protected], 419-530-2652 Gary Ferland - University of Kentucky [email protected], 859-257-879 Adam Frank - University of Rochester [email protected], 585-275-1717 Wick Haxton - University of Washington [email protected], 206-685-2397 Eric Herbst - Ohio State University [email protected], 614-292-6951 Michael Mumma - NASA/GSFC [email protected], 301-286-6994 Farid Salama - NASA/Ames Research Center [email protected], 650-604-3384 Daniel Wolf Savin - Columbia University [email protected], 212-854-4124, Lucy Ziurys – University of Arizona [email protected], 520-621-6525 1 Brief Description: The WGLA of the AAS promotes collaboration and exchange of knowledge between astronomy and planetary sciences and the laboratory sciences (physics, chemistry, and biology).
    [Show full text]
  • Computational Surface Modelling of Ices and Minerals of Interstellar Interest—Insights and Perspectives
    minerals Review Computational Surface Modelling of Ices and Minerals of Interstellar Interest—Insights and Perspectives Albert Rimola 1,* , Stefano Ferrero 1, Aurèle Germain 2 , Marta Corno 2 and Piero Ugliengo 2,3 1 Departament de Química, Universitat Autònoma de Barcelona, 08193 Bellaterra, Catalonia, Spain; [email protected] 2 Dipartimento di Chimica, Università degli Studi di Torino, 10125 Torino, Italy; [email protected] (A.G.); [email protected] (M.C.); [email protected] (P.U.) 3 Nanostructured Interfaces and Surfaces (NIS) Centre, Università degli Studi di Torino, 10125 Torino, Italy * Correspondence: [email protected]; Tel.: +34-93-581-3723 Abstract: The universe is molecularly rich, comprising from the simplest molecule (H2) to complex organic molecules (e.g., CH3CHO and NH2CHO), some of which of biological relevance (e.g., amino acids). This chemical richness is intimately linked to the different physical phases forming Solar-like planetary systems, in which at each phase, molecules of increasing complexity form. Interestingly, synthesis of some of these compounds only takes place in the presence of interstellar (IS) grains, i.e., solid-state sub-micron sized particles consisting of naked dust of silicates or carbonaceous materials that can be covered by water-dominated ice mantles. Surfaces of IS grains exhibit particular characteristics that allow the occurrence of pivotal chemical reactions, such as the presence of binding/catalytic sites and the capability to dissipate energy excesses through the grain phonons. The present know-how on the physicochemical features of IS grains has been obtained by the fruitful synergy of astronomical observational with astrochemical modelling and laboratory experiments.
    [Show full text]
  • Interstellar Dust Within the Life Cycle of the Interstellar Medium K
    EPJ Web of Conferences 18, 03001 (2011) DOI: 10.1051/epjconf/20111803001 C Owned by the authors, published by EDP Sciences, 2011 Interstellar dust within the life cycle of the interstellar medium K. Demyk1,2,a 1Université de Toulouse, UPS-OMP, IRAP, Toulouse, France 2CNRS, IRAP, 9 Av. colonel Roche, BP. 44346, 31028 Toulouse Cedex 4, France Abstract. Cosmic dust is omnipresent in the Universe. Its presence influences the evolution of the astronomical objects which in turn modify its physical and chemical properties. The nature of cosmic dust, its intimate coupling with its environment, constitute a rich field of research based on observations, modelling and experimental work. This review presents the observations of the different components of interstellar dust and discusses their evolution during the life cycle of the interstellar medium. 1. INTRODUCTION Interstellar dust grains are found everywhere in the Universe: in the Solar System, around stars at all evolutionary stages, in interstellar clouds of all kind, in galaxies and in the intergalactic medium. Cosmic dust is intimately mixed with the gas-phase and represents about 1% of the gas (in mass) in our Galaxy. The interstellar extinction and the emission of diffuse interstellar clouds is reproduced by three dust components: a population of large grains, the BGs (Big Grains, ∼10–500 nm) made of silicate and a refractory mantle, a population of carbonaceous nanograins, the VSGs (Very Small Grains, 1–10 nm) and a population of macro-molecules the PAHs (Polycyclic Aromatic Hydrocarbons) [1]. These three components are more or less abundant in the diverse astrophysical environments reflecting the coupling of dust with the environment and its evolution according to the physical and dynamical conditions.
    [Show full text]
  • Carbohydrates: Occurrence, Structures and Chemistry
    Carbohydrates: Occurrence, Structures and Chemistry FRIEDER W. LICHTENTHALER, Clemens-Schopf-Institut€ fur€ Organische Chemie und Biochemie, Technische Universit€at Darmstadt, Darmstadt, Germany 1. Introduction..................... 1 6.3. Isomerization .................. 17 2. Monosaccharides ................. 2 6.4. Decomposition ................. 18 2.1. Structure and Configuration ...... 2 7. Reactions at the Carbonyl Group . 18 2.2. Ring Forms of Sugars: Cyclic 7.1. Glycosides .................... 18 Hemiacetals ................... 3 7.2. Thioacetals and Thioglycosides .... 19 2.3. Conformation of Pyranoses and 7.3. Glycosylamines, Hydrazones, and Furanoses..................... 4 Osazones ..................... 19 2.4. Structural Variations of 7.4. Chain Extension................ 20 Monosaccharides ............... 6 7.5. Chain Degradation. ........... 21 3. Oligosaccharides ................. 7 7.6. Reductions to Alditols ........... 21 3.1. Common Disaccharides .......... 7 7.7. Oxidation .................... 23 3.2. Cyclodextrins .................. 10 8. Reactions at the Hydroxyl Groups. 23 4. Polysaccharides ................. 11 8.1. Ethers ....................... 23 5. Nomenclature .................. 15 8.2. Esters of Inorganic Acids......... 24 6. General Reactions . ............ 16 8.3. Esters of Organic Acids .......... 25 6.1. Hydrolysis .................... 16 8.4. Acylated Glycosyl Halides ........ 25 6.2. Dehydration ................... 16 8.5. Acetals ....................... 26 1. Introduction replacement of one or more hydroxyl group (s) by a hydrogen atom, an amino group, a thiol Terrestrial biomass constitutes a multifaceted group, or similar heteroatomic groups. A simi- conglomeration of low and high molecular mass larly broad meaning applies to the word ‘sugar’, products, exemplified by sugars, hydroxy and which is often used as a synonym for amino acids, lipids, and biopolymers such as ‘monosaccharide’, but may also be applied to cellulose, hemicelluloses, chitin, starch, lignin simple compounds containing more than one and proteins.
    [Show full text]
  • Interstellar Ice Photochemistry and the Deuterium Enrichment and Chemical Properties of Meteoritic Polycyclic Aromatic Hydrocarbons S
    63rd Annual Meteoritical Society Meeting 5003.pdf INTERSTELLAR ICE PHOTOCHEMISTRY AND THE DEUTERIUM ENRICHMENT AND CHEMICAL PROPERTIES OF METEORITIC POLYCYCLIC AROMATIC HYDROCARBONS S. A. Sandford1, M. P. Bernstein1,2, L. J. Allamandola1, J. S. Gillette3, and R. N. Zare3, 1NASA-Ames Research Center, MS 245-6, Moffett Field CA 94035 ([email protected]), 2SETI Institute, 2035 Landings Drive, Mountain View CA 94043, USA, 3Department of Chemistry, Stanford University, Stanford CA 94305, USA. Introduction: Polycyclic aromatic hydrocarbons surroundings over time. However, exchanged D atoms (PAHs) are known to be abundant and ubiquitous in at the other sites are labile only under UV irradiation; the interstellar medium (ISM) [1]. At the temperatures once irradiation ceases these atoms will not exchange typical of dense interstellar molecular clouds (T = 10–- with the environment. 50 K), the birth sites of stars and planetary systems, Because the aromatic fractions of meteoritic PAHs will be frozen out of the gas phase into icy grain organics are known to be enriched in deuterium [6], mantles. These mantles contain a number of molecular this raises the possibility that interstellar species, the most abundant being H2O, CH3OH, CO, photoprocessing of PAHs in D-enriched interstellar CO2, NH3, CH 4, and possibly N2 and O2 [2]. Many of ices has occurred [7]. The measured D/H ratios of these molecules are expected to be enriched in interstellar ices [8] and the observed exchange rates for deuterium via a number of interstellar chemical coronene (C 24H12)-D2O and d12-coronene (C24D12)-H2O processes [2]. While frozen in these D-enriched ices, isotopic substitution experiments show that PAHs in the PAHs will be exposed to ultraviolet photons from interstellar ices could easily attain the D/H levels nearby stars, the attenuated diffuse ISM radiation field, observed in meteorites [7].
    [Show full text]
  • AP Biology Summer Assignment Holy Spirit Prep 2019
    AP Biology Summer Assignment Holy Spirit Prep 2019 Textbook: “Principle of Life” 2nd edition, for the AP course 2018 Chapters 1-3 (pages 1-59) This summer assignment will cover the introduction to biology, chemistry of life, and essential macromolecules for life. The concepts covered in these chapters are either review from previous classes or relatively easy enough to allow you to work through them on your own. The more complex connections between these chapters will be discussed during the first two weeks of the school year. Biozone Workbook: “AP Biology 1” Student edition, 2nd edition 2017 and Biozone Workbook: “AP Biology 2” Student edition, 2nd edition 2017 Read each chapter in the text book, answer all the questions listed below, and complete the corresponding pages in the biozone workbooks covering those topics. The answers can be typed or handwritten for the questions below and written in the workbook for the biozone pages listed. Do not tear out the biozone workbook pages. I will check your answers directly from the workbook. This assignment will be due on Wednesday, Aug 21, 2019. We will have a test over the material during the second week of the school year. For questions, contact Mr. Harrison at [email protected] Chapter 1: Principles of Life Answer the following: 1. Organisms share many conserved biological, chemical, and structural characteristics. Briefly outline the 8 distinctive characteristics of life shared by all living organisms. 2. How do the shared characteristics on your list (in #1) provide evidence for evolution? 3. There are several competing hypotheses about the evolution of early life on Earth, but as life evolved, all cells clearly had requirements for raw materials and energy transfers.
    [Show full text]
  • Infrared Observations of Interstellar Ices
    Infrared Observations of Interstellar Ices Adwin Boogert NASA Herschel Science Center IPAC, Caltech Pasadena, CA, USA 05 June 2012 Interstellar Dust School (Cuijk): Interstellar Ices (Boogert) 1 Scope ●Lecture 1 (Monday): What you need to know when planning, reducing, or analyzing infrared spectroscopic observations of dust and ices. ●Lecture 2 (Tuesday): Basic physical and chemical information derived from interstellar ice observations. Not discussed: laboratory techniques (see Palumbo lectures) and surface chemistry (see Cuppen lectures). ●Lecture 3 (Tuesday): Infrared spectroscopic databases. What's in them and how (not) to use them. ●Drylabs (Tuesday): Using databases of interstellar infrared spectra and of laboratory ices. Deriving ice abundances and analyzing ice band profiles. NOTE: Please download all presentations and drylab tar file: spider.ipac.caltech.edu/~aboogert/Cuijk/ 05 June 2012 Interstellar Dust School (Cuijk): Interstellar Ices (Boogert) 2 Topics ●Basics ● Ice mantle formation ● Deriving ice column densities and abundances ●YSO and background source selection ●Continuum determination ●Vibrational modes ●The interstellar ice inventory ●Ice band profile analysis: ● Polar versus apolar ices ● Amorphous versus crystalline ices ● Segregation in the ices ● Grain size and shape effects ●Location of ices ●Processing of ices by YSOs ●Complex molecules in ices? 05 June 2012 Interstellar Dust School (Cuijk): Interstellar Ices (Boogert) 3 Background Reading ● For the basics: Dust in the galactic environment, 2nd ed. by D.C.B. Whittet. Bristol: Institute of Physics (IOP) Publishing, 2003 Series in Astronomy and Astrophysics, ISBN 0750306246. ● More advanced: Chapter 10 in “The Physics and Chemistry of the Interstellar Medium”, A. G. G. M. Tielens, ISBN 0521826349. Cambridge, UK: Cambridge University Press, 2005.
    [Show full text]
  • Aerospace Medicine & Biology Space Medicine & Biology Aero 9
    Aerospace Medicine NASA SP-7011 (232) and Biology May 1982 IWNSA A Continuing Bibliography with Indexes (NASA-SP-701 1 (232) ) AT. CE MEDICINE AND N82-2898U BIOLOGY: A CONTINUING BIBLIOGRAPHY WITH INDEXES (SUPPLEMENT 232) (National Aeronautics and Space Administration) 137 p Unclas Hc <7.QQ CSCL Ofa£ 00/52 25483 National Aeronautics and Space Administration Aerospace Medicine & Biology space Medicine & Biology Aero 9 Medicine & Biology Aerospao dicine & Biology Aerospace M ne & Biology AerosjatoiMedici Biology Aerospace Medicine & gy Aerospace Medicine & Biolo 3rospace Medicine & Biology / pace Medicine & Biology Aeros Medicine & Biology Aerospace cine & Biology Aerospace Med & Biology Aerospace Medicine < ACCESSION NUMBER RANGES Accession numbers cited in this Supplement fall within the following ranges. STAR (N-10000 Series) N82-16040 - N82-18118 IAA (A-10000 Series) A82-18840 - A82-22250 This bibliography was prepared by the NASA Scientific and Technical Information Facility operated for the National Aeronautics and Space Administration by PRC Government Information Systems. NASA SP-7011(232) AEROSPACE MEDICINE AND BIOLOGY A CONTINUING BIBLIOGRAPHY WITH INDEXES (Supplement 232) A selection of annotated references to unclassified reports and journal articles that were introduced into the NASA scientific and technical information sys- tem and announced in April 1982 in Scientific and Technical Aerospace Reports (STAR) International Aerospace Abstracts (IA A). Scientific and Technical Information Branch 1982 National Aeronautics and Space Administration Washington, DC NASA SP-7011 and its supplements are available from the National Technical Information Service (NTIS). Questions on the availability of the predecessor publications, Aerospace Medicine and Biology (Volumes I - XI) should be directed to NTIS. This supplement is available as NTISUB/123/093 from the National Technical Information Service (NTIS), Springfield, Virginia 22161 at the price of $7.00 domestic; $14.00 foreign.
    [Show full text]
  • UV Photolysis of Quinoline in Interstellar Ice Analogs
    Meteoritics & Planetary Science 41, Nr 5, 785–796 (2006) Abstract available online at http://meteoritics.org UV photolysis of quinoline in interstellar ice analogs Jamie E. ELSILA1*, Matthew R. HAMMOND2, Max P. BERNSTEIN1, Scott A. SANDFORD1, and Richard N. ZARE2 1NASA Ames Research Center, MS 245-6, Moffett Field, California 94035–1000, USA 2Department of Chemistry, Stanford University, Stanford, California 94305–5080, USA *Corresponding author. E-mail: [email protected] (Received 16 November 2005; revision accepted 03 February 2006) Abstract–The polycyclic aromatic nitrogen heterocycle (PANH) quinoline (C9H7N) was frozen at 20 K in interstellar ice analogs containing either pure water or water mixed with methanol or methane and exposed to ultraviolet (UV) radiation. Upon warming, the photolysis products were analyzed by high-performance liquid chromatography and nanoscale liquid chromatography-electrospray ionization mass spectrometry. A suite of hydroxyquinolines, which were formed by the addition of oxygen atoms to quinoline, was observed as the primary product in all the ices. Quinoline N oxide was not formed, but five hydroxyquinoline isomers were produced with no clear dominance of one isomer. Reduction products, formed by hydrogen atom addition, were also created. Ices created at 20 K with H2O: quinoline ratios of 10:1 to 100:1 showed similar product distributions to those at 122 K, with no apparent temperature or concentration dependence. Increasing the UV dose led to a decrease in overall yield, indicating that quinoline and its products may be photo-destroyed. Methylquinolines were formed upon photolysis of the methanol- and methane-containing ices. In addition, possible methoxyquinolines or quinoline methylene alcohols were formed in the methanol- containing ice, while methylhydroxyquinolines were created in the methane-containing ice.
    [Show full text]
  • Gudipati Keck Comet Physical and Chemical Composition of Comet
    Present Understanding of Comet Nucleus Physical and Chemical Composition Murthy S. Gudipati Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 Keck Study – Comet – June 5, 2017 Outline Comet – Physical Composition Comet - Chemical Composition Comet – History 2 Comet – Physical Composition Physical Composition of Comets 3 Comet Physical Composition Gas (Volatiles, now Super Volatiles) Dust (Silicate Grains) Water (in the form of Ice – major component) The Elephant in the Room: How these three components are put together in a comet’s nucleus? 4 Porosity Science, 349, aab0639, 2015 Dust/Ice = 0.4 – 2.6 Porosity = 75 -85% Enrichment of Dust Regions and vice versa? Dust = Carbonaceous Chondrites (high percentages of water & organics; silicates, oxides, sulfides, olivine, serpentine, etc.) 5 Density Icarus 277 (2016) 257–278 Density = 532 ± 7 kg m−3 Crystalline water-ice = 920 kg m−3 Amorphous water-ice = ~500 - 800 kg m−3 Carbonaceous chondrites = ~3 to 3.7 kg m−3 6 Thermal Inertia Science, 349, aab0464, 2015 Thermal Inertia:85±35 J m-2K-1s-1/2 Thermal gradient? How Deep to reach <30 K? 7 Surface Science, 349, aaa9816, 2015 ~20 cm granular (soft) Below hard crust How thick is the crust – cm range or m range? 8 Simultaneous UV & IR Absorption + Fluorescence Pyrene in H2O Ice UV - PAH IR - Ice Flu - PAH Lignell & Gudipati J. Phys. Chem A. 119 (2015) 2607 9 Are Comets Like Deep Fried Ice Cream? ~0.1 m Comet CG/67P Lignell & Gudipati J. Phys. Chem A. 119 (2015) 2607 10 Comet – Chemical Composition Chemical Composition of Comets 11 Composition of Interstellar Medium At 1 atm.
    [Show full text]
  • Food Carbohydrate Chemistry Food Carbohydrate Chemistry
    Food Carbohydrate Chemistry Food Food Carbohydrate Chemistry Carbohydrates are major components of foods. They account for more than 90 percent of the dry matter of fruits and vegetables and provide 70 to 80 percent Food Carbohydrate of human caloric intake worldwide so, from a quantitative perspective alone, they warrant the attention of food chemists. From the standpoint of food quality, carbohydrates are multifunctional. Sugars are the major source of sweetness, but in addition, carbohydrates provide flavor, color, and texture – desirable, Chemistry undesirable, and neutral – as well as having functional roles as thickeners, gelling agents, bodying agents, and stabilizers in foods. When it comes to nutrition, carbohydrates are often blamed for such health issues as obesity, diabetes, and dental caries. It should be realized that carbohydrates are, or should be, the principal source of energy in our diet and that good nutrition Ronald E. Wrolstad is based on the consumption of the appropriate carbohydrates, in the right amounts, and in balance with other nutrients. Food Carbohydrate Chemistry relates basic carbohydrate chemistry to the quality attributes and functional properties of foods. Structure and nomenclature Press of sugars and sugar derivatives are covered but limited to those compounds that exist naturally in foods or are used as food additives and food ingredients. Review and presentation of fundamental carbohydrate chemistry is minimal, with the assumption that readers have already taken general organic chemistry and general biochemistry. Chemical reactions focus on those that have an impact on food quality and occur under processing and storage conditions. How chemical and physical properties of sugars and polysaccharides affect the functional properties of foods is emphasized.
    [Show full text]
  • H2O Ice Mixtures with CH3OH and NH3 in the Far-IR Region B
    A&A 592, A81 (2016) Astronomy DOI: 10.1051/0004-6361/201628324 & c ESO 2016 Astrophysics Interstellar ice analogs: H2O ice mixtures with CH3OH and NH3 in the far-IR region B. M. Giuliano1; 4, R. Martín-Doménech1, R. M. Escribano2, J. Manzano-Santamaría1; 3, and G. M. Muñoz Caro1 1 Centro de Astrobiología, INTA-CSIC, Carretera de Ajalvir, km 4, Torrejón de Ardoz, 28850 Madrid, Spain e-mail: [email protected] 2 Instituto de Estructura de la Materia-Consejo Superior de Investigaciones Científicas (IEM-CSIC), 28006 Madrid, Spain 3 Dept. de Matemática Aplicada, Ciencia e Ingeniería de Materiales, ESCET, Universidad Rey Juan Carlos. C/ Tulipán s/n, Móstoles 28933 Madrid, Spain 4 Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany Received 17 February 2016 / Accepted 29 May 2016 ABSTRACT Context. New spectroscopic observations in the far-infrared (IR) range are expected from future planned missions. Although water ice is the only species detected so far in interstellar ices in this range, the presence of ice mixtures requires laboratory characterization of the corresponding spectra. Aims. We present an investigation on far-IR spectra of binary ice mixtures relevant in various astrophysical environments. The fore- most goal is to compare the spectroscopic features of the ice mixtures to those of pure ices, and to search for changes in peak frequencies, intensities, and band strengths of the main bands. Methods. Mixtures H2O:CH3OH and H2O:NH3 of different ratios have been deposited on a diamond substrate at astrophysically relevant conditions. We measured the spectra in the near- and mid-IR regions to derive ice column densities that were subsequently used to calculate the apparent band strengths in the far-IR region.
    [Show full text]