Class 3. The PAH Spectrum, what does it tell us??
|
|
- Johnathan Bond
- 6 years ago
- Views:
Transcription
1 Class 3 The PAH Spectrum, what does it tell us??
2 PAH Vibrations! CH str! CC str! CC str /CH ip! CH oop! 3! 4! 5! 6! 7! 8! 9! 10! 15! Wavelength (µm)! NASA Ames! Astrochemisty Lab! Vibration - S. Langhoff! Orion ISO Spectrum - E. Peeters!
3 But the Real Treasure (and some nice surprises) are in the Details... The global similarity of the interstellar emission" single chemical family; molecule-sized polycyclic aromatic compounds" Differences at the most detailed levels" reflect spectroscopic characteristics of that portion of the population that is changing in response to changing physical and chemical conditions. " Therefore, it is the details of the interstellar spectra that hold the key to exploiting PAHs as probes of the emitting regions. " Slide adapted from Hudgins- IAU Symposium 231!
4 Analysis of the 6.2 µm Emission Band Observations of the 6.2 µm emission feature have shown: Range: 6.203µm µm. Composite of 2 bands, not a continuous dist n of 1. Class A, B bands by far the most common. Emission at this position is dominated by PAH ions Large PAH cations (N C > 50 C atoms) can accommodate Class C emission component Class A component anomalous A" B" C" Peeters et al A&A, 360, Composite" spectra of PAH ions"
5 Polycyclic Aromatic Nitrogen Heterocycles - PANHs Exhibit 1600 IR spectroscopic cm -1 CC stretching characteristics features very that are similar very to similar those to those of the of parent the parent PAH. PAH PANH Position of strongest cm -1 cation band (parent PAH) PANH Position of strongest cm -1 cation band (parent PAH) N 1549 cm -1, µm (1553 cm -1, µm) N 1538, cm -1, µm (1540 cm -1, µm) N 1559 cm -1, µm (1560 cm -1, µm) N 1531 cm -1, µm (1540 cm -1, µm) N 1553 cm -1, µm (1560 cm -1, µm) N 1568 cm -1, µm 1585 cm -1, µm N 1564 cm -1, µm (1560 cm -1, µm) N 1574 cm -1, µm (1590 cm -1, µm) Chem. & Phys. Matrix Isolated Species 5
6 Polycyclic Aromatic Nitrogen Heterocycles - PANHs Substitution at an edge site = exoskeletal PANH Substitution at an internal site = endoskeletal PANH" Chem. & Phys. Matrix Isolated Species 6
7 N Substituted coronene cations 6.10 Wavelength (µm) Theoretical Calculations - C. Bauschlicher Normalized Absorbance N1b-Coronene Cation, C 23 H 11 N Wavenumber (cm -1 ) Chem. & Phys. Matrix Isolated Species Coronene Cation, C 24 H
8 N Substituted coronene cations 6.10 Wavelength (µm) Theoretical Calculations - C. Bauschlicher Normalized Absorbance N3b-Coronene Cation, C 23 H 11 N + N2b-Coronene Cation, C 23 H 11 N + N1b-Coronene Cation, C 23 H 11 N Wavenumber (cm -1 ) Chem. & Phys. Matrix Isolated Species Coronene Cation, C 24 H
9 Endoskeletal PANHs and the 6.2 µm Emission Band" Normalized Absorbance 6.10 Wavelength (µm) N-Circumcor N19 Cation + 4N-Circumcor N21 Cation + 3N-Circumcor N29 Cation + 2N-Circumcor N35 Cation + N substitution within the carbon skeleton of a PAH produces a depth-dependant "blue shift in the" "position of the" "dominant CC" "stretching" "feature near " "6.2 µm." Circumcoronene Cation, C 54 CH 5418 H Wavenumber (cm -1 ) 1 N-Circumcor N23 Cation + The position of the! nominal interstellar 6.2 µm emission band may provide a tracer of N in interstellar dust. Chem. & Phys. Matrix Isolated Species 9
10 PANHs have a large permanent dipole (µ), PAHs do not N Microwave observatories should be able to detect the finger prints of PANHs in the interstellar environment. This would allow the identification of individual aromatic molecules in the interstellar medium.. Image Gallery-Radio Telescopes Andy Mattioda
11 PANH cations all possess significant dipole moments " Dipole Moments (Debye) Dipole Moments (Debye) Species µ a µ b µ Species µ a µ b µ N-coronene cations N-circumcoronene cations 1N N N 'N N N N N-ovalene cations 4N N N 'N ''N N-circum-circumcoronene cations 1'''N N N 'N 'N N N 'N 'N N N N N N Hudgins, Bauschlicher, & Allamandola (2005)! 11
12 and rotational constants in the" GHz ( MHz) range " Rotational Constants (GHz) Species R a R b R c N-coronenes N-ovalenes N-circumcoronenes N-circum-circumcoronenes Hudgins, Bauschlicher, & Allamandola (2005)! Interstellar PANHs should produce a dense forest of lines over a very broad spectral range." Interstellar PANHs may contribute to anomalous galactic background emission at radio wavelengths. " Interstellar PANHs may represent an interesting, albeit challenging, subject for an interstellar search." Chem. & Phys. Matrix Isolated Species 12
13 The Anomalous Microwave Emission (AME) on the Cosmic Microwave Background 10 5 Model Ancillary data WMAP Planck Flux density [Jy] Planck Data Frequency [GHz] The AME (10 to 100 MHz) falls precisely in the range expected from large PANHs (and PAHs)!!!
14 PAH Vibrations! CH str! CC str! CC str /CH ip! CH oop! 3! 4! 5! 6! 7! 8! 9! 10! 15! Wavelength (µm)! NASA Ames! Astrochemisty Lab! Vibration - S. Langhoff! Orion ISO Spectrum - E. Peeters!
15
16
17
18
19
20
21 End part 1 Class 3 Go to Christiaan s work
ANALYZING ASTRONOMICAL OBSERVATIONS WITH THE NASA AMES PAH DATABASE
PAHs and the Universe C. Joblin and A.G.G.M. Tielens (eds) EAS Publications Series, 46 (2011) 117-122 www.eas.org ANALYZING ASTRONOMICAL OBSERVATIONS WITH THE NASA AMES PAH DATABASE J. Cami 1, 2 Abstract.
More informationarxiv: v1 [astro-ph] 7 Feb 2008
The infrared spectra of very large, compact, highly symmetric, polycyclic aromatic hydrocarbons (PAHs) Charles W. Bauschlicher, Jr. 1, Els Peeters 2,3,4, Louis J. Allamandola 5 arxiv:0802.1071v1 [astro-ph]
More informationDust: Grain Populations, Extinction Curves, and Emission Spectra Monday, January 31, 2011
Dust: Grain Populations, Extinction Curves, and Emission Spectra Monday, January 31, 2011 CONTENTS: 1. Introduction 2. The Extinction Curve and Abundance Constraints A. Formalities B. Features 3. Infrared
More informationLecture 11. IR Theory. Next Class: Lecture Problem 4 due Thin-Layer Chromatography
Lecture 11 IR Theory Next Class: Lecture Problem 4 due Thin-Layer Chromatography This Week In Lab: Ch 6: Procedures 2 & 3 Procedure 4 (outside of lab) Next Week in Lab: Ch 7: PreLab Due Quiz 4 Ch 5 Final
More informationIncreasing energy. ( 10 4 cm -1 ) ( 10 2 cm -1 )
The branch of science which deals with the interaction of electromagnetic radiation with matter is called spectroscopy The energy absorbed or emitted in each transition corresponds to a definite frequency
More informationPlanck and Virtual Observatories: Far Infra-red / Sub-mm Specificities
JF Sygnet (Planck HFI DPCM) Planck and Virtual Observatories: Far Infra-red / Sub-mm Specificities Planck Mission, Planck Data and its Specificities (4) Data Treatment and its Specificities (4) Planck
More informationRadiant energy is proportional to its frequency (cycles/s = Hz) as a wave (Amplitude is its height) Different types are classified by frequency or
CHEM 241 UNIT 5: PART B INFRA-RED RED SPECTROSCOPY 1 Spectroscopy of the Electromagnetic Spectrum Radiant energy is proportional to its frequency (cycles/s = Hz) as a wave (Amplitude is its height) Different
More informationAstrochemistry (2) Interstellar extinction. Measurement of the reddening
Measurement of the reddening The reddening of stellar colours casts light on the properties of interstellar dust Astrochemistry (2) Planets and Astrobiology (2016-2017) G. Vladilo The reddening is measured
More informationUniversity of Groningen. Infrared emission features Boersma, Christiaan
University of Groningen Infrared emission features Boersma, Christiaan IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the
More informationInfrared Spectroscopy
Infrared Spectroscopy Introduction Spectroscopy is an analytical technique which helps determine structure. It destroys little or no sample. The amount of light absorbed by the sample is measured as wavelength
More informationAromatic Features in M101 HII Regions and Starburst Galaxies
**FULL TITLE** ASP Conference Series, Vol. **VOLUME**, **YEAR OF PUBLICATION** **NAMES OF EDITORS** Aromatic Features in M101 HII Regions and Starburst Galaxies Karl D. Gordon, Charles Engelbracht, J.D.T.
More informationChemistry 213 Practical Spectroscopy
Chemistry 213 Practical Spectroscopy Dave Berg djberg@uvic.ca Elliott 314 A course in determining structure by spectroscopic methods Different types of spectroscopy afford different information about molecules
More informationarxiv: v1 [astro-ph.ga] 29 Jun 2011
Astronomy & Astrophysics manuscript no. final c ESO 2 June 3, 2 arxiv:6.5899v [astro-ph.ga] 29 Jun 2 Coupled Blind Signal Separation and Spectroscopic Database Fitting of the Mid Infrared PAH Features
More informationAstrochimistry Spring 2013 Lecture 4: Interstellar PAHs NGC HST
Astrochimistry Spring 2013 Lecture 4: Interstellar PAHs NGC 7023 - HST Julien Montillaud 8th February 2013 Outline I. From Unidentified to Aromatic Infrared Bands (7 p.) I.1 Historical background I.2 Observational
More information2. Infrared spectroscopy
2. Infrared spectroscopy 2-1Theoretical principles An important tool of the organic chemist is Infrared Spectroscopy, or IR. IR spectra are acquired on a special instrument, called an IR spectrometer.
More information8: Composition and Physical state of Interstellar Dust
8: Composition and Physical state of Interstellar Dust James Graham UC, Berkeley 1 Reading Tielens, Interstellar Medium, Ch. 5 Mathis, J. S. 1990, AARA, 28, 37 Draine, B. T., 2003, AARA, 41, 241 2 Nature
More informationSimulating chemistry on interstellar dust grains in the laboratory
From Stars to Life, April 3-6 2013, Gainesville FL Simulating chemistry on interstellar dust grains in the laboratory Nicolas Polfer University of Florida Department of Chemistry http://www.cosmotography.com/images/cosmic_nurseries.html
More informationLABORATORY SPECTROSCOPY OF PROTONATED PAH MOLECULES RELEVANT FOR INTERSTELLAR CHEMISTRY
PAHs and the Universe C. Joblin and A.G.G.M. Tielens (eds) EAS Publications Series, 46 (2011) 103-108 www.eas.org LABORATORY SPECTROSCOPY OF PROTONATED PAH MOLECULES RELEVANT FOR INTERSTELLAR CHEMISTRY
More informationROTATIONAL SPECTRA OF SMALL PAHs: ACENAPHTHENE, ACENAPHTHYLENE, AZULENE, AND FLUORENE
The Astrophysical Journal, 662:1309 Y 1314, 27 June 20 # 27. The American Astronomical Society. All rights reserved. Printed in U.S.A. A ROTATIONAL SPECTRA OF SMALL PAHs: ACENAPHTHENE, ACENAPHTHYLENE,
More informationSPECTROSCOPY MEASURES THE INTERACTION BETWEEN LIGHT AND MATTER
SPECTROSCOPY MEASURES THE INTERACTION BETWEEN LIGHT AND MATTER c = c: speed of light 3.00 x 10 8 m/s (lamda): wavelength (m) (nu): frequency (Hz) Increasing E (J) Increasing (Hz) E = h h - Planck s constant
More informationLecture 18 Long Wavelength Spectroscopy
Lecture 18 Long Wavelength Spectroscopy 1. Introduction. The Carriers of the Spectra 3. Molecular Structure 4. Emission and Absorption References Herzberg, Molecular Spectra & Molecular Structure (c. 1950,
More informationCHEM 301: Homework assignment #12
CHEM 301: Homework assignment #12 Solutions 1. Let s practice converting between wavelengths, frequencies, and wavenumbers. (10%) Express a wavelength of 442 nm as a frequency and as a wavenumber. What
More informationarxiv: v1 [astro-ph.ga] 5 Dec 2018
Draft version December 7, 2018 Typeset using LATEX twocolumn style in AASTeX62 Examining the class B-to-A shift of the 7.7 µm PAH band with the NASA Ames PAH IR Spectroscopic Database Matthew J. Shannon
More informationPhotodissociation Regions Radiative Transfer. Dr. Thomas G. Bisbas
Photodissociation Regions Radiative Transfer Dr. Thomas G. Bisbas tbisbas@ufl.edu Interstellar Radiation Field In the solar neighbourhood, the ISRF is dominated by six components Schematic sketch of the
More informationLecture 5. Interstellar Dust: Chemical & Thermal Properties
Lecture 5. Interstellar Dust: Chemical & Thermal Properties!. Spectral Features 2. Grain populations and Models 3. Thermal Properties 4. Small Grains and Large Molecules -------------------------------------------------
More informationCHE 325 SPECTROSCOPY (A) CHAP 13A ASSIGN CH 2 CH CH 2 CH CHCH 3
CE 325 SPECTRSCPY (A) CAP 13A ASSIGN 1. Which compound would have a UV absorption band at longest wavelength? A. I B. II C. III D. IV E. V C CC 3 CC C 2 C CC 3 I II III C 2 C C 2 C CC 3 IV V 2. Select
More informationExploring ISM dust with IRSIS. Emmanuel DARTOIS IAS-CNRS
Exploring ISM dust with IRSIS Emmanuel DARTOIS IAS-CNRS IRSIS meeting 05-12-2007 Overview Intestellar ice mantles Hydrocarbons in the galaxy and outside Polycyclic Aromatic Hydrocarbons (PAHs) Interstellar
More informationCHEM 3.2 (AS91388) 3 credits. Demonstrate understanding of spectroscopic data in chemistry
CHEM 3.2 (AS91388) 3 credits Demonstrate understanding of spectroscopic data in chemistry Spectroscopic data is limited to mass, infrared (IR) and 13 C nuclear magnetic resonance (NMR) spectroscopy. Organic
More informationPolycyclic Aromatic Hydrocarbon from the Magellanic Clouds
Polycyclic Aromatic Hydrocarbon from the Magellanic Clouds Hony and Spitzer/SAGE-SPEC team Galliano, Seok, Neelamkodan, Kemper, Madden, Indebetouw, Gordon, Sandstrom 11 Aug 2017 S. Hony (Heidelberg University)
More informationDust emission. D.Maino. Radio Astronomy II. Physics Dept., University of Milano. D.Maino Dust emission 1/24
Dust emission D.Maino Physics Dept., University of Milano Radio Astronomy II D.Maino Dust emission 1/24 New insight on Dust Emission Before WMAP and Planck with only COBE-DMR, dust is well described by
More informationChapter 12 Mass Spectrometry and Infrared Spectroscopy
Organic Chemistry, 6 th Edition L. G. Wade, Jr. Chapter 12 Mass Spectrometry and Infrared Spectroscopy Jo Blackburn Richland College, Dallas, TX Dallas County Community College District 2006, Prentice
More informationA. G. G. M. TIELENS SRON, Kapteyn Astronomical Institute, P.O. Box 800, 9700 AV Groningen, The Netherlands
THE ASTROPHYSICAL JOURNAL, 560:261È271, 2001 October 10 ( 2001. The American Astronomical Society. All rights reserved. Printed in U.S.A. THEORETICAL MODELING OF INFRARED EMISSION FROM NEUTRAL AND CHARGED
More informationInterstellar Dust and Extinction
University of Oxford, Astrophysics November 12, 2007 Outline Extinction Spectral Features Emission Scattering Polarization Grain Models & Evolution Conclusions What and Why? Dust covers a range of compound
More informationIntroduction. The analysis of the outcome of a reaction requires that we know the full structure of the products as well as the reactants
Introduction The analysis of the outcome of a reaction requires that we know the full structure of the products as well as the reactants Spectroscopy and the Electromagnetic Spectrum Unlike mass spectrometry,
More informationPDF hosted at the Radboud Repository of the Radboud University Nijmegen
PDF hosted at the Radboud Repository of the Radboud University Nijmegen The following full text is a publisher's version. For additional information about this publication click this link. http://hdl.handle.net/2066/169460
More informationPC Laboratory Raman Spectroscopy
PC Laboratory Raman Spectroscopy Schedule: Week of September 5-9: Student presentations Week of September 19-23:Student experiments Learning goals: (1) Hands-on experience with setting up a spectrometer.
More informationINTRODUCTION TO MICROWAVE REMOTE SENSING - II. Dr. A. Bhattacharya
1 INTRODUCTION TO MICROWAVE REMOTE SENSING - II Dr. A. Bhattacharya The Radiation Framework The information about features on the Earth s surface using RS depends on measuring energy emanating from the
More informationStructure Determination. How to determine what compound that you have? One way to determine compound is to get an elemental analysis
Structure Determination How to determine what compound that you have? ne way to determine compound is to get an elemental analysis -basically burn the compound to determine %C, %H, %, etc. from these percentages
More informationInfrared Spectroscopy
Infrared Spectroscopy IR Spectroscopy Used to identify organic compounds IR spectroscopy provides a 100% identification if the spectrum is matched. If not, IR at least provides information about the types
More informationMolecular spectroscopy
Molecular spectroscopy Origin of spectral lines = absorption, emission and scattering of a photon when the energy of a molecule changes: rad( ) M M * rad( ' ) ' v' 0 0 absorption( ) emission ( ) scattering
More informationOrganic Compound Identification Using Infrared Spectroscopy. Description
Return to paper Organic Compound Identification Using Infrared Spectroscopy Dr. Walt Volland, Bellevue Community College All rights reserved 1999, Bellevue, Washington Description This exercise is intended
More informationThe Interstellar Medium in Galaxies: SOFIA Science
The Interstellar Medium in Galaxies: SOFIA Science Margaret Meixner (STScI) Xander Tielens (NASA/Ames/Leiden Univ.), Jesse Dotson (NASA/ARC), Bruce Draine (Princeton), Mark Wolfire (U. Maryland), Jackie
More informationChemical Enrichment of the ISM by Stellar Ejecta
Chemical Enrichment of the ISM by Stellar Ejecta Sun Kwok The University of Hong Kong IAU GA Beijing, Special Session 12, August 31, 2012 Molecular synthesis in the late stages of stellar evolution It
More informationStatus of the Diffuse Interstellar Band Problem
Status of the Diffuse Interstellar Band Problem Ben McCall Department of Chemistry and Department of Astronomy University of Illinois at Urbana-Champaign APO DIB Collaboration: Tom Fishman (Chicago), Scott
More informationInfrared Spectroscopy An Instrumental Method for Detecting Functional Groups
Infrared Spectroscopy An Instrumental Method for Detecting Functional Groups 1 The Electromagnetic Spectrum Infrared Spectroscopy I. Physics Review Frequency, υ (nu), is the number of wave cycles that
More informationInfrared spectroscopy Basic theory
Infrared spectroscopy Basic theory Dr. Davide Ferri Paul Scherrer Institut 056 310 27 81 davide.ferri@psi.ch Importance of IR spectroscopy in catalysis IR Raman NMR XAFS UV-Vis EPR 0 200 400 600 800 1000
More informationBeyond the Visible -- Exploring the Infrared Universe
Beyond the Visible -- Exploring the Infrared Universe Prof. T. Jarrett (UCT) Infrared Window Telescopes ISM -- Galaxies Infrared Window Near-infrared: 1 to 5 µm Mid-infrared: 5 to 50 µm
More informationThe High-Energy Interstellar Medium
The High-Energy Interstellar Medium Andy Strong MPE Garching on behalf of Fermi-LAT collaboration Cosmic Ray Interactions: Bridging High and Low Energy Astrophysics Lorentz Centre Workshop March 14-18
More informationMidterm Results. The Milky Way in the Infrared. The Milk Way from Above (artist conception) 3/2/10
Lecture 13 : The Interstellar Medium and Cosmic Recycling Midterm Results A2020 Prof. Tom Megeath The Milky Way in the Infrared View from the Earth: Edge On Infrared light penetrates the clouds and shows
More informationClassification of spectroscopic methods
Introduction Spectroscopy is the study of the interaction between the electromagnetic radiation and the matter. Spectrophotometry is the measurement of these interactions i.e. the measurement of the intensity
More informationWelcome to Organic Chemistry II
Welcome to Organic Chemistry II Erika Bryant, Ph.D. erika.bryant@hccs.edu Class Syllabus 3 CHAPTER 12: STRUCTURE DETERMINATION 4 What is this solution Soda Tea Coffee??? 5 What is this solution Soda Tea
More informationIntroduction to Electromagnetic Radiation and Radiative Transfer
Introduction to Electromagnetic Radiation and Radiative Transfer Temperature Dice Results Visible light, infrared (IR), ultraviolet (UV), X-rays, γ-rays, microwaves, and radio are all forms of electromagnetic
More information12. Structure Determination: Mass Spectrometry and Infrared Spectroscopy
12. Structure Determination: Mass Spectrometry and Infrared Spectroscopy Determining the Structure of an Organic Compound The analysis of the outcome of a reaction requires that we know the full structure
More informationInterstellar Medium and Star Birth
Interstellar Medium and Star Birth Interstellar dust Lagoon nebula: dust + gas Interstellar Dust Extinction and scattering responsible for localized patches of darkness (dark clouds), as well as widespread
More informationFrequencies and Normal Modes of Vibration of Benz[a]anthracene Radical Ions
Frequencies and Normal Modes of Vibration of Benz[a]anthracene Radical Ions Rehab M. Kubba, Raghida I. Al-ani, and Muthana Shanshal Department of Chemistry, College of Science, University of Baghdad, Jadiriya,
More informationEXPT. 7 CHARACTERISATION OF FUNCTIONAL GROUPS USING IR SPECTROSCOPY
EXPT. 7 CHARACTERISATION OF FUNCTIONAL GROUPS USING IR SPECTROSCOPY Structure 7.1 Introduction Objectives 7.2 Principle 7.3 Requirements 7.4 Strategy for the Interpretation of IR Spectra 7.5 Practice Problems
More informationThe NASA Ames PAH IR Spectroscopic Database
Chapter 5 The NASA Ames PAH IR Spectroscopic Database C. Boersma, L.J. Allamandola, C.W. Bauschlicher Jr., A. Ricca, J. Cami, A.L. Mattioda, A.G.G.M. Tielens Abstract Some thirty-five years after the initial
More informationInterstellar gamma rays. New insights from Fermi. Andy Strong. on behalf of Fermi-LAT collaboration. COSPAR Scientific Assembly, Bremen, July 2010
Interstellar gamma rays New insights from Fermi Andy Strong on behalf of Fermi-LAT collaboration COSPAR Scientific Assembly, Bremen, July 2010 Session E110: ' The next generation of ground-based Cerenkov
More informationThe Diffuse Interstellar Bands and Carbon Chains
The Diffuse Interstellar Bands and Carbon Chains Ben McCall Miller Institute for Basic Research in Science Department of Chemistry and Department of Astronomy University of California at Berkeley U. Chicago:
More informationWave Description. Transverse and Longitudinal Waves. Physics Department 2/13/2019. Phys1411 Goderya 1. PHYS 1403 Stars and Galaxies
PHYS 1403 Stars and Galaxies for Today s Class 1. How do we explain the motion of energy? 2. What is a wave and what are its properties 3. What is an electromagnetic spectrum? 4. What is a black body and
More informationUniversity of Groningen. Infrared emission features Boersma, Christiaan
University of Groningen Infrared emission features Boersma, Christiaan IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the
More informationASTR2050 Spring Please turn in your homework now! In this class we will discuss the Interstellar Medium:
ASTR2050 Spring 2005 Lecture 10am 29 March 2005 Please turn in your homework now! In this class we will discuss the Interstellar Medium: Introduction: Dust and Gas Extinction and Reddening Physics of Dust
More informationLABORATORY INFRARED SPECTRA OF POLYCYCLIC AROMATIC NITROGEN HETEROCYCLES: QUINOLINE AND PHENANTHRIDINE IN SOLID ARGON AND H 2 O
The Astrophysical Journal, 626:909 918, 2005 June 20 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. LABORATORY INFRARED SPECTRA OF POLYCYCLIC AROMATIC NITROGEN HETEROCYCLES:
More informationChristine Joblin Institut de Recherche en Astrophysique et Planétologie Université de Toulouse [UPS] CNRS
Christine Joblin Institut de Recherche en Astrophysique et Planétologie Université de Toulouse [UPS] CNRS Negative ions and molecules in astrophysics Gothenburg and Onsala, Sweden 22-24/08/2011 Outline
More informationProbing Bonding Using Infrared Spectroscopy Chem
Probing Bonding Using Infrared Spectroscopy Chem 112-2011 INTRODUCTION First, watch the short video on how to record an infrared spectrum using an infrared spectrometer, linked at: http://employees.oneonta.edu/viningwj/chem112/labs/ir_video/ir_video_controller.swf
More informationAstronomy 106, Fall September 2015
Today in Astronomy 106: molecules to molecular clouds to stars Aromatic (benzene-ring) molecules in space Formation of molecules, on dust-grain surfaces and in the gas phase Interstellar molecular clouds
More informationMolekularne vibracije i IR (infra crvena spektroskopija)
Molekularne vibracije i IR (infra crvena spektroskopija) Vibracije What is a vibration in a molecule? Any change in shape of the molecule- stretching of bonds, bending of bonds, or internal rotation around
More informationLABORATORY INFRARED SPECTROSCOPY OF GASEOUS NEGATIVELY CHARGED POLYAROMATIC HYDROCARBONS
The Astrophysical Journal, 787:17 (11pp), 214 June 1 C 214. The American Astronomical Society. All rights reserved. Printed in the U.S.A. doi:1.188/4-637x/787/2/17 LABORATORY INFRARED SPECTROSCOPY OF GASEOUS
More informationNUCLEAR MAGNETIC RESONANCE AND INTRODUCTION TO MASS SPECTROMETRY
NUCLEAR MAGNETIC RESONANCE AND INTRODUCTION TO MASS SPECTROMETRY A STUDENT SHOULD BE ABLE TO: 1. Identify and explain the processes involved in proton ( 1 H) and carbon-13 ( 13 C) nuclear magnetic resonance
More informationAKARI Near-Infrared Spectroscopy Towards Young Stellar Objects
AKARI Near-Infrared Spectroscopy Towards Young Stellar Objects Aleksandra Ardaseva 1,TakashiOnaka 2 1 University of St Andrews, United Kingdom 2 Department of Astronomy, Graduate School of Science, University
More informationExtrasolar Planets: Molecules and Disks
Extrasolar Planets: Molecules and Disks The basic question: Is our solar system typical of what we should affect around other stars (inhabited or not), or is it an unusual freak? One approach is to look
More informationPAPER No.12 :Organic Spectroscopy MODULE No.30: Combined problem on UV, IR, 1 H NMR, 13 C NMR and Mass - Part II
Subject Chemistry Paper No and Title Module No and Title Module Tag 12 : rganic Spectroscopy 30: Combined problem on UV, IR, 1 H NMR, 13 C NMR and Mass Part-II CHE_P12_M30 TABLE F CNTENTS 1. Learning utcomes
More informationCHEM 3760 Orgo I, F14 (Lab #11) (TECH 710)
CHEM 3760 Orgo I, F14 (Lab #11) (TECH 710) Identification of an Unknown by IR PRELAB (PreLab is due before entering the lab.) Every student has to prepare for each experiment by answering the Pre-Laboratory
More information1) What do all waves transport from one place to another?
Pre Quiz 1) What do all waves transport from one place to another? 2) In which of the following scenarios would the Doppler effect be present? a) A police car, with its siren sounding, speeds past you
More informationLecture 18 - Photon Dominated Regions
Lecture 18 - Photon Dominated Regions 1. What is a PDR? 2. Physical and Chemical Concepts 3. Molecules in Diffuse Clouds 4. Galactic and Extragalactic PDRs References Tielens, Ch. 9 Hollenbach & Tielens,
More informationProperties of Electromagnetic Radiation Chapter 5. What is light? What is a wave? Radiation carries information
Concepts: Properties of Electromagnetic Radiation Chapter 5 Electromagnetic waves Types of spectra Temperature Blackbody radiation Dual nature of radiation Atomic structure Interaction of light and matter
More informationMultiphysics Simulation of Polymer-Based Filters for Sub-Millimetre Space Optics
Multiphysics Simulation of Polymer-Based Filters for Sub-Millimetre Space Optics N. Baccichet 1, G. Savini 1 1 Department of Physics and Astronomy, University College London, London, UK Sponsored by: EU
More informationRadio infrared correlation for galaxies: from today's instruments to SKA
Radio infrared correlation for galaxies: from today's instruments to SKA Agata P piak 1 T.T. Takeuchi 2, A. Pollo 1,3, A. Solarz 2, and AKARI team 1 Astronomical Observatory of the Jagiellonian University,
More informationLaser Dissociation of Protonated PAHs
100 Chapter 5 Laser Dissociation of Protonated PAHs 5.1 Experiments The photodissociation experiments were performed with protonated PAHs using different laser sources. The calculations from Chapter 3
More informationkev e - and H + ECR source Shock wave Molecular ices 3 C 2 H 2 C 6 H 6 2 C 3 H 3 Dust impact Europa
B Sivaraman kev e - and H + Shock wave Molecular ices ECR source 3 C 2 H 2 C 6 H 6 Europa Dust impact 2 C 3 H 3 C 6 H 6 Temperature, K 273 K 70 / 80 90 K 50 60 K < 20 K New molecules (ISM) C 60 - C 70
More informationPhysics 224 The Interstellar Medium
Physics 224 The Interstellar Medium Lecture #11: Dust Composition, Photoelectric Heating, Neutral Gas Outline Part I: Dust Heating & Cooling continued Part III: Dust Emission & Photoelectric Heating Part
More information(2) Read each statement carefully and pick the one that is incorrect in its information.
Organic Chemistry - Problem Drill 17: IR and Mass Spectra No. 1 of 10 1. Which statement about infrared spectroscopy is incorrect? (A) IR spectroscopy is a method of structure determination based on the
More informationTHE MID-INFRARED LABORATORY SPECTRA OF NAPHTHALENE (C 10 H 8 ) IN SOLID H 2 O
The Astrophysical Journal, 607:346 360, 2004 May 20 # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE MID-INFRARED LABORATORY SPECTRA OF NAPHTHALENE (C 10 H 8 ) IN SOLID
More informationObserving Habitable Environments Light & Radiation
Homework 1 Due Thurs 1/14 Observing Habitable Environments Light & Radiation Given what we know about the origin of life on Earth, how would you recognize life on another world? Would this require a physical
More informationLecture 2: Molecular Clouds: Galactic Context and Observational Tracers. Corona Australis molecular cloud: Andrew Oreshko
Lecture 2: Molecular Clouds: Galactic Context and Observational Tracers Corona Australis molecular cloud: Andrew Oreshko Classification of Young Stellar Objects (YSOs) Spectral Index Hartmann: Accretion
More informationLecture 6 - spectroscopy
Lecture 6 - spectroscopy 1 Light Electromagnetic radiation can be thought of as either a wave or as a particle (particle/wave duality). For scattering of light by particles, air, and surfaces, wave theory
More informationSpectral Energy Distributions as probes of star formation in the distant Universe
MODULO meeting 2-3 December 2010 Spectral Energy Distributions as probes of star formation in the distant Universe Simona Bovinelli ISSI International Space Science Institute IRAS (1983), ISO (1995) and
More informationCMB. Suggested Reading: Ryden, Chapter 9
CMB Suggested Reading: Ryden, Chapter 9 1934, Richard Tolman, blackbody radiation in an expanding universe cools but retains its thermal distribution and remains a blackbody 1941, Andrew McKellar, excitation
More informationCMB Foreground and separation methods. Astro 448 Yuxi Zhao 12/5/2018
CMB Foreground and separation methods Astro 448 Yuxi Zhao 12/5/2018 Outline CMB foreground overview Thermal Dust AME (spin dust, spinning nanodiamonds? ) Synchrotron Free-free CO Zodiacal light, CIB Component
More information- Strong extinction due to dust
The Galactic Centre - Strong extinction due to dust At optical wavelemgth the absorption is almost total Information from the 21 line, IR and radio 10 Region between and cm 14 10 22 1 arcsec at the distance
More informationEffect of mass attached to the spring: 1. Replace the small stopper with the large stopper. Repeat steps 3-9 for each spring set.
EXERCISE 1: Representing molecular vibrations with spring oscillations A spring is a common model for covalent chemical bonds. One of the interesting interpretations of quantum mechanics is that bonds
More informationInfrared Spectroscopy: Identification of Unknown Substances
Infrared Spectroscopy: Identification of Unknown Substances Suppose a white powder is one of the four following molecules. How can they be differentiated? H N N H H H H Na H H H H H A technique that is
More informationMeasurement of Galactic Rotation Curve
Measurement of Galactic Rotation Curve Objective: The 21-cm line produced by neutral hydrogen in interstellar space provides radio astronomers with a very useful probe for studying the differential rotation
More informationMethyl Formate as a probe of temperature and structure of Orion-KL
Methyl Formate as a probe of temperature and structure of Orion-KL Cécile Favre Århus University - Institut for Fysik og Astronomy (IFA) N. Brouillet (LAB), D. Despois (LAB), A. Baudry (LAB), A. Wootten
More informationA Far-ultraviolet Fluorescent Molecular Hydrogen Emission Map of the Milky Way Galaxy
A Far-ultraviolet Fluorescent Molecular Hydrogen Emission Map of the Milky Way Galaxy (The Astrophysical Journal Supplement Series, 231:21 (16pp), 2017 August) November 14, 2017 Young-Soo Jo Young-Soo
More informationGround State Calculations for Protonated PAHs
15 Chapter 2 Ground State Calculations for Protonated PAHs 2.1 Introduction Ab initio ground electronic state calculations can be used to determine geometries and energies of all possible protonated PAH
More informationLecture 14 Organic Chemistry 1
CHEM 232 Organic Chemistry I at Chicago Lecture 14 Organic Chemistry 1 Professor Duncan Wardrop February 25, 2010 1 CHEM 232 Organic Chemistry I at Chicago Mass Spectrometry Sections: 13.24-13.25 2 Spectroscopy
More informationInterstellar Medium. Alain Abergel. IAS, Université Paris-Sud, Orsay Cedex, France
Interstellar Medium Alain Abergel IAS, Université Paris-Sud, 91405 Orsay Cedex, France ISO Legacy Colloquium, Dec 13, 2006 Main Topics Elemental abundances in the ionised gas of HII regions Interstellar
More informationMore information can be found in Chapter 12 in your textbook for CHEM 3750/ 3770 and on pages in your laboratory manual.
CHEM 3780 rganic Chemistry II Infrared Spectroscopy and Mass Spectrometry Review More information can be found in Chapter 12 in your textbook for CHEM 3750/ 3770 and on pages 13-28 in your laboratory manual.
More informationGalaxy Formation/Evolution and Cosmic Reionization Probed with Multi-wavelength Observations of Distant Galaxies. Kazuaki Ota
Galaxy Formation/Evolution and Cosmic Reionization Probed with Multi-wavelength Observations of Distant Galaxies Kazuaki Ota Department of Astronomy Kyoto University 2013 Feb. 14 GCOE Symposium Outline
More information