Class 3. The PAH Spectrum, what does it tell us??

Size: px
Start display at page:

Download "Class 3. The PAH Spectrum, what does it tell us??"

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

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 information

arxiv: v1 [astro-ph] 7 Feb 2008

arxiv: 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 information

Dust: Grain Populations, Extinction Curves, and Emission Spectra Monday, January 31, 2011

Dust: 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 information

Lecture 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 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 information

Increasing energy. ( 10 4 cm -1 ) ( 10 2 cm -1 )

Increasing 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 information

Planck and Virtual Observatories: Far Infra-red / Sub-mm Specificities

Planck 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 information

Radiant energy is proportional to its frequency (cycles/s = Hz) as a wave (Amplitude is its height) Different types are classified by frequency or

Radiant 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 information

Astrochemistry (2) Interstellar extinction. Measurement of the reddening

Astrochemistry (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 information

University of Groningen. Infrared emission features Boersma, Christiaan

University 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 information

Infrared Spectroscopy

Infrared 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 information

Aromatic Features in M101 HII Regions and Starburst Galaxies

Aromatic 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 information

Chemistry 213 Practical Spectroscopy

Chemistry 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 information

arxiv: v1 [astro-ph.ga] 29 Jun 2011

arxiv: 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 information

Astrochimistry Spring 2013 Lecture 4: Interstellar PAHs NGC HST

Astrochimistry 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 information

2. Infrared spectroscopy

2. 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 information

8: Composition and Physical state of Interstellar Dust

8: 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 information

Simulating chemistry on interstellar dust grains in the laboratory

Simulating 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 information

LABORATORY SPECTROSCOPY OF PROTONATED PAH MOLECULES RELEVANT FOR INTERSTELLAR CHEMISTRY

LABORATORY 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 information

ROTATIONAL SPECTRA OF SMALL PAHs: ACENAPHTHENE, ACENAPHTHYLENE, AZULENE, AND FLUORENE

ROTATIONAL 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 information

SPECTROSCOPY MEASURES THE INTERACTION BETWEEN LIGHT AND MATTER

SPECTROSCOPY 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 information

Lecture 18 Long Wavelength Spectroscopy

Lecture 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 information

CHEM 301: Homework assignment #12

CHEM 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 information

arxiv: v1 [astro-ph.ga] 5 Dec 2018

arxiv: 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 information

Photodissociation Regions Radiative Transfer. Dr. Thomas G. Bisbas

Photodissociation 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 information

Lecture 5. Interstellar Dust: Chemical & Thermal Properties

Lecture 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 information

CHE 325 SPECTROSCOPY (A) CHAP 13A ASSIGN CH 2 CH CH 2 CH CHCH 3

CHE 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 information

Exploring ISM dust with IRSIS. Emmanuel DARTOIS IAS-CNRS

Exploring 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 information

CHEM 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 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 information

Polycyclic Aromatic Hydrocarbon from the Magellanic Clouds

Polycyclic 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 information

Dust emission. D.Maino. Radio Astronomy II. Physics Dept., University of Milano. D.Maino Dust emission 1/24

Dust 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 information

Chapter 12 Mass Spectrometry and Infrared Spectroscopy

Chapter 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 information

A. G. G. M. TIELENS SRON, Kapteyn Astronomical Institute, P.O. Box 800, 9700 AV Groningen, The Netherlands

A. 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 information

Interstellar Dust and Extinction

Interstellar 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 information

Introduction. 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 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 information

PDF hosted at the Radboud Repository of the Radboud University Nijmegen

PDF 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 information

PC Laboratory Raman Spectroscopy

PC 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 information

INTRODUCTION TO MICROWAVE REMOTE SENSING - II. Dr. A. Bhattacharya

INTRODUCTION 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 information

Structure 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? 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 information

Infrared Spectroscopy

Infrared 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 information

Molecular spectroscopy

Molecular 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 information

Organic Compound Identification Using Infrared Spectroscopy. Description

Organic 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 information

The Interstellar Medium in Galaxies: SOFIA Science

The 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 information

Chemical Enrichment of the ISM by Stellar Ejecta

Chemical 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 information

Status of the Diffuse Interstellar Band Problem

Status 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 information

Infrared Spectroscopy An Instrumental Method for Detecting Functional Groups

Infrared 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 information

Infrared spectroscopy Basic theory

Infrared 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 information

Beyond the Visible -- Exploring the Infrared Universe

Beyond 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 information

The High-Energy Interstellar Medium

The 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 information

Midterm Results. The Milky Way in the Infrared. The Milk Way from Above (artist conception) 3/2/10

Midterm 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 information

Classification of spectroscopic methods

Classification 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 information

Welcome to Organic Chemistry II

Welcome 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 information

Introduction to Electromagnetic Radiation and Radiative Transfer

Introduction 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 information

12. Structure Determination: Mass Spectrometry and Infrared Spectroscopy

12. 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 information

Interstellar Medium and Star Birth

Interstellar 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 information

Frequencies and Normal Modes of Vibration of Benz[a]anthracene Radical Ions

Frequencies 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 information

EXPT. 7 CHARACTERISATION OF FUNCTIONAL GROUPS USING IR SPECTROSCOPY

EXPT. 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 information

The NASA Ames PAH IR Spectroscopic Database

The 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 information

Interstellar 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 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 information

The Diffuse Interstellar Bands and Carbon Chains

The 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 information

Wave Description. Transverse and Longitudinal Waves. Physics Department 2/13/2019. Phys1411 Goderya 1. PHYS 1403 Stars and Galaxies

Wave 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 information

University of Groningen. Infrared emission features Boersma, Christiaan

University 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 information

ASTR2050 Spring Please turn in your homework now! In this class we will discuss the Interstellar Medium:

ASTR2050 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 information

LABORATORY INFRARED SPECTRA OF POLYCYCLIC AROMATIC NITROGEN HETEROCYCLES: QUINOLINE AND PHENANTHRIDINE IN SOLID ARGON AND H 2 O

LABORATORY 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 information

Christine 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 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 information

Probing Bonding Using Infrared Spectroscopy Chem

Probing 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 information

Astronomy 106, Fall September 2015

Astronomy 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 information

Molekularne vibracije i IR (infra crvena spektroskopija)

Molekularne 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 information

LABORATORY INFRARED SPECTROSCOPY OF GASEOUS NEGATIVELY CHARGED POLYAROMATIC HYDROCARBONS

LABORATORY 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 information

NUCLEAR MAGNETIC RESONANCE AND INTRODUCTION TO MASS SPECTROMETRY

NUCLEAR 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 information

AKARI Near-Infrared Spectroscopy Towards Young Stellar Objects

AKARI 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 information

Extrasolar Planets: Molecules and Disks

Extrasolar 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 information

PAPER No.12 :Organic Spectroscopy MODULE No.30: Combined problem on UV, IR, 1 H NMR, 13 C NMR and Mass - Part II

PAPER 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 information

CHEM 3760 Orgo I, F14 (Lab #11) (TECH 710)

CHEM 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 information

1) What do all waves transport from one place to another?

1) 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 information

Lecture 18 - Photon Dominated Regions

Lecture 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 information

Properties of Electromagnetic Radiation Chapter 5. What is light? What is a wave? Radiation carries information

Properties 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 information

Multiphysics Simulation of Polymer-Based Filters for Sub-Millimetre Space Optics

Multiphysics 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 information

Radio infrared correlation for galaxies: from today's instruments to SKA

Radio 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 information

Laser Dissociation of Protonated PAHs

Laser 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 information

kev 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

kev 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 information

Physics 224 The Interstellar Medium

Physics 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.

(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 information

THE MID-INFRARED LABORATORY SPECTRA OF NAPHTHALENE (C 10 H 8 ) IN SOLID H 2 O

THE 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 information

Observing Habitable Environments Light & Radiation

Observing 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 information

Lecture 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 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 information

Lecture 6 - spectroscopy

Lecture 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 information

Spectral Energy Distributions as probes of star formation in the distant Universe

Spectral 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 information

CMB. Suggested Reading: Ryden, Chapter 9

CMB. 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 information

CMB Foreground and separation methods. Astro 448 Yuxi Zhao 12/5/2018

CMB 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

- 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 information

Effect of mass attached to the spring: 1. Replace the small stopper with the large stopper. Repeat steps 3-9 for each spring set.

Effect 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 information

Infrared Spectroscopy: Identification of Unknown Substances

Infrared 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 information

Measurement of Galactic Rotation Curve

Measurement 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 information

Methyl Formate as a probe of temperature and structure of Orion-KL

Methyl 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 information

A 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 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 information

Ground State Calculations for Protonated PAHs

Ground 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 information

Lecture 14 Organic Chemistry 1

Lecture 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 information

Interstellar Medium. Alain Abergel. IAS, Université Paris-Sud, Orsay Cedex, France

Interstellar 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 information

More information can be found in Chapter 12 in your textbook for CHEM 3750/ 3770 and on pages in your laboratory manual.

More 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 information

Galaxy 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 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