DUST2016, Garching, Sept 2016
|
|
|
- Cecil Townsend
- 5 years ago
- Views:
Transcription
1 Emmanuel Dartois, IAS, Orsay, France Ivan Alata, Markus Bender, Karine Beroff, Marin Chabot, Gustavo A. Cruz- Diaz, Marie Godard, Aurélie Jallat, Rafael Martín-Doménech, Guillermo M. Muñoz Caro, Thomas Pino, Daniel Severin, Christina Trautmann DUST2016, Garching, Sept 2016
2 Outline( Context VUV Hydrocarbons production from a-ch dust Application to DISM Modeling of a PDR CRs SHI of ISM carbonaceous dust grain analogues Lupus 3 dark cloud ESO/F. Comeron(
3 Some carbonaceous solids observed in the ISM (Nano1)( Diamond( Fullerenes( AIBs1PAHs(:(( Class(A(to(C( Amorphous(( carbon( Hydrogenated(( amorphous(carbon( + organic matter Ice(mantles(( residues(
4 Hydrogenated amorphous carbons (a-c:h or HAC) DISM CH stretch abs. observed against IR bkgd sources Viehmann et al. A&A 2004 Pendleton(&(Allamandola(ApJ(2002( Pendleton et al Sun( UGC12158((Credit(NASA/ESA( Dartois,(Geballe,(Pino(et(al.(2007(
5 ISM (ext. galaxies) ***Arom.*CH*UPPER*LIMIT* OBSERVED* IRAS* * OLEF.* OLEF./AROM.* BACKBONE* Dartois,(Geballe,(Pino(et(al.(2007( Precursor Substrate
6 Hydrogenated amorphous carbons (a-c:h or HAC) CH stretch abs. Galactic ISM CH bendings abs. extragalactic DISM Godard et al. 2013, Sandford et al e.g. Sandford et al. 1995, Pendleton et al. ApJ 1994; Duley et al. ApJ 1994, 1998; Dartois et al 1997 τ (3.4)(:( 2.6%(to(35%((lab(HAC)(of(cosmic(C(( Dartois & Munoz Caro 2007 e.g. Risaliti et al. 2006, Imanishi et al. 2006; Mason et al. 2004, 1998; Pendelton et al 1994 τ(6.85)(~(0.12(τ(silicates)( 15%(+17%(of(the((cosmic( carbon( Up(to(40%(in(extreme(cases(?(
7 VUV Hydrocarbons molecules detections C 2, C 3, C 2 H 2, CCH, c-c 3 H 2, C 4 H. PDR: Photon Dominated Regions Top-down chemistry? Dense, cold molecular gas C 2 H C 3 H 2 C 3 H + Pety(et(al.(2005( One-dimensional Photo-Dissociation Region, The Horsehead (PDR) Guzman(et(al.(2015(
8 Objectives Study the evolution of a-c:h under simulated ISM conditions Interaction with VUV photons & Cosmic rays MgF 2( Cutoff( 115nm( Lyman-alpha nm LABORATORY* < E photon > = 8.6 ev/photon Ф= 2.7 x photon.cm -2.s -1 Madrid(2013( G.(Adolfo,(G.(M.(Munoz(Caro( ASTRO*MODEL* Chen(et(al.(2014;(Cruz1Diaz(et(al.(2014( Gredel(et(al.(1989( Test astrophysical models with the photoproducts H 2 formation Formation of hydrocarbons in PDRs regions. Astrophysical timescales
9 a-c:h Vacuum*chamber* Experiments T~10K* 45 * IR*Beam** IR*detector* VUV* Diaphragm** Beam*spliUer* RF*cavity* H2* VUV*source* P H2 =*0.75*mbar* I. Alata Bunch*of*ions* Irradiation at T=10 K TPD 5K/min QMS* Quadrupole*Mass* *Spectrometer* P ~ 2x10-8 mbar P ~ mbar
10 To enhance detection limits, both a-c:h and a-c:d analogues Optical depth a- C:D a-c:d a-c:h Number of N (C-H) & N (C-D) a-c:d a-c:h Wavenumber destruction cross-section σ CH (VUV) = 3 ± cm 2 Mennella(et(al.(1999,(2001( Alata(et(al.(2014( Gadallah(et(al.(2011,2013( σ CH (VUV) = 1(to(5( (10 19( cm 2( σ CH (VUV) similar (
11 Mean VUV penetration depth ( nm) measured ~ 80 nm (SOLEIL Synchrotron DISCO Beam line). Formation on the surface & in the volume UV-VUV Post irradiation TPD 5h irradiation then TPD 5K/min D2 Blank exp.
12 Photolytic H 2 formation rate CH abundance( extinction( Yield( Destruction cross-section( VUV photons flux( VUV Rate coefficient
13 VUV H 2 Rate coefficient With 5-10% C locked into a-c:h & PDR: χ/n(h) up to 0.25 R c up to cm 3 s -1 This(mechanism(can( provide(high(h 2 ( formadon(rates(at(low( to(high(grain(t( Habart(et(al.(2004(
14 Other photolytic products: CD 4 C 2 D y C 3 D y C 4 D y a-c:d Alata(et(al.(2015;(Jallat(2015(
15 CH 4 C 2 H y C 3 H y C 4 H y a-c:h Alata(et(al.(2015;(Jallat(2015(
16 Model(implementadon:( a1c:h(+(vuv(photon(!(a1c:h(+(c x H y (( Photoproduced ( ( (Yield( ( ( ((((Photolydc(rate( species ( ( ( ( ((%) ( ( ( ( ((10 14 s 1 )(( ( H 2 ( ( ( ( ( ( (96.5(((±3.0)( ( ( (2.79( (10 3 (( } CH 4 ( ( ( ( ( (3.0((((±1.0)( ( ( (86( Model(I( C 2 H 2 ( ( ( ( ( (0.081((((±0.060) ( (2.3(( C 2 H 4 ( ( ( ( ( (0.195((((±0.072) ( (5.6(( C 2 H 6 ( ( ( ( ( (0.246((((±0.063) ( (7.1(( } Model(II( C 3 H 4 ( ( ( ( ( (0.042((((±0.036) ( (1.2(( C 3 H 6 ( ( ( ( ( (0.114((((±0.057) ( (3.3(( C 3 H 8 ( ( ( ( ( (0.075((((±0.060) ( (2.2(( C 4 H 4 ( ( ( ( ( (0.009( ( ( ( (1( C 4 H 6 ( ( ( ( ( (0.027( ( ( ( (1(( C 4 H 8 ( ( ( ( ( (0.027( ( ( ( (1( C 4 H 8 ( ( ( ( ( (0.027( ( ( ( (1( } Model(III( Alata(et(al.(2015;(Jallat(2015(
17 1st step Meudon Code: Le(Pedt(et(al.(2006( Radiative transfer + Chemical reactions + Thermal balance A. Jallat Horsehead(nebula( T( (100(K(( n H ( ( (cm3(( χ( (60(Draine(units(( ζ(=( (s 11 ( [S]/n H (=(3.5x10 16 (( N H (cm -3 )* Distance to the star*
18 2nd step Nahoon Code: Wakelam(2006( Time dependence of a-ch perturbation Abundance / N H* C 4 H* +a-c:h photolysis* Initial* Abundance ratio* Distance to the star*
19 Abundance( Abundance ratio( CCH( c-c 3 H( C 4 H( c-c 3 H 2( PDR advection front velocity: ~ 1 km/s Alata(et(al.(2015;(Jallat(2015( d(0.5a V ) ~ cm, equivalent to yrs
20 Take home message VUV Bulk of the interstellar grains as important as surface a-c:h (& polyaromatic dust of AIBs-PAHs) photolytic reactions! formation of H 2 & hydrocarbons in the ISM Reduce gap between observed and modeled hydrocarbons abundances in PDRs Destruction timescale! in line with PDR advection front velocity (1 km/s) Models chemical network! include highly hydrogenated hydrocarbon species.
21 CRs(in(Diffuse(ISM(&(clouds:( ( (( ( ( (SHI(of(ISM(carbonaceous(dust((grain(analogues( Top-down chemistry? Dense, cold molecular gas C 2 H C 3 H 2 C 3 H + Pety(et(al.(2005( One-dimensional Photo-Dissociation Region, The Horsehead (PDR) Guzman(et(al.(2015(
22 GSI (Darmstadt) QMS* Quadrupole*Mass* *Spectrometer* IR*detector* Ion*Beam** a[c:h* 45 * Ion*Beam** VUV* Vacuum*chamber* Mass spectrometer a-c:h sample Irradiation at T= K + TPD 5K/min FTIR a-c:h sample Ion Beam
23 IR monitoring cross section of the solid phase processing Xe 0.6 GeV
24 H 2 CH 4 C 2 H y C 3 H y C 4 H y a-c:h Dartois(et(al.(submived(to(A&A( Ion*Beam** Cosmic rays release carbonaceous species Feeds the ladder of large gaseous C species
25 GSI (Darmstadt) 300K QMS* Ion*Beam** Post Irradiation TPD 5K/min 100K 40K
26 Dartois(et(al.(2016(submived(to(A&A(
27 Xe 0.6 GeV
28 Dartois(et(al.(2016(submived(to(A&A(
29 Relative abundance f (Z) Atomic number Z Φ(Z,E) Φ(Z,E) MeV/nucleon
30 Se(Z,E) f (Z) σ(z,e)(=(σ(se(z,e))( + η(se) Φ(Z,E) R GCR( d [s 11 ]=( ( (σ(z,e) f(z)(φ(z,e) de( CR
31 R d GCR [s -1 ] 8x10-16 s -1 (for ζ = 3.5x10-16 s -1 ) n X n tot a few η(x) e τ d f[n(x)] Diffuse medium (τd << 1) CR insufficient to be significant high energy CR penetrates deep in dense regions Photodissociation e τd! secondary UV induced (10 3/10-4 at AV > 7) abundance increases to values closer to observations and models (Guzmán et al. 2015; Alata et al. 2015; Pety et al. 2012).
32 One(more(slide ( " SHI in CR, desp. low abundance, have a role to play " CRs less significant for a-c:h in DISM " CRs induce a top-down chemistry for refractory dust grains in dense clouds " CRs radiolysis participate to the erosion of icy grains see poster by C. Jäger Sabri(et(al.(2015( " CRs participate to the replenishing of the dense cloud gas phase by ice e- sputtering e.g(dartois(et(al.(2013;( Rothard(et(al.(2016( " Lab eval needed, many space processes are concomitant (CRs, surface, thermal, UV, shocks ) Fantasdc(4(
33 I.(Alata( L.(Gavilan( E.(Dartois(( A.(Jallat((( M.(Chabot( G.(M.(Muñoz(Caro( G.(A.(Cruz(Diaz( T.(Pino( K.(Beroff(( R.(Mar n1doménech( M.(Bender( D.(Severin( C.(Trautmann(( Thank you! M.(Godard(
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
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
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
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
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
UV photodesorption of intact molecules and of photofragments from solid formaledhyde and methanol
UV photodesorption of intact molecules and of photofragments from solid formaledhyde and methanol Mathieu Bertin, Xavier Michaut, Claire Romanzin, Géraldine Féraud, Pascal Jeseck, Laurent Philippe, Harold
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
Unscrambling the Egg. Yvonne Pendleton NASA Ames Research Center. JWST Workshop Nov. 14, 2017
Unscrambling the Egg Yvonne Pendleton NASA Ames Research Center JWST Workshop Nov. 14, 2017 From interstellar dust to new stars and planets Comparisons between material forming new planetary systems and
The Interstellar Medium
The Interstellar Medium Fall 2014 Lecturer: Dr. Paul van der Werf Oortgebouw 565, ext 5883 pvdwerf@strw.leidenuniv.nl Assistant: Kirstin Doney Huygenslaboratorium 528 doney@strw.leidenuniv.nl Class Schedule
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,
Galactic dust in the Herschel and Planck era. François Boulanger Institut d Astrophysique Spatiale
Galactic dust in the Herschel and Planck era François Boulanger Institut d Astrophysique Spatiale Motivation Dust emission Dust models Dust life cycle Planck early results Dust polarisation Outline Dust
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
19. Interstellar Chemistry
19. Interstellar Chemistry 1. Introduction to Interstellar Chemistry 2. Chemical Processes & Models 3. Formation & Destruction of H 2 4. Formation & Destruction of CO References Duley & Williams, "Interstellar
MOLECULES IN THE CIRCUMNUCLEAR DISK OF THE GALACTIC CENTER
MOLECULES IN THE CIRCUMNUCLEAR DISK OF THE GALACTIC CENTER Implications from Chemical Modeling Nanase Harada 1, Denise Riquelme 1, Serena Viti 2, Karl Menten 1, Miguel Requena-Torres 1, Rolf Güsten 1,
Dust. The four letter word in astrophysics. Interstellar Emission
Dust The four letter word in astrophysics Interstellar Emission Why Dust Dust attenuates and scatters UV/optical/NIR Amount of attenuation and spectral shape depends on dust properties (grain size/type)
IR Spectroscopy and physicochemical effects on astrophysical ices produced by energetic ions collisions
IR Spectroscopy and physicochemical effects on astrophysical ices produced by energetic ions collisions Ana Lucia de Barros Physics Department Centro Federal de Educação Tecnológica Celso Suckow da Fonseca
Physics and Chemistry of the Interstellar Medium
Physics and Chemistry of the Interstellar Medium Sun Kwok The University of Hong Kong UNIVERSITY SCIENCE BOOKS Sausalito, California * Preface xi The Interstellar Medium.1.1 States of Matter in the ISM
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
Astrochemistry and Molecular Astrophysics Paola Caselli
School of Physics and Astronomy FACULTY OF MATHEMATICS & PHYSICAL SCIENCES Astrochemistry and Molecular Astrophysics Paola Caselli Outline 1. The formation of H 2 2. The formation of H 3 + 3. The chemistry
The KInetic Database for Astrochemistry
The KInetic Database for Astrochemistry Valentine Wakelam and the KIDA team Laboratory astrophysics of Bordeaux France ICE Interstellar chemical models Compute species abundances as a function of time
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
Interstellar Chemistry
4 Interstellar Chemistry Pascale Ehrenfreund Leiden Observatory, Leiden, The Netherlands The space between the stars, called the interstellar medium (ISM), is composed primarily of H and He gases incorporating
Astrophysics of Gaseous Nebulae and Active Galactic Nuclei
SECOND EDITION Astrophysics of Gaseous Nebulae and Active Galactic Nuclei Donald E. Osterbrock Lick Observatory, University of California, Santa Cruz Gary J. Ferland Department of Physics and Astronomy,
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 -------------------------------------------------
Lecture 6: Molecular Transitions (1) Astrochemistry
Lecture 6: Molecular Transitions (1) Astrochemistry Ehrenfreund & Charnley 2000, ARA&A, 38, 427 Outline Astrochemical processes: The formation of H2 H3 formation The chemistry initiated by H3 Formation
2- The chemistry in the. The formation of water : gas phase and grain surface formation. The present models. Observations of molecules in the ISM.
2- The chemistry in the ISM. The formation of water : gas phase and grain surface formation. The present models. Observations of molecules in the ISM. 1 Why studying the ISM chemistry? 1- The thermal balance,
Magnetospheric Ion Implantation in the Icy Moons of Giant Planets
Magnetospheric Ion Implantation in the Icy Moons of Giant Planets Giovanni Strazzulla INAF Osservatorio Astrofisico di Catania NWO visitor (May-July 2012) gianni@oact.inaf.it; http://web.ct.astro.it/weblab/
Diffuse Interstellar Medium
Diffuse Interstellar Medium Basics, velocity widths H I 21-cm radiation (emission) Interstellar absorption lines Radiative transfer Resolved Lines, column densities Unresolved lines, curve of growth Abundances,
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
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
Astrochemistry the summary
Astrochemistry the summary Astro 736 Nienke van der Marel April 27th 2017 Astrochemistry When the first interstellar molecules were discovered, chemists were very surprised. Why? Conditions in space are
Radioresistance of adenine to cosmic rays
Radioresistance of adenine to cosmic rays Gabriel Vignoli Muniz ; Christian F. Mejía ; Rafael Martinez; Basile Auge; Hermann Rothard; Alicja Domaracka and Philippe Boduch muniz@ganil.fr Centre de Recherche
Interstellar molecules uncover cosmic rays properties
Interstellar molecules uncover cosmic rays properties Solenn Vaupre, P. Hily-Blant, C. Ceccarelli, G. Dubus, S. Gabici and T. Montmerle Institute of Planetology and Astrophysics of Grenoble (IPAG) Oct
Effects of Massive Stars
Effects of Massive Stars Classical HII Regions Ultracompact HII Regions Stahler Palla: Sections 15.1, 15. HII Regions The salient characteristic of any massive star is its extreme energy output, much of
Cosmic-ray induced diffusion, reactions and destruction of molecules in interstellar ices
Juris Kalvāns Engineering Research Institute «Ventspils International Radio Astronomy Center» of Ventspils University College, Inženieru 101, Ventspils, Latvia, LV-3601 (VIRAC) Cosmic-ray induced diffusion,
21. Introduction to Interstellar Chemistry
21. Introduction to Interstellar Chemistry 1. Background 2. Gas Phase Chemistry 3. Formation and Destruction of H 2 4. Formation and Destruction of CO 5. Other Simple Molecules References Tielens, Physics
The Dusty Universe. Joe Weingartner George Mason University Dept of Physics and Astronomy
The Dusty Universe Joe Weingartner George Mason University Dept of Physics and Astronomy To astronomers, dust means: sub micron solid grains (1 micron = 1 m = 10 6 m = one millionth of a meter) Typical
Relaxation of energized PAHs
Relaxation of energized PAHs 2018 1 st year PhD student Supervisor: Dr. Christine Joblin May 16, 2018 Mid-Infrared Spectra Emission features 3.3, 6.2, 7.7, 8.6, 11.2, 12.7 µm Vibrational modes of PAHs
arxiv: v1 [astro-ph.ga] 21 Nov 2014
![arxiv: v1 [astro-ph.ga] 21 Nov 2014](/thumbs/93/114376943.jpg "arxiv: v1 [astro-ph.ga] 21 Nov 2014")
The cycling of carbon into and out of dust arxiv:1411.5877v1 [astro-ph.ga] 21 Nov 2014 Anthony P. Jones, a, Nathalie Ysard a, Melanie Köhler a, Lapo Fanciullo a, Marco Bocchio a, Elisabetta Micelotta a,
Astrochemical Models. Eric Herbst Departments of Chemistry and Astronomy University of Virginia
Astrochemical Models Eric Herbst Departments of Chemistry and Astronomy University of Virginia Chemical Models Gas-phase reactions 1000 s of reactions Grain-surface reactions Abundances, columns, spectra
Galactic Observations of Terahertz C+ (GOT C+): CII Detection of Hidden H2 in the ISM
Galactic Observations of Terahertz C+ (GOT C+): CII Detection of Hidden H2 in the ISM Bill Langer GOT C+ Team: P. Goldsmith, D. Li, J. Pineda, T. Velusamy, & H. Yorke Jet Propulsion Laboratory, California
7. Dust Grains & Interstellar Extinction. James R. Graham University of California, Berkeley
7. Dust Grains & Interstellar Extinction James R. Graham University of California, Berkeley Visual Extinction Presence of interstellar gas or nebulae has a long history Existence of absorbing interstellar
Formation and evolution of a complex organic molecule : from interstellar ices to asteroids
Formation and evolution of a complex organic molecule : from interstellar ices to asteroids V. Vinogradoff, S. Bernard, Duvernay F., C. Le Guillou, Chiavassa T., L. Remusat Molecules in Interstellar ices
ESO in the 2020s: Astrobiology
ESO in the 2020s: Astrobiology Izaskun Jimenez-Serra (IIF Marie Curie Fellow, ESO) Leonardo Testi (ESO), Paola Caselli (MPE) & Serena Viti (UCL) 1 From the ISM to the Origin of Life Molecular clouds (Pre-stellar
Photochemistry and Astrochemistry: Photochemical Pathways to Interstellar Complex Organic Molecules
pubs.acs.org/cr Photochemistry and Astrochemistry: Photochemical Pathways to Interstellar Complex Organic Molecules Karin I. O berg* Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge,
The Physics of the Interstellar Medium
The Physics of the Interstellar Medium Ulrike Heiter Contact: 471 5970 ulrike@astro.uu.se www.astro.uu.se Matter between stars Average distance between stars in solar neighbourhood: 1 pc = 3 x 1013 km,
Present Understanding of Comet Nucleus Physical and Chemical Composition
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 OF A GAS-GRAIN CHEMICAL CODE. Dima Semenov MPIA Heidelberg
OUTLINE OF A GAS-GRAIN CHEMICAL CODE Dima Semenov MPIA Heidelberg MOTTO OF ASTROCHEMISTRY CODE DEVELOPMENT We had 5 ODE solvers, 9 Jacobi matrix inversion routines, several approaches to calculate reaction
Carbamic acid produced by the UV/EUV irradiation of interstellar ice analogs ABSTRACT. 12 CO 2 by 13 CO 2 in the starting mixture. They ascribed this
A&A 464, 253 257 (2007) DOI: 10.1051/0004-6361:20066631 c ESO 2007 Astronomy & Astrophysics Carbamic acid produced by the UV/EUV irradiation of interstellar ice analogs Y.-J. Chen 1,M.Nuevo 1,J.-M.Hsieh
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
Improving the basic ISM model (some bells and whistles...)
Improving the basic ISM model (some bells and whistles... CO as a tracer of cold dense gas Although we are interested in H2 from a theoretical viewpoint, it s not what we observe. First energy-level of
Supernova Remnants and Cosmic. Rays
Stars: Their Life and Afterlife Supernova Remnants and Cosmic 68 th Rays Brian Humensky Series, Compton Lecture #5 November 8, 2008 th Series, Compton Lecture #5 Outline Evolution of Supernova Remnants
PDR Modelling with KOSMA-τ
PDR Modelling with KOSMA-τ M. Röllig, V. Ossenkopf-Okada, C. Bruckmann; Y. Okada, N. Schneider, U. Graf, J. Stutzki I. Physikalisches Institut, Universität zu Köln The KOSMA-τ PDR Code 1-D, spherical geometry
Lecture 5. Interstellar Dust: Optical Properties
Lecture 5. Interstellar Dust: Optical Properties 1. Introduction 2. Extinction 3. Mie Scattering 4. Dust to Gas Ratio 5. Appendices References Spitzer Ch. 7, Osterbrock Ch. 7 DC Whittet, Dust in the Galactic
A resonant energy transfer toy model for CO ice
A resonant energy transfer toy model for CO ice Octavio Roncero Inst. Física Fundamental, CSIC Madrid (Spain) octavio.roncero@csic.es Outline Introduction 2 Förster Resonance Energy transfer 3 Reactivity
3/1/18 LETTER. Instructors: Jim Cordes & Shami Chatterjee. Reading: as indicated in Syllabus on web
Astro 2299 The Search for Life in the Universe Lecture 9 Last time: Star formation Formation of protostars and planetary systems This time A few things about the epoch of reionization and free fall times
Galaxies of Many Colours: Star Formation Across Cosmic Time. z=0, t= /-0.037x10 9 years (Now)
Galaxies of Many Colours: Star Formation Across Cosmic Time z=0, t=13.798+/-0.037x10 9 years (Now) And if you want to study the initial conditions for star formation the colour is black Dense Gas SDC335:
Astrochimistry Spring 2013
Astrochimistry Spring 2013 Lecture 3: H2 Formation NGC 7023 - HST Julien Montillaud 1st February 2013 Outline I. The most abundant molecule in the Universe (6 p.) I.1 Relative abundances I.2 Historical
The 158 Micron [C II] Line: A Measure of Global Star Formation Activity in Galaxies Stacey et al. (1991) ApJ, 373, 423
![The 158 Micron [C II] Line: A Measure of Global Star Formation Activity in Galaxies Stacey et al. (1991) ApJ, 373, 423](/thumbs/81/83212129.jpg "The 158 Micron [C II] Line: A Measure of Global Star Formation Activity in Galaxies Stacey et al. (1991) ApJ, 373, 423")
The 158 Micron [C II] Line: A Measure of Global Star Formation Activity in Galaxies Stacey et al. (1991) ApJ, 373, 423 Presented by Shannon Guiles Astronomy 671 April 24, 2006 Image:[C II] map of the galaxy
Chapter 10 The Interstellar Medium
Chapter 10 The Interstellar Medium Guidepost You have begun your study of the sun and other stars, but now it is time to study the thin gas and dust that drifts through space between the stars. This chapter
Warm Molecular Hydrogen at high redshift with JWST
Warm Molecular Hydrogen at high redshift with JWST Pierre Guillard Institut d Astrophysique de Paris Université Pierre et Marie Curie he Warm H 2 with JWST Outline and take-home messages 1. Observations
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
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
Cover Page. The handle holds various files of this Leiden University dissertation.
Cover Page The handle http://hdl.handle.net/1887/58690 holds various files of this Leiden University dissertation. Author: Ligterink, N.F.W. Title: The astrochemical factory: A solid base for interstellar
Hydrogenation of solid hydrogen cyanide HCN and methanimine CH 2 NH at low temperature
Hydrogenation of solid hydrogen cyanide HCN and methanimine CH 2 NH at low temperature P. Theule, F. Borget, F. Mispelaer, G. Danger, F. Duvernay, J. C. Guillemin, and T. Chiavassa 5 534,A64 (2011) By
NEARBY GALAXIES AND ALMA
NEARBY GALAXIES AND ALMA Jean Turner, UCLA nearby galaxies close-up views of star formation & nuclear fueling on scales of GMCs and star clusters - where & how do galaxies form stars? - where does gas
FUSE results concerning the diffuse and translucent clouds. Franck Le Petit
FUSE results concerning the diffuse and translucent clouds Franck Le Petit Outline I Diffuse and transluscent clouds a) Generalities b) The Meudon PDR code II Results of the FUSE survey a) H2 and HD in
Cosmic rays in the local interstellar medium
Cosmic rays in the local interstellar medium Igor V. Moskalenko Igor V. Moskalenko/NASA-GSFC 1 LMC (Magellanic Cloud Emission Nuclear Data-2004/09/28, Line Survey: Smith, Points) Santa Fe R - H G - [S
The Excited and Exciting ISM in Galaxies: PDRs, XDRs and Shocks as Probes and Triggers
The Excited and Exciting ISM in Galaxies: PDRs, XDRs and Shocks as Probes and Triggers Marco Spaans (Groningen) Rowin Meijerink (Groningen), Paul van der Werf (Leiden), Juan Pablo Pérez Beaupuits (Bonn),
arxiv: v2 [astro-ph.ga] 5 Jul 2017
![arxiv: v2 [astro-ph.ga] 5 Jul 2017](/thumbs/71/66133656.jpg "arxiv: v2 [astro-ph.ga] 5 Jul 2017")
Astronomy & Astrophysics manuscript no. Horsehead-chemical-study_2columns_to_publish c ESO 2017 July 5, 2017 A new study of the chemical structure of the Horsehead nebula: the influence of grain-surface
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
arxiv: v2 [astro-ph] 7 May 2007
![arxiv: v2 [astro-ph] 7 May 2007](/thumbs/90/104090637.jpg "arxiv: v2 [astro-ph] 7 May 2007")
Hydrocarbon anions in interstellar clouds and circumstellar envelopes T. J. Millar, C. Walsh and M. A. Cordiner arxiv:0705.0639v2 [astro-ph] 7 May 2007 Astrophysics Research Centre, School of Mathematics
6. Interstellar Medium. Emission nebulae are diffuse patches of emission surrounding hot O and
6-1 6. Interstellar Medium 6.1 Nebulae Emission nebulae are diffuse patches of emission surrounding hot O and early B-type stars. Gas is ionized and heated by radiation from the parent stars. In size,
Cosmic Rays in the Interstellar Medium. Nick Indriolo University of Illinois at Urbana- Champaign
Cosmic Rays in the Interstellar Medium Nick Indriolo University of Illinois at Urbana- Champaign November 3, 2010 Stormy Cosmos Cosmic Ray Basics Energetic charged particles and nuclei protons, alpha particles,
Physical Processes in Astrophysics
Physical Processes in Astrophysics Huirong Yan Uni Potsdam & Desy Email: hyan@mail.desy.de 1 Reference Books: Plasma Physics for Astrophysics, Russell M. Kulsrud (2005) The Physics of Astrophysics, Frank
A World of Dust. Bare-Eye Nebula: Orion. Interstellar Medium
Interstellar Medium Physics 113 Goderya Chapter(s): 10 Learning Outcomes: A World of Dust The space between the stars is not completely empty, but filled with very dilute gas and dust, producing some of
Physics and chemistry of the interstellar medium. Lecturers: Simon Glover, Rowan Smith Tutor: Raquel Chicharro
Physics and chemistry of the interstellar medium Lecturers: Simon Glover, Rowan Smith Tutor: Raquel Chicharro This course consists of three components: Lectures Exercises Seminar [Wed., 2-4] [Thu., 4-5]
arxiv: v1 [astro-ph.ga] 5 Nov 2015
![arxiv: v1 [astro-ph.ga] 5 Nov 2015](/thumbs/93/111780665.jpg "arxiv: v1 [astro-ph.ga] 5 Nov 2015")
Astronomy& Astrophysics manuscript no. ach_evolution_paper_iii c ESO 2015 November 6, 2015 Variations on a theme the evolution of hydrocarbon solids: III. Size-dependent properties the optec (s) (a) model
Carbonaceous dust grains in luminous infrared galaxies. Spitzer/IRS reveals a-c:h as an abundant and ubiquitous ISM component ABSTRACT
A&A 476, 1235 1242 (2007) DOI: 10.1051/0004-6361:20077798 c ESO 2007 Astronomy & Astrophysics Carbonaceous dust grains in luminous infrared galaxies Spitzer/IRS reveals a-c:h as an abundant and ubiquitous
arxiv:astro-ph/ v1 15 Mar 2007
Noname manuscript No. (will be inserted by the editor) Sulfur chemistry in the Horsehead An interferometric view of the Horsehead PDR arxiv:astro-ph/0703393v1 15 Mar 2007 J.R. Goicoechea 1 J. Pety 1,2
Published in: LOW-METALLICITY STAR FORMATION: FROM THE FIRST STARS TO DWARF GALAXIES
University of Groningen Interstellar Chemistry Spaans, Marco Published in: LOW-METALLICITY STAR FORMATION: FROM THE FIRST STARS TO DWARF GALAXIES DOI: 10.1017/S1743921308024885 IMPORTANT NOTE: You are
The role of cosmic rays in the formation of interstellar and circumstellar molecules
The role of cosmic rays in the formation of interstellar and circumstellar molecules Maria Elisabetta Palumbo INAF Osservatorio Astrofisico di Catania mepalumbo@oact.inaf.it http://www.oact.inaf.it/weblab/
Interstellar Medium by Eye
Interstellar Medium by Eye Nebula Latin for cloud = cloud of interstellar gas & dust Wide angle: Milky Way Summer Triangle (right) α&β Centauri, Coal Sack Southern Cross (below) Dust-Found in the Plane
Laboratory Simulations of Space Weathering Effects Giovanni Strazzulla INAF Osservatorio Astrofisico di Catania, Italy
Laboratory Simulations of Space Weathering Effects Giovanni Strazzulla INAF Osservatorio Astrofisico di Catania, Italy gianni@oact.inaf.it http://web.ct.astro.it/weblab/ 1 NNNNNNNN kev-mev ions ELECTRONS
Molecular Astrophysics
Optical/NIR studies of the ISM I. i. Brief history, astrophysical context Molecular Astrophysics II. III. Diffuse and translucent molecular clouds i. unresolved problems from observations Required modifications
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
THE ROLE OF LABORATORY IN ASTROPHYSICS: LABORATORY EXPERIMENTS ON ICES AND ASTROPHYSICAL APPLICATIONS. 1 Introduction
THE ROLE OF LABORATORY IN ASTROPHYSICS: LABORATORY EXPERIMENTS ON ICES AND ASTROPHYSICAL APPLICATIONS MIGUEL ÁNGEL SATORRE, MANUEL DOMINGO, OSCAR GOMIS, RAMÓN LUNA Departamento de Física Aplicada, Escuela
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](/thumbs/95/123499834.jpg "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
Symbiotic Stars: an ISO overview. R. Angeloni 1,2, M. Contini 2,1, S. Ciroi 1, P. Rafanelli 1 AJ, , 205. Rodolfo Angeloni May SNA
Silicate Dust in D-type Symbiotic Stars: an ISO overview R. Angeloni 1,2, M. Contini 2,1, S. Ciroi 1, P. Rafanelli 1 AJ, 2007-134, 205 1 Dept. of Astronomy, University of Padova, Italy 2 School of Physics
First results of the UHV system 'LIFE' (Light Irradiation Facility for Exochemistry)
Osservatorio Astronomico di Palermo (INAF-OAPa) First results of the UHV system '' (Light Irradiation Facility for Exochemistry) Antonio Jimenez-Escobar Angela Ciaravella Cesare Cecchi-Pestellini Giuliana
Water in protoplanetary disks: D/H ra4o
Water in protoplanetary disks: D/H ra4o Kenji Furuya, Yuri Aikawa (Kobe Univ) Hideko Nomura (Kyoto Univ) Franck Hersant, Valen4ne Wakelam (Bordeaux Obs) Water - Major Oxygen reservoire - Major ice (+ other
Astronomy. Astrophysics. UV irradiated hydrogenated amorphous carbon (HAC) materials as a carrier candidate of the interstellar UV bump at 217.
DOI: 10.1051/0004-6361/201015542 c ESO 2011 Astronomy & Astrophysics UV irradiated hydrogenated amorphous carbon (HAC) materials as a carrier candidate of the interstellar UV bump at 217.5 nm K. A. K.
Absorption spectroscopy with Herschel/HIFI and IRAM-PdBI : Promises for ALMA
PRISMAS PRobing InterStellar Molecules with Absorption line Studies Absorption spectroscopy with Herschel/HIFI and IRAM-PdBI : Promises for ALMA Maryvonne Gerin Why Absorption Spectroscopy? Sensitivity
Thomas Schwarz-Selinger. Max-Planck-Institut for Plasmaphysics, Garching Material Science Division Reactive Plasma Processes
Max-Planck-Institut für Plasmaphysik Thomas Schwarz-Selinger Max-Planck-Institut for Plasmaphysics, Garching Material Science Division Reactive Plasma Processes personal research interests / latest work
THE NITRILES PROJECT: MOLECULE FORMATION IN THE GALACTIC CENTER
THE NITRILES PROJECT: MOLECULE FORMATION IN THE GALACTIC CENTER JOANNA CORBY (www.astro.virginia.edu/~jfc9va) University of Virginia, Department of Astronomy Advised by Anthony Remijan, National Radio
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
99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park
99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park #5 How do Cosmic Rays gain their energy? I. Acceleration mechanism of CR
Dust in the Diffuse Universe
Dust in the Diffuse Universe Obscuring Effects Chemical Effects Thermal Effects Dynamical Effects Diagnostic Power Evidence for Grains: Chemical Effects Catalyzes molecular hydrogen formation. Depletion
Chapter 4: Astrochemistry: Synthesis and Modelling
Chapter 4: Astrochemistry: Synthesis and Modelling Valentine Wakelam Univ. Bordeaux, LAB, UMR 5804, F-33270, Floirac, France CNRS, LAB, UMR 5804, F-33270, Floirac, France Herma M. Cuppen Theoretical Chemistry,
X-ray Studies of Interstellar and Intergalactic Dust
X-ray Studies of Interstellar and Intergalactic Dust Lia Corrales Columbia University NASA Earth and Space Science Fellow Advised by Frits Paerels X-ray scattering tools for studying the ISM Cygnus X-3: