Post on 11-Jan-2016
Cumber01.ppt 30.5.2001
Thomas HenningMax Planck Institute for Astronomy, Heidelberg
The Lifecycle of Dust in the UniverseFrom Alpha to Omega
M 31 with Herschel/PACS (70 + 160 μm) + SPIRE (250 μm) (Groves et al. 12; Smith et al. 12, Krause et al. 14; Dust: Draine et al. 13) Dust Emission extends to 25 kpc
Two observationsTwo observations
The Evolution of a Scientist Poster -> Contributed Talk -> Invited Talk -> Organizer -> Summary Talk
Possibility a) Start again b) That is the end …. c) The field comes to an end …
The Taipei tour guide:30% Reality – 70% ImaginationEven new molecule names have been invented during the conference
Hawaii Diamonds
• ~ 55 Talks
• ~ 90 Posters
Important chemical ingredient of the meeting – C,N,O
Are we making progress?10 things we know about dust?
Examples: Depletion studies, Polarisation,FIR emission, Dust properties at high z, SN,GEMS, Experiments
Towards a Dusty Universe – The Infrared Decade
AKARI (06-11) Spitzer (03-09/…) Herschel/Planck (09-13)WISE (09-10)
• Basic understanding of grain properties in galaxies
• Formation and evolution of grains in various environments
• Dust grains as initial seeds for planet formation
Discovery of CDiscovery of C6060 and C and C7070 in a PN in a PN
Red – C60
Blue – C70
Cami et al. (2010, Continuum Subtracted Spitzer Spectrum) Talk by Jeronimo Bernard-Salas
B 68 – From Spitzer to WISE and Herschel
Dust continuum dataModelled by ray tracing
Nielbock et al. 2012, Launhardt et al. 2013: Herschel/EPOS project
T
N
7
Investigated PAHs in the UV – ISM Abundances
DIB spectrum from Jenniskens & DésertMolecules studied: phenanthrene, fluorene, pyrene, benzofluorene, anthracene, benzo[ghi]perylene, fluoranthene, perylene (e.g. Rouille et al. 2012)
First Abundance Determination of PAHs in the ISM: Gredel et al. 11, Tan et al. 11, See also Steglich et al. 2013
The (MW) Facts• Mg, Si, Fe in grains, 50-70% C, 20% O (?)• Amorphous silicates and hydrogenated carbonaceous dust • Broad size distribution• Additional materials in circumstellar environments (crystalline silicates, carbides, nanodiamonds, fullerenes, …)
• Molecular ices in cold clouds• Moderate grain growth in molecular cloudsIS dust system of small particles
Silicates: Henning, ARAA, 48, 21, 2010 Carbonaceous Solids: Jäger et al., EAS Publ. Ser. 46, 293, 2011
Dust Emission Spectrum – Size Distribution
Désert, Boulanger & Puget (1990); See Compiègne et al. (2011)
What is the physical Nature of „PAHs“ and the VSGs?
Dust Emission SpectrumDwarf Galaxy NGC 1569
(Low-metallicity Environment)
Galliano et al. 2003
A Generation of New Models
Compiègne et al. (2011), Jones et al. (2013), Siebenmorgenet al. (2013) …..Isolated C/silicate grains vs. mixed models
Extinction, Scattering, Emission, Polarization
Basic Types of Dust Mixtures
Stardust/SN
Interstellar Dust
Molecular Cloud Dust
Protostellar Dust
Interplanetary DustTime
Original dust formation
UV/cosmic ray processing;Modification by shocks (Destruction/Shattering)
Surface chemistryIce mantlesCoagulation
Dorschner & Henning (1995)Accretion of gas atoms
What are the FIR/mm properties of the materials? • Structural composition of the material (e.g. Jäger et al. 1998, K. Demyk)
• Grain size/agglomeration state (e.g. Henning & Stognienko 96, M. Min) • Material temperature (e.g. Mennella ea. 98, Boudet ea.05, Coupeaud et al. 11 K. Demyk)
• Fe-containing nanoparticles (e.g. Draine & Hensley 2012, 2013)
M 31 with PACS (70 + 160 μm) + SPIRE (250 μm)
Results from Planck (2013)
ß(mm) ~ 1.60±0.06 vs. ß(FIR) ~ 1.88±0.08ß correlates with dust optical depthAtomic phase: 1.53 Molecular phase: 1.65
Dust properties must change …
• Spatial metallicity gradient in MW and other galaxies• Abundance of C-rich stars decreases towards GC• Contribution from ISM dust formation vs. stellar sources = f(t)• Dust properties as function of radiation fields/metallicities
Radius (kpc)Lemasle et al.(2008)
[Fe/H]
Dust in the Andromeda Galaxy
Draine et al. (2013)
Dust-to-gas ratio function goes with metallicityDust Properties in M31 Center similar to dust in s.n.
Origin of the Strong UV Resonance
• Remarkable constancy of peak position (4.60 m-1; variations smaller 1%)
• Peak width varies around mean value of 1.0 m-1 (variations smaller 25%)
• Lack of correlation between variation of peak position and width (except for the widest bumps: systematic shift to larger peak wavenumbers)
• Strength of the feature requires abundant element as part of the carrier
• Feature is pure absorption feature
What is the contribution of absorption in the FUV?
Extinction Curves
Gordon et al. (2003), Different phases of ISM?
Extinction Curves = f(Environment)?
Zafar et al. (2012), Talk by Daniel Perley: SFR does not seem to be the answer … But: Kriek & Conroy (2013) – Bump strength is function of SFRSee also talk about quasars: Simona Gallerani
What is the nature of the UV bump carrier?
• a-C:H nanoparticles (e.g. Schnaiter et al. 1998, Gaballah et al. 2011)
• Large PAHs (e.g. Beegle et al. 1997, Steglich et al. 2010, 2012)
Coronene
HBC
Electronic π-π* transition in sp2 hybridized a-C:H
C42H18
Dust in the Diffuse ISM - InfraredDust in the Diffuse ISM - Infrared
No evidence for crystalline silicates in the galactic diffuse ISM (<2%, e.g., Li & Draine 2001, Jäger et al. 2003, Kemper et al. 2004)
Amorphization by cosmic rays/shock processing in ISM/re-condensation of amorphous silicates in the ISM (Jäger et al. 2003)
3.4 micron absorption feature – aliphatic hydrocarbons (Pendleton & Allamandola 2002, C dust evolution – Mennella+)
Whittet et al. (1997)
See Chiar et al. (2000),Chiar & Tielens (2006),Van Breemen et al. (2011)
Silicate Dust Properties in the Universe
Van Breemen et al. (2011)
• Dust towards GC different
• Diffuse ISM Dust & MC dust different (Av/E(B-V) goes from 3.1 to 5.5)
• Dust in MC cannot grow much larger than a few microns
• Mg-rich dust + Fe + oxides in diffuse ISM X-ray spectr. : Elisa Costantini
• GEMS particles: S. Messenger
• Diversity in QAS systems: M. Aller
Infrared Feature at 3.4 μm
Schnaiter et al. (1999), „Activation“ processes: V. Mennella et al.
Why does interstellar dust exist?
Destruction in diffuse ISM more efficient than production by AGB stars (Draine 2009, Jones & Nuth 2011, Talk by Marco Bocchio)
Even more severe problem at high redshift
Solutions• Dust formation in the cold and „dense“ ISM (Metallicity treshold) (Rémy-Puyer et al. 2013, Talks by F. Galliano+Y. Shi; Zhukovska 2013, GRB?s)• Dust formation in core-collapse SN (Survival in reverse shocks) (Talk by E. Micelotta)
Why does interstellar dust exist?
SN 1987A(Matsuura et al.2011)
• Crab nebula (no reverse shock?): 0.1-0.2 Msun (Gomez + 12)
• Cas A: 0.1 Msun (Barlow+ 10)
• SN 1987A: 0.4-0.7 Msun (Matsuura+ 11)
Predictions: 0.3-0.9 Msun for II-P (Todini & Ferrara 2001, Kozasa et al. 2009)Linking early and late dust masses (Talks: C. Gall, H. Gomez), Dust prop. (P.Owen)Optical data as a function of sp2/sp3 ratio: Jäger, Mutschke & Henning (1998)
Formation of Silicon-based Particles at low T
Si + H2O
SiO + H2O
• Formation of cyclic (SiO)x clusters• Formation of nanoscale amorphous SiO grains
Krasnokutskiet al. (2013,submitted)
Open Questions
• Where is the iron? Where is the oxygen? (Mg/Fe ratio in silicates, Fe-containining nanoparticles, FeS/Fe grains in disks)
• How dust-free are young galaxies? (e.g. Himiko at z=6.6 – 840 Myrs after Big Bang I Zw 18: Gas-to-Dust Ratio 10-6 to 10-5, Fisher ea.13)
• How do dust properties change in extreme environments?
• Source of excess emission at long wavelengths
• What are the main sources of ISM dust?
Optical Data of Amorphous Silicates: MgxFe1-xSiO3
(J. Dorschner, B. Begemann, Th. Henning, C. Jäger and H. Mutschke, A&A 1995)
Increaseof NIR absorptivitywith Fe content(Fe3+ vs. Fe2+)
x=1.0
x=0.4
Near-infrared Extinction LawNear-infrared Extinction Law
Fritz et al. 11
Open Questions
• Where is the iron? Where is the oxygen? (Mg/Fe ratio in silicates, Fe-containining nanoparticles, FeS/Fe grains in disks)
• How dust-free are young galaxies? (e.g. Himiko at z=6.6 – 840 Myrs after Big Bang I Zw 18: Gas-to-Dust Ratio 10-6 to 10-5, Fisher ea.13)
• How do dust properties change in extreme environments?
• Source of excess emission at long wavelengths
• What are the main sources of ISM dust?
Many happy astronomers ….
Happy Birthday!
Remember: There is always better equipment ….
A big „Thank you“ to Franciska Kemper & the LOC/SOC
Cindy Chiu + Hiroyuki Hirashita
Astrophysics of Dust, Rocky Mountains 2003
Cosmic Dust – Near and Far, Heidelberg 2008
The Lifecycle of Dust in the Universe, Taipei 2013
??? – ALMA, ALMA, ALMA 2018