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