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Cumber01 30.5.2001

Thomas Henning Max Planck Institute for Astronomy, Heidelberg. _______________. The Lifecycle of Dust in the Universe From Alpha to Omega. M 31 with Herschel/PACS (70 + 160 μ m) + SPIRE (250 μ m) (Groves et al. 12; Smith et al. 12, Krause et al. 14; Dust: Draine et al. 13)

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Cumber01 30.5.2001

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  1. Thomas Henning Max Planck Institute for Astronomy, Heidelberg _______________ The Lifecycle of Dust in the Universe From 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 Cumber01.ppt 30.5.2001

  2. Hawaii Diamonds Twoobservations 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% Imagination Even new molecule names have been invented during the conference

  3. Are we making progress? 10 things we know about dust? Examples: Depletion studies, Polarisation, FIR emission, Dust properties at high z, SN, GEMS, Experiments • ~ 55 Talks • ~ 90 Posters • Important chemical ingredient of the meeting – C,N,O

  4. 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

  5. Discovery of C60and C70 in a PN Red – C60 Blue – C70 Cami et al. (2010, Continuum Subtracted Spitzer Spectrum) Talk by Jeronimo Bernard-Salas

  6. B 68 – From Spitzer to WISE and Herschel T N Dust continuum data Modelled by ray tracing Nielbock et al. 2012, Launhardt et al. 2013: Herschel/EPOS project

  7. _______________ Investigated PAHs in the UV – ISM Abundances DIB spectrum from Jenniskens & Désert Molecules 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

  8. 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 clouds • IS dust system of small particles Silicates: Henning, ARAA, 48, 21, 2010 Carbonaceous Solids: Jäger et al., EAS Publ. Ser. 46, 293, 2011

  9. Dust Emission Spectrum – Size Distribution __________ What is the physical Nature of „PAHs“ and the VSGs? Désert, Boulanger & Puget (1990); See Compiègne et al. (2011)

  10. Dust Emission Spectrum Dwarf Galaxy NGC 1569 (Low-metallicity Environment) __________ Galliano et al. 2003

  11. A Generation of New Models Compiègne et al. (2011), Jones et al. (2013), Siebenmorgen et al. (2013) …..Isolated C/silicate grains vs. mixed models Extinction, Scattering, Emission, Polarization

  12. Basic Types of Dust Mixtures Original dust formation Stardust/SN UV/cosmic ray processing; Modification by shocks (Destruction/Shattering) Interstellar Dust Surface chemistry Ice mantles Coagulation Molecular Cloud Dust Protostellar Dust Time Interplanetary Dust Accretion of gas atoms Dorschner & Henning (1995)

  13. 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)

  14. Results from Planck (2013) __________ ß(mm) ~ 1.60±0.06 vs. ß(FIR) ~ 1.88±0.08 ß correlates with dust optical depth Atomic phase: 1.53 Molecular phase: 1.65

  15. Dust properties must change … [Fe/H] Radius (kpc) Lemasle et al. (2008) • 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

  16. Dust in the Andromeda Galaxy __________ Draine et al. (2013) Dust-to-gas ratio function goes with metallicity Dust Properties in M31 Center similar to dust in s.n.

  17. 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?

  18. Extinction Curves Gordon et al. (2003), Different phases of ISM?

  19. 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 SFR See also talk about quasars: Simona Gallerani

  20. 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 C42H18 HBC Electronic π-π* transition in sp2 hybridized a-C:H

  21. Dust in the Diffuse ISM - Infrared Whittet et al. (1997) See Chiar et al. (2000), Chiar & Tielens (2006), Van Breemen et al. (2011) 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+)

  22. Silicate Dust Properties in the Universe • 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 Van Breemen et al. (2011)

  23. Infrared Feature at 3.4 μm Schnaiter et al. (1999), „Activation“ processes: V. Mennella et al.

  24. 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)

  25. 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)

  26. Formation of Silicon-based Particles at low T Si + H2O SiO + H2O Krasnokutski et al. (2013, submitted) • Formation of cyclic (SiO)x clusters • Formation of nanoscale amorphous SiO grains

  27. 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?

  28. Optical Data of Amorphous Silicates: MgxFe1-xSiO3 Increase of NIR absorptivity with Fe content (Fe3+ vs. Fe2+) x=0.4 x=1.0 (J. Dorschner, B. Begemann, Th. Henning, C. Jäger and H. Mutschke, A&A 1995)

  29. Near-infraredExtinction Law Fritz et al. 11

  30. 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?

  31. Many happy astronomers ….

  32. Happy Birthday!

  33. Remember: There is always better equipment ….

  34. 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 A big „Thank you“ to Franciska Kemper & the LOC/SOC Cindy Chiu + Hiroyuki Hirashita

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