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Silicate Emission in Active Galaxies

[OIV]25.89. [NeII]12.81. PAH11.3. PAH12.7. PAH7.7/8.6. PAH6.2. Silicate Emission in Active Galaxies. Mario Schweitzer. MPE. E. Sturm, D. Lutz, R. Genzel, S. Veilleux, D. Rupke, D.-C. Kim, B. Groves, D. Tomono, Hagai Netzer.

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Silicate Emission in Active Galaxies

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  1. [OIV]25.89 [NeII]12.81 PAH11.3 PAH12.7 PAH7.7/8.6 PAH6.2 Silicate Emission in Active Galaxies Mario Schweitzer MPE E. Sturm, D. Lutz, R. Genzel, S. Veilleux, D. Rupke, D.-C. Kim, B. Groves, D. Tomono, Hagai Netzer Emission From The Torus Or (And) Extended Emission ??? QUEST Quasar And ULIRG Evolution Study

  2. Si-O stretching Si-O-Si bending F.Molster et al. (2004)

  3. 10m Silicate emission in Type 1 AGN Original prediction of torus models, but not really observed until very recently… Suggested modifications to explain absence of silicate emission: • changes of grain size distribution (Laor & Draine 1993, Maiolino et al. 2001) • Special geometries, e.g. tapered disks (Efstathiou & Rowan-Robinson 1995) • Clumpy tori (Nenkova et al. 2002) q : power law exponent for radial clump distribution ß: power law exponent of size distribution 0.1 1 10m 100 1000 Opt. thin dust, different size distributions (Laor & Draine 93) Type 1 SED for different radial distributions of clumps (Nenkova et al. 02)

  4. Spitzer finally finds silicate emission in luminous AGNs (PG QSOs) Siebenmorgen et al. 2005 Hao et al. 2005

  5. PG-QSOs (Type 1) QUEST (Veilleux et al.) Schweitzer et al. 2006

  6. Conditions in the silicate emitting region Siebenmorgen et al. 2005 Hao et al. 2005 Weingartner & Draine 2001

  7. The Unification model sublimation temperature between 800 and 1500 K (Kimura et al. 2002) But estimated temperatures are ~ 200 K  too cold

  8. Silicate emission – the Torus? Silicate emission in Type 2 objects! NGC 4725: Type 2 AGN from Ho sample (SINGS data, Kennicutt et al.) QSO2s: Sturm et al. 2006 IRASF10214+4724: Teplitz et al. 2006

  9. cold temperatures + silicate emission in type 2  possibly spatially extended silicate emission Model the silicate emission

  10. Modelling silicate emission  spatial extension Illuminated cloud models: Brent Groves (MPA)

  11. ? AGN Silicate emitting dust Radius: ~200 L460.5pc Dust outside sublimation Radius: > ~0.5 L460.5pc

  12. ? AGN Silicate emitting dust Radius: ~200 L460.5pc Dust outside sublimation Radius: > ~0.5 L460.5pc

  13. …and at lower luminosityA testcase for the spatial extension of the silicate emission region NGC 3998 (Liner 1.9) Sturm et al. 2005 L (2-10 keV) = 3 x 10 ^41 ergs/s (Ptak et al. 2004) (from feature ratio and ISM silicate emissivity profile). T~180K

  14. fluxdensity [Jy] C8.6 - I11.7 I8.6 2MASS JHK-band (NED) Follow-up SUBARU (COMICS) observation of NGC3998 A preliminary result (together with DaigoTomono) image size : 200 pc2

  15. = image size : 200 pc2

  16. Subtracting the normalized PSF (center images on maximum) -

  17. ~35pc First image of extended (residual) silicate emission in AGN this is a upper limit since no PSF-correction ! D ~ 35 pc • Using illuminated cloud • models from Brent • Groves (MPA): • D ~ 30 pc = image size : 200 pc2

  18. Conclusions - Silicate emission detected in AGNs over four orders of magnitude in luminosity. Origin in torus or extended emission ? - Arguments for extended emission: • Estimated temperatures (optical thin) are much lower then the sublimation temperature ! 2) Silicate emission has been detected also in type 2 AGNs. 3) For the LINER NGC 3998 we find silicateemission on a scale of D ~ 30 pc (preliminary result) In addition to more Spitzer spectroscopy, these issues call for very high resolution observations and interferometry!

  19. 12.5 µm res. : 0.1´´ (~7 pc) wavelength: 12.5 µm NGC 1068: ~2/3 of emission extended (overlapping the NLR) and likely isotropic (Cameron et al. 1993, Bock et al. 1998, 2000, Tomono et al. 2001)

  20. Details not well fit by standard astronomical silicate Sturm et al. 2005 peak shift: - temperature - grain sizes - crystallization - composition used synthetic ISM-extinction curve from Weingartner and Draine (2001)

  21. Rdust: ~200 L460.5pc L46~ 4.84e-3 (estimated by scaling Lbol of PG0050+124 by ratio of x-ray (2-10keV) luminosities)  Rdust ~ 14 pcD ~ 30 pc From Imaging : D ~ 35 pc Fitting of NGC3998: Using illuminated cloud models: Brent Groves (MPA) Hotter component also needed 2e3 erg s-1cm-2 2e5 erg s-1cm-2

  22. 1100 K 180 K ISM extinction curve by Weingartner and Draine (2001) wavelength [µm] Jacquelin Kessler-Silacci et al.

  23. The QUEST-project Evolution of Activity in Massive Gas-Rich Mergers -study basic physical processes involved in -creating massive early type hosts -growing/feeding of massive BH in galaxy mergers 50% of cosmic star formation at high z and most of the big BH´s appear to be formed in this process  understand this process better in the local univers  apply knowledge to high z. -Test the Sanders-scenario …

  24. ~1pc Rout < 100 pc ~100 pc – few kpc M~ 107 – 1010 M Rout < 35 pc : NGC 1068 (Keck 8-25 µm Bock et al 00) NGC 4151 (Gemini 10 & 18 µm Radomski et al 03)

  25. fluxdensity [Jy] S11.7 C8.6 c11.7 - I11.7 1.88 x I8.6 2MASS JHK-band (NED) Follow-up SUBARU (COMICS) observation of NGC3998 A preliminary result (together with DaigoTomono) image size : 200 pc2

  26. Similar Galactic SEDs: flared, passive irradiated protostellardisks Dullemond et al. 2001, 2004 … but of course cannot be scaled simply!

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