AGN dust model of 3CR sources

1. AGN dust model of 3CR sources Frank Heymann (PhD), Martin Haas, EndrikKrűgel, Christian Leipski • MIR imaging & spectroscopy • ISM dust model & PAH • vectorized Monte Carlo model • SED of a clumpy AGN torus CenA (ESO)

2. 1) Ground based MIR imaging Nuclear activity in nearby galaxies Surface brightness  AGN viz. starbursts 10m telescopes

3. 1) Ground based MIR imaging Nuclear activity in nearby galaxies Surface brightness  AGN viz. starbursts unresolved resolved 10m telescopes Siebenmorgen et al. (2008)

4. ELT 42m MIR surface brightness diagnostics up to D ~ 500Mpc

5. 2) MIR spectroscopy PAH No PAH Silicate emission Siebenmorgen et al. (2004, 2005)

6. 3) Spitzer photometry of 3CR sources • powerfull AGN: 178MHz flux limited, isotropic sample • 23 quasars, 38 radio galaxies (Spitzer GTO: Fazio ) • 1 < z < 2.5  rest frame 1.6-10µm Haas et al. (2008)

7. 3) Spitzer photometry of 3CR sources • powerfull AGN: 178MHz flux limited, isotropic sample • 23 quasars, 38 radio galaxies (Spitzer GTO: Fazio ) • 1 < z < 2.5  rest frame 1.6-10µm • SED consistent with unification: • Quasar: ~flat • RG: reddened quasar + host • 24μm surveys biased to type I Haas et al. (2008)

8. 4) Spitzer spectroscopy of 3CR sources mean SED normalised to 178 MHz luminosity • Quasar (11) ~ flat RG (9): reddened quasar + host • no PAH similar emission line ratios Leipski et al. (2010)

9. 5) Herschel observations of 3CR sources at z<1 (proposed by Haas + 19 CoIs) filling the gap between Spitzer + SCUBA/MAMBO

10. 3D Monte Carlo radiative transfer models ISM dust model PAH: SB emission & AGN destruction MC model clumpy AGN torus models CenA (ESO)

11. 1) ISM dust 2010 Abundances [X/H in ppm]: 31Si + 150aC + 50gr + 30PAH solar neighborhood extinction Si + aC: 60Å < a <0.2-0.3µm ~ a-3.5 Graphite : 5Å < a < 80 Å~a-3.5 PAH : 30 C + 200 C

12. 2) PAH emission Radiativetransfer in the nuclei of star bursts Nucleus of NGC1808 Distribution of stars + “Hot spots” Tutokov & Krűgel(1978); Siebenmorgen et al. (2001)

13. 2) PAH emission Radiativetransfer in the nuclei of star bursts PAH cross section Siebenmorgen et al. (2001), Draine & Li (2007); Tielens (2008)

14. SED library for SB • www.eso.org/~rsiebenm • luminosity • size • mass Siebenmorgen et al. (2007)

15. SMG at high z Efstathiou & Siebenmorgen (2009)

16. 2) PAH destruction Eo T [K] tcool time Unimolecular dissociation Arrhenius form: tdis~ exp(Eo/kT) / ν0«tcool~ 1s Tmin = Eo/k ln(ν0) ~2000K; Eo~ 5eV; ν0 = 1013Hz ΔE = 3NckTmin ~ 0.1 Nc.Eb=> Nc < 2 ΔE /[eV] (PAH unstable) tabs ~ 1h Tielens (2005) ; Micelotta et al. (2010) ; Siebenmorgen & Krűgel (2010)

17. 2) PAH destruction Eo Arrhenius form: tdis~ exp(Eo/kT) / ν0«tcool~ 1s Tmin = Eo/k ln(ν0) ~2000K; Eo~ 5eV; ν0 = 1013Hz ΔE = 3NckTmin ~ 0.1 Nc.Eb=> Nc < 2 ΔE /[eV] (PAH unstable) single hard photon : independent of distance many soft photons : ~inner torus Tielens (2005) ; Micelotta et al. (2010) ; Siebenmorgen & Krűgel (2010)

18. 3) Monte Carlo • Arbitrary dust distribution • Pseudo adaptive mesh geometry Krűgel (2006)

19. Monte Carlo • Source emits “photon packages” of equal energy geometry source

20. Monte Carlo • absorption/ scattering / no interaction = - ln(ζ) geometry source inter-action dust temperature

21. Monte Carlo • Photons escape model cloud geometry source inter-action temperature detection

22. Multiple photons at a time: MC parallelization • Challenges • Cell locked when hit byphoton • Parallel random number generator(Mersene Twister) • Computer games Graphical Processing Units (CUDA) Heymann (2010, PhD)

23. Comparison of 2 ray tracing codes Dust sphere: AV = 1000mag, heated by star Benchmark = ‘Dusty’ code (Iveciz et al. 1999): unphysical at faint flux levels

24. 1D Sphere T* = 2500K ρ(r) = const. MC versus benchmark 1 AV=10 100 1000 mag ~5% for 0

25. MC methods

26. 2D benchmark Disk: T* = 5800K L * = Lsun ρ(r) : hydro static equilibrium (Chiang & Goldreich 1997) Pascucci et al. (2004)

27. 2D benchmark 1 = 10 100 face-on edge-on ~10% for 0

28. PAH in 3D Monte Carlo + PAH • store PAH absorption events of each cell • compute PAH emission • neglect PAH self absorption

29. PAH in 3D Monte Carlo + PAH

30. 4) clumpy AGN torus - density structure edge-on face-on 3D models: Heymann (PhD) Schartmann et al. (2008) MIDI: Tristram (2007) Statistical model: Nenkova et al.(2002, 2008)

31. Shadows caused by clump structure dark side: cold bright side: hot 10μm emission face-on

32. Number of clouds  SED of AGN Quasar RG

33. Mean SED of 3CR sources  Data: Haas et al (2008), Leipski et al. (2010)

34. MIR observations consistent with unified scheme. Dust model of the diffuse ISM for extinction and emission. PAH destruction by hard photons. Monte Carlo dust radiative transfer model including PAH using vectorised computing technology. Clumpy AGN torus model consistent with SED of 3CR sources. Conclusion

35. PAH in a mono-energetic heating bath if | Uf– Ui– hν | < ½ ΔUf : Afi = KνFν/ hν Siebenmorgen & Krűgel (2010)

36. PAH replenishment Vertical mixing in torus? ℓ /v┴ = texp> NC tabs Siebenmorgen & Krűgel (2010)

37. AGN andhard photons (EUV, soft X-ray)

38. 4) IRS spectroscopy of 3CR sources • Quasar (10) : ~ flat • RG (9): reddened quasar +host • similar emission line ratios • no PAH Leipski et al. (2010)