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Hot Dust in Radio-Loud AGNs

Hot Dust in Radio-Loud AGNs. Wolfram Freudling Space Telescope – European Coordinating Facility. ISOCAM Survey of 3C galaxies Questions: How do SEDs of various AGNs types differ ? Are dust SEDs consistent with Unified Schemes? What heats the dust (AGN vs SB contribution)

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Hot Dust in Radio-Loud AGNs

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  1. Hot Dust in Radio-Loud AGNs Wolfram Freudling Space Telescope – European Coordinating Facility • ISOCAM Survey of 3C galaxies • Questions: • How do SEDs of various AGNs types differ? • Are dust SEDs consistent with Unified Schemes? • What heats the dust (AGN vs SB contribution) • What do we expect at higher redshifts? • Publications: Freudling, Siebenmorgen, Haas, 2003, ApJ Letters 599, 13; Siebenmorgen, Freudling, Krügel, Haas, 2003, A&A, submitted Hot Dust in Radio-Loud AGNs

  2. ISOCAM 3C Survey Siebenmorgen, Freudling, Krügel, Haas, 2003, A&A, submitted • 88 fields in ISOCAM archive include 3C source • All fields homogenously co-added and calibrated • About 50% NLRGs, 25% QSOs, 25% BLRGs • 71 3CR sources detected • In 60 of them evidence for dust Hot Dust in Radio-Loud AGNs

  3. ISOCAM Images of 3C Sources Hot Dust in Radio-Loud AGNs

  4. HST imaging by Martel et al, 1999, ApJS 122, 88 ISOCAM pixel size Hot Dust in Radio-Loud AGNs

  5. Results: SEDs Hot Dust in Radio-Loud AGNs

  6. Mean SEDs Type1 Type2 Freudling, Siebenmorgen, Haas 2003, ApJ Letters 599, L13 Hot Dust in Radio-Loud AGNs

  7. Dust Heating in AGNs Model 1 (e.g. Farrah et al. 2003, MNRAS 345, 585 ; Rowand-Robinson 2000, MNRAS 316, 575) SB heats local dust clouds Cool dust  50K AGN heats dust torus Hot dust  300K

  8. HST imaging of Galactic Nuclei Martel et al. 2000, ApJS 130, 267 Hot Dust in Radio-Loud AGNs

  9. Dust Heating in AGNs Model 2 (AGN effects throughout host galaxy)

  10. Spherical Dust model • Model parameters: • radius • AGN luminosity • extinction Av

  11. Mean SEDs Type1 Type2 Freudling, Siebenmorgen, Haas 2003, ApJ Letters 599, L13 Hot Dust in Radio-Loud AGNs

  12. Best fit radius=2 kpc Radius of dust sphere  Best fit radius=4 kpc Hot Dust in Radio-Loud AGNs

  13. Conclusions 1 • AGNs can heat dust throughout the host • The presence of cold dust does not necessarily imply a SB component  do not use SEDs to identify starburst contribution to dust heating Hot Dust in Radio-Loud AGNs

  14. Differences between AGN and SB heating Hard radation by AGN distroys PAHs Siebenmorgen et al. 2003 Hot Dust in Radio-Loud AGNs

  15. Mean SEDs of local (z<~1) AGNs ISO data suggest that dust throughout the host is heated by the central engine Type1 Type2 SEDs predict PAH spectra Freudling, Siebenmorgen, Haas 2003, ApJL 599, L13

  16. PAH spectra by AGN type ISOPHOT spectra of PG QSOs by Haas et al. 2003 A&A 402, 87 ISOPHOT spectra of four 3CR sources extracted from archive Freudling et al. 2003 ISOPHOT spectra of Seyfert 2s by Clavel et al. 2000 A&A 357, 839 Hot Dust in Radio-Loud AGNs

  17. Dust in high-z QSOs Redshifted local QSOs Freudling et al. 2003, ApJL 599, L13 High-z QSOs Bertoldi et al. 2003, AA 406, L55 Hot Dust in Radio-Loud AGNs

  18. Summary & Conclusions • ISOCAM detected most of the 3C sources within its field of view, mostly because of dust emission. • There is a clear correlation between the AGN type and the peak of the SEDs: • type 1 peak around 40m • 2 100m • PAHs emmission is stronger in type 2 AGNs with same dust luminosity as their type 1 counterparts • AGN can heat dust throughout the host Hot Dust in Radio-Loud AGNs

  19. The End Hot Dust in Radio-Loud AGNs

  20. The End Hot Dust in Radio-Loud AGNs

  21. Dust Heating in AGNs Model 2 (AGN effects throughout host galaxy: Hot Dust in Radio-Loud AGNs

  22. Fitting Procedure Plot data synchrotron stellar dust Hot Dust in Radio-Loud AGNs

  23. Example M82 log L= 10 Av= 25 R=2 kpc Krügel & Siebenmorgen, 1994, AA 288, 929: log L= 10.5 Av=25 R=1 kpc Hot Dust in Radio-Loud AGNs

  24. NO Hot Dust in Radio-Loud AGNs

  25. 0.05 < z < 0.4 Hot Dust in Radio-Loud AGNs

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