MIDI Observations of AGNs Walter Jaffe: Leiden Observatory Klaus Meisenheimer:MPIA Heidelberg Konrad

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AGNs with the VLTI
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Cygnus AI
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N1068 ions
NGC 1068
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What do we see with VLTI

• What do we see with VLTI (10 mas)
• at the distance of 14 Mpc? (170pc)
• Radio Jet (maybe optically thick core)
• Narrow Line Region _at_ 14 (too big)
• Dusty torus/disk _at_14 mas (!)
• Broad Line Region _at_ 1 mas (too small)
• Hot Accretion disk _at_ 1 microarcsec ()
• Black Hole (108 Mo) _at_ 0.1 microarcsec

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What do we see from dust?

• What do we expect to see from dust?
• T 1000-30 K (r1 pc -gt 200 pc)
• 1000 K sublimation temperature
• ? 4 ? -gt 100 ?

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Granato plots
Granato et al 1997
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• Old Questions
• Do obscuring torii really exist?
• Are they the same for Sy1/2?
• Details
• optical thickness
• flaring/throat shape
• chemistry
• What supports thick disk/torus?

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What do we see from dust?

• Seyfert 1 Seyfert 2
• Round Flattened
• If optically thick
• Core dominated? Extended
• Silicate emission? Silicate absorption

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• MIDI Prime Targets
• AGNs with unresolved TIMMI2 flux gt 1Jy
• Close, big, bright many UV-points
• NGC 1068, Circinus, Cen A
• Secondary Targets gt1 UV point
• not so close/big/bright
• 10 Sy 12 1 quasar (3C273)
• 1 Starburster

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N1068 uv
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First data plots n1068
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N1068 dirty map
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Pink ellipse
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Circinus Gaussian fit
Two blackbody Gaussians
Log of model flux distribution at 11µm
Tristram et al. 2007
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• Greenhill 2003 Water Masers

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Cen A NGC 5128
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Centaurus A Fluxes
2.0
N
Total flux spectrum
PA108, BL60.3m
PA 37, BL45.3m
1.5
? mostly unresolved
Flux in F Jy
1.0
0.5
0.0
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Wavelength ? µm
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MIDI
1013
1012
Energy ?F? Hz Jy
1011
1010
109
109
1010
1011
1012
1013
1014
Frequency ? Hz
Meisenheimer et al. 2007
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Bulk of the MIR radiation is synchrotron emission
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jet axis
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• Conclusions from 3 detailed
• sources
• Disk Tilt
• Hot inner disk in NGC 1068
• Dust sublimation?
• SiO absorption
• Synchrotron dominance in Cen A
• Evidence for clumpiness

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• New Questions for new sources
• Is there a unified model?
• Disk Tilt?
• SiO absorption/emission?
• Sy 1,2 still a question
• Luminosity/size relation

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3C 273
1.0
ozone band
correlated flux Fcor (2007 Feb 07)
power law fit Fcor ?2.0
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VISIR photometry (1.1", 2007 Mar 01)
Spitzer spectrum (2004 Jan 06)
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Flux F Jy
0.4
0.2
0.0
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Wavelength ? µm
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conclusions

• Preliminary Survey Conclusions
• Most sources detected, many resolved
• Luminosity size relation probably OK
• All look pretty similar, even Sy1/2
• No (or little) SiO features
• No hot inner ridge
• Need more data
• Confirm Lum/Size relation
• Check orientation of disk
• Better SiO information

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conclusions

• Conclusions
• Best studied dust disks
• Agree in size/orientation with H2O masers.
• Disks are smaller than (some) SED predictions,
  and probably clumpy
• NGC1068 disk is tipped wrt both
• jet and ionization cone.
• Interesting dust chemistry.

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conclusions

• NONUNIFIED TORI
• Some are tipped wrt natural axes
• Some arent.
• Some have inner edge at sublimation
• radius. Some dont.
• Some have strong MIR emission
• (Sy 2, quasar). Some dont (RG).
• Basic Sy1/2 unification not yet tested
• but see NGC 4151.