from the theoretical unified model to ngc 1068 : new uv ... · the case of non-collimated winds :...
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![Page 1: From the theoretical Unified Model to NGC 1068 : new UV ... · The case of non-collimated winds : NGC 1068 Marin, Goosmann & Dovciak (2012) Marin et al. (in prep.) Raban et al. (2009)](https://reader035.vdocuments.mx/reader035/viewer/2022080722/5f7bd44c06602a6c63248350/html5/thumbnails/1.jpg)
From the theoretical Unified Model to NGC 1068 : new UV/optical constraints on the AGN reprocessing regions
Frédéric Marin
René W. GoosmannC. Martin GaskellDelphine PorquetGiorgio MattMichal Dovciak
Brussels - 2012
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Goals
AGNs : several emission and reprocessing regions→ radiative coupling
Regions spatially unresolvedReprocessing and scattering polarizeSpectropolarimetry as a diagnostic tool
: to obtain a coherent model of the polarization resulting from the radiative coupling
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Goals
AGNs : several emission and reprocessing regions→ radiative coupling
Regions spatially unresolvedReprocessing and scattering polarizeSpectropolarimetry as a diagnostic tool
: to obtain a coherent model of the polarization resulting from the radiative coupling
: to derive new constraints on the geometry and composition from the observations
![Page 4: From the theoretical Unified Model to NGC 1068 : new UV ... · The case of non-collimated winds : NGC 1068 Marin, Goosmann & Dovciak (2012) Marin et al. (in prep.) Raban et al. (2009)](https://reader035.vdocuments.mx/reader035/viewer/2022080722/5f7bd44c06602a6c63248350/html5/thumbnails/4.jpg)
Goals
AGNs : several emission and reprocessing regions→ radiative coupling
Regions spatially unresolvedReprocessing and scattering polarizeSpectropolarimetry as a diagnostic tool
: to obtain a coherent model of the polarization resulting from the radiative coupling
: to derive new constraints on the geometry and composition from the observations
Radio-quiet, thermal AGNs
![Page 5: From the theoretical Unified Model to NGC 1068 : new UV ... · The case of non-collimated winds : NGC 1068 Marin, Goosmann & Dovciak (2012) Marin et al. (in prep.) Raban et al. (2009)](https://reader035.vdocuments.mx/reader035/viewer/2022080722/5f7bd44c06602a6c63248350/html5/thumbnails/5.jpg)
Linear polarization
UV and optical scattering- electron (Thomson) scattering
![Page 6: From the theoretical Unified Model to NGC 1068 : new UV ... · The case of non-collimated winds : NGC 1068 Marin, Goosmann & Dovciak (2012) Marin et al. (in prep.) Raban et al. (2009)](https://reader035.vdocuments.mx/reader035/viewer/2022080722/5f7bd44c06602a6c63248350/html5/thumbnails/6.jpg)
Linear polarization
UV and optical scattering- electron (Thomson) scattering
Thomson scattering phase function
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Linear and circular polarization
UV and optical scattering- electron (Thomson) scattering- dust (Mie) scattering
Linear polarization Circular polarization
Steinacker et al. (2002)
Angel et al. (1976)
S = I,0,0,0
S = I,Q,U,0 S = I,Q,U,V
![Page 8: From the theoretical Unified Model to NGC 1068 : new UV ... · The case of non-collimated winds : NGC 1068 Marin, Goosmann & Dovciak (2012) Marin et al. (in prep.) Raban et al. (2009)](https://reader035.vdocuments.mx/reader035/viewer/2022080722/5f7bd44c06602a6c63248350/html5/thumbnails/8.jpg)
Polarization dichotomy
Observed dichotomy - pole-on
parallel* polarizationnegative P
- edge-onperpend. polarizationpositive P
* Parallel / perpendicular polarization : E-vector aligned / orthogonal with the small scale radio structure
Edge-on
Pole-on
P
P
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Modeling with STOKES
STOKES : Monte Carlo radiative transfer code
Spectropolarimetry & polarization mappingMultiple scatteringSeveral scattering regions
From isolated, reprocessingregions to a complex, three-component AGN model
Goosmann & Gaskell (2007)Marin et al. (2012)
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Isolated region : polar winds
Ionized polar windsτ ~ 0.3 θ ~ 30°
Goosmann & Gaskell (2007)Marin et al. (2012)
Thomson scattering→ λ-independent
Perpendicular (positive) P
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Isolated region : equatorial inflow
Radiation supported discτ ~ 1 θ ~ 10°
Antonucci (1984)Smith et al. (2004) Goosmann & Gaskell (2007)Marin et al. (2012)
Thomson scattering→ λ-independent
Parallel (negative) P
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Isolated region : dusty torus
Circumnuclear dust regionτ ~ 750 θ ~ 30°
Goosmann & Gaskell (2007)Marin et al. (2012)
Mie scattering→ λ-dependent
Perpendicular P
Graphite feature (2175 Å)
57°
41°
70°
81°
19°
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Coupled region : AGN model
3-component AGN
Marin & Goosmann (2011)Marin et al. (2012)
Pole-on : para/perp polarization
Edge-on : max P λ-independent
84°
73°
60°
46°
26°
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Impact of morphology and composition
Marin et al. (2012)
θop
30°
θop
45°
θop
60°
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Impact of morphology and composition
Inflow between torus and BLR
- geometrically thin- optically thick (1 < τ < 3)- < 1% P
Marin et al. (2012)Smith et al. (2002)
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Impact of morphology and composition
Polar scattering dominated AGN
- torus 30° < θop
< 45°
- optically thick winds- optically thin inflow
Marin et al. (2012)
Smith et al. (2002/2004)
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Impact of morphology and composition
Torus geometry
- θop
> 60°
- optically thick - high P- clumpy structure
Marin et al. (2012)
Kay (1994)
Hönig & Kishimoto (2010)Nenkova et al. (2003/2008)
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Impact of morphology and composition
Torus-collimated outflows
- optically thin τ < 1 - high P- clumpy structure- are they really collimated ?
Marin et al. (2012)Ogle et al. (2003)
Kay (1994)
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The case of non-collimated winds : NGC 1068
Marin, Goosmann & Dovciak (2012)Marin et al. (in prep.)
Raban et al. (2009)
Outflows out of the plane-of-the-skyInvestigating the broken symmetry Credits : Alix Videlier
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The case of non-collimated winds : NGC 1068
Marin et al. (in prep.)
Fine-tuning of the polar and azimuthal tilting angle needed
Goosmann & Matt (2011)
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Capetti et al. (1995)Kishimoto (1999)Marin, Goosmann & Dovciak (2012)Marin et al. (in prep.)
The case of non-collimated winds : NGC 1068
Polarization mapping
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The case of non-collimated winds : NGC 1068
Marin et al. (in prep.)
Circular polarization (Milky Way dust model)
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Summary and perspectives
Unified model new constraints : - geometrically thin, 1< τ < 3 inflowing medium between the BLR and the torus - with torus-collimated outflows → τ < 1 - torus more likely to have a θ
op > 60°
- polar scattering dominated AGN → torus 30° < θop
< 45°
To be further explored : - fragmented media
torus winds
- non-axisymmetric winds (NGC 1068)hollow winds ?
Das et al. (2006)Kartje & Königl (1994)