1. Testing the AGN unified model using spectropolarimetry
Cristina Ramos Almeida Andrés Asensio Ramos, María Jesús Martínez González, Rafael Manso Sáinz, José Antonio Acosta Pulido & the CanariCam AGN team “Los Piratas”

2. Modeling Clumpy Torus Models
Torus dust grains absorb optical & UV photons from matter accretion  re-emission in the infrared (peaking at mid-IR  5-30 μm).
Dust distributed in clumps instead of homogeneously filling torus volume (Nenkova et al. 2002; Hönig et al. 2006; Schartmann et al. 2008).
Nenkova et al. (2002)
16th October - Polarization & AGN Cristina Ramos Almeida

3. Isolation of Torus emission
Observations
Isolation of Torus emission
IR range (mid-IR) key to constrain parameters of torus models.
Goal: isolation of torus emission (Ro< 10 pc; interferometry & mid-IR).
Large aperture data (e.g. ISO, Spitzer, IRAS) contaminated with circunnuclear stellar emission.
High-spatial resolution infrared observations (e.g., CanariCam, T-ReCS, Michelle, VISIR) key to isolate torus emission.
16th October - Polarization & AGN Cristina Ramos Almeida

4. Isolation of Torus emission
Observations
Isolation of Torus emission
8 m Gemini
85 cm Spitzer
16th October - Polarization & AGN Cristina Ramos Almeida

5. Mid-IR imaging: space (Spitzer/IRAC) vs
Mid-IR imaging: space (Spitzer/IRAC) vs. ground (Gemini/T-ReCS) observations
Díaz-Santos (2009, PhD)

6. RA et al. 2009, 2011; Alonso-Herrero et al. 2011
Observations
RA et al. 2009, 2011; Alonso-Herrero et al. 2011
Ground-based subarcsecond resolution mid-IR imaging data for 21 nearby Seyfert galaxies.
Compilation of near-IR nuclear fluxes from the literature of similar resolutions as mid-IR data.
Herschel far-IR data also available (GT + GO programmes).
AGN-dominated SEDs = torus emission (Sy2) & torus+AGN emission (Sy1).
16th October - Polarization & AGN Cristina Ramos Almeida

7. NIR + MIR spectral energy distributions
Results
NIR + MIR spectral energy distributions
Posible poner la figura en la que comparaba con la SED de baja resolucion, es mucho mas interesante!!!
16th October - Polarization & AGN Cristina Ramos Almeida

8. SED modelling BayesClumpy
Bayesian code to fit the clumpy models of Nenkova et al. 2008a,b.
PCA decomposition + Neural networks to approximate Clumpy Database (6 parameters-based models).
Solution to the Clumpy Database degeneracy 
Possibility of interpolating within the database 
Simultaneous fit of both SED + spectrum 
Prediction of next observation to add to SED 
Available for the astrophysical community 
Asensio Ramos & Ramos Almeida 2009, 2012
16th October - Polarization & AGN Cristina Ramos Almeida

9. 16th October - Polarization & AGN Cristina Ramos Almeida

10. Circinus NGC 7469 NIR data from NACO / VLT (Prieto et al. 2010)
MIR data from T-ReCS /Gemini-South (Packham et al. 2005; RA et al. 2011)
NIR data from NACO / VLT (Prieto et al. 2010)
Circinus
NGC 7469
16th October - Polarization & AGN Cristina Ramos Almeida

11. Are the obscuring tori of Type 1 and 2 Seyferts different?
Results
Are the obscuring tori of Type 1 and 2 Seyferts different?
NIR+MIR emission reproduced with small tori (Ro< 6 pc)
16th October - Polarization & AGN Cristina Ramos Almeida

12. Are the obscuring tori of Type 1 and 2 Seyferts different?
Results
Are the obscuring tori of Type 1 and 2 Seyferts different?
Sy1 tori covering factors < Sy2 tori covering factors
Sy Sy1
Sy Sy2
Sy1 photon escape prob. > Sy2 photon escape prob.
16th October - Polarization & AGN Cristina Ramos Almeida

13. Are the obscuring tori of Type 1 and 2 Seyferts different?
Results
Are the obscuring tori of Type 1 and 2 Seyferts different?
-Expected from warped disk torus models (Lawrence & Elvis 2010)
-also from X-ray observations of Seyfert galaxies (Ricci et al. 2011)
Ver si es Mueller o muller o como
Lawrence & Elvis (2010)
-Highly inclined Seyfert 1 tori:
Bi-conical outflows (SINFONI; Müller-Sanchez et al. 2011)
Accretion disk orientation from X-ray data (Nandra et al. 2007)
16th October - Polarization & AGN Cristina Ramos Almeida

14. Are the obscuring tori of Type 1 and 2 Seyferts different?
Results
Are the obscuring tori of Type 1 and 2 Seyferts different?
If all Seyfert nuclei are identical, as simple unification predicts, only the viewing angle determines the classification.
Our results suggest that the classification as Type-1 or Type-2 may also depend on the intrinsic properties of the torus.
Schartmann et al. (2008)
16th October - Polarization & AGN Cristina Ramos Almeida

15. Are the obscuring tori of Type 1 and 2 Seyferts different?
Project
Are the obscuring tori of Type 1 and 2 Seyferts different?
Origin of unification scheme for Seyfert galaxies (Antonucci & Miller 1985)  detection of polarized broad lines in NGC 1068 nuclei.
Only 30-50% of nearby Sy2s show a Sy1-type polarized spectrum (Tran 2001). Implications?
1) not all Seyferts harbour a hidden BLR (Tran 2001, 2003; Gu & Huang 2002)
2) distribution of dust within the torus and its inclination not as simple as predicted by the unified model.
16th October - Polarization & AGN Cristina Ramos Almeida

16. Are the obscuring tori of Type 1 and 2 Seyferts different?
Project
Are the obscuring tori of Type 1 and 2 Seyferts different?
Results from our modelling with torus models could explain lack of polarized broad lines in 50-70% of nearby Seyfert 2 galaxies.
The torus has to have a determined orientation (close to edge-on) and enough clumps to make the broad lines visible in polarized light.
GALAXY NGC IC 5063
POLARIZED
BROAD LINES ✗ ✔
i FROM
MODELLING 43°±19°22° 81°±5°8°
16th October - Polarization & AGN Cristina Ramos Almeida

17. Are the obscuring tori of Type 1 and 2 Seyferts different?
Project
Are the obscuring tori of Type 1 and 2 Seyferts different?
Results from our modelling with torus models could explain lack of polarized broad lines in 50-70% of nearby Seyfert 2 galaxies.
The torus has to have a determined orientation (close to edge-on) and enough clumps to make the broad lines visible in polarized light.
NGC ✗ IC ✔
POLARIZED
BROAD LINES ✔ ✗
i FROM
MODELLING 81°±5°8° 43°±19°22°
16th October - Polarization & AGN Cristina Ramos Almeida

18. Are the obscuring tori of Type 1 and 2 Seyferts different?
Project
Are the obscuring tori of Type 1 and 2 Seyferts different?
Results from our modelling with torus models could explain lack of polarized broad lines in 50-70% of nearby Seyfert 2 galaxies.
The torus has to have a determined orientation (close to edge-on) and enough clumps to make the broad lines visible in polarized light.
Comparison between RA11+AH11 results and a homogeneous data set of spectropolarimetric data.
16th October - Polarization & AGN Cristina Ramos Almeida

19. Are the obscuring tori of Type 1 and 2 Seyferts different?
Futre observations
Are the obscuring tori of Type 1 and 2 Seyferts different?
Homogeneous dataset of polarized optical spectra of a representative sample of Seyfert galaxies for which we have constraints on their torus properties.
ISIS/WHT observations scheduled in Jan 2013  16 objects.
FORS2/VLT observations requested in 2013A  18 objects.
Sample contains similar numbers of Seyfert 1, 1.2, 1.5, 1.9 and 2 types  study how polarization signal varies between types.
16th October - Polarization & AGN Cristina Ramos Almeida

20. Futre observations GOALS
Analize in a consistent way linear polarization signal and high angular resolution infrared data using torus models.
Confirm whether or not the lack of polarized broad lines in 50-70% of Sy2 population due to low torus inclinations and/or small covering factors.
Directly compare between linear polarization signal in Sy1s and Sy2s.
16th October - Polarization & AGN Cristina Ramos Almeida

21. Thanks!