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”

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

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

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

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

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

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

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

16th October - Polarization & AGN Cristina Ramos Almeida

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

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

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 Sy1 Sy1 Sy2 Sy2 Sy1 photon escape prob. > Sy2 photon escape prob. 16th October - Polarization & AGN Cristina Ramos Almeida

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

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

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

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 7582 IC 5063 POLARIZED BROAD LINES ✗ ✔ i FROM MODELLING 43°±19°22° 81°±5°8° 16th October - Polarization & AGN Cristina Ramos Almeida

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 7582 ✗ IC 5063 ✔ POLARIZED BROAD LINES ✔ ✗ i FROM MODELLING 81°±5°8° 43°±19°22° 16th October - Polarization & AGN Cristina Ramos Almeida

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

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

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

Thanks!