Table 8: Results of SED fitting for IR-peakers requiring an AGN component. The fit consists in the combination of a simple stellar population and a torus model (Fritz et al. 2006). The 3$\sigma $ ranges for the main geometrical and dust properties of the torus are reported, as well as stellar population ages, extinctions and masses.
ID Type Class z Torus Stellar population Total % AGN
SWIRE phot. spec. spec. $\frac{R_{\rm out}}{R_{\rm in}}$ $\Theta^\dagger$ $\tau_{9.7}$ $\Psi^\ddagger$ $L_{\rm BH}$ $\alpha$ age E(B-V) Mass $L_{\rm IR}$ 8.0 $\mu $m IR
          [deg]   [deg] $[10^{45}~L_\odot]$ index$^\ast$ [106 yr] [mag] $[10^{10}~M_\odot]$ [1011 $L_\odot]$    
EN1_202260 P2,X BLAGN 1.545 100-300 100-140 0.6-2.0 0-30 0.79-1.58 -1.0 50-300 0.2-0.4 3.98-10.0 4.23-7.05 53-71% 10-62%
EN1_282078 P3 BLAGN 1.685 20-100 60-100 6.0-10.0 0-60 1.58-3.16 -1.0 50-100 0.6-0.8 3.98-6.31 10.4-23.7 53-65% 2-40%
EN1_279954 P3,pow BLAGN 2.409 30-100 60-140 0.6-3.0 0-50 1.58-3.16 -0.5 10-100 0.6-1.0 2.51-15.8 15.4-27.1 49-63% 5-31%
EN1_339960 P3 BLAGN 1.475 30-100 60-140 0.6-1.0 0-50 0.20-0.32 -1.0 50-500 0.2-0.6 3.98-25.1 3.83-5.50 39-49% 10-48%
EN2_275226 P2 BLAGN 1.710 30-100 100-140 1.0-6.0 0-20 0.32-1.58 -0.5 10-50 0.6-0.8 1.58-2.51 15.3-26.1 37-54% 1-20%
EN2_273717 P3 BLAGN 1.800 30-100 100-140 0.3-3.0 0-20 1.00-2.51 -0.5 10-50 0.6-0.8 1.00-2.51 26.4-38.2 48-62% 2-24%
EN2_172324 P3 NLAGN 1.739 30-100 60-140 0.3-2.0 40-90 1.00-3.16 -1.0 50-100 0.4-0.6 15.8-25.1 16.4-23.4 32-45% 3-39%
EN2_165986 P3,pow BLAGN 2.163 20-100 80-140 3.0-10.0 30-50 3.16-10.0 -1.0 10-100 0.2-0.6 1.00-10.0 11.5-18.6 64-80% 20-53%
LH_574364 P3,R NLAGN 1.474 100-300 100-140 0.3-3.0 30-70 1.58-1.99 -0.5 50-100 0.4-0.8 2.51-6.31 7.42-9.01 55-63% 30-77%
$^\dagger$ The aperture angle $\Theta$ is computed starting from the equatorial plane, and it is doubled, accounting for equatorial symmetry.
$^\ddagger$ The viewing angle $\Psi$ is computed starting from the polar axis.
$^\ast$ Source power law slope in UV-optical-IR range ( $\lambda~ L[\lambda]\propto\lambda^\alpha$).

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