1. Spectral Energy Distribution of the central parsecs of AGN M. Almudena Prieto (IAC) Preston, September 2011

2. PARSEC project  Focus on the nearest and brightest AGN  Widest spectral range coverage  Angular scales < 0.1”  UV + OP + IR + radio Adaptive Optics 1 - 5 µm  θ < 0.1” 8-10 m diffraction 10 - 20 µm  θ < 0.4” HST 0.3 - 0.9 µm  θ < 0.1” VLA-A/ ATCA  θ < 0.1”

3. 1”/parsec Core size in parsecs 1 - 5 µm T2 CenA 16 < 1 T2 Circinus 19 ~ 2 L Sombrero 66 < 12 T2 N1068 70 < 4 L N1097 70 < 11 L M 87 80 < 11 T2 N1365 87 < 6 T1 N1566 96 < 11 L N1052 100 < 13 T2 MCG-05-23-16 168 < 19 T1 N3783 196 < 16 T1 N7469 330 < 26 T1.5 Mrk1239 384 < 40 QSO 3C273 3200 < 180 Some of the nearest …

4. Impact on the Spectral Energy Distribution S1 S2 L cm IR OPUV X S2

5. S1 “+ “ IRAS, ISO, SPITZER, and/or millimetre data L cm IR OPUV X S2

6. S1 average S1 average S2 SEDs central 10 parcsec average S1 average S2 Elvis+ 94: RL quasar template

7. IR core IR(Large-aperture IRcore /Total / core Li N1097 10 41 500 90 % S2/RG CenA 10 42 20 60 % S1 N1566 80 35 % S2 Circinus 10 43 7 80 % S2 N7582 25 70 % S2 N1068 10 99 % S2 N5506 10 44 1 99 % S1 N7469 7 90 % S1 N3783 1 90 % Q/RL Elvis+ 10 45 ? 50% Q/RL 3C 273 10 46 1 30 % The true energy output in the IR

8. Summary IRAS / ISO/ SPITZER data used successfully to characterise AGN: IR colors, IR-radio correlations, IR-line- emission correlations … This is surprising considering that: –Core SEDs differ dramatically from those derived from large aperture data –Core luminosities overestimated by order of magnitude High spatial resolution SEDs show progressive transition from Seyfert 2 to 1 to RL Quasars: variations explained in terms of central dust obscuration and view angle.