1. Spectral energy distribution of AGN radio-quiet vs radio-loud M. Almudena Prieto (IAC) Leiden, November 2009

2. PARSEC program High spatial resolution study of the Nearest Active Galactic Nuclei Compilation of the highest spatial resolution data available Angular scales of θ < 0.1” UV + OP + IR + radio What is new: subarcsec scales in the 1 to 20µm range 1 - 5 µm  θ < 0.1” 10 - 20 µm  θ < 0.5” Interferometry at 10 µm  θ < 0.05“ What we have: HST 0.3 - 0.9 µm  θ < 0.1” What we partially have: VLA-A/ VLBA  θ < 0.1”

3. FWHM core 2 µm 11 μm T2/RL CenA < 1 pc< 0.5 pc T2 Circinus ~ 2 pc ~2 pc T1 N4151 ~2pc T2 N1068 ~ 2 pc ~2 pc L N1097 < 11 pc < 27 pc T2 N1386 < 8 pc < 32 pc T2 N7582 < 11 pc < 30 pc L/RL M87 <11 pc < 25 pc T1 N3783 < 16 pc <~3.5 pc T1 N7469 < 26 pc <100 pc Q/RL 3C273 < 180 pc < 50 pc Prieto+ 2004, 05,09; Jaffe+ 2004, Meisenheimer + 2006; Haering-Neumayer+ 2007, Reunanen+ 2009, Tristram+ 2009 Some of the nearest …

4. 3C 273 NGC 5506 Sy 1.9 Some AGN dominate the galaxy light regardless of the aperture size AGN in the IR 2MASS

5. In others, the galaxy dominates the IR light by at least an order of magnitude AGN in the IR NGC 1068 Centaurus A NGC 1566 Circinus 2MASS

6. CIRCINUS NGC 5506 Obscured AGN shows up only from ~ 2 μ m onward HST 6000A HST 6600 A NACO 2 μm NGC 7582 NACO 2 μm + HST HST 6600 A HST 8140 A NACO 2 μm

7. S2 S2/RL S1 LINER Modest AGN: their IR luminosity is a few percent of the total IR integrated light Radio IR OP X-rays

8. S2 S2/RL S1 LINER “+ “ IRAS, ISO, SPITZER, and/or millimetre data

9. S1 S2 Dominating AGN: their IR luminosity is ~100% of the total IR emission of the galaxy QSO

10. Comparison with an average Seyfert 2 SED (from Polletta et al. 2007)

11. Average SEDs of nearby AGNs S2S1 average S1 average S2 average S1 average S2 Elvis+ 94: Radio-loud quasars template and 3C 273

12. IRcore IR(large/core) X >20keV / IRcore Li N1097 3x10 41 500 15 % T2/RL CenA 2x10 42 20 65 % T1 N1566 2x10 42 80 200 % T2 Circinus 8x10 42 7 5% T2 N7582 1x10 43 25 35 % T2 N1068 8x10 43 10 2 % T2 N5506 1x10 44 1 5 % T1 N3783 2x10 44 1 15 % T1 N7469 2x10 44 7 13% Q/RL 3C 273 2x10 46 1 200% The true energy output in the IR

13. IRcore IR(large/core) X >20keV / IRcore Li N1097 3x10 41 500 15 % T2/RL CenA 2x10 42 20 65 % T1 N1566 2x10 42 80 200 % T2 Circinus 8x10 42 7 5% T2 N7582 1x10 43 25 35 % T2 N1068 8x10 43 10 2 % T2 N5506 1x10 44 1 5 % T1 N3783 2x10 44 1 15 % Q/RQ Elvis+ 7x10 45 ? 30 % Q/RL Elvis+ 6x10 45 ? 50% Q/RL 3C 273 2x10 46 1 200% The true energy output in the IR

14. AGNs in the IR The upper limit size to any central obscuring structure is FWHM < few 10 of pc. At parsec-scale resolution, the IR resolves into a structure of a few parsecs IR SED of this core region: narrow bump in the 2 - 10 µm range: hotter inner dust fully visible in RL > 10 um, BB shape T~ 300 K, outer dust radius ~ few 10 of pc IR core luminosities > 70% of total in RQ ( L total = L IR-core + L 20-100 keV ) … but are order of magnitude lower than that of the host galaxy for AGN with luminosities ≤ 10 44 erg/s