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Spectral energy distribution of AGN radio-quiet vs radio-loud

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

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Spectral energy distribution of AGN radio-quiet vs radio-loud

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

  2. PARSEC programHigh 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. Some of the nearest … • 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

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

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

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

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

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

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

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

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

  12. The true energy output in the IR • IRcore IR(large/core) X>20keV / IRcore • Li N1097 3x1041 500 15 % • T2/RL CenA 2x104220 65 % • T1 N1566 2x1042 80 200 % • T2 Circinus 8x1042 7 5% • T2 N7582 1x1043 25 35 % • T2 N1068 8x1043 10 2 % • T2 N5506 1x1044 1 5 % • T1 N37832x1044 1 15 % • T1 N74692x1044 7 13% • Q/RL 3C 273 2x1046 1 200%

  13. The true energy output in the IR • IRcore IR(large/core) X>20keV / IRcore • Li N1097 3x1041 500 15 % • T2/RL CenA 2x104220 65 % • T1 N1566 2x1042 80 200 % • T2 Circinus 8x1042 7 5% • T2 N7582 1x1043 25 35 % • T2 N1068 8x1043 10 2 % • T2 N5506 1x1044 1 5 % • T1 N37832x1044 1 15 % • Q/RQ Elvis+ 7x1045 ? 30 % • Q/RL Elvis+ 6x1045 ? 50% • Q/RL 3C 273 2x1046 1 200%

  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: < 2 um, the emission falls steeply in type 2, shallower in type 1, even less shallower in RL-Qso => 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 ( Ltotal = LIR-core + L 20-100 keV) … but are order of magnitude lower than that of the host galaxy for AGN with luminosities ≤ 1044 erg/s

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