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

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Presentation on theme: "Spectral energy distribution of AGN radio-quiet vs radio-loud M. Almudena Prieto (IAC) Leiden, November 2009."— Presentation transcript:

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 µm  θ < 0.1” µm  θ < 0.5” Interferometry at 10 µm  θ < 0.05“ What we have: HST 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 ; Haering-Neumayer+ 2007, Reunanen+ 2009, Tristram 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 3x % T2/RL CenA 2x % T1 N1566 2x % T2 Circinus 8x % T2 N7582 1x % T2 N1068 8x % T2 N5506 1x % T1 N3783 2x % T1 N7469 2x % Q/RL 3C 273 2x % The true energy output in the IR

13 IRcore IR(large/core) X >20keV / IRcore Li N1097 3x % T2/RL CenA 2x % T1 N1566 2x % T2 Circinus 8x % T2 N7582 1x % T2 N1068 8x % T2 N5506 1x % T1 N3783 2x % Q/RQ Elvis+ 7x10 45 ? 30 % Q/RL Elvis+ 6x10 45 ? 50% Q/RL 3C 273 2x % 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 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 keV ) … but are order of magnitude lower than that of the host galaxy for AGN with luminosities ≤ erg/s


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