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Spectral energy distribution of AGNradio-quiet vs radio-loud
M. Almudena Prieto (IAC)
Leiden, November 2009
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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”
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FWHM core 2 µm 11 μm
T2/RL CenA < 1 pc < 0.5 pcT2 Circinus ~ 2 pc ~2 pcT1 N4151 ~2pcT2 N1068 ~ 2 pc ~2 pc
L N1097 < 11 pc < 27 pcT2 N1386 < 8 pc < 32 pcT2 N7582 < 11 pc < 30 pcL/RL M87 <11 pc < 25 pc
T1 N3783 < 16 pc <~3.5 pcT1 N7469 < 26 pc <100 pcQ/RL 3C273 < 180 pc < 50 pcPrieto+ 2004, 05,09; Jaffe+ 2004, Meisenheimer + 2006; Haering-Neumayer+ 2007, Reunanen+ 2009, Tristram+ 2009
Some of the nearest …
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3C 273 NGC 5506 Sy 1.9
Some AGN dominate the galaxy light regardless of the aperture size
AGN in the IR
2MASS
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In others, the galaxy dominates the IR light by at least an order of magnitude
AGN in the IRNGC 1068 Centaurus A
NGC 1566 Circinus
2MASS
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CIRCINUSNGC 5506
Obscured AGN shows up only from ~ 2 μm onward
HST 6000A
HST 6600 A
NACO 2 μm
NGC 7582
NACO 2 μm + HST
HST 6600 A HST 8140 A
NACO 2 μm
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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
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S2 S2/RL
S1 LINER
“+ “ IRAS, ISO, SPITZER, and/or millimetre data
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S1 S2
Dominating AGN: their IR luminosity is ~100% of the total IR emission of the galaxy
QSO
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Comparison with an average Seyfert 2 SED (from Polletta et al. 2007)
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Average SEDs of nearby AGNs
S2 S1
average S1average S2
average S1average S2
Elvis+ 94: Radio-loud quasars template
and 3C 273
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IRcore IR(large/core) X>20keV / IRcore
Li N1097 3x1041 500 15 %
T2/RL CenA 2x1042 20 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 N3783 2x1044 1 15 % T1 N7469 2x1044 7 13%Q/RL 3C 273 2x1046 1 200%
The true energy output in the IR
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IRcore IR(large/core) X>20keV / IRcore
Li N1097 3x1041 500 15 %
T2/RL CenA 2x1042 20 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 N3783 2x1044 1 15 % Q/RQ Elvis+ 7x1045 ?
30 %Q/RL Elvis+ 6x1045 ?
50%Q/RL 3C 273 2x1046 1 200%
The true energy output in the IR
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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