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

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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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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” - PowerPoint PPT Presentation

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

Page 1: Spectral energy distribution of AGN radio-quiet vs radio-loud

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