Spectral energy distribution of AGNradio-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”• 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”

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 …

3C 273 NGC 5506 Sy 1.9

Some AGN dominate the galaxy light regardless of the aperture size

AGN in the IR

2MASS

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

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

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

S2 S2/RL

S1 LINER

“+ “ IRAS, ISO, SPITZER, and/or millimetre data

S1 S2

Dominating AGN: their IR luminosity is ~100% of the total IR emission of the galaxy

QSO

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

Average SEDs of nearby AGNs

S2 S1

average S1average S2

average S1average S2

Elvis+ 94: Radio-loud quasars template

and 3C 273

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

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

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