Multi-wavelength AGN spectra and modeling

Paolo Giommi

ASI

Stars+Galaxies (black body)

AP-AGN (accretion onto SMBH)

Radio Galaxies

non-thermal emission

Non-thermal emission

Microwave Optical X-Ray -Ray TeVRadio

AGN Types

•Accretion Dominated AGN (AD-AGN) Radio-quiet QSO Seyfert galaxies Obscured AGN about 90% of AGN

• Non-Thermal Radiation Dominated AGN (NT-AGN)Blazars (FSRQ + BLLACS)Misdirected NT-AGN (Radio Galaxies, SSRQs) about 10% of AGN

Blazars

•AGN •Highly variable at all frequencies •Highly polarized•Radio core dominance•Superluminal speeds

Observed at a small angle to the jet and therefore rare AGN : 5-8% of all AGN(but only at optical or X-ray frequencies!)

Blazars are the dominant population of extragalactic point sources at

• Gamma-ray• TeV• Microwave frequencies

Normally the electromagnetic emission from blazars is assumed to be due to the Synchrotron-Self Compton mechanism (SSC) or SSC+External Component of a population of electrons in a jet of material that is moving at relativistic speed at a small angle with respect to the observer.

Radio Microwave Optical X-ray -ray TeV

LBL Objects

HBL Objects

Radio Microwave Optical X-ray -ray TeV

LBL Objects

HBL Objects

UHBL Objects ?

Swift/AGILE ToO observations of S5 0716+714 (Oct-Nov 2007)

Giommi et al. 2008, A&A in press, arXiv:0806.1855

Swift observations of 3C454.3during the giant flare of May 2005

Giommi et al. 2006, A&A 456, 911

XRT data

BeppoSAX

TeV dectected BL LacsTramacere et al. 2006

SED of MRK 421 in 2005: large changes in luminosity and peak energy.

SED of 1H1100 – 230 observed on 30 June (blue) and 13 July 2005 (red). BeppoSAX 1997 and 1998 data are shown as open symbols.

UVOT data

TeV dectected BL Lacs

SED of 1ES 1959+650 (19 April 2005)

SED of 1ES 1553+113 observed on 20 April (red), 6 Octobe (blue), and 8 October 2005 (green)

May 1999

MKN421 in a bright state: the BeppoSAX observation of May 2000Massaro, Perri, Giommi, Nesci, 2004 A&A

Log parabolic photon spectra can be explained as due to Synchrotron radiation from a log-parabolic particle distribution

(Massaro et al. 2004a A&A 413, 489, 2004b, A&A 422,103)

SSC from a log parabolic electron distribution(Massaro et al. 2005, in press)

• Spectral curvature observed around the Synchrotron peak is due to intrinsic curvature of emitting particle distribution

• SSC of a particle distribution distributed as a Log-Parabola implies intrinsic curvature around Inverse Compton peak leaving little room for curvature resulting from EBL absorption

• Absorption due to EBL could be significantly lower than previously thought

• Supported also by – Aharonian et al. 2005 A&A 437, 395 Cut off energy in TeV spectrum of MKN421 (3.1TeV) lower than that of

MKN501 (6.2 TeV), but redshift is very similar – Aharonian et al. 2005 astro/ph 0508073 HESS detection of the “high redshift” Blazars: H2356-309 (z=0.165) and 1ES1101-232

Swift observation of MKN421 in 2006

Tramacere et al. 2008 in preparation

WMAP bright foreground source catalog

•140 FSRQs•23 BL Lacs•13 Radio galaxies•5 Steep Spectrum QSOs•2 starburst galaxies•2 planetary nebule

•17 unidentified•6 without radio counterpart (probably spurious)

208 bright sources, of which

The vast majority of bright WMAP foreground sources are Blazars

WMAP CMB fluctuation map

Radio Galaxy PKS 0518-45 Radio Galaxy 3C 111

Fiocchi, Grandi et al. in preparation

Boomerang 90 GHz CMB MAPDe Bernardis et al. 2000

PKS 0521-365

PKS 0438-436

PKS 0537-441PKS 0422-380

PKS 0454-463

PKS 0513-491l

PKS 0539-543

PKS 0549-575PKS 0252-549

PKS 0405-385

PKS 0506-61

PMN J0419-3010

[Giommi & Colafrancesco 2003]

PKS 0521-365

PKS 0438-436

PKS 0537-441

RGal PKS 0518-45

PKS 0422-380

PKS 0435 -300

PKS 0426-380PKS 0448-392

PKS 0534-340 PKS 0602-31

PKS 0610-316

PKS 0558-396

PKS 0524-485

PKS 0454-463

WGA 0624-3230WGA 0428.2-3805

PKS 0446-519PKS 0452-515

PKS 0513-491l

WGA 0533-5817

PKS 0431-512

PKS 0514-459

RXS J 0606-4730

PMNJ0529-3555

PKS 0548-322

PKS 0524-460

PKS 0427-435 Pictor A

PKS 0402-362

PKS 0355-483

PKS 0618-37

PKS 0622-441

PKS 0539-543

PKS 0549-575

PKS 0548-317

PKS 0558-504

PKS 0252-549

PKS 0405-385

PKS 0506-61

WGA 0631-5404

PKS 0257-51

WGA 0424-3849

PKS 0646-437

PKS 0532-378

PKS 0443-387 PMN J0525-3343

PKS 0439-331

PMN J0419-3010

1RXS0432-3506

1RXS0543-3956

PKS 0613-312

1RXS0531-3533

1RXS0557-3728

1RXS0606-3447

PMN 0422-3844

PMN0510-3533

1RXS0502-4221

1RXS0608-3041

[Giommi & Colafrancesco 2003]

WMAP SEDsWMAP 035 = 3C345WMAP 047 = CTA 102WMAP 067 = 3C371WMAP 108 = 3C120WMAP 139 = PKS 0521-365WMAP 150 = Pictor A

Nuclear compact radio emission

WMAP 190 = PKS 2153-69

The Blazar LogN-LogS

Giommi & Colafrancesco 2003

All microwave selected blazars are X-ray sources.

2007 A&A, 468, 571

From wave flux to X-rays and vice-versa

x

Nu

mb

er

of

WM

AP

so

urc

es

de

tec

ted

at

94

GH

z

x> = -1.07

= 0.08f94GHz = f1keV • 106.41 x>

f94GHz = 10 0.086.41 • f94GHz

f94GHz ~ 3 • f94GHz

f94GHz = 106.85 • f1keV

Microwave fluxes can be estimated from X-ray fluxto within a factor 3

f94GHz = 7.1 • 106 f1keV

Effect of 3 variability

LBL Blazar contribution to soft CXB: 4%, total (LBL+HBL 12%)

€

x = −log( f 94GHz / f 1keV)

log(ν 94GHz /ν 1keV)= −

log( f 94GHz / f 1keV)

6.41

From -wave to X-rays

Fixed at -wavesx

Hard-Xray/Soft Gamma-Ray Cosmic Background

Contribution to the X and -ray backgrounds

Radio — -ray flux ratio & duty cycle

Blazar Name f-source/<background>

(background=-0.994)

BZQ J0204+1514 -0.892 14.5

BZU J0210-5101 -0.887 16.6

BZB J0339-0146 -0.902 11.2

BZQ J0423-0120 -0.907 9.7

BZQ J0455-4615 -0.913 8.3

BZQ J0457-2324 -0.908 9.6

BZU J0522-3627 -0.926 6.0

BZB J0538-4405 -0.892 14.4

BZQ J1256-0547 (3C 279)

-0.870 25.5

)/log(

)/log(

νν

FF

≡Define a slope/trend:

Duty cycle

(%)

6.9

6.0

8.9

10.3

12.0

10.4

16.7

6.9

3.9

QuickTime™ e undecompressore TIFF (LZW)

sono necessari per visualizzare quest'immagine.

Max EGRET

Min EGRET

A ~10 mJy Blazar

Planck LFI+HFI Swift XRT

Swift UVOT

Swift BATGLAST LAT

3C 279 scaled down by a factor 1000 (1milli 3C279)