Multi-wavelength AGN spectra and modeling Paolo Giommi ASI Radio - - PowerPoint PPT Presentation

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Multi-wavelength AGN spectra and modeling Paolo Giommi ASI Radio - - PowerPoint PPT Presentation

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Multi-wavelength AGN spectra and modeling Paolo Giommi ASI Radio Microwave R a d i o G a l a x i e s n o n - t h e r m a l e m i s s i o n Optical Stars+Galaxies (black body) N N o o n n - - t t h h

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Multi-wavelength AGN spectra and modeling

Paolo Giommi ASI

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Stars+Galaxies (black body)

AP-AGN (accretion onto SMBH)

R a d i

  • G

a l a x i e s n

  • n
  • t

h e r m a l e m i s s i

  • n

N

  • n
  • t

h e r m a l N

  • n
  • t

h e r m a l e m i s s i

  • n

e m i s s i

  • n

Microwave Optical X-Ray γ-Ray TeV Radio

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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

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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
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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.

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Radio Microwave Optical X-ray

γ-ray

TeV LBL Objects HBL Objects Radio Microwave Optical X-ray

γ-ray

TeV LBL Objects HBL Objects UHBL Objects ?

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Swift/AGILE ToO observations

  • f S5 0716+714 (Oct-Nov 2007)

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

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Swift observations of 3C454.3

during the giant flare of May 2005

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

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XRT data BeppoSAX

TeV dectected BL Lacs

Tramacere 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

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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)

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May 1999

MKN421 in a bright state: the BeppoSAX observation of May 2000

Massaro, Perri, Giommi, Nesci, 2004 A&A

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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)

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  • 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

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Swift observation of MKN421 in 2006

Tramacere et al. 2008 in preparation

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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

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Radio Galaxy PKS 0518-45 Radio Galaxy 3C 111

Fiocchi, Grandi et al. in preparation

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Boomerang 90 GHz CMB MAP

De Bernardis et al. 2000

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PKS 0521-365 PKS 0438-436 PKS 0537-441 PKS 0422-380 PKS 0454-463 PKS 0513-491l PKS 0539-543 PKS 0549-575 PKS 0252-549 PKS 0405-385 PKS 0506-61 PMN J0419-3010

[Giommi & Colafrancesco 2003]

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PKS 0521-365 PKS 0438-436 PKS 0537-441 RGal PKS 0518-45 PKS 0422-380 PKS 0435 -300 PKS 0426-380 PKS 0448-392 PKS 0534-340 PKS 0602-31 PKS 0610-316 PKS 0558-396 PKS 0524-485 PKS 0454-463 WGA 0624-3230 WGA 0428.2-3805 PKS 0446-519 PKS 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]

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WMAP SEDs

WMAP 035 = 3C345 WMAP 047 = CTA 102 WMAP 067 = 3C371 WMAP 108 = 3C120 WMAP 139 = PKS 0521-365 WMAP 150 = Pictor A

Nuclear compact radio emission

WMAP 190 = PKS 2153-69

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The Blazar LogN-LogS

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Giommi & Colafrancesco 2003

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All microwave selected blazars are X-ray sources.

2007 A&A, 468, 571

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From µ−wave flux to X-rays and vice-versa

αµx

Number of WMAP sources detected at 94 GHz

<αµx> = -1.07

σ = 0.08

f94GHz = f1keV • 106.41 <αµx> σf94GHz = 10 0.08⋅6.41 • f94GHz σf94GHz ~ 3 • f94GHz f94GHz = 106.85 • f1keV

Microwave fluxes can be estimated from X-ray flux to within a factor ≤ 3

f94GHz = 7.1 • 106 f1keV

Effect of ± 3 variability

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

αµx = − log( f 94GHz / f 1keV) log(ν 94GHz /ν1keV) = − log( f 94GHz / f 1keV) 6.41

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From µ-wave to X-rays

Fixed at µ-waves

αµx = −1.07

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Hard-Xray/Soft Gamma-Ray Cosmic Background

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Contribution to the X and γ-ray backgrounds

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Radio — γ-ray flux ratio & duty cycle

25.5

  • 0.870

BZQ J1256-0547 (3C 279) 14.4

  • 0.892

BZB J0538-4405 6.0

  • 0.926

BZU J0522-3627 9.6

  • 0.908

BZQ J0457-2324 8.3

  • 0.913

BZQ J0455-4615 9.7

  • 0.907

BZQ J0423-0120 11.2

  • 0.902

BZB J0339-0146 16.6

  • 0.887

BZU J0210-5101 14.5

  • 0.892

BZQ J0204+1514

fγ-source/<γ−background>

(αµγbackground=-0.994)

αµγ Blazar Name

) / log( ) / log(

γ µ γ µ µγ

ν ν α F F ≡

Define a slope/trend:

3.9 6.9 16.7 10.4 12.0 10.3 8.9 6.0 6.9 Duty cycle (%)

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Max EGRET Min EGRET

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A ~10 mJy Blazar

Planck LFI+HFI Swift XRT Swift UVOT Swift BAT GLAST LAT

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