Multi-wavelength AGN spectra and modeling Paolo Giommi ASI

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Multi-wavelength AGN spectra and modeling
Paolo GiommiASI
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AP-AGN (accretion onto SMBH)
Radio Galaxies non-thermal emission
StarsGalaxies (black body)
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AGN Types
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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
  SSCExternal 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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Swift/AGILE ToO observations of S5 0716714
(Oct-Nov 2007)
Giommi et al. 2008, AA in press, arXiv0806.1855
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Swift observations of 3C454.3during the giant
flare of May 2005Giommi et al. 2006, AA 456, 911
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TeV dectected BL LacsTramacere et al. 2006

UVOT data
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.
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TeV dectected BL Lacs
SED of 1ES 1553113 observed on 20 April (red), 6
Octobe (blue), and 8 October 2005 (green)
SED of 1ES 1959650 (19 April 2005)
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MKN421 in a bright state the BeppoSAX
observation of May 2000 Massaro, Perri, Giommi,
Nesci, 2004 AA
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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 AA 413, 489, 2004b, AA
  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 AA 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 (z0.165) and 1ES1101-232

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Swift observation of MKN421 in 2006Tramacere et
al. 2008 in preparation
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WMAP bright foreground source catalog
208 bright sources, of which
WMAP CMB fluctuation map

• 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)

The vast majority of bright WMAP foreground
sources are Blazars
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Boomerang 90 GHz CMB MAP De Bernardis et al. 2000
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WMAP SEDs
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The Blazar LogN-LogS
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Giommi Colafrancesco 2003
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2007 AA, 468, 571
All microwave selected blazars are X-ray sources.

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From ??wave flux to X-rays and vice-versa
f94GHz f1keV 106.41 lt??xgt
f94GHz 106.85 f1keV
f94GHz 7.1 106 f1keV
Effect of ? 3 variability

• f94GHz 10 0.08?6.41 f94GHz
• f94GHz 3 f94GHz

Microwave fluxes can be estimated from X-ray
flux to within a factor ? 3
LBL Blazar contribution to soft CXB 4, total
(LBLHBL 12)
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From ?-wave to X-rays
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Hard-Xray/Soft Gamma-Ray Cosmic Background
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Contribution to the X and ?-ray backgrounds
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Radio ?-ray flux ratio duty cycle
Define a slope/trend
Blazar Name ??? f?-source/lt?-backgroundgt (???background-0.994)
BZQ J02041514 -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
Duty cycle ()
6.9
6.0
8.9
10.3
12.0
10.4
16.7
6.9
3.9
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A 10 mJy Blazar