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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)