From radio to gamma-rays:

1
From radio to gamma-rays 3C 273 reveals its
multi-component structure
Simona Soldi ISDC
The X-ray Universe 2008, Granada, Spain May 30,
2008
2
Simona Soldi
The quasar 3C 273

• The brightest quasar in the sky (V 12.9)
• z 0.158
• Emission from radio to ?-ray energies,
• with large flux variations
• Jet with apparent superluminal motion
• Both blazar and Seyfert-like properties

20-70 keV 5 keV V
K 3.3 mm 15 GHz
g-rays
radio-mm
X-rays
IR
V
UV
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The X-ray Universe 2008 May 30, 2008
3
Simona Soldi
The 3C 273 multi-wavelength database
http//isdc.unige.ch/3c273/ . Türler et al.
1999 Soldi et al. 2008, astro-ph/0805.3411

• 40 years of observations
• gt 22,000 observations
• 70 light curves
• from radio to g-rays
• 15 years of intense X-ray
• monitoring

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The X-ray Universe 2008 May 30, 2008
4
Simona Soldi
Thermal emission from dust
(Soldi et al. 2008)

IR
V
IR lag
V lag
UV

• Correlation between optical-UV and IR
• Different IR lags, increasing with IR wavelength
• Clear signature from dust thermal emission

IR lag
UV lag
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The X-ray Universe 2008 May 30, 2008
5
Simona Soldi
Infrared emission at the jet minimum
(Türler et al. 2006)

• Historic jet-emission
• minimum in June 2004
• Multi-l campaign
• IR excess
• no variations in the near-IR
• several dust components

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The X-ray Universe 2008 May 30, 2008
6
Simona Soldi
Long-term X-ray variations
Chernyakova et al. 2007
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The X-ray Universe 2008 May 30, 2008
7
Simona Soldi
Hard X-ray - mm relation
X-ray lag
1.3 mm lag
? the dominant process in the hard X-rays is not
related to the radio-mm flaring emission
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The X-ray Universe 2008 May 30, 2008
8
Simona Soldi
The origin of the hard X-ray emission
X-ray lag
V lag
? hard X-rays from inverse Compton of
optical/synchrotron electrons?
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The X-ray Universe 2008 May 30, 2008
9
Simona Soldi
Variability properties of the X-ray emission
BATSE
? different variability properties of medium
and hard X-rays One or two components contributin
g?
From structure function analysis
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10
Simona Soldi
Discussion and conclusions

• Hard X-ray electrons not related to the jet
  flaring emission
• Synchrotron emission in the optical band
• Dust emission is dominant in the near-IR, but
  also
• synchrotron components are contributing
• In spite of the large amount of data, still
  unclear what is
• at the origin of the X-ray emission
• Multi-wavelength databases are a precious tool!

For more details, see Soldi et al. 2008, AA in
press, astro-ph/0805.3411
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The X-ray Universe 2008 May 30, 2008