1. From radio to gamma-rays: 3C 273 reveals its multi-component structure
Simona Soldi
ISDC
M. Türler, S. Paltani, H.D. Aller, M.F. Aller,
G. Burki, M. Chernyakova, A. Lähteenmäki,
I.M. McHardy, E.I. Robson, R. Staubert,
M. Tornikoski, R. Walter and T.J.-L. Courvoisier
The X-ray Universe 2008, Granada, Spain
May 30, 2008

2. The quasar 3C 273 The brightest quasar in the sky (V = 12.9) z = 0.158
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 keV V K mm GHz
radio-mm IR V UV
X-rays
g-rays
The X-ray Universe 2008 – May 30, 2008
2/10

3. The 3C 273 multi-wavelength database
Simona Soldi
The 3C 273 multi-wavelength database .
Türler et al. 1999
Soldi et al. 2008, astro-ph/
40 years of observations
> 22,000 observations
70 light curves
from radio to g-rays
15 years of intense X-ray
monitoring
The X-ray Universe 2008 – May 30, 2008
3/10

4. Thermal emission from dust
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
The X-ray Universe 2008 – May 30, 2008
4/10

5. Infrared emission at the jet minimum
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
The X-ray Universe 2008 – May 30, 2008
5/10

6. Long-term X-ray variations
Simona Soldi
Long-term X-ray variations
Chernyakova et al. 2007
The X-ray Universe 2008 – May 30, 2008
6/10

7. Hard X-ray - mm relation
Simona Soldi
Hard X-ray - mm relation
1.3 mm lag
X-ray lag
⇒ the dominant process in the hard X-rays
is not related to the radio-mm flaring emission
The X-ray Universe 2008 – May 30, 2008
7/10

8. The origin of the hard X-ray emission
Simona Soldi
The origin of the hard X-ray emission
V lag
X-ray lag
⇒ hard X-rays from inverse Compton of optical/synchrotron electrons?
The X-ray Universe 2008 – May 30, 2008
8/10

9. Variability properties of the X-ray emission
Simona Soldi
Variability properties of the X-ray emission
BATSE
⇒ different variability
properties of
medium and hard X-rays
One or two components
contributing?
From structure
function analysis
The X-ray Universe 2008 – May 30, 2008
9/10

10. Discussion and conclusions
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, A&A in press, astro-ph/
The X-ray Universe 2008 – May 30, 2008
10/10