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

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 5 keV V K 3.3 mm 15 GHz radio-mm IR V UV X-rays g-rays The X-ray Universe 2008 – May 30, 2008 2/10

The 3C 273 multi-wavelength database 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 > 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

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

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

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

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

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

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

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/0805.3411 The X-ray Universe 2008 – May 30, 2008 10/10