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Muliti-frequency observations of Blazars

P. Giommi Agenzia Spaziale Italiana + many collaborators: Swift team, S. Puccetti, M. Capalbi, M. Perri, D. Gasparrini, E. Cavazzuti, (ASDC), S. Colafrancesco, E. Massaro, P. Padovani. Muliti-frequency observations of Blazars. Blazars and the AGN paradigm. AGN : Two main categories

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Muliti-frequency observations of Blazars

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  1. P. Giommi Agenzia Spaziale Italiana + many collaborators: Swift team, S. Puccetti, M. Capalbi, M. Perri, D. Gasparrini, E. Cavazzuti, (ASDC), S. Colafrancesco, E. Massaro, P. Padovani. Muliti-frequency observations of Blazars

  2. Blazars and the AGN paradigm AGN : Two main categories • Dominated by accretion - disk emission - AP-AGN • Dominated by Non-Thermal radiation - jet emission - NT-AGN Blazars: NT-AGN viewed at a small angle w.r.t. jet axis Radio Galaxies: NT-AGN viewed at a large angle w.r.t. jet axis Broad-line radio galaxies (e.g. 3c120) : A combination of AP-AGN and “mis-directed” NT-AGN

  3. Two blazar types FSRQ BL Lac objects

  4. 3C 279 : a Low energy peaked Blazar (LBL)

  5. MKN 421 : a High energy peaked BL Lac (HBL)

  6. All blazars presently known(see poster by Massaro et al.) Catalog of confirmed literature blazars. Compiled in support to AGILE and GLAST missions Currently covers 0 < R.A. < 15 hrs : 1449 objects > 2000 objects when complete (~ end 2007)

  7. Courtesy of P. Padovani Simbol-X energy band

  8. AP-AGN (accretion onto SMBH) Radio Galaxies non-thermal emission Stars+Galaxies (black body)

  9. Blazars are the dominant population of extragalactic sources at • Microwave frequencies • Gamma-ray • TeV band

  10. Blazars @ -wave frequencies: the 3-year WMAP data Bright foreground source catalog WMAP CMB fluctuation map 323 bright sources • 194 FSRQs • 38 BL Lacs • 30 Radio galaxies • 15 Steep sp. QSO • 2 starburst galaxies • 2 planetary nebule • 41 unidentified The large majority of bright WMAP foreground sources are blazars or radio galaxies Planck will be in a vey similar situation to that of GLAST - LAT (thousands of deteced blazars + contribution to unresolved flux).

  11. 2007 A&A, in press All microwave selected blazars are X-ray sources.

  12. GLAST-LAT - 1 year simulation • - 3,000-10,000 detected blazars • significant contribution to CGB from unresolved blazars with radio/-wave flux <~ 100 mJy

  13. ~20% at 30 keV Simbol-X bandpass ~30-50% at 80 keV ~10% at 1 keV Blazar contribution to CXB and Simbol-X

  14. Swift XRT serendipitous sources in GRBs pointigs :the “perfect” serendipitous survey ~1 blazar/field expected with radio flux > 10 mJy!

  15. Swift XRT serendipitous survey in GRB deep fields: status as of end of April 2007 209 deep (4x104-6x105 seconds) GRB exposures analyzed ~15,500 sources detected with positional uncertainty of 4-6 arscecs. 143 fields are at |bII| > 20 : ~11,500 sources 242 radio/X-ray matches (blazar candidates)

  16. Swift J015700.6+085403 : fx ~5x10-14erg/cm2/s, 122 mJy @ 1.4 GHz

  17. Swift J101724.4+432905: FSRQ, z=1.1735 fx ~6x10-14erg/cm2/s, 197 mJy @ 1.4 GHz

  18. Deep Blazars survey in Swift GRB fields • >200 Swift deep GRB fields available today (>20 sq deg of sky) • (300 at the end of 2007) • 150-200 blazars in radio flux limited sample (f5GHz = 10 mJy) • 400-500 blazars in X-ray flux limite sample • Extensive multi-frequency data available (in principle) • (from GRB follow-up observations) • Radio LogN-LogS to 10 mJy, radio LF + Cosmological evolution • Volume-limited X-ray survey to z=0.5 for Lx > 5.e42 erg/s • Tight constraints to microwave, hard-Xray and gamma-ray backgrounds,including a better estimate on the number of absorbed AGN needed to explain the CXB.

  19. Rosat SDSS data NVSS High-power HBLsThe case of BZB J1456+5048 (Z=0.479) SDSS optical spectrum Rosat luminosity ~ 5x1046 erg/s

  20. High-power HBLsThe case of BZB J1456+5048 (Z=0.479)

  21. A Simbol-X observation of 3C279 with same spectrum as in Jan 2007and with flux/100 = 6 Crab

  22. A Simbol-X observation ofBZB J1456+5048

  23. Conclusions Simbol-X has will greatly improve the statistics of blazars in a very poorly explored energy band and will be a great instrument to study non-thermal emission from accelerated particles in radio galaxies and blazars jets Blazar population studies in different wavebands will tightly constrain their contribution to the CXB and will better quantify the need for absorbed AGN in CXB synthesis models.

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