INTEGRAL Blazars Catching Blazars in their ordinary life

INTEGRAL Blazars Catching Blazars in their ordinary life A. De Rosa, S. Gianni’, L. Bassani, P. Ubertini B. On behalf of the INTEGRAL AGN survey team A. De Rosa - 7 th AGILE workshop 29 Sept 2009

Outline Hard X-rays selected Blazars: ordinary vs out of ordinary life Blazars in the INTEGRAL survey Characterizing the X-ray spectra: broadband study Absorption properties in RL QSOs Finding peculiar objects: blue FSRQs/bulk Compton emission X vs Gamma-rays properties: population study with INTEGRAL, AGILE & Fermi A. De Rosa - 7 th AGILE workshop The future and work 29 Septin 2009 progress

Observing blazars in hard-X rays Giommivariable 07 Blazars are extremely rare believed that it is- widely objects (<5% all AGNs) that the can lowbe energy peak is detected in hard-X (>10 ke. V)due through to large area surveys: Because of the rarity and the Synchrotron low space density of blazars, "pencil beam" of relativistic surveys (. . ) are poorly suitedradiation for finding blazars. . (Perlman 1998). electrons in a jet, while the high Two different waysenergy one is due to • Long monitoring: average Inverse flux states Compton • To. O pointed observation: scattering flaring activity (IC) of the same electrons A. De Rosa - 7 th AGILE workshop 29 Sept 2009 with a photon field

Out of ordinary vs ordinary life 3 c 454. 3 Lucky To. O Unlucky To. O. . Lucky detection 300 rev - 1000 days Unlucky detection Vercellone et al 2009 Pian et al. 2006 A. De Rosa - 7 th AGILE workshop 29 Sept 2009

The sample source F 20 -40 Ke. V F 40 -100 ke. V 1 ES 0033+59. 5 RX J 0137. 7+5814 SWIFT j 0218. 0+7348 IGR J 03532 -6820 QSO B 0836+710 MKN 421 4 C 04. 42 3 C 273 3 C 279 H 1426+428 MKN 501 SWIFT 1656. 3 -3302 PKS J 1830 -211 1 RXS J 192450. 8 -291437 QSO B 1933 -400 PKS 2149 -306 Bl Lac IGR J 22517+2218 3 C 454. 3 1. 3 0. 4 1. 2 1. 3 2. 4 25. 6 0. 8 10. 4 1. 1 1. 0 3. 1 1. 4 2. 4 0. 9 0. 5 1. 2 1. 3 9. 4 0. 9 <0. 4 1. 9 <0. 8 4. 2 19. 4 1. 8 12. 3 1. 4 1. 1 2. 1 3. 2 0. 8 1. 0 1. 7 1. 5 2. 3 12. 8 z 0. 086 2. 367 type HBL BLlac BLLac 2. 172 FSRQ 0. 03 HBL 0. 965 FSRQ 0. 158 FSRQ 0. 5362 FSRQ 0. 129 HBL 0. 03366 HBL 2. 40 FSRQ 2. 705 FSRQ 0. 352 FSRQ 0. 965 FSRQ? 2. 345 FSRQ 0. 0686 BLLac 3. 668 FSRQ 0. 859 FSRQ

Characterising the X-ray spectra 2 -10 ke. V observations with XMM, Chandra, XRT We built a broadband spectrum 0. 1 -200 ke. V for 9 sources (more are coming) Main Results Flattening wrt a power-law in the soft X-rays range : If due tointrinsic absorption -> Nh vs redshift evolution Finding peculiar sources: blue quasar candidate IGR J 22517+2218 - possible bulk Compton motion in 4 C 04. 42 A. De Rosa - 7 th AGILE workshop 29 Sept 2009

Characterising the X-ray spectra Evidence of flattening below 2 ke. V (rest frame) has been found in several high-z QSO up to z=4. 4 (Yuan et al. 2006) Intrinsic curvature - absorption (cold/warm) Clear trend NH vs z has been measured Excess of emission has be found in very few cases (Sambruna et al. 2006, Kataoka et al. 2007, De Rosa et al. 2008) A. De Rosa - 7 th AGILE workshop 29 Sept 2009

Characterising the X-ray spectra: absorption Ratio Page et al. 05 data/continuum power-law fit to the energy band above 2 ke. V (observer frame) extrapolated over the low energy range Statistical warning!! A. De Rosa - 7 th AGILE workshop 29 Sept 2009

Characterising the X-ray spectra: bulk Compton emission in 4 C 04. 42? PRELIMINARY! Energy Budget AGILE 10 days Fermi 1 month BC= 2 BLR/(1+z) ˜ 1 ke. V De Rosa et al. 2008 LBC=4/3 c 4 UBLR 2 Ncold ˜ 1046 Ncold/Nrel, LBC˜ 1045 erg/s => Ncold/Nrel ˜ 0. 1 Multifrequency program: Kataoka et al. 2007 INTEGRAL & AGILE (quick look courtesy of L. A. De Rosa - 7 th AGILE workshop Pacciani)+ public Fermi 29 Sept 2009

Characterising the X-ray spectra Finding peculiar objects Blazars spectral sequence (Fossati et. al 1998)? The peaks of the Synch A reanalysis shows & Bassani IC Shifting thatcomp. the EC et al. 2007 systematically tothe component in higher with SEDfrequencies bis well decreasing luminosity. reproduced by the XRed (high luminosity) rays data. These peak? and blue. Synch (low luminosity) objects are two red Synch peak? blazars. high luminosity BL Lacs blazars, in agreement blue blazars prediction: with. Athe spectral ØROXA J 081009. 9+384757. 0 z = Strong 3. 95 blue powerful. NO blue powerful blazar… sequence Maraschi et al. 2008 blazar? ØIGR J 22517+2218, z=3. 668 a gamma-ray lighthouse: A. De FSRQs? Rosa - 7 th AGILE workshop • a high energy peaked 29 Sept 2009 • FSRQsetred Giommi al. blazars 2007

X and Gamma-rays population INTEGRAL IBIS Fermi LBAS AGILE GRID total 723 132 47 BLLac 7 (37%) 58 (56%) 4 (31%) FSRQ 12 (63%) 42 (40%) 7 (54%) unknown 21(AGNs? ) 4 2

X and Gamma-rays population I. photon index distribution: IBIS & LBAS Abdo et al. 09 Ajello et al. 09 BAT 15 -55 ke. V FSRQs BLlacs

X and Gamma-rays population I. photon index distribution BLLacs Following the spectral sequence, gamma and X-ray spectral ranges match different emission processes in blue and red blazars FSRQs A. De Rosa - 7 th AGILE workshop 29 Sept 2009

X and Gamma-rays population II. Luminosity vs redshift FSRQs BLLacs Abdo et al. 09 F(20 -100 ke. V)=1. 2 e-11 cgs (0. 8 m. Crab), Crab like spectrum A. De Rosa - 7 th AGILE workshop 29 Sept 2009 Texp=2 Ms

The future and work in progress Deep extragalactic fields will be observed in the 7 th INTEGRAL AO. New sources X-rays coverage: XMM large programme for INTEGRAL (hard-X rays selected) AGNs is actually on going, and we hope so for the near future. . AO 9. . ? Simultaneous observations: Gamma-rays & Te. V energy ranges Define a complete sample of hard X-rays selected blazars Populations study: are FSRQs and BLLacs two separate classes? Implication on CXRB in hard X-rays and Me. V energy range A. De Rosa - 7 th AGILE workshop 29 Sept 2009

Everything unexpected… Thanks for your attention A. De Rosa - 7 th AGILE workshop 29 Sept 2009