The hard X-ray Extra-Galactic sky with INTEGRAL/IBIS High-z QSOs A.De Rosa on behalf of the INTEGRAL/AGN survey team

INTEGRAL (INTErnational Gamma-Ray Astrophysics Laboratory) INTEGRAL (INTErnational Gamma-Ray Astrophysics Laboratory) Astronomical satellite for observing the gamma-ray sky launched on October 17, 2002 Imager IBIS angular resolution of 12 arcmin point source location accuracy of a few arcmin energy range between 15 keV and above 1 MeV

5th AGILE Science Workshop ESRIN,12-13 Jun surveys provided so far, 4 th on-going 3 surveys provided so far, 4 th on-going 2 nd catalogue (209 sources) + 1 st HE catalogue (2006) 1 st catalogue (2005) 126 sources 3 rd catalogue (2007) 421 sources 4 th LE and 2 nd HE catalogue on going pointed science windows: 57 Ms Spans a duration of 1250 days

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 The sky according to IBIS AGN distribution (131 sources) (131 sources)

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 Optical spectroscopy of most likely counterparts Telescopes: Loiano-Bologna Italy, South Africa, CTIO-Chile, La Silla Chile, CASLEO Argentina Sey1 Sey2 Narrow-Line Sey1 X-ray bright optically dull AGN A first catalogue of 60 AGN (Bassani et al. 2006) 82% Seyferts Sey2/Sey1=1 Gamma ray selection favours broad line sources Masetti et al. 2004,

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 The IBIS complete sample of AGNs The INTEGAL AGN complete sample 74 objects: 36 type 1 74 objects: 36 type 1 30 type 2 30 type 2 8 blazars/QSO 8 blazars/QSO BAT complete sample: 24 AGNs 19 Seyferts 3 blazars 3 blazars 1 qso 1 qso 1XBONG 1XBONG The IBIS AGN total sample: 131 objects 58 type 1 (circles) 60 type 2 (squares) 13 blazars (triangles) + 21 AGN candidates “High-z” QSOs

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 High-z INTEGRAL QSOs: the sample PKS De Rosa et al. 2005, Zhang et al PKS De Rosa et al. 2005, Zhang et al Swift J Masetti et al Swift J Masetti et al IGR J Bassani et al IGR J Bassani et al QSO B QSO B C De Rosa et al C De Rosa et al RXS J RXS J IGR J IGR J QSO B PKS PKS PKS Possibly detected in keV PKS Possibly detected in keV QSO Possibly detected in keV QSO Possibly detected in keV PKS De Rosa et al. 2005, Zhang et al PKS De Rosa et al. 2005, Zhang et al Swift J Masetti et al Swift J Masetti et al IGR J Bassani et al IGR J Bassani et al QSO B QSO B C De Rosa et al C De Rosa et al RXS J RXS J IGR J IGR J QSO B PKS PKS PKS Possibly detected in keV PKS Possibly detected in keV QSO Possibly detected in keV QSO Possibly detected in keV Source zReference   

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 L(2-10 keV)=0.3x10 48 erg/s L( keV)= 5x10 48 erg/s X-ray/radio  1000 Blue quasar candidate: High energy peaked FSRQ? (see ROXA J Giommi et al ) IGR J , z=3.668 a gamma-ray lighthouse Bassani et al. ApJL 2007  =1.5+/-0.2 N H =3+/-2 x cm -2  =0.5 E b =1-2 keV AGILE

 ~1.1 N H,z ~2x10 22 cm -2 N H,z,ion ~10 23 cm -2  <100 erg cm/s PKS , z=2.507 Foschini et al De Rosa et al. 2005

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 The FSRQ 4C04.42, z=0.965  Radio loudness parameter Kellerman et al 1989 R=S 5Ghz /S 4400A ˜ 1000  INTEGRAL above 20 keV with F(20-40 keV) = 7.6x cgs F ( keV) = 18.8x cgs  MOJAVE: 1-2Jy all radio frequencies  Radio loudness parameter Kellerman et al 1989 R=S 5Ghz /S 4400A ˜ 1000  INTEGRAL above 20 keV with F(20-40 keV) = 7.6x cgs F ( keV) = 18.8x cgs  MOJAVE: 1-2Jy all radio frequencies

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 XMM & INTEGRAL Inst. Exp(s) cts (s -1 ) XMM-MOS1 (thin) ±0.005 XMM-MOS2 (thin) ±0.006 XMM-pn (thin) ±0.005 INTEGRAL-isgri ±0.02 Inst. Exp(s) cts (s -1 ) XMM-MOS1 (thin) ±0.005 XMM-MOS2 (thin) ±0.006 XMM-pn (thin) ±0.005 INTEGRAL-isgri ±0.02

5th AGILE Science Workshop ESRIN,12-13 Jun C04.42 z=0.965 z=0.361 Kataoka et al 2007 Broad band spectral analysis  Continuum power- law fit extrapolated below 2 keV   =1.21±0.06  Continuum power- law fit extrapolated below 2 keV   =1.21±0.06 Excess of emission below 2 keV obs frame Excess of emission below 2 keV obs frame

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 I. Broken power-law  1 =1.59±0.05,  2 =1.17±0.09, E bkn =2.2±0.4 keV  2 /dof=364/363

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 II. Partial covering absorption  =1.57±0.04 f cov ~0.5 N H,z ~7x10 23 cm -2  2 /dof=375/363

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 III. Thermal black-body kT BB =0.15±0.02 keV L BB = erg/s  2 /dof=383/363 z= C04.42 z=0.965 Kataoka et al L BB = 3x10 44 erg/s

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 The Spectral Energy Distribution External Compton SynchrotronSynchrotron Self-Synchrotron Compton Disk emission BLR emission 4C04.42 AGILE ? ?

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 SED: model parameters  e - density distribution N(  )  -p in  min <  max.  min =1  max =1000  Magnetic field B=2Gauss  Lorentz factor   Doppler factor D=   Photon field density U (U SSC, U ext ) U ext = U BLR = 0.1L disk /4  cR 2 BLR  e - density distribution N(  )  -p in  min <  max.  min =1  max =1000  Magnetic field B=2Gauss  Lorentz factor   Doppler factor D=   Photon field density U (U SSC, U ext ) U ext = U BLR = 0.1L disk /4  cR 2 BLR Synchr & SSC SSCSynchr & ExternalComptonExternalCompton

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 (missing) The (missing) Spectral Energy Distribution External Compton SynchrotronSynchrotron Self-Synchrotron Compton Disk emission BLR emission ?

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 Bulk Compton Celotti et al Inverse Compton Scattering of cold electrons  ˜1 on the external photons field:  E  2.. UV-->soft X) Energy Budget BC =  2 BLR /(1+z) ˜ 1 keV L BC =4/3  c  4 U BLR  2 N cold ˜ N cold /N rel, L BC ˜10 45 erg/s => N cold /N rel ˜ 0.1 Energy Budget BC =  2 BLR /(1+z) ˜ 1 keV L BC =4/3  c  4 U BLR  2 N cold ˜ N cold /N rel, L BC ˜10 45 erg/s => N cold /N rel ˜ 0.1

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 Evidence of BC? 4C04.42 z=0.965 z=0.361

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 Alternative models  Increasing contribution of the SSC component in the X-ray band  Accretion flows from the central region like radio quiet AGN  High energy peaked FSRQ (like IGR J22517)  Disk emission including reflection component ( , , , (Sambruna et al. 2006)  Realistic emission spectrum for BLR to compute the EC component (Tavecchio & Ghisellini 2008)  Increasing contribution of the SSC component in the X-ray band  Accretion flows from the central region like radio quiet AGN  High energy peaked FSRQ (like IGR J22517)  Disk emission including reflection component ( , , , (Sambruna et al. 2006)  Realistic emission spectrum for BLR to compute the EC component (Tavecchio & Ghisellini 2008) 4C04.42 Tavecchio & Ghisellini 2008 Sambruna et al. 2006

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 The jet-disk connection P jet =  R 2  2 cU, U=U B +U e +U p

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 The jet-disk connection L disk /P jet ~ 0.1 A large fraction of the accretion power is converted in bulk kinetic energy Log P jet (10 46 erg/s) Sambruna et al 2006, Maraschi & Tavecchio 2003

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 High-z QSO & soft X-ray feature  Evidence of flattening below 2 keV (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 N H vs z has been measured  Excess of emission (4C04.42 like) has be found in very few cases ( Sambruna et al. 2006, Kataoka et al. 2007, De Rosa et al )  Evidence of flattening below 2 keV (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 N H vs z has been measured  Excess of emission (4C04.42 like) has be found in very few cases ( Sambruna et al. 2006, Kataoka et al. 2007, De Rosa et al )

5th AGILE Science Workshop ESRIN,12-13 Jun 2008 INTEGRAL & “high-z” QSO  Define a class of observed objects ( ˜ 10 sur3, more coming from sur4)  Broad-band spectral analysis: low energies break, evidence of BC  Information of number density of cold electrons, Doppler/Lorentz factor  Disk-jet connection  Define a class of observed objects ( ˜ 10 sur3, more coming from sur4)  Broad-band spectral analysis: low energies break, evidence of BC  Information of number density of cold electrons, Doppler/Lorentz factor  Disk-jet connection

5th AGILE Science Workshop ESRIN,12-13 Jun To be continued