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AGN and Surveys with the new X-ray observatories

AGN and Surveys with the new X-ray observatories. Xavier Barcons Instituto de Física de Cantabria (CSIC-UC). Index. Introduction: The AGN paradigm and X-ray observations New windows with the new X-ray observatories The inner disk: Fe line diagnostics

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AGN and Surveys with the new X-ray observatories

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  1. AGN and Surveys with the new X-ray observatories Xavier Barcons Instituto de Física de Cantabria (CSIC-UC) AGN and Surveys with the new X-ray observatories

  2. Index • Introduction: The AGN paradigm and X-ray observations • New windows with the new X-ray observatories • The inner disk: Fe line diagnostics • The circum-nuclear environment: warm absorbers, jets and outflows • Challenges to the AGN unified model • X-ray Surveys, Obscured accretion, and the X-ray background • A few questions for the future AGN and Surveys with the new X-ray observatories

  3. Acknowledgements • The IFCA X-ray Astronomy group: Francisco Carrera, Maite Ceballos, Silvia Mateos, Amalia Corral, Jacobo Ebrero • The XMM-Newton Survey Science Centre, especially: Mike Watson, Mat Page, Tommaso Maccacaro, Roberto Della Ceca, Paola Severgnini, Axel Schwope, etc. • The Lockman Hole team, especially: Günther Hasinger, Alina Streblyanska, Ingo Lehmann, Thomas Boller and the • Andy Fabian AGN and Surveys with the new X-ray observatories

  4. The X-ray view of an AGN C. Done, Durham U AGN and Surveys with the new X-ray observatories

  5. The X-ray spectrum of an AGN • Radiation from the accretion disk, reprocessed by a relativistic electron corona • Reflection (fluorescence lines and Compton recoil bump) • Absorbers • Soft excess (direct disk radiation) AGN and Surveys with the new X-ray observatories

  6. The new X-ray observatories XMM-Newton (ESA) December 1999 Chandra (NASA) July 1999 AGN and Surveys with the new X-ray observatories

  7. How does an X-ray telescope work? AGN and Surveys with the new X-ray observatories

  8. High-resolution camera (HRC): Micro-Channel Plate Advanced CCD Imaging Spectrometer (ACIS) Low Energy Transmission Grating Spectrometer (LETGS): 0.08-2 keV, E/E=30-2000 (+HRC-S) High Energy Transmission Grating Spectrometer (HETGS): 0.4-10 keV, E/E1000 (+ACIS-S) Chandra • Spatially resolved (0.5“) low resolution spectroscopy (E/E~20-50) • Intermediate resolution dispersive spectroscopy (0.02-0.04 Ang, E/E~200-500) AGN and Surveys with the new X-ray observatories

  9. XMM-Newton • Spatially resolved (15“) low-resolution spectroscopy (E/E~20-50) • Intermediate resolution dispersive spectrometry (0.03-0.06 Ang, E/E~200-500) • EPIC: (3) CCD spectroscopic imaging cameras 0.1-12 keV • (2) Reflection Grating Spectrometers (RGS): 0.05-3 keV • (1) Optical monitor (OM): Optical/UV imaging and grism spectroscopy. AGN and Surveys with the new X-ray observatories

  10. Comparison between Chandra and XMM-Newton • XMM-Newton: • Effective area 0.4 m2 • Angular resolution: 15’’ HEW • Limiting sensitivity: 10-15 erg cm-2 s-1 • Chandra: • Effective area: 0.08 m2 • Angular resolution: 0.5’’ HEW • Limiting sensitivity: <10-16 erg cm-2 s-1 AGN and Surveys with the new X-ray observatories

  11. XMM/Chandra Rosat log NH= New windows: Hard X-ray energies Sensitivity to hard X-ray energies (up to 12 keV with XMM-Newton) Absorbed sources can be seen! AGN and Surveys with the new X-ray observatories

  12. New windows: high-resolution imaging over wide FOV Chandra images down to Sub-arcsec resolution (0.5-1”) XMM-Newton images a FOV of 30’ with moderate resolution (15”) AGN and Surveys with the new X-ray observatories

  13. New windows: moderate resolution dispersive spectroscopy AGN and Surveys with the new X-ray observatories

  14. The inner disk: Fe line diagnostics AGN and Surveys with the new X-ray observatories

  15. Radiation from the accretion disk Reflection Incident radiation Emission Transmission AGN and Surveys with the new X-ray observatories

  16. Reflection from cold matter George & Fabian 91 AGN and Surveys with the new X-ray observatories

  17. XMM-Newton spectrum of the Circinus Galaxy Molendi, Bianchi & Matt 03 Fe Kα,β and Ni Kα Fluorescence lines AGN and Surveys with the new X-ray observatories

  18. Reflection from photoionized matter (Ross & Fabian 93, 04) Increasing ionisation parameter AGN and Surveys with the new X-ray observatories

  19. Relativistic line broadening Schwarzschild Kerr Fabian et al 91 AGN and Surveys with the new X-ray observatories

  20. Discovery of broad Fe lines MCG-6-30-15 ASCA Tanaka et al 1995 AGN and Surveys with the new X-ray observatories

  21. More broad lines in AGN MCG-5-23-16 (Dewangan 2003) NGC 3516 (Turner 02) PG 1211+143 (Pounds 2003) IRAS 18325 (Iwasawa 2004) AGN and Surveys with the new X-ray observatories

  22. XMM-Newton observations of the Fe line in MCG-6-30-15 pn MOS 1,2 Vaughan 04 AGN and Surveys with the new X-ray observatories

  23. Simultaneous XMM-Newton and BeppoSAX observations of MCG-6-30-15 Compton reflection hump AGN and Surveys with the new X-ray observatories

  24. Spectral changes seen in MCG-6-30-15 The Fe line stays virtually constant, in spite of strong changes in the continuum: NO REVERBERATION? AGN and Surveys with the new X-ray observatories

  25. Fe line Understanding spectral variability in MCG-6-30-15 Spectrum of the variable component Spectrum of the constant component AGN and Surveys with the new X-ray observatories

  26. Light bending model in a Kerr BH Miniutti et al 03,04 Kevin Rauch JHU AGN and Surveys with the new X-ray observatories

  27. Fe line – PLC correlation I II III Regime III: large source height and anti-correlation Regime II: intermediate source height and constant Fe line AGN and Surveys with the new X-ray observatories

  28. Nandra (2001) Reeves et al (2001) Torus Disk ASCA XMM The variety of Fe line profiles AGN and Surveys with the new X-ray observatories

  29. Branduardi-Raymont et al (2001) More relativistic emission lines? Lee et al (2001) XMM Chandra AGN and Surveys with the new X-ray observatories

  30. Ionised absorbers, outflows and jets AGN and Surveys with the new X-ray observatories

  31. Photoionisation edge XMM-Newton IUE Warm absorbers: the low resolution view H1419+480 z=0.07229 X-ray ionized absorbers ~ “Associated” UV absorbers Barcons, Carrera & Ceballos 2003b AGN and Surveys with the new X-ray observatories

  32. Low ionisation component Fe M Unresolved Transition Array (UTA) High ionisation component The high-resolution view of warm absorbers Sako et al 2001 AGN and Surveys with the new X-ray observatories

  33. NGC 3783 (Krongold et al 2003) Chandra/HETGS ~100 features detected; Two-phase absorbing medium, pressure equilibrium Outflowing velocity ~750 km/s; Turbulence ~300 km/s AGN and Surveys with the new X-ray observatories

  34. Jets detected in X-rays Pks 0637-752: First “point-like” target for Chandra AGN and Surveys with the new X-ray observatories

  35. Jets commonly seen in X-rays Cen-A AGN and Surveys with the new X-ray observatories

  36. M87 AGN and Surveys with the new X-ray observatories

  37. Chandra 3C273 MERLIN HST Chandra SEDs indicate that synchrotron might be dominant in most knots, but additional processes might Be required in other cases. Marshall et al (2001) AGN and Surveys with the new X-ray observatories

  38. NGC 6240 NGC 6240 AGN Starburst Chandra Komossa et al (2002) Binary BHs in the centres of AGN AGN and Surveys with the new X-ray observatories

  39. Challenges to the AGN unified model AGN and Surveys with the new X-ray observatories

  40. Maiolino (2001) The unified AGN scheme confronts X-ray observations Since type 2 AGN are seen through absorbing material, they should display higher photoelectric absorption in X-rays • … but there are apparent • discrepancies: • Type 1 AGN with absorbed X-ray • spectra • Type 1.8/1.9/2 AGN with low or • no photoelectric absorption AGN and Surveys with the new X-ray observatories

  41. Type 1 AGN (moderately) absorbed in X-rays XMMU J061515.2+710204 S 0.5-4.5 keV= 7.2 x 10-14 erg cm-2 s-1 XMM NH=2.81021 cm-2 z=0.872 L 2-10=3.21044 erg s-1 WHT/ISIS Broad-Line AGN AGN and Surveys with the new X-ray observatories

  42. A type1.9 AGN with no absorption XMM-Newton: Disk + reprocessing Absorption<1020 cm-2 H1320+551, z=0.0653 Seyfert 1.8/1.9 H/H>27 Expected absorption: >1022 cm-2 Barcons, Carrera & Ceballos 2003 AGN and Surveys with the new X-ray observatories

  43. Photoelectric absorption • The AXIS survey • Slim(0.5-4.5 keV)~10-14 erg cm-2 s-1 • 10% of type 1 AGN are absorbed • (with NH<1022 cm-2) • 40% of type 2 AGN are absorbed • The Lockman Hole survey • Slim(0.5-4.5 keV)~10-14 erg cm-2 s-1 • 15% (<30% at 3) of type 1 AGN • are absorbed (with NH<1022 cm-2) • 80% (>50% at 3) of type 2 AGN • are absorbed. But 5/28 are unabsorbed Mateos et al (2004b) See talk by Maite Ceballos Mateos et al (2004a) AGN and Surveys with the new X-ray observatories

  44. Options/explanations • The 10-15% of absorbed type 1 AGN could be ~BALs, or hosted by edge-on galaxies [this should be testable] • Unabsorbed type 2 AGN: • These are Compton-thick Seyfert 2 galaxies, where only unabsorbed scattered X-rays are seen [but Fe line is weak or absent and should be very strong] • Optical spectroscopy properties and X-ray absorption agree with each other, but the absorbing material varies [should be testable with simultaneous X-ray and optical spectroscopy] • The optical spectroscopic properties are intrinsic to the Broad Line Region, and not associated to absorbing material. AGN and Surveys with the new X-ray observatories

  45. 3.5m/TWIN XMM Optical: Seyfert 1.8 Balmer decrement=9 (NH~ 5 1021 cm-2) X-ray: weak absorption (NH~ 7 1020 cm-2) X-ray/optical mismatches: variability? Simultaneous XMM-Newton and 3.5m/CAHA spectroscopy of Mkn 993; z=0.0155 (Changing type Seyfert) Poster by A. Corral Optical spectral type intrinsic to BLR, not due to absorption AGN and Surveys with the new X-ray observatories

  46. X-ray Surveys, obscured accretion and the X-ray background. AGN and Surveys with the new X-ray observatories

  47. The XMM-Newton Survey Science Centre serendipitous sky Surveys • Thanks to its large field of view and sensitivity, every XMM-Newton pointing discovers ~30-150 serendipitous X-ray sources. • The 1XMM source catalogue contains 30000 sources. The 2XMM catalogue will contain 150000 X-ray sources • The Survey Science Centre sky survey consists of: • Core programme: • Bright Source Sample • Medium Flux Survey • Faint Surveys (i.e., LH) • Galactic Plane Surveys • Optical imaging programme of many XMM-Newton fields • Statistical identification of many catalogued sources OY Car AGN and Surveys with the new X-ray observatories

  48. Gilli et al 2000 The X-ray background and the AGN unified model • The spectral energy distribution of the XRB peaks at ~30 keV, far beyond existing X-ray telescopes. • Unified model: The XRB is produced by a superposition of unabsorbed and absorbed AGN. • Predictions: • The majority of accretion onto super-massive black holes is absorbed • A large number of type 2 QSOs is expected. AGN and Surveys with the new X-ray observatories

  49. z=0.044 LX=1042 erg/s TNG Subaru Optically dull, X-ray luminous galaxies Severgnini et al (2003) XMM =1.7 NH=2 1023 cm-2 AGN and Surveys with the new X-ray observatories

  50. Type 2 (Radio) QSOs • Selected by its X-ray • emission • Only narrow emission lines • at z=1.246 • X-ray luminosity > 1045 erg/s • Double-lobed radio-source • X-ray emission unrelated • to radio lobes • “Normal” AGN mildly • absorbed in X-rays RX J1011.2+5545 WHT/ISIS XMM VLA XMM NH=4 1022 cm-2 Barcons et al 1998 Barcons et al 2003 AGN and Surveys with the new X-ray observatories

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