JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Xavier Barcons Instituto de Física de Cantabria (CSIC-UC)

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories 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

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories 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

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories The X-ray view of an AGN C. Done, Durham U

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories The X-ray spectrum of an AGN nRadiation from the accretion disk, reprocessed by a relativistic electron corona nReflection (fluorescence lines and Compton recoil bump) nAbsorbers nSoft excess (direct disk radiation)

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories The new X-ray observatories Chandra (NASA) July 1999 XMM-Newton (ESA) December 1999

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories How does an X-ray telescope work?

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Chandra High-resolution camera (HRC): Micro-Channel Plate Advanced CCD Imaging Spectrometer (ACIS) Low Energy Transmission Grating Spectrometer (LETGS): keV, E/  E= (+HRC-S) High Energy Transmission Grating Spectrometer (HETGS): keV, E/  E  1000 (+ACIS-S) Spatially resolved (0.5“) low resolution spectroscopy (E/  E~20-50) Intermediate resolution dispersive spectroscopy ( Ang, E/  E~ )

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories XMM-Newton Spatially resolved (15“) low- resolution spectroscopy (E/  E~20-50) Intermediate resolution dispersive spectrometry ( Ang, E/  E~ ) EPIC: (3) CCD spectroscopic imaging cameras keV (2) Reflection Grating Spectrometers (RGS): keV (1) Optical monitor (OM): Optical/UV imaging and grism spectroscopy.

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Comparison between Chandra and XMM-Newton XMM-Newton : Effective area 0.4 m 2 Angular resolution: 15 ’’ HEW Limiting sensitivity: erg cm -2 s -1 Chandra: Effective area: 0.08 m 2 Angular resolution: 0.5 ’’ HEW Limiting sensitivity: < erg cm -2 s -1

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories New windows: Hard X-ray energies Sensitivity to hard X-ray energies (up to 12 keV with XMM-Newton) Rosat XMM/Chandra log N H = Absorbed sources can be seen!

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories New windows: high-resolution imaging over wide FOV XMM-Newton images a FOV of 30’ with moderate resolution (15”) Chandra images down to Sub-arcsec resolution (0.5-1”)

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories New windows: moderate resolution dispersive spectroscopy

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories The inner disk: Fe line diagnostics

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Radiation from the accretion disk Incident radiation Reflection Transmission Emission

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Reflection from cold matter George & Fabian 91

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories XMM-Newton spectrum of the Circinus Galaxy Fe K α,β and Ni Kα Molendi, Bianchi & Matt 03 Fluorescence lines

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Reflection from photoionized matter (Ross & Fabian 93, 04) Increasing ionisation parameter

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Relativistic line broadening Schwarzschild Kerr Fabian et al 91

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Discovery of broad Fe lines ASCA Tanaka et al 1995 MCG

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories More broad lines in AGN MCG (Dewangan 2003) NGC 3516 (Turner 02) PG (Pounds 2003) IRAS (Iwasawa 2004)

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories XMM-Newton observations of the Fe line in MCG pn MOS 1,2 Vaughan 04

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Simultaneous XMM-Newton and BeppoSAX observations of MCG Compton reflection hump

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Spectral changes seen in MCG The Fe line stays virtually constant, in spite of strong changes in the continuum: NO REVERBERATION?

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Spectrum of the variable component Understanding spectral variability in MCG Spectrum of the constant component Fe line

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Light bending model in a Kerr BH Kevin Rauch JHU Miniutti et al 03,04

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Regime III: large source height and anti-correlationRegime II: intermediate source height and constant Fe line IIIIII Fe line – PLC correlation

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories The variety of Fe line profiles Reeves et al (2001) Disk Torus XMM Nandra (2001) ASCA

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories More relativistic emission lines? Branduardi-Raymont et al (2001) Lee et al (2001) Chandra XMM

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Ionised absorbers, outflows and jets

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Warm absorbers: the low resolution view H z= IUE XMM-Newton Barcons, Carrera & Ceballos 2003b X-ray ionized absorbers ~ “Associated” UV absorbers Photoionisation edge

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories The high-resolution view of warm absorbers Sako et al 2001 Fe M Unresolved Transition Array (UTA) Low ionisation component High ionisation component

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories 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

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Jets detected in X-rays Pks : First “point-like” target for Chandra

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Jets commonly seen in X-rays Cen-A

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories M87

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories 3C273 Chandra Marshall et al (2001) MERLINHST Chandra SEDs indicate that synchrotron might be dominant in most knots, but additional processes might Be required in other cases.

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories NGC 6240 Binary BHs in the centres of AGN Chandra Komossa et al (2002) NGC 6240 Starburst AGN

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Challenges to the AGN unified model

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories The unified AGN scheme confronts X-ray observations Maiolino (2001) 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

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Type 1 AGN (moderately) absorbed in X-rays S keV = 7.2 x erg cm -2 s -1 z=0.872 N H =2.8  cm -2 Broad-Line AGN L 2-10 =3.2  erg s -1 WHT/ISIS XMM XMMU J

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories A type1.9 AGN with no absorption Barcons, Carrera & Ceballos 2003 H , z= Seyfert 1.8/1.9 H  /H  >27 Expected absorption: >10 22 cm -2 XMM-Newton: Disk + reprocessing Absorption<10 20 cm -2

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Photoelectric absorption The AXIS survey S lim ( keV)~ erg cm -2 s -1 10% of type 1 AGN are absorbed (with N H <10 22 cm -2 ) 40% of type 2 AGN are absorbed Mateos et al (2004a) The Lockman Hole survey S lim ( keV)~ erg cm -2 s -1 15% (<30% at 3  ) of type 1 AGN are absorbed (with N H <10 22 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

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories 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.

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories X-ray/optical mismatches: variability? Simultaneous XMM-Newton and 3.5m/CAHA spectroscopy of Mkn 993; z= (Changing type Seyfert) 3.5m/TWIN XMM Optical: Seyfert 1.8 Balmer decrement=9 (N H ~ cm -2 ) X-ray: weak absorption (N H ~ cm -2 ) Poster by A. Corral Optical spectral type intrinsic to BLR, not due to absorption

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories X-ray Surveys, obscured accretion and the X-ray background.

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories The XMM-Newton Survey Science Centre serendipitous sky Surveys Thanks to its large field of view and sensitivity, every XMM-Newton pointing discovers ~ serendipitous X-ray sources. The 1XMM source catalogue contains sources. The 2XMM catalogue will contain 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

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories 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. Gilli et al 2000

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Optically dull, X-ray luminous galaxies z=0.044 L X =10 42 erg/s TNG Subaru  =1.7 N H = cm -2 XMM Severgnini et al (2003)

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Type 2 (Radio) QSOs Selected by its X-ray emission Only narrow emission lines at z=1.246 X-ray luminosity > erg/s Double-lobed radio-source X-ray emission unrelated to radio lobes “Normal” AGN mildly absorbed in X-rays Barcons et al 1998 Barcons et al 2003 XMM VLA RX J N H = cm -2 XMM WHT/ISIS

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Type-2 Radio-Quiet QSOs AAT/2dF (Mat Page) XMM N H ~ cm -2 z=2.978 (Ly , CIV, CIII]) X-ray flux (2-10 keV) = erg cm -2 s -1 Intrinsic X-ray luminosity = erg s -1

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories The various classes of AGN F X /F opt =1 F X /F opt =10 F X /F opt =0.1 AGN Obscured AGN Gal

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Optical colours of X-ray sources QSOs Early-type galaxies

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories The Chandra deep fields The bulk of X-ray emissivity (50%) in the Universe (AGNs) occurs at z<1 Sources are increasingly reddened in the optical, including EROs. Tozzi et al 2001, Barger et al 2003, Alexander et al 2003

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories The redshift distribution in deep X-ray surveys Barger et al (2003) Mostly AGN-2 Mostly AGN-1

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Obscured accretion Most of the growth of the black holes by accretion occurs in obscured sources. Assuming that the growth of BHs is dominated by accretion and not by mergers, the local BH density can set constraints on the amount of obscured accretion Salvati et al (2004)

JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories Some questions for the future Perform reverberation mapping on relevant timescales. Test properties of supermassive black holes out to very high z’s (mass, angular momentum, accretion rate) Reach the “thermal limit” in X-ray high-resolution spectroscopy to do proper Astrophysics on circumnuclear matter Trace the cosmic evolution of obscured and unobscured accretion What was first: Supermassive Black Holes or Stars in the history of galaxies?