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XMM-Newton Surveys

XMM-Newton Surveys. Xavier Barcons. Acknowledgements. The XMM-Newton Survey Science Centre (SSC), especially Mike Watson , Christian Motch, Francisco Carrera, Axel Schwope and Mat Page among others The Lockman Hole team, especially Günther Hasinger and Andy Fabian

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XMM-Newton Surveys

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  1. XMM-Newton Surveys Xavier Barcons XMM-Newton Surveys

  2. Acknowledgements • The XMM-Newton Survey Science Centre (SSC), especially Mike Watson, Christian Motch, Francisco Carrera, Axel Schwope and Mat Page among others • The Lockman Hole team, especially Günther Hasinger and Andy Fabian • The X-ray Astronomy group at my Institute (IFCA), the only (and best) one in Spain • The Spanish National Space Programme (project ESP2003-00812) • The whole XMM-Newton project for support and making things happen, including SOC, SSC, instrument teams, Users Group and more. XMM-Newton Surveys

  3. Index • What do X-rays tell us about the Universe? • The XMM-Newton X-ray space observatory • The XMM-Newton serendipitous X-ray survey • The XMM catalogue • Extragalactic Surveys • Surveying the Galactic Plane • The future of XMM-Newton surveys XMM-Newton Surveys

  4. Physical processes that produce X-rays • Plasmas (ionised gases) at temperatures of millions of degrees (bremsstrahlung and line emission) • Very energetic electrons in strong magnetic fields (synchrotron radiation) • Inverse Compton scattering on high energy electrons. • Matter falling towards compact objects or black holes (accretion) • Electron-positron pair cascades XMM-Newton Surveys

  5. OVIII OVII N132D SNR Fe line XMM-Newton Surveys

  6. Pulsar SNRs and Pulsars The Crab nebula Chandra XMM-Newton Surveys

  7. The magnetic field of isolated neutron stars First unambiguous detection of cyclotron absorption lines in the X-ray spectrum of an isolated neutron star: direct measurement of the magnetic field strength. B~8 x 1010 Gauss Cyclotron lines 1E1207.4–5209 Bignami, Caraveo, De Luca & Mereghetti 2003 XMM-Newton Surveys

  8. The Galactic centre in X-rays XMM-Newton Surveys

  9. Coma Clusters of galaxies Sérsic 159-03 XMM-Newton Surveys

  10. The X-ray view of Active Galactic Nuclei C. Done, Durham U (Chris Done, Univ of Durham) XMM-Newton Surveys

  11. The X-ray spectrum of AGN • Radiation from the accretion disk, reprocessed by a corona of hot electrons • Refection (Fe line and Compton recoil) • Absorption by surrounding material • Soft excess (direct radiation from the accretion disk) XMM-Newton Surveys

  12. Gilli et al 2000 The importance of absorption in AGN: the Cosmic X-ray background • The spectral energy distribution peaks at ~30 keV • Unified model: The right mixture of absorbed and unabsorbed AGN produces the spectrum of the Cosmic X-ray background • Predictions: • The majority of X-rays in the Universe are produced in absorbed objects • Many absorbed quasars should be found XMM-Newton Surveys

  13. The new X-ray observatories XMM-Newton (ESA) December 1999 Chandra (NASA) July 1999 XMM-Newton Surveys

  14. How does an X-ray telescope work? XMM-Newton Surveys

  15. 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. XMM-Newton Surveys

  16. XMM/Chandra Rosat log NH= A new window: Hard X-ray energies Sensitivity to hard X-ray energies (up to 12 keV with XMM-Newton) Absorbed sources can be seen! XMM-Newton Surveys

  17. The XMM-Newton serendipitous sky survey • Every new XMM-Newton pointing (with EPIC in full window mode) discovers ~30-150 serendipitous X-ray sources. • About 30,000 new X-ray sources/year, with positional and X-ray spectral information XMM-Newton Surveys

  18. The XMM-Newton catalogue • Compiled by the SSC • All EPIC detected sources, flags and large amount of information • Accessible through XSA, LUX, CDS • 1XMM released April 2003 (30,000 sources) • 2XMM released 2005 (100,000-150,000 sources) XMM-Newton Surveys

  19. 1XMM: Sky distribution XMM-Newton Surveys

  20. 1XMM: The X-ray population B1=0.2-0.5 keV B2=0.5-2.0 keV B3=2.0-4.5 keV B4=4.5-7.5 keV B5=7.5-12 keV HR1=(B2-B1)/(B2+B1) HR2=(B3-B2)/(B3+B2) HR3=(B4-B3)/(B4+B3) XMM-Newton Surveys

  21. Hard sources Soft sources 1XMM XMM-Newton Surveys

  22. The Survey Science Centre identification programme • Core programme (~1000 sources/sample): • High b faint sample (10-15 erg cm-2 s-1) • High b medium sample (10-14 erg cm-2 s-1) • High b bright sample (10-13 erg cm-2 s-1) • Galactic Plane Sample • Imaging programme (u,g’,r’,i’,Z,H) • Statistical identifications based on X-ray properties & imaging programme. XMM-Newton Surveys

  23. Sy 2 z=0.238 NGC 4291 z=0.0058 QSO z=0.565 QSO z=2.649 Sy 1 z=0.330 dMe Star XMM-Newton Surveys

  24. The XMM-Newton Medium Sensitivity Survey XMM-Newton Surveys

  25. The XMM-Newton Medium Sensitivity Survey (XMS) • 25 XMM fields • XID:0.5-4.5 keV • SXID>210-14cgs • Ω=3.5 deg2 • 298 sources • 200 identified (67%) Barcons et al 2002 Carrera et al 2005 XMM-Newton Surveys

  26. Identification strategy • Deep (~23mag) optical/NIR imaging of full EPIC field of view (La Palma, ESO) • Search for candidate counterparts • Optical spectroscopy (fibre+long slit) • AXIS (An XMM-Newton International Survey) international programme at La Palma (April 2000- April 2002) • Calar Alto, 3.5m telescope with MOSCA (2003-2005) http://www.ifca.unican.es/~xray/AXIS XMM-Newton Surveys

  27. XMS spectroscopic identifications Search for candidate counterparts i’-band sources within either: 5 (statistical) or 5 arcsec 95% of the X-ray sources have a potential optical candidate counterpart In > 75% of these cases, the candidate counterpart is unique XMM-Newton Surveys

  28. NGC4291 XMS: Luminosity vs. redshift XMM-Newton Surveys

  29. Early-type galaxies QSOs NGC4291 XMS: Optical colours • 228 sources have all both g.r, r-i colours: 60 UnID, 168 ID XMM-Newton Surveys

  30. Star/AGN separation NGC4291 XMS: fXID/fopt vs. HR2 XMM-Newton Surveys

  31. “Empty” sources and EROs Most of these sources are Extremely Red Objects (EROs) with R-K>5 Fiore et al 2003 XMM-Newton Surveys

  32. Extremely Red Objects and obscured AGNs Brusa, Comastri et al (2004) XMM-Newton Surveys

  33. Rotating supermassive Black Holes Absorption in AGN Distant galaxy cluster (z=1.2) The deepest XMM-Newton observation in the Lockman Hole XMM-Newton Surveys

  34. Average rest-frame spectra show relativistic Fe-lines type-1 AGN EW~500eV type-2 AGN EW~400eV Streblyanskaya et al., 2004 Lockman Hole800 ks XMM-Newton observation Average line profile calls for BH rotation XMM-Newton Surveys

  35. Best X-ray spectrum of a z>1 cluster kT~5 keV XMM 800 ks Determination of Fe abundance and redshift in a very distant cluster Abundance independent of z Elements formed at z>1.3! Hashimoto et al 2004 XMM-Newton Surveys

  36. Photoelectric absorption • Medium Survey (XMS) • 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 • Deep Survey (Lockman Hole) • 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 (2005) Mateos et al (2004) XMM-Newton Surveys

  37. 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 XMM-Newton Surveys

  38. A type 1.9 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 XMM-Newton Surveys

  39. 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) Optical spectral type intrinsic to BLR, not due to absorption XMM-Newton Surveys

  40. More type 1.8-2 AGN with no X-ray absorption ESO 602-G031 (Sy 1.8) UGC 12138 (Sy 1.8) soft component soft component z=0.0337 z=0.0250 MRK 702 (Sy 1.9) No or very low intrinsic absorption !!! soft component Lehmann et al 04 XMM-Newton Surveys z=0.0356

  41. Type 2 AGN without absorption (Lockman Hole deep survey) Type 2 AGN (narrow lines only) z=0.711 =1.8 NH=0 Mateos et al 2005 XMM-Newton Surveys

  42. XMM AAT/2dF (Mat Page) NH~5 1022 cm-2 Type-2 Radio-Quiet QSOs z=2.978 (Ly, CIV, CIII]) X-ray flux (2-10 keV) = 8 10-15 erg cm-2 s-1 Intrinsic X-ray luminosity = 4 1044 erg s-1 XMM-Newton Surveys

  43. 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 XMM-Newton Surveys

  44. Optically dull, X-ray luminous galaxies (“Fiore 3”) R=18, z=0.15 Early type galaxy Flux (2-10 keV)= 3 10-14 erg cm-2 s-1 Comastri et al 2002 XMM-Newton Surveys

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