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Lockman Hole (XMM PV)

PV Team. B. Altieri (ESA) M. Arnaud (CEA) X. Barcons (IFCA) J. Bergeron (ESO) H. Brunner (AIP) M. Dadina (Bologna) K. Dennerl (MPE) P. Ferrando (CEA) A. Finoguenov (MPE) R. Griffiths (CMU, co-chair) Y. Hashimoto (AIP) G. Hasinger (AIP, chair) D. Lumb (ESA) K. Mason (MSSL).

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Lockman Hole (XMM PV)

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  1. PV Team • B. Altieri (ESA) • M. Arnaud (CEA) • X. Barcons (IFCA) • J. Bergeron (ESO) • H. Brunner (AIP) • M. Dadina (Bologna) • K. Dennerl (MPE) • P. Ferrando (CEA) • A. Finoguenov (MPE) • R. Griffiths (CMU, co-chair) • Y. Hashimoto (AIP) • G. Hasinger (AIP, chair) • D. Lumb (ESA) • K. Mason (MSSL) • S. Mateos (IFCA) • R. McMahon (IoA) • T. Miyaji (CMU) • M. Page (MSSL) • F. Paerels (Columbia) • P. Rosati (ESO) • A. Ptak (CMU) • T. Sasseen (UCSB) • N. Schartel (ESA) • G. Szokoly (AIP) • J. Trümper (MPE) • M. Turner (Leicester) • B. Warwick (Leicester) • M. Watson (Leicester) Lockman Hole (XMM PV) PN CCD (MPE Garching) MOS1 CCD (Leicester U) PV Observations 27.4-18.5 2000 190 ksec data 100 ksec low background

  2. Colour Image 0.5-0.2 keV 2-4.5 keV4.5-10 keV PN+MOS1+MOS2

  3. Comparison XMM/ROSAT XMM X-ray Colours (0.5-10 keV) ROSAT HRI-PSPC (0.1-2 keV)

  4. logN-logS XMM Chandra Giacconi et al. ROSAT ASCA ROSAT fluctuations. BeppoSAX fluctuations.

  5. Very hard logN-logS (5-10 keV) XMM/BeppoSAX Gilli model

  6. X-ray Diagnostics logNH=23 1  = 0 2 22.5 3 + + + + + + 22 + + New XMM sources are significantly harder than ROSAT sources, but mainly have absorbed, intrinsically soft continua => type-2 AGN !

  7. Kerr Schwarz- schild 6.4 keV restframe 2 Kerr BH Inclination  15o Ri 5 RG Ro 20 RG 1

  8. A surprise ! Inclination=45o Ri unconstrained Ro 20 RG

  9. Keck NIRPEC Thompson et al., 2000 High-redshift cluster

  10. Sample cluster spectra z=1.26 kT=5 keV Constraints on Temperature and abundance possible for very high redshift or low luminosity z=0.26 kT=1.5 keV

  11. z=1.26   z=0.26 Cluster Luminosity/Temperature Relation Borgani, Tozzi, Rosati (2000)

  12. LH Optical/NIR coverage V, I: CFHT 8K < 25.5 mag* R: Keck LRIS < 25 mag K: Calar Alto ‘ < 20 mag** (largest K-band survey at that mag) 30 arcmin *courtesy G. Wilson, IfA **partially courtesy K. Meisenheimer (CADIS)

  13. Optical Identifications K, I, V colour image PSPC HRI 14Z K, I, V colour image 84Z Keck LRIS + NIRC Schmidt et al., 1998; Lehmann et al., 2000

  14. EROs Photometric redshifts Chandra/XMM limit  XMM XMM optical IDs fX/fopt=1 fX/fopt=1 spectroscopy limit spectroscopy limit + + + + + + + +  AGN type1  AGN type2 Cluster/group Star + unidentified

  15. Photometric Redshifts K H J z I z=1.9 R V z=1.5 z=1.4 poor fit! z=1.2 Courtesy: L. Pozzetti

  16. Colour Segregation Ellipticals  AGN type 1  AGN type 2  Cluster/group  Star + unidentified + + + Sb-gal. Type 2 AGN show galaxy colours + Photometric z techniques work QSO-2 at high redshift

  17. Hardness vs. Colour HR2 HR1 + + + + + + + + EROs have hard X-ray spectra  AGN

  18. NGC 6240 QSO average (Elvis et al.) NGC 6240 QSO-2 Spectra

  19. Summary • ROSAT: first evidence of high-z QSO-2 • XMM PV data substantially deeper than ROSAT • deeper than published Chandra in 2-10 keV band • Giacconi 2-10 keV logN-logS confirmed • New: 5-10 keV logN-logS, consistent with XRB model • high-quality spectral fits for ROSAT sources: unobscured power laws for type-1 AGN, obscured PL for type-2 • tantalizing indication of relativistic disk lines at z=1 • temperature determination of z=1.26 cluster • new XMM sources are preferentially EROs • EROs have hard X-ray spectra, therefore are AGN • so far XMM+Chandra data are fully consistent with obscured AGN XRB model Watch this space !

  20. [NeV] line Large Balmer decrement Chandra obscured AGN => obscured AGN indicators Chandra findings are entirely consistent with the obscured AGN model for the X-ray background Mushotzky et al., 2000

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