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

2. Colour Image 0.5-0.2 keV 2-4.5 keV 4.5-10 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 fluctuations. ROSAT BeppoSAX fluctuations. ASCA

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

6. X-ray Diagnostics  = 01 2 3 logN H =23 22.5 22 New XMM sources are significantly harder than ROSAT sources, but mainly have absorbed, intrinsically soft continua => type-2 AGN ! + + + + + + + +

7. 6.4 keV restframe Kerr BH Inclination  15 o R i  5 R G R o  20 R G 11 22 Kerr Schwarz- schild

8. A surprise ! Inclination=45 o R i unconstrained R o  20 R G

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

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

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

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

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

14. XMM optical IDs AGN type1 AGN type2  Cluster/group  Star + unidentified  XMM spectroscopy limit 1 f X /f opt = 1 Chandra/XMM limit EROs spectroscopy limit 1 f X /f opt = 1 + + + + + + + + Photometric redshifts

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

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

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

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

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