1. New XMM-Newton deep Survey in the Lockman Hole Vincenzo Mainieri MPE Workshop on AGN Surveys, Puebla, June 23- July 11, 2003 Guenther Hasinger Hans Boehringer Hermann Brunner Ingo Lehmann Yas Hashimoto Gyula Szokoly Xavier BarconsAndy Fabian

2. Motivation ROSAT All Sky Survey Resolve the XRB! Nature of the sources? (N H =5.9 x 10 19 cm -2 ) Lockman Hole Field ROSAT PSPC

3. ROSAT observations ROSAT HRI-PSPC (0.1-2 keV) ROSAT DeepSurvey (RDS) Ultra Deep Survey (UDS) 207 ksec PSPC (0.5-2.0keV) 50 sources Flux limit: 5.5 x 10 -14 cgs 1.3 Msec HRI (0.5-2.0 keV) 94 sources Flux limit: 1.2 x 10 -15 cgs Hasinger et al. 1998, Lehmann et al. 2001

4. Lockman Hole - PV (120 ksec) Hasinger et al., 2001 0.5-2.0 keV 2.0-4.5 keV 4.5-10 keV XMM Deep Survey 106 sources: 3.8  10 -16 cgs 69 sources: 2.1  10 -15 cgs 34 sources: 3.2  10 -15 cgs  48 ROSAT sources

5. XMM PN+MOS (PV): 100 ks Lockman Hole 0.5-2.0 keV 2.0-4.5 keV 4.5-10 keV

6. XMM EPIC PV + AO1 (PI: Barcons) + AO2 (PI: Hasinger): 700 ks Lockman Hole 0.5-2.0 keV 2.0-4.5 keV 4.5-10 keV

7. XMM EPIC PV + AO1 (PI: Barcons) + AO2 (PI: Hasinger): 700 ks Lockman Hole 0.5-2.0 keV 2.0-4.5 keV 4.5-10 keV 10’ 128 (PV) -> 252 sources

8. logN-logS Rosati et al. 02 Chandra Deep Field South (940 ksec) XMM LH 100 ksec Gilli et al., 2001 models HDF North Fluctuations (970 ksec) Miyaji&Griffiths XMM LH 700 ksec

9. XMM PN+MOS

11. ROSAT #12A Sy 2-Galaxy z=0.99 Two independent X-ray continua? ROSAT Chandra XMM-Newton hard soft

13. X-ray color-color plot Type-I Type-II Unidentified

14. LH Optical/NIR coverage 30 arcmin V, I: UH 8K < 25.5 mag* R: Keck LRIS < 25 mag K: Calar Alto  ‘ < 20 mag** *courtesy G. Wilson, IfA, Kaiser et al., 2000 **partially courtesy K. Meisenheimer (CADIS) Keck/SUBARU M. Schmidt (Caltech) P. Henry (Hawaii) M. Akiyama (Subaru) Y. Hashimoto (MPE) I. Lehmann (MPE) G. Szokoly (MPE)

15. ID status of the XMM-PV Survey Spec. ID Non spec. ID  ERO‘s Non ERO‘s Phot. Redshift V-image (Wilson & Kaiser, priv. com.)

16. Keck spectroscopy XMM-PV type II AGN GAL (log L X =40.2, soft source) type II AGN (log L X ~43.0) type II/Gal (log L X ~42.0)

17. Type II AGNs vs. Galaxies High ionization narrow emission lines (e.g, Ne V) Hydrogen column density log N H > 22.0 ->Intrinsic absorption X-ray luminosity log L X > 43.0 Narrow emission lines (no NeV) or galaxy- like spectra Hydrogen column density log N H ~ 20.0 No intrinsic absorpt. X-ray luminosity log L X < 42.0

18. 0.5-2 keV2-4.5 keV4.5-10 keV AGN type I342813 AGN type II20  37%19  68%14  79 % Type II/Gal51- Gal3-- Group/Cluster2-- Star1-- No ID, (EROs)41 (15)21 (10)7 (3) Completeness61 %70 %79 % Source Populations

19. Redshift distribution Majority type II AGN at z<1

20. Spectroscopic follow-up of the 700ksec sample …on going with DEIMOS@KECK 4 masks in March ………some new-z from Ingo…

21. RX J105343+5735 high-z cluster XMM EPIC Chandra HRC Hashimoto et al., 2003New redshift! Optically confirmed

22. Summary Flux limit in the [5-10 keV] lower than in 1Msec Chandra surveys ->highly absorbed sources High quality X-ray spectra High identification completeness for the hard sample On going Keck spectroscopy on the newly detected X-ray sources