2. X-ray Surveys Lockman Hole Team Giacconi (JHU) Gunn (Princeton)
Schmidt et al., Hasinger et al., 1999
PSPC keV HRI keV PSPC keV
Lockman Hole
Team
Giacconi (JHU)
Gunn (Princeton)
Hasinger (AIP)
Lehmann (Penn State)
Schmidt (Caltech)
Schneider (Penn State)
Szokoly (AIP)
Thompson (Caltech)
Trümper (MPE)
Zamorani (Bologna)
et al.

3. 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)

4. 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

5. Optical/NIR correlations
fX/fopt=1
spectroscopy
limit +
Photometric redshifts + + + + +
ROSAT limit
 AGN type1  AGN type2  Cluster/group  Star + unidentified

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

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

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

9. Lockman Hole (XMM PV) PV Team PV Observations 27.4-18.5 2000
PN CCD (MPE Garching) MOS1 CCD (Leicester U)
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)
PV Team
PV Observations
190 ksec data
100 ksec low background

12. Exposure map
Raw Image
Exposure corrected
Exposure correction

13. Colour Image
keV keV keV PN+MOS1+MOS2

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

15. Detection Summary
Algorithm: multi-band, multi-ML source detect and parameter
estimation, developed in Potsdam for XMM SAS, building on
ROSAT experience
Detection: ML> 10 at off-axis angles < 10 arcmin, no exposure
map (yet), vignetting fudged.

16. Soft logN-logS (0.5-2 keV)
XMM/ROSAT
Chandra
Giacconi
Mushotzky

17. Hard logN-logS (2-10 keV)
XMM/ASCA
Chandra
Mushotzky
Giacconi

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

19. Spectral fits XMM PN, MOS1, MOS2 and PSPC combined PN MOS1+2 PSPC
Mostly excellent fits are obtained with the same spectral shape for all four instruments,
only varying the relative normalization by ~20%.

20. Sample QOS/Sy1 spectra Sample QSO/Sy1 spectra
Type-1 sources have typically simple, steep,
unabsorbed power law spectra.
NH consistent with neutral galactic hydrogen
(no evidence for Reynolds layer)

21. Sample Sy-2/QSO-2 spectra
Type-2 sources have steep power law
spectra with significant intrinsic absorption.
NH = cm-2

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

23. 6.4 keV
restframe
Kerr BH
Inclination  15o
Ri  5 RG
Ro  20 RG 1 2
Kerr
Schwarz-
schild

24. Opt/NIR ID of XMM sources
I-band (CFHT 8K) K-band (Calar Alto)
Extremely Red Object (ERO)
10“

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

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

28. Summary Watch this space ! 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 !

29. Absorbed vs. unabsorbed
Optical absorbed
 Mushotzky et al., 2000
 Fiore et al., 2000
More than half of the AGN
will optically appear as
„normal“ galaxies.
=> look out for high-excitation
lines and large Balmer
decrement
courtesy R.Gilli, 2000

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