Lockman Hole (XMM PV) Lockman Hole (XMM PV)

PN CCD (MPE Garching) MOS1 CCD (Leicester U)PN CCD (MPE Garching) MOS1 CCD (Leicester U)

PV Observations27.4-18.5 2000190 ksec data100 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 (LeicesterM. Watson (Leicester))

PV Team

Colour ImageColour Image

0.5-0.2 keV 0.5-0.2 keV 2-4.5 keV2-4.5 keV 4.5-10 keV 4.5-10 keV PN+MOS1+MOS2 PN+MOS1+MOS2

Comparison XMM/ROSATComparison XMM/ROSAT

XMM X-ray Colours (0.5-10 keV) ROSAT HRI-PSPC (0.1-2 keV)

logN-logSlogN-logS

XMM

ChandraGiacconi et al.

ROSATfluctuations.

ROSAT

BeppoSAXfluctuations.

ASCA

Very hard logN-logS (5-10 keV)Very hard logN-logS (5-10 keV)

XMM/BeppoSAX

Gilli model

X-ray DiagnosticsX-ray Diagnostics

= 01

2

3

logNH=23

22.5

22

New XMM sources are significantly harder than ROSAT sources,but mainly have absorbed, intrinsically soft continua

=> type-2 AGN !

+++

+ +

++

+

6.4 keVrestframe

Kerr BHInclination 15o

Ri 5 RG Ro 20 RG

1

2

Kerr Schwarz-schild

A surprise !A surprise !

Inclination=45o

Ri unconstrainedRo 20 RG

High-redshift clusterHigh-redshift clusterKeck NIRPEC

Thompson et al., 2000

Sample cluster Sample cluster spectraspectra

z=1.26 kT=5 keVz=1.26 kT=5 keV

z=0.26 kT=1.5 keVz=0.26 kT=1.5 keV

Constraints on Temperature and abundance possible for very high redshift or low luminosity

Cluster Luminosity/Temperature Relation

Cluster Luminosity/Temperature Relation

Borgani, Tozzi,Rosati (2000)

z=1.26

z=0.26

LH Optical/NIR coverageLH Optical/NIR coverage

30

ar c

min

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)

HRI

PSPC

14Z

K, I, V colour image

Optical IdentificationsOptical Identifications

Keck LRIS + NIRC

84Z

K, I, V colour image

Schmidt et al., 1998; Lehmann et al., 2000

XMM optical IDsXMM optical IDs

AGN type1 AGN type2 Cluster/group Star + unidentified XMMXMM

spectroscopylimit

fX/fopt=11

Chandra/XMM limit

EROs

spectroscopylimit

fX/fopt=11

+++

+++

+

+

Photometric redshifts

Photometric RedshiftsPhotometric Redshifts

Courtesy: L. PozzettiCourtesy: L. Pozzetti

poor fit!

V RI

zJ H K

z=1.9 z=1.5

z=1.2 z=1.4

Colour SegregationColour 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 athigh redshift

+

+ +

+

Hardness vs. Colour Hardness vs. Colour

EROs have hard X-ray spectra AGN

HR1 HR2

+++

+++

++

NGC 6240

QSO-2 SpectraQSO-2 Spectra

NGC 6240NGC 6240

QSO averageQSO average(Elvis et al.)(Elvis et al.)

SummarySummary

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 !

Chandra obscured AGNChandra 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