lockman hole (xmm pv) pn ccd (mpe garching) mos1 ccd (leicester u) pn ccd (mpe garching) mos1 ccd...
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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
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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
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Comparison XMM/ROSATComparison XMM/ROSAT
XMM X-ray Colours (0.5-10 keV) ROSAT HRI-PSPC (0.1-2 keV)
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logN-logSlogN-logS
XMM
ChandraGiacconi et al.
ROSATfluctuations.
ROSAT
BeppoSAXfluctuations.
ASCA
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Very hard logN-logS (5-10 keV)Very hard logN-logS (5-10 keV)
XMM/BeppoSAX
Gilli model
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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 !
+++
+ +
++
+
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6.4 keVrestframe
Kerr BHInclination 15o
Ri 5 RG Ro 20 RG
1
2
Kerr Schwarz-schild
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A surprise !A surprise !
Inclination=45o
Ri unconstrainedRo 20 RG
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High-redshift clusterHigh-redshift clusterKeck NIRPEC
Thompson et al., 2000
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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
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Cluster Luminosity/Temperature Relation
Cluster Luminosity/Temperature Relation
Borgani, Tozzi,Rosati (2000)
z=1.26
z=0.26
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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)
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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
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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
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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
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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
+
+ +
+
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Hardness vs. Colour Hardness vs. Colour
EROs have hard X-ray spectra AGN
HR1 HR2
+++
+++
++
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NGC 6240
QSO-2 SpectraQSO-2 Spectra
NGC 6240NGC 6240
QSO averageQSO average(Elvis et al.)(Elvis et al.)
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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 !
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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