New XMM-Newton deep Survey in the
Lockman HoleVincenzo Mainieri
MPE
Workshop on AGN Surveys, Puebla, June 23- July 11, 2003
Guenther HasingerHans BoehringerHermann BrunnerIngo LehmannYas HashimotoGyula Szokoly
Xavier Barcons Andy Fabian
Motivation
ROSAT All Sky Survey
Resolve the XRB!Nature of the sources?
(NH=5.9 x 1019 cm-2)
Lockman Hole Field
ROSAT PSPC
ROSAT observationsROSAT HRI-PSPC (0.1-2 keV)
ROSAT DeepSurvey (RDS)
Ultra Deep Survey (UDS)
207 ksec PSPC (0.5-2.0keV)50 sourcesFlux limit: 5.5 x 10-14 cgs
1.3 Msec HRI (0.5-2.0 keV)94 sourcesFlux limit: 1.2 x 10-15 cgs
Hasinger et al. 1998, Lehmann et al. 2001
Lockman Hole - PV (120 ksec)
Hasinger et al., 2001
0.5-2.0 keV2.0-4.5 keV4.5-10 keV
XMM Deep Survey
106 sources: 3.810-16 cgs
69 sources: 2.110-15 cgs
34 sources: 3.210-15 cgs
48 ROSAT sources
XMM PN+MOS (PV): 100 ks
Lockman Hole
0.5-2.0 keV2.0-4.5 keV4.5-10 keV
XMM EPIC PV + AO1 (PI: Barcons) + AO2 (PI: Hasinger): 700 ks
Lockman Hole
0.5-2.0 keV2.0-4.5 keV4.5-10 keV
XMM EPIC PV + AO1 (PI: Barcons) + AO2 (PI: Hasinger): 700 ks
Lockman Hole
0.5-2.0 keV2.0-4.5 keV4.5-10 keV
10’
128 (PV) -> 252 sources
logN-logS
Rosati et al. 02
Chandra DeepField South(940 ksec)XMM LH 100 ksec
Gilli et al., 2001 models
HDF NorthFluctuations(970 ksec)Miyaji&Griffiths
XMM LH 700 ksec
XMM PN+MOSXMM PN+MOS
XMM PN+MOSXMM PN+MOS
ROSAT #12A
Sy 2-Galaxy z=0.99
Two independent X-ray continua?
ROSAT
Chandra
XMM-Newton
hard
soft
X-ray color-color plot
Type-I
Type-II
Unidentified
LH Optical/NIR coverage
30
ar c
min
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)
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.)
Keck spectroscopy XMM-PV
type II AGN
GAL (log LX=40.2, soft source)
type II AGN (log LX~43.0)
type II/Gal (log LX~42.0)
Type II AGNs vs. Galaxies
• High ionization narrow emission lines (e.g, Ne V)
• Hydrogen column density log NH > 22.0->Intrinsic absorption
• X-ray luminosity log LX > 43.0
• Narrow emission lines (no NeV) or galaxy-like spectra
• Hydrogen column
density log NH~ 20.0
No intrinsic absorpt.
• X-ray luminosity log LX< 42.0
0.5-2 keV 2-4.5 keV
4.5-10 keV
AGN type I 34 28 13
AGN type II 20 37%
19 68%
14 79 %
Type II/Gal 5 1 -
Gal 3 - -
Group/Cluster
2 - -
Star 1 - -
No ID, (EROs)
41 (15) 21 (10) 7 (3)
Completeness
61 % 70 % 79 %
Source Populations
Redshift distribution
Majority type II AGN at z<1
Spectroscopic follow-up of the 700ksec sample
…on going with DEIMOS@KECK
4 masks in March
………some new-z from Ingo…
RX J105343+5735high-z cluster
XMM EPIC Chandra HRC
Hashimoto et al., 2003 New redshift! Optically confirmed
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