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