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The population of high-redshift type-2 quasars found in deep Chandra and XMM-Newton surveys The Formation and Early Evolution of Galaxies, Irsee Workshop, July 1th 2003 Ingo Lehmann MPE-Garching, Germany

Content XMM-Newton Deep Survey in the Lockman Hole & Chandra Deep Field-South Survey XMM-Newton Deep Survey in the Lockman Hole & Chandra Deep Field-South Survey Optical/X-ray properties of the new sources Optical/X-ray properties of the new sources The population of type-2 Quasars The population of type-2 Quasars Summary Summary

Collaboration Maarten Schmidt (Caltech) Günther Hasinger, Gyula Szokoly (MPE) Vincenzo Mainieri, Yas Hashimot (MPE) Jaqueline Bergeron (Institut d‘Astroph. Paris) Piero Rosati (ESO) Andy Fabian (Cambridge, UK) Roberto Della Ceca (Osserv. Astron. di Brera) Steve S. Murray (Cambridge, US) Pat Henry (University of Hawaii) Masayuki Akiyama (Subaru) Xavier Barcons (Santander)

ROSAT All Sky Survey (N H =5.9 x cm -2 ) Lockman Hole Field 106 sources: 3.8  cgs 69 sources: 2.1  cgs 34 sources: 3.2  cgs keV keV keV ~100 ksec PN/MOS1+2 Soft/Hard/Ultrahard samples: CDF-S HDF-N 12 / 7 sources not detected in the soft band XMM-Newton Deep Survey

Comparison ROSAT/XMM ROSAT HRI-PSPC (0.1-2 keV) 1.3 Msec 100 ksec XMM EPIC pn/Mos ( keV) Flux factor: ~3 (CDFS/HDF-N 1Msec ~ 6 times fainter) ( keV) Giacconi et al. 2001, Brandt et al. 2001

XMM PN+MOS (PV): 100 ksec keV keV keV Hasinger et al. 2001

860 ksec PV+AO1+AO keV keV keV Core sample: 213 sources: 1.0  cgs 173 sources: 2.7  cgs 78 sources: 1.0  cgs (253 sources in keV band)

940 ksec exposure ACIS-I 64 arcmin 2 S min = 6* keV keV keV Giacconi et al., 2001 Giacconi Bergeron Borgani Chen Gilli Gilmozzi Hasinger Lehmann Kellermann Kewley Nonino Norman Rosati Schreier Szokoly Tozzi Zheng Chandra Deep Field-South Survey

logN-logS Rosati et al. 02 Chandra Deep Field South (940 ksec) XMM LH 100 ksec Gilli et al., 2001 models HDF North Fluctuations (970 ksec) Miyaji&Griffiths 2002 XMM LH 860 ksec % of the keV XRB ~60% of the 5-10 keV XRB

ROSAT/XMM optical/NIR IDs AGN type1 AGN type2  Cluster/group  Star + unidentified spectroscopy limit 1 f X /f opt = 1 XMM limit spectroscopy limit 1 f X /f opt = EROs

Photometric redshifts R-K‘>5.0 EROs V R I z JH K H  line z=2.42 Lehmann et al (L. Pozzetti) Subaru ICRS* H  line z=2.45 (*PI: M. Akiyama, P. Henry)

Optical counterparts type II AGN GAL (log L X =40.2,soft source) type II AGN (log L X ~43.0) type II/Gal (log L X ~42.0) Keck LRIS spectra PI: M. Schmidt

DEIMOS Spectroscopy of the 860 ksec Lockman sources 4 masks observed in March 2003

360 Mbyte per file DEIMOS – mask Red CCD Blue CCD

High-redshift cluster (z=1.13) KECK VIK z=2.57 ARC ERO z=1.13 ERO ERO‘s High-z Cluster Merging? Hasinger et al Thompson et al Hashimoto et al DEIMOS LRIS

XMM absorbed AGN spectra AGN type II – intrinsic absorption ( cm -2 ) AGN type IAGN type IIFe II K line

Colour segregation Lehmann et al. (2001) Mainieri et al. (2002) type-2 AGN show galaxy colours Lockman Hole CDF-S Intrinsic absorption

Photon index vs. Intrinsic Abs. Mainieri et al AGN type II strongly absorbed Sign for intrinsic absorption in several AGN type I ! 74 (98) sources, counts >70

NGC 6240 ROSAT XMM/Chandra AGN model – absorbed AGN (II) Starburst galaxy XMM/Chandra reveal AGN Komossa et al. 2002

VLT IDs of CDFS sources 153 spectroscopic redshifts (131 high quality) R<24 sample : 116/155 (~75%) Type-1 :57 Type-2 :67 Gal :26 Star :4 QSO-2 :9

CDFS Redshift Distribution Redshift Number Most X-ray sources at lower redshift (z<1) Lockman Hole

Definition of type-2 Quasars No broad emission lines in the optical/near- infrared spectrum Intrinsic absorption with Hydrogen column densities of N H > cm -2 Intrinsic X-ray luminosity L X >10 44 erg s -1 in the keV or in the keV energy bands

Pre-XMM/Chandra Era EMSS field z=0.338 Stocke et al IRAS z=0.185 Elizalde, Steiner 1994 ROSAT QSO Survey z=2.350 Almaini et al ASCA Lynx field z=0.900 Ohta et al Deep ASCA Survey z=0.672 Boyle et al ASCA LSS field z=0.653 Akiyama et al EMSS z=2.35 Georgantopoulos et al No evidence for type-2 Quasars ! broad H  Halpern et al. 1999

First high-z type-2 Quasars Stern et al Dawson et al Norman et al HDF-N*CDF-S Lynx field Futher: Crawford et al. 2001, Fabian et al Fe K   =0.51  0.27 N H ~10 24 cm -2 R-Ks=2.5 L 2-10 =10 45  0.5 Radio quiet EW K  ~1keV

CDF-S type-2 Quasars FHWM< 2000 km/s Szokoly et al z=2.940 z=2.562z=3.660 z=3.240

X-ray/optical properties of type-2 QSO CDF-S 1 f X /f opt = 1 3 mag fainter in R Type-2 Quasar are ~3 mag fainter than type-1 quasar

Fraction of type-2 QSOs CDFS Lockman Hole ~10 %  Significant population!!!

Search for low-z type-2 Quasars L X, obs ~5 x erg/s

XMM-Newton MOS1+2/PN group or cluster pointing PI: M.Watson XX Serendipity source

EPIC-pn spectrum N h ~2 x10 22 cm -2 Photon index ~1.6 Black body ~0.12 kT flux ~3 x erg s -1 cm -2 ( keV) First check! L =10 45 erg/s X-ray bright type-2 Quasar !!!

XMM SSC XID proposal Optical identification of ultrahard X-ray sources  Search for X-ray bright type-2 Quasars (z<1) Sample selection: X-ray sources from the XCAT-DB X-ray flux keV > erg s -1 cm -2 (XID-band) Detection likelyhood > 16 HR2 > -0.3, optical counterpart with 3“ in radius |b| > 30 degree, R < 21. m 0  Southern sample consists of 31 objects !

Low-z type-2 Quasar candidates Source XID flux [ cgs] [ cgs]HR2 z L XID,obs L XID,obs [10 44 erg/s]     

Summary ~90 % of the 2-10 keV X-ray background resolved ~90 % of the 2-10 keV X-ray background resolved Most new XMM sources - ERO‘s (R-K‘> 5.0) Most new XMM sources - ERO‘s (R-K‘> 5.0) XMM hard sources - type II AGN at z<1, power law spectra with significant intrinsic, absorption. XMM hard sources - type II AGN at z<1, power law spectra with significant intrinsic, absorption. Significant population of type-2 Quasars Significant population of type-2 Quasars Important to search for low-z type-2 quasars Important to search for low-z type-2 quasars

AGN Space Density Miyaji et al., 2000 ?

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X-ray/Sub-mm Correlation Fox et al I-band K-band LH850.8 HRI VLA 450mJy AGN type I NELG ERO z~0.9 z~0.7 Extremely hard to identify!

LLAGN Luminosity Function! z=0 z>2 Galaxies AGN HST