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New XMM-Newton deep Survey in the Lockman Hole

New XMM-Newton deep Survey in the Lockman Hole. Vincenzo Mainieri MPE. Guenther Hasinger Hans Boehringer Hermann Brunner Ingo Lehmann Yas Hashimoto Gyula Szokoly. Xavier Barcons. Andy Fabian. Workshop on AGN Surveys, Puebla, June 23- July 11, 2003. Motivation. ROSAT All Sky Survey.

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New XMM-Newton deep Survey in the Lockman Hole

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  1. New XMM-Newton deep Survey in the Lockman Hole Vincenzo Mainieri MPE Guenther Hasinger Hans Boehringer Hermann Brunner Ingo Lehmann Yas Hashimoto Gyula Szokoly Xavier Barcons Andy Fabian Workshop on AGN Surveys, Puebla, June 23- July 11, 2003

  2. Motivation ROSAT All Sky Survey Lockman Hole Field ROSAT PSPC Resolve the XRB! Nature of the sources? (NH=5.9 x 1019 cm-2)

  3. ROSAT observations ROSAT HRI-PSPC (0.1-2 keV) ROSAT DeepSurvey (RDS) 207 ksec PSPC (0.5-2.0keV) 50 sources Flux limit: 5.5 x 10-14 cgs Ultra Deep Survey (UDS) 1.3 Msec HRI (0.5-2.0 keV) 94 sources Flux limit: 1.2 x 10-15 cgs Hasinger et al. 1998, Lehmann et al. 2001

  4. Lockman Hole - PV (120 ksec) 0.5-2.0 keV 2.0-4.5 keV 4.5-10 keV XMM Deep Survey 106 sources:3.810-16 cgs 69 sources: 2.110-15 cgs 34 sources:3.210-15 cgs  48 ROSAT sources Hasinger et al., 2001

  5. Lockman Hole 0.5-2.0 keV 2.0-4.5 keV 4.5-10 keV XMM PN+MOS (PV): 100 ks

  6. XMM EPIC PV + AO1 (PI: Barcons) + AO2 (PI: Hasinger): 700 ks Lockman Hole 0.5-2.0 keV 2.0-4.5 keV 4.5-10 keV

  7. XMM EPIC PV + AO1 (PI: Barcons) + AO2 (PI: Hasinger): 700 ks Lockman Hole 10’ 128 (PV) ->252 sources 0.5-2.0 keV 2.0-4.5 keV 4.5-10 keV

  8. XMM LH 100 ksec logN-logS HDF North Fluctuations (970 ksec) Miyaji&Griffiths XMM LH 700 ksec Chandra Deep Field South (940 ksec) Rosati et al. 02 Gilli et al., 2001 models

  9. XMM PN+MOS XMM PN+MOS

  10. XMM PN+MOS XMM PN+MOS

  11. ROSAT #12A ROSAT hard Chandra XMM-Newton soft Sy 2-Galaxy z=0.99 Two independent X-ray continua?

  12. X-ray color-color plot Type-I Type-II Unidentified

  13. LH Optical/NIR coverage V, I: UH 8K < 25.5 mag* R: Keck LRIS < 25 mag K: Calar Alto ‘ < 20 mag** 30 arcmin Keck/SUBARU M. Schmidt (Caltech) P. Henry (Hawaii) M. Akiyama (Subaru) Y. Hashimoto (MPE) I. Lehmann (MPE) G. Szokoly (MPE) *courtesy G. Wilson, IfA, Kaiser et al., 2000 **partially courtesy K. Meisenheimer (CADIS)

  14. 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.)

  15. Keck spectroscopy XMM-PV type II AGN(log LX~43.0) type II AGN type II/Gal(log LX~42.0) GAL(log LX=40.2, soft source)

  16. 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 Type II AGNs vs. Galaxies

  17. Source Populations

  18. Redshift distribution Majority type II AGN at z<1

  19. Spectroscopic follow-up of the 700ksec sample …on going with DEIMOS@KECK 4 masks in March ………some new-z from Ingo…

  20. RX J105343+5735high-z cluster XMM EPIC Chandra HRC Hashimoto et al., 2003 New redshift! Optically confirmed

  21. 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

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