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An XMM-Newton International Survey (AXIS): A progress report

An XMM-Newton International Survey (AXIS): A progress report. Xavier Barcons & Francisco Carrera Instituto de Física de Cantabria (CSIC-UC) on behalf of the AXIS consortium and the XMM Survey Science Centre XID wg. The AXIS team http://www.ifca.unican.es/~xray/AXIS.

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An XMM-Newton International Survey (AXIS): A progress report

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  1. An XMM-Newton International Survey (AXIS): A progress report Xavier Barcons & Francisco Carrera Instituto de Física de Cantabria (CSIC-UC) on behalf of the AXIS consortium and the XMM Survey Science Centre XID wg

  2. The AXIS teamhttp://www.ifca.unican.es/~xray/AXIS • Astrophysikalisches Institut Potsdam (Germany): Y. Hashimoto, G. Hasinger, G. Lamer, G. Szokoly, A. Schwope • Centre d'Etude Spatiale des Rayonnements (France): N. Webb • Institute of Astronomy, Cambridge (UK): R.G. McMahon, A.C. Fabian, C.S. Crawford • Instituto de Astrofísica de Canarias, Tenerife (Spain):I. Pérez-Fournon • Instituto de Física de Cantabria, Santander (Spain): X. Barcons, F.J. Carrera, M.T. Ceballos, S. Mateos • Laboratorio de Astrofísica Espacial y Física Fundamental, Madrid (Spain): J.M. Mas-Hesse • Max-Planck-Institut fuer extraterrestriche Physik (Germany): T. Boller • Mullard Space Science Laboratory, UCL (UK): M.S. Cropper, K.O. Mason, J.P.D. Mittaz, M.J. Page, S. R. Rosen • Observatoire Astronomique de Strasbourg (France): C. Motch, P. Guillout, L. Mirioni, I. Negueruela • Osservatorio Astronomico di Brera, Milano (Italy): T. Maccacaro, R. Della Ceca, P. Severgnini • University of Bristol (UK): D.M. Worrall, M. Bremer, M. Birkinshaw • University of Central Lancashire (UK): G.E. Bromage, B.J.M. Hassall • University of Leicester, (UK): M.G. Watson, J.P. Pye, G.C. Stewart, T. Roberts, J.P. Osborne, N. Schurch, P.J. Wheatley, M.J. Ward, R.S. Warwick • XMM Science Operations Centre, (Spain): N. Schartel

  3. The XMM Survey Science Centre XID programme • Expect 50,000 new X-ray sources/year • Core programme (1000 sources/sample): • High b faint sample (10-15 erg cm-2 s-1) • High b medium sample (10-14 erg cm-2 s-1) • High b bright sample (10-13 erg cm-2 s-1) • Galactic Plane Sample • Imaging programme (u,g’,r’,i’,Z,H) • Statistical identifications based on X-ray properties & imaging programme.

  4. The Observatorio del Roque de los Muchachos NOT (2.5) JKT (1.0) WHT (4.2) INT (2.5) GTC (10) TNG (3.5)

  5. We are here now! AXIS:Breakdown of observing nights

  6. AXIS instruments used

  7. AXIS wide-field imaging (includes M. Watson’s PATT Imaging proposal) Optical: INT/WFC Near IR: INT/CIRSI

  8. AXIS: Search for candidate counterparts i’-band sources within either: 5 (statistical) or 5 arcsec Clusters? Reddened sources? AGNs beyond the Galaxy?

  9. Candidate counterparts &systematics • Count rate > 0.005 ct s-1 • |b|>10º • Single candidate counterpart • 108 sources 66% Pobs(x)=f0*P(x|0)+ f1*P(x|x1) x1=2, 33% f0=0.67; x0=0 (fixed) f1=0.33; x1=2.0 P(x|x0)=|x-x0|* exp(-|x-x0|2/2)

  10. AXIS identifications(as of March 1, 2001)

  11. The AXIS medium sample • 35 sources brighter than 2 10-14 erg cm-2 s-1 in the 0.5-4.5 keV band (2 XMM fields, excluding targets). • 32/35 identified (>90%); remaining 3 have i’>22.5

  12. Medium sample: offsets

  13. Medium sample: L-z

  14. Medium sample: z distribution Most objects at z~1-2 as expected from XRB synthesis models

  15. Medium sample: type 1 vs type 2 AGN • Expect ~60% of AGN to be unabsorbed in the Comastri et al XRB model • We find 22/34 (65%) BLAGN among the extragalactic sources

  16. Medium Sample: BAL QSOs • BAL QSOs in previous X-ray surveys: • 1 in Chandra deep survey (Giacconi et al 2001) • 1 in hard X-ray selected ROSAT sample (Page et al 2001) • 1 in ISO/BeppoSAX survey (Alexander et al 2001) • In the medium sample we have 1 confirmed and 2 highly suggestive BAL QSOs (~5-10% of BLAGN): • Higher sensitivity of XMM-Newton • Harder photon energies (even @ 4.5 keV)

  17. Medium sample: BAL QSO spectra z=1.82 z=0.79? z=1.91 Z=1.82

  18. SS279 AXIS Galactic Plane sample: the G21.5-09 field (b=-1º)

  19. A Be+NS/WD? accreting binary

  20. AXIS Galactic Plane sample: Active Coronae Higher sensitivity highlights AC with very weak e.l.s

  21. We are here now! AXIS expectations

  22. Conclusions • Sensitivity & response to hard X-rays of XMM-Newton make it sensitive to new classes of objects • Medium sample (> 2 10-14 erg cm-2 s-1): • 68% of sources are BLAGNs (consistency with unified XRB models) • z-distribution peaks at z~1-2 • 5-10% of BLAGNS are BALs • Galactic Plane: • Active Coronae with very weak emission lines • Accreting binaries

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