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Tracing cosmic accretion through the XMM-Newton Medium Survey (XMS)

Tracing cosmic accretion through the XMM-Newton Medium Survey (XMS). Xavier Barcons On behalf of the AXIS/XMS/SSC team. Index. The role of medium sensitivity surveys The XMS survey The content of the XMS survey Tips for statistical identifications Outlook and future work.

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Tracing cosmic accretion through the XMM-Newton Medium Survey (XMS)

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  1. Tracing cosmic accretion through the XMM-Newton Medium Survey (XMS) Xavier Barcons On behalf of the AXIS/XMS/SSC team

  2. Index • The role of medium sensitivity surveys • The XMS survey • The content of the XMS survey • Tips for statistical identifications • Outlook and future work The X-ray Universe 2005

  3. The role of Medium Surveys • Bridge between most popular deep surveys and surveys of the local Universe • The average XMM-Newton observation (10-20 ks of GTI) is a Medium Sensitivity Survey: • The 2XMM catalogue will be a huge MSS • The bulk of the cosmic X-ray background resides at intermediate X-ray fluxes (~10-14 erg cm-2 s-1) The X-ray Universe 2005

  4. Relative contribution to XRB per flux decade  S dN(S)/d log S The X-ray Universe 2005

  5. Fraction of XRB resolved by X-ray surveys The XMS resolves ~50% of the 0.5-4.5 keV X-ray background XMS BSS Deep The X-ray Universe 2005

  6. The XMS survey and its optical identification

  7. NGC4291 Definition of the XMS sample Mrk 205 • 25 XMM-Newton target fields: • Galactic latitude |b|>20 deg • X-ray observations with EPIC-pn detector in FULL-FRAME-MODE • ~Avoided fields with bright and/or extended targets • Good time intervals > 10 ksec • Available early on in the mission • Using SAS v6.1.1 to produce final source list and products: • Exposure and background maps • Source detection • Spectra and calibration matrices • Areas around target + OOT+ near the pn CCD gaps excluded • Own empirical sentitivity maps from detected source parameters • 284 sources with 0.5-4.5 keV flux >2 10-14 erg cm-2 s-1 • Very detailed source screening The X-ray Universe 2005

  8. Statistics of XMS fields The X-ray Universe 2005

  9. Optical identification of XMS • Optical imaging: g’,r’,i’ and more to r’~23-24mag • Reliable & unique candidate counterpart in r’/i’ for virtually all sources (< 5” or < 5) • Optical spectroscopy • 50% from AXIS programme (WHT, TNG, NOT): multi-fibre and long-slit spectroscopy • 20% from Calar Alto/3.5m long-slit spectroscopy • 15% from VLT/FORS2 long-slit spectroscopy • A few from AAT/2dF, SUBARU/FOCAS, and others • Preliminary results from 2 XMM-Newton fields (~30 sources) in Barcons et al (2002) The X-ray Universe 2005

  10. XMS Identification status • 25 XMM fields • XID:0.5-4.5 keV • SXID>210-14cgs • Ω=3.3 deg2 The X-ray Universe 2005

  11. The content of the XMS Identification breakdown Remaining incompleteness & biases Towards the X-ray luminosity function

  12. Breakdown of identified sources in the XMS The X-ray Universe 2005

  13. Fluxes and redshifts The X-ray Universe 2005

  14. Incompleteness and remaining biases The X-ray Universe 2005

  15. Redshift distribution The X-ray Universe 2005

  16. QSO-2s S(0.5-4.5)=1.1 10-13 erg cm-2 s-1 z=0.711 LX=1044.4 erg s-1 Absorbed: =0.55 The X-ray Universe 2005

  17. Bright Source Survey Deep Surveys The L-z plane and the X-ray Luminosity Function Unfortunately, photo-z’s do not work with our limited colour information The X-ray Universe 2005

  18. Γd=1.34+0.01-0.07 Γu=2.55+0.03-0.04 Sb=1.69+0.02-0.0110-14 cgs Source counts See poster G.2 for more details The X-ray Universe 2005

  19. Spectra of individual sources well matched to unified model, but with exceptions (Mateos et al 2005) X-ray spectral templates: de-redshifted average spectra (see poster E.11 by Corral et al) ? ? X-ray spectral properties of AGN The X-ray Universe 2005

  20. Tips on statistical identification

  21. Statistical identification • Probabilistic classification of X-ray sources, based on: • X-ray colours • Optical colours • X-ray to optical flux ratios • X-ray and/or optical morphology • Large parameter space: start with “preliminary inspection” (fishing expedition), later apply mathematical tools (PCA, ANNs, etc.) The X-ray Universe 2005

  22. >50% NELG >60% NELG >80% NELG 100% NELG >75% ALG 100% Stars >85% BLAGN HR2=(H-S)/(H+S) H=2.0-4.5 keV S=0.5-2.0 keV The X-ray Universe 2005

  23. Optical colour-colour diagrams 50% NELGs 50% “red” BLAGNs SDSS Early-type galaxies SDSS QSOs 95% BLAGNs The X-ray Universe 2005

  24. Red & Hard NELGs Red & Soft ALG Blue BLAGN Optical vs X-ray colours The X-ray Universe 2005

  25. Obscuration/reddening The X-ray Universe 2005

  26. Obscuration/reddening The X-ray Universe 2005

  27. Tips for statistical identifications • Sources with log (fX/fopt)<-1.5 are invariably stars • Optically blue objects are 95% BLAGN • Optically red objects include both broad-line and narrow line AGN • Red & soft galaxies do not have emission lines • Red & hard galaxies have narrow emission lines • There is a large patch of parameter space shared by both broad and narrow line AGN. The X-ray Universe 2005

  28. Outlook and future work • Spectroscopic identification of remaining 15% objects needed (photo-z’s do not work) • Combine with Bright and Deep Surveys to compute AGN X-ray luminosity function and evolution • Compute Accretion power as a function of z, both for absorbed and unabsorbed sources • Explore larger sample (XMM/2dF) in the search for statistical identification handles • Apply statistical identification to 2XMM catalogue The X-ray Universe 2005

  29. Thanks to: • Francisco Carrera • Maite Ceballos • Silvia Mateos • Amalia Corral • Francesca Panessa • Jacobo Ebrero • Mat Page • Axel Schwope • Mike Watson • Roberto Della Ceca • Jonathan Tedds • Tommaso Maccacaro • And many more… The X-ray Universe 2005

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