Tracing cosmic accretion through the XMMNewton Medium Survey XMS

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

• Xavier Barcons
• On behalf of the AXIS/XMS/SSC team

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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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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)

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Relative contribution to XRB per flux decade
? S dN(S)/d log S
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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
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The XMS survey and its optical identification
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Definition of the XMS sample
Mrk 205

• 25 XMM-Newton target fields
• Galactic latitude bgt20 deg
• X-ray observations with EPIC-pn detector in
  FULL-FRAME-MODE
• Avoided fields with bright and/or extended
  targets
• Good time intervals gt 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
• gt2 10-14 erg cm-2 s-1
• Very detailed source screening

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Statistics of XMS fields
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Optical identification of XMS

• Optical imaging g,r,i and more to r23-24mag
• Reliable unique candidate counterpart in r/i
  for virtually all sources (lt 5 or lt 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)

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XMS Identification status

• 25 XMM fields
• XID0.5-4.5 keV
• SXIDgt2?10-14cgs
• O3.3 deg2

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The content of the XMS

• Identification breakdown
• Remaining incompleteness biases
• Towards the X-ray luminosity function

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Breakdown of identified sources in the XMS
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Fluxes and redshifts
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Incompleteness and remaining biases
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Redshift distribution
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QSO-2s
S(0.5-4.5)1.1 10-13 erg cm-2 s-1 z0.711 LX1044.
4 erg s-1 Absorbed ?0.55
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The L-z plane and the X-ray Luminosity Function
Unfortunately, photo-zs do not work with our
limited colour information
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Source counts
See poster G.2 for more details
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X-ray spectral properties of AGN

• 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)

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Tips on statistical identification
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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.)

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gt85 BLAGN
HR2(H-S)/(HS) H2.0-4.5 keV S0.5-2.0 keV
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Optical colour-colour diagrams
50 NELGs 50 red BLAGNs
SDSS Early-type galaxies
SDSS QSOs
95 BLAGNs
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Optical vs X-ray colours
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Obscuration/reddening
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Obscuration/reddening
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Tips for statistical identifications

• Sources with log (fX/fopt)lt-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.

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Outlook and future work

• Spectroscopic identification of remaining 15
  objects needed (photo-zs 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

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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