Xray source populations from the XMMNewton Medium Survey

1
X-ray source populations from the XMM-Newton
Medium Survey

• Francisco J. Carrera, X. Barcons, J. Bussons, J.
  Ebrero, M. Ceballos, A. Corral (IFCA,
  CSIC-UC, Spain)
• XMM-Newton Survey Science Centre
• (S. Mateos, M. J. Page, M.G. Watson, J. Tedds, R.
  Della Ceca ...)

X-ray Surveys, Rodos, 2 July 2006
2
Definition of the surveys
Mrk 205

• AXIS (Carrera07)
• 36 XMM-Newton target fields
• Galactic latitude bgt20 deg
• Good quality source screening
• Solid angle 4.8 deg2
• Total of 1434 distinct X-ray sources with
  detection likelihood gt15
• XMS subset of AXIS (Barcons07)
• 25 fields chosen for follow-up 3.3 deg2
• Flux limited in Soft, Hard and XID total of 319
  sources
• Optical imaging g,r,i (SDSS) to r23-24
• Reliable unique candidate counterpart in r/i
  for virtually all sources (lt 5 or lt 5?) only 8
  empties
• Optical spectroscopy
• 5m and 8m-class longslit spectra

3
The XMS samples
4
Breakdown of identified sources
2 BL Lacs
Clear differences between Soft/XID and
Hard/Ultrahard selected samples
5
Luminosities and redshifts
Krumpe07
log(LSoft cgs)
Soft
QSOs
z
log(LHard cgs)
Seyferts
Hard
Some of these NELGs have optical line
ratios typical of STB (Barcons) All UnIDed Hard
sources are optically extended galaxies too
z
6
Redshift distribution
Soft
Peak of QSO distribution (z1.5) well sampled.
BLAGN

NELG
Gal
Hard
BLAGN
z
Obscured population out to z1 in Hard sample

Gal
NELG
z
7
X-ray spectral analysis
8
X-ray spectral analysis Corral07
Full sample
NH
z

• Extracted X-ray spectra (pnMOS) for all 319
  sources
• Fitted Gal. abs. power law
• Fitted Gal. abs. Intrinsic abs. power law
• F-test 95 X-ray absorbed 70 ? Filled symbols
• 17 BLAGN 92
• 20 NELG 427
• 9 Gal 6911

9
X-ray spectral analysis Corral07
Full sample
22 (567) UnIDed X-ray absorbed ? UnID obscured
AGN?
10
Averaging X-ray spectraCorral07 (see poster 1)
AXISXWAS NELGs
AXISXWAS BLAGN

• Averaging AXISXWAS (Tedds07)
• BLAGN (606) ?1.88 Fe line _at_6.4 keV EW11010 eV
  red wing????
• NELG (113) ?1.34 Fe line _at_6.4 keV EW15010
  eV red wing????

11
Obscured and Unobscured AGN
12
X-ray to optical ratio a marker for obscuration?
log(FSoft/Fopt)

• 3 of sources with FX/Foptgt10
• 33 of FX/Foptgt10 obscured AGN

log(FHard/Fopt)
Hard

• 21 of sources with FX/Foptgt10
• 24-79 of FX/Foptgt10 obscured AGN

FX(10-14cgs)
13
Tips for statistical identification
80 unobscured AGN
log(FHard/Fopt)
40 Obscured AGN (most Xabs) 40 UnID (most
Xabs)
Full sample
Stars
HR2
14
Optical colours
r-i
g-r
g-r
Hard
Soft

15
Optical versus X-ray colours Hard
Bussons07
Harder sources are 40-80 obscured AGN Softer
sources Optically blue unabsorbed AGN
Optically red mix of abs unabs AGN
g-r
Hard
HR2
16
Fainter sources are not redder
Soft
g-r
FX(10-14cgs)
Hard
g-r
FX(10-14cgs)
17
Conclusions
18

• Unobscured accretion dominates, but increasingly
  important contribution from obscured objects.
• X-ray absorption and optical obscuration not
  equivalent
• 10 of type 1 AGN are X-ray absorbed
• 15 of type 2 AGN are not X-ray absorbed
• 25 of FX/Foptgt10 hard X-ray sources are type 1
  AGN
• 10 of X-ray selected type 1 AGN have red colours
• Even at medium fluxes, an important fraction of
  the X-ray sources have optically faint and red
  optical counterparts
• Need 10m class observing time
• Most unIDed objects faint (r/igt21.5), ext. and
  Xabs NELGs?
• On-going work
• Average spectra show narrow Fe lines in both
  BLAGN and NELGs (Amalia Corrals poster 1)
• Luminosity function and spatial correlation
  function (Jacobo Ebreros
  poster 4)