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Obscured and unobscured growth of Super-massive Black Holes from the XMM-Newton Medium Survey. Francisco J. Carrera, X. Barcons, J. Bussons, J. Ebrero, M. Ceballos, A. Corral (IFCA, CSIC-UC, Spain) and many SSC colleagues. SSC#20, Potsdam, Nov. 13, 2006. NGC4291. - PowerPoint PPT Presentation
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Obscured and unobscured growth of Super-massive Black Holes
from the XMM-Newton Medium Survey
Francisco J. Carrera, X. Barcons, J. Bussons, J. Ebrero, M. Ceballos, A. Corral
(IFCA, CSIC-UC, Spain)and many SSC colleagues
SSC#20, Potsdam, Nov. 13, 2006
Definition of the AXIS survey Carrera et
al 06 • 36 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
• Areas around target + OOT+ near the pn CCD gaps excluded
• Solid angle ~4.8 deg2
• Using SAS v6.1.1 to produce final source list and products: – Exposure and background maps– Source detection– Spectra and calibration matrices
• Own empirical sentitivity maps from detected source parameters
• Very detailed source screening• Total of 1433 distinct X-ray sources
with detection likelihood >15 in any of 4 bands (see below)
NGC4291
Mrk 205
Soft0.5-2 keV
XID0.5-4.5
keV
Hard2-10 keV
Ultrahard4.5-7.5 keV
X-ray source counts (BSS/HBS Della Ceca et al. 2004 & CDF Bauer et al. 2004 & AMSS Ueda et al. 2005)
The contribution to the X-ray background
ShallowMediumDeep Surveys
Medium surveysresolve the
brightest50% of the
X-raybackground
Soft
Hard
XID
Ultra-hard
• Detected significant (>99%) clustering in soft/XID:– In whole sky
• No clustering in hard/ultrahard: because not enough sources?• No clustering in hard-spectrum sources
Angular clustering
The XMS samples Barcons et al. 07
Name Band (keV)
Flux limit 10-14 cgs
# sources(unique)
# identified (fraction)
Soft XMS-S
0.5-2 1.5 210 (1) 200 (95%)
Hard XMS-H
2-10 3.3 159 (20) 132 (83%)
XID XMS-X
0.5-4.5 2.0 284 (56) 261 (92%)
Ultrahard XMS-U
4.5-7.5 - 70 (2) 60 (86%)
• Subset of AXIS:– 25 fields chosen for follow-up: 3.3 deg2
– Flux limited in Soft, Hard and XID: total of 318 sources
Optical identification of the XMS
• Optical imaging: g,r,i (SDSS), Z (Gunn), mostly at the INT/WFC to r~23-24mag
• Reliable & unique candidate counterpart in r/i for virtually all sources (< 5” or < 5): only 5 “empties”
• 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, SAO and
others
4m spec lim
10m spec lim
Deep Medium Shallow
Full sample
Breakdown of identified sources
XMS-S Soft
XMS-H Hard
XMS-X XID
XMS-U Ultrahard
Broad-line AGN
75% (148/200)
63% (83/132)
73% (190/261)
65% (39/60)
Narrow-line galaxies (AGN)
13% (27/200)
27%(35/132)
15% (39/261)
27% (16/60)
Absorption line galaxies+clust
4% (8/200)
7% (9/132)
4% (10/261)
5% (3/60)
Stars 8% (15/200)
2% (3/132)
8% (20/261)
0% (0/60)
Redshift distribution
Peak of QSO distribution(z~1.5) well sampled.
Obscured population outto z~1 in Hard sample
Soft
Hard
z
z
#
#
Luminosities and redshifts
Soft
QSO-2 @ z=2.2
QSOs
“Seyferts”
z
z
All galaxiesconsistent with hosting
AGN LX>1042 erg/s:obscured AGN
log
(LS
oft c
gs)
log
(LH
ard
cg
s)
Hard
(Preliminary) X-ray spectral analysis
• Extracted X-ray spectra (pn+MOS) for all 318 sources• Fitted Gal. abs. * power law• Fitted Gal. abs. * Intrinsic abs. * power law • F-test 95%: X-ray absorbed 72 Filled symbols
– 12 BLAGN– 17 NELG– 5 Gal
NH
z
Full sample
16/35 unidentified sources X-ray absorbed
(obscured AGN?)Full sample
(Preliminary) X-ray spectral analysis
• Procedure still being tested• Selecting X-ray spectra with >80cts• Unfolding with best fit Galactic+Intrinsic absorption power law• De-absorbing (correcting for Galactic NH)• De-redshifting• Renormalizing using flux in 2-8 keV band• Averaging in final bins (≥500 cts)• Averaging AXIS:
– BLAGN (200 sources)– NELG (43)
• Much improved averaging AXIS+XMM-2dF:– BLAGN (549): =1.95±0.02 Fe line @6.5±0.2 keV EW=130±60 eV: ~3 – NELG (113): =1.53±0.02 Fe line @6.6±0.4 keV EW=130±100 eV:
<~2
Averaging X-ray spectraCorral et al., in preparation
AXIS+XMM-2dFBLAGN
AXIS+XMM-2dFNELGs
• Procedure still being tested• Selecting X-ray spectra with >80cts• Unfolding with best fit Galactic+Intrinsic absorption power law• De-absorbing (correcting for Galactic NH)• De-redshifting• Renormalizing using flux in 2-8 keV band• Averaging in final bins (≥500 cts)• Averaging AXIS:
– BLAGN (200 sources)– NELG (43)
• Much improved averaging AXIS+XMM-2dF:– BLAGN (549): =1.95±0.02 Fe line @6.5±0.2 keV EW=130±60 eV: ~3 – NELG (113): =1.53±0.02 Fe line @6.6±0.4 keV EW=130±100 eV:
<~2
AXIS+XMM-2dFBLAGN
AXIS+XMM-2dFNELGs
Averaging X-ray spectraCorral et al., in preparation
Tips for statistical identification
~90% Obscured AGN (most Xabs)
90% unobscured AGN
Stars
HR2
log
(FH
ard
/Fop
t)
Full sample
X-ray to optical ratio:
a marker for obscuration?
Soft•5% of sources with FX/Fopt>10•≥40% of FX/Fopt>10 obscured AGN
FX/Fopt >10
Hard
log
(FH
ard
/Fop
t)
•15% of sources with FX/Fopt>10•~70% of FX/Fopt>10 obscured AGN
log
(FS
oft/F
op
t)
FX(10-
14cgs)
FX(10-14cgs)
Optical colours
QSOsS+Irr
E+S0
10% of QSOsare red
QSOsS+Irr
E+S0
HardSoft
r-i
g-r g-r
#
Optical versus X-ray “colours”: Hard
Hard Softer
Harder sources are >90% obscured AGNSofter sources: Optically blue: unabsorbed AGN Optically red: mix of abs & unabs AGN
HR2
g-r
Red
der
• On-going work• Brightest 50% of the X-ray background dominated by
AGN.• 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/Fopt>10 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/i>21.5) and Xabs: NELGs?• Results from average spectra show Fe lines in both
BLAGN and NELGs
Publications
• Carrera et al. 2006 (submitted): X-ray catalogue of AXIS sources– logN-logS– angular correlation– Answer from the referee ~OK: expected re-submission by end
of year
• Corral et al. 2007 (in prep.): spectral stacking analysis of AXIS and XMS sources (+2dF?)
• Barcons et al. ~2007: XMS IDs and col-col plots• Ebrero et al. ~2007: luminosity function• Bussons et al. ~2007: SEDs• ?? et al. ~2007: statistical IDs with 2dF?
Observing proposals
• Submitted:– SAO/6m 6 nights March: XMS/UH mag>21.5– CAHA/3.5m Omega2000: wide-field IR im.– XMM: deep look (200ks) at 4 Compton-thick
candidates
• Planned:– CAHA/3.5m Omega2000: wide-field/QSO2 IR im.– VLT/VIMOS LBQS2212?: MOS spectroscopy