Tracing cosmic accretion through the XMM-Newton Medium Survey (XMS)
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Transcript of Tracing cosmic accretion through the XMM-Newton Medium Survey (XMS)
Tracing cosmic accretion Tracing cosmic accretion through the through the
XMM-Newton Medium Survey XMM-Newton Medium Survey (XMS)(XMS)
Xavier BarconsXavier Barcons
On behalf of the AXIS/XMS/SSC teamOn behalf of the AXIS/XMS/SSC team
El Escorial The X-ray Universe 2005
IndexIndex
The role of medium sensitivity surveysThe role of medium sensitivity surveys The XMS survey The XMS survey The content of the XMS surveyThe content of the XMS survey Tips for statistical identificationsTips for statistical identifications Outlook and future workOutlook and future work
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The role of Medium SurveysThe role of Medium Surveys
Bridge between most popular Bridge between most popular deep surveysdeep surveys and surveys of the and surveys of the locallocal Universe Universe
The average XMM-Newton observation (10-20 The average XMM-Newton observation (10-20 ks of GTI) is a Medium Sensitivity Survey: ks of GTI) is a Medium Sensitivity Survey: * The 2XMM catalogue will be a huge MSSThe 2XMM catalogue will be a huge MSS
The bulk of the cosmic X-ray background The bulk of the cosmic X-ray background resides at resides at intermediateintermediate X-ray fluxes (~10 X-ray fluxes (~10-14-14 erg erg cmcm-2-2 s s-1-1))
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Relative contribution to XRB per Relative contribution to XRB per flux decadeflux decade
0,0E+00
1,0E-12
2,0E-12
3,0E-12
4,0E-12
5,0E-12
6,0E-12
7,0E-12
1,0E-16 1,0E-15 1,0E-14 1,0E-13 1,0E-12
X-ray flux (cgs)
Fra
ctio
nal
co
ntr
ibu
tio
n t
o X
RB
0.5-2 keV
0.5-4.5 keV
2-10 keV
S dN(S)/d log S
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Fraction of XRB resolved by Fraction of XRB resolved by X-ray surveysX-ray surveys
0
0,1
0,2
0,3
0,4
0,5
0,6
0,7
0,8
0,9
1
1,0E-16 1,0E-15 1,0E-14 1,0E-13 1,0E-12
X-ray flux (cgs)
Fra
ctio
n o
f X
RB
Deep
XMS
BSS
The XMS resolves~50% of the 0.5-4.5 keV
X-ray background
The XMS survey and its optical The XMS survey and its optical identificationidentification
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Definition of the XMS sampleDefinition of the XMS sample 25 XMM-Newton target fields:25 XMM-Newton target fields:
* Galactic latitude |b|>20 degGalactic latitude |b|>20 deg* X-ray observations with EPIC-pn X-ray observations with EPIC-pn
detector in FULL-FRAME-MODEdetector in FULL-FRAME-MODE* ~Avoided fields with bright and/or ~Avoided fields with bright and/or
extended targetsextended targets* Good time intervals > 10 ksecGood time intervals > 10 ksec* Available early on in the missionAvailable early on in the mission
Using SAS v6.1.1 to produce final source Using SAS v6.1.1 to produce final source list and products: list and products: * Exposure and background mapsExposure and background maps* Source detectionSource detection* Spectra and calibration matricesSpectra and calibration matrices
Areas around target + OOT+ near the Areas around target + OOT+ near the pn CCD gaps excludedpn CCD gaps excluded
Own empirical sentitivity maps from Own empirical sentitivity maps from detected source parametersdetected source parameters
284284 sources with 0.5-4.5 keV flux sources with 0.5-4.5 keV flux >2 10>2 10-14 -14 erg cmerg cm-2-2 s s-1-1
Very detailed source screeningVery detailed source screening
NGC4291
Mrk 205
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Statistics of XMS fieldsStatistics of XMS fieldsFieldField GTIGTI ## g’g’ r’r’ i’i’
A1837A1837 4545 99
A399A399 1414 1111
B21028B21028 2323 1111
B21128B21128 1414 1515
Cl0016Cl0016 2929 1414
Cl0939Cl0939 4444 77
Eq PegEq Peg 1212 1414
G133_2G133_2 1818 1111
G133_1G133_1 2020 88
HD1175HD117555
3333 1616
IRAS224IRAS224 2020 1212
LBQS22LBQS2211
9090 1313
UZ LibUZ Lib 2323 77
Mkn205Mkn205 1717 1818
Mkn3Mkn3 2323 1313
MS0737MS0737 2020 1111
MS1229MS1229 2828 99
PB5062PB5062 2828 66
PHL5200PHL5200 4343 1818
PKS2126PKS2126 1616 99
PKS2135PKS2135 2828 1313
S50836S50836 2525 1111
SDS1SDS1 4343 1313
SDS2SDS2 4141 99
SDS3SDS3 1414 66
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Optical identification of XMSOptical identification of XMS
Optical imaging: g’,r’,i’ and more to r’~23-24Optical imaging: g’,r’,i’ and more to r’~23-24magmag
Reliable & unique candidate counterpart in r’/i’ Reliable & unique candidate counterpart in r’/i’ for virtually all sources (< 5” or < 5for virtually all sources (< 5” or < 5))
Optical spectroscopyOptical spectroscopy* 50% from AXIS programme (WHT, TNG, NOT): 50% from AXIS programme (WHT, TNG, NOT):
multi-fibre and long-slit spectroscopymulti-fibre and long-slit spectroscopy* 20% from Calar Alto/3.5m long-slit spectroscopy20% from Calar Alto/3.5m long-slit spectroscopy* 15% from VLT/FORS2 long-slit spectroscopy15% from VLT/FORS2 long-slit spectroscopy* A few from AAT/2dF, SUBARU/FOCAS, and othersA few from AAT/2dF, SUBARU/FOCAS, and others
Preliminary results from 2 XMM-Newton fields Preliminary results from 2 XMM-Newton fields (~30 sources) in Barcons et al (2002)(~30 sources) in Barcons et al (2002)
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XMS Identification statusXMS Identification status
Sources Number % X-ray 284 100 Identified 242 85 Unid R<20 6 2.5 Unid 20<R<21 6 2.5 Unid 21<R<22 4 1.5 Unid R>22 24 8 Empty 2 1 Need imaging 1 0
2525 XMM fields XMM fields XID:0.5-4.5 keVXID:0.5-4.5 keV SSXIDXID>2>21010-14-14cgscgs ΩΩ=3.3 deg=3.3 deg22
The content of the XMSThe content of the XMS
Identification breakdownIdentification breakdown
Remaining incompleteness & biasesRemaining incompleteness & biases
Towards the X-ray luminosity functionTowards the X-ray luminosity function
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Breakdown of identified sources Breakdown of identified sources in the XMSin the XMS
ClassClass NumberNumber %%
Broad-Line Broad-Line AGNAGN
178178 7474
Narrow LineNarrow Line
GalaxiesGalaxies3737 1515
Absorption Absorption Line GalaxiesLine Galaxies
88 44
StarsStars 1818 77BL LacBL Lac 11 00
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Fluxes and redshiftsFluxes and redshifts
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Incompleteness and remaining Incompleteness and remaining biasesbiases
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Redshift distributionRedshift distribution
0
5
10
15
20
25
30
0 0,2 0,4 0,6 0,8 1 1,2 1,4 1,6 1,8 2 2,2 2,4 2,6 2,8
z
Nu
mb
er ALG
NELG
BLAGN
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QSO-2sQSO-2s
S(0.5-4.5)=1.1 10-13 erg cm-2 s-1
z=0.711LX=1044.4 erg s-1
Absorbed: =0.55
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The L-z plane and the X-ray The L-z plane and the X-ray Luminosity FunctionLuminosity Function
Deep S
urvey
s
Bright S
ourc
e Surv
ey
Unfortunately,photo-z’s do notwork with our limited colourinformation
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Source countsSource counts
Sb=1.69+0.02-0.0110-14 cgs
Γu=2.55+0.03-0.04
Γd=1.34+0.01-
0.07
See poster G.2 for more details
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X-ray spectral properties of AGNX-ray spectral properties of AGN
Spectra of individual Spectra of individual sources well matched to sources well matched to unified model, but with unified model, but with exceptions (Mateos et al exceptions (Mateos et al 2005)2005)
X-ray spectral templates: X-ray spectral templates: de-redshifted average de-redshifted average spectra (see poster E.11 spectra (see poster E.11 by Corral et al)by Corral et al)
?
?
Tips on statistical identificationTips on statistical identification
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Statistical identificationStatistical identification
Probabilistic classification of X-ray sources, Probabilistic classification of X-ray sources, based on:based on:* X-ray colours X-ray colours * Optical colours Optical colours * X-ray to optical flux ratiosX-ray to optical flux ratios* X-ray and/or optical morphologyX-ray and/or optical morphology
Large parameter space: start with “preliminary Large parameter space: start with “preliminary inspection” (fishing expedition), later apply inspection” (fishing expedition), later apply mathematical tools (PCA, ANNs, etc.)mathematical tools (PCA, ANNs, etc.)
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HR2=(H-S)/(H+S)H=2.0-4.5 keVS=0.5-2.0 keV
100%
Sta
rs
>75%
ALG
100% NELG>80% NELG
>60% NELG>50% NELG
>85% BLAGN
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Optical colour-colour Optical colour-colour diagramsdiagrams
-1
-0,5
0
0,5
1
1,5
2
2,5
-1 -0,5 0 0,5 1 1,5 2 2,5
g'-r'
r'-i
'
BLAGNNELGGalStarNoid
SDSSQSOs
SDSSEarly-type galaxies
50% NELGs50% “red” BLAGNs
95% BLAGNs
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Optical vs X-ray colours Optical vs X-ray colours
-1
-0,5
0
0,5
1
1,5
2
2,5
-1,2 -1 -0,8 -0,6 -0,4 -0,2 0 0,2 0,4
HR2
g'-
r'
BLAGN
NELG
Gal
Star
Noid
Red & SoftALG
Red & HardNELGs
BlueBLAGN
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Obscuration/reddeningObscuration/reddening
-2
-1,5
-1
-0,5
0
0,5
1
1,5
2
-1 -0,5 0 0,5 1 1,5 2 2,5
g'-r'
log
(fX
/fo
pt) BLAGN
NELGGalStarNoid
-2
-1,5
-1
-0,5
0
0,5
1
1,5
2
-1 -0,5 0 0,5 1 1,5 2 2,5
r'-i'
log
(fX
/fo
pt) BLAGN
NELGGalStarNoid
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Obscuration/reddeningObscuration/reddening
-2
-1,5
-1
-0,5
0
0,5
1
1,5
2
-1 -0,5 0 0,5 1 1,5 2 2,5
r'-i'
log
(fX
/fo
pt) BLAGN
NELGGalStarNoid
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Tips for statistical identificationsTips for statistical identifications
Sources with log (fSources with log (fXX/f/foptopt)<-1.5 are invariably )<-1.5 are invariably starsstars
Optically blue objects are 95% BLAGNOptically blue objects are 95% BLAGN Optically red objects include both broad-line Optically red objects include both broad-line
and narrow line AGNand narrow line AGN Red & soft galaxies do not have emission linesRed & soft galaxies do not have emission lines Red & hard galaxies have narrow emission Red & hard galaxies have narrow emission
lineslines There is a large patch of parameter space There is a large patch of parameter space
shared by both broad and narrow line AGN.shared by both broad and narrow line AGN.
El Escorial The X-ray Universe 2005
Outlook and future workOutlook and future work
Spectroscopic identification of remaining 15% Spectroscopic identification of remaining 15% objects needed (photo-z’s do not work)objects needed (photo-z’s do not work)
Combine with Bright and Deep Surveys to Combine with Bright and Deep Surveys to compute AGN X-ray luminosity function and compute AGN X-ray luminosity function and evolutionevolution
Compute Accretion power as a function of z, Compute Accretion power as a function of z, both for absorbed and unabsorbed sourcesboth for absorbed and unabsorbed sources
Explore larger sample (XMM/2dF) in the search Explore larger sample (XMM/2dF) in the search for statistical identification handlesfor statistical identification handles
Apply statistical identification to 2XMM Apply statistical identification to 2XMM cataloguecatalogue
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Thanks to:Thanks to:
Francisco CarreraFrancisco Carrera Maite CeballosMaite Ceballos Silvia MateosSilvia Mateos Amalia CorralAmalia Corral Francesca PanessaFrancesca Panessa Jacobo EbreroJacobo Ebrero Mat PageMat Page Axel SchwopeAxel Schwope Mike WatsonMike Watson Roberto Della CecaRoberto Della Ceca Jonathan TeddsJonathan Tedds Tommaso MaccacaroTommaso Maccacaro And many more…And many more…