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


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))


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


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


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


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


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)


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


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


Fluxes and redshiftsFluxes and redshifts


Incompleteness and remaining Incompleteness and remaining biasesbiases


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


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


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


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


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


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.)


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


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


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


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


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


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.


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


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…

tracing cosmic accretion through the xmm-newton medium survey (xms)

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