the xmm-newton survey science centre identifdication (xid) programme xavier barcons instituto de...

The XMM-Newton Survey The XMM-Newton Survey Science Centre Science Centre

identifdication (XID) identifdication (XID) programmeprogramme

Xavier BarconsXavier BarconsInstituto de Física de Cantabria (CSIC-Instituto de Física de Cantabria (CSIC-

UC)UC)

Santander, SpainSantander, Spain

Xavier Barcons, IFCA, Santander, Spain

… … on behalf of the on behalf of the SSCentre XID working SSCentre XID working

groupgroup•Astrophysikalisches Institut Potsdam (Germany): Y. Hashimoto, G. Lamer, G. Szokoly, A. Schwope•Centre d'Etude Spatiale des Rayonnements (France): N. Webb• Institute of Astronomy, Cambridge (UK): R.G. McMahon, W. Yuan, A.C. Fabian, C.S. Crawford • Instituto de Astrofísica de Canarias, Tenerife (Spain):I. Pérez-Fournon • Instituto de Física de Cantabria, Santander (Spain): X. Barcons, F.J. Carrera, M.T. Ceballos, S. Mateos • Subaru Telescope: K. Sekiguchi• Max-Planck-Institut fuer extraterrestriche Physik (Germany): T. Boller, G. Hasinger, W. Pietsch• Mullard Space Science Laboratory, UCL (UK): M.S. Cropper, K.O. Mason, M.J. Page, S. R. Rosen• Observatoire Astr de Strasbourg (France): C. Motch, P. Guillout, L. Mirioni, I. Negueruela, M. Pakull• Osservatorio Astronomico di Brera, Milano (Italy): T. Maccacaro, R. Della Ceca, P. Severgnini • University of Bristol (UK): D.M. Worrall, M. Bremer, M. Birkinshaw • University of Central Lancashire (UK): G.E. Bromage, B.J.M. Hassall• University of Leicester, (UK): M.G. Watson, J.P. Pye, D. Baskill, G.C. Stewart, T.P. Roberts, J.P. Osborne, N. Schurch, P.J. Wheatley, M.J. Ward, R.S. Warwick, J.A. Tedds• XMM Science Operations Centre, (Spain): N. Schartel• Harvard Smithsonian Astrophysical Observatory: M. Elvis


IndexIndex The XID programme: goals and strategyThe XID programme: goals and strategy The imaging programmeThe imaging programme The extragalactic core programme:The extragalactic core programme:

The faint sample (almost nothing to report)The faint sample (almost nothing to report) The medium sampleThe medium sample The bright sample (The bright sample (talk by R. Della Cecatalk by R. Della Ceca))

The Galactic Plane sample (The Galactic Plane sample (poster by C. Motchposter by C. Motch)) Other activitiesOther activities OutlookOutlook


The XMM-Newton The XMM-Newton serendipitous sky surveyserendipitous sky survey

Every new XMM-Newton Every new XMM-Newton pointing discovers ~30-pointing discovers ~30-150 serendipitous X-ray 150 serendipitous X-ray sources.sources.

About 50,000 new X-ray About 50,000 new X-ray sources/yearsources/year

Overall goal: build up a Overall goal: build up a catalogue with catalogue with all all serendipitous X-ray serendipitous X-ray sources and their sources and their likelylikely identificationsidentifications


The XID strategy: The XID strategy: statistical identificationsstatistical identifications

X-ray properties

Optical/IR photometricimaging

+ Probable identification

=

Need a large trainingsample with properspectroscopic id’s:

the core programme


XID programme detailsXID programme details Core programmeCore programme (1000 sources/sample): (1000 sources/sample):

High b High b faint samplefaint sample (~10 (~10-15-15 erg cm erg cm-2-2 s s-1-1) ) High b High b medium samplemedium sample (~10 (~10-14-14 erg cm erg cm-2-2 s s-1-1)) High b High b bright samplebright sample (~10 (~10-13-13 erg cm erg cm-2-2 s s-1-1)) Galactic Plane Sample Galactic Plane Sample (~7 10(~7 10-15-15 erg cm erg cm-2-2 s s-1)-1)

Imaging programmeImaging programme (u,g’,r’,i’,Z,H): a (u,g’,r’,i’,Z,H): a large number of XMM-Newton observationslarge number of XMM-Newton observations


XID ground-based XID ground-based resourcesresources

Optical/IR imaging: INT 2.5m with WFC ESO 2.2m with WFI Subaru 8.3m with SuprimeCam & FOCAS

Optical spectroscopy WHT 4.2m with ISIS WHT 4.2m with WYFFOS/AUTOFIB2 TNG 3.5m with DOLORES NOT 2.5m with ALFOSC Subaru 8.3m with FOCAS


XID observational strategyXID observational strategy

sample sourcesdeg-2

imaging Spectroscopy

Bright 10 DSS 2m longslitMed &Gal

100 2m 4m fibres &longslit

Faint 1000 4m 8m multiobj


AXIS: An XMM-Newton International AXIS: An XMM-Newton International SurveySurvey

International Time Project (ITP) International Time Project (ITP) approved by the approved by the Comité Científico Comité Científico InternacionalInternacional for years 2000 and 2001: for years 2000 and 2001: total of 85 nights spread in 4 telescopestotal of 85 nights spread in 4 telescopes

Major boost to XID programme in:Major boost to XID programme in: Imaging programmeImaging programme High galactic latitude medium sampleHigh galactic latitude medium sample High galactic latitude bright sampleHigh galactic latitude bright sample Galactic Plane surveyGalactic Plane survey


Imaging programmeImaging programme

u B g’ V R r’ I i’ Z H H Total38 12 64 21 37 81 23 70 60 9 16 107

Optical: INT2.5m/WFC + ESO2.2m/WFI

Near IR: INT2.5m/CIRSI

XMM-Newton imaged fields in various filtersLast Updated: 28 October 2001


Depth of imagesDepth of images

SDSS

GalaxiesStars


Seeing distributionSeeing distribution


Astrometric calibrationAstrometric calibration

100-200 APM or 100-200 APM or USNO stars per USNO stars per CCD; each of 4 CCD CCD; each of 4 CCD chips is fit chips is fit independentlyindependently

Median rms 0.25”;Median rms 0.25”; believed due to believed due to internal errors in internal errors in external catalogue external catalogue and proper and proper motionsmotions

Chip-4


Automated Photometric Automated Photometric calibrationcalibration

The majority of the images have photometric calibration error < 0.1 mag

Currently exploring systematics due to variations in zero-point and extinction constants


Public release of XID Public release of XID optical imagesoptical images

Fully-reduced CCD mosaics covering Fully-reduced CCD mosaics covering almost entire EPIC FOV in various almost entire EPIC FOV in various filtersfilters

Astrometrically and photometrically Astrometrically and photometrically calibrated images and optical source calibrated images and optical source cataloguescatalogues

Release of optical images Release of optical images corresponding to public XMM-Newton corresponding to public XMM-Newton datadata

Release by end of January 2002


Spectroscopic Spectroscopic identificationsidentifications

Search for candidate counterpartsi’-band sources within either:

5 (statistical) or5 arcsec

Bright Sample: >95% success with 1 single candidateMedium Sample: 90% success, 3/4 with single candidateGalactic Plane:

•|b|~10-20º, 85% success, 1/2 with single candidate•|b|~0-10º, very large star density: no unique candidate


High-b identificationsHigh-b identifications0.5-4.5 keV

0.0001

0.0010

0.0100

0.1000

1.0000

10.0000

100.0000

0.001 0.01 0.1 1 10z

Lo

g L

44

BLAGN (119)BLLAC (2)Gal (15)NELG (23)

119 BLAGN

23 NELG

15 Galaxies

2 BLLAC

41 Stars


The high-b medium The high-b medium samplesample

Flux limit 2Flux limit 21010-14-14 erg cm erg cm-2-2 s s-1 -1 (0.5-4.5 KeV)(0.5-4.5 KeV) Source density ~110 sources degSource density ~110 sources deg-2-2

30 fields in the North: 498 X-ray sources30 fields in the North: 498 X-ray sources 122 identifications (25%)122 identifications (25%)

By ~March 2002, expect a sample of 15 By ~March 2002, expect a sample of 15 fields (212 X-ray sources) identified to ~90% fields (212 X-ray sources) identified to ~90%

~a few % of X-ray sources do not show ~a few % of X-ray sources do not show opticaloptical counterpart within ~22.5 counterpart within ~22.5magmag


Medium Sample: Medium Sample: preliminary resultspreliminary results

2 fields (Mkn205 and G133-69 Pos_2), 2 fields (Mkn205 and G133-69 Pos_2), 29 X-ray sources over 0.26 deg29 X-ray sources over 0.26 deg-2-2:: 19 Broad Line AGN (incl 2 BAL QSOs)19 Broad Line AGN (incl 2 BAL QSOs) 6 Narrow-Line AGN6 Narrow-Line AGN 1 Abs line Galaxy (NGC 4291)1 Abs line Galaxy (NGC 4291) 1 Active Coronal Star1 Active Coronal Star 2 Unidentified (1 unobserved, 1 very faint)2 Unidentified (1 unobserved, 1 very faint)


MS: Hardness ratiosMS: Hardness ratios

HR1= 0.5-2.0 keV 2.0-4.5 keVHR2= 2.0-4.5 keV 4.5-10 keV

Sample <HR1> <HR2>All -0.690.03 -0.370.03BLAGN -0.680.01 -0.310.04NLAGN -0.480.11 -0.370.04

Marginal evidence for NLAGN being absorbed BLAGN

BLAGN have ~2 at 0.5-4.5 keVand ~1.6 at 4.5-10 keV


MS: The X-ray source MS: The X-ray source populationpopulation

ASCA 2-10 keV

ROSAT 0.5-2 keV

14.0

15.0

16.0

17.0

18.0

19.0

20.0

21.0

22.0

23.0

1.0E-14 1.0E-13 1.0E-12X-ray flux (0.5-4.5)

i-m

ag

nit

ud

e

BLAGN

AC

NELG

0.0

0.2

0.4

0.6

0.8

1.0

1.2

1.4

1.6

-0.5 0.0 0.5 1.0 1.5 2.0 2.5g'-r'

r'-i

'

NELG

BLAGN

AC

E/S0 templ

SDSS QSO

Sbc temp


-12.1-12.1109109+48°49+48°49 23h3323h33ZAndZAnd

0.00.020.420.4-11°00-11°0018h2818h28Ridge 4Ridge 4

0.00.020.020.0-11°29-11°2918h2718h27Ridge 3Ridge 3

-0.9-0.921.521.5-10° 34-10° 3418h3318h33G 21.5 -09G 21.5 -09

bbllDecDecRaRaFieldField

+16.7+16.7237237-13°04-13°04 08h3608h36GRB 001025GRB 001025

The Galactic Plane sample

~0.18 deg~0.18 deg229.6 ksec9.6 ksecRidge 3Ridge 3

~ 0.36 deg~ 0.36 deg2230 ksec30 ksecG21.5-09G21.5-09

AreaAreaExposure timeExposure timeFieldField


The Galactic plane at |b|=0º

0011Extragalac. Extragalac. sourcessources

7 (33 %)7 (33 %)57 (74%)57 (74%)UnidentifiedUnidentified

0011Accreting Accreting sourcessources

14 (66%)14 (66%)18 (23%)18 (23%)Stellar Stellar coronaecoronae

21217777Number of Number of sourcessources

Ridge 3Ridge 3G21.5-09G21.5-09FieldField


Me Stars

H flux versus X-ray flux for ROSAT and XMM Me stars

G21.5-09&

Ridge 3

Rosat CygnusRegion(Motch et al. 1997)


The Galactic Plane landscapeThe Galactic Plane landscapeActive coronae exhibit soft X-ray spectra (HR2

< ~ 0)Most soft X-ray sources have active coronae counterpartsThe population of Me stars seen by XMM-Newtin is similar to that detected by ROSAT, just seen farther away….The Me to K-A star ratio is ~ 30%, similar to that of ROSATNo Cataclysmic Variable has been yet detected down to an estimated R magnitude of ~ 19.


The Be accreting binary The Be accreting binary SS397SS397

SS397


SS397: a Be+NS/WD SS397: a Be+NS/WD accreting binary?accreting binary?

Too X-ray luminous to be an isolated Too X-ray luminous to be an isolated Be0.5 star: binaryBe0.5 star: binary

Hard X-ray spectrum (Hard X-ray spectrum (=1.5 or kT= 9 =1.5 or kT= 9 keV)keV)

LLXX~10~103232 erg s erg s-1-1, very low for a NS , very low for a NS accreting binaryaccreting binary

A very good candidate to Be+WD A very good candidate to Be+WD binarybinary


Other on-going or planned Other on-going or planned XID activitiesXID activities

Pilot cluster surveyPilot cluster survey Pilot hard X-ray source surveyPilot hard X-ray source survey EPIC astrometry studies (poster by EPIC astrometry studies (poster by

J. Tedds & Mike Watson)J. Tedds & Mike Watson) X-ray spectral templates / X-ray X-ray spectral templates / X-ray

colours of various populationscolours of various populations Bi-variate flux distributionsBi-variate flux distributions


Special thanks to...Special thanks to... Mike Watson, Jonathan Tedds: Mike Watson, Jonathan Tedds: X-ray sources, overall X-ray sources, overall

managingmanaging Mat Page: Mat Page: Fibre spectroscopyFibre spectroscopy Francisco Carrera: Francisco Carrera: AXIS programme and much moreAXIS programme and much more Richard McMahon: Richard McMahon: Imaging programmeImaging programme Christian Motch: Christian Motch: Galactic plane surveyGalactic plane survey Axel Schwope: Axel Schwope: Southern observationsSouthern observations Tommaso Maccacaro, Roberto Della Ceca: Tommaso Maccacaro, Roberto Della Ceca: Bright Bright

samplesample

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