An XMM-Newton An XMM-Newton International Survey International Survey

(AXIS): (AXIS): A progress reportA progress report

Xavier Barcons & Francisco CarreraXavier Barcons & Francisco Carrera

Instituto de Física de Cantabria Instituto de Física de Cantabria (CSIC-UC)(CSIC-UC)

on behalf of the AXIS consortium and the on behalf of the AXIS consortium and the

XMM Survey Science Centre XID wgXMM Survey Science Centre XID wg

The AXIS teamThe AXIS teamhttp://www.ifca.unican.es/~xray/AXIhttp://www.ifca.unican.es/~xray/AXI

SS

•Astrophysikalisches Institut Potsdam (Germany): Y. Hashimoto, G. Hasinger, G. Lamer, G. Szokoly, A. Schwope•Centre d'Etude Spatiale des Rayonnements (France): N. Webb• Institute of Astronomy, Cambridge (UK): R.G. McMahon, 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 • Laboratorio de Astrofísica Espacial y Física Fundamental, Madrid (Spain): J.M. Mas-Hesse• Max-Planck-Institut fuer extraterrestriche Physik (Germany): T. Boller • Mullard Space Science Laboratory, UCL (UK): M.S. Cropper, K.O. Mason, J.P.D. Mittaz, M.J. Page, S. R. Rosen• Observatoire Astronomique de Strasbourg (France): C. Motch, P. Guillout, L. Mirioni, I. Negueruela• 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, G.C. Stewart, T. Roberts, J.P. Osborne, N. Schurch, P.J. Wheatley, M.J. Ward, R.S. Warwick • XMM Science Operations Centre, (Spain): N. Schartel

The XMM Survey Science The XMM Survey Science Centre XID programmeCentre XID programme

Expect 50,000 new X-ray sources/yearExpect 50,000 new X-ray sources/year 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 SampleGalactic Plane Sample

Imaging programmeImaging programme (u,g’,r’,i’,Z,H) (u,g’,r’,i’,Z,H) Statistical identificationsStatistical identifications based on X-ray based on X-ray

properties & imaging programme.properties & imaging programme.

The Observatorio del The Observatorio del Roque de los MuchachosRoque de los Muchachos

JKT (1.0)

GTC (10)

TNG (3.5)

INT (2.5) WHT (4.2)

NOT (2.5)

AXIS:Breakdown of AXIS:Breakdown of observing nightsobserving nights

Telescope 2000 2001 TotalINT (2.5m) 10 8 18WHT (4.2m) 9 14 23TNG (3.5m) 7 14 21NOT(2.5m) 9 16 25Total 35 52 87Fraction 40% 60% 100%

We are here now!

AXIS instruments usedAXIS instruments used

Telescope Instrument CommentsINT 2.5m WFC WF optical imaging

CIRSI WF NIR imaging (H)WHT 4.2m WYFFOS Fibre (2.7”) spectroscopy

ISIS Long-slit spectroscopyNOT 2.5m ALFOSC Long-slit spectroscopyTNG 3.5m OIG Optical imaging

DOLORES Long-slit spectroscopy

AXIS wide-field imagingAXIS wide-field imaging

U(RGO)

g’(SDSS)

r’(SDSS)

i’(SDSS)

Z(Gunn)

H H Total

20 53 58 52 48 14 4 71

Optical: INT/WFCNear IR: INT/CIRSI

(includes M. Watson’s PATT Imaging proposal)

AXIS: Search for candidate AXIS: Search for candidate counterpartscounterparts

# counterparts 0 1 >1 TotalMed Sample field 2(10%) 18(78%) 3(12%) 23Galactic field 10(12%) 34(42%) 37(46%) 81

i’-band sources within either:5 (statistical) or5 arcsec

Clusters?Reddened sources?

AGNs beyond the Galaxy?

Candidate counterparts &Candidate counterparts &systematicssystematics

•Count rate > 0.005 ct s-1

•|b|>10º•Single candidate counterpart•108 sources66%

x1=2, 33%

P(x|x0)=|x-x0|*exp(-|x-x0|2/2)

Pobs(x)=f0*P(x|0)+f1*P(x|x1)

f0=0.67; x0=0 (fixed) f1=0.33; x1=2.0

AXIS identificationsAXIS identifications(as of March 1, 2001)(as of March 1, 2001)

Sources |b|>20 |b|<20 TotalBLAGN 55 5 60Act Coronae 10 14 24Stars 10 11 21NELGs 9 2 11Galaxies 11 - 11Acc binaries - 1 1Total 95 33 128

The AXIS medium sampleThe AXIS medium sample

35 sources brighter than 2 1035 sources brighter than 2 10-14-14 erg cm erg cm-2-2 s s-1 -1 in in the 0.5-4.5 keV band (2 XMM fields, the 0.5-4.5 keV band (2 XMM fields, excluding targets).excluding targets).

32/35 identified (>90%); remaining 3 have 32/35 identified (>90%); remaining 3 have i’>22.5i’>22.5

BLAGN 22 63%NELG 7 20%Gal 2 6%

AC 1 3%

Faint 3 8%

Medium sample: offsetsMedium sample: offsets

Medium sample: L-zMedium sample: L-z

Medium sample: z Medium sample: z distributiondistribution

0123456789

0.5

1.5

2.5

Redshift#

GalNELGBLAGN

Most objects at z~1-2 as expected from XRB

synthesis models

Medium sample: Medium sample: type 1 vs type 2 AGNtype 1 vs type 2 AGN

Expect ~60% of Expect ~60% of AGN to be AGN to be unabsorbed in the unabsorbed in the Comastri et al XRB Comastri et al XRB model model

We find 22/34 (65%) We find 22/34 (65%) BLAGN among the BLAGN among the extragalactic extragalactic sourcessources

Medium Sample: BAL Medium Sample: BAL QSOsQSOs

BAL QSOs in previous X-ray surveys:BAL QSOs in previous X-ray surveys:– 1 in Chandra deep survey (Giacconi et al 2001)1 in Chandra deep survey (Giacconi et al 2001)– 1 in hard X-ray selected ROSAT sample (Page et al 2001)1 in hard X-ray selected ROSAT sample (Page et al 2001)

– 1 in ISO/BeppoSAX survey (Alexander et al 2001)1 in ISO/BeppoSAX survey (Alexander et al 2001) In the medium sample we have 1 confirmed In the medium sample we have 1 confirmed

and 2 highly suggestive BAL QSOs (~5-10% and 2 highly suggestive BAL QSOs (~5-10% of BLAGN):of BLAGN):– Higher sensitivity of XMM-NewtonHigher sensitivity of XMM-Newton– Harder photon energies (even @ 4.5 keV)Harder photon energies (even @ 4.5 keV)

Medium sample: Medium sample: BAL QSO spectraBAL QSO spectra

Z=1.82

z=1.91

z=0.79?z=1.82

AXIS Galactic Plane AXIS Galactic Plane sample: sample:

the G21.5-09 field (b=-1º)the G21.5-09 field (b=-1º)

SS279

A Be+NS/WD? accreting A Be+NS/WD? accreting binarybinary

AXIS Galactic Plane AXIS Galactic Plane sample: sample:

Active CoronaeActive Coronae

Higher sensitivity highlights AC with very weak e.l.s

AXIS expectationsAXIS expectationsGoal AXIS-I AXIS-I + AXIS-IIIP (optical) 75 fields ~100 fieldsIP (infrared) 4 fields ~50 fieldsMS 100 sources 500 sourcesGP 50 sources 300 sourcesBS 50 sources 200 sources

We are here now!

ConclusionsConclusions Sensitivity & response to hard X-rays of XMM-Sensitivity & response to hard X-rays of XMM-

Newton make it sensitive to new classes of Newton make it sensitive to new classes of objectsobjects

Medium sample (> 2 10Medium sample (> 2 10-14-14 erg cm erg cm-2-2 s s-1-1): ): – 68% of sources are BLAGNs (consistency with unified XRB 68% of sources are BLAGNs (consistency with unified XRB

models)models)– z-distribution peaks at z~1-2z-distribution peaks at z~1-2– 5-10% of BLAGNS are BALs5-10% of BLAGNS are BALs

Galactic Plane:Galactic Plane:– Active Coronae with very weak emission linesActive Coronae with very weak emission lines– Accreting binariesAccreting binaries