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XID ProgrammeXID Programme

Imaging Programme: multiband Imaging Programme: multiband optical/NIR imaging of XMM fieldsoptical/NIR imaging of XMM fields

Core programme: spectroscopic/archival Core programme: spectroscopic/archival identification ofidentification of 1000 high b sources 0.5-4 keV > 101000 high b sources 0.5-4 keV > 10-13-13 erg cm erg cm-2-2 s s-1-1

1000 high b sources 0.5-4 keV > 101000 high b sources 0.5-4 keV > 10-14-14 erg cm erg cm-2-2 s s-1-1

1000 high b sources 0.5-4 keV > 101000 high b sources 0.5-4 keV > 10-15-15 erg cm erg cm-2-2 s s-1-1

1000 low b sources 0.1-10 keV > 101000 low b sources 0.1-10 keV > 10-14-14 erg cm erg cm-2-2 s s-1-1

AXIS highlightsAXIS highlights International Time Programme at International Time Programme at

La Palma: ~90 observing nights La Palma: ~90 observing nights Apr 2000 to Apr 2002Apr 2000 to Apr 2002

~20% of time used~20% of time usedMostly as expected:

Broad line AGN at high bActive Coronae at low b

But also:A BAL QSOA Be+White Dwarf? accreting binarySeveral NELGs

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AXIS wide-field imagingAXIS wide-field imaging

U(RGO)

g’(SDSS)

r’(SDSS)

i’(SDSS)

Z(Gunn)

H H Total

9 35 43 34 35 12 3 53

Optical: INT/WFCNear IR: INT/CIRSI

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AXIS identificationsAXIS identifications(as of December 1, 2000)(as of December 1, 2000)

Sources |b|>20 |b|<20 TotalAGN 19 - 19Act Coronae 4 12 16Nonact Stars 6 - 6NELGs 4 - 4Galaxies 4 - 4Acc binaries - 1 1Total 37 13 50

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Active CoronaeActive Coronae

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More active coronaeMore active coronae

Ca H&K

H

7

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

SS279

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A Be+WD? accretion A Be+WD? accretion binarybinary

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Broad Line AGNs and Broad Line AGNs and QSOsQSOs

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Redshift vs fluxRedshift vs flux

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A BAL QSO at z=1.82A BAL QSO at z=1.82

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Narrow-line X-ray emitting Narrow-line X-ray emitting galaxiesgalaxies

z=0.3

LX~8 1042 erg s-1

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What next?What next?

Another 15-20 optical spectra Another 15-20 optical spectra obtainedobtained

7.5 more spectroscopic nights before 7.5 more spectroscopic nights before end of 2000end of 2000

~100 spectroscopic identifications by the end of the year