Figure 3: A compendium of hard x-ray surveys. This class needs specific XMM pointings (about 100-400 ks), which will
have to be made for the purpose of deep surveys.
In the XMM PV-Cal and GT programme, a few groups have already put in deep pointings
fulfilling this purpose (e.g. Giacconi deep field, MSSL field,
Lockman Hole).
At least in part the Subaru deep survey (which will be
carried out in GT for the SSC) will fulfill some of the goals,
although the average XMM exposure time of 50 ks per field will not be
sensitive enough.
To fight source confusion teaming up with Chandra
deep surveys is a good strategy, which has already partially happened
since two of the XMM deep fields (Giacconi field and Lockman Hole)
will also be observed with Chandra.
The optical follow-up of the
deep XMM fields definitely needs 8m-class telescopes and the
respective teams to have access to these (e.g. Keck, VLT, Gemini, Subaru,
later LBT, GTC).
Figure 3: A compendium of hard x-ray surveys.
Last modified 26th August 1999
Text based on AXIS proposal by X.Barcons and the SSC consortium.
Page designed by J.Verdon
www_astro@mssl.ucl.ac.uk