XMM-Newton XMM-LSS  

Index - ... - The survey characteristics - Scientific Goals - Simulations (1/3) - ...

3. Scientific Goals

The unrivaled sensitivity and good point-spread function of XMM will open a new era for X-ray large-scale structure studies.

Some 1000 times more sensitive than the REFLEX survey - the largest cluster survey over a single area to date (Böhringer et al 2001) - the XMM-LSS survey is designed to probe the large scale distribution of clusters of galaxies out to z ~ 1 and of QSOs much further out. This will provide unprecedented insight onto LSS formation and, thus, cosmology. We will be able to probe the nature and amount of dark matter, the initial fluctuation spectrum and other fundamental cosmological parameters.

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Constraints upon the cosmological parameters m and 8 (the amplitude of mass fluctuations on 8 h-1 Mpc scale) for a CDM universe. Cluster abundance data provides strong constraints upon the m - 8 combination. Constraints upon the cosmological parameters m and (the shape of the power spectrum) for a CDM universe. The correlation function is a powerful tool to constrain the shape of the initial spectrum.
Solid lines: XMM-LSS cluster counts - Dashed lines: correlation function.
In each case, the 68%, 90% and 95% confidence level contours are shown along with the assumed model (cross).
These calculations have been performed assuming that only the redshifts over the [0<z<1] x [64 deg2] volume are available. (Predictions from Refregier et al., 2001.)

In addition, identification of a "Coma-type" cluster within the XMM-LSS over the redshift range 1.5 < z < 2 has a probability of ~ 6.5 10-7 in the current CDM scenario. Therefore, any such discoveries in the  survey would put the currently favoured cosmological model in great observational difficulty.

The primary science goals are:

Index - ... - The survey characteristics - Scientific Goals - Simulations (1/3) - ...
Web Pages : Alain Detal, Oct 2001.