1. XMM-Newton 1 M.Stuhlinger, March 2010 Status of XMM-Newton cross-calibration using SASv10.0 Madrid, 24. March 2010

2. XMM-Newton 2 M.Stuhlinger, March 2010 Example: 1H0414+009 SW modes without pile-up. Absorbed single power law model.

3. XMM-Newton 3 M.Stuhlinger, March 2010 Examples: Recent observations SW modes with pile-up. PKS2155-304: Absorbed broken power law model. 3C273: Absorbed double power law model.

4. XMM-Newton 4 M.Stuhlinger, March 2010 Example: Galaxy clusters FF modes. Absorbed plasma model (mekal). A2029:kT ~ 7.2 keV A262: kT ~ 2.2 keV

5. XMM-Newton 5 M.Stuhlinger, March 2010 M. Stuhlinger Statistical evaluation: Flux distributions

6. XMM-Newton 6 M.Stuhlinger, March 2010 Statistical evaluation: Time evolution

7. XMM-Newton 7 M.Stuhlinger, March 2010 Statistical evaluation: Flux distribution 2XMM MOS1/pnMOS2/pn Matteo Guainazzi

8. XMM-Newton 8 M.Stuhlinger, March 2010 Statistical evaluation: Time evolution 2XMM Matteo Guainazzi MOS1/pnMOS2/pn

9. XMM-Newton 9 M.Stuhlinger, March 2010 Summary Statistical analyses of XCAL archive (dominated by piled-up SW observations) and 2XMM sample (285 pile-up free FF observations) are consistent. Significant spread between single observations in nearly all energy bands, both for fluxes and slopes. EPICs show only weak flux time evolution for higher energies (>0.85 keV), some evolution is seen at lower energies (<0.85 keV). RGS and EPIC fluxes diverge with time at low energies. Nearly no time evolution of EPIC/RGS slopes in any of the energy bands.