XMM-Newton

1

M.Stuhlinger, March 2010

Status of XMM-Newton

cross-calibration using SASv10.0

Madrid, 24. March 2010

XMM-Newton

2

M.Stuhlinger, March 2010

Example: 1H0414+009

SW modeswithout pile-up.

Absorbed single power law model.

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.

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

XMM-Newton

5

M.Stuhlinger, March 2010

M. Stuhlinger

Statistical evaluation: Flux distributions

XMM-Newton

6

M.Stuhlinger, March 2010

Statistical evaluation: Time evolution

XMM-Newton

7

M.Stuhlinger, March 2010

Statistical evaluation: Flux distribution 2XMM

MOS1/pn MOS2/pn

Matteo Guainazzi

XMM-Newton

8

M.Stuhlinger, March 2010

Statistical evaluation: Time evolution 2XMM

Matteo Guainazzi

MOS1/pn MOS2/pn

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.