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Bruno Altieri ESAC, 18.05.2005

Status of the XMM- Newton Cross-calibration. EPIC-MOSs. EPIC-pn. RGSs. OM. Bruno Altieri ESAC, 18.05.2005. Talk outline. Improvement from SAS-6.0 to SAS-6.1 Response stability at low energies : EPIC-pn stability MOS low-energy patch New EPIC rmf’s Major improvement with new MOS rmf

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Bruno Altieri ESAC, 18.05.2005

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  1. Status of the XMM-Newton Cross-calibration EPIC-MOSs EPIC-pn RGSs OM Bruno Altieri ESAC, 18.05.2005

  2. Talk outline • Improvement from SAS-6.0 to SAS-6.1 • Response stability at low energies : • EPIC-pn stability • MOS low-energy patch • New EPIC rmf’s • Major improvement with new MOS rmf • Qualitative improvement with pn rmf tuning • Status of cross-calibration with latest rmf’s •  Need of RGS effective area change • Chandra/Newton cross-calibration • Other cross-calibration problems: • EPIC high-energy discrepancy • Final tuning of MOS & pn redistribution • Conclusions

  3. SAS6.1 : effect of new pn RMF (1) SAS 6.0 SAS 6.1 H1426+428, rev278, single MOS/OM power-law model

  4. SAS-6.1 : effect of new pn RMF (2) M.Kirsch M.Kirsch SAS-6.0 SAS-6.1 • Same 0.5 keV non-physical dip of pn residuals • combined fit is possibly the “truth” ? PKS 2155-504, rev 545

  5. EPIC-pn flux stability: RXJ1856 • Flux deviate by less than 1% F. Haberl

  6. EPIC flux stability: SNR • N132D 0.4-0.8 keV band: • EPIC-pn: • pn flux is stable • pn-LW lower fluxes than pn-SW due to pile-up • MOSs : • MOS1 lower than MOS2 by 5% • Both MOSs have decreased by ~10% since launch M.P. Esquej

  7. MOS rmf change: N132D MOS1 MOS2 • Some changes at low energies (0.5-1keV) at ~5-10% level. • spatial dependent • time dependent • Rev771 vs 83: • flux decrease in 0.5-1 keV • Redistributed below 0.4 keV

  8. cooling Flux stability: The AGN view Sample of AGNs mostly in SW/Medium analysed in 15-40 arcsec annulus used, hence excluding the “MOS patch.” • Low-energy problem : • MOSs & RGSs loose flux relative to pn at the same rate : 8% in 800 revs (I) because of : • MOS on-axis redistribution ? • RGS ?? • contamination of MOSs and RGSs, cooler CCDs than pn. S. Sembay

  9. MOS low-energy on-axis patch

  10. Taking care of MOS patch effect A major improvement ! S. Sembay

  11. But strange pn residuals at low-energy

  12. New pn rmf tuning SAS 6.5 SAS 6.1 Flat residuals

  13. Single powerlaw residuals SAS 6.5 SAS 6.1 Statistics now dominated by residual edges !

  14. Latest EPIC rmf

  15. Latest EPIC rmf

  16. RGS versus EPICs

  17. Full XMM cross-calibration

  18. EPIC high-E discrepancy • MOSs return higher fluxes than pn above 3 keV • F5-10 keV (MOS) higher than F5-10 keV(pn) by 10-15% • MOS1 > MOS2 > pn • MOS (MOS1) finds always • Harder spectra (AGNs) • Hotter temperature (galaxy clusters)

  19. Newton/Chandra cross-cal.: PKS2155 Rev 362 Rev 545 • LETG agrees very well with MOSs • pn low-energy excess higher in rev.545 Model: wabs*bknpower Best fit: MOSs

  20. Newton/Chandra cross-cal.: 3C273 (1) Rev.277

  21. Newton/Chandra cross-cal.: 3C273 (2) Rev.655 EPIC-pn excess also higher with time MOS/LETG agreement excellent.

  22. Conclusion • EPIC are reconciled • Long-standing pn/MOS excess finally solved • CCF for pn already available • time- and spatial- dependent MOS redistribution requires s/w and CCF change, to be implemented in SAS 6.5 • RGS effective area to be corrected with new CCF • Open issues • Decrease of flux/sensitivity of RGS vs EPIC pn at low-energies, still to be quantified, contamination ? • MOS / pn excess at high energies. • Shape of EPIC rmf’s at low energies

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