Astrometry and EPIC flux cross-calibration in 2XMMp/2XMM

1. Astrometry and EPIC flux cross-calibration in 2XMMp/2XMM Silvia Mateos R. Saxton, S. Sembay and the XMM-Newton Survey Science Centre

2. SDSS-DR5 spectroscopic BLAGN sample (~600 objects) 2XMMp astrometry syserr=0.3 blue & stellar fx/fopt> -1 SDSS-DR5 statistically identified BLAGN syserr=0.3

3. 2XMMp (and 2XMM) ECFs obtained with • spectral model : =1.7 & NH=3x1020 cm-2 • One set of M1/M2 rmfs (from rev 534) • Selected good quality sources • >250 cts per camera and energy bad • (avoid Eddington bias) • fluxes<6x10-12 erg cm-2 s-1 per camera and energy band • (avoid pile up effects) Statistical evaluation of 2XMMp/2XMM fluxes • Evaluation of EPIC flux cross-calibration from observed • distributions of flux differences (normalised) between cameras • for each energy band • different M1 off-axis angle • revolution (time dependence)

4. M2-M1 E1 E2 E4 E3

5. M2-M1 E5 Flux calibration differences between M1 and M2 cameras <5% level in all energy bands

6. pn-M1 E2 E1 E3 E4

7. pn-M1 E5 pn-MOS flux differences ≤10% for energy bands 1-4 and ≤15% for energy band 5

8. on-axis: <5 arcmin (~M1 central chip)off-axis: >5 arcmin pn-M1 M2-M1

9. pn-M1 M2-M1

10. Time dependence of 2XMMp/2XMM flux cross-calibration pn-M1 M2-M1 29-250 250-750 >750 29-250 250-750 >750 Small dependence with time of EPIC flux cross-calibration Largest differences observed for M2-M1 energy band 1 (0.2-0.5 keV)

11. Summary • Statistical analysis of EPIC flux cross-calibration in agreement with results from bright calibration objects • M2-M1 flux differences ≤5% for all energy bands • pn-MOS differences ≤10% for energy bands 1-4 and ≤15% for energy band 5 (4.5-12 keV) • See dependence of EPIC flux cross-calibration with off-axis sources • Small time dependence of EPIC flux cross-calibration • except for M2-M1 energy band 1

14. pn-M1

15. pn-M1