XMM-Newton Users Handbook

List of Tables

• 1. XMM-Newton characteristics - an overview
• 2. The on-axis in orbit and on ground 1.5 keV PSFs of the different X-ray telescopes
• 3. Basic numbers for the science modes of EPIC
• 4. Detection limits (i.e., minimum detectable flux at 4$\sigma$ in units of $10^{-15}$ erg cm$^{-2}$ s$^{-1}$) for different energy bands in the 1.16 Ms observation of the Lockman Hole (Hasinger et al., 2001, A&A 365, L45; Brunner et al. 2008, A&A, 479, 283).
• 5. The effect of pile-up on spectral fits
• 6. EPIC Out-of-Time (OoT) events. The percentage of OoT events is given by the mode dependent ratio of readout time and integration time
• 7. List of EPIC event patterns
• 8. RGS In-orbit Performance
• 9. Wavelength and energy ranges covered by the chips of RGS1 and RGS2 for an on-axis source in first order. Due to the scattering, the chip boundaries do not cause sharp features in the effective area. Values in brackets correspond to the non-operational chains.
• 10. Wavelength ranges covered by the RGS in different grating orders
• 11. Flux per CCD$^1$ for a $<$ 2% pile-up for point sources in Spectroscopy mode and using 8 CCDs$^2$
• 12. RGS science data acquisition modes
• 13. RGS1 detector defects and corresponding wavelengths for on-axis sources.
• 14. RGS2 detector defects and corresponding wavelengths for on-axis sources. Since the introduction of single-node operations, the node boundary that applies between the two nodes of the RGS1 CCDs is no longer relevant in RGS2.
• 15. OM characteristics - an overview
• 16. OM optical elements
• 17. OM filters: effective wavelengths, widths and Zeropoints
• 18. OM UV grism sensitivity [detected flux: erg cm$^{-2}$ s$^{-1}$ Å$^{-1}$ ] for different detection levels. The Visible grism is one order of magnitude more sensitive than the UV one.
• 19. OM on-board PSF FWHM in different lenticular filters
• 20. OM count rates [$10^{-4}$ counts s$^{-1}$ ] as function of spectral type for stars with $m_V~=~20$ mag under the assumption of a detector with zero deadtime, no coincidence loss and no time sensitivity degradation.
• 21. OM coincidence loss corrections for high count rates.
• 22. Limiting magnitudes$^1$ for a 5-$\sigma$ detection in 1000 s
• 23. Observed limiting magnitudes$^1$ for a 5-sigma detection (scaled to 1000s)
• 24. Levels of different OM background contributors
• 25. The $m_V$ brightness limits for all OM filters. An A0 type star spectrum is assumed.
• 26. The science data acquisition modes of OM
• 27. OM exposure time constraints
• 28. Comparison of XMM-Newton with other X-ray satellites
• 29. Evolution of Orbital Parameters of XMM-Newton