Next: 1 Glossary
Up: XMM-Newton UHB
Previous: List of Figures
- 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 in units of erg cm s)
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
- 10. Wavelength ranges covered by the RGS in different grating orders
- 11. RGS 2% pile-up flux limits per CCD for point sources in
Spectroscopy mode and using 8 CCDs
- 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 s Å ]
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 [ counts s ]
as function of spectral
type for stars with mag under the assumption of a detector with
zero deadtime, no coincidence loss and no time sensitivity degradation.
- 21. Limiting magnitudes for a 5- detection in 1000 s
- 22. Observed limiting magnitudes for a 5-sigma detection
(scaled to 1000s)
- 23. Levels of different OM background contributors
- 24. The brightness limits for all OM filters.
An A0 type star spectrum is assumed.
- 25. The science data acquisition modes of OM
- 26. OM exposure time constraints
- 27. Comparison of XMM-Newton with other X-ray satellites
- 28. Evolution of Orbital Parameters of XMM-Newton
European Space Agency - XMM-Newton Science Operations Centre