Документ взят из кэша поисковой машины. Адрес оригинального документа : http://xmm.vilspa.esa.es/docs/documents/Appendix/DL/rad_meet.html
Дата изменения: Wed Dec 13 12:22:23 2000
Дата индексирования: Sat Dec 22 14:02:48 2007
Кодировка:

EPIC Background

D Lumb

December 13, 2000

 

Figure 1: Data from selected high latitude pointings overlaid in detector co-ordinates. 132ksec total low proton flare conditions, and bright point sources excised

 

Figure 2: Same data set from selected high latitude pointings but in 0.2-2keV only. Note the effects of remnant bright source excision, and the true X-ray background from faint sources and the Galaxy. Note also the vignetted portion shadowed by the filter wheel in the image corners

 

Figure 3: Same data set from selected high latitude pointings but in 2-10keV only. Note that the background is almost flat - indicating it is dominated by particle-induced background

 

Figure 4: Same data set from selected high latitude pointings but plotted as spectra (PATTERNS==0&&#XMMEA_EP), and normalised for approx 1 arcmin square. Note the Cu K fluorescent lines at 8keV, AL K At 1.5 keV. Also signs of O emission from the soft Galactic component. This spectrum is steeper than presented by Molendi in accompanying presentation

 

Figure: EPIC MOS data set from selected high latitude pointings plotted as spectra (PATTERNS$\leq$12&&#XMMEA_EM), and normalised for approx 1 arcmin square. Note the MOS is not subject to Cu K emission, but there is a Si K fluorescence in addition to the Al K. Also signs of emission lines from the soft Galactic component are more evident than in PN. This spectrum is steeper than presented by Molendi in accompanying presentation

 

Figure 6: PN background data plotted as radial intensity distribution. Although this is not properly exposure corrected the distinct difference between flat 2-10 keV (dotted) and the vignetted 0-2-2keV (solid) data is clearly visible