Документ взят из кэша поисковой машины. Адрес оригинального документа : http://xmm.vilspa.esa.es/external/xmm_sw_cal/icwg/presentations/WS_CT.pdf Дата изменения: Tue Jun 20 16:46:30 2006 Дата индексирования: Sat Dec 22 14:42:53 2007 Кодировка: Поисковые слова: р п р п р п р п р п р п р п п р п п р п п р п р п п р п р п п р п

Workshop CAL TARGETS - What do we aim for in this session? -Cal targets highly depend on he mission. Some targets can be fine for XMM or Chandra, but RXTE or INTEGRAL can not see them. - Also depend on scientific subjects: imaging, timing, energy range,... - Sources with simple physics, because we have to understand what the sources do. - Clusters of galaxies: extended, illuminate large area of the detector, but show spatial structures with spectral differences. - How to connect low energy targets/missions to high energy ones? Problem of different time scales for exposures, e.g. ksec versus Msec. Simultaneous observations are needed. - How to calibrate the energy scale for higher energies of future gratings? Difficult to find astronomical targets with well defined lines. On-board calibration sources or defined fluorescence lines from detector structure or even moveable metal plates could help, (e.g. see copper line for XMM pn). Source Energy Flux keV HZ 43 < 0.2 Bright Sirius B < 0.2 HZ43 /10 RXJ1856 < 1 Faint Simplicity Var WD WD No No No No Yes Yes Extend Lines Point Point Point 1' Point Point Point No Point Point Yes No Yes Yes Yes Yes Point Point, jet Point Cont Cont Cont Cont Lines Cont Lines Lines Lines Lines Cont purpose

NS, simple 1ES0102 0.4-1.5 Bright Complex PKS2155 0.2Med Blazer 20+ Capella 0.2-2 Bright Brems + lines AR Lac Brems + lines HR 1099 0.5-6 Bright Brems + lines Algol 0.5-6 Bright Brems + lines Crab 0.5Bright Cas A PSR 1509 3C273 Bright Mkn421 Bright


O836+71 1-100 Perseus cluster A2199 Ophi <20 cluster Cygnus 0.3-5 loop On-board calibration sources with instrumental fluorescence lines Bursters

Bright FSRQ

Yes, spectral constant Yes Yes

Cont

Line Move block of metal below detector, e.g. as seen from XMM pn copper Yes Line

contaminati on

Star clusters Ngc2516 Highly absorbed sources Closed

Variability tracking, timing alignment Astrometry Star cluster Astrometry redistributio n Instrumental background Needs Energy scale > 6 keV, line shapes Lines with widths known < 100 km/s Comments Grating calibration, XMS

Future missions Con-X

Bright stellar flares On-board calibration sources with instrumental fluorescence lines Transfer standards

Connection of low energy sources with high energy sources, targets for simultaneousobservations

Problem of different exposure times to get high quality spectra, e.g. ksec for low x-rays but Msec for high energy missions