Документ взят из кэша поисковой машины. Адрес оригинального документа : http://xmm.vilspa.esa.es/calibration/documentation/epic_cal_meetings/200704/Haberl.pdf Дата изменения: Tue May 13 17:54:00 2014 Дата индексирования: Wed Apr 13 13:14:20 2016 Кодировка: Поисковые слова: п п п п п п п п п

EPIC-pn effective area and response
· Effective area above 4 keV · Gain/CTI correction TI mode · Re-distribution

Frank Haberl
EPIC cal meeting, Palermo, 12-13 April 2007


SAS 7.0.0 + XRT3_XAREA_0010.CCF


Modified mirror areas XRT3_XAREA_0011.CCF public since 2007-03-24

old 0010 new 0011


SAS 7.0.0 + XRT3_XAREA_0011.CCF


SAS 7.0.0 + XRT3_XAREA_0010.CCF


Comparison XRT3_XAREA_00xx.CCF 10 11
Spectra 3C273 SW H1426+428 SW PKS2155 SW PKS2155 TI 2 4748 4196 5193 1650 2 red 1. 1. 1. 1. 202 262 159 313 2 4592 3986 5097 1511 2 red 1. 1. 1. 1. 163 199 137 202 dof 3950 3325 4520 1257

ring

Powerlaw index: 3C273 SW 1.6187 1.5842 1.5928 1.5940 1.5974 1.7665 1.6839 1.7030 1.6817 1.5836 1.6157 1.5822 1.5900 1.5940 1.5950 1.7647 1.6804 1.6986 1.6919 1.5689 H1426+428 SW 1.7978 2.1650 2.1871 2.2010 2.0054 2.1531 1.7938 2.1589 2.1799 2.1941 1.9997 2.1457

Index decreases (spectra become harder) by 0.003-0.007


Timing mode ­ Gain/CTI correction

EPN_CTI_0015.CCF

EPN_CTI_0016.CCF in development


Re-distribution A Problem around 370 eV


Re-distribution: A Problem around 370 eV


Re-distribution: Model spectrum for Zeta Puppis
RGS 1/2 Continuum from EPIC-pn powerlaw 28 Gaussians Concept: Apply RGS model to pn spectra. Allow some degrees of freedom and fit to pn. Re-apply the new model to RGS. Investigate the discrepancies.


Re-distribution: Model spectrum for Zeta Puppis

RGS model for EPIC-pn: Fix For Fi Fi For all line widths line-complexes which are unresolved in pn: x line energies relative to each other x line intensity ratios each line complex: 1 free energy and 1 free normalization

Improvements: add some weak lines combine more lines iterate continuum


Re-distribution: Zeta Puppis
Fit of RGS model to pn All line energies fixed Free normalizations (one per line complex)


Re-distribution: Zeta Puppis

Re-application o Discrepancies: Lines above 800 Residuals in the The C VI line at

f model to RGS: Fit of overall normalization factor eV are stronger in RGS spectra pn spectra above 800 eV 367.6 eV is much stronger in pn spectra


Re-distribution: Zeta Puppis
Free line energies for the 3 line complexes above 800 eV RGS 810.1 900.7 1000.6 pn 806.0 eV 894.6 eV 996.4 eV

about -5 eV shift for pn A SW mode problem?


Small Window mode 1E0102

3 Line complexes (2 O, 1 Ne)

2 Line complexes (1 O, 1 Ne with more lines)

Summary: More lines need to be linked together for pn SW mode needs slight energy correction at 800-1100 eV Re-distribution problem below 500 eV