Документ взят из кэша поисковой машины. Адрес оригинального документа : http://xmm.vilspa.esa.es/calibration/documentation/epic_cal_meetings/200502/af_deep_bkg.pdf Дата изменения: Fri May 16 13:28:28 2014 Дата индексирования: Wed Apr 13 13:23:33 2016 Кодировка:

EPIC-pn background in deep fields ­ taking a deep breath before diving
Finoguenov Alexis


HDFS


LH


COSMOS



COSMOS 9.5-12 keV


0.5-2 keV

COSMOS

Andy Read


2-4.5 keV

COSMOS

Andy Read


OOTE


Singles vs doubles


Spectral compari so n


After Renormalization


Clean Andy


Detector Outskirts: the golden Mile


.. and renormalized


The effect of OOTE


Is there some sky background in there?


A msg from Andy Fabian


Strategy for background subtraction
· Observation is filtered for flares · We use the Filter wheel closed accumulation of Michael Freyberg for pn · The above is similar to De Luca & Molendi · We remove the sources identified by both Chandra and XMM (5-10% residual contamination) · Two regions are used to test the in-field background




Components of the residual spectrum
· · · Hard X-ray background: 0.9-1.0 slope Galactic emission of 0.1 and 0.2 keV Intrumental background: quiescent soft protons background slope 3 Flux is similar to total CXB


Conclusions
· Background in deep fields appears to be similar · Initial problems with use of Andy Read`s or David Lumb`s background seems to resolve in difference in the cleaning · A consistent answer to 2-10 keV Cosmoc background with De Luca&Molendi · Quiescent soft proton flux is not evolving during 2002-2004