11 October 2004 Improving XMM-Newton EPIC pn data at low energies: method and application to the Vela SNR
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Abstract
High quantum efficiency over a broad spectral range is one of the main properties of the EPIC pn camera on-board XMM-Newton. The quantum efficiency rises from ~75% at 0.2 keV to ~100% at 1 keV, stays close to 100% until 8 keV, and is still ~90% at 10 keV. The EPIC pn camera is attached to an X-ray telescope which has the highest collecting area currently available, in particular at low energies (more than 1400 cm2 between 0.1 and 2.0 keV). Thus, this instrument is very sensitive to the low-energy X-ray emission. However, X-ray data at energies below ~0.2 keV are considerably affected by detector effects, which become more and more important towards the lowest transmitted energies. In addition to that, pixels which have received incorrect offsets during the calculation of the offset map at the beginning of each observation, show up as bright patches in low-energy images. Here we describe a method which is not only capable of suppressing the contaminations found at low energies, but which also improves the data quality throughout the whole EPIC pn spectral range. This method is then applied to data from the Vela supernova remnant.
© (2004) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Konrad Dennerl, Konrad Dennerl, Bernd Aschenbach, Bernd Aschenbach, Ulrich G. Briel, Ulrich G. Briel, Hermann Brunner, Hermann Brunner, Vadim Burwitz, Vadim Burwitz, Jakob Englhauser, Jakob Englhauser, Michael J. Freyberg, Michael J. Freyberg, Frank Haberl, Frank Haberl, Gisela Hartner, Gisela Hartner, Anatoli F. Iyudin, Anatoli F. Iyudin, Eckhard Kendziorra, Eckhard Kendziorra, Norbert Meidinger, Norbert Meidinger, Elmar Pfeffermann, Elmar Pfeffermann, Wolfgang Pietsch, Wolfgang Pietsch, Lothar Strueder, Lothar Strueder, Vyacheslav E. Zavlin, Vyacheslav E. Zavlin, } "Improving XMM-Newton EPIC pn data at low energies: method and application to the Vela SNR", Proc. SPIE 5488, UV and Gamma-Ray Space Telescope Systems, (11 October 2004); doi: 10.1117/12.551307; https://doi.org/10.1117/12.551307
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