Improving XMM-Newton EPIC pn data at low energies: method and application to the Vela SNR

Konrad Dennerl; Bernd Aschenbach; Ulrich G. Briel; Hermann Brunner; Vadim Burwitz; Jakob Englhauser; Michael J. Freyberg; Frank Haberl; Gisela Hartner; Anatoli F. Iyudin; Eckhard Kendziorra; Norbert Meidinger; Elmar Pfeffermann; Wolfgang Pietsch; Lothar Strueder; Vyacheslav E. Zavlin

doi:10.1117/12.551307

11 October 2004 Improving XMM-Newton EPIC pn data at low energies: method and application to the Vela SNR

Konrad Dennerl, Bernd Aschenbach, Ulrich G. Briel, Hermann Brunner, Vadim Burwitz, Jakob Englhauser, Michael J. Freyberg, Frank Haberl, Gisela Hartner, Anatoli F. Iyudin, Eckhard Kendziorra, Norbert Meidinger, Elmar Pfeffermann, Wolfgang Pietsch, Lothar Strueder, Vyacheslav E. Zavlin

Author Affiliations +

Proceedings Volume 5488, UV and Gamma-Ray Space Telescope Systems; (2004) https://doi.org/10.1117/12.551307
Event: SPIE Astronomical Telescopes + Instrumentation, 2004, Glasgow, United Kingdom

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.

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Konrad Dennerl, Bernd Aschenbach, Ulrich G. Briel, Hermann Brunner, Vadim Burwitz, Jakob Englhauser, Michael J. Freyberg, Frank Haberl, Gisela Hartner, Anatoli F. Iyudin, Eckhard Kendziorra, Norbert Meidinger, Elmar Pfeffermann, Wolfgang Pietsch, Lothar Strueder, and 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); https://doi.org/10.1117/12.551307

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