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XMM-Newton Science Analysis System Page: 1
testodf
July 1, 2008
Abstract
Articially created ODFs to be used for testing.
1 Description
This packages contains a number of test ODFs that are used in the testing of the XMM SAS.
When working in the SAS environment, the location of a given ODF should be inquired as follows:
saslocate lib/testodf/scisimsimple
where scisimple is the name of the sought ODF.
The ODFs are generated with scisim-2.1.
1.1 scisimsimple
This test ODF contains one X-ray source (1 keV, broadened with a 20 eV Gaussian), and several optical
sources. The ODF was generated using the default conguration modes for all of the XMM instruments
as provided by SciSim.
1.2 scisimquad
This test ODF is an observation of four point sources with an incident angle of 0.05 degrees and positioned
in a square. Two have a Gaussian spectrum centered around 1 keV and 100 eV width, and two have a
powerlaw spectrum between 10 eV and 10 keV with a slope of -1. Two are point sources, two are extended
sources with a radius of 0.01 degrees. Two have a constant ux, one has a sinusoidal ux variation with
a period of 10 s and one with a period of 30 s.
These sources are observed during 3 ks with the instrument in the default mode.
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1.3 scisimmultimode
This test ODF contains three exposures, each with a dierent conguration of the instruments. There is
one X-ray source (1 keV, broadened with a 20 eV Gaussian), and several optical sources. The intensity of
the X-ray source is modulated with a sinusoid of 10 s period.
The rst exposure was generated using the default conguration modes for all of the XMM instruments
as provided by SciSim 2.1 (see scisimsimple).
In the second exposure EPIC PN is in primeLargeWindowCentral mode with the thick lter, EPIC MOS
is in PrimePartialW2 mode with the thick lter, and RFC is high time resolution mode (HTR) with only
CCD 5.
In the third exposure EPIC PN is in FastModeTiming mode with the thin lter, EPIC MOS is in
FastModeUncompressed with the thin lter, and RFC is in HTR mode with all CCDs.
1.4 scisimmultiline
This test ODF is an observation of a point source that is placed on-axis, and whose spectrum consists of
30 lines. Each line has a Gaussian prole; the width is 1/100th of the energy of the center of the peak.
This source is observed with all instruments in their 'default' conguration during 10 ks.
1.5 scisimwobble
This test ODF is a simulation of an observation of a point source. The spectrum is a narrow Gaussian
line at 1 keV. The source is located in an arbitrary location in the sky, and the spacecraft is initially
pointing twoards the source. The spacecraft is drifting slowly away from the source and at the same time
some jitter occurs.
1.6 scisimdrift
This test ODF is an observation of a point source in an arbitrary location in the sky. Its spectrum is
a narrow Gaussian at 1 keV. The source is observed for 500 s while the spacecraft pointing is slowly
drifting.
1.7 scisimf
This test ODF is an observation of nine point sources. Five form an F shape, and the other four form
a smaller F shape with the middle source of the large F. The cluster extends over 0.25 degrees. Each
source has a narrow Gaussian line spectrum, each around its own energy (1 keV, 2 keV up to 5 keV).
These sources are observed with a spacecraft that is initially pointing to the source in the center and is
drifting slowly during the observation.
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1.8 scisimwga
The eld from the WGAcat x-ray catalogue centred on Ra=5.7 deg, Dec=4.5 deg is simulated with scisim
with a position angle of 0.0 deg. There is a source which is obviously brighter than the rest at Ra=5.8338
deg Dec=4.4829 deg.
1.9 scisimngc2516
This is a simulation of an observation of the cluster NGC2516 observed for 10 ks with the instruments
in their default conguration.
1.10 scisimlong
This test ODF contains a model for NGC4472 and several optical sources. These sources are observed
for 70 ks. All instruments are in the default conguration mode as provided by SciSim.
References
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