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About the PANTER Test Facility
For the characterization and calibration of X-ray telescopes and
detectors
MPE operates the test facility PANTER. This instrument was originally
built
between 1977 and 1980 for the characterization of ROSAT and extended
due
to the experimental requirements in the following years.
Nevertheless, during
the last decades nearly all astronomical X-ray experiments or parts of
them have been tested at this facility. The test history contends the
following
X-ray missions:
| rocket experiments |
1977 - 1987 |
| ROSAT |
1977- 1990 |
| EXOSAT |
1980 - 1982 |
| MIR-HEXE |
1981 |
| AXAF |
1982 - 1996 |
| SAX |
1985 - 1994 |
| ROSAT-WFC |
1987 - 1990 |
| JET-X |
1990 - 1997 |
| SOHO/CDS |
1991- 1994 |
| XMM |
since 1987 |
| ABRIXAS |
1995-1999 |
| SWIFT-XRT |
2000,2002 |
ASTRO E2
|
2003
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These measurement campaigns include work in international
projects and
also the MPE participation at the scientific data output of the
experiments.
 An
aerial photograph of the facility is shown in the enclosed figure. At
one
end of the vacuum system an X-ray source is installed, the other end is
given by the test chamber. The test chamber has a diameter of 3.5 m and
a length of 12 m to assimilate X-ray telescopes and small satellites.
The
distance of 130 m between X-ray source and telescope was chosen to
approximate
the infinite source distance of an astronomical X-ray object. By
operation
of several manipulators telescope and detectors can be positioned with
high precision
The main task of the PANTER facility is the characterization
of X-raytelescopes.
This includes the measurement of reflectivity and straylight of plane
mirrors
and single mirror shells, and the characterization of the image
qualities
of complete telescopes. Also focal instruments (detectors,gratings,
filters)
are measured at PANTER. Before launch the flight configuration is
calibrated
in an end-to-end test. In addition thermal cycling and thermal-vacuum
tests
for the qualification of satellite parts are performed in two smaller
vacuum
chambers, too.
The technical work during the last years was characterized by
improvements
of the facility and technical developments, especially required for the
XMM experiments. By the MPE personnel and the MPE-PANTER team
(Aschenbach,Bräuninger,
Burkert, Döhring, Egger, Elender, Hartner, Lechner, Oppitz,
Predehl,
Strüder, Wölfl) the following work has been done:
- the absolute calibration of detectors
- the enlargement of the cleanroom
- the optimization of a X-ray monochromator
- the development of new software programmes
- the installation of a new computer network system
- the installation of new X-ray sources
- the implementation of a new control and archiving system
for the
facility
- the installation of new manipulators based on XMM
requirements
- the installation of a monitor system in front of the mirror
systems
- the installation of a monitor system (drift chamber) near
the
source
and also by supporting ESA the installation of two new X-ray channels
at
the CSL test facility. The scientific program at the PANTER facility
during
the last two years was also determined by the XMM experiments.
Nevertheless,the
measurement of other experiments (ABRIXAS, AXAF, Jet-X) has also been
done.
In detail, the following tests have been performed at the
PANTER facility
in 1996 and 1997
|
AXAF
|
thermal balance test |
Bräuninger, Burkert, Kettenring, Predehl,
Wölfl |
|
Jet-X
|
end-to-end test |
Bräuninger, Burkert, Döhring, Egger,
Elender, Oppitz, Trümper,Wölfl |
|
ABRIXAS
|
mirror calibration |
Aschenbach, Bräuninger, Burkert, Döhring,
Egger, Elender, Oppitz, Predehl, Trümper,
Wölfl |
|
ABRIXAS
|
thermal balance test of QM mirror system |
Bräuninger, Kettenring, PredeHl, Wölfl |
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EPIC-pn CCD
|
thermal balance test of focal instrumentation |
Bräuninger, Heuschmann, Reppin, EPIC team |
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XMM
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calibration of mirror systems QM, FM1, FM2 |
Aschenbach, Bräuninger, Burkert, Döhring,
Egger, Elender, Hartner,
Lechner, Oppitz, Strüder, Trümper, Wölfl, ROSAT-PSPC-team |
|
XMM
|
end-to-end tests of QM-mirror + RGS, FM2 mirror + RGS |
Aschenbach, Bräuninger, Burkert, Döhring,
Egger, Elender, Lechner,
Oppitz, Strüder, Trümper, Wölfl, ROSAT-PSPC team |
|
XMM
|
end-to-end tests of QM-mirror + EPIC-MOS CCD |
Aschenbach, Bräuninger, Burkert, Döhring,
Egger, Elender, Lechner,
Oppitz, Strüder, Trümper, Wölfl, ROSAT-PSPC team |
|
XMM
|
end-to-end tests of QM-mirror + EPIC-pn CCD |
Aschenbach, Bräuninger, Burkert, Döhring,
Egger, Elender, Lechner,
Oppitz, Strüder,Trümper, Wölfl, ROSAT-PSPC team |
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![[Back to MPE]](http://www.mpe.mpg.de/panter/bilder/logo-mpe-green.gif){kind=logo}
![[Back to MPG]](http://www.mpe.mpg.de/panter/bilder/logo-mpg-minerva-green.gif){kind=logo}
An
aerial photograph of the facility is shown in the enclosed figure. At
one
end of the vacuum system an X-ray source is installed, the other end is
given by the test chamber. The test chamber has a diameter of 3.5 m and
a length of 12 m to assimilate X-ray telescopes and small satellites.
The
distance of 130 m between X-ray source and telescope was chosen to
approximate
the infinite source distance of an astronomical X-ray object. By
operation
of several manipulators telescope and detectors can be positioned with
high precision