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Sahnow, D. J. & Dixon, W. Van Dyke 2003, in ASP Conf. Ser., Vol. 295 Astronomical Data Analysis Software and Systems XII, eds. H. E. Payne, R. I. Jedrzejewski, & R. N.
Hook (San Francisco: ASP), 245
The Next Step for the FUSE Calibration Pipeline
David J. Sahnow, W. Van Dyke Dixon, and the FUSE Science Data
Processing Group
Department of Physics and Astronomy, The Johns Hopkins University,
Baltimore, MD 21218, Email: sahnow@pha.jhu.edu
Abstract:
The calibration pipeline for the Far Ultraviolet
Spectroscopic Explorer
(FUSE) satellite was designed years before it was
launch-ed.
Since then, a number of unexpected instrumental features were
discovered and the pipeline
was modified appropriately. Eventually, these changes made the design
so cumbersome that the pipeline became difficult to maintain. In 2002,
we began to develop a new pipeline concept that takes into account the
actual instrument characteristics.
We present our plans for this improved calibration pipeline.
The design of the CalFUSE pipeline dates to well before the launch
of FUSE.
As the primary FUSE mission draws to a close and an extended mission begins,
the resources available for maintaining the existing
pipeline will diminish. Thus, it is prudent to rethink the design,
consider ways to make it easier to maintain, and investigate changes
which may improve the data quality. This process
was begun in the summer of 2002 when we proposed that for version 3 of the
pipeline, a new method for calibrating the data be used. These changes,
which are described in the following sections, are
intended to improve the data quality while ensuring flexibility for future
modifications. The ideas for these changes have been prompted by our
three years of experience with FUSE data, along with information obtained
during the design of the pipeline for the
Cosmic Origins Spectrograph, which will use a similar detector
(Beland et al., this conference).
The present FUSE pipeline (Dixon et al. 2003) is less flexible than desired
when dealing with a number of instrument properties which were discovered (or
appreciated more
clearly) after launch. These include the thermally-induced motions of the
mirrors and gratings, changes in the detector y scale as a function of count
rate, event bursts, the ``worm,'' and the decrease in pointing stability due
to the failure of reaction wheels. Some of these effects are due to
unexpected performance of the instrument hardware, while others are a
consequence of the analog nature of the double delay line detectors. Among the
shortcomings of the original design are the fact that time-tag data was
converted
into a two-dimensional image in an early step. Although this would work well if
there were no time-varying effects on the data, this is not the case for
FUSE.
In addition to being developed with the instrument anomalies in
mind, the new design is more flexible, so that any new effects discovered as
the instrument
ages can be dealt with more gracefully. The modular design should allow for
the addition of new modules with little or no effects on the existing ones.
Although the current design also permitted modules to be added, the fact that
each created its own output file and expected a unique format for its input
made this difficult.
Figure 1 shows the path of a photon through the instrument.
This list describes each effect. Items marked with an
asterisk were not considered in the original pipeline design.
1.1 |
Doppler Shift due to motion of satellite. |
1.2 |
Wavelength shift due to heliocentric motion. |
2. |
*Satellite pointing jitter. |
3. |
Four Barrel design -- divides incoming light among channels. |
Figure 1:
A schematic view of the path of a photon through the FUSE instrument.
The steps which affect the data (and consequently, the pipeline) are
numbered; each of these must be compensated for in the pipeline process.
|
4.1 |
*Mirror motions due to thermal effects, which cause motion of the spots
at the FPAs. |
4.2 |
Mirror reflectivity. |
5. |
Focal Plane Assembly (FPA) position, which shifts the location of the
spectra on the detectors. |
6.1 |
Grating efficiency. |
6.2 |
Dispersion & astigmatism due to grating design & alignment. |
6.3 |
*Grating motions due to thermal effects, which cause motion of the
spectra on the detector. |
7. |
*The ``worm,'' caused by an interaction of the optical design and the
detector grid wires. |
8.1 |
Detector quantum efficiency. |
8.2 |
Detector flat field. |
8.3 |
Detector bad pixels. |
8.4 |
Detector background. |
9.1 |
*Detector ``walk'' -- position of photon depends on pulse
height. |
9.2 |
Detector geometric distortion effects. |
9.3 |
*Detector change in Y scale as a function of count rate. |
9.4 |
Detector shift and stretch as a function of temperature. |
9.5 |
Detector electronics dead time. |
10. |
Instrument Data System (IDS) computer dead time. |
A major improvement in version 3 is the use of a single Intermediate Data File
(IDF) for the entire pipeline.
The IDF is a FITS file containing a binary table in the first extension.
This extension contains one row per photon, and has columns for time, x, y,
and
pulse height from the raw data; x and y in the geometrically undistorted
detector frame; a weighting factor for each photon; x and y after all motions
are removed; channel; and wavelength. Nearly all of the pipeline modules
operate
on this one file, by reading and writing particular columns.
A simplified outline of the processing steps is presented below. The numbers
in parentheses refer to the steps in the previous section.
- Put all photons in a rectified image frame:
- Adjust photon weight for IDS dead time (10).
- Adjust photon weight for detector electronics dead time (9.5).
- Correct (x,y) position of photon for thermal stretch & shift
(9.4).
- Adjust y position of photon based on count rate (9.3).
- Correct (x,y) position of photon for geometric distortion (9.2).
- Adjust x position of photons to account for detector ``walk''
(9.1).
- Remove Motions:
- Identify channel (LiF1, SiC1, etc.) for each photon.
- Calculate the time-dependent y centroid for each aperture.
- Adjust (x,y) position of photons to correct for grating motions
(6.3).
- Adjust x position of photons to compensate for FPA offsets (5)
- Adjust (x,y) position of photons to correct for mirror motions
(4.1).
- Use satellite jitter to discard data during particular times (2).
- Calculate the y centroid for all photons in each aperture.
- Assign Wavelengths:
- Assign a wavelength to each photon based on position & channel
(6.2).
- Correct for the heliocentric motion (1.2).
- Correct for the Doppler shift (1.1).
- Screen the Data:
- Identify times when limb angle constraints are violated, or the
satellite is in the SAA.
- Identify times when the detector high voltage values are
outside of their nominal ranges.
- Find times when event bursts occurred.
- Exclude events which have pulse heights outside the nominal
range.
- Calibration:
- Convert each photon weight into units of erg cm (4.2,
6.1, 8.1)
- Extract a one dimensional spectrum as a function of wavelength
for each channel; correct for detector background and flat field (8.2, 8.4).
- Correct for the worm (7).
The single Intermediate Data File means that the I/O is the same for all
pipeline modules, and thus the order of modules can be changed, or new ones
added, with a minimum of complication. The fact that the flow of the pipeline
processing steps more closely follows the inverse of
the ``life of the photon'' than previous version did makes it easier for
users to understand the steps, and makes it easier to maintain.
Housekeeping (pointing stability, count rates, and high voltage values)
data are used where appropriate to improve the quality of the data.
Since every pixel is assigned a floating point wavelength -- rather than
having
every photon put in a wavelength bin as happens now -- the final
1-dimensional spectrum can be binned to any convenient
wavelength scale. This permits a straightforward addition of data from
multiple segments. Because the
analog photon positions (with times attached) are maintained for as long
as possible, roundoff problems that currently exist will be minimized.
Acknowledgments
The NASA-CNES-CSA FUSE mission is operated by the Johns Hopkins University
under NASA contract NAS5-32985.
References
Dixon, W. V. and Sahnow, D. J. 2003, this volume, 241
© Copyright 2003 Astronomical Society of the Pacific, 390 Ashton Avenue, San Francisco, California 94112, USA
Next: Middle Tier Services Accessing the Chandra X-Ray Center Data Archive
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Previous: CalFUSE v2.2: An Improved Data Calibration Pipeline for the Far Ultraviolet Spectroscopic Explorer (FUSE)
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