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Next: The Interaction of the ISO-SWS Pipeline Software and the ISO-SWS
Interactive Analysis System
Up: Dataflow and Scheduling
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S. Ott1 and R. Gastaud2,
A. Abergel3, B. Altieri1,
J-L. Auguères2, H. Aussel2,
J-P. Bernard3, A. Biviano1,4,
J. Blommaert1, O. Boulade2,
F. Boulanger3, C. Cesarsky5,
D.A. Cesarsky3, V. Charmandaris2,
A. Claret2, M. Delaney1,6,
C. Delattre2, T. Deschamps2,
F-X. Désert3, P. Didelon2,
D. Elbaz2, P. Gallais3,
K. Ganga7, S. Guest1,8, G. Helou7,
M. Kong7, F. Lacombe9,
D. Landriu2, O. Laurent2,
P. Lecoupanec9, J. Li7,
L. Metcalfe1, K. Okumura1,
M. Pérault3, A. Pollock1,
D. Rouan9, J. Sam-Lone2,
M. Sauvage2, R. Siebenmorgen1,
J-L. Starck2, D. Tran2,
D. Van Buren7, L. Vigroux2 and
F. Vivares3
ISO Science Operations Centre, Astrophysics Division
of ESA, Villafranca del Castillo, Spain
CEA, DSM/DAPNIA, CE-Saclay, Gif-sur-Yvette, France
IAS, CNRS, University of Paris Sud, Orsay, France
Istituto TESRE, CNR, Bologna, Italy
CEA, DSM, CE-Saclay, Gif-sur-Yvette, France
UCD, Belfield, Dublin, Ireland
IPAC, JPL and Caltech, Pasadena, CA, USA
RAL, Chilton, Didcot, Oxon, England
DESPA, Observatoire de Paris, Meudon, France
We review the algorithms currently implemented in CIA and present some examples. We will also outline foreseen changes to accommodate future improvements for these algorithms.
ESA's Infrared Space Observatory (ISO) was successfully launched on November
17th, 1995.
ISO is an astronomical, three-axis-stabilized
satellite with a 60-cm diameter primary mirror (Kessler et al. 1996). Its four
instruments (a camera, ISOCAM, an imaging photo-polarimeter and two
spectrometers) operate at wavelengths between 2.5-240 microns at temperatures
of 2-8 K.
ISOCAM takes images of the sky in the wavelength range 2.5 to 18 microns (Cesarsky et al. 1996). It features two independent 32 x 32 pixel detectors: the short-wavelength channel (2.5 to 5.5 microns), and the long-wavelength channel (4 to 18 microns). A multitude of filters and lenses enable the observer to perform measurements at different wavelengths, with different fields of view or with polarizers.
The development of CIA was started in 1994, its main goals being to calibrate ISOCAM, to provide the means to perform any sort of investigation requested for problem diagnostics, to assess the quality of ISOCAM pipeline data products, to debug, validate and refine the ISOCAM pipeline and to perform astronomical data-processing of ISOCAM data. The overall system now represents an effort of 20 man-years and comprises over 1300 IDL and 350 FORTRAN, C, and C++ modules and 30 MB of calibration data.
At the moment CIA is distributed to experienced users upon approval; currently it is used at 30 authorized sites. However, this policy will change with the end of ISO operations in summer 1998. Thereafter CIA V3.0 will be made generally available for the astronomical community.
At the moment, the following steps for astronomical ISOCAM data processing are
generally performed:
CIA contains various algorithms for deglitching and transient correction. Multiresolution median and temporal median filtering algorithms are most commonly used for deglitching. Similarly the most commonly used algorithms for transient correction are the inversion-method and exponential fitting. The resulting quality depends on the amount of data available. Therefore we will try in the future to treat a whole revolution instead of single observations.
Flat-fielding with library-flats and automatic flat-fielding using the raster observation being analysed are both implemented in CIA. However, the lens wheel does not always come to exactly the same position. When the wheel position for the observation differs from the wheel position reached when the flat-field was obtained, this affects the quality of the final image. Therefore we hope to implement a correction for this effect (lens-wheel jitter) in the flat-field algorithm.
Various algorithms can be used for the dark current subtraction. Currently implemented are the dark correction with library or user supplied darks (e.g., handover darks) as well as a second order dark correction. Studies have shown that the dark can be better predicted as a function of the observation time or by scaling with a reference dark. It is planned to implement these new dark corrections in near future.
CIA users can overlay a contour plot of one image on a colour display of another. The two input images can come from different instruments, have different size and resolution -- the only requirement is that there is astrometry information associated with each image and that they overlap spatially. The images can be shifted and annotated.
Kessler, M., Steinz, J.A. et al. 1996, A & A, Vol. 315, L27
Cesarsky, C., et al. 1996, A & A, Vol. 315, L32
Delaney, M. ed., ISOCAM Interactive Analysis User's Manual, ESA Document
Ott, S., et al. 1997, ``Design and Implementation of CIA, the ISOCAM Interactive Analysis System", in Astronomical Data Analysis Software and Systems VI, ASP Conf. Ser., Vol. 125, eds. Gareth Hunt and H. E. Payne (San Francisco, ASP), 34
Siebenmorgen, R. et al. ISOCAM Data User's Manual, ESA Document, Reference SAI/95-221/DC
Starck, J-L., & Murtagh, F., et al. Image Processing and Data Analysis -- The Multiscale Approach, Cambridge University Press
Next: The Interaction of the ISO-SWS Pipeline Software and the ISO-SWS
Interactive Analysis System
Up: Dataflow and Scheduling
Previous: Achieving Stable Observing Schedules in an Unstable World
Table of Contents -- Index -- PS reprint -- PDF reprint