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The European Space Agency (ESA) Infrared Space
Observatory ( ISO) was launched on 17 November 1995.
The Long Wavelength Spectrometer (LWS) is one of two
complementary spectrometers aboard ISO. The LWS
contains ten dectectors to cover the
wavelength range 43-196.9m.
It operates in two observing modes, corresponding to medium and high
spectral resolution.
In medium resolution mode, the LWS contains a reflection grating to give a
spectral resolving power (
) from
150 to 200.
In high resolution mode, a Fabry-Perot (FP)
Interferometer is inserted before the grating to give a spectral resolution
ranging from 6800-9700 across the entire wavelength range
(Clegg et al. 1996; Swinyard et al. 1999).
The LWS Interactive Analysis (LIA) is a software package designed to allow users to inspect, reprocess, and recalibrate their LWS data with the possibility of interactively customizing the various data reduction stages to their particular set of data. It is a joint development of the ISO-LWS Instrument Team at Rutherford Appleton Laboratories (RAL, UK--the PI institute) and the Infrared Processing & Analysis Center (IPAC, USA). LIA development started in 1997 (Sidher et al. 1997). The current version is LIA 8.1. The final version will be LIA 10, which will operate on products from OLP 10--the final pipeline processing software to be released. The current version of LIA can be obtained via LIA/UKIDC web site and LIA/IPAC web site.
LIA is written under the Interactive Data Language (IDL) environment. The programming language used in this package is also IDL. IDL provides the ability to plot and visualize data easily and immediately. The ISO Spectral Analysis Package (ISAP), which is required to run LIA, is also written in IDL.
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ISAP is a software package for the reduction and scientific analysis of the ISO SWS (Short Wavelength Spectrometer) and LWS Auto Analysis Results (AARs). AARs are the end product of the official automatic pipeline processing, which processes the raw data as they are received from the satellite, via a number of intermediate stages.
During the early post- ISO mission stage, the calibration accuracy of these products was generally good to within 20% on average. One of the advantages of LIA is that it allows users to check the quality of their scientific and calibrated data, and also to recalibrate them if necessary.
There are three classes of routines are available under LIA. They are Inspection Routines, Recalibration Routines, and Interactive Routines.
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Automatic routines: One of the advantages of LIA 10 will be that it process large amounts of data without manual intervention.
Planned recalibration routines
S. J. Chan thanks the Program Organizing Committee of the Tenth Annual Conference on Astronomical Data Analysis Software and Systems for offering her financial support to attend the conference.
Clegg, P. E., et al. 1996, A&A, 315, L38
Sidher, S. D. 1997, ESA SP-419, 297
Swinyard, B. M., et al. 1998, in SPIE Proc., Vol. 3354, 888