List of Figures

• 2.1. The LWS with optical path overlay
• 2.2. Mirror 2
• 2.3. Photograph of the LWS
• 2.4. The LWS grating
• 2.5. The LWS spectral range
• 2.6. LWS flight model filters
• 2.7. LWS flight model detector responses
• 2.8. Grating efficiency measurements
• 2.9. The construction of a Fabry-Pérot etalon
• 2.10. FP finesse and transmission as a function of reflectance
• 2.11. Drawing of the LWS detector block
• 2.12. Integrating amplifier circuit
• 2.13. LWS ramps
• 2.14. The effect of a bias boost
• 2.15. An example of a glitched ramp
• 3.1. Modes of the LWS
• 4.1. Data processing overview
• 4.2. Schematic overview of Derive-SPD
• 4.3. Overview of Auto-Analysis
• 4.4. Illuminator flash sequence
• 4.5. Comparison of OLP 8 and OLP 10 illuminator processing
• 5.1. Uranus model
• 5.2. Relative Spectral Response Function (RSRF)
• 5.3. Derivation of the FPS throughput with Mars `mixed-mode' observations
• 5.4. Derivation of the FPL throughput with Mars `mixed-mode' observations
• 5.5. Martian rotational modulation detected at 3% level
• 5.6. Comparison of IRAS and LWS fluxes at 100 m for a wide range of fluxes
• 5.7. Ratio of the IRAS flux to LWS flux at 100 m for various source types
• 5.8. LWS versus IRAS flux comparison at 100m for three different samples
• 5.9. LWS versus IRAS flux comparison at 60m
• 5.10. A curved ramp
• 5.11. Modelled versus observed photocurrents of Saturn for LW3
• 5.12. Strong source corrected spectrum
• 5.13. A curved half-second ramp
• 5.14. Ramps hitting the ADC rail
• 5.15. LW5 SagittariusB2 with quarter- and half-second processing
• 5.16. Offset positions of the Mars beam profile observations
• 5.17. The mean beam profile for each detector
• 5.18. FWHM vs. detector for the four alignments
• 5.19. Correction factor for extended sources versus wavelength
• 5.20. Comparison of LWS and IRAS 100 m fluxes in Trumpler 14 and 16, and Galactic Centre
• 5.21. Model of the point spread function as sampled with the LWS
• 5.22. Main LWS grating wavelength standards
• 5.23. Deviation of the measured line center
• 5.24. Measured grating profiles
• 5.25. Gap between plates versus encoded position for FPS and FPL
• 5.26. Monitoring data for FPL
• 5.27. Velocity residuals for ORION CO lines
• 5.28. L01 full grating spectrum of a background position
• 5.29. Comparison between serendipity and grating rest observation
• 5.30. Parallel map in the Galactic Centre region
• 5.31. Comparison between map fluxes and raster fluxes
• 6.1. Example of a remaining glitch in the calibrated data
• 6.2. Example of fringes in the spectrum of an extended source
• 6.3. Example of spectrum fracturing
• 6.4. Double-peaked feature in SW1
• 6.5. Example of features due to the near-IR leak in the spectrum of Aldebaran
• 6.6. Straylight features on LW detectors
• 6.7. Examples of transients in fixed-grating observations
• 6.8. Variation of transient effect correction parameters with time
• 6.9. Result of the transient correction for an extended source
• 6.10. Result of the transient correction for a non-extended source
• 6.11. Example of `saggy' sub-spectra
• 6.12. Stability and systematic errors in the FP wavelength calibration
• 6.13. Example of the raw data recorded on a `non-prime' detector
• 6.14. Location of the FP `useful' data on the grating profile
• 6.15. Comparison of prime and co-added non-prime data
• 6.16. FP transmission for orders at wavelengths from to
• 6.17. Grating profile with the contribution from the two FP side orders