List of Figures

• 1.1. The ISO satellite flight model
• 1.2. The ISO Data Centre at VILSPA
• 2.1. ISO project organisation
• 2.2. Structure of the industrial consortium
• 2.3. Industrial contractors by country contribution
• 2.4. The pre-launch ISO project schedule
• 2.5. Principal Investigator (PI) organisations by country and instrument
• 2.6. The ISO Spacecraft Control Room
• 2.7. The ISO Instrument Control Room
• 3.1. Cut-away schematic of the ISO satellite
• 3.2. Definition of the spacecraft axes
• 3.3. Cryostat and telescope design
• 3.4. Helium flow diagram for ISO in orbit
• 3.5. ISO telescope optical layout.
• 3.6. ISO focal plane map
• 3.7. Attitude and Orbit Control Subsystem
• 3.8. Schematic of the Camera (ISOCAM)
• 3.9. Schematic of the Long Wavelength Spectrometer (LWS)
• 3.10. Schematic of the Photo-polarimeter (ISOPHOT)
• 3.11. Schematic of the Short Wavelength Spectrometer (SWS)
• 4.1. The ISO orbit
• 4.2. Visibility constraints of ISO
• 4.3. ESA's Villafranca Satellite Tracking Station in Spain
• 4.4. Skeleton schedule of ISO activities along an orbit
• 4.5. The ISO Mission Control System
• 4.6. Data flow within the Spacecraft Control Centre at Villafranca
• 4.7. Distribution of observing time
• 4.8. Distribution of ISO observation pointings
• 4.9. Mapping with ISO: Orientation 0°
• 4.10. Mapping with ISO: Orientation 47°
• 4.11. Usage of the instrument observing modes by time and number
• 5.1. Image of the ISOCAM PSF
• 5.2. Plot of the ISOCAM PSF
• 5.3. Straylight observed in a PHT22 raster map
• 5.4. Straylight observed in a CAM parallel image
• 5.5. Trapped electron fluxes as a function of ISO orbital time
• 5.6. Daily proton fluence during the ISO mission
• 5.7. Effect of the solar proton event of November 1997 on ISOCAM images
• 5.8. Example of a fader glitch in ISOCAM data
• 5.9. Example of a dipper glitch in ISOCAM data
• 5.10. Short term transient and long term drift in ISOCAM LW detectors
• 5.11. Raster observation suffering from long term drift and the correction
• 5.12. Transients in ISOPHOT-P1 detector
• 5.13. Transients in SWS detectors
• 5.14. Transients in ISOPHOT-P3 detector at intermediate flux level
• 5.15. Transients in ISOPHOT-P3 detector at low flux level
• 5.16. Transients in ISOPHOT-C100 detector
• 5.17. Transients in ISOPHOT-C200 detector
• 5.18. Transients in LWS-SW4 detector
• 5.19. Transients in LWS-LW2 detector
• 5.20. Transients in LWS-LW5 detector
• 5.21. Forward and backward scans in LWS-SW4 detector
• 5.22. Forward and backward scans in LWS-LW2 detector
• 5.23. Forward and backward scans of Uranus in LWS-LW2 detector after transient correction
• 5.24. Memory effects in ISOCAM SW detectors
• 5.25. ISOPHOT-P2 detector transients induced by chopper modulation
• 5.26. Transients in LWS-SW1 detector
• 5.27. Forward and backward scans of Uranus in LWS-SW1 detector
• 5.28. Forward and backward scans of Uranus in LWS-SW1 detector after transient correction
• 5.29. Forward and backward scans of NGC 6302 in LWS-SW1 detector
• 5.30. Forward and backward scans of NGC 6302 in LWS-SW1 detector after transient correction
• 5.31. Memory effects in band 4 of SWS
• 6.1. Bad pointing and extended source effects in SWS spectra
• 6.2. SWS versus PHT-s cross-calibration comparison
• 6.3. SWS versus PHT-S cross-calibration comparison in two faint sources
• 6.4. SWS versus CAM-CVF cross-calibration comparison
• 6.5. CAM-CVF versus PHT-S cross-calibration comparison
• 6.6. Composite SWS+LWS spectra of sources used for cross-calibration
• 6.7. PHT-S versus ISOCAM LW2 and LW7 filter measurements
• 6.8. ISOCAM filter versus SWS cross-calibration comparison
• 6.9. ISOPHOT photometry versus PHT-S, SWS and LWS spectroscopy of Comet Hale-Bopp
• 6.10. LWS fixed grating versus LWS grating scan and ISOPHOT measurements of Ceres
• 6.11. LWS fixed grating versus ISOPHOT measurements of Pallas
• 6.12. LWS fixed grating versus ISOPHOT measurements of Vesta
• 6.13. LWS fixed grating versus LWS grating scan and ISOPHOT measurements of Hygiea
• 6.14. SWS versus IRAS photometry at 12 $\mu$m
• 6.15. SWS versus IRAS photometry at 25 $\mu$m
• 6.16. Distribution of discrepancies between ISO and IRAS photometry at 12 and 25 $\mu$m
• 6.17. LWS/IRAS flux density ratios versus IRAS flux density at 100 $\mu$m
• 6.18. LWS versus IRAS photometry at 100 $\mu$m
• 6.19. Difference between LWS and IRAS fluxes at 60 and 100 $\mu$m
• 6.20. LWS versus IRAS photometry at 60 and 100 $\mu$m for a sample of extragalactic sources
• 6.21. ISO/IRAS flux density ratios versus IRAS flux density at 60 $\mu$m
• 6.22. ISO/IRAS flux density ratios versus IRAS flux density at 100 $\mu$m
• 6.23. LWS raster scans versus IRAS photometry at 100 $\mu$m
• 6.24. Chopped PHT-P and -C photometry versus IRAS photometry
• 6.25. SWS versus MSX filter A photometry
• 6.26. SWS versus MSX filter C photometry
• 6.27. SWS versus MSX filter D photometry
• 6.28. SWS versus MSX filter E photometry
• 6.29. Distribution of discrepancies between SWS and MSX photometry
• 6.30. PHT-S sky background versus COBE/DIRBE photometry
• 6.31. ISOCAM photometry of HIC 67485 versus model predictions
• 6.32. ISOCAM photometry of HIC 77277 versus model predictions
• 6.33. LWS grating scan observations of Uranus versus model predictions (full spectral range)
• 6.34. LWS grating scan observations of Uranus versus model predictions (per detector)
• 6.35. LWS grating scan observations showing the SW1 conspicuous double-peaked shape
• 6.36. LWS fixed grating observations of Uranus versus model predictions (full spectral range)
• 6.37. LWS fixed grating observations of Neptune versus model predictions (full spectral range)
• 6.38. LWS fixed grating observations of Ceres versus model predictions
• 6.39. LWS fixed grating observations of $\alpha$ Boo versus model predictions
• 6.40. Staring PHT-S spectra versus model predictions
• 6.41. Chopped PHT-S spectra versus model predictions
• 6.42. PHT-P and PHT-C multi-filter photometry versus model predictions
• 6.43. PHT-P and PHT-C absolute photometry versus model predictions of $\gamma$ Dra
• 6.44. PHT-P absolute photometry of Sirius versus model predictions
• 6.45. PHT-P absolute photometry of $\alpha$ Ari versus model predictions
• 6.46. C200 absolute photometry of Uranus versus model predictions
• 6.47. SWS01 observations of stars with different spectral types versus model predictions
• 6.48. SWS01 observations of stars with different brightness versus model predictions
• 6.49. SWS versus model predictions and other observational data for a sample of stars
• 7.1. ISO Data Archive 3-tier architecture
• 7.2. ISO pipeline products Quality Control statistics
• 7.3. ISO Data Archive main query panel
• 7.4. ISO Data Archive query results panel with associated browse products
• 7.5. ISO Data Archive users registration
• 7.6. ISO Data Archive users distribution by country
• 7.7. ISO Data Archive queries
• 7.8. ISO Data Archive active users
• 7.9. ISO Data Archive observations retrieval