5. Calibration and Performance

• 5.1 Introduction
• 5.2 Absolute Flux Calibration and Grating Relative Response
  • 5.2.1 Absolute flux calibration
  • 5.2.2 Relative spectral response function
• 5.3 Fabry-Pérot Flux Calibration
• 5.4 Dark Current Determination
• 5.5 In-orbit Sensitivity of the LWS - Detector Performance
• 5.6 Photometric Accuracy
  • 5.6.1 Calibration sources used for photometric purposes
  • 5.6.2 LWS photometric stability checked with observations of Mars
  • 5.6.3 Comparison with IRAS fluxes
  • 5.6.4 Checking the Fabry-Pérot photometric accuracy
• 5.7 The Strong Source Correction
  • 5.7.1 The reason for the correction
  • 5.7.2 The correction
  • 5.7.3 Future
• 5.8 Quarter-Second Processing
  • 5.8.1 LW5: quarter- versus half-second processing
  • 5.8.2 Summary of processing for various strength sources
• 5.9 Instrumental Field of View: The Beam Profile
  • 5.9.1 The beam profile
  • 5.9.2 Asymmetry
  • 5.9.3 Flux correction for extended sources
  • 5.9.4 Extended source flux per unit area
  • 5.9.5 Effect of the ISO PSF at large distances: check of the straylight around Jupiter
• 5.10 Grating Wavelength Calibration
  • 5.10.1 Basic principles and calibration strategy
  • 5.10.2 Calibration sources and types of observations
  • 5.10.3 Detector angles
  • 5.10.4 Time dependence
  • 5.10.5 Assessment of the achieved wavelength accuracy
• 5.11 Grating Resolution and Characterisation of the Line
  Profiles
  • 5.11.1 Preparation of the data
  • 5.11.2 Stability of the line profiles
  • 5.11.3 Characteristics of the profiles. Comparison to Gaussians.
  • 5.11.4 Effect of a lower spectral sampling
• 5.12 Fabry-Pérot Wavelength Calibration
  • 5.12.1 Introduction
  • 5.12.2 Strategy of calibration
  • 5.12.3 Calibration for OLP Version 10
  • 5.12.4 Monitoring the Fabry-Pérot wavelength calibration
  • 5.12.5 Fabry-Pérot wavelength accuracy
• 5.13 Fabry-Pérot Resolution and Line Profiles
• 5.14 Accuracy of the Parallel and Serendipity Mode Calibration
  • 5.14.1 Prime mode observations coincident with parallel observations
  • 5.14.2 Comparison with prime mode from stabilisation periods
  • 5.14.3 Comparison between overlapping parallel rasters
  • 5.14.4 Comparison with other instruments