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A.3 Infrared Astronomical Calibrators

The absolute flux calibration of three of the four ISO instruments (CAM, PHT - at short wavelengths - and SWS) is based primarily on results from the Ground-Based Preparatory Programme (GBPP, Jourdain de Muizon & Habing 1992, [91]; Hammersley & Jourdain de Muizon 2001, [73]) and of the Cohen, Walker, Witeborn et al. (CWW) absolute calibration programme (Cohen et al. 1992a, [28]; 1992b, [29]; 1995, [31]; 1996, [32] and 1998, [33]), and more recently on detailed models provided by Decin et al. 2002, [41]; 2003a, [42]; 2003b, [43] and 2003c, [44]).

The long wavelength filters of PHT also use planets and asteroids to cover the bright and intermediate part of their dynamic range (Müller & Lagerros 1998, [125]; Griffin & Orton 1993, [64]; Orton 2001, [132]). The absolute flux calibration of LWS is based on Uranus as primary source (Sidher et al. 2001, [150]).

A catalogue of calibration source observations as well as many of the reference models used for the calibration of the four ISO instruments are available on-line at the ISO IDC web site:

http://www.iso.vilspa.esa.es/ $\rightarrow$ ISO Explanatory Library $\rightarrow$ Performance and Calibration.

 


next up previous contents index
Next: B. ISO Scientific Observations Up: A. Infrared Astronomy Previous: A.2 Astronomical Background Radiation
ISO Handbook Volume I (GEN), Version 2.0, SAI/2000-035/Dc