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Astron. Astrophys. 315, L60-L63 (1996)

The wavelength calibration and resolution of the SWS*

E.A. Valentijn1,3, H. Feuchtgruber2,3, D.J.M. Kester1, P.R. Roelfsema1,3, P. Barr3, O.H. Bauer2, D.A. Beintema1,3, D.R. Boxhoorn1,3, Th. de Graauw1, L.N. Haser2, A. Heske3, A.M. Heras3, R.O. Katterloher2, F. Lahuis1,3, D. Lutz2, K.J. Leech3, P.W. Morris3,5, A. Salama3, S.G. Schaeidt2,3, H.W.W. Spoon2,5, B. Vandenbussche3,4, E. Wieprecht2,3, W. Luinge1, and K.J. Wildeman1

1 SRON, P.O. Box 800, 9700 AV Groningen, The Netherlands
2 Max-Planck-Institut für extraterrestrische Physik, Postfach 1603, D-85740 Garching, Germany
3 ISO Science Operations Centre, Astrophysics Division of ESA, P.O. Box 50727, E-28080 Villafranca/Madrid, Spain
4 Institute for Astronomy, University of Leuven, B-3001 Heverlee, Belgium
5 SRON, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands

Received 1 August 1996 / Accepted 18 September 1996

Abstract. The laboratory wavelength calibration of the SWS has been succesfully transferred to the in orbit situation. The achieved accuracies for the grating sections are img6.gif . Any remaining errors in the wavelength scale are dominated by uncertainties of the relative position of the target in the img7.gif wide slits. The grating spectral profile is very well represented by a Gaussian shape. The width of the grating spectral profile can be accurately predicted by a theoretical model. The wavelength calibration of the FP's is accurate to within 1/3 of a resolution element, corresponding to img8.gif . The wavelength stability of the gratings and FP is excellent, no measurable changes were found during the first 6 months of the ISO mission.

Key words: wavelength calibration, spectral resolution, infrared spectroscopy

* ISO is an ESA project with instruments funded by ESA Member States (especially the PI countries: France Germany, the Netherlands and the United Kingdom) and with the participation of ISAS and NASA. SWS is a joint project of SRON and MPE (DARA grants no 50 QI9402 3 and 50 QI8610 8) with contributions from KU Leuven, Steward Observatory, and Phillips Laboratory.

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Last change: December 16, 1996
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