EDP Sciences
Free access
Volume 414, Number 2, February I 2004
Page(s) 677 - 697
Section Formation and evolution of planetary systems
DOI http://dx.doi.org/10.1051/0004-6361:20031579

A&A 414, 677-697 (2004)
DOI: 10.1051/0004-6361:20031579

On the analysis of band 3 of the ISO-SWS calibration sources

R. Van Malderen1, L. Decin1, D. Kester2, B. Vandenbussche1, C. Waelkens1, J. Cami3 and R. F. Shipman2

1  Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium
2  Space Research Organization Netherlands, PO Box 800, 9700 AV Groningen, The Netherlands
3  NASA Ames Research Center, Mail Stop 245-6, Moffett Field, CA 94035-1000, USA

(Received 2 January 2003 / Accepted 2 October 2003 )

We analyse ISO-SWS 01 ( $R \sim 1500$) $12{-}27.5\,\mu$m (band 3) spectra of the 10 standard calibration stars with the highest flux using synthetic spectra generated from (MARCS) atmosphere models. The comparison between the observed and synthetic spectra reveals the quality of (1) the atmospheric model construction and subsequent synthetic spectra computation and of (2) the (OLP 10.1) calibration and data reduction of the spectrometer at these wavelengths.

The models represent the general features of the observations, but the synthetic spectrum computation is hampered by the lack of comprehensive molecular and atomic line lists. We also suspect some problems with the temperature distribution in the outer layers of the model and inaccuracies in the extrapolation of the collision-induced absorption coefficients of H 2 pairs. We detect baseline ripples and fringes in the observed spectra, that survive the calibration and detailed reduction process. Photometric calibration uncertainties are estimated by means of the scaling factors between the synthetic and observed spectra.

Key words: stars: atmospheres -- stars: fundamental parameters -- instrumentation: spectrographs -- molecular data

Offprint request: R. Van Malderen, Roeland.VanMalderen@ster.kuleuven.ac.be

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