The first ISO workshop on analytical spectroscopy with SWS, LWS, PHT-S and CAM-CVF

(Oct 6-8, 1997, Madrid, Spain)

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Comparison between ISO-SWS observations and synthetic spectra of K and M giants

L. Decin1 - C. Waelkens 1 - B. Gustafsson 2 - K. Eriksson 2 - B. Plez 2,3 - J. Sauval 4

1 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200B, B-3000 Leuven, Belgium -
2 Astronomiska observatoriet, Box 515, S-75120 Uppsala, Sweden -
3 Atomspektroskopi, Fysika institution, Box 118, S-22100, Lund, Sweden -
4 Observatoire Royal de Belgique, Avenue Circulaire 3, B-1180 Bruxelles, Belgium

The photometric absolute calibration of ISO-SWS is reliable up to 30% and the relative calibration up to 10%. To judge the obtained ISO-SWS spectra on their reliability, we compare them with synthetic spectra.

The detailed comparison between the ISO-SWS data for the K2III giant tex2html_wrap_inline28 Boo and the M2.5III giant tex2html_wrap_inline30 Peg and the synthetic spectra generated by the use of the new Uppsala models (Plez et al., 1992; Plez et al., 1993) give us not only an indication on the still remaining ISO-SWS calibration problems, but also on the shortcomings of the synthetic spectra. Constructing a stellar model and generating a synthetic spectrum require a detailed knowledge of the stellar atmosphere, but an accurate physical description of the atmosphere of cool giants is still lacking. We hope that our results will not only contribute to a better convergence between the ISO-SWS data and the generated synthetic spectra, but also to a better understanding of the atmospheres of cool giants.

tex2html_wrap_inline28 Boo and tex2html_wrap_inline30 Peg

Postscript version