Synthetic spectra of cool stars observed with the Short-Wavelength Spectrometer: improving the models and the calibration of the instrument

Details Synthetic spectra of cool stars observed with the Short-Wavelength Spectrometer: improving the models and the calibration of the instrument Synthetic spectra of cool stars observed with the Short-Wavelength Spectrometer: improving the models and the calibration of the instrument

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000phdt........16d&link_type=abstract

PhD thesis, Catholique University of Leuven, 2000, 337 pages.

Astronomy and Astrophysics

Astronomy

31

Iso-Sws, Calibration, Red Giants, Theoretical Models

Scientific paper

In this work, we present an elaborate study on a sample of cool, mostly bright stars observed with the Short Wavelength Spectrometer (SWS) on-board the Infrared Space Observatory (ISO). The `Instituut voor Sterrenkunde' is part of the consortium of the SWS, and almost all observations in this dissertation are taken with this instrument. These stars were obse rved with the specific aims to achieve an accurate calibration of the SWS spectrometers and to improve model atmospheres for cool stars. To calibrate the ISO-SWS spectrometers accurately, standard stars are observed. In the SWS spectral region, the primary standard calibration candles are bright, mostly cool stars. Since ISO-SWS offered the astronomical community the first opportunity to perform accurate intermediate resolution spectroscopic observations in the infrared spectral window (2.38 - 45.2 micron), our theoretical understanding of cool stellar sources - and more precisely cool stellar atmospheres - is not as refined as it is for hotter sources, which radiate more in the visible spectral window. A full interpretation of the ISO-SWS data will therefore result from an iterative process, in which both better theoretical modeling and more accurate instrumental calibration are involved. Since two years, we have the unique opportunity to use the state-of-the-art MARCS-code developed by the Uppsala group to compute atmospheric models and corresponding synthetic spectra. This code is the most advanced one for the generation of spherically symmetric opacity sampling models for cool stars. The main task of this thesis was to disentangle calibration problems and problems in constructing the model or computing the synthetic spectrum by an in-depth comparison between the ISO-SWS data and corresponding synthetic spectra of these cool stars. The results of this study are implemented in the new version of the calibration files and are used to improve the theoretical atmospheric models.

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