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The ISO-SWS flux standard stars: synthetic spectra and observations

Published online by Cambridge University Press:  25 May 2016

N.S. van der Bliek ,
P.W. Morris ,
B. Vandenbussche ,
L.B.F.M. Waters ,
P. Zaal ,
R.A. Bell ,
B. Gustafsson ,
K. Eriksson  and
Th. de Graauw
N.S. van der Bliek
Affiliation:
Sterrewacht Leiden, The Netherlands
P.W. Morris
Affiliation:
SRON Utrecht, The Netherlands
B. Vandenbussche
Affiliation:
Instituut voor Sterrenkunde, K. U. Leuven, Belgium
L.B.F.M. Waters
Affiliation:
Sterrenkundig Instituut Amsterdam, The Netherlands
P. Zaal
Affiliation:
Sterrenkundig Instituut Amsterdam, The Netherlands
R.A. Bell
Affiliation:
Astronomy Department, University of Maryland, USA
B. Gustafsson
Affiliation:
Uppsala Observatory, Sweden
K. Eriksson
Affiliation:
Uppsala Observatory, Sweden
Th. de Graauw
Affiliation:
SRON Groningen, The Netherlands

Extract

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We present flux-calibrated, synthetic spectra for the calibration stars of the Short Wavelength Spectrometer of the Infrared Space Observatory ISO-SWS (cf. Kessler et al. 1996). ISO-SWS covers a wavelength range of 2.4 to 45 μm (cf. de Graauw et al. 1996), and although in the NIR the flux calibration of Vega can be used, at longer wavelengths the flux calibration has to be extrapolated by other means, because (i) Vega has at λ ≥ 25 μm an IR excess due to circumstellar dust and (ii) there is an, as yet, unresolved controversy about Vega's flux at 10 μm (cf. Rieke et al. 1985). The majority of the standard stars of SWS are of MK class G and K III, as cool giants are amongst the brightest objects in the IR, and model atmospheres for cool giants are available and well-studied (cf. Jørgensen and Gustafsson 1994).

Type
Stellar Flux Distributions
Information
Symposium - International Astronomical Union , Volume 189: Fundamental Stellar Properties: The Interaction Between Observation and Theory , 1997 , pp. 89 - 92
Copyright
Copyright © Kluwer 1997 

References

Bell, R.A. 1993, MNRAS 264, 345 Google Scholar
Bell, R.A., Gustafsson, B. 1989, MNRAS 236, 653 CrossRefGoogle Scholar
de Graauw, T., et al. 1996, A&A 315, L49 Google Scholar
Dreiling, L.A., Bell, R.A. 1980, ApJ 241, 736 Google Scholar
Gustafsson, B., Bell, R.A., Eriksson, K., Nordlund, Å. 1975, A&A 42, 407 Google Scholar
Kessler, M.F., et al. 1996, A&A 315, L27 Google Scholar
Mégessier, C. 1995, A&A 296, 771 (M95) Google Scholar
Rieke, G.H., Lebofsky, M.J., Low, F.J. 1985, AJ 90, 900 CrossRefGoogle Scholar
Schaeidt, S.G., et al. 1996, A&A 315, L55 Google Scholar
van der Bliek, N.S., Gustafsson, B., Eriksson, K. 1996, A&A 309, 849 Google Scholar