ISO-SWS calibration and the accurate modelling of cool-star atmospheres - IV. G9 to M2 stars
Astron.Astrophys.400:709-728,2003 presented. The 2.38 -- 4.08 micron wavelength-range of band 1 of ISO-SWS (Short-Wavelength Spectrometers on board of the Infrared Space Observatory) in which many different molecules -- with their own dependence on each of the stellar parameters -- are absorbing, en...
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Zusammenfassung: | Astron.Astrophys.400:709-728,2003 presented. The 2.38 -- 4.08 micron wavelength-range of band 1 of ISO-SWS
(Short-Wavelength Spectrometers on board of the Infrared Space Observatory) in
which many different molecules -- with their own dependence on each of the
stellar parameters -- are absorbing, enables us to estimate the effective
temperature, the gravity, the microturbulence, the metallicity, the
CNO-abundances, the 12C/13C-ratio and the angular diameter from the ISO-SWS
data. Using the Hipparcos' parallax, the radius, luminosity and
gravity-inferred mass are derived. The stellar parameters obtained are in good
agreement with other published values, though also some discrepancies with
values deduced by other authors are noted. For a few stars (Delta Dra, Xi Dra,
Alpha Tuc, H Sco and Alpha Cet) some parameters -- e.g. the CNO-abundances --
are derived for the first time. By examining the correspondence between
different ISO-SWS observations of the same object and between the ISO-SWS data
and the corresponding synthetic spectrum, it is shown that the relative
accuracy of ISO-SWS in band 1 (2.38 -- 4.0 micron) is better than 2% for these
high-flux sources. The high level of correspondence between observations and
theoretical predictions, together with a confrontation of the estimated
Teff(ISO) value with Teff-values derived from colours -- which demonstrates the
consistency between V-K, BC(K), Teff and the angular diameter derived from
optical or IR data -- proves that both the used MARCS models to derive the
stellar quantities and the flux calibration of the ISO-SWS detectors have
reached a high level of reliability. |
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DOI: | 10.48550/arxiv.astro-ph/0207653 |