EDP Sciences
Free Access
Volume 390, Number 3, August II 2002
Page(s) 1033 - 1048
Section Formation, structure and evolution of stars
DOI https://doi.org/10.1051/0004-6361:20020767
Published online 14 August 2002

A&A 390, 1033-1048 (2002)
DOI: 10.1051/0004-6361:20020767

The ISO-SWS post-helium atlas of near-infrared stellar spectra

B. Vandenbussche1, D. Beintema2, T. de Graauw2, L. Decin1, H. Feuchtgruber3, A. Heras4, D. Kester2, F. Lahuis2, A. Lenorzer5, R. Lorente6, A. Salama6, C. Waelkens1, L. Waters1, 5 and E. Wieprecht3

1  Instituut voor Sterrenkunde, K.U.Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium
2  SRON National Institute for Space Research, Groningen, The Netherlands
3  Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany
4  Astrophysics Missions Division, Research and Scientific Support Department of ESA, ESTEC, PO Box 299, 2200 AG Noordwijk, The Netherlands
5  Sterrenkundig Instituut "Anton Pannekoek", Amsterdam, The Netherlands
6  ISO Data Center, Astrophysics Division of ESA, Villafranca del Castillo, Spain

(Received 11 March 2002 / Accepted 15 May 2002 )

We present an atlas of near-infrared spectra (2.36  $\mu$m-4.1  $\mu$m) of ~300 stars at moderate resolution ( $\lambda$/ $\delta~\lambda \approx 1500$-2000). The spectra were recorded using the Short-Wavelength Spectrometer aboard the Infrared Space Observatory (ISO-SWS). The bulk of the observations were performed during a dedicated observation campaign after the liquid helium depletion of the ISO satellite, the so-called post-helium programme. This programme was aimed at extending the MK-classification to the near-infrared. Therefore the programme covers a large range of spectral types and luminosity classes. The 2.36  $\mu$m-4.05  $\mu$m region is a valuable spectral probe for both hot and cool stars. H I lines (Bracket, Pfund and Humphreys series), He I and He II lines, atomic lines and molecular lines (CO, H 2O, NH, OH, SiO, HCN, C 2H 2, ...) are sensitive to temperature, gravity and/or the nature of the outer layers of the stellar atmosphere (outflows, hot circumstellar discs, etc.). Another objective of the programme was to construct a homogeneous dataset of near-infrared stellar spectra that can be used for population synthesis studies of galaxies. At near-infrared wavelengths these objects emit the integrated light of all stars in the system. In this paper we present the dataset of post-helium spectra completed with observations obtained during the nominal operations of the ISO-SWS. We discuss the calibration of the SWS data obtained after the liquid helium boil-off and the data reduction. We also give a first qualitative overview of how the spectral features in this wavelength range change with spectral type. The dataset is scrutinised in two papers on the quantitative classification of near-infrared spectra of early-type stars (Lenorzer et al. 2002) and late-type stars (Vandenbussche et al., in prep).

Key words: stars: general -- infrared: stars -- atlases

Offprint request: B. Vandenbussche, Bart.Vandenbussche@ster.kuleuven.ac.be

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