Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aj....116.1915h&link_type=abstract
The Astronomical Journal, Volume 116, Issue 4, pp. 1915-1921.
Astronomy and Astrophysics
Astronomy
40
Atlases, Infrared Radiation, Stars: Early-Type, Stars: Fundamental Parameters
Scientific paper
We examine the spectral characteristics of normal OB stars with high-signal-to-noise ratio (>120) H-band (1.6 μm) spectra at a resolution of 2000. We find that several atomic lines vary smoothly with stellar temperature, as first shown by Blum et al. However, we find a previously unreported, significant variation in the strength of some of these lines with stellar luminosity. B supergiant stars show stronger He i and weaker Br 11 as compared with low-luminosity B dwarf stars of the same spectral class. It is for this reason that luminosity class must also be determined to obtain an accurate spectral type for a given star using H-band spectra. We suggest a method for estimating the spectral type and luminosity of an OB star over the wavelength range from 1.66 to 1.72 μm using hydrogen Br 11 at 1.681 mum, He i at 1.700 mum, and He ii at 1.693 mum. The use of the near-infrared spectral range for classification has obvious advantages over optical classification when applied to heavily reddened stars, such as in star-forming regions or deeply embedded lines of sight within the plane of the Galaxy, such as the Galactic center. Furthermore, the H band is less likely to be contaminated by infrared excess emission, which is frequently seen around massive young stellar objects beyond 2 mum.
Hanson Margaret Murray
Luhman Kevin L.
Rieke George H.
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