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M.M. Hanson (Cincinnati), M.A. Kenworthy (Steward Observatory), J. Puls (Universitäts-Sternwarte München), R.-P. Kudritzki, A.T. Tokunaga (Institute for Astronomy)
We present new, high-resolution, near-infrared spectroscopy of three dozen O and early-B stars. The spectra cover most of the wavelength range between 1.62 \mum to 2.2 \mum and includes the most prominent lines of Hydrogen, Helium (both neutral and ionized) as well as three important metal lines in the H- and K-band region. These spectra have more than 4 times the resolution and 2-3 times the signal-to-noise of the the original O and B star spectral atlases of Hanson, Conti, and Rieke (1996) and Hanson, Rieke, and Luhman (1998). Our interest in obtaining higher resolution and signal-to-noise spectra was to aide in the development of quantitative spectroscopic analysis at near-infrared wavelengths which members in our group are carrying out. The new spectra obtained in this study are of high enough quality to allow for direct modeling of the line profiles to constrain effective temperature, gravity, rotational velocity and general wind characteristics. The development of atmospheric modeling routines for the near-infrared regime is fundamental to constraining the nature of heavily embedded and distant O and B stars presently being located throughout the disk of our Galaxy via deep near-infrared imaging surveys (2MASS, DENIS, MSX, GLIMPSE, etc). These results are based upon work supported by the National Science Foundation under Grant No.\ 0094050 to the University of Cincinnati.
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Bulletin of the American Astronomical Society, 36 #2
© YEAR. The American Astronomical Soceity.