A Comparison of Water Vapour Line Lists

Details A Comparison of Water Vapour Line Lists A Comparison of Water Vapour Line Lists

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003csss...12..899j&link_type=abstract

The Future of Cool-Star Astrophysics: 12th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (2001 July 30 - August

Astronomy and Astrophysics

Astrophysics

7

Water, M Dwarfs, Model Atmospheres

Scientific paper

M dwarf spectra, at wavelengths beyond 1.35 μm, are dominated by water vapour yet terrestrial water vapour makes it notoriously difficult to make accurate measurement from ground-based observations. We have used the short wavelength spectrometer on the Infrared Space Observatory to obtain the 2.5--3.0 μm region. The observations show a good match with synthetic spectra based on the Partridge & Schwenke (1997) line list though not with the SCAN (Jorgensen et al. 2001) line list. Nonetheless, the Partridge & Schwenke calculations for water vapour lines still need to be extended to higher energy levels with good convergence for reliable modelling of hot water vapour. Then water bands can assume their natural role as the primary tool for the spectroscopic analysis of M stars.

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