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C. DI LAURO, F. LATTANZI, Dipartimento di Chimica Farmaceutica e Tossicologia, Università di Napoli Federico II , I-80131 Naples, Italy; K. SUNG, L. R. BROWN, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA; J. VANDER AUWERA, Service de Chimie Quantique et Photophysique, Université Libre de Bruxelles, CP 160/09, 50 avenue F.D. Roosevelt, B-1050 Brussels, Belgium; A. W. MANTZ, Dept. of Physics, Astronomy and Geophysics, Connecticut College, New London, CT 06320, USA; M. A. H. SMITH, Science Directorate, NASA Langley Research Center, Hampton, VA 23681, USA.
Building upon our previous contributions, we are re-investigating the ethane spectrum between 1330 and 1610 cm-1. For this, spectral data were obtained at room and cold (130 K) temperatures with two Bruker Fourier transform spectrometers (at 0.002 cm-1 resolution in Brussels and at 0.003 cm-1 resolution in Pasadena). Over 3300 lines were assigned to
6,
8,
4+
12 and 2
4+
9 cold bands, and one hot band (
4+
8-
4). Note that
6,
8,
9, and
12 are near 1379, 1472, 823, and 1195 cm-1, respectively, and
4 is the torsional mode near 289 cm-1. Our new analysis includes an improved implementation of the theoretical Hamiltonian needed to interpret the very complex spectral structures caused by numerous interactions between these 5 vibrational modes. From this, an empirical line list of positions and estimated intensities is being generated for planetary applications.