The CH3D absorption spectrum in the 1.58 μm transparency window of methane: Empirical line lists at 81 K and 294 K and temperature dependence

In spite of its low isotopic abundance in methane (about 5×10−4), CH3D contributes greatly to the very weak absorption in the 1.58 μm methane transparency window. This methane window deserves to be characterized in details because it is important for planetary applications in particular for Titan and the giant planets. In this work, we recorded the CH3D spectrum by high sensitivity differential absorption spectroscopy (αmin≈5×10−8 cm−1) both at room temperature and at 81 K. A list of more than 9000 lines was constructed from the 81 K spectrum for the 6099-6530 cm−1 region. In order to get the temperature dependence of the line intensities, the low energy values have to be determined. The rovibrational assignments available in the literature provide low energy values for about 380 strong transitions of the region. This is insufficient to characterize the temperature dependence of the CH3D absorption between 6200 and 6400 cm−1. In this interval, a list of 5500 lines was constructed from the room temperature spectrum. The empirical energy values of the transitions were derived from the ratio of the intensities at 81 K and 294 K. The exact and empirical lower state energies included in the final line lists provided as Supplementary Material, allow for accounting for the temperature dependence of the CH3D spectrum in the entire 6099-6530 cm−1 region.Our measurements have been compared to the spectroscopic parameters and assignments available in the literature in particular those adopted in the HITRAN database. Improvements and corrections are proposed for the wavenumber calibration and for some lower state energies.

► Importance of the 1.58 μm transparency window of methane for planetology. ► CH3D, major contributor to the methane absorption in the region. ► Absorption spectrum of CH3D recorded at 81 K and 294 K between 6900 and 7900 cm−1. ► List of about 9000 and 5500 lines constructed from the 81 and 294 K spectra. ► Temperature dependence obtained for most of the CH3D absorption of the region.