Theoretical brightness temperature profiles of atmospheric pure H2 rotational quadrupole lines - Jupiter and Uranus

With the advent of high-resolution instruments and their use high above most of the telluric water vapor, the hydrogen pure rotational quadrupole lines at 28, 17, and 12 microns from the atmospheres of the outer planets may be observed. Best values for the line strengths, pressure-broadening coefficients, diffusion constants, and pressure shifts for these rotational transitions are calculated. The collisionally narrowed Galatry profile is used to calculate brightness temperature line profiles for these H2 transitions for the outer planets, Jupiter and Uranus. The effects of the H2 rotational-translational continuum and of the NH3 v2 band are also included.