Optical Constants of Ices Important to Planetary Science From Laboratory Reflectance Spectroscopy

Laboratory-derived optical constants are essential for identifying ices and measuring their relative abundances on Solar System objects. Almost all optical constants of ices important to planetary science come from experiments with transmission geometries. Here, we describe our new experimental setup and the modification of an iterative algorithm in the literature to measure the optical constants of ices from experiments with reflectance geometries. We apply our techniques to CH4 ice and H2O ice samples and find good agreement between our values and those in the literature, except for one CH4 band in the literature that likely suffers from saturation. The work we present here demonstrates that labs with reflectance geometries can generate optical constants essential for the proper analysis of near- and mid-infrared spectra of outer Solar System objects such as those obtained with the James Webb Space Telescope

Optical Constants of Ices Important to Planetary Science From Laboratory Reflectance Spectroscopy

Laboratory-derived optical constants are essential for identifying ices and measuring their relative abundances on Solar System objects. Almost all optical constants of ices important to planetary science come from experiments with transmission geometries. Here, we describe our new experimental setup and the modification of an iterative algorithm in the literature to measure the optical constants of ices from experiments with reflectance geometries. We apply our techniques to CH4 ice and H2O ice samples and find good agreement between our values and those in the literature, except for one CH4 band in the literature that likely suffers from saturation. The work we present here demonstrates that labs with reflectance geometries can generate optical constants essential for the proper analysis of near- and mid-infrared spectra of outer Solar System objects such as those obtained with the James Webb Space Telescope

Laboratory Measurement of Volatile Ice Vapor Pressures With a Quartz Crystal Microbalance

Nitrogen, carbon monoxide, and methane are key materials in the far outer Solar System where their high volatility enables them to sublimate, potentially driving activity at very low temperatures. Knowledge of their vapor pressures and latent heats of sublimation at relevant temperatures is needed to model the processes involved. We describe a method for using a quartz crystal microbalance to measure the sublimation flux of these volatile ices in the free molecular flow regime, accounting for the simultaneous sublimation from and condensation onto the quartz crystal to derive vapor pressures and latent heats of sublimation. We find vapor pressures to be somewhat lower than previous estimates in literature, with carbon monoxide being the most discrepant of the three species, almost an order of magnitude lower than had been thought. These results have important implications across a variety of astrophysical and planetary environments