M. D. Dyar

TL;DR: Analysis of recent infrared mapping by Chandrayaan-1 and Deep Impact, and reexamining Cassini data obtained during its early flyby of the Moon, Pieters et al. reveal a noticeable absorption signal for H2O and OH across much of the surface, implying that solar wind is depositing and/or somehow forming water and OH in minerals near the lunar surface, and that this trapped water is dynamic.

TL;DR: In this paper, the authors used the coordination of visible/near-infrared reflectance/mid-in infrared reflectance and emissivity spectra of four groups of phyllosilicates to provide insights into the differences within and among groups of smectites, kaolinite serpentines, chlorites and micas.

TL;DR: Higher abundances of chlorinated hydrocarbons in the mudstone compared with Rocknest windblown materials previously analyzed by Curiosity suggest that indigenous martian or meteoritic organic carbon sources may be preserved in the Mudstone; however, the carbon source for the chlorinatedHydrocarbons is not definitively of martian origin.

TL;DR: The absence of predicted geochemical variations indicates that magnetite and phyllosilicates formed by diagenesis under low-temperature, circumneutral pH, rock-dominated aqueous conditions during the early history of Mars.

TL;DR: The first planetary science instrument on the Mars Science Laboratory rover, Curiosity, employed laser-induced breakdown spectroscopy (LIBS) to determine the compositions of geological samples on another planet as mentioned in this paper.