How did you deconvolute the overlapping EELS signals at the O-K edge to reliably distinguish between molecular O₂, SiO, and other oxygen-bearing species within vesicles, given the limited energy resolution of 0.5–0.7 eV and the lack of shown reference spectra for these specific gas phases?
Can you provide the quantitative iron content (wt% or at%) of the adjacent K-rich glass phase in the multiphase clast to substantiate the claim that the absence of npFe is due to phase-dependent decomposition rather than simply a lack of available iron?
How did your thermodynamic equilibrium calculations account for the dynamic, non-equilibrium conditions of micrometeorite impacts, including transient heating/cooling rates and possible kinetic barriers to olivine decomposition at the grain surface?
What specific microstructural criteria (e.g., vesicle morphology, interface structure, or spatial correlation with other features) were used to conclusively attribute the vesicles within npFe to decomposition-derived gas trapping rather than to radiation-induced void formation or solar wind implantation artifacts?
Do you have any quantitative spectral data or optical modeling results to demonstrate that the relatively large (10–35 nm) npFe particles you observed contribute to the characteristic reddening and darkening effects, and how do you reconcile their presence with the established dominance of ~3 nm vapor-deposited npFe in lunar space weathering spectra?
