Laboratory mid-IR spectra of equilibrated and igneous meteorites. Searching for observables of planetesimal debris

TL;DR

This study provides new mid-infrared spectra of meteorites to help interpret space telescope data, revealing distinct spectral features that differentiate meteorite types and their parent bodies.

Contribution

The paper introduces a comprehensive set of mid-IR transmission spectra of various meteorites, aiding in the identification of asteroid debris in space observations.

Findings

Distinct spectral differences between meteorite groups

Pyroxene-olivine feature ratio as an identifier

Olivine peak shift indicates iron content

Abstract

Meteorites contain minerals from Solar System asteroids with different properties (like size, presence of water, core formation). We provide new mid-IR transmission spectra of powdered meteorites to obtain templates of how mid-IR spectra of asteroidal debris would look like. This is essential for interpreting mid-IR spectra of past and future space observatories, like the James Webb Space Telescope. We show that the transmission spectra of wet and dry chondrites, carbonaceous and ordinary chondrites and achondrite and chondrite meteorites are distinctly different in a way one can distinguish in astronomical mid-IR spectra. The two observables that spectroscopically separate the different meteorites groups (and thus the different types of parent bodies) are the pyroxene-olivine feature strength ratio and the peak shift of the olivine spectral features due to an increase in the iron concentration of the olivine.