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Asymptotic Giant Branch (AGB) stars are major contributors of cosmic dust tothe universe. Typically, dust around AGB stars is investigated via radiativetransfer (RT) modeling, or via simple deconstruction of observed spectra.However, methodologies applied vary. Using archival spectroscopic, photometric,and temporal data for the archetypal dusty star, Mira, we identify itscircumstellar silicate dust grains. This is achieved by matching the positionsand widths of observed spectral features with laboratory data. To do thiscomparison properly, it is necessary to account for the continuum emission.Here we investigate various ways in which a continuum is eliminated fromobservational spectra and how it affects the interpretation of spectralfeatures. We find that while the precise continuum shapes and temperatures donot have a critical impact on the positions and shapes of dust spectralfeatures, it is important to eliminate continua in a specific way. It isimportant to understand what contributes to the spectrum in order to remove thecontinuum in a way that allows comparison with laboratory spectra of candidatedust species. Our methodologies are applicable to optically thin systems, likethat of Mira. Higher optical depths will require RT modeling, which cannotinclude many different potential astrominerals because there is a lack ofcomplex refractive indices. Finally, we found that the classic silicate featureexhibited by Mira is not consistent with a real amorphous silicate alone butmay be best explained with a small alumina contribution to match the observedFWHM of the 10 micron feature.

The Effect of Continuum Elimination in Identifying Circumstellar Dust around Mira