ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O B-Instrument O B-Instrument O O O O O O O O O O O O O O O O O O O O O O B-Telescope O O B-Telescope O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Telescope O O B-Instrument O B-Instrument O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Software B-Citation I-Citation I-Citation I-Citation O O O O O O B-CelestialObject O O O O O B-Software O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O B-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O B-Model O O O O B-Model I-Model O O O O O O O O B-Wavelength I-Wavelength I-Wavelength O O O O O O O O O O O O O B-Wavelength I-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O B-Telescope O B-Telescope O O O O O O O O O O B-Instrument O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O B-Wavelength I-Wavelength I-Wavelength O O O O O O B-Wavelength I-Wavelength I-Wavelength O O O B-Telescope O O O B-Wavelength I-Wavelength I-Wavelength O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Telescope B-Tag I-Tag I-Tag I-Tag I-Tag I-Tag I-Tag O O O O B-Wavelength I-Wavelength I-Wavelength O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O
tokens: et al. 2009 )). This provides a framework on which to interpret the line fluxes in a quantitative manner in Section 4 . The EXES and TEXES spectra contain contributions from the stellar photosphere, inner CSE outflow, and large scale optically thin wind dust emission. Allowing for image quality (SOFIA) and diffraction (IRTF) and the angular size of the emission, the relatively compact line and extended dust emission experience different throughput losses at the slit. Model differential corrections combined with ISO fluxes provide EXES and TEXES flux spectra, which we expect to be accurate to ±30%. Line profile shifts and distortions can arise from features in the underlying photospheric continuum, so we simulated the photospheric component using MARCS (Gustafsson et al. 2008 ) model atmospheres ( K, , solar abundances, 15 macroturbulence) using the BSYN code in a similar manner to Ryde et al. ( 2002 ; see references therein). The synthetic spectrum for the K is rather featureless, except for weak absorption features 5% below continuum level. However, there is not a good understanding of the mid-IR photospheric spectra of luminous cool evolved stars (see, for example, Sloan et al. 2015 and Ryde et al. 2015 ). Inspired by Ryde et al. ( 2006a , 2006b ), we examined a model for K, and this spectra showed deeper absorption features at the 20% level. Taking into account the accuracy of the Barber et al. ( 2006 ) H 2 O line list used in the synthetic spectra, we added Gaussian emission profiles at different wavelengths to the synthetic spectra; convolved them with the instrumental Line Spread Function (LSF), which is assumed to be Gaussian; and then performed a Gaussian fit to the resulting profiles. We found that at 25.99 μ m, centroid velocity shifts only occurred at the percent of a level, while near 17.4 μ m we found that the underlying H 2 O features induced a redshift of up to ∼0.4 to the emission. Close to the [Fe ii ] lines, photospheric water lines are the strongest features. The observed line profiles of Betelgeuse from SOFIA-EXES and IRTF-TEXES are shown in Figures 3 and 4 , and a TEXES observation of α Sco is shown in Figure 5 . The line profile measurements are summarized in Table 3 . We discuss the [Fe ii ] 25.99 and 17.94 μ m lines first, and the non-detections of 22.9 μ m last. Figure 3. SOFIA-EXES [Fe ii ] 25.99 μ m spectrum from α Ori. The blueshifted emission that is well separated from the telluric contamination near . The Callisto spectrum is shown below. Table 3 Observed [Fe ii ] Line Properties Note. a Residual contamination after division by telluric calibrator, leading to additional uncertainties at the 1 level. 3.1. SOFIA-EXES: <inline-formula> <tex-math> </tex-math> <inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa566fieqn153.gif"></inline-graphic> </inline-formula> Figure 3 shows the 25.99 μ m spectrum for α Ori, which is cleanly separated from the telluric feature, as confirmed by the