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Waters have been detected from the ground in only a few star-forming regions. Most of these detections have come from the hot cores of massive star-forming regions such as Orion or W49N, which are characterized by unusually high temperatures, and have been attributed to H2O formation either by ablation or grain evaporation and sublimation (e.g. Calioud et al., 2004). As a result of this, studies have focused on the formation of H2O in these environments and the possible formation mechanisms and timescales using infrared observations. The mid-infrared spectrum of some of these sources have also been observed and interpreted in terms of ice chemistry (Caraux et al., 1994; Gerakines et al., 1999; van Dishoeck et al., 2003). However, there is still no clear consensus on the formation of water in the cold interstellar medium. Here we present the spectra of molecular ices in the 10-35· range, as obtained from the CCM models, that include the highly volatile species, such as CO, H2O, HNC, HCO2H, CH2O, CH3OH, NH3. The best agreement with observations in the band range of two of these ices is obtained in the case of CO and water. In contrast, our calculations do not reproduce the observations of CH2O better than about a factor of three, and for the other species the results compare poorly with the observed spectra. We find that the best agreement with the observed spectrum of CO corresponds to a mix between thin and thick ice. This is independent of the settling of the ice mantles, whose effect is to increase the emergent synthetic spectrum. This is a good agreement with the results obtained by the analysis of the shape of the profile of the CO sub-band at about 22·. We have also computed the extinction factors for these species as a function of the grain size and found that, in the case of ice CO and water, the peak at a wavelength of 20· shifts in the expected direction, compared with the pure crystalline form, according to the grain size, whereas for the rest of the species, the peak does not change in the expected wavelength as the grain size increases.
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