The c2d Spitzer Spectroscopic Survey of Ices Around Low-mass Young Stellar Objects. IV. NH3 and CH3OH

NH₃ and CH₃OH are key molecules in astrochemical networks leading to the formation of more complex N- and O-bearing molecules, such as CH₃CN and CH₃OCH₃. Despite a number of recent studies, little is known about their abundances in the solid state. This is particularly the case for low-mass protostars, for which only the launch of the Spitzer Space Telescope has permitted high-sensitivity observations of the ices around these objects. In this work, we investigate the ~8-10 μm region in the Spitzer IRS (InfraRed Spectrograph) spectra of 41 low-mass young stellar objects (YSOs). These data are part of a survey of interstellar ices in a sample of low-mass YSOs studied in earlier papers in this series. We used both an empirical and a local continuum method to correct for the contribution from the 10 μm silicate absorption in the recorded spectra. In addition, we conducted a systematic laboratory study of NH₃- and CH₃OH-containing ices to help interpret the astronomical spectra. We clearly detect a feature at ~9 μm in 24 low-mass YSOs. Within the uncertainty in continuum determination, we identify this feature with the NH₃ ν₂ umbrella mode and derive abundances with respect to water between ~2% and 15%. Simultaneously, we also revisited the case of CH₃OH ice by studying the ν₄ C-O stretch mode of this molecule at ~9.7 μm in 16 objects, yielding abundances consistent with those derived by Boogert et al. based on a simultaneous 9.75 and 3.53 μm data analysis. Our study indicates that NH₃ is present primarily in H₂O-rich ices, but that in some cases, such ices are insufficient to explain the observed narrow FWHM. The laboratory data point to CH₃OH being in an almost pure methanol ice, or mixed mainly with CO or CO₂, consistent with its formation through hydrogenation on grains. Finally, we use our derived NH₃ abundances in combination with previously published abundances of other solid N-bearing species to find that up to 10%-20% of nitrogen is locked up in known ices.