SIMBAD references

Context. In the near future, high spatial and spectral infrared (IR) data of star-forming regions obtained by the James Webb Space Telescope may reveal new solid-state features of various species, including more intriguing classes of chemical compounds. The identification of complex organic molecules (COMs) in the upcoming data will only be possible when laboratory IR ice spectra of these species under astronomically relevant conditions are available for comparison. For this purpose, systematic series of laboratory measurements are performed, providing high-resolution IR spectra of COMs. Here, spectra of pure methylamine (CH₃NH₂) and methylamine-containing ices are discussed.
Aims. The work is aimed at characterizing the mid-IR (500-4000cm^–1, 20-2.5µm) spectra of methylamine in pure and mixed ices to provide accurate spectroscopic data of vibrational bands that are most suited to trace this species in interstellar ices.
Methods. Fourier transform infrared spectroscopy is used to record spectra of CH₃NH₂ in the pure form and mixed with H₂O, CH₄, and NH₃, for temperatures ranging from 15 to 160K. The IR spectra in combination with HeNe laser (632.8 nm) interference data of pure CH₃NH₂ ice was used to derive the IR band strengths of methylamine in pure and mixed ices.
Results. The refractive index of amorphous methylamine ice at 15K was determined as being 1.30±0.01. Accurate spectroscopic information and band strength values are systematically presented for a large set of methylamine-containing ices and different temperatures. Selected bands are characterized and their use as methylamine tracers is discussed. The selected bands include the following: the CH₃ antisymmetric stretch band at 2881.3cm^–1 (3.471µm), the CH₃ symmetric stretch band at 2791.9cm^–1 (3.582µm), the CH₃ antisymmetric deformation bands, at 1455.0 and 1478.6cm^–1 (6.873 and 6.761µm), the CH₃ symmetric deformation band at 1420.3cm^–1 (7.042µm), and the CH₃ rock at 1159.2cm^–1 (8.621µm). Using the laboratory data recorded in this work and ground-based spectra of ices toward YSOs (Young Stellar Objects), upper-limits for the methylamine ice abundances are derived. In some of these YSOs, the methylamine abundance is less than 4% relative to H₂O.