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The increasing sensitivity and resolution of ground-based telescopes have enabled the detection of gas-phase complex organic molecules (COMs) across a variety of environments. Many of the detected species are expected to form on the icy surface of interstellar grains and transfer later into the gas phase. Therefore, icy material is regarded as a primordial source of COMs in the ISM. Upcoming JWST observations of interstellar ices in star-forming regions will reveal IR features of frozen molecules with unprecedented resolution and sensitivity. To identify COM features in the JWST data, lab IR spectra of ices for conditions that simulate interstellar environments are needed. This work presents FTIR spectra (500-4000 cm$^{-1}$/20-2.5$\mu$m, with a resolution of 1 cm$^{-1}$) of methyl cyanide (CH$_3$CN, aka acetonitrile) mixed with H$_2$O, CO, CO$_2$, CH$_4$, and NH$_3$, at temperatures from 15-150 K. The refractive index of pure amorphous CH$_3$CN ice at 15K and the band strength, peak position, and FWHM of selected IR bands are also measured. These bands are: the CH$_3$ sym stretching at 2940.9 cm$^{-1}$, the CN stretching at 2252.2 cm$^{-1}$, a combination of modes at 1448.3 cm$^{-1}$ , the CH$_3$ antisym def. at 1410 cm$^{-1}$ , the CH$_3$ sym def. at 1374.5 cm$^{-1}$, and the CH$_3$ rock at 1041.6 cm$^{-1}$. The lab spectra of CH$_3$CN are compared to observations of ices toward W33A and three low-mass YSOs. Since an unambiguous identification of CH$_3$CN is not possible, upper limits for the CH$_3$CN column density are determined as $\leq 2.4\times 10^{17}$ molecules cm$^{-2}$ for W33A and $5.2 \times 10^{16}$, $1.9\times 10^{17}$, and $3.8\times 10^{16}$ molecules cm$^{-2}$ for EC92, IRAS 03235, and L1455 IRS3, respectively. W.r.t solid H$_2$O, these values correspond to relative abundances of 1.9, 3.1, 1.3, and 4.1\%, for W33A, EC92, IRAS 03235, and L1455 IRS3, respectively., Comment: 26 pages, 11 figures, accepted for publication in A&A