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Context. Infrared spectroscopy of star and planet forming regions is at thedawn of a new age with the upcoming James Webb Space Telescope. In support ofthese observations, laboratory spectra are required to identify complex organicmolecules in the ices that cover the dust grains in these regions.  Aims. This study aims to provide reference spectra to firmly detect icymethyl formate in the different stages of star and planet forming regions.Methyl formate is mixed in astronomically relevant matrices, and the peakpositions, FWHMs, and relative band intensities are characterized for differenttemperatures to provide an analytical tool for astronomers.  Methods. Methyl formate is deposited at 15 K under high-vacuum conditions.Specifically, methyl formate is deposited pure and mixed with CO, H$_2$CO,CH$_3$OH, H$_2$O, and CO:H$_2$CO:CH$_3$OH combined. Throughout the experimentinfrared spectra are acquired with a FTIR spectrometer in the range from4000-500 cm$^{-1}$ (2.5-20 $\mu$m) at a spectral resolution of 0.5 cm$^{-1}$.  Results. We present the characterization of five solid-state methyl formatevibrational modes in pure and astronomically relevant ice matrices. The fiveselected vibrational modes, namely the C=O stretch, C$-$O stretch, CH$_3$rocking, O$-$CH$_3$ stretching, and OCO deformation, are best suited for a JWSTidentification of methyl formate. For each of these vibrational modes, and eachof the mixtures the TvS heatmaps, peak position versus FWHM, and relative bandintensities are given. Additionally, the acquired reference spectra of methylformate are compared with Spitzer observations of HH 46. A tentative detectionof methyl formate provides an upper limit to the column density of$1.7\times10^{17}$ cm$^{-2}$, corresponding to an upper limit relative to waterof $\leq 2.2\%$ and $\leq 40\%$ with respect to methanol.

Infrared spectra of complex organic molecules in astronomically relevant ice matrices. III. Methyl formate and its tentative solid-state detection