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Determining the importance of magnetic fields in star forming environments ishampered by the difficulty of accurately measuring both field strength and gasproperties in molecular clouds. We post-process three-dimensional non-idealmagnetohydrodynamic simulations of prestellar cores with a time-dependentchemical network, and use radiative transfer modelling to calculateself-consistent molecular line profiles. Varying the initial mass-to-flux ratiofrom sub- to super-critical results in significant changes to both theintensity and shape of several observationally important molecular lines. Weidentify the peak intensity ratio of N$_2$H$^+$ to CS lines, and the CS $J=2-1$blue-to-red peak intensity ratio, as promising diagnostics of the initialmass-to-flux ratio, with N$_2$H$^+$/CS values of $>0.6$ ($<0.2$) and CSblue/red values of $<3$ ($>5$) indicating subcritical (supercritial) collapse.These criteria suggest that, despite presently being magneticallysupercritical, L1498 formed from subcritical initial conditions.

Investigating the role of magnetic fields in star formation using molecular line profiles