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The properties of magnetic fields at the earliest stages of star
formation are largely unexplored today. We present recent ALMA
polarization observations toward the high-mass starless region
IRDC18310-4 revealing the magnetic field properties toward this very
young region. The polarized emission is clearly detected in four
sub-cores. In general it shows a smooth distribution, also along
elongated cores. Estimating the magnetic field strength via the
Davis-Chandrasekhar-Fermi method, we find comparably large magnetic
field strengths between 0.25 and 1.27mG. Comparing the data to spectral
line observations, the turbulent-to-magnetic energy ratio is low,
indicating that turbulence does not significantly contribute to the
stability of the gas clump. A mass-to-flux ratio >=1 indicates that the
region starts to collapse which is consistent with previous spectral
line analysis of the region.
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