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We report on the near-infrared polarimetric observations of G11.11-0.12(hereafter G11) obtained with SIRPOL on the 1.4 m IRSF telescope. The starlightpolarisation of the background stars reveals the on-sky component of magneticfields in G11, and these are consistent with the field orientation observedfrom polarised dust emission at $850\,\mu$m. The magnetic fields in G11 areperpendicular to the filament, and are independent of the filament'sorientation relative to the Galactic plane. The field strength in the envelopeof G11 is in the range $50-100\,\mu$G, derived from two methods. The analysesof the magnetic fields and gas velocity dispersion indicate that the envelopeof G11 is supersonic but sub-Alfv{\'e}nic. The critical mass-to-flux ratio inthe envelope of G11 is close to 1 and increases to $\gtrsim 1$ on the spine ofG11. The relative weights on the importance of magnetic fields, turbulence andgravity indicate that gravity dominates the dynamical state of G11, but withsignificant contribution from magnetic fields. The field strength,$|\mathbf{B}|$, increases slower than the gas density, $n$, from the envelopeto the spine of G11, characterized by $|\mathbf{B}|\propto n^{0.3}$. Theobserved strength and orientation of magnetic fields in G11 imply thatsupersonic and sub-Alfv{\'e}nic gas flow is channelled by the strong magneticfields and is assembled into filaments perpendicular to the magnetic fields.The formation of low-mass stars is enhanced in the filaments with high columndensity, in agreement with the excess of low-mass protostars detected in thedensest regions of G11.

The Role of Magnetic Fields in the Formation of the Filamentary Infrared Dark Cloud G11.11-0.12