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As a novel approach for tracing interstellar magnetic fields, the VelocityGradient Technique (VGT) has been proven to be effective for probing magneticfields in the diffuse interstellar medium (ISM). In this work, we verify theVGT in a broader context by applying the technique to a molecular cloudinteracting with the supernovae remnant (SNR) W44. We probe the magnetic fieldswith the VGT using CO, $\rm HCO^+$, and H I emission lines and make acomparison with the Planck 353 GHZ dust polarization. We show that the VGTgives an accurate measurement that coheres with the Planck polarizationespecially in intense molecular gas emission regions. We further study theforeground's contribution to the polarization that results in a misalignmentbetween the VGT and the Planck measurements in low-intensity molecular gasareas. We advance the VGT to achieve magnetic field tomography by decomposingthe W44 into various velocity components. We show that W44's velocity componentat $v\sim45$ km s$^{-1}$ exhibits the largest coverage and gives the bestagreement with Planck polarization in terms of magnetic field orientation.

Velocity Gradients: Magnetic Field Tomography towards the Supernova Remnant W44