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tokens: measurement. 4. We claim that VGT–PCA as a modification of the VGT is advantageous in studying the magnetic field morphology and predicting the contribution from the Galactic foreground. Appendix A GALFA-H <sc>i</sc> Data Selection In this work, the ensemble GALFA-H i data is separated into three data sets: East (A), North pole (B), and West (C). Each data set is divided into five individual subregions. The velocity range of each data set is selected, such that the majority of the Galactic neutral hydrogen gas is included. Table 1 gives the description of the GALFA-H i data set used in this work. The uncertainty on the AM is given by the standard error of the mean, i.e., the standard deviation divided by the square root of the sample size. Figures 11 – 16 show the morphology of the POS magnetic fields inferred from Planck polarization and VGT–PCA with resolution ≃1°. Figure 11. The morphology of the POS magnetic fields on the sky patch with (a): R.A. from 240 to 480 and decl. from −12 to 371, and (b): R.A. from 480 to 720 and decl. from −12 to 371. Left: the magnetic field predicted from VGT–PCA (red segments) with resolution ≃1°. Middle: the magnetic fields inferred from Planck polarization (blue segments). Right top: the histogram of the relative orientation between the magnetic field predicted by VGT–PCA and the one inferred from Planck polarization. Right bottom: the variation of the AM with respect to the polarization percentage. Figure 12. The morphology of the POS magnetic fields on the sky patch with (a): R.A. from 720 to 960 and decl. from −12 to 371, and (b): R.A. from 960 to 1200 and decl. from −12 to 371. Left: the magnetic field predicted from VGT–PCA (red segments) with resolution ≃1°. Middle: the magnetic fields inferred from Planck polarization (blue segments). Right top: the histogram of the relative orientation between the magnetic field predicted by VGT–PCA and the one inferred from Planck polarization. Right bottom: the variation of the AM with respect to the polarization percentage. Figure 13. The morphology of the POS magnetic fields on the sky patch with (a): R.A. from 2640 to 2880 and decl. from −12 to 371, and (b): R.A. from 2880 to 3120 and decl. from −12 to 371. Left: the magnetic field predicted from VGT–PCA (red segments) with resolution ≃1°. Middle: the magnetic fields inferred from Planck polarization (blue segments). Right top: the histogram of the relative orientation between the magnetic field predicted by VGT–PCA and the one inferred from Planck polarization. Right bottom: the variation of the AM with respect to the polarization percentage. Figure 14. The morphology of the POS magnetic fields on the sky patch with (a): R.A. from 3120 to 3360 and decl. from −12 to 371, and (b): R.A. from 3360 to 3600 and decl. from −12 to 371. Left: the magnetic field predicted from VGT–PCA (red segments) with resolution ≃1°. Middle: the magnetic fields inferred from Planck polarization (blue segments). Right top: the