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We derived the dust-to-HI ratio of the intermediate-velocity clouds (IVCs),the high-velocity clouds (HVCs), and the local HI gas, by carrying out amultiple-regression analysis of the 21cm HI emission combined with the sub-mmdust optical depth. The method covers over 80 per cent of the sky contiguouslyat a resolution of 47arcmin and is distinguished from the absorption linemeasurements toward bright galaxies and stars covering a tiny fraction of thesky. Major results include that the ratio of the IVCs is in a range of 0.1--1.5with a mode at 0.6 (relative to the solar-neighbourhood value, likewise below)and that a significant fraction, ~20 per cent, of the IVCs include dust-poorgas with a ratio of <0.5. It is confirmed that 50 per cent of the HVC Complex Chas a ratio of <0.3, and that the Magellanic Stream has the lowest ratio with amode at ~0.1. The results prove that some IVCs have low metallicity gas,contrary to the previous absorption line measurements. Considering that therecent works show that the IVCs are interacting and exchanging momentum withthe high-metallicity Galactic halo gas, we argue that the high-metallicity gascontaminates a significant fraction of the IVCs. Accordingly, we argue that theIVCs include a significant fraction of the low metallicity gas supplied fromoutside the Galaxy as an alternative to the Galactic-fountain model.

Dust-to-neutral gas ratio of the intermediate and high velocity HI clouds derived based on the sub-mm dust emission for the whole sky