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We found that an intermediate velocity cloud (IVC) IVC 86-36 in HI 21 cmemission shows a head-tail distribution toward the Galactic plane with markedparallel filamentary streamers, which is extended over 40 degrees in the sky.The distance of IVC 86-36 is constrained to be less than ~3 kpc from absorptionof a background star as determined from opticalspectroscopy. There is a bridgefeature in velocity between the IVC and the local ISM with velocity separationof ~50 km s-1, which may indicate dynamical interaction of the IVC with thedisk. If the interaction is correct, the distance estimate d of the IVC rangesfrom 200 pc to 3 kpc, and the mass of the IVC head is estimated to be7X103(d/1kpc)2Msol. The IVC shares similar properties to the Smith cloudlocated at 12 kpc, including the head-tail distribution, streamers, and bridgefeature, while the mass of the IVC is less than ~0.1 of the Smith cloud. Acomparison between the Hi and the Planck/IRAS dust emission indicates that thedust emission of IVC 86-36 is not detectable in spite of its HI column densityof 2X10^20 cm-2, indicating low metalicity of IVC 86-36 by a factor of ~< 0.2as compared with the solar neighbor. We conclude that IVC 86-38 is an infallingcloud which likely originated in the low-metallicity environment of theGalactic halo or the Magellanic system.

An Intermediate Velocity HI Cloud Falling to the Galactic Disk; Possible Evidence for Low Metallicity HI Gas Originated Outside the Galactic Disk