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We present the highest-resolution study to date of the ISM in galaxiesundergoing ram pressure stripping, using HST BVI imaging of NGC 4522 and NGC4402, Virgo Cluster spirals that are well-known to be experiencing ICM rampressure. We find that throughout most of both galaxies, the main dust lane hasa fairly well-defined edge, with a population of GMC-sized (tens- tohundreds-of-pc scale), isolated, highly extincting dust clouds located up to~1.5 kpc radially beyond it. Outside of these dense clouds, the area has littleor no diffuse dust extinction, indicating that the clouds have decoupled fromthe lower-density ISM material that has already been stripped. Several of thedust clouds have elongated morphologies that indicate active ram pressure,including two large (kpc-scale) filaments in NGC 4402 that are elongated in theprojected ICM wind direction. We calculate a lower limit on the HI + H_2 massesof these clouds based on their dust extinctions and find that a correctionfactor of ~10 gives cloud masses consistent with those measured in CO forclouds of similar diameters, probably due to the complicating factors offoreground light, cloud substructure, and resolution limitations. Assuming thatthe clouds' actual masses are consistent with those of GMCs of similardiameters (~10^4-10^5 M_sun), we estimate that only a small fraction (~1-10%)of the original HI + H_2 remains in the parts of the disks with decoupledclouds. Based on H-alpha images, a similar fraction of star formation persistsin these regions, 2-3% of the estimated pre-stripping star formation rate. Wefind that the decoupled cloud lifetimes may be up to 150-200 Myr.

HST Imaging of Decoupled Dust Clouds in the Ram Pressure Stripped Virgo Spirals NGC 4402 and NGC 4522