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We employ CaII K and NaI D interstellar absorption-line spectroscopy ofearly-type stars in the Large and Small Magellanic Clouds to investigate thelarge- and small-scale structure in foreground Intermediate and High VelocityClouds (I/HVCs). These data include FLAMES-GIRAFFE CaII K observations of 403stars in four open clusters, plus FEROS or UVES spectra of 156 stars in the LMCand SMC. The FLAMES observations are amongst the most extensive probes to dateof CaII structures on 20 arcsec scales  From the FLAMES data within a 0.5 degree field-of-view, the CaII K equivalentwidth in the I/HVC components towards three clusters varies by factors of >10.There are no detections of molecular gas in absorption at intermediate or highvelocities, although molecular absorption is present at LMC and Galacticvelocities towards some sightlines. The sightlines show variations in EWexceeding a factor 7 in CH+ towards NGC 1761 over scales of less than 10arcminutes.  The FEROS/UVES data show CaII K I/HVC absorption in $\sim$60 per cent ofsightlines. No NaI D is found at non-Magellanic HVC velocities aside from atentative detection towards the star LHA 120-S 93. The range in the CaII/NaIratio in I/HVCs is from -0.45 to +1.5 dex, similar to previous measurements forI/HVCs.  In ten sightlines we find CaII/OI ratios in I/HVC gas ranging from 0.2 to 1.5dex below the solar value, indicating either dust or ionisation effects. Innine sightlines I/HVC gas is detected in both HI and CaII, and shows similarCaII/HI ratios to typical I/HVCs, and similar velocities, implying that inthese sightlines the two elements form part of the same structure.

Large and small-scale structure of the Intermediate and High Velocity Clouds towards the LMC and SMC