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We present images from the Solar Blind Channel on HST that resolve hundredsof far ultraviolet (FUV) emitting stars in two ~1 kpc$^2$ interarm regions ofthe grand-design spiral M101. The luminosity functions of these stars arecompared with predicted distributions from simple star formation histories, andare best reproduced when the star formation rate has declined recently (past10-50 Myr). This pattern is consistent with stars forming within spiral armsand then streaming into the interarm regions. We measure the diffuse FUVsurface brightness after subtracting all of the detected stars, clusters andbackground galaxies. A residual flux is found for both regions which can beexplained by a mix of stars below our detection limit and scattered FUV light.The amount of scattered light required is much larger for the regionimmediately adjacent to a spiral arm, a bright source of FUV photons.

Origin of the Diffuse, Far Ultraviolet Emission in the Interarm Regions of M101