A mosaic of four UIT far-UV ( FUV ) ( \lambda _ { eff } = 1620Å ) images , with derived stellar and H II region photometry , is presented for most of the Bar of the SMC .
The UV morphology of the SMC ’ s Bar shows that recent star formation there has left striking features including : a ) four concentrations of UV-bright stars spread from northeast to southwest at nearly equal ( \sim 30 arcmin=0.5 kpc ) spacings ; b ) one of the concentrations , near DEM 55 , comprises a well-defined 8-arcmin diameter ring surrounded by a larger H \alpha ring , suggestive of sequential star formation .

FUV PSF photometry is obtained for 11,306 stars in the FUV images , resulting in magnitudes m ( 162 ) .
We present a FUV luminosity function for the SMC bar , complete to m ( 162 ) \sim 14.5 .
Detected objects are well correlated with other SMC Population I material ; of 711 H \alpha emission-line stars and small nebulae within the UIT fields of view , 520 are identified with FUV sources .
The FUV photometry is compared with available ground-based catalogs of supergiants , yielding 191 detections of 195 supergiants with spectral type earlier than F0 in the UIT fields .
The ( m ( 162 ) - V ) color for supergiants is a sensitive measure of spectral type .
The bluest observed colors for each type agree well with colors computed from unreddened Galactic spectral atlas stars for types earlier than about A0 ; for later spectral types the observed SMC stars range significantly bluer , as predicted by comparison of low-metallicity and Galactic-composition models .
Redder colors for some stars of all spectral types are attributed to the strong FUV extinction arising from even small amounts of SMC dust .
Internal SMC reddenings are determined for all catalog stars .
All stars with E ( B - V ) > 0.15 are within regions of visible H \alpha emission .

FUV photometry for 42 H \alpha -selected H II regions in the SMC Bar is obtained for stars and for total emission ( as measured in H II -region-sized apertures ) .
The flux-weighted average ratio of total to stellar FUV flux is 2.15 ; consideration of the stellar FUV luminosity function indicates that most of the excess total flux is due to scattered FUV radiation , rather than stars fainter than m ( 162 ) =14.5 .
Both stellar and total emission are well correlated with H \alpha fluxes measured by Kennicutt and Hodge ( 1986 ; hereafter KH ) , yielding FUV/H \alpha flux ratios that are consistent with models of SMC metallicity , ages from 1-5 Myr , and moderate ( E ( B - V ) =0.0–0.1 mag ) internal SMC extinction .