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We present far-UV spectroscopy of the giant elliptical galaxy NGC 1399,obtained with the Far Ultraviolet Spectroscopic Explorer. Of all quiescentellipticals, NGC 1399 has the strongest known ``UV upturn'' -- a sharp spectralrise shortward of 2500 A. It is now well-established that this emission comesfrom hot horizontal branch (HB) stars and their progeny; however, the chemicalcomposition of these stars has been the subject of a long-standing debate. Forthe first time in observations of any elliptical galaxy, our spectra clearlyshow photospheric metallic absorption lines within the UV upturn. The abundanceof N is at 45% solar, Si is at 13% solar, and C is at 2% solar. Such abundanceanomalies are a natural consequence of gravitational diffusion. Thesephotospheric abundances fall in the range observed for subdwarf B stars of theGalactic field.  Although NGC1399 is at the center of the Fornax cluster, we find no evidencefor O VI cooling flow emission. The upper limit to 1032,1038 emission is3.9E-15 erg/s/cm2, equivalent to 0.14 M_sun/yr, and less than that predicted bysimple cooling flow models of the NGC 1399 X-ray luminosity.Comment: 4 pages, Latex. 2 figures. Uses corrected version of emulateapj.sty  and apjfonts.sty (included). Accepted for publication in ApJ Letters. Revised  figure placemen

Photospheric Abundances of the Hot Stars in NGC 1399 and Limits on the Fornax Cluster Cooling Flow