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tokens: GO-14161, with R. Peterson as PI. As described further by Peterson (in prep.), this spectrum was acquired with the E230H grating of the STIS echelle spectrograph and the slit for a resolving power . Adopting five of the six E230H “prime” wavelength settings, with central wavelengths 201.3 nm, 226.3 nm, 251.3 nm, 276.2 nm, and 301.3 nm, resulted in an analysis coverage of 188.0–314.0 nm. The total exposure time of 106.4 ks (29.5 h) yielded per two-pixel resolution element at all wavelengths, except for the bluest and reddest. To compare the abundances deduced from the HST spectra and the visible, we also used ground-based spectra from the ESO Very Large Telescope archives (spectrographs UVES and HARPS). For wavelengths shorter than 400 nm we used HARPS spectra. They have a resolving power and a signal-to-noise per pixel (S/N) better than 150 per pixel. At longer wavelengths, in the blue we combined the individual UVES spectra to a mean UVES spectrum with a resolving power and a S/N per pixel better than 500. In the red, in order to minimise the influence of the telluric lines, and taking advantage of the fact that following Carney Latham (1987) and de Bruijne Eilers (2012) , HD 84937 shows no detectable velocity variability, we used three different mean spectra each obtained by combining individual spectra with almost the same geocentric radial velocity. Therefore, the positions of the telluric lines relative to the stellar lines are almost the same. These three mean spectra were obtained consecutively on a single night every year between 2002 and 2004. The resulting mean red spectra reach a resolving power of about 45 000 and a S/N per pixel equal to 310, 510, and 350, respectively, in the region of the red C i lines. 3. Spectral analysis and abundance measurements In our analysis we used OSMARCS model atmospheres ( Gustafsson et al. 2008 ) together with the turbospectrum LTE synthesis code ( Alvarez Plez 1998 ; Plez 2012 ). In this code, the collisional broadening by neutral hydrogen is generally computed following the theory developed by Anstee O’Mara (1991) , Barklem et al. (2000) and Barklem O’Mara (2000) . For the computations we adopted the model parameters and [Fe/H] derived for HD 84937 in the same way as in Peterson Kurucz (2015) and Peterson (in prep.): = 6300 K, = 4.0, and = 1.3 , along with the iron abundance they derived with these parameters, . These values deduced only from the UV spectra are in excellent agreement with the values derived for this star by Lawler et al. (2013) and Sneden et al. (2016) based on photometry and accurate H ipparcos parallaxes. The parameters and deduced abundance for each atomic line considered for this analysis are listed in Table 1 . The mean abundances of the different elements are given in Table 2 . For the computations of [X/H] we adopted the solar abundances (C) = 8.5 4 , (Mg) = 7.54, (Si) = 7.52, (P) = 5.46, (S) = 7.16, (K) = 5.11, and (Ca) = 6.33, following Caffau et al. (2011b) or Lodders et