READ ME Ð UV Spectrum of RY Lup This spectrum was produced by stitching together data from four different observing modes: 1) COS G140L 2) COS G130M/G160M 3) STIS G230L 4) STIS G430L The file RYLup_lowres_finalspectrum.txt contains the following four columns: 1) wavelength [Ang] - The entire stitched spectrum was convolved with a Gaussian to smooth it to 1 Ang resolution and then re-binned to a pixel scale of 0.25 Ang/pixel. 2) flux_observed [erg cm-2 s-1 Ang-1] - Each of the four original spectra was interpolated onto the wavelength grid with pixel scale 0.25 Ang/pixel. The noisiest parts of the spectra were removed, and a linear interpolation was used to join them in the regions where the observed fluxes overlapped. The original LyA profile is included here. 3) flux_red_corrected [erg cm-2 s-1 Ang-1] Ð A Cardelli Extinction correction (Av = 0.4, Rv = 3.1) was applied to de-redden the data in flux_observed. The original LyA profile was replaced with a reconstructed version, which has been corrected for the effects of interstellar HI absorption and geocoronal HI emission. 4) flux_red_corrected_continuum [erg cm-2 s-1 Ang-1] Ð Emission line-free regions of flux_red_corrected were used to produce a second order continuum fit spanning 912-1700 Ang. The reconstructed LyA profile was stitched into the continuum fit, which was then used to replace the de-reddened spectrum in this wavelength range.