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The goal of this program is to obtain external data to allow us to derive FUV dispersion solutions for COS-FUV G130M grating at LP5. The G130M dispersion solutions are 1st order polynomials and the goal of this program is to 1) derive updated dispersion coefficients and 2) derive updated zero points. The emission-line target epsilon Eridani is used. This program is split into two visits (3 orbits and 2 orbits) so that we avoid a single 4 orbit visit. It is instead designed such that Visit 01 will obtain G130M-FUVA 1291 comma 1300 comma and 1327 data comma and visit 02 will obtain G130M-FUVA 1318 and 1309 data. Wavelength solutions for G130M-FUVB (1291) will be derived using data of AV75 from the LP5 spectral resolution program comma 16467 comma as was done at LP4. G130M cenwave 1222 will remain at LP4 comma so we will not be calibrating it at LP5. The exposure times comma and the number of orbits requested comma are driven by the number of counts needed to achieve good correlations. The Eps Eri spectrum contains many chromospheric emission lines across the FUV region comma but Lyman alpha is too bright for G130M FUVB. The Eps Eri spectrum needs to achieve at least S-N virgul5 (virgul25 counts) in the peak of the weaker emission lines to allow good cross correlation for the primary cenwaves. Different weak features across the difference G130M cenwaves were used to calculate the exposure times needed and comma it was determined that a full orbit exposure will give us the needed S-N needed.