The helium abundance in the Jovian atmosphere is derived from Voyager 1 data by two methods. The first method uses only infrared spectra from selected locations on the planet while the second method uses a thermal profile independently derived from radio occulation measurements and infrared spectra recorded near the occulation point. A hydrogen mole fraction of 0.897¿0.030 is obtained from the first method, while the second method give 0.880¿0.036, corresponding to helium mass fractions of 0.19¿0.05 and 0.21¿0.06, respectively. The estimated errors for the first method are primarily due to systematic uncertainties in the H2 and He absorption coefficients, while those for the second method result mainly from errors in the radio occultation profile and are less well known. Random errors in the measured infrared spectra are found to be negligible in both cases. The results are consistent with a uniform mix of hydrogen and helium within Jupiter's interior, but a modest amount of helium depletion (ΔY? 0.05) cannot be excluded.