The intensities of the (S II) 6717, 31 Å and (S III) 9532 Å lines have been measured for the first time in the three known extreme halo planetaries. Preliminary estimates of the S/H ratios are: (4.7 ± 6.5) x 10−7 for 108 – 76o1, (1.4 ± 0.6) x 10−7 for K 648, and (2.0 ± 1.3) x 10−7 for 49 + 88o1. The S/H ratio in K 648 (the planetary in M 15) is 0.014 of that measured in the Ring Nebula (Barker, 1980, Ap. J., 240, 99), consistent with the Fe/H abundance of about 1/100 solar found (Cohen, 1978, Ap. J. 223, 487) in the stars in M 15. The average of the S/O ratios in the halo planetaries is an eighth the value in the Ring Nebula, similar to the low Ar/O ratios found previously (Barker, 1980, Ap. J. 237, 482). The implication is either that the abundances of lighter elements such as O have been enhanced by nuclear reactions in the planetary progenitors or that S and Ar were synthesized galactically at a slower rate than lighter elements. In either case, it appears that S and Ar may be more representative of the true heavy metal abundances in planetaries than O.