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We study the persistent black hole X-ray binary Cyg X-1, recently observed by XRISM Resolve and simultaneously by NICER and NuSTAR in its hard spectral state. We confirm the result of Draghis et al. that fits of the Resolve data alone with the simplest available relativistic reflection model, relxill, yield a black hole spin parameter close to the maximum, a<SUB>*</SUB> ≍ 0.99. However, fitting with an improved, Comptonization-based model, relxillCp, yields a low a<SUB>*</SUB> = 0. 0<SUP>+0.17</SUP>. A similarly low range is obtained with another Comptonization-based model, reflkerrD. Then fits to the combined data require two Comptonization model components but are consistent with any spin value. We conclude that the spin value of Cyg X-1 is strongly model dependent. However, low spin values are consistent with the constraints from gravitational waves. All of the models constrain the inner disk radius to be ≲10 gravitational radii, which is consistent with a recent finding of the weakness of thermal reverberation in Cyg X-1. The suggested source geometry is that of an outflowing disk corona, which was also proposed to explain the X-ray polarization observed from this source.