  The purpose of this preliminary work is to determine if Large Magellanic
Cloud (LMC) Cepheids have stellar winds. If a Cepheid undergoes mass loss then
at some distance from the star, a fraction of the gas becomes dust, which
causes an infrared excess. Mass loss is tested using OGLE II optical
observations and SAGE infrared observations for a sample of 488 Cepheids. The
resultant mass-loss rates range from $10^{-12}$ to $10^{-7}$ $M_\odot/yr$.
Using the mass--loss model we compute infrared stellar luminosities for the
sample of Cepheids and compare predicted infrared PL relations with observed
relations. The predicted relations not only vary from the observed relations,
implying mass loss plays a significant role, but also show evidence for
non-linearity. It is determined that mass loss is important for LMC Cepheids.
