  Pulsars convert a significant fraction of their total spin-down power into
very high-energy electrons, leading to the formation of TeV halos. It is not
yet known, however, whether these sources also efficiently accelerate electrons
at lower energies and, if so, how those particles propagate through the
surrounding environment. If pulsars produce $\sim 50-300 \, {\rm GeV}$
electrons, these particles would produce a spatially extended halo of
synchrotron emission in the frequency range measured by Planck. Such emission
could be used to constrain the low-energy diffusion coefficient in the regions
surrounding these pulsars, as well as the spectrum and intensity of the
electrons that are accelerated in this energy range. In this study, we attempt
to use Planck data to constrain the nature of the Geminga pulsar's TeV halo. We
find no conclusive evidence of this emission in Planck's frequency range,
however, and calculate that the synchrotron flux from Geminga should be well
below the total flux measured by Planck, even for models with favorable
diffusion parameters or soft injection spectra. At this time, these
measurements are not capable of significantly constraining the values of these
parameters.
