  We observed the planet-hosting system PDS 70 with the James Webb
Interferometer, JWST's Aperture Masking Interferometric (AMI) mode within
NIRISS. Observing with the F480M filter centered at 4.8 $\mu$m, we
simultaneously fit a geometric model to the outer disk and the two known
planetary companions. We re-detect the protoplanets PDS 70 b and c at an SNR of
21 and 11, respectively. Our photometry of both PDS 70 b and c provide evidence
for circumplanetary disk emission through fitting SED models to these new
measurements and those found in the literature. We also newly detect emission
within the disk gap at an SNR of $\sim$4, at a position angle of
$207^{+11}_{-10}$ degrees, and an unconstrained separation within $\sim$200
mas. Follow-up observations will be needed to determine the nature of this
emission. We place a 5$\sigma$ upper limit of $\Delta$mag = 7.56 on the
contrast of the candidate PDS 70 d at 4.8 $\mu$m, which indicates that if the
previously observed emission at shorter wavelengths is due to a planet, this
putative planet has a different atmospheric composition than PDS 70 b or c.
Finally, we place upper limits on emission from any additional planets in the
disk gap. We find an azimuthally averaged 5$\sigma$ upper limit of $\Delta$mag
$\approx$ 7.5 at separations greater than 125 mas. These are the deepest limits
to date within $\sim$250 mas at 4.8 $\mu$m and the first space-based
interferometric observations of this system.
