  Type III radio bursts are the result of plasma emission from mildly
relativistic electron beams propagating from the low solar corona into the
heliosphere where they can eventually be detected in situ if they align with
the location of a heliospheric spacecraft. Here we observe a type III radio
burst from 0.1-16 MHz using the Parker Solar Probe (PSP) FIELDS Radio Frequency
Spectrometer (RFS), and from 20-80 MHz using the Low Frequency Array (LOFAR).
This event was not associated with any detectable flare activity but was part
of an ongoing type III and noise storm that occurred during PSP encounter 2. A
deprojection of the LOFAR radio sources into 3D space shows that the type III
radio burst sources were located on open magnetic field from 1.6-3 R$_\odot$
and originated from a near-equatorial active region around longitude E48$^o$.
Combining PSP/RFS observations with WIND/WAVES and STEREO/WAVES, we reconstruct
the type III radio source trajectory in the heliosphere interior to PSP's
position, assuming ecliptic confinement. An energetic electron enhancement is
subsequently detected in situ at the STEREO-A spacecraft at compatible times
although the onset and duration suggests the individual burst contributes a
subset of the enhancement. This work shows relatively small-scale flux
emergence in the corona can cause the injection of electron beams from the low
corona into the heliosphere, without needing a strong solar flare. The
complementary nature of combined ground and space-based radio observations,
especially in the era of PSP, is also clearly highlighted by this study.
