  This work presents an extended, neutral Hydrogen emission map around
Magellanic-type dwarf irregular galaxy (dIm) NGC 1569. In the Spring of 2010,
the Robert C. Byrd Green Bank Telescope (GBT) was used to map a 9 degree x 2
degree region in HI line emission that includes NGC 1569 and IC 342 as well as
two other dwarf galaxies. The primary objective for these observations was to
search for structures potentially connecting NGC 1569 with IC 342 group members
in order to trace previous interactions and thus, provide an explanation for
the starburst and peculiar kinematics prevalent in NGC 1569. A large,
half-degree diameter HI cloud was detected that shares the same position and
velocity as NGC 1569. Also, two long structures were discovered that are
reminiscent of intergalactic filaments extending out in a v-shaped manner from
NGC 1569 toward UGCA 92, a nearby dwarf galaxy. These filamentary structures
extend for about 1.5 degrees, which is 77 kpc at NGC 1569. There is a
continuous velocity succession with the 0.5 degree HI cloud, filaments, and
main body of the galaxy. The 0.5 degree HI cloud and filamentary structures may
be foreground Milky Way, but are suggestive as possible remnants of an
interaction between NGC 1569 and UGCA 92. The data also show two tidal tails
extending from UGCA 86 and IC 342, respectively. These structures may be part
of a continuous HI bridge but more data are needed to determine if this is the
case.
