  In this work we study the striking case of a narrow blue stream around the
NGC 7241 galaxy and its foreground dwarf companion. We want to figure out if
the stream was generated by tidal interaction with NGC 7241 or it first
interacted with the foreground dwarf companion and later both fell together
towards NGC 7241. We use four sets of observations, including a follow-up
spectroscopic study with the MEGARA instrument at the 10.4-m Gran Telescopio
Canarias. Our data suggest that the compact object we detected in the stream is
a foreground Milky Way halo star. Near this compact object we detect emission
lines overlapping a bluer and fainter blob of the stream that is clearly
visible in both ultra-violet and optical deep images. From its heliocentric
systemic radial velocity (Vsyst= 1548.58+/-1.80 km s^-1) and new UV and optical
broad-band photometry, we conclude that this over-density could be the actual
core of the stream, with an absolute magnitude of M_g ~ -10 and a (g-r) = 0.08
+/- 0.11, consistent with a remnant of a low-mass dwarf satellite undergoing a
current episode of star formation. From the width of the stream and assuming a
circular orbit, we calculate that the progenitor mass can be the typical of a
dwarf galaxy, but it could also be substantially lower if the stream is on a
very radial orbit or it was created by tidal interaction with the companion
dwarf instead of with NGC 7241. Finally, we find that blue stellar streams
containing star formation regions are commonly predicted by high-resolution
cosmological simulations of galaxies lighter than the Milky Way. This scenario
is consistent with the processes explaining the bursty star formation history
of some dwarf satellites, which are followed by a gas depletion and a fast
quenching once they enter within the virial radius of their host galaxies for
the first time.
