  The supernova impostor PSN J09132750+7627410 in NGC 2748 reached a maximum
luminosity of approximately -14 mag. It was quickly realized that its was not a
true supernova, but another example of a non-terminal giant eruption. PSN
J09132750+7627410 is distinguished by multiple P Cygni absorption minima in the
Balmer emission lines that correspond to outflow velocities of -400, -1100, and
-1600 km/s. Multiple outflows have been observed in only a few other objects.
In this paper we describe the evolution of the spectrum and the P Cygni
profiles for three months past maximum, the post-maximum formation of a cool,
dense wind, and the identification of a possible progenitor. One of the
possible progenitors is an infrared source. Its pre-eruption spectral energy
distribution suggests a bolometric luminosity of -8.3 mag and a dust
temperature of 780 degrees K. If it is the progenitor it is above the AGB limit
unlike the intermediate luminosity red transients. The three P Cygni profiles
could be due to ejecta from the current eruption, the wind of the progenitor,
or previous mass loss events. We suggest that they were all formed as part of
the same high mass loss event and are due to material ejected at different
velocities or energies. We also suggest that multiple outflows during giant
eruptions may be more common than reported.
