  A nova in the Local Group irregular dwarf galaxy IC 1613 was discovered on
2015 September 10 and is the first nova in that galaxy to be spectroscopically
confirmed. We conducted a detailed multi-wavelength observing campaign of the
eruption with the Liverpool Telescope, the LCO 2m telescope at Siding Spring
Observatory, and Swift, the results of which we present here. The nova peaked
at $M_V=-7.93\pm0.08$ and was fast-fading, with decline times of
$t_{2(V)}=13\pm2$ and $t_{3(V)}=26\pm2$ days. The overall light curve decline
was relatively smooth, as often seen in fast-fading novae. Swift observations
spanned 40 days to 332 days post-discovery, but no X-ray source was detected.
Optical spectra show the nova to be a member of the hybrid spectroscopic class,
simultaneously showing Fe II and N II lines of similar strength during the
early decline phase. The spectra cover the eruption from the early optically
thick phase, through the early decline and into the nebular phase. The
H$\gamma$ absorption minimum from the optically thick spectrum indicates an
expansion velocity of $1200\pm200$ km s$^{-1}$. The FWHM of the H$\alpha$
emission line between 10.54 and 57.51 days post-discovery shows no significant
evolution and remains at $\sim1750$ km s$^{-1}$, although the morphology of
this line does show some evolution. The nova appears close to a faint stellar
source in archival imaging, however we find the most likely explanation for
this is simply a chance alignment.
