  We describe 2016 January to April observations of the fragments of
332P/Ikeya-Murakami, a comet earlier observed in a 2010 October outburst
(Ishiguro et al 2014). We present photometry of the fragments, and perform
simulations to infer the time of breakup. We argue that the eastern-most
rapidly brightening fragment ($F4$) best corresponds to the original nucleus,
rather than the initial bright fragment $F1$. We compute radial and tangential
non-gravitational parameters, $A_1 = (1.5 \pm 0.4) \times 10^{-8}$ AU
day$^{-2}$ and $(7.2 \pm 1.9) \times 10^{-9}$ AU day$^{-2}$; both are
consistent with zero at the $4\sigma$ level. Monte Carlo simulations indicate
that the fragments were emitted on the outbound journey well after the 2010
outburst, with bright fragment $F1$ splitting in mid--2013 and the fainter
fragments within months of the 2016 January recovery. Western fragment $F7$ is
the oldest, dating from 2011. We suggest that the delayed onset of the
splitting is consistent with a self-propagating crystallization of water ice.
