  Type-I Superluminous Supernovae (SLSNe) are an exotic class of core-collapse
SN (CCSN) that can be up to 100 times brighter and more slowly-evolving than
normal CCSNe. SLSNe represent the end-stages of the most massive stripped
stars, and are thought to be powered by the spin-down energy of a millisecond
magnetar. Studying them and measuring their physical parameters can help us to
better understand stellar mass-loss, evolution, and explosions. Moreover,
thanks to their high luminosities, SLSNe can be seen up to greater distances,
allowing us to explore how stellar physics evolves as a function of redshift.
The High Latitude Time Domain Survey (HLTDS) will provide us with an exquisite
dataset that will discover 100s of SLSNe. Here, we focus on the question of
which sets of filters and cadences will allow us to best characterize the
physical parameters of these SLSNe. We simulate a set of SLSNe at redshifts
ranging from z = 0.1 to z = 5.0, using six different sets of filters, and
cadences ranging from 5 to 100 days. We then fit these simulated light curves
to attempt to recover the input parameter values for their ejecta mass, ejecta
velocity, magnetic field strength, and magnetar spin period. We find that four
filters are sufficient to accurately characterize SLSNe at redshifts below $z =
3$, and that cadences faster than 20 days are required to obtain measurements
with an uncertainty below 10\%, although a cadence of 70 days is still
acceptable under certain conditions. Finally, we find that the nominal survey
strategy will not be able to properly characterize the most distant SLSNe at $z
= 5$. We find that the addition of 60-day cadence observations for 4 years to
the nominal HLTDS survey can greatly improve the prospect of characterizing
these most extreme and distant SNe, with only an 8\% increase to the time
commitment of the survey.
