  Core-collapse supernovae (CCSNe) are potentially capable of producing large
quantities of dust, with strong evidence that ejecta dust masses can grow
significantly over extended periods of time. Red-blue asymmetries in the broad
emission lines of CCSNe can be modelled using the Monte Carlo radiative
transfer code DAMOCLES, to determine ejecta dust masses. To facilitate easier
use of DAMOCLES, we present a Tkinter graphical user interface (GUI) running
DAMOCLES. The GUI was tested by high school students as part of the Original
Research By Young Twinkle Students (ORBYTS) programme, who used it to measure
the dust masses formed at two epochs in two Type IIP CCSNe: SN 2012aw and
iPTF14hls, demonstrating that a wide range of people can contribute
significantly to scientific advancement. Bayesian methods were used to quantify
uncertainties on our model parameters. From the presence of a red scattering
wing in the day 1863 H$\alpha$ profile of SN 2012aw, we were able to constrain
the dust composition to large (radius $>0.1 \mu$m) silicate grains, with a dust
mass of $6.0^{+21.9}_{-3.6}\times10^{-4} M_\odot$. From the day 1158 H$\alpha$
profile of SN 2012aw, we found a dust mass of $3.0^{+14}_{-2.5}\times10^{-4}$
M$_\odot$. For iPTF14hls, we found a day 1170 dust mass of 8.1
$^{+81}_{-7.6}\times10^{-5}$ M$_{\odot}$ for a dust composition consisting of
50% amorphous carbon and 50% astronomical silicate. At 1000 days post
explosion, SN 2012aw and iPTF14hls have formed less dust than SN 1987A,
suggesting that SN 1987A could form larger dust masses than other Type IIP's.
