We present observations and analysis of PSN J17292918+7542390, a low-luminosity Type
II-P supernova (LL SN IIP). The observed sample of such events is still low, and their
nature is still under debate. Such SNe are similar to SN 2005cs, a well-observed LL
Type II-P event, having low expansion velocities, and small ejected 56Ni mass. We
have developed a robust and relatively fast Monte Carlo code that fits semi-analytic
models to light curves of core-collapse SNe. This allows the estimation of the most
important physical parameters, like the radius of the progenitor star, the mass of
the ejected envelope, the mass of the radioactive nickel synthesized during the explosion,
among others. PSN J17292918+7542390 has $R_0 = 91_{-70}^{+119} \times 10^{11} \, \text{cm}$,
$M_\text{ej} = 9.89_{-1.00}^{+2.10} \, \mathrm{ M}_{\odot }$, $E_{\mbox{kin}} = 0.65_{-0.18}^{+0.19}
\, \text{foe}$, and $v_{\mbox{exp}} = 3332_{-347}^{+216}$ km s−1, for its progenitor
radius, ejecta mass, kinetic energy, and expansion velocity, respectively. The initial
nickel mass of the PSN J17292918+7542390 turned out to be $1.55_{-0.70}^{+0.75} \times
10^{-3} \, \mathrm{M}_{\odot }$. The measured photospheric velocity at the earliest
observed phase is 7000 km s−1. As far as we can tell based on the small population
of observed LL SNe IIP, the determined values are typical for these events.
