  The origin of low-luminosity Type IIP supernovae is unclear: they have been
proposed to originate either from massive (about 25 Msun) or low-mass (about 9
Msun) stars. We wish to determine parameters of the low-luminosity Type IIP
supernova 2003Z, to estimate a mass-loss rate of the presupernova, and to
recover a progenitor mass. We compute the hydrodynamic models of the supernova
to describe the light curves and the observed expansion velocities. The wind
density of the presupernova is estimated using a thin shell model for the
interaction with circumstellar matter. We estimate an ejecta mass of 14 Msun,
an explosion energy of 2.45x10^50 erg, a presupernova radius of 229 Rsun, and a
radioactive Ni-56 amount of 0.0063 Msun. The upper limit of the wind density
parameter in the presupernova vicinity is 10^13 g/cm, and the mass lost at the
red/yellow supergiant stage is less than 0.6 Msun assuming the constant
mass-loss rate. The estimated progenitor mass is in the range of 14.4-17.4
Msun. The presupernova of SN 2003Z was probably a yellow supergiant at the time
of the explosion. The progenitor mass of SN 2003Z is lower than those of SN
1987A and SN 1999em, normal Type IIP supernovae, but higher than the lower
limit of stars undergoing a core collapse. We propose an observational test
based on the circumstellar interaction to discriminate between the massive
(about 25 Msun) and moderate-mass (about 16 Msun) scenarios.
