Ejecta and progenitor of the low-luminosity type IIP supernova 2003Z

¹ Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching, Germany
² Institute of Theoretical and Experimental Physics, B. Cheremushkinskaya St. 25, 117218 Moscow, Russia e-mail: utrobin@itep.ru
³ Institute of Astronomy of Russian Academy of Sciences, Pyatnitskaya St. 48, 109017 Moscow, Russia
⁴ Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, UK

Received: 5 September 2007
Accepted: 28 September 2007

Abstract

Context. The origin of low-luminosity type IIP supernovae is unclear: they have been proposed to originate either from massive (~) or low-mass (~) stars.

Aims. 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.

Methods. 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.

Results. We estimate an ejecta mass of , an explosion energy of erg, a presupernova radius of , and a radioactive ⁵⁶Ni amount of . The upper limit of the wind density parameter in the presupernova vicinity is 10¹³ g cm^-1, and the mass lost at the red/yellow supergiant stage is ≤ assuming the constant mass-loss rate. The estimated progenitor mass is in the range of 14.4–17.4 . The presupernova of SN 2003Z was probably a yellow supergiant at the time of the explosion.

Conclusions. 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 (~) and moderate-mass (~) scenarios.