SN 2008gz - most likely a normal type IIP event

TL;DR

SN 2008gz is a typical type IIP supernova with unique features like a significant V magnitude drop, providing insights into explosion energy and progenitor mass through detailed photometric and spectroscopic analysis.

Contribution

This study presents detailed photometric and spectroscopic observations of SN 2008gz, revealing its unique light curve features and estimating explosion parameters and progenitor mass.

Findings

SN 2008gz exhibits a rare 1.5 mag drop during plateau to nebular transition.

Estimated synthesized $^{56}$Ni mass is 0.05 M☉.

Explosion energy is between 2-3 x 10^{51} erg, with a progenitor mass up to 17 M☉.

Abstract

We present BV RI photometric and low-resolution spectroscopic investigation of a type II core-collapse supernova (SN) 2008gz, which occurred in a star forming arm and within a half-light radius (solar metallicity region) of a nearby spiral galaxy NGC 3672. The SN event was detected late and a detailed investigation of its light curves and spectra spanning 200 days suggest that it is an event of type IIP similar to archetypal SNe 2004et and 1999em. However, in contrast to other events of its class, the SN 2008gz exhibits rarely observed V magnitude drop of 1.5 over the period of a month during plateau to nebular phase. Using 0.21 mag of Av as a lower limit and a distance of 25.5 Mpc, we estimate synthesized $^{56}$Ni mass of 0.05 \pm 0.01 M* and a mid-plateau Mv of -16.6 \pm 0.2 mag. The photospheric velocity is observed to be higher than that was observed for SN 2004et at similar epochs, indicating explosion energy was comparable to or higher than SN 2004et. Similar trend was also seen for the expansion velocity of H-envelopes. By comparing its properties with other well studied events as well as by using a recent simulation of pre-SN models of Dessart, Livne & Waldman (2010), we infer an explosion energy range of 2 - 3 x 10$^{51}$ erg and this coupled with the observed width of the forbidden [O I] 6300-6364 {\AA} line at 275 days after the explosion gives an upper limit for the main-sequence (non-rotating, solar metallicity) progenitor mass of 17 M*. Our narrow-band H{\alpha} observation, taken nearly 560 days after the explosion and the presence of an emission kink at zero velocity in the Doppler corrected spectra of SN indicate that the event took place in a low luminosity star forming H II region.