The birth place of the type Ic Supernova 2007gr

TL;DR

This study attempts to identify the progenitor of supernova 2007gr using pre-explosion HST images, suggesting it may have been part of a star cluster with an estimated initial mass based on cluster age.

Contribution

First to analyze the progenitor environment of SN 2007gr using high-precision image alignment and cluster modeling, providing new insights into its possible origin.

Findings

Progenitor likely associated with a star cluster.

Estimated cluster ages of 7 and 20-30 million years.

Progenitor initial mass estimated between 9 and 28 solar masses.

Abstract

We report our attempts to locate the progenitor of the peculiar type Ic SN 2007gr in HST pre-explosion images of the host galaxy, NGC 1058. Aligning adaptive optics Altair/NIRI imaging of SN 2007gr from the Gemini (North) Telescope with the pre-explosion HST WFPC2 images, we identify the SN position on the HST frames with an accuracy of 20 mas. Although nothing is detected at the SN position we show that it lies on the edge of a bright source, 134+/-23 mas (6.9 pc) from its nominal centre. Based on its luminosity we suggest that this object is possibly an unresolved, compact and coeval cluster and that the SN progenitor was a cluster member, although we note that model profile fitting favours a single bright star. We find two solutions for the age of this assumed cluster; 7-/+0.5 Myrs and 20-30 Myrs, with turn-off masses of 28+/-4 Msun and 12-9 Msun respectively. Pre-explosion ground-based K-band images marginally favour the younger cluster age/higher turn-off mass. Assuming the SN progenitor was a cluster member, the turn-off mass provides the best estimate for its initial mass. More detailed observations, after the SN has faded, should determine if the progenitor was indeed part of a cluster, and if so allow an age estimate to within ~2 Myrs thereby favouring either a high mass single star or lower mass interacting binary progenitor.