Optical and IR observations of SN 2002dj: some possible common properties of fast expanding SNe Ia

TL;DR

This study presents detailed optical and infrared observations of SN 2002dj, a high-velocity gradient Type Ia supernova, revealing common photometric and spectroscopic properties that distinguish it from normal SNe Ia.

Contribution

It identifies and characterizes the photometric and spectroscopic features of high-velocity gradient SNe Ia, highlighting their distinct properties and possible progenitor metallicity effects.

Findings

High-velocity gradient SNe Ia have faster rise to maximum brightness.

They exhibit more blueshifted absorption features and lower temperatures.

These supernovae show different colour evolution compared to normal SNe Ia.

Abstract

As part of the European Supernova Collaboration we obtained extensive photometry and spectroscopy of the type Ia SN 2002dj covering epochs from 11 days before to nearly two years after maximum. Detailed optical and near-infrared observations show that this object belongs to the class of the high-velocity gradient events as indicated by Si, S and Ca lines. The light curve shape and velocity evolution of SN 2002dj appear to be nearly identical to SN 2002bo. The only significant difference is observed in the optical to near-IR colours and a reduced spectral emission beyond 6500 A. For high-velocity gradient Type Ia supernovae, we tentatively identify a faster rise to maximum, a more pronounced inflection in the V and R light curves after maximum and a brighter, slower declining late-time B light curve as common photometric properties of this class of objects. They also seem to be characterized by a different colour and colour evolution with respect to ``normal'' SNe Ia. The usual light curve shape parameters do not distinguish these events. Stronger, more blueshifted absorption features of intermediate-mass elements and lower temperatures are the most prominent spectroscopic features of Type Ia supernovae displaying high velocity gradients. It appears that these events burn more intermediate-mass elements in the outer layers. Possible connections to the metallicity of the progenitor star are explored.