Calcium versus silicon ejecta velocities and decline rates in supernovae Ia: The role of high-velocity features

TL;DR

This study investigates the velocities and decline rates of supernova Ia ejecta, revealing differences in line formation depths and the impact of high-velocity features on ejecta kinematics across supernova subclasses.

Contribution

It provides the first comparison of Ca II and Si II velocity distributions at the same phases, highlighting subclass-dependent formation depths and the influence of HVFs on ejecta velocity correlations.

Findings

Ca II PVF velocity distribution is unimodal, unlike the bimodal Si II PVF.

Positive correlation between $ riangle m_{15}$ and Ca II - Si II velocity offset.

Negative correlation between Si II PVF velocity and $ riangle m_{15}$ in HVF-weak SNe.

Abstract

Photospheric and high-velocity features (PVFs and HVFs) of Si II $\lambda$6355 and Ca II IR3 lines in supernova Ia (SN Ia) spectra provide insights into ejecta structure, energetics, and circumstellar interaction, yet their interplay remains poorly understood. We analyse a representative sample of 145 nearby SNe Ia observed within $\pm$5 days of B-band maximum light, including normal, 91T-, and 91bg-like events with measured light-curve decline rates ($\Delta m_{15}$) and Si II and Ca II line properties from the literature. We model PVF and HVF velocity distributions using Gaussian Mixture Models, compare Si II and Ca II PVF velocity distributions, assess Ca II HVF properties, and test correlations between Si II PVF velocities and $\Delta m_{15}$, with emphasis on HVF effects. For the first time, we show that the Ca II PVF velocity distribution, measured for the same events at the same phases as Si II, is predominantly unimodal, in contrast to the well-known bimodal Si II PVF distribution that supports the high-velocity/normal-velocity division. This contrast likely reflects a subclass-dependent formation depth of the Ca II line, as supported by a positive correlation ($>3.3\sigma$) between $\Delta m_{15}$ and the velocity offset between Ca II and Si II PVFs, particularly in faster-declining SNe Ia. Importantly, HVFs do not significantly bias PVF velocity distributions. A significant negative correlation ($>3.3\sigma$) between Si II PVF velocity and $\Delta m_{15}$ is found only for HVF-weak SNe Ia, consistent with more energetic explosions yielding faster ejecta, while this trend vanishes in HVF-strong events, likely due to circumstellar interaction. These results underscore the critical role of HVFs and SN Ia subclass in interpreting ejecta kinematics in both models and observations.