Spectral Models for Early Time SN 2011fe Observations

TL;DR

This study uses spectral modeling to analyze SN 2011fe, showing that progenitor metallicity has limited impact on spectra and that observed features align with a delayed-detonation model, though some discrepancies remain.

Contribution

It demonstrates the applicability of delayed-detonation models to SN 2011fe and explores the effects of progenitor metallicity and density profiles on spectral features.

Findings

Progenitor metallicity has a small effect on synthetic spectra.

SN 2011fe's abundance stratification closely matches a delayed detonation model.

Lower metallicity models better reproduce observed spectra, especially in the U band.

Abstract

We use observed UV through near IR spectra to examine whether SN 2011fe can be understood in the framework of Branch-normal SNe Ia and to examine its individual peculiarities. As a benchmark, we use a delayed-detonation model with a progenitor metallicity of Z_solar/20. We study the sensitivity of features to variations in progenitor metallicity, the outer density profile, and the distribution of radioactive nickel. The effect of metallicity variations in the progenitor have a relatively small effect on the synthetic spectra. We also find that the abundance stratification of SN 2011fe resembles closely that of a delayed detonation model with a transition density that has been fit to other Branch-normal Type Ia supernovae. At early times, the model photosphere is formed in material with velocities that are too high, indicating that the photosphere recedes too slowly or that SN 2011fe has a lower specific energy in the outer ~0.1 M_sun than does the model. We discuss several explanations for the discrepancies. Finally, we examine variations in both the spectral energy distribution and in the colors due to variations in the progenitor metallicity, which suggests that colors are only weak indicators for the progenitor metallicity, in the particular explosion model that we have studied. We do find that the flux in the U band is significantly higher at maximum light in the solar metallicity model than in the lower metallicity model and the lower metallicity model much better matches the observed spectrum.