Circumstellar Interaction in the Ultraviolet Spectra of SN 2023ixf 14-66 Days After Explosion

TL;DR

This study presents ultraviolet spectra of SN 2023ixf over 66 days, revealing ongoing circumstellar interaction, spectral features dominated by specific elements, and insights into the progenitor's mass-loss history and CSM density profile.

Contribution

First detailed UV spectral analysis of SN 2023ixf showing CSM interaction evolution and progenitor mass-loss history within 33 years prior to explosion.

Findings

CSM interaction power decreases from 5×10^{42} to 1×10^{40} erg s^{-1}

Spectral features dominated by iron, nickel, magnesium, and chromium

Mg II emission asymmetry is not unique to this supernova

Abstract

SN 2023ixf was discovered in M101 within a day of explosion and rapidly classified as a Type II supernova with flash features. Here we present ultraviolet (UV) spectra obtained with the Hubble Space Telescope 14, 19, 24, and 66 days after explosion. Interaction between the supernova ejecta and circumstellar material (CSM) is seen in the UV throughout our observations in the flux of the first three epochs and asymmetric Mg II emission on day 66. We compare our observations to CMFGEN supernova models that include CSM interaction ($\dot{M}<10^{-3}$ M$_{\odot}$ yr$^{-1}$) and find that the power from CSM interaction is decreasing with time, from $L_{\rm sh}\approx5\times10^{42}$ erg s$^{-1}$ to $L_{\rm sh}\approx1\times10^{40}$ erg s$^{-1}$ between days 14 and 66. We examine the contribution of individual atomic species to the spectra on days 14 and 19, showing that the majority of the features are dominated by iron, nickel, magnesium, and chromium absorption in the ejecta. The UV spectral energy distribution of SN 2023ixf sits between that of supernovae which show no definitive signs of CSM interaction and those with persistent signatures assuming the same progenitor radius and metallicity. Finally, we show that the evolution and asymmetric shape of the Mg II $\lambda\lambda$ 2796, 2802 emission are not unique to SN 2023ixf. These observations add to the early measurements of dense, confined CSM interaction, tracing the mass-loss history of SN 2023ixf to $\sim33$ yr prior to the explosion and the density profile to a radius of $\sim5.7\times10^{15}$ cm. They show the relatively short evolution from a quiescent red supergiant wind to high mass loss.