No evidence of circumstellar gas surrounding Type Ia Supernova SN 2017cbv

TL;DR

This study used high-resolution spectra of SN 2017cbv to search for circumstellar gas and found no evidence of such material, constraining progenitor models that deposit little gas in their environment.

Contribution

The paper provides the first detailed time-series analysis of high-resolution spectra to constrain circumstellar gas around SN 2017cbv, ruling out significant gas presence.

Findings

No detectable changes in Na I D and Ca II H&K lines over time.

Limits on circumstellar gas mass around SN 2017cbv.

Progenitor models with minimal circumstellar gas are favored.

Abstract

Nearby type Ia supernovae (SNe Ia), such as SN 2017cbv, are useful events to address the question of what the elusive progenitor systems of the explosions are. Hosseinzadeh et al. (2017) suggested that the early blue excess of the lightcurve of SN 2017cbv could be due to the supernova ejecta interacting with a non-degenerate companion star. Some SN Ia progenitor models suggest the existence of circumstellar (CS) environments in which strong outflows create low density cavities of different radii. Matter deposited at the edges of the cavities, should be at distances at which photoionisation due to early ultraviolet (UV) radiation of SNe Ia causes detectable changes to the observable Na I D and Ca II H&K absorption lines. To study possible narrow absorption lines from such material, we obtained a time-series of high-resolution spectra of SN 2017cbv at phases between $-14.8$ and $+83$ days with respect to $B$-band maximum, covering the time at which photoionisation is predicted to occur. Both narrow Na I D and Ca II H&K are detected in all spectra, with no measurable changes between the epochs. We use photoionisation models to rule out the presence of Na I and Ca II gas clouds along the line-of-sight of SN 2017cbv between $\sim8\times10^{16}$--$2\times10^{19}$~cm and $\sim10^{15}$--$10^{17}$~cm, respectively. Assuming typical abundances, the mass of a homogenous spherical CS gas shell with radius $R$ must be limited to $M^{\rm CSM}_{\rm HI}<3\times10^{-4}\times(R/10^{17}[{\rm cm}])^2$ M$_{\odot}$. The bounds point to progenitor models that deposit little gas in their CS environment.