High-resolution spectroscopy of SN 2017hcc and its blueshifted line profiles from post-shock dust formation

TL;DR

This study presents high-resolution spectra of SN2017hcc, revealing dust formation in the post-shock shell and a mildly bipolar CSM, providing insights into its line profile evolution and mass-loss history.

Contribution

It is the first detailed spectral analysis of SN2017hcc showing dust formation effects and CSM geometry in a superluminous Type IIn supernova.

Findings

Blueshifted line profiles indicate dust formation in the post-shock shell.

SN2017hcc's CSM is mildly bipolar, similar to SN2010jl.

Progenitor lost about 10 solar masses before explosion.

Abstract

SN2017hcc was remarkable for being a nearby and strongly polarized superluminous TypeIIn supernova (SN). We obtained high-resolution echelle spectra that we combine with other spectra to investigate its line profile evolution. All epochs reveal narrow P~Cygni components from pre-shock circumstellar material (CSM), indicating an axisymmetric outflow from the progenitor of 40-50 km/s. Intermediate-width and broad components exhibit the classic evolution seen in luminous SNe~IIn: symmetric Lorentzian profiles from pre-shock CSM lines broadened by electron scattering at early times, transitioning at late times to multi-component, irregular profiles coming from the SN ejecta and post-shock shell. As in many SNe~IIn, profiles show a progressively increasing blueshift, with a clear flux deficit in red wings of the intermediate and broad velocity components after day 200. This blueshift develops after the continuum luminosity fades, and in the intermediate-width component, persists at late times even after the SN ejecta fade. In SN2017hcc, the blueshift cannot be explained as occultation by the SN photosphere, pre-shock acceleration of CSM, or a lopsided explosion or CSM. Instead, the blueshift arises from dust formation in the post-shock shell and in the SN ejecta. The effect has a wavelength dependence characteristic of dust, exhibiting an extinction law consistent with large grains. Thus, SN2017hcc experienced post-shock dust formation and had a mildly bipolar CSM shell, similar to SN2010jl. Like other superluminous SNeIIn, the progenitor lost around 10Msun due to extreme eruptive mass loss in the decade before exploding.