Optical to X-ray Signatures of Dense Circumstellar Interaction in Core-Collapse Supernovae

TL;DR

This paper models the X-ray and optical/UV signatures of dense circumstellar material interaction in core-collapse supernovae, providing a framework to infer stellar mass loss properties from observations.

Contribution

It introduces a detailed treatment of X-ray transients from supernovae interacting with truncated dense CSM, including post-interaction phases and absorption effects.

Findings

eROSITA will detect many CSM X-ray transients

Optical/UV signatures depend on CSM optical depth

Framework for inferring CSM properties from X-ray data

Abstract

Progenitors of core-collapse supernovae (SNe) can shed significant mass to circumstellar material (CSM) in the months--years preceding core-collapse. The ensuing SN explosion launches ejecta that may subsequently collide with this CSM, producing shocks that can power emission across the electromagnetic spectrum. In this work we explore the thermal signatures of dense CSM interaction, when the CSM density profile is truncated at some outer radius. CSM with optical depth $>c/v$ (where $v$ is the shock velocity) will produce primarily $\sim$blackbody optical/UV emission whereas lower optical-depth CSM will power bremsstrahlung X-ray emission. Focusing on the latter, we derive light-curves and spectra of the resulting X-ray transients, that include a detailed treatment of Comptonization. Due to strong photoelectric absorption, the X-ray light-curve is dominated by the `post-interaction' phase that occurs after the shock reaches the CSM truncation radius. We treat this regime here for the first time. Using these results, we present the phase-space of optical, UV, and X-ray transients as a function of CSM properties, and discuss detectability prospects. We find that ROSAT would not have been sensitive to CSM X-ray transients but that eROSITA is expected to detect many such events. Future wide-field UV missions such as ULTRASAT will dramatically enhance sensitivity to large optical-depth CSM configurations. Finally, we present a framework within which CSM properties may be directly inferred from observable features of X-ray transients. This can serve as an important tool for studying stellar mass loss using SN X-ray detections.