511 keV Gamma Ray Echo from Particle Decays in Supernovae

TL;DR

This paper predicts a novel 511 keV gamma-ray echo from positron annihilation in supernovae caused by decaying BSM particles, providing new constraints on axion-like particles and prospects for future gamma-ray observations.

Contribution

It introduces the concept of a gamma-ray echo from supernovae due to BSM particle decays and derives bounds on ALPs using observational data, also assessing future telescope sensitivities.

Findings

Derived bounds on ALP-photon coupling from SN 1987A data.

Predicted gamma-ray echo as a generic signature of BSM particle decays.

Evaluated future telescope capabilities for detecting the echo.

Abstract

The formation of a hot and dense core in a core-collapse supernova (SN) can produce massive Beyond Standard Model (BSM) particles. These particles can decay in the stellar envelope, generating positrons either directly or through secondary processes involving neutrinos or photons. We show for the first time that such positrons regardless of their production channel, can thermalize and annihilate at rest with ambient electrons in the outer SN envelope, producing a characteristic echo of 511 keV gamma rays. For axion-like particles (ALPs), we derive bounds on the ALP-photon coupling ($G_{a \gamma}$) using Pioneer Venus Orbiter observations of SN 1987A. We also evaluate the sensitivity of upcoming MeV gap gamma-ray telescopes in the 511 keV range, such as COSI and AMEGO, for future Galactic SNe, which can improve existing constraints or enable ALP discovery. The echo signal is a generic prediction for any particle species that efficiently produces positrons near the stellar surface.