G7.7-3.7: a young supernova remnant probably associated with the guest star in 386 CE (SN 386)

TL;DR

This study presents X-ray observations of supernova remnant G7.7-3.7, proposing its association with the 386 CE guest star, and suggests it was a low-luminosity supernova visible for a few months.

Contribution

It provides the first detailed X-ray analysis linking G7.7-3.7 to the historical 386 CE supernova, supporting its identification as a young, low-luminosity remnant.

Findings

G7.7-3.7 shows an arc-like X-ray morphology with under-ionized plasma.

The remnant's age is estimated at about 1.2 kyr, consistent with the 386 CE event.

The supernova was likely low-luminosity, explaining its short visibility.

Abstract

Although the Galactic supernova rate is about 2 per century, only few supernova remnants are associated with historical records. There are a few ancient Chinese records of "guest stars" that are probably sightings of supernovae for which the associated supernova remnant is not established. Here we present an X-ray study of the supernova remnant G7.7-3.7, as observed by XMM-Newton, and discuss its probable association with the guest star of 386 CE. This guest star occurred in the ancient Chinese asterism Nan-Dou, which is part of Sagittarius. The X-ray morphology of G7.7-3.7 shows an arc-like feature in the SNR south, which is characterized by an under-ionized plasma with sub-solar abundances, a temperature of 0.4--0.8 keV, and a density of $\sim 0.5(d/4 kpc)^{-0.5}$ cm$^{-3}$. A small shock age of $1.2\pm 0.6 (d/4 kpc)^{0.5}$ kyr is inferred from the low ionization timescale of $2.4^{+1.1}_{-1.3}\times 10^{10}$ cm$^{-3}$ s of the X-ray arc. The low foreground absorption ($N_H=3.5\pm0.5\times 10^{21}$ cm$^{-2}$) of G7.7-3.7 made the supernova explosion visible to the naked eyes on the Earth. The position of G7.7-3.7 is consistent with the event of 386 CE, and the X-ray properties suggest that also its age is consistent. Interestingly, the association between G7.7-3.7 and guest star 386 would suggest the supernova to be a low-luminosity supernova, in order to explain the not very long visibility (2--4 months) of the guest star.