Constraints on the narrow-line region of the X-ray quasi-periodic eruption source GSN 069

TL;DR

This study analyzes HST images of GSN 069 to characterize its nuclear [O III] emission, constraining the gas density, size, and origin, and providing insights into the environment of its quasi-periodic eruptions.

Contribution

First detailed analysis of the nuclear [O III] region in GSN 069, constraining gas properties and suggesting a molecular cloud origin for the dense nuclear gas.

Findings

Compact [O III] emission region $\\lesssim 35$ pc in size.

Hydrogen density of $5 imes 10^{3} < n_{\rm H} \lesssim 10^{8}$ cm$^{-3}$.

Estimated accretion system age between 10 and 100 years.

Abstract

The origins of quasi-periodic eruptions (QPEs) are poorly understood, although most theoretical explanations invoke an accretion disk around a supermassive black hole. The gas and stellar environments in the galactic nuclei of these sources are also poorly constrained. In this paper, we present an analysis of archival Hubble Space Telescope (HST) images to study the narrow-line [O III] emission in the QPE source GSN 069. We find strong evidence for a compact nuclear [O III] emission region of size $\lesssim 35$ pc, overlaid on top of extended [O III] emission up to 2 kpc away from the nucleus. The age of the accretion system is estimated to be between 10 and 100 yr. The [O III] luminosity of the compact region was measured to be $(2.1 \pm 0.3) \times 10^{40}\,\rm erg\,s^{-1}$. Based on CLOUDY simulations, we constrain that the [O III] emitting gas has a hydrogen number density in the range $5 \times 10^{3} < n_{\rm H} \lesssim 10^{8}\,\rm cm^{-3}$ and volume filling factor $f_{\rm V} < 2 \times 10^{-3}$. We suggest that the dense gas in the nuclear region of GSN 069 originates from molecular clouds (with total mass $\gtrsim 3 \times 10^{3}\,M_{\odot}$), which are freshly ionised by the soft X-ray photons from the accretion disk. We predict possible evolution of the compact narrow-line region on emission-line diagnostic diagrams, and hence future HST or integral-field unit observations can be used to further pin down the age of this puzzling system.