Optical and near-infrared recombination lines of oxygen ions from Cassiopeia A knots

TL;DR

This paper predicts observable oxygen recombination lines in optical and near-infrared spectra of supernova remnant knots, enabling detailed studies of shock cooling, ion abundances, and model validation.

Contribution

It introduces a theoretical framework for detecting metal recombination lines in supernova remnant knots, expanding observational possibilities.

Findings

Oxygen recombination lines are detectable with modern telescopes.

Line ratios can probe shock cooling and ion abundances.

Results support testing and refining supernova remnant models.

Abstract

Context. Fast-moving knots (FMK) in the Galactic supernova remnant Cassiopeia A consist mainly of metals and allow to study element production in supernovae and shock physics in great detail. Aims. We work out theoretically and suggest to observe previously unexplored class of spectral lines -- metal recombination lines in optical and near-infrared bands -- emitted by the cold ionized and cooling plasma in the fast-moving knots. Methods. By tracing ion radiative and dielectronic recombination, collisional $l$-redistribution and radiative cascade processes, we compute resulting oxygen, silicon and sulphur recombination line emissivities. It allows us to determine the oxygen recombination line fluxes, based on the fast-moving knot model of Sutherland and Dopita (1995b), that predicts existence of highly-ionized ions from moderate to very low plasma temperatures. Results. The calculations predict oxygen ion recombination line fluxes detectable on modern optical telescopes in the wavelength range from 0.5 to 3 microns. Line ratios to collisionally-excited lines will allow to probe in detail the process of rapid cloud cooling after passage of a shock front, to test high abundances of O V and O VI ions at low temperatures and measure them, to test existing theoretical models of a FMK and to build more precise ones.