Near-Infrared Spectroscopy of the Recurrent Nova M31N 2008-12a

TL;DR

This paper presents the first near-infrared spectra of the recurrent nova M31N 2008-12a during its 2024 eruption, analyzing emission lines and ejecta behavior to understand its properties and compare with other novae.

Contribution

First NIR spectral observations of M31N 2008-12a during eruption, providing insights into ejecta interaction and emission line evolution.

Findings

HeI 1.083μm line observed on day 6.3, then faded by day 10.3.

Ejecta deceleration consistent with previous optical observations.

Infrared spectra align with predictions based on optical line strengths.

Abstract

Near infrared (NIR) 0.9--2.5$\mu$m spectra of the remarkable recurrent nova M31N 2008-12a were obtained on days 6.3 and 10.3 after discovery of its 2024 outburst, and are the first NIR spectra of this object. The only prominent line seen in the spectra is that of HeI 1.083$\mu$m, on day 6.3. Apart from this HeI line, there are only two other weak emission features: one at 1.0786$\mu$m, suggested to be the [FeXIII] 1.075$\mu$m coronal line, and one unidentified feature at 1.0969$\mu$m. The observed full width at half maximum of the HeI line on day 6.3 (1350 km s$^{-1}$) is consistent with the behaviour of optical HeI lines during earlier eruptions of this RN, which show that the nova ejecta decelerate as they interact with the secondary's wind. The HeI 1.083$\mu$m line faded rapidly, and was absent in the day 10.3 spectrum, along with any other emission lines. We use the relative strengths of optical He and H lines in previous eruptions to estimate the expected strengths of the HeI 1.083$\mu$m line and of other infrared (including coronal) lines at 6.3 days after eruption. Our findings are consistent with the infrared spectra we observed during the 2024 eruption. We apply our analysis to account for the relative weakness of NIR coronal emission in known Galactic recurrent novae with giant secondaries.