Multi-wavelength Observations of the 2015 Nova in the Local Group Irregular Dwarf Galaxy IC 1613

TL;DR

This paper reports the first spectroscopically confirmed nova in the galaxy IC 1613, detailing its multi-wavelength observations, spectral classification, and physical properties, with no X-ray detection over an extended period.

Contribution

It provides the first detailed multi-wavelength observational analysis of a nova in IC 1613, including spectral classification and physical parameters, expanding knowledge of extragalactic nova characteristics.

Findings

Peak magnitude of -7.93 in V-band

Fast decline with t2=13 days and t3=26 days

Spectroscopic classification as hybrid nova

Abstract

A nova in the Local Group irregular dwarf galaxy IC 1613 was discovered on 2015 September 10 and is the first nova in that galaxy to be spectroscopically confirmed. We conducted a detailed multi-wavelength observing campaign of the eruption with the Liverpool Telescope, the LCO 2m telescope at Siding Spring Observatory, and Swift, the results of which we present here. The nova peaked at $M_V=-7.93\pm0.08$ and was fast-fading, with decline times of $t_{2(V)}=13\pm2$ and $t_{3(V)}=26\pm2$ days. The overall light curve decline was relatively smooth, as often seen in fast-fading novae. Swift observations spanned 40 days to 332 days post-discovery, but no X-ray source was detected. Optical spectra show the nova to be a member of the hybrid spectroscopic class, simultaneously showing Fe II and N II lines of similar strength during the early decline phase. The spectra cover the eruption from the early optically thick phase, through the early decline and into the nebular phase. The H$\gamma$ absorption minimum from the optically thick spectrum indicates an expansion velocity of $1200\pm200$ km s$^{-1}$. The FWHM of the H$\alpha$ emission line between 10.54 and 57.51 days post-discovery shows no significant evolution and remains at $\sim1750$ km s$^{-1}$, although the morphology of this line does show some evolution. The nova appears close to a faint stellar source in archival imaging, however we find the most likely explanation for this is simply a chance alignment.