# Study of the variability of Nova V5668 Sgr, based on high resolution spectroscopic monitoring

## TL;DR

This study provides a detailed spectroscopic analysis of Nova V5668 Sgr, revealing how spectral line velocities and features evolve during different phases of the nova's light curve, highlighting dynamic changes in its ejecta.

## Contribution

It offers the first high-resolution spectroscopic monitoring of Nova V5668 Sgr, correlating spectral line variations with light curve phases to understand nova evolution.

## Key findings

- Absorption features shift to higher velocities during decline
- Disappearance and reappearance of specific spectral lines during phases
- Evolution of emission line profiles showing double peaks

## Abstract

We present results of our dense spectroscopic monitoring of Nova V5668 Sgr. Starting on March 19 in 2015, only a few days after discovery, we have obtained a series of spectra with the TIGRE telescope and its HEROS echelle spectrograph which offers a resolution of R = 20,000 and covers the optical wavelength range from 3800 to 8800 {\AA}. We performed a line identification of the discernible features for four spectra which are representative for the respective phases in the light curve evolution of that nova. By simultaneously analysing the variations in the visual light curve and the corresponding spectra of Nova V5668 Sgr, we found that during the declining phases of the nova the absorption features in all hydrogen and many other lines had shifted to higher expansion velocities of -2000 km s^-1. Conversely, during the rise towards the following maximum, these observed absorption features had returned to lower expansion velocities.We found that the absorption features of some Fe II lines displayed the same behaviour, but in addition disappeared for a few days during some declining phases. Features of several N I lines also disappeared while new N II lines appeared in emission for a few days during some of the declining phases of the light curve of Nova V5668 Sgr. The shape of the emission features is changing during the evolution and shows a clear double peak structure after the deep minimum.