The nova-like nebular optical spectrum of V404 Cygni at the beginning of the 2015 outburst decay

TL;DR

This study presents optical spectroscopy of V404 Cygni during the initial phase of its 2015 outburst decay, revealing complex emission features, variability, and evidence of a nova-like nebula formed by accretion disc wind remnants.

Contribution

It provides the first detailed optical spectral analysis of V404 Cygni at outburst decay, highlighting the presence of a nova-like nebula and its role in the observed emission features.

Findings

Broad emission lines are optically thick and originate from a circumbinary nebula.

The nebula is likely formed by cooling remnants of accretion disc winds.

Optical continuum may be produced by shocks within the nebula.

Abstract

We report on FORS2 optical spectroscopy of the black hole X-ray binary V404 Cygni, performed at the very beginning of its 2015 outburst decay, complemented by quasi-simultaneous $Swift$ X-ray and ultra-violet as well as REM near-infrared observations. Its peculiar spectrum is dominated by a wealth of emission signatures of HI, HeI, and higher ionisation species, in particular FeII. The spectral features are divided between broad red-shifted and narrow stationary varieties, the latter being emitted in the outer regions. Continuum and line variability at short time scale is high and we find Baldwin effect-like anti-correlations between the full-widths at half-maximum and equivalent widths of the broad lines with their local continua. The Balmer decrement H{\alpha}/H{\beta} is also abnormally large at $4.61\pm0.62$. We argue that these properties hint at the broad lines being optically thick and arising within a circumbinary component in which shocks between faster optically thick and slower optically thin regions may occur. We associate it to a nova-like nebula formed by the cooling remnant of strong accretion disc winds that turned off when the mass-accretion rate dropped following the last major flare. The FeII lines likely arise from the overlap region between this nebula and the companion star winds, whereas we favour the shocks within the nebula as responsible for the optical continuum via self-absorbed optically thin bremsstrahlung. The presence of a near-infrared excess also points towards the contribution of a strongly variable compact jet or a dusty component.