Near-infrared and optical studies of the highly obscured nova V1831 Aquilae (Nova Aquilae 2015)

TL;DR

This study presents detailed near-infrared and optical observations of nova V1831 Aquilae, analyzing its dust formation, spectral classification, and physical parameters during the early decline phase.

Contribution

It provides the first comprehensive NIR and optical analysis of V1831 Aquilae, including dust formation details and physical parameter estimates, which were previously unreported.

Findings

Classified as Fe II nova based on NIR spectrum

Estimated distance of 6.1 kpc and extinction of A_v ~ 9.02

Detected early dust formation around day 19.2 with a temperature of 1461 K

Abstract

Near Infrared (NIR) and optical photometry and spectroscopy are presented for the nova V1831 Aquilae, covering the early decline and dust forming phases during the first $\sim$90 days after its discovery. The nova is highly reddened due to interstellar extinction. Based solely on the nature of NIR spectrum we are able to classify the nova to be of the Fe II class. The distance and extinction to the nova are estimated to be 6.1 $\pm$ 0.5 kpc and $A_{\rm v}$ $\sim$ 9.02 respectively. Lower limits of the electron density, emission measure and ionized ejecta mass are made from a Case B analysis of the NIR Brackett lines while the neutral gas mass is estimated from the optical [OI] lines. We discuss the cause for a rapid strengthening of the He I 1.0830 $\mu$m line during the early stages. V1831 Aql formed a modest amount of dust fairly early ($\sim$ 19.2 days after discovery); the dust shell is not seen to be optically thick. Estimates are made of the dust temperature, dust mass and grain size. Dust formation commences around day 19.2 at a condensation temperature of 1461 $\pm$ 15 K, suggestive of a carbon composition, following which the temperature is seen to gradually decrease to 950K. The dust mass shows a rapid initial increase which we interpret as being due to an increase in the number of grains, followed by a period of constancy suggesting the absence of grain destruction processes during this latter time. A discussion is made of the evolution of these parameters, including certain peculiarities seen in the grain radius evolution.