The dusty nova v1065 centauri (nova cen 2007): Aspectroscopic analysis of abundances and dust properties

We examine the ejecta evolution of the classical nova V1065 Centauri, constructing a detailed picture of the system based on spectrophotometric observations obtained from 9 to approximately 900 days post-outburst with extensive coverage from optical to mid-infrared wavelengths. We estimate a reddening toward the system of E(B -V) = 0.5 ± 0.1, based upon the B-V color and analysis of the Balmer decrement, and derive a distance estimate of 8.7_-2.1^+2.8kpc. The optical spectral evolution is classified as P_feN_neA₀ according to the CTIO Nova Classification system of Williams et al. Photoionization modeling yields absolute abundance values by number, relative to solar of He/H = 1.6 ± 0.3, N/H = 144 ± 34,0/H = 58 ± 18, and Ne/H = 316 ± 58 for the ejecta. We derive an ejected gas mass of M_g = (1.6 ± 0.2) × 10^-4 M₀. The infrared excess at late epochs in the evolution of the nova arises from dust condensed in the ejecta composed primarily of silicate grains. We estimate a total dust mass, M₁/, of order (0.2-3.7) × 10^-7 M₀, inferred from modeling the spectral energy distribution observed with the Spitzer IRS and Gemini-South GNIRS spectrometers. Based on the speed class, neon abundance, and the predominance of silicate dust, we classify V1065 Cen as an ONe-type classical nova.