2010AJ....140.1347H

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^+2.8_–2.1kpc. The optical spectral evolution is classified as P ^ o ^_feN_neA_o 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, O/H = 58 ±18, and Ne/H = 316±58 for the ejecta. We derive an ejected gas mass of M_g= (1.6±0.2)x10^–4 M_☉. 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, M_d, of order (0.2-3.7)x10^–7 M_☉, 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.