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 –2.1 kpc. The optical spectral evolution is classified as P o fe N ne A 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 Mg = (1.6 ± 0.2) × 10–4 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, Md , of order (0.2-3.7) × 10–7 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.
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机译：我们检查了经典新星V1065 Centauri的射出演化，基于从爆发后9到大约900天获得的分光光度观测结果构建了该系统的详细图片，该覆盖范围涵盖了从光学到中红外波长的广泛范围。基于B – V颜色和Balmer减量的分析，我们估计向E（B-V）= 0.5±0.1的系统变红，得出的距离估计为8.7 + 2.8 –2.1 kpc。根据Williams等人的CTIO Nova分类系统，光谱演变被分类为P ofe N ne A o。相对于太阳光，电离建模产生相对于太阳的绝对丰度值（相对于太阳）He / H = 1.6±0.3，N / H = 144±34，O / H = 58±18和Ne / H = 316±58。我们得出喷射气体质量为Mg =（1.6±0.2）×10–4 M☉。在新星演化的后期，红外过量是由于尘埃聚集在主要由硅酸盐颗粒组成的喷出物中而引起的。我们通过对Spitzer IRS和Gemini-South GNIRS光谱仪观测到的光谱能量分布进行建模，可以估算出总尘埃质量Md约为（0.2-3.7）×10-7 M☉。根据速度等级，霓虹灯丰度和硅酸盐粉尘的优势，我们将V1065 Cen归类为ONe型经典新星。
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