Abstract
We report 1.25-18.5 μm infrared spectrophotometric measurements of Nova Aquilae 1995. Photometric measurements were obtained over a four month period following the formation of an optically thin dust shell. Hydrogen and helium emission lines were evident throughout this period, along with strong near-infrared coronal line emission that appeared approximately 120 days after outburst. Both the photometric and the spectroscopic data suggest that the ejecta were clumpy, and that they contained both a dust component and a hot gas component. The outflow velocity of the ionized ejecta was observed to be ∼1365-1600 km s<SUP>-1</SUP> (FWHM), and no appreciable deceleration of the ejecta was observed over the duration of these observations. Based on a M<SUB>v</SUB>-t<SUB>2</SUB> light decline relationship, we calculate a distance of ∼3.6-4.8 kpc.
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