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We present new resolved near‐ and mid‐infrared (mid‐IR) imaging and  N ‐band spectroscopy of the two nuclei in the merger system NGC 3256, the most IR luminous galaxy in the nearby Universe. The results from the spectral energy distribution fit to the data are consistent with previous estimates of the amount of obscuration towards the nuclei and the nuclear star formation rates. However, we also find substantial differences in the infrared emission from the two nuclei which cannot be explained by obscuration alone. We conclude that the northern nucleus requires an additional component of warm dust in order to explain its properties. This suggests that local star‐forming conditions can vary significantly within the environment of a single system.

An infrared study of the double nucleus in NGC 3256