SuperNova Remnants

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    SuperNova Remnants

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        Supernova Remnants acquire images in the hydrogen emission line Hα and sulphur [SII] Supernova remnants, narrow band filters, forbidden line emission, Balmer line emission determine the [SII]/ Hα ratio and consequently

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          The aim of this exercise focuses on the analysis of narrow band images (as in the case of planetary nebulae) and on the nature of the emission from extended objects. Emission observed in Hα at 6563 A and the forbidden lines of singly ionized sulphur at 6716 and 6731 A may originate from photoionization or from shock heated gas. Their relation can be a useful diagnostic tool.
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