A relation between H2 V = 1-0 S(1) and 3.28 micron emission in Seyfert and starburst galaxies
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Abstract
This Letter reports the results of a comparison of the H_2_ v = 1-0 S(1) emission line with the 3.28 micron emission feature on a sample of 24 galaxies containing an active galactic nucleus (AGN) or a starburst nucleus (SBN). In the SBNs, we found a good linear correlation between these emissions. If we assume that the S(1) line is due to shock heating by supernova events and the 3.28 micron feature is due to UV radiation of young stars, this correlation is well explained by starburst models publisbed by Rieke et al. In 1980 and Gehrz, Sramek, and Weedman in 1983. In the AGNs, on the other hand, the relative strengths of 3.28 micron feature to S(1) are smaller than those in the SBNs. This trend is interpreted as due to enhanced excitation of S(1) and destruction of 3.28 micron-emitting material caused by abundant X-ray photons from the Seyfert nuclei.