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Register a new userThe Hyper-Stable Disc of UGC 8839
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The low surface brightness (LSB) spiral UGC 8839 is nearly devoid of star formation aside from a large HII region complex located in the extreme outer disc. In order to understand the origin and nature of this complex, we compare new H{alpha} and archival broad-band images of UGC 8839 to similar data for four other spiral galaxies. We conclude that the extreme off-axis star formation in UGC 8839 is likely due to a hyper-stable disc that is dark matter dominated at all radii, with the Toomre parameter reaching a minimum only in the extreme outer disc. Using analysis strategies designed to be particularly insensitive to the pitfalls of low-surface brightness objects and small number statistics, we determine that the presence of this complex in UGC 8839 is not exceptional when the HII region luminosity function is modelled by a power law, suggesting that it is a native structure and not a merging satellite. However, we find that the entire population of HII regions in UGC 8839 shows a preference for larger galactocentric radii when compared to HII regions in the other galaxies in our sample. UGC 8839 dramatically highlights the relationship between the baryonic/dark matter ratio and disk stability. A three-body interaction, similar to a scaled-down version of the interaction suspected to be responsible for Malin 1, is consistent with the extreme outer disk star formation that we see in the extended disk of UGC 8839.
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We present results of the analysis of photometric and spectroscopic observations of the young stellar complexes in the late giant spiral galaxy UGC 11973. Photometric analysis in the UBVRI bands have been carried out for the 13 largest complexes. For one of them, metallicity of the surrounding gas Z = 0.013+-0.005, the mass M = (4.6+-1.6)*10^6 Msun, and the age of the stellar complex t = (2.0+-1.1)*10^6 yr were evaluated, using spectroscopic data. It is shown that all complexes are massive (M >= 1.7*10^5 Msun) stellar groups younger than 3*10^8 yr.
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