H II regions are clouds of glowing, ionised gas associated with regions of recent star formation. By studying the light emitted by these regions, we can learn about their physical conditions and chemical composition, providing important clues about how stars and galaxies form and evolve. One of the key properties we need to know is the temperature of the gas. We can measure it from the emission lines of different chemical elements, which probe different parts of an H II region. However, it is not always possible to measure all these temperatures directly. In these cases, we need to estimate
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