# Abstract

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The post-reionization thermal state of the intergalactic medium is characterized by a power-law relationship between temperature and density, with a slope determined by the parameter $$\gamma$$. We describe a new method to measure $$\gamma$$ using the ratio of flux curvature in the Lyman-$$\alpha$$ and $$\beta$$ forests. At a given redshift, this curvature ratio incorporates information from the different gas densities traced by Lyman-$$\alpha$$ and $$\beta$$ absorption. It is relatively simple and fast to compute and appears robust against several observational uncertainties. We apply this technique to a sample of 27 high-resolution quasar spectra from the Very Large Telescope. While promising statistical errors on $$\gamma$$ appear to be achievable with these spectra, to reach its full potential, the dependence of the curvature ratio on the thermal state of the gas in the foreground Lyman-$$\alpha$$ forest will require further, detailed forward modelling.