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Fig. 8


Relation between the dispersion from the SFR calibrations for [Cii] (top), and [Oi]63 (bottom) as a function of dust temperature, Tdust, on global galaxy scales. The galaxy I Zw 18 was not detected at PACS 160 μm wavelengths and, therefore, the fitting procedure was not attempted in Rémy-Ruyer et al. (2013). Herrera-Camus et al. (2012) estimated a lower limit for the dust temperature Td ≥ 33.7 K based on the PACS 70 μm flux and PACS 160 μm upper limit, which is used to indicate the position of I Zw 18 in the plots of Fig. 4. The image format is the same as explained in Fig. 7.

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