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Fig. A.1


Logarithm of the Hi to stellar mass ratio, log MHI/M, as a function of the logarithm of the stellar mass, log M (in units of M) for the galaxies in our high sSFR sample. Detections with S/N> 5 are shown as hexagons, marginal detections of S/N 3–5 are shown as crosses, and upper limits shown as downward pointing triangles. The colors indicate the telescope used, or if the detection are from the literature as indicated in the legend. We indicate the typical uncertainty in each quantity for individual galaxies by the black cross in the lower left corner of the plot (see text for details). The red line is the best fit using the Buckley-James method to fit censored data (i.e., including our upper limits, which gives log MHI/M = −0.59log  M + 5.9; Isobe et al. 1986). The black line is the fit to the reference sample of local galaxies with typical sSFR from Papastergis et al. (2012).

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