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Fig. 11

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Upper panels: comparison of the inner (red) and outer (black) HDO abundances estimated in the low-mass protostars IRAS 16293-2422, NGC 1333 IRAS 4A, NGC 1333 IRAS 2A, and L1448-mm (see also Table 3) as a function of a) the ratio between the submillimeter and bolometric luminosities Lsmm/Lbol; b) the bolometric luminosity Lbol; c) the submillimeter luminosity Lsmm; d) the bolometric temperature Tbol; e) the ratio /Menv. Lower panels: comparison of the ratio between the inner and outer HDO abundances Xin/Xout as a function of f) the Lsmm/Lbol ratio; g)Lbol; h)Lsmm; i) Tbol; j) /Menv. The different values of the parameters (Lsmm/Lbol, Lbol, Lsmm, Tbol, and Menv) come from Kristensen et al. (2012), Karska et al. (2013), Evans et al. (2009), Froebrich (2005), and Crimier et al. (2010). The HDO abundance is only estimated in the inner part of the protostellar envelope of L1448-mm using interferometric data (Codella et al. 2010). No uncertainty is provided for this value.

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