Fig. 3
Variation of the observed spectral index α1−3mm derived in the baseline bins of Fig. 1 as a function of its associated 3.2 mm flux density. Each symbol represents adifferent protostellar envelope and symbols are color coded with respect to the physical distances probed (in au). Thebottom left arrow indicates the trend predicted when the grain size is increasing (see models from Miotello et al. 2014).
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