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Fig. 9


Distributions of a) dust and gas mass; b) H2 volume density; c) H2 column density; d) electron density; e) ionized gas mass; f) number of ionizing photons or Lyman contiuum; g) number of lines per GHz; h) line luminosity; and i) percentage of line luminosity with respect to the total luminosity (line plus continuum) for the ALMA continuum sources detected toward Sgr B2 (see Table 3). The gray filled area shows the distribution of all the sources, while the blue solid line corresponds to the sources in Sgr B2(N) and the red solid line corresponds to the sources in Sgr B2(M). The black dashed line in the middle panels is derived from the physical parameters of all the Hii regions detected in the Sgr B2 star-forming complex (see Appendix B of Schmiedeke et al. 2016). All the KDE distributions are normalized to their maximum value to better show differences between the different regions.

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