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Fig. 3


Fractional chemical abundances, relative to H2, of C18O (red lines), N2H+ (blue lines), and CH3OH (green lines), computed by Astrochem for the envelope structures of IRAS4A (top left), L1448C (top right), L1157 (bottom left), and IRAS4B (bottom right). The light gray dotted lines show the HWHM of the modeled emission, the dark gray dotted lines the HWHM of the observed emission in C18O (see Table 3), while the light blue dashed line shows the location of the CO snow line in the model (see Table 5). The figure also indicates the dust temperature values at the respective radii. In IRAS4B, the observed and modeled HWHM are the same.

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