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Fig. 5


Cumulative distribution of the stellar masses (including the old stellar population) of the LGRB hosts in our sample (dotted line: whole sample; solid line: with LogM> 8.4 M, to comply with the simulation limits) compared to what is obtained by LGRB host galaxy simulations. The observed distribution is explained by a metallicity cut favouring low metallicities (Z < 0.5 Z).

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