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Fig. 3.

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Normalised star formation rate in the age–[Fe/H] plane derived from CMDft.Gaia for the various samples analysed in this work, namely HelmiA, HelmiB, and HelmiC (top row) and the ‘disc-dominated’ subset, the ‘local retrograde halo’ subset, and HelmiA* (bottom row). In the right-most panels, the horizontal dashed line tentatively separates the Helmi stream progenitor population from contamination by the hot thick disc (at [Fe/H] = −1).

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