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The Giant Stellar Stream (GSS) is a prominent tidal feature in the halo ofthe Andromeda Galaxy (M31), representing the ongoing destruction of a satellitegalaxy. In this paper, we investigate the formation of the GSS through detailednumerical simulations of the tidal disruption of a progenitor system. Assumingthat the stream was created in a single merger event between M31 and a dwarfspheroidal galaxy with stellar mass of $10^{9}M_{\odot}$, we successfullyreproduce the dynamical properties of the GSS. As the metallicity distributionalong the stream has been well determined from the observations (PAndAS andAMIGA data sets), we use Monte Carlo simulations to reconstruct the originalmetallicity distribution of the dwarf progenitor. We find that a progenitordwarf galaxy with a negative radial metallicity gradient, $\Delta$FeH = -$0.3\pm 0.2$, reproduces the observed GSS properties at a time between 2.4 and 2.9Gyrs into the merger. We also show that the observed double peak metallicitydistribution along the stream is a transitory structure caused by unique mergercircumstances where two groups of streaming stars are moving in oppositedirections, intersecting to produce the peaks.

Metallicity distribution of the progenitor of the Giant Stellar Stream in the Andromeda Galaxy