The dynamical evolution of the stellar clumps in the Sparkler galaxy

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Table 2.

Best-fitting parameters of the mass distributions for the initial (third column) and survived (fourth-to-sixth columns) samples of clumps.

p	θ	Initial	Face-on	Edge-on	Spherical
𝒢	$log ({\tilde{M}}_{} / M_{⊙})$ $\log (\widetilde{M}_/\mathrm{M_\odot})$	6.86	6.76	6.77	6.69
		σ	0.31	0.28	0.27	0.23

Notes. The distribution of log M_* is modelled as a Gaussian distribution with mean $log {\tilde{M}}_{*}$ $\log \widetilde{M}_*$ and standard deviation σ (first and second rows). The three configurations (face-on, edge-on and spherical) are defined as in Sect. 2.4.

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