Extended Data Fig. 2: Cumulative distribution of the delay from formation of stars to their first identification in a (persistent) multiple system (binary, triple, or quadruple). | Nature Astronomy

Extended Data Fig. 2: Cumulative distribution of the delay from formation of stars to their first identification in a (persistent) multiple system (binary, triple, or quadruple).

From: The bound origin of low-mass stellar binaries

Extended Data Fig. 2

Each coloured line corresponds to 1 of 10 logarithmically spaced mass bins, where stars are binned by their final masses. Persistent multiples are those that survive for more than one snapshot and at least one period. Note that many low mass stars are never in multiples, so the maximum cumulative fraction remains below one.

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