[4] This nebula is in the western part[4] of the Perseus molecular cloud and is a young region of very active star formation,[6] being one of the best-studied objects of its type.

[4] It contains a fairly typical hierarchy of star clusters that are still embedded in the molecular cloud in which they formed,[7] which are split into two main sub-groups to the north and south.

This spectral type corresponds to a mass of a planetary-mass object (PMO) at the age of NGC 1333.

[9] Parker & Alves de Oliveira on the other hand argue that the distribution of PMOs in NGC 1333 follows N-body simulations of objects that form like stars and that none of the PMOs has a peculiar motion, which is predicted for ejected planets.

One source, called NIRISS-NGC1333-5 (NN5), shows infrared excess, which is an indication of a disk around the object.