Although NGC 1333 (Catalogued also as VDB 17, DG 18, Ced 16, Bernes 56, LBN 741, LBN 158.31-20.44, Magakian 44 and GC 710) is mapped as a reflection nebula, it is actually a complex region and part of the Perseus OB2 molecular cloud complex. It is illuminated by a star of magnitude 10.5 and spectral class B8P. This is a star forming region and is particularly rich in young stellar objects. The distance of these nebulous complexes is estimated at about 1000 light years. The total mass of the nebula and associated stars is around 450 M⊙. Through observations in X-rays (ROSAT), have been identified 16 young stars, while using the increased sensitivity of the Chandra X-ray Observatory were discovered 127 sources, of which one hundred are extremely weak and distinguishable with difficulty. Among these sources, two (HJ 110 3 and BD + 30 547) are probably stars placed in more remote galactic regions, while about thirty appear to be associated with extragalactic objects; the remaining 96 are instead part of the cloud and are members of the star cluster in formation. Of these, about 80 are T Tauri stars, 8 coincide with extremely young objects, 7 are Class I and II stars with associated jets and one is deeply immersed in the cloud associated with HH objects cataloged as HH 7-11 (see mouseover). In the late nineties, over 30 groups of HH objects were discovered in the cloud, associated with at least a dozen active jets, aged less than 1 million years and within a radius of about 3 light years. Some of these objects were known since the seventies, when they were identified as jets and later cataloged as HH 5, HH 6, the HH group 7-11 and HH 12.