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IRAS 09002-4732 is a poorly studied embedded cluster of stars in the VelaMolecular Ridge at a distance of 1.7kpc. Deep observations with the ChandraX-ray Observatory, combined with existing optical and infrared surveys, producea catalog of 441 probable pre-main sequence members of the region. The stellarspatial distribution has two components: most stars reside in a rich, compact,elliptical cluster, but a minority reside within a molecular filament severalparsecs long that straddles the cluster. The filament has active distributedstar formation with dozens of unclustered protostars. The cluster pre-mainsequence population is $\leq 0.8$ Myr old and deeply embedded; its most massivemember is extremely young producing an ultracompact H II region. The clustertotal population deduced from the X-ray luminosity function is surprisinglyrich, twice that of the Orion Nebula Cluster. The cluster core is remarkablydense where strong N-body interactions should be occurring; its Initial MassFunction may be deficient in massive stars. We infer that IRAS 09002-4732 is arare case where a rich cluster is forming today in a molecular filament,consistent with astrophysical models of cluster formation in clouds thatinvolve the hierarchical formation and merging of groups in molecularfilaments.

IRAS 09002-4732: A Laboratory for the Formation of Rich Stellar Clusters