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NGC 2362 is a richly populated Galactic cluster, devoid of natal moleculargas and dust. The cluster represents the final product of the star formingprocess and hosts an unobscured and near-complete initial mass function. NGC2362 is dominated by the O9 Ib multiple star, tau CMa, as well as several dozenunevolved B-type stars. Distributed throughout the cluster are several hundredsuspected intermediate and low-mass pre-main sequence members. Variouspost-main sequence evolutionary models have been used to infer an age of 5 Myrfor the one evolved member, tau CMa. These estimates are in close agreementwith the ages derived by fitting pre-main sequence isochrones to thecontracting, low-mass stellar population of the cluster. The extremely narrowsequence of stars, which extends more than 9 mag in the optical color-magnitudediagram, suggests that star formation within the cluster occurred rapidly andcoevally across the full mass spectrum. Ground-based near infrared and H-alphaemission surveys of NGC 2362 concluded that most (~90%) of the low-mass membershave already dissipated their optically-thick, inner(< 1 AU) circumstellardisks. Spitzer IRAC observations of the cluster have confirmed these results,placing an upper limit on the primordial, optically thick disk fraction of thecluster at 7(+/-)2%. The presence of circumstellar disks among candidatemembers of NGC 2362 is also strongly mass-dependent, such that no stars moremassive than 1.2 Msun exhibit significant infrared excess shortward of 8microns. The well-defined upper main sequence of NGC 2362, its large populationof low-mass stars, and the narrow age spread evident in the color-magnitudediagram ensure its role as a standard model of cluster as well as stellarevolution.

NGC 2362: The Terminus of Star Formation