1. Determine the shape and distribution of the luminosity and mass function.
2. Investigate mass segregation with cluster age.
3. Determine the fraction of unequal mass binaries as a function of primary mass.

NGC 188		NGC 1039 (M34)
NGC 1817		NGC 1912 (M38)
NGC 1960 (M36)		NGC 2099 (M37)
NGC 2158		NGC 2168 (M35)
NGC 2682 (M67)		Melotte 66
IC 4651		Berkeley 39
NGC 2477		NGC 3680
Collinder 261		NGC 6819

The primary facility for Mid-IR imaging is the Spitzer Space Telescope (formerly SIRTF, the Space Infrared Telescope Facility). Consisting of a 0.85-meter telescope and the cryogenically-cooled IRAC camera, Spitzer allows the WOCS clusters to be investigated by obtaining photometry at 3.6, 4.5, 5.8, and 8.0 microns. We hope to obtain phtometry down to (17.5/17.0/16.0/14.5) magnitudes with the IRAC observations.

The NIR (i.e., J,H,K) observation are being conducted with a number of facilities. First, northern hemisphere data is being obtained with FANCAM, the facility instrument of the 31" telescope at the Fan Mountain Observatory, operated by the University of Virginia. FANCAM will be able to provide deep observations reaching (19/18/17) mag in the respective (J H Ks) bands.

Southern hemisphere data collection has begun with observation using the CPAPIR instrument on the CTIO 1.5-m telescope operated by the SMARTS consortium. The clusters NGC 2447, NGC 3680, Collinder 261, and Melotte 66 are planned to be observed in Spring 2007. CPAPIR should also provide deep observations reaching (19/18/17) mag in the respective (J H Ks) bands.