Brief program summary and its significance:

Bica, Dottori, Geisler, Claria (Consortium non-member)

We are presently studying  HR diagrams of LMC clusters through Washington
and Johnson photometry, especially those older than 1Gyr. 
Questions that could be addressed with the SOAR telescope:- Completeness
of the LF to lower mass stars. - Cluster dynamical evolution, e.g. Mass 
segregation of stars. -Cluster luminosity profile by stellar counts. 

Present problem in cluster observation is that of crowding, which can easily
cause a loss of 1 to 1.5 mg as we experimented with the 1.0mt CTIO telescope
with a seeing of ~ 1 arcsec. 



Required minimum field of view (arcmin):
2 to 5 cluster diameters, 5arcmin is OK

Required psf (FWHM, profile details):
0.2" will allow to overcome most of the crowdiness problems

Typical target separation if multiple targets per exposure:
Understanding cluster members as targets, from fraction of arcsec,
in crowded cores, to several arcsec is loose clusters and perifery of
clusters. Capability to hit faint stars near bright ones is important.

Signal/noise required per resolution element:
3 sigma at V=25
Typical exposure time for this S/N & lunar phase:
20 to 60 minutes

Anticipated photometric dynamic range required:
more than 1000 would be fine.

What additional photometric calibrations are required?
very good flat fielding, background unperturbed by spurious sources.

If IR, is tip/tilt feasible (consider isoplanatic patch)?

Anticipated number of separate pointings to complete program:
Number of clusters with integrated UBV photometry LMC+SMC 624; Washington
photometry ~ 100. Number of known clusters LMC+SMC ~6000. So
we would like to observe about 30%. It will allow us, additionally, 
to map the spatial distribution of ages throughout the LMC and SMC.
  
Can this program execute in a queue?
yes, for most clusters.

Anticipated post-focus instrumentation requirements (filters, gratings,
etc.):
O and IR CCD imager.
Required instruments (spectral R, filters, wavelength range):
Johnson and Washington filters.

How soon might you need to revisit this target with another instrument?
not important in this case.
Why can't this program execute on the Blanco 4m?
due to PSF requierements.

References (for non-mainstream applications):