The Burrell Schmidt
Ideally, we would like to do the ICL search for nearby galaxy clusters. Why?
  • Complementary studies of discrete ICL tracers on small scales: 
    • PNe (Arnaboldi et al 1996, 2004; Feldmeier et al 1998, 2004; Aguerri et al 2005) 
    • RGB (Fergusen et al 1998; Durrell et al 2002)
      • Metallicity
    • GCs (ACS Virgo Study; Cote, West et al, ongoing)
      • Progenitors again
  • Detailed connections with individual galaxies
    • Tons of ancillary data (optical, HI/CO, infrared, ultraviolet, X-ray...)
    • Identify tidal interactions
    • Discrimination between tidal mechanisms and ram pressure stripping
    • Assess tidal models for dwarf galaxy evolution 

But it's hard! Need to control flat fielding and scattered light systematics to extreme tolerances, achieve very accurate sky subtraction, and do it all over angular scales > 1 degree!




The Burrell Schmidt
  • 24/36" wide field telescope
  • atop Kitt Peak
  • Case owned/operated
  • SITe 2048x4096 CCD delivers 1.5o x 0.75o FOV
  • Closed tube minimizes scattered light
  • Manually operated (the Schmidt Spa and Fitness Center)

Upgrades and Engineering (aka "Schmidt Happens!")