Why SPLASH

SPLASH combines a large area with unprecedented depth in the optical and mid-IR.  The in total 3.6 square degrees are split over two detached fields (COSMOS and SXDS). Both fields contain a wealth of auxiliary data that covers the electromagnetic spectrum from X-ray to sub-millimeter in imaging as well as spectroscopy. SPLASH allows the study of rare galaxy populations, the high-z universe, time sensitive events and large-scale structures.

The following makes SPLASH unique:

  • The deep 3.6μm and 4.5μm data allows to measure reliable stellar masses at z > 4.
  • The depth of SPLASH (optical and mid-IR) allows reliable measurements of photometric redshifts to accuracies better than 2%.
  • The in total 3.6 square degrees allow the study of rare galaxy populations (e.g., massive galaxies at high redshifts) and to pinpoint their abundances and physical properties.
  • The 1.8 square degrees of each field allows the study of over-densities in the early universe (typically 15 arc minutes in size).
  • The two detached fields allow an investigation of cosmic variance.
  • The data is taken in two consecutive years and therefore allows the study of (rare) transients (e.g., supernovae at high-z).

That’s it? – No, SPLASH will provide a treasure trove of targets for the James Webb Space Telescope.