Welcome to SED Machine’s documentation!

The SED Machine is very low resolution (\(\frac{\lambda}{\Delta \lambda}\sim100\)) optical (365 - 1,000 nm) integral field (30”x”30”) spectrograph and a rainbow imager with a 13’ x 13’ field. The rainbow camera images are partitioned into u, g, r, and i bands, each with a 6’ x 6’ field of view. The instrument was designed for rapid classification of supernovae from transient surveys. To achieve this goal, the instrument was designed to have:

  • Low resolution (\(R=\frac{\lambda}{\Delta \lambda}\sim100\)), sufficient for classification.
  • High “Slit to detector” photon throughput.
  • 0.1 mag precision spectrophotometry.

The hardware project was funded by the NSF with a grant to Caltech. Many people were and are involved. A partial list is here:

  • Nick Konidaris (Principle Investigator)
  • Robert Quimby (Project Scientist)
  • Jack Davis, and Sagi Ben-Ami (Weizmann institute grad students)
  • Don Neill (Commissioning Scientist, IFU pipeline)
  • Nadejda Blagorodnova (Science results, RCam photometry pipeline)
  • Richard Walters (Telescope/Instrument Operations and Scheduling)
  • Karl Vyhmeister (SEDM Database)
  • Chris Cannella (Marshal interface, ATels)

Here we document the instrument for observers and developers. Observers will want to refer to the Quick Reference below.

Data products produced by the semi-automatic pipeline can be found here.


Last updated on 16 March 2017