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 involved. Current members of the team are:

  • Michael Feeney (Instrument Master, Caltech)
  • Richard Walters (Telescope/Instrument Operations and Scheduling, Caltech)
  • Don Neill (Commissioning Scientist, IFU pipeline automation, Caltech)
  • Nadejda Blagorodnova (Science results, RCam photometry pipeline, Caltech)
  • Mickael Rigault (IFU pipeline lead developer, CNRS/IN2P3, France)
  • Jamey Eriksen (Operations Support, Palomar)
  • Jeff Zolkower (Operations Support, Palomar)

Former members, some of whom are still consulted for advice are:

  • Nick Konidaris (Principle Investigator)
  • Robert Quimby (Project Scientist)
  • Jack Davis, and Sagi Ben-Ami (Weizmann institute grad students)
  • 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 Observer’s Reference below.

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

Contents:

Last updated on 09 Oct 2018