Instruments

Magellan 1 - Baade Telescope

• IMACS
  The Inamori Magellan Areal Camera and Spectrograph (IMACS) is a very versatile wide-field imager and multi-object spectrograph. See technical specifications.
• FourStar
  A wide field near-infrared camera for the Baade NASE platform. See technical specifications.
• FIRE
  The Folded port InfraRed Echellette (FIRE) spectrograph is a moderate resolution near-infrared echellette. See technical specifications.
• MagE
  The MagE (Magellan Echellette) Spectrograph is a moderate-resolution optical echellette. See technical specifications.

Magellan 2 - Clay Telescope

• MIKE
  The Magellan Inamori Kyocera Echelle (MIKE) is a high-throughput double echelle spectrograph. See technical specifications.
• LDSS3
  The Low Dispersion Survey Spectrograph (LDSS3-C) is a high efficiency, wide-field multislit spectrograph. See technical specifications.
• MEGACAM
  Megacam is a large mosaic CCD camera with a 24' x 24' field-of-view. The camera uses 36 2048 x 4608 pixel CCDs with a scale of 0.08"/pixel. Megacam is operated in campaign mode at the f/5 CASS focus.
• MagAO
  Magellan Adaptive Optics system  (VisAO and CLIO2). Continuing commissioning and science operations.

Other Instruments

• PFS
  The Planet Finding Spectrograph is supported as a P.I. instrument that can be installed in place of MIKE at the Clay NASE platform.
• M2FS
  The Michigan/Magellan Fiber Spectrograph is a P.I. instrument that can be installed in the place of MIKE at the Clay NASE platform.
• PISCO
  A simultaneous multi band visible imager is a P.I. instrument that can be installed in the place of MIKE at the Clay NASE platform.

Irénée du Pont Telescope

• CCD
  Direct CCD camera, available for direct imaging giving a scale of 0.259" per pixel over a field of 8.85 arcmin square.
• WFCCD
  Wide field reimaging CCD camera. WFCCD reimages a 25 arc-minute diameter field onto the WF4K CCD camera, with a scale of 0.484 arcsec/pixel. It produces images of approximately two pixels over the full field, and has good transmission from 3800 Å to 9000 Å. Metal slit masks are used to provide a multi-object spectroscopy capability.
• Boller & Chivens Spectrograph
  The B & C slit spectrograph uses a Marconi CCD mated to a Bowen Schmidt camera as the detector. When used with the 600 line/mm grating the dispersion is 1.5 Å/pixel with a wavelength coverage of 3100 Å. The spatial scale on the du Pont Telescope is 0.70 arcsec/pixel, and the maximum slit length 271 arcsec.
• Echelle
  Echelle spectrograph, it provides simultaneous wavelength coverage from ~3700-7000 Å at a typical resolution of ~40,000.
• CAPSCam
  Specialized astrometric camera designed for an astrometric search for Jupiter-like planets.  The camera employs a Rockwell Hawaii-2RG HyViSI array, and the design is optimized for high accuracy astrometry of red dwarf stars.
• RetroCam
  Near-IR imager built especially for the Carnegie Supernova Program, but which is generally available to users.  RetroCam employs a Rockwell Hawaii-1 HgCdTe 1024x1024 array. The focal plane scale is 0.201 arcsec/pixel, with a total field size of  3.4arcmin square. A single filter wheel containing Y, J, and H filters is available.

Henrietta Swope Telescope

• CCD
  Direct CCD camera, E2V 4kx4k, available for direct imaging.