Magellan Instruments

An overview and documentation for current Magellan instrumentation can be found at the LCO Magellan page. More information, including future instruments for Magellan, can be found on the Magellan Technical pages.

Instruments on the Baade telescope

  • The Inamori-Magellan Areal Camera & Spectrograph (IMACS) is a highly-versatile wide field imager, longslit, and multislit spectrograph. It offers a large range of modes:
    • 15.5' x 15.5' field of view at 0.11 arcsec/pixel imaging with the f/4 camera.
    • 27.2' x 27.2' field of view at 0.20 arcsec/pixel imaging with the f/2 camera.
    • Longslit spectroscopy, with a slit-viewing option.
    • Multislit spectroscopy, with a Nod-and-Shuffle option.
    • Integral Field Spectroscopy with the Durham-built IFU.
    • GISMO is an image-slicing reformatter that installs into the slitmask area of IMACS at the focal surface of the Baade telescope. Its purpose is to slice up into 16 sectors a ~4'x4' area at the center of the IMACS f/4 field and reimage them back in the focal plane at the same scale and f-ratio, but covering the entire f/4 field. This allows multislit spectroscopy of densely packed fields ( >5 targets/sq arcmin) whose spectra would normally interfere in the central area, but not once the slices have been separated.
    • The Maryland-Magellan Tunable Filter (MMTF) is a narrow-band filter which is tunable in both central wavelength and transmission bandpass, similar to the old Taurus Tunable Filter. The MMTF is based on a Fabry-Perot etalon that operates in low orders (close plate settings) to provide a large "monochromatic spot" (region of constant wavelength) across the field of view. Its tunability, sensitivity, narrow bandpass, and wide field make this a unique capability applicable to a wide range of programs. Observers intending to request time with the MMTF should contact Sylvain Veilleux (veilleux -@- astro.umd.edu) before applying.
    • The Multi-Object Echelle (MOE) transforms IMACS into a spectrograph with properties similar to ESI on Keck, however with a significant multiplexing capability. MOE on IMACS permits crossed-dispersed echelle spectra to be obtained over the 15' x 15' field of the f/4 camera, accomplished by the use of a grating and cross-dispersing prism mounted on the IMACS grating wheel.
  • FourStar is a wide-field (11' x 11' at 0.16 arcsec per pixel) near-infrared imager using four HAWAII-2RG array detectors, equipped with Y, J, H, and Ks filters, plus other narrower-band filters available by collaboration with the instrument PI Eric Persson (persson -@- obs.carnegiescience.edu).
  • The Folded port InfraRed Echellette (FIRE) provides R~6000 cross-dispersed spectroscopy covering the entire near-IR, as well as a lower-resolution (R=2500 in J, R=1300 in H, R=900 in K), higher-throughput mode. A new 0.45" slit has been installed.
  • The Magellan Echellette Spectrograph (MagE) complements MIKE by pushing further into the blue (3100 - 10000 Å) and having a lower resolution (R~4000 through the 1 arcsec slit), is capable of going significantly fainter.

 

Instruments on the Clay telescope

  • Megacam is a CCD mosaic optical camera covering a 25' x 25' field of view at 0.08 arcsec per pixel with SDSS u', g', r', i' and z' filters. A special g'+r' filter is available by arrangement.
  • The Magellan Adaptive Optics (MagAO) facility is a natural guide star system for the Clay telescope that uses a high-order wavefront sensor and adaptive secondary mirror to deliver near diffraction-limited imaging performance simultaneously with both an optical (VisAO) and an infrared (Clio2) camera. Those interested in using MagAO should contact Laird Close (lclose -@- as.arizona.edu) before submitting a proposal.
  • The Magellan Inamori Kyocera Echelle (MIKE) is a high-throughput double echelle spectrograph.
  • LDSS3 is a high-efficiency, wide-field multislit spectrograph. LDSS3 is available in shared-risks mode as a facility instrument with the Sloan filter set for imaging, and VPH grisms for spectroscopy. A CCD with much-improved red sensitivity is now the default detector for LDSS3, although programs focusing on bluer wavelengths will have the option to use the original CCD in certain blocks.
  • The Planet Finder Spectrograph (PFS) is a high resolution echelle spectrograph optimized for precision radial velocity measurements. PFS is a PI instrument and is currently only available via collaborative arrangement with the instrument team. Contact Paul Butler (bluaper -@- gmail.com) and/or Steve Shectman (shec -@- obs.carnegiescience.edu) before submitting a proposal.
  • The Michigan/Magellan Fibre System (M2FS) is a new fiber-fed, multi-object, optical spectrograph with both high (20K < R < 34K) and low (1,500 < R < 2,700) resolution modes offering full wavelength coverage from 370 to 950nm for up to 256 objects over a 30 arcmin field of view. M2FS is a PI instrument and is only available via collaborative arrangement with the instrument team. Contact Mario Mateo (mmateo -@- umich.edu) before submitting a proposal.
  • The Parallel Imager for Southern Cosmology Observations (PISCO) provides simultaneous imaging in the 4 SDSS bands g', r', i', and z' over a 7.3 x 5.4 arcminute field of view at 0.11 arcsec/pixel. PISCO is a PI instrument and is only available via collaborative arrangement with the instrument team. Contact Tony Stark (astark -@- cfa.harvard.edu) before submitting a proposal.