MIKE: A Double Echelle Spectrograph for the Magellan Telescopes at Las Campanas Observatory

By R. Bernstein, S. Shectman, S. Gunnels, St. Mochnacki, A. Athey. SPIE Astronomical Telescopes + Instrumentation, 2003

445 citations recorded by the source corpus.

Subfields: Atomic and Molecular Physics, and Optics, Instrumentation, Surfaces, Coatings and Films

View Paper: https://www.semanticscholar.org/paper/ceda17fcaf78f9f12f4e11cf1880bbfee1b3d2ad

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Citations in the corpus

APF—The Lick Observatory Automated Planet Finder (2014, methodology): “Accordingly, we chose an optical configuration based on the Magellan Inamori Kyocera Echelle (MIKE) instrument (Bernstein et al. 2003), a scheme also used in Planet Finder Spectrograph (PFS) (Crane et al. 2010).”
KINEMATIC AND SPATIAL SUBSTRUCTURE IN NGC 2264 (2015, methodology): “MIKE Fibers has two independent spectrograph channels; at 5200 Å we are able to use both channels with 128 fibers going to each channel.”
STELLAR VELOCITIES IN THE CARINA, FORNAX, SCULPTOR, AND SEXTANS dSph GALAXIES: DATA FROM THE MAGELLAN/MMFS SURVEY (2008, methodology): “We use repeat measurements of stars measured on both the blue and the red channels of the MIKE spectrograph to quantify any systematic difference that may arise due to channeldependent dispersion characteristics (Bernstein et al. 2003; Paper I).”
The T Tauri Phase Down to Nearly Planetary Masses: Echelle Spectra of 82 Very Low Mass Stars and Brown Dwarfs (2005, methodology): “For the Cha I, R CrA, and TW HyA southern targets, we used the Magellan Inamori Kyocera Echelle (MIKE) spectrograph (Bernstein et al. 2003) on the Baade 6.5 m telescope at Las Campanas Observatory, Chile.”
Internal Kinematics of the Fornax Dwarf Spheroidal Galaxy (2005, unknown): “The 2002 spectra were acquired at the Magellan 6.5m Clay Telescope with the Magellan Inamori Kyocera Echelle (MIKE) spectrograph (Bernstein et al. 2003) using a 1.0”× 5.0” slit and MIKE’s red-side CCD detector set to obtain spectra between 4400− 8000 Å.”
A Direct Precision Measurement of the Intergalactic Lyα Opacity at 2 ≤ z ≤ 4.2 (2007, methodology): “Our data set consists of quasar spectra obtained with the High Resolution Echelle Spectrometer (Vogt et al. 1994, HIRES) and Spectrograph and Imager (Sheinis et al. 2002, ESI) spectrographs on the Keck telescopes and with the Magellan Inamori Kyocera Echelle (Bernstein et al. 2003, MIKE) spectrograp”
ON THE SOURCE OF THE DUST EXTINCTION IN TYPE Ia SUPERNOVAE AND THE DISCOVERY OF ANOMALOUSLY STRONG Na i ABSORPTION (2013, result): “The remaining 24 spectra in our data set correspond to unpublished observations of SNe and AGNs obtained with the Magellan Inamori Kyocera Echelle (MIKE; Bernstein et al. 2003) on the 6.5 m Clay telescope.”
A FIRST CONSTRAINT ON THE THICK DISK SCALE LENGTH: DIFFERENTIAL RADIAL ABUNDANCES IN K GIANTS AT GALACTOCENTRIC RADII 4, 8, AND 12 kpc (2011, methodology): “Methods Twenty red giants in the outer disk, selected from the 2MASS catalogue, were observed with the MIKE spectrograph (Bernstein et al. 2003) on the Magellan telescopes in Nov. 2007.”
THE ABUNDANCES OF NEUTRON-CAPTURE SPECIES IN THE VERY METAL-POOR GLOBULAR CLUSTER M15: A UNIFORM ANALYSIS OF RED GIANT BRANCH AND RED HORIZONTAL BRANCH STARS (2011, methodology): “5-m telescope of the Las Campanas Observatory with the Magellan Inamori Kyocera Echelle (MIKE) spectrograph (Bernstein et al. 2003)(11).”
Quasars Probing Quasars. I. Optically Thick Absorbers near Luminous Quasars (2006, methodology): “…quasars SDSS J0303 0023 and SDSS J1204+0221, observed with the High Resolution Echelle Spectrometer (HIRES; Vogt et al. 1994; FWHM 10 km s 1) on the Keck I telescope, and SDSS J1429 0145, observed with the Magellan Inamori Kyocera Echelle spectrograph (MIKE; Bernstein et al. 2003; FWHM 10 km s 1).”
The Transiting Extrasolar Giant Planet around the Star OGLE-TR-113 (2004, methodology): “Our high-resolution spectroscopic observations were carried out with the MIKE spec- trograph (Bernstein et al. 2003) on the Magellan I (Baade) telescope at the Las Campanas Observatory in Chile.”
A SEARCH FOR STARS OF VERY LOW METAL ABUNDANCE. VI. DETAILED ABUNDANCES OF 313 METAL-POOR STARS (2014, methodology): “High Resolution Spectroscopy Observations conducted at Las Campanas Observatory were made with the Magellan Inamori Kyocera Echelle (MIKE) spectrograph (Bernstein et al. 2003).”
Chemical similarities between Galactic bulge and local thick disk red giants: O, Na, Mg, Al, Si, Ca, and Ti (2010, methodology): “…analysis of thin disk, thick disk and halo stars is based mostly on high-resolution (R= 65,000) optical spectra taken in April 2007 with the MIKE spectrograph (Bernstein et al. 2003) on the Clay 6.5 m Magellan telescope, and complemented with observations using the 2dcoudé spectrograph (Tull etal.”