The MagE spectrograph

By J. Marshall, S. Burles, I. Thompson, S. Shectman, B. Bigelow, G. Burley, C. Birk, J. Estrada, Patricio Jones, Matthew J. Smith and 4 more. Astronomical Telescopes + Instrumentation, 2008

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The Magellan Echellette (MagE) spectrograph is a single-object optical echellette spectrograph for the Magellan Clay telescope. MagE has been designed to have high throughput in the blue; the peak throughput is 22% at 5600 Å including the telescope. The wavelength coverage includes the entire optical window (3100 Å - 1 μm). The spectral resolution for a 1" slit is R~4100. MagE is a very simple spectrograph with only four moving parts, prism cross-dispersion, and a vacuum Schmidt camera. The instrument saw first light in November 2007 and is now routinely taking science observations.

Subfields: Geophysics, Instrumentation, Ocean Engineering

View Paper: https://www.semanticscholar.org/paper/6adaa8b964bb2e9151a9fd852acc502ef0f721fb

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Citations in the corpus

PS16dtm: A Tidal Disruption Event in a Narrow-line Seyfert 1 Galaxy (2017, methodology): “…Ohio State Multiple Object Spectrograph (OSMOS; Martini et al. 2011) on the 2.4- m Hiltner telescope at MDM Observatory, the Wide-Field Reimaging CCD (WFCCD) on the 100-inch DuPont telescope, and the Magellan Echellete Spectrograph (MagE; Marshall et al. 2008) on the 6.5-m Magellan Baade telescope.”
A ∼50,000 M⊙ SOLAR MASS BLACK HOLE IN THE NUCLEUS OF RGG 118 (2015, methodology): “MagE Spectra of RGG 118 were taken on 18 April 2013 with the 6.5m Magellan II telescope at Las Campanas Observatory, using the Magellan Echellette Spectrograph (MagE; Marshall et al. 2008).”
AN EMPIRICAL CHARACTERIZATION OF EXTENDED COOL GAS AROUND GALAXIES USING Mg ii ABSORPTION FEATURES (2010, methodology): “A journal of the MagE QSO observations is in Table 2.”
COSMOLOGICAL CONSTRAINTS FROM MEASUREMENTS OF TYPE Ia SUPERNOVAE DISCOVERED DURING THE FIRST 1.5 yr OF THE Pan-STARRS1 SURVEY (2013, background): “…(GMOS; Hook et al. 2004) on both Gemini North and South, the Low Dispersion Survey Spectrograph-3 (LDSS322) and the Magellan Echellette (MagE; Marshall et al. 2008) on the 6.5- m Magellan Clay telescope, and the Inamori-Magellan Areal Camera and Spectrograph (IMACS; Dressler et al. 2011) on…”
THE z = 5 QUASAR LUMINOSITY FUNCTION FROM SDSS STRIPE 82 (2012, methodology): “We first observed four candidates at the Magellan Clay 6.5m on 2011 Jun 11- 13 using the Magellan Echellette spectrograph (MAGE; Marshall et al. 2008).”
The Complete Light-curve Sample of Spectroscopically Confirmed SNe Ia from Pan-STARRS1 and Cosmological Constraints from the Combined Pantheon Sample (2017, background): “…(GMOS; Hook et al. 2004) on both Gemini North and South, the Low Dispersion Survey Spectrograph-3 (LDSS323) and the Magellan Echellette (MagE; Marshall et al. 2008) on the 6.5 m Magellan Clay telescope, the Inamori-Magellan Areal Camera and Spectrograph (IMACS; Dressler et al. 2011) on the…”
DISCOVERIES FROM A NEAR-INFRARED PROPER MOTION SURVEY USING MULTI-EPOCH TWO MICRON ALL-SKY SURVEY DATA (2010, methodology): “The Magellan Echellette (MagE) Spectrograph (Marshall et al. 2008) on the Magellan Clay Telescope was also used for follow-up.”