ESI, a New Keck Observatory Echellette Spectrograph and Imager

By A. Sheinis, M. Bolte, H. Epps, R. Kibrick, J. Miller, M. Radovan, B. Bigelow, B. Sutin. 2002

312 citations recorded by the source corpus.

The Echellette Spectrograph and Imager (ESI) is a multipurpose instrument that has been delivered by the Instrument Development Laboratory of Lick Observatory for use at the Cassegrain focus of the Keck II telescope. ESI saw first light on 1999 August 29. ESI is a multimode instrument that enables the observer to seamlessly switch between three modes during an observation. The three modes of ESI are an R = 13,000 echellette mode, a low‐dispersion prismatic mode, and a direct‐imaging mode. ESI contains a unique flexure compensation system that reduces the small instrument flexure to negligible proportions. Long‐exposure images on the sky show FWHM spot diameters of 34 μm (0.″34) averaged over the entire field of view. These are the best non–adaptive optics images taken in the visible at Keck Observatory to date. Maximum efficiencies are measured to be 28% for the echellette mode and greater than 41% for low‐dispersion prismatic mode including atmospheric, telescope, and detector losses. In this paper, we describe the instrument and its development. We also discuss the performance testing and some observational results.

Subfields: Atomic and Molecular Physics, and Optics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/2731b75bcdc6cc4c3fb67189d03e44d19534d704

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Citations in the corpus

SPECTRA AND HUBBLE SPACE TELESCOPE LIGHT CURVES OF SIX TYPE Ia SUPERNOVAE AT 0.511 < z < 1.12 AND THE UNION2 COMPILATION (2010, background): “ESI The two highest redshift candidates, 2001gn and 2001hb, were observed with the echelette mode of ESI (Sheinis et al. 2002).”
The ESSENCE Supernova Survey: Survey Optimization, Observations, and Supernova Photometry (2007, background): “…of ESSENCE targets are performed at a wide variety of ground-based telescopes: the 10mKeck I (+LRIS; Oke et al. 1995) and Keck II (+ESI, Sheinis et al. 2002; +DEIMOS, Faber et al. 2003) telescopes; the 8 m VLT (+FORS1;Appenzeller et al. 1998),GeminiNorth and South (+GMOS; Hook et al.…”
The MagE spectrograph (2008, methodology): “The optical layout of the instrument, shown in Figure 2, is similar to the layout of the instrument ESI at Keck (Sheinis et al. 2002).”
SN 2006tf: Precursor Eruptions and the Optically Thick Regime of Extremely Luminous Type IIn Supernovae (2008, methodology): “We also obtained one late-time optical spectrum on 2008 March 1, day 445 after discovery, using the Echelle Spectrograph and Imager (ESI; Sheinis et al. 2002) on the Keck II telescope (see Table 2).”
REST-FRAME OPTICAL SPECTRA OF THREE STRONGLY LENSED GALAXIES AT z ∼ 2 (2009, methodology): “Using Keck II Echelle Spectrograph and Imager (ESI; Sheinis et al. 2002) rest-frame ultraviolet spectra of the Cosmic Horseshoe and the Clone, Quider et al. (2009) and Quider et al. (in preparation) analyze several of the strongest interstellar absorption features for kinematic evidence of…”
Outflows in Infrared-Luminous Starbursts at z < 0.5. I. Sample, Na I D Spectra, and Profile Fitting (2005, methodology): “For the most distant targets, we used the Echellette Spectrograph and Imager (ESI; Sheinis et al. 2002) on Keck II in echellette mode.”
The Dark Matter Distribution in the Central Regions of Galaxy Clusters: Implications for Cold Dark Matter (2003, methodology): “All spectroscopic measurements – yielding arc redshifts and/or a BCG velocity dispersion– were made with either the Low Resolution Imager and Spectrograph (LRIS) on Keck I (Oke et al. 1995) or ESI on Keck II (Sheinis et al. 2002).”
THE DENSITY PROFILES OF MASSIVE, RELAXED GALAXY CLUSTERS. I. THE TOTAL DENSITY OVER THREE DECADES IN RADIUS (2012, methodology): “MS2137 was observed using the Echelle Spectrograph and Imager (ESI; Sheinis et al. 2002) on the Keck II telescope, as presented by Sand et al. (2002).”
The Structure and Dynamics of Luminous and Dark Matter in the Early-Type Lens Galaxy of 0047–281 at z = 0.485 (2002, methodology): “Keck Spectroscopy We observed 0047 281 using the Echelle Spectrograph and Imager (ESI; Sheinis et al. 2002) on the Keck II Telescope during four consecutive nights (2001 July 23–26), for a total integration time of 20,700 s (7 1800 sþ 3 2700 s).”
Twenty-Three High-Redshift Supernovae from the Institute for Astronomy Deep Survey: Doubling the Supernova Sample at z > 0.7 (2004, methodology): “Keck II ESI We obtained spectra of SN candidates with ESI (Sheinis et al. 2002) on the Keck II telescope during two separate observing runs in 2001October andNovember.”
Outflows in Active Galactic Nucleus/Starburst-Composite Ultraluminous Infrared Galaxies (2005, methodology): “RUPKE, VEILLEUX, & SANDERS752 Vol. 632 Several faint galaxies were observed with the Echellette Spectrograph and Imager (ESI; Sheinis et al. 2002) on Keck II.”
Closing in on a Short-Hard Burst Progenitor: Constraints from Early-Time Optical Imaging and Spectroscopy of a Possible Host Galaxy of GRB 050509b (2005, methodology): “On 17 May 2005, 08:05.5, 8.17 d after the GRB, we obtained deep R(Ellis) (which is similar to Harris R; Bacon et al. 2003) imaging on the Echellete Spectrograph and Imager (ESI; Sheinis et al. 2002) on the Keck II 10 m telescope.”
H0LiCOW – I. H0 Lenses in COSMOGRAIL's wellspring: program overview (2016, background): “Abbreviations are LRIS (Low Resolution Imaging Spectrometer; Oke et al. 1995; Rockosi et al. 2010), ESI (Echellete Spectrograph and Imager; Sheinis et al. 2002), VLT (Very Large Telescope), FORS2 (FOcal Reducer and low dispersion Spectrograph; Appenzeller et al. 1998), and GMOS (Gemini Multi-Object ”
A SURVEY OF z ∼ 6 QUASARS IN THE SLOAN DIGITAL SKY SURVEY DEEP STRIPE. I. A FLUX-LIMITED SAMPLE AT zAB < 21 (2007, methodology): “Optical spectroscopy of the candidates was carried out using the Echelle Spectrograph and Imager (ESI; Sheinis et al. 2002) on the Keck-II in January 2006 and the Low Dispersion Survey Spectrograph (LDSS-3) on Magellan-II in October 2006.”
THE LICK AGN MONITORING PROJECT: THE MBH–σ* RELATION FOR REVERBERATION-MAPPED ACTIVE GALAXIES (2010, methodology): “Keck Observations Five galaxies were observed with the Echellete Spectrograph and Imager (ESI; Sheinis et al. 2002) at the Keck-II 10-m telescope.”
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”
The SDSS Damped Lyα Survey: Data Release 3 (2005, background): “…and C II∗ analysis; Prochaska et al. 2003b; Wolfe 3In general this corresponds to the first data release when the quasar was observed by SDSS although errors in our bookkeeping may have delayed its analysis. et al. 2004) with the Echellette Spectrometer and Imager (ESI; Sheinis et al. 2002).”