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Title:
ESI, a New Keck Observatory Echellette Spectrograph and Imager
Authors:
Sheinis, A. I.; Bolte, M.; Epps, H. W.; Kibrick, R. I.; Miller, J. S.; Radovan, M. V.; Bigelow, B. C.; Sutin, B. M.
Affiliation:
AA(UCO/Lick Observatory, University of California, Santa Cruz, Interdisciplinary Science Building, Santa Cruz, CA 95064; , , , , , .), AB(UCO/Lick Observatory, University of California, Santa Cruz, Interdisciplinary Science Building, Santa Cruz, CA 95064; , , , , , .), AC(UCO/Lick Observatory, University of California, Santa Cruz, Interdisciplinary Science Building, Santa Cruz, CA 95064; , , , , , .), AD(UCO/Lick Observatory, University of California, Santa Cruz, Interdisciplinary Science Building, Santa Cruz, CA 95064; , , , , , .), AE(UCO/Lick Observatory, University of California, Santa Cruz, Interdisciplinary Science Building, Santa Cruz, CA 95064; , , , , , .), AF(UCO/Lick Observatory, University of California, Santa Cruz, Interdisciplinary Science Building, Santa Cruz, CA 95064; , , , , , .), AG(Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101; , .), AH(Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101; , .)
Publication:
The Publications of the Astronomical Society of the Pacific, Volume 114, Issue 798, pp. 851-865. (PASP Homepage)
Publication Date:
08/2002
Origin:
UCP
PASP Keywords:
Instrumentation: Spectrographs, Techniques: Spectroscopic
DOI:
10.1086/341706
Bibliographic Code:
2002PASP..114..851S

Abstract

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.
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