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| High Resolution Echelle Spectrometer | |
|---|---|
| Name | High Resolution Echelle Spectrometer |
| Type | Spectrograph |
| Wavelength | Optical, Near-infrared, Ultraviolet |
| Resolution | High |
High Resolution Echelle Spectrometer The High Resolution Echelle Spectrometer is an astronomical instrument used on observatories such as W. M. Keck Observatory, European Southern Observatory, McDonald Observatory and Gemini Observatory to obtain high-dispersion spectra for studies in stellar astrophysics, planetary science, and cosmology. It combines an echelle grating with cross-dispersing optics to separate overlapping orders, enabling detailed analysis of spectral lines from targets observed by telescopes like Hale Telescope, Keck I, Very Large Telescope, and Subaru Telescope. Developed through collaborations among institutions including California Institute of Technology, Harvard University, Smithsonian Astrophysical Observatory, and Max Planck Society, these spectrometers have been used in programs involving Kepler mission, Hubble Space Telescope, Gaia mission, and ground-based surveys.
High-resolution echelle spectrometers serve projects led by organizations such as National Aeronautics and Space Administration, European Space Agency, National Science Foundation, and Royal Astronomical Society to deliver resolving power sufficient for studies related to Extrasolar planet detection, Stellar evolution, Chemical abundances, and tests of fundamental physics like variation of constants explored by teams at University of Cambridge and Princeton University. Instruments are often mounted on telescopes built by firms or consortia involving Tinsley Laboratories, Lick Observatory, Yerkes Observatory, and research groups at University of California, Berkeley and University of Chicago. Funding and oversight frequently involve agencies including Department of Energy (United States), European Southern Observatory Council, and national academies such as National Academy of Sciences.
An instrument comprises components manufactured or designed by groups from Ball Aerospace, SOFIA Project, Boller and Chivens, and university labs at University of Arizona and University of Hawaii. Typical subsystems include an entrance slit coupled to Cassegrain focus or Nasmyth focus, collimator mirrors developed with partners like Zeiss, an echelle grating produced by firms such as Richardson Grating Laboratory, cross-disperser prisms or gratings, camera optics often specified by Rutherford Appleton Laboratory, and detector arrays from Teledyne, Hamamatsu, or E2V Technologies used in campaigns comparing performance with instruments like HIRES, UVES, and HARPS. Mechanical and thermal control units are engineered by teams affiliated with Jet Propulsion Laboratory and Brookhaven National Laboratory.
The design exploits concepts developed in work by George Ellery Hale, William Huggins, and later optical physicists at Royal Society institutions; modern echelle gratings employ blaze angles and groove densities optimized by manufacturers collaborating with Institute of Optics (University of Rochester) and Fraunhofer Society. The high-dispersion orders are cross-dispersed using prisms or gratings patterned following techniques from diffraction grating research at Imperial College London and École Polytechnique. Beam propagation is analyzed using methods from Isaac Newton's optics lineage and later developments at Max Planck Institute for Astronomy, with alignment procedures influenced by standards from National Institute of Standards and Technology.
Performance metrics are benchmarked against instruments like HIRES on Keck Observatory, UVES on Very Large Telescope, HARPS on 3.6 m Telescope (La Silla) and SOPHIE at Observatoire de Haute-Provence. Resolving power varies from R~20,000 to R>100,000 depending on slit width, grating parameters, and adaptive optics systems developed with contributions from Laboratoire d'Astrophysique de Marseille and Caltech Optical Observatories. Detector characteristics such as read noise, dark current, and quantum efficiency are specified by manufacturers including Sony Corporation and enable measurements used in analyses by research groups at University of Geneva, University of Texas at Austin, and Massachusetts Institute of Technology.
Calibration strategies adopt techniques used by teams at Space Telescope Science Institute, European Southern Observatory Data Management Division, and Harvard & Smithsonian including thorium-argon lamps, iodine absorption cells, and laser frequency combs developed jointly by National Institute of Standards and Technology and Menlo Systems. Data reduction pipelines draw on software traditions from IRAF development at National Optical Astronomy Observatory, ESO Reflex workflows, and algorithms used by projects at Carnegie Institution for Science and Keck Observatory Archive. Teams at University of Notre Dame and Princeton University have published methods for extracting order traces, flat-fielding, and wavelength calibration used across the community.
Applications span radial velocity surveys associated with California Planet Survey, chemical tagging efforts linked to GALAH survey, and studies of intergalactic medium absorption lines pursued by groups at University of Cambridge and Institute of Astronomy, Cambridge. Notable instruments include HIRES, UVES, HARPS, ESPRESSO, and spectrographs on Subaru Telescope and Magellan Telescopes, each contributing to discoveries involving 51 Pegasi b, Proxima Centauri b, and elemental abundance studies of stars in Omega Centauri and M13 (globular cluster). Collaborative programs with observatories like McDonald Observatory and Mount Wilson Observatory have leveraged echelle spectrometers for time-domain and asteroseismology research.
The evolution follows milestones set by early spectroscopists at Royal Observatory, Greenwich and innovations from researchers at Mount Wilson Observatory, with later decades seeing advances at institutions such as Caltech, University of Chicago, and Max Planck Institute. Breakthroughs include cross-dispersion techniques refined by teams at Leiden Observatory and wavelength calibration improvements driven by NIST and industrial partners. Modern laser frequency comb calibration, adaptive optics coupling, and stabilized vacuum-enclosed spectrographs emerged from collaborations involving European Southern Observatory, Harvard–Smithsonian Center for Astrophysics, and technology firms including Menlo Systems.
Category:Astronomical instruments