Results 101 to 110 of about 291 (152)
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Compact echelle spectrometer employing a cross-grating
Applied Optics, 2018The concept and the implementation of a compact and simplified echelle spectrometer are presented, and the working principle is demonstrated by first experimental measurements. The crucial element of the setup is a cross-grating, combining an echelle grating utilizing several higher diffraction orders (5th up to 11th) and a superposed perpendicular ...
Daniel, Thomae +6 more
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Advantages of an off-Littrow mounting of an echelle grating
Applied Optics, 1988A phenomenon is described in which the size of the exit-slit image of the entrance slit is influenced by the angle at which an echelle grating is used. The phenomenon becomes significant only for large deviations from Littrow conditions. A mathematical treatment and experimental results are presented to show that proper exploitation of the effect ...
R, Masters, C, Hsiech, H L, Pardue
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Echelle gratings acting as one
Applied Optics, 2003A new device for producing order-sortable echelle spectra by use of consecutive diffactions in several echelle grating surfaces is described. This echelle emulating device (EED) comprises a prism placed in the path between a pair of echelle grating surfaces. The refractive angle of the prism is fixed through a simple relation. The device reproduces all
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An echelle diffraction grating for imaging spectrometer
SPIE Proceedings, 2016We demonstrate an echelle diffraction grating (EDG) of 17 input waveguides and 33 output waveguides. For each input waveguide, only 17 of 33 output waveguides are used, receiving light ranging from 1520 nm to 1600 nm wavelength. The channel spacing of the EDG is 5 nm, with loss of -6dB and crosstalk of -17dB for center input waveguide and -15dB for ...
Minyue Yang +3 more
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Astronomical near-infrared echelle gratings
SPIE Proceedings, 2014High-resolution near-infrared echelle spectrographs require coarse rulings in order to match the free spectral range to the detector size. Standard near-IR detector arrays typically are 2 K x 2 K or 4 K x 4 K. Detectors of this size combined with resolutions in the range 30000 to 100000 require grating groove spacings in the range 5 to 20 lines/mm ...
Kenneth H. Hinkle +2 more
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Large-ruled monolithic echelle gratings
SPIE Proceedings, 2000This paper will present test and performance data on the two largest monolithic, echelle gratings ever ruled. These cryogenically cooled gratings were manufactured by Hyperfine, Inc. and were developed for the Stratospheric Observatory For Infrared Astronomy (SOFIA).
Kirk G. Bach, Bernhard W. Bach, Jr.
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A Diffraction Model for Echelle Gratings
Journal of Modern Optics, 1991Abstract The diffraction model of echelle gratings is quite special because of its surface structure. Considering the shadow effect by neighbouring grooves, from geometrical deductions, a new diffraction model for echelles has been constructed and used successfully to analyse the values of blaze angle with experimental data.
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Fabrication and testing of chemically micromachined silicon echelle gratings
Applied Optics, 2000We have fabricated large, coarsely ruled, echelle patterns on silicon wafers by using photolithography and chemical-etching techniques. The grating patterns consist of 142-microm-wide, V-shaped grooves with an opening angle of 70.6 degrees, blazed at 54.7 degrees.
L D, Keller +4 more
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High Dispersion Stellar Spectroscopy with an Echelle Grating
Applied Optics, 1970The design and operation of a new 3.7-m echelle spectrograph are described. Both photographic (with image intensifier tube) and photoelectric results are presented, together with a critique of the general performance of the instrument.
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Attainment of High Resolution with Diffraction Gratings and Echelles*
Journal of the Optical Society of America, 1960The availability of increased resolution, dispersion, and luminosity from plane gratings at high angles of incidence and diffraction is discussed from the standpoints of theory and practice. Reduction in the resolution given by actual gratings at angles above a certain maximum for a given wavelength usually arises from close-lying line-satellites ...
George R. Harrison, George W. Stroke
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