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First Observations with Multi-Pupil Integral Field Spectrograph on 4-meter Mayall Telescope

Published online by Cambridge University Press:  12 April 2016

V. L. Afanasiev ,
V. V. Vlasiouk  and
R. F. Green
V. L. Afanasiev
Affiliation:
Special Astrophysical Observatory of Russian Academy of Sciences, Nyzhnij Arkhyz, Russia, 357147
V. V. Vlasiouk
Affiliation:
Special Astrophysical Observatory of Russian Academy of Sciences, Nyzhnij Arkhyz, Russia, 357147
R. F. Green
Affiliation:
National Optical Astronomy Observatories, Tucson, AZ 85719, USA

Extract

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First attempts to get spectra from extended areas were in the middle of 80-th, using fibers techniques: DensePack (Barden, Scott, 1986), SILFID (Vanderriest and Lemonnier, 1988). Bundle of fibers were put at the focus of the telescope and the other ends of fibers rearranged to produce a long slit of the spectrograph.

Another method of bidimensional spectroscopy, not using optical fibers, was proposed by Prof. G. Courtes (Courtes et al, 1988). He recommended to put behind the telescope focal plane a bidimensional array of microlenses and to project on it an enlarged image. The lens array separates continuous input image and forms an array of micro-pupils that are images of the main mirror illuminating each lens. They create an input image for a classical spectrograph instead of a normal slit. Using of square lenses allows to achieve correct data sampling, and such scheme is ideal for spectrophotometry, allowing integration of total energy from the observed sky area.

Type
3. Integral Field Spectrographs and Spectrometers
Information
International Astronomical Union Colloquium , Volume 149: Tridimensional Optical Spectroscopic Methods in Astrophysics , 1995 , pp. 266 - 268
Copyright
Copyright © Astronomical Society of the Pacific 1995

References

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