Slitless spectroscopy: Difference between revisions
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==See also== |
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*[[Fine Guidance Sensor and Near Infrared Imager and Slitless Spectrograph]] (JWST component) |
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[[Category:Astronomical spectroscopy]] |
[[Category:Astronomical spectroscopy]] |
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Revision as of 22:37, 5 December 2016
Slitless spectroscopy is astronomical spectroscopy done without a small slit to allow only light from a small region to be diffracted. It works best in sparsely populated fields, as it spreads each point source out into its spectrum, and crowded fields will be too confused to be useful. It also faces the problem that for extended sources, nearby emission lines will overlap.
The Crossley telescope utilized a slitless spectrograph that was originally employed by Nicholas Mayall.[1]
References
- ^ Wilson 2004, p. 432
Cited sources
- Wilson, Ray N. (2004), Reflecting Telescope Optics, Volume 1: Basic design theory and its historical development, Astronomy and astrophysics library, vol. 1, Springer, ISBN 978-3-540-40106-3
See also
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