OSA's Digital Library

Journal of the Optical Society of America

Journal of the Optical Society of America

  • Vol. 42, Iss. 10 — Oct. 1, 1952
  • pp: 706–709

Optics InfoBase > JOSA > Volume 42 > Issue 10 > A Fixed-Focus Broad-Range Echelle Spectrograph of High Speed and Resolving Power

A Fixed-Focus Broad-Range Echelle Spectrograph of High Speed and Resolving Power

GEORGE R. HARRISON, JAMES E. ARCHER, and JEAN CAMUS  »View Author Affiliations


JOSA, Vol. 42, Issue 10, pp. 706-709 (1952)
http://dx.doi.org/10.1364/JOSA.42.000706


View Full Text Article

Acrobat PDF (1513 KB)





Browse Journals / Lookup Meetings

Browse by Journal and Year


   


Lookup Conference Papers

Close Browse Journals / Lookup Meetings

Article Tools

Share
Citations

Abstract

From the basic formulas governing echelle performance, simple expressions for echelle and groove dimensions are derived for producing a two-dimensional echelle spectrogram having any desired characteristics. Several possible mountings of Bausch & Lomb echelles having 200 grooves per inch and resolving powers in the range 200,000 to 500,000 have been tested with the objective of covering as much as possible of the spectral range 2000 to 7000A in a single exposure with high photographic speed. This type of spectrograph is of increasing importance for the analysis of complex spectra of materials available in only minute samples. The mounting thus far found most satisfactory involves making the light from a horizontal slit parallel with an 8-inch concave mirror of 10.5-ft focus, placing the echelle with its grooves horizontal in the resulting collimated beam nearly over the slit, and illuminating a 21-ft concave grating with grooves vertical with the slightly diverging parallel beams from the echelle. The vertical plate factor thus produced on 30 inches of plate set in the focal plane at the grating normal varies from 0.47 A/mm at 7000A to 0.14A/mm at 2000A, and the spectral region from 7000 to 2000A can be covered in a single exposure at such dispersion. The reduction of optical parts to mirror, echelle, and grating gives high speed, so that exposure times of from 20 to 60 sec suffice for most arc spectra. To combine the echelle and grating characteristics effectively, the spectrum below 3600A is made to overlap in the second order of the grating that from 7200 to 3500A in the first. Measured resolving powers vary from 220,000 at 7000A to 450,000 or more at 2537A. Even in complex Zeeman spectra of the rare earths, the statistical distribution of lines is found to be such that little interference results from the partial overlapping of two grating orders. The spectral images are found to be stigmatic and sharp out to 15 inches on either side of the normal to the grating.This echelle spectrograph is found to have more than twice the resolving power of our best 35-ft concave grating mount, and from five to ten times its speed. Even with dispersion greater than that given by the grating instrument the plate length required is only 30 in. instead of 750 in. The spectrograph, which has the added advantage of being stigmatic, occupies 35 square feet instead of the 700 sq ft required by the grating mount. This echelle instrument has been used to photograph at high field intensities the Zeeman effects of erbium, holmium, terbium, gadolinium, neodymium, and praseodymium.

Citation
GEORGE R. HARRISON, JAMES E. ARCHER, and JEAN CAMUS, "A Fixed-Focus Broad-Range Echelle Spectrograph of High Speed and Resolving Power," J. Opt. Soc. Am. 42, 706-709 (1952)
http://www.opticsinfobase.org/josa/abstract.cfm?URI=josa-42-10-706


Sort:  Author  |  Journal  |  Reset

References

  1. G. R. Harrison, J. Opt. Soc. Am. 39, 522 (1949). The term echelle grating has been used to designate an echelle produced on an ordinary ruling engine by processes similar to those used in producing high quality diffraction gratings.
  2. G. R. Harrison and C. L. Bausch, Proc. London Conference on Optical Instruments (Chapman and Hall, Ltd., London, July 16–27, 1950).
  3. G. R. Harrison, J. Opt. Soc. Am. 39, 524 (1949). These formulas come directly from those derived by W. E. Williams and others for the reflection echelon.
  4. R. W. Wood, J. Opt. Soc. Am. 37, 733 (1947). Wood crossed a transmission replica of an echelette having 1400 grooves per in. with a reflection echelette having 1800 grooves per in. to try out Shane's suggestion for reducing the spread of astronomical spectra. Our echelle gratings are extreme cases of Wood's echelettes, but differ in using the edge rather than the face of the groove and in their methods of production, and derive more from the reflection echelon.
  5. Griffin, Loring, Werner, and McNally, Southeastern Section Meeting of Am. Phys. Soc., North Carolina State College, April 10–12, 1952.
  6. G. R. Harrison, J. Opt. Soc. Am. 40, 134 (1950).

Cited By

Alert me when this paper is cited

OSA is able to provide readers links to articles that cite this paper by participating in CrossRef's Cited-By Linking service. CrossRef includes content from more than 3000 publishers and societies. In addition to listing OSA journal articles that cite this paper, citing articles from other participating publishers will also be listed.

« Previous Article  |  Next Article »

OSA is a member of CrossRef.

CrossCheck Deposited