Abstract

The horizontal foci of a Tandem Wadsworth spectrograph are calculated by using the correct ruling densities for both gratings. Results are quite different from those of previous analyses that used approximate ruling densities. Ray tracings confirm the analyses with the correct ruling densities and also indicate that this spectrograph possesses the excellent, nearly stigmatic properties found by the approximate analyses.

© 1979 Optical Society of America

Full Article  |  PDF Article

References

  • View by:
  • |
  • |
  • |

  1. J-D. F. Bartoe and G. E. Brueckner, “New stigmatic, coma-free, concave-grating spectrograph,” J. Opt. Soc. Am. 65, 13–21 (1975).
    [CrossRef]
  2. G. E. Brueckner, J-D. F. Bartoe, and M.E. Van Hoosier, “High spatial resolution observations of the solar EUV spectrum,” to be published in Proceedings of the OSO-8 Workshop edited by E. Hansen and S. Schaffner (University of Colorado, Boulder, 1978).
  3. S. O. Kastner and W. M. Neupert, “Image construction for concave gratings at grazing incidence, by ray tracing,” J. Opt. Soc. Am. 53, 1180–1184 (1963).
    [CrossRef]
  4. H. Noda, T. Namioka, and M. Seya, “Ray tracing through holographic gratings,” J. Opt. Soc. Am. 64, 1037–1042 (1974).
    [CrossRef]

1975 (1)

1974 (1)

1963 (1)

Bartoe, J-D. F.

J-D. F. Bartoe and G. E. Brueckner, “New stigmatic, coma-free, concave-grating spectrograph,” J. Opt. Soc. Am. 65, 13–21 (1975).
[CrossRef]

G. E. Brueckner, J-D. F. Bartoe, and M.E. Van Hoosier, “High spatial resolution observations of the solar EUV spectrum,” to be published in Proceedings of the OSO-8 Workshop edited by E. Hansen and S. Schaffner (University of Colorado, Boulder, 1978).

Brueckner, G. E.

J-D. F. Bartoe and G. E. Brueckner, “New stigmatic, coma-free, concave-grating spectrograph,” J. Opt. Soc. Am. 65, 13–21 (1975).
[CrossRef]

G. E. Brueckner, J-D. F. Bartoe, and M.E. Van Hoosier, “High spatial resolution observations of the solar EUV spectrum,” to be published in Proceedings of the OSO-8 Workshop edited by E. Hansen and S. Schaffner (University of Colorado, Boulder, 1978).

Kastner, S. O.

Namioka, T.

Neupert, W. M.

Noda, H.

Seya, M.

Van Hoosier, M.E.

G. E. Brueckner, J-D. F. Bartoe, and M.E. Van Hoosier, “High spatial resolution observations of the solar EUV spectrum,” to be published in Proceedings of the OSO-8 Workshop edited by E. Hansen and S. Schaffner (University of Colorado, Boulder, 1978).

Cited By

OSA participates in CrossRef's Cited-By Linking service. Citing articles from OSA journals and other participating publishers are listed here.

Alert me when this article is cited.


Figures (4)

FIG. 1
FIG. 1

Geometry near the first grating for obtaining the angle θ1 between the local normal and the central normal (dashed line). Rays leave the entrance aperture on the central normal and are incident on the grating at angle α1 to the local normal.

FIG. 2
FIG. 2

The geometry for obtaining the angle θ2 between the local normal and the central normal at the second grating. The dashed lines give the central normals for both gratings and the ray path between the first and second gratings for the stigmatic wavelength λs which is diffracted from the first grating at angle βs. The solid lines give local normals at both grating and the ray path between the two gratings.

FIG. 3
FIG. 3

Calculated horizontal foci, r 2 h , for the spectrograph of Brueckner et al. as a function of wavelengths. The curves labeled with f numbers, which are used instead of θ1, are obtained by using the correct ruling densities for the gratings. The curve labeled BB is from the paper by Bartoe and Breuckner in which constant ruling densities along the surface of the grating are assumed.

FIG. 4
FIG. 4

Schematic of ray paths near foci in the central plane for λs from ray tracing. The short segments give calculated foci for three f numbers and indicate good agreement between these calculations and the results of ray tracing.

Equations (6)

Equations on this page are rendered with MathJax. Learn more.

tan α 1 = sin θ 1 1 cos θ 1 + 1 / cos β s .
sin β 1 = ( m λ / σ 0 ) cos θ 1 sin α 1 .
θ 2 = 2 β 1 2 β s + θ 1 .
sin β 2 = ( m λ / σ 0 ) cos θ 2 sin α 2 .
r 2 h ( θ 1 0 ) = R ( X 2 + R 2 2 X R cos β 2 ) 1 / 2 X = R cos β 2 [ 1 + 1 cos β 2 ( m λ σ 0 sin 2 ( β 1 β s ) + cos β 1 cos β s 2 cos β s cos β 1 ) ] 1 .
r 2 h ( θ 1 ) = r 2 h ( θ 1 0 ) 0.0115 θ 1 2