Abstract

We describe the properties of the Zeiss Universal Birefringent Filter and its optical and electronic interface with the Sacramento Peak Observatory's vacuum telescope. The instrument permits observations of solar intensities, velocities, and/or magnetic fields in rapid succession in any Fraunhofer line in the 410–700-nm wavelength region with high spectral (0.004–0.013 nm) and high spatial (∼1/3 sec of arc) resolution.

© 1975 Optical Society of America

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References

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  1. J. M. Beckers, R. B. Dunn, AFCRL Instrum. Paper 75 (1965).
  2. J. M. Beckers, Appl. Opt. 10, 973 (1971).
    [CrossRef] [PubMed]
  3. J. M. Beckers, Appl. Opt. 11, 681 (1972).
    [CrossRef] [PubMed]
  4. S. Pancharatnam, Proc. Indian Acad. Sci. A41, 130, 137 (1955).
  5. R. B. Dunn, Appl. Opt. 3, 1353 (1964).
    [CrossRef]
  6. J. M. Beckers, AFCRL Instrum. Paper, in preparation (1975).

1972 (1)

1971 (1)

1964 (1)

1955 (1)

S. Pancharatnam, Proc. Indian Acad. Sci. A41, 130, 137 (1955).

Beckers, J. M.

J. M. Beckers, Appl. Opt. 11, 681 (1972).
[CrossRef] [PubMed]

J. M. Beckers, Appl. Opt. 10, 973 (1971).
[CrossRef] [PubMed]

J. M. Beckers, AFCRL Instrum. Paper, in preparation (1975).

J. M. Beckers, R. B. Dunn, AFCRL Instrum. Paper 75 (1965).

Dunn, R. B.

R. B. Dunn, Appl. Opt. 3, 1353 (1964).
[CrossRef]

J. M. Beckers, R. B. Dunn, AFCRL Instrum. Paper 75 (1965).

Pancharatnam, S.

S. Pancharatnam, Proc. Indian Acad. Sci. A41, 130, 137 (1955).

Appl. Opt. (3)

Proc. Indian Acad. Sci. (1)

S. Pancharatnam, Proc. Indian Acad. Sci. A41, 130, 137 (1955).

Other (2)

J. M. Beckers, AFCRL Instrum. Paper, in preparation (1975).

J. M. Beckers, R. B. Dunn, AFCRL Instrum. Paper 75 (1965).

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Figures (7)

Fig. 1
Fig. 1

Optical diagram of Zeiss (Oberkochen) universal birefringent filter. Upper half of the figure shows the optical configuration of a tunable wide (angular) field element and narrow (angular) field element. The lower half shows how nine of these elements are combined to make the UBF. The bandwidth of each of the elements at the line (656.3 nm) is given in angstroms. Tuning of the filter is done by rotation of the entrance polarizer and of the eight thinnest elements. A prefilter is used in front of the filter to eliminate the unwanted maxima and to reduce the heating of the filter by incident sunlight.

Fig. 2
Fig. 2

Optical diagram of the extra element. The element is similar to the wide field element shown in Fig. 1 except that λ/4 waveplates are used on both sides of the element. This permits greater flexibility in the orientation of entrance and exit polarizers.

Fig. 3
Fig. 3

Transmission profile of Zeiss UBF when tuned to 670 nm.

Fig. 4
Fig. 4

Diagram of the optical system connecting the filters to the vacuum solar telescope. S1 and S2 are solar images; LA, LZ, LF, LB, and LTV reimaging lenses; W1, W2, and W3 removable Wollaston prisms; and P1, P2, P3, and P4 folding prisms.

Fig. 5
Fig. 5

(a) Filtergram of a small solar active region at + 0.0 Å. The solar diameter equals 12 times the diagonal of this image. (b) As (a) except taken in the blue wing of the magnesium b1 line (b1 − 0.4 Å).

Fig. 6
Fig. 6

Solar flare of 10 September 1974 as observed near flare maximum in the helium D3 line. Solar limb is in upper left-hand corner.

Fig. 7
Fig. 7

The post flare loop system that developed after the flare shown in Fig. 6 as observed at + 0.6 Å.

Tables (2)

Tables Icon

Table I Properties of Zeiss Universal Birefringent Filter

Tables Icon

Table II Coefficients a0 to a6 of Eq. (2) for the Nine Elements of the Zeiss Universal Birefringent Filter and for the Extra Element

Equations (2)

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Ω = Ω 0 + R ( mod 1 . ) · 180 ° ,
R ( λ ) R 0 = λ 1 ( a 0 + a 1 λ + a 2 λ 2 + a 3 λ 3 + a 4 λ 1 + a 5 λ 2 + a 6 λ 3 ) .

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