Abstract

A simple scheme of an optical setup to enhance the spectral resolution of diffraction gratings without increasing the number of grooves is presented. A plane-parallel mirror pair, which consists of a 100% reflectivity mirror and a 50% reflectivity mirror, is placed upon a grating. For certain values of the mirror gap and the angle between the grating and the mirrors, the effective size of the grating doubles, as does the resolution. Using a grating of 830grooves/mm and a narrow-band diode laser that is tunable around 773 nm, we experimentally demonstrated an enhancement of the resolution by a factor of 2.

© 2011 Optical Society of America

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References

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  1. N. Savage, Nat. Photon. 3, 601 (2009).
    [CrossRef]
  2. E. Hecht, Optics, 4th ed. (Addison Wesley Longman, 2002).
  3. L. Kleint, A. Feller, and D. Gisler, Astron. Astrophys. 529, A78 (2011).
    [CrossRef]
  4. S. Persson and T. Geballe, Publ. Astron. Soc. Pac. 94, 381 (1982).
    [CrossRef]
  5. D. Erskine, J. Edelstein, W. Feuerstein, and B. Welsh, The Astrophysical Journal Letters 592, L103 (2003).
  6. C. Yang, K. Shi, P. Edwards, K. Shi, and Z. Liu, Opt. Express 18, 23529 (2010).
    [CrossRef]
  7. C. Yang, P. Edwards, K. Shi, and Z. Liu, Opt. Lett. 36, 2023 (2011).
    [CrossRef]
  8. E. Lee and J. Lee, J. Opt. Soc. Korea 15, 216 (2011).
    [CrossRef]

2011 (3)

2010 (1)

2009 (1)

N. Savage, Nat. Photon. 3, 601 (2009).
[CrossRef]

2003 (1)

D. Erskine, J. Edelstein, W. Feuerstein, and B. Welsh, The Astrophysical Journal Letters 592, L103 (2003).

1982 (1)

S. Persson and T. Geballe, Publ. Astron. Soc. Pac. 94, 381 (1982).
[CrossRef]

Edelstein, J.

D. Erskine, J. Edelstein, W. Feuerstein, and B. Welsh, The Astrophysical Journal Letters 592, L103 (2003).

Edwards, P.

Erskine, D.

D. Erskine, J. Edelstein, W. Feuerstein, and B. Welsh, The Astrophysical Journal Letters 592, L103 (2003).

Feller, A.

L. Kleint, A. Feller, and D. Gisler, Astron. Astrophys. 529, A78 (2011).
[CrossRef]

Feuerstein, W.

D. Erskine, J. Edelstein, W. Feuerstein, and B. Welsh, The Astrophysical Journal Letters 592, L103 (2003).

Geballe, T.

S. Persson and T. Geballe, Publ. Astron. Soc. Pac. 94, 381 (1982).
[CrossRef]

Gisler, D.

L. Kleint, A. Feller, and D. Gisler, Astron. Astrophys. 529, A78 (2011).
[CrossRef]

Hecht, E.

E. Hecht, Optics, 4th ed. (Addison Wesley Longman, 2002).

Kleint, L.

L. Kleint, A. Feller, and D. Gisler, Astron. Astrophys. 529, A78 (2011).
[CrossRef]

Lee, E.

Lee, J.

Liu, Z.

Persson, S.

S. Persson and T. Geballe, Publ. Astron. Soc. Pac. 94, 381 (1982).
[CrossRef]

Savage, N.

N. Savage, Nat. Photon. 3, 601 (2009).
[CrossRef]

Shi, K.

Welsh, B.

D. Erskine, J. Edelstein, W. Feuerstein, and B. Welsh, The Astrophysical Journal Letters 592, L103 (2003).

Yang, C.

Astron. Astrophys. (1)

L. Kleint, A. Feller, and D. Gisler, Astron. Astrophys. 529, A78 (2011).
[CrossRef]

J. Opt. Soc. Korea (1)

Nat. Photon. (1)

N. Savage, Nat. Photon. 3, 601 (2009).
[CrossRef]

Opt. Express (1)

Opt. Lett. (1)

Publ. Astron. Soc. Pac. (1)

S. Persson and T. Geballe, Publ. Astron. Soc. Pac. 94, 381 (1982).
[CrossRef]

The Astrophysical Journal Letters (1)

D. Erskine, J. Edelstein, W. Feuerstein, and B. Welsh, The Astrophysical Journal Letters 592, L103 (2003).

Other (1)

E. Hecht, Optics, 4th ed. (Addison Wesley Longman, 2002).

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Figures (3)

Fig. 1.
Fig. 1.

Field translation induced by a pair of plane-parallel mirrors, M1 and M2. Under certain conditions, the translated field phase can be identical to the original diffracted one. Inset: mirror deployment scheme for more than one mirror pair.

Fig. 2.
Fig. 2.

Calculated results of the phase mismatch between the original diffracted field and the translated field. (a) The mirror planes are orthogonal to the grating surface. Notice the large phase variation. (b) As the mirror planes rotate 4 degrees clockwise from the orthogonal direction, the phase mismatch curve becomes flat near a specified wavelength.

Fig. 3.
Fig. 3.

The spectral line shapes measured with only the bare grating (a) without a mirror pair, (b) with a mirror pair that is orthogonal to the grating surface, and (c) with a mirror pair that is rotated 4 degrees clockwise from the orthogonal direction according to the calculated result. A reduced spectral linewidth is preserved over the entire wavelength range.

Equations (4)

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2dcos(θ+θm(λ))=nλ(n=integer),
b(sinθm(λ)sinθi)=mλ(m=integer),
nb2dm=sin(θ+θm(λ))cosθm(λ)atλ=λ0.
bλmcosθm(λ)=tan(θ+θm(λ)),

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