• Title/Summary/Keyword: Coude mirror

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Wavefront Distortion caused by High Energy Laser Beam in the Relay Mirrors of the Laser Beam Director (고에너지 레이저빔에 의해 유발된 광집속장치 반사경 광파면 왜곡)

  • Choi, Jong-Ho;Kim, Yeon-Soo
    • Korean Journal of Optics and Photonics
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    • v.19 no.2
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    • pp.144-149
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    • 2008
  • Thermal distortion of the laser mirrors which are the Coude mirrors of the laser beam director and the wavefront error caused by the thermal distortion are studied. Coude mirrors consist of three relay mirrors and one fast steering mirror. The mirrors have reflectivity of 99.5% with respect to the laser wavelength of $3.8\;{\mu}m$, and absorption of 500 W per second. Thermal distortion and its related wavefront errors are studied with laser beam irradiation for 5 seconds. For the relay mirror, the wavefront error is 334 nm_PV, 98 nm rms and for fast steering mirror, $11.5\;{\mu}m$_PV, $3{\mu}m$ rms.

Optimal Design of a Coudé Mirror Assembly for a 1-m Class Ground Telescope

  • Jaehyun Lee;Hyug-Gyo Rhee;Eui Seung Son;Jeon Geon Kang;Ji-Young Jeong;Pilseong Kang
    • Current Optics and Photonics
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    • v.7 no.4
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    • pp.435-442
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    • 2023
  • These days, the size of a reflective telescope has been increasing for astronomical observation. An additional optical system usually assists a large ground telescope for image analysis or the compensation of air turbulence. To guide collimated light to the external optical system through a designated path, a coudé mirror is usually adopted. Including a collimator, a coudé mirror of a ground telescope is affected by gravity, depending on the telescope's pointing direction. The mirror surface is deformed by the weight of the mirror itself and its mount, which deteriorates the optical performance. In this research, we propose an optimization method for the coudé mirror assembly for a 1-m class ground telescope that minimizes the gravitational surface error (SFE). Here the mirror support positions and the sizes of the mount structure are optimized using finite element analysis and the response surface optimization method in both the horizontal and vertical directions, considering the telescope's altitude angle. Throughout the whole design process, the coefficients of the Zernike polynomials are calculated and their amplitude changes are monitored to determine the optimal design parameters. At the same time, the design budgets for the thermal SFE and the mass and size of the mount are reflected in the study.