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Conceptual Design of the NISS onboard NEXTSat-1
Jeong, Woong-Seob,Park, Sung-Joon,Park, Kwijong,Lee, Dae-Hee,Pyo, Jeonghyun,Moon, Bongkon,Park, Youngsik,Kim, Il-Joong,Park, Won-Kee,Lee, Duk-Hang,Park, Chan,Ko, Kyeongyeon,Matsumoto, Toshio,Takeyama, 한국우주과학회 2014 Journal of Astronomy and Space Sciences Vol.31 No.1
The NISS onboard NEXTSat-1 is being developed by Korea astronomy and space science institute (KASI). For the study of the cosmic star formation history, the NISS performs the imaging spectroscopic observation in the near-infrared range for nearby galaxies, low background regions, star-forming regions and so on. It is designed to cover a wide field of view (2 x 2 deg) and a wide wavelength range from 0.95 to 3.8 μm by using linear variable filters. In order to reduce the thermal noise, the telescope and the infrared sensor are cooled down to 200 K and 80 K, respectively. Evading a stray light outside the field of view and making the most use of limited space, the NISS adopts the off-axis reflective optical system. The primary and the secondary mirrors, the opto-mechanical part and the mechanical structure are designed to be made of aluminum material. It reduces the degradation of optical performance due to a thermal variation. This paper presents the study on the conceptual design of the NISS.
Accuracy Assessment for Measuring Surface Figures of Large Aspheric Mirrors
Young-Soo Kim,Ki-Beom Ahn,Kwijong Park,Il Kweon Moon,양호순 한국광학회 2009 Current Optics and Photonics Vol.13 No.2
At the time that the Keck-I 10m telescope was constructed in 1993, the era of Very Large Telescopes (VLTs) was opened. Now thirteen VLTs are in operation, and the largest of the monolithic mirrors is 8.4 m in diameter. Such monolithic mirrors are mostly aspheric and require high accuracies on the surface figures, reaching up to the diffraction limit. At present, next generation telescopes, Giant telescopes, are being developed. One is the GMT (Giant Magellan Telescope) whose size is 25.4 m in diameter. The primary mirror consists of seven segments figuring elliptical shapes on the surface. The surrounding six segments are off-axis and the edges are steep, as the fast focal ratio is adopted. It means that testing of the mirrors is a challenging task. In this paper, testing methods for the GMT primary mirror are reviewed, and accuracy of measuring devices is assessed. Results and discussions follow.
Detector Mount Design for IGRINS
Oh, Jae Sok,Park, Chan,Cha, Sang-Mok,Yuk, In-Soo,Park, Kwijong,Kim, Kang-Min,Chun, Moo-Young,Ko, Kyeongyeon,Oh, Heeyoung,Jeong, Ueejeong,Nah, Jakyoung,Lee, Hanshin,Jaffe, Daniel T. The Korean Space Science Society 2014 Journal of Astronomy and Space Sciences Vol.31 No.2
The Immersion Grating Infrared Spectrometer (IGRINS) is a near-infrared wide-band high-resolution spectrograph jointly developed by the Korea Astronomy and Space Science Institute and the University of Texas at Austin. IGRINS employs three HAWAII-2RG Focal Plane Array (H2RG FPA) detectors. We present the design and fabrication of the detector mount for the H2RG detector. The detector mount consists of a detector housing, an ASIC housing, a Field Flattener Lens (FFL) mount, and a support base frame. The detector and the ASIC housing should be kept at 65 K and the support base frame at 130 K. Therefore they are thermally isolated by the support made of GFRP material. The detector mount is designed so that it has features of fine adjusting the position of the detector surface in the optical axis and of fine adjusting yaw and pitch angles in order to utilize as an optical system alignment compensator. We optimized the structural stability and thermal characteristics of the mount design using computer-aided 3D modeling and finite element analysis. Based on the structural and thermal analysis, the designed detector mount meets an optical stability tolerance and system thermal requirements. Actual detector mount fabricated based on the design has been installed into the IGRINS cryostat and successfully passed a vacuum test and a cold test.
Detector Mount Design for IGRINS
Jae Sok Oh,Chan Park,Sang-Mok Cha,In-Soo Yuk,Kwijong Park,Kang-Min Kim,Moo-Young Chun,Kyeongyeon Ko,Heeyoung Oh,Ueejeong Jeong,Jakyoung Nah,Hanshin Lee,Daniel T. Jaffe 한국우주과학회 2014 Journal of Astronomy and Space Sciences Vol.31 No.2
The Immersion Grating Infrared Spectrometer (IGRINS) is a near-infrared wide-band high-resolution spectrograph jointly developed by the Korea Astronomy and Space Science Institute and the University of Texas at Austin. IGRINS employs three HAWAII-2RG Focal Plane Array (H2RG FPA) detectors. We present the design and fabrication of the detector mount for the H2RG detector. The detector mount consists of a detector housing, an ASIC housing, a Field Flattener Lens (FFL) mount, and a support base frame. The detector and the ASIC housing should be kept at 65 K and the support base frame at 130 K. Therefore they are thermally isolated by the support made of GFRP material. The detector mount is designed so that it has features of fine adjusting the position of the detector surface in the optical axis and of fine adjusting yaw and pitch angles in order to utilize as an optical system alignment compensator. We optimized the structural stability and thermal characteristics of the mount design using computer-aided 3D modeling and finite element analysis. Based on the structural and thermal analysis, the designed detector mount meets an optical stability tolerance and system thermal requirements. Actual detector mount fabricated based on the design has been installed into the IGRINS cryostat and successfully passed a vacuum test and a cold test.