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TILT CORRECTION FOR A WIDE-FIELD ON-AXIS TELESCOPE USING THE SYMMETRICITY OF OPTICAL ABERRATIONS
Lee, Chung-Uk,Kim, Yunjong,Kim, Seung-Lee,Lee, Dong-Joo,Cha, Sang-Mok,Lee, Yongseok,Kim, Dong-Jin The Korean Astronomical Society 2021 Journal of The Korean Astronomical Society Vol.54 No.4
It is difficult for observers to conduct an optical alignment at an observatory without the assistance of an optical engineer if optomechanical parts are to be replaced at night. We present a practical tilt correction method to obtain the optimal optical alignment condition using the symmetricity of optical aberrations of a wide-field on-axis telescope at night. We conducted coarse tilt correction by visually examining the symmetry of two representative star shapes obtained at two guide chips facing each other, such as east-west or north-south pairs. After coarse correction, we observed four sets of small stamp images using four guide cameras located at each cardinal position by changing the focus positions in 10-㎛ increments and passing through the optimum focus position in the range of ±200 ㎛. The standard deviation of each image, as a function of the focus position, was fitted with a second-order polynomial function to derive the optimal focus position at each cardinal edge. We derived the tilt angles from the slopes converted by the distance and the focus position difference between two paired guide chip combinations such as east-west and north-south. We used this method to collimate the on-axis wide-field telescope KMTNet in Chile after replacing two old focus actuators. The total optical alignment time was less than 30 min. Our method is practical and straightforward for maintaining the optical performance of wide-field telescopes such as KMTNet.
Lee, So Jin,Huh, Myung Sook,Lee, Seung Young,Min, Solki,Lee, Seulki,Koo, Heebeom,Chu, Jun‐,Uk,Lee, Kyung Eun,Jeon, Hyesung,Choi, Yongseok,Choi, Kuiwon,Byun, Youngro,Jeong, Seo Young,Park, Kinam WILEY‐VCH Verlag 2012 Angewandte Chemie Vol.124 No.29
<P><B>Die kondensierte Fassung</B>: Thioliertes Glycolchitosan bildet durch Ladungs‐Ladungs‐Wechselwirkungen und Netzbildung mit polymerisierten siRNAs stabile Nanopartikel (siehe Schema). Die Poly‐siRNA/Glycolchitosan‐Nanopartikel (psi‐TGC) sind in vivo genügend stabil für den systemischen Transport von siRNAs. Das Abschalten von Tumorproteinen durch psi‐TGC resultierte in reduzierten Tumorgrößen und verminderter Tumorvaskularisation.</P>
Photometric Properties of the HW Vir-type Binary OGLE-GD-ECL-11388
Hong, Kyeongsoo,Lee, Jae Woo,Lee, Dong-Joo,Kim, Seung-Lee,Koo, Jae-Rim,Park, Jang-Ho,Lee, Chung-Uk,Kim, Dong-Jin,Cha, Sang-Mok,Lee, Yongseok Astronomical Society of the Pacific 2017 Publications of the Astronomical Society of the Pa Vol.129 No.971
<P>We present the first extensive photometric results for the eclipsing binary OGLE-GD-ECL-11388 with a period of about 3.5 hours located in the Galactic disk. For the photometric solutions, we obtained the BVI light curves from both the KMTNet observations in 2015 and the OGLE -III survey data from 2001-2009, which show striking reflection effects and very sharp eclipses. The light curve synthesis indicates that the eclipsing system is a HW Virtype binary with a mass ratio of q = 0.289, an orbital inclination of i = 81.9 deg, and a temperature ratio between both components of T-2/T-1 = 0.091. A frequency analysis was applied to the light residuals from our binary model; however, no pulsating periodicity from the subdwarf B -type primary component was detected under signal-tonoise amplitude ratios larger than 4 0 A total of 27 minimum epochs spanning 15 yr were used to analyze the eclipse timing variations of OGLE-GD-ECL-11388. It was found that the orbital period has varied due to a continuous period decrease at a rate of dP/dt = -1.1 x 10(-8) day yr(-1) or a sinusoidal oscillation with a semiamplitude of K = 35 s and a cycle of P-3 = 8.9 yr. The period decrease may be explained by an angular momentum loss via magnetic stellar wind braking or may be only a part of the sinusoidal variation. We think the most likely interpretation of the orbital period change, at present, is the light -time effect via the presence of a third body with a mass of M-3 sin i(3) = 12.5 M-Jup, putting it in the boundary zone between planets and brown dwarfs.</P>