• Journal of Korean Ophthalmic Optics Society
• /
• v.20 no.2
• /
• pp.167-175
• /
• 2015

Purpose: The new-type rangefinder, which is using the biprism principle, is introduced to develop the range finder which can be easily carried by soldiers, and in order to realize those technologies specifically, we try to develop a scope for military rangefinder by doing optical design which can secure enough space to move the biprism. Methods: After setting up the verious initial condition to realize two kinds of goals, that are the securement of enough space to move the biprism and the easy-exchangeability of two kinds of biprisms, and then the optical system was optimized by using optical design program CodeV in order to minimize the finite ray aberrations. Results: We designed the biprism housing to makes it possible to swap the two kinds of biprisms. It was appeared that the Schmidt prism is suitable as erecting prism which can make sure the space to move the biprism. 16.5 mm was good for the face length of Schmidt prism. The optical system with a Schmidt prism and a biprism was designed, and the finite ray aberrations was minimized. Conclusions: We developed a 5X scope for an optical rangefinder using a biprism and a Schmidt prism with 16.5 mm face length. This scope is valid for the optical system which has the effective field angle of ${\pm}3.6^{\circ}$, and the finite ray aberrations are well controlled within the ${\pm}8.95^{\prime}$.

• Publications of The Korean Astronomical Society
• /
• v.8 no.1
• /
• pp.17-31
• /
• 1993

In order to check whether the 4-degree objective prism spectra can be used for deep spectroscopic studies of galactic structure, we measured the Rose(1984)'s seven indices between 3500 A and 4400 A for 19 Hyades stars on the Kiso Schmidt prism plate, K3496. By comparing the $4^{\circ}$-indices with those of Rose(1984), we have found that $H{\delta}/FeI$, $H{\gamma}/4325$, and P(3912)/P(CN) measured on the 4-degree prism spectra, are still useful for the derivation physical parameters.

• Journal of The Korean Astronomical Society
• /
• v.33 no.2
• /
• pp.75-80
• /
• 2000

In order to identify the candidates of emission-line galaxies inside the southern Hydra Void, photo-graphic objective-prism observations with the UK Schmidt Telescope were carried out using the Tech-Pan films for five fields. All observed prism plates were scanned with the APM Facility and the scanned data was processed to determine the APM plate parameters and to draw spectra. For all galaxy spectra, the emission features, the distance between emission features of H$\beta$4861, [OIII]${\lambda}{\lambda}$ 4959, 5007 and the overlapping by nearby objects were investigated by eyeballing. A total of 7 candidates of emission-line galaxies inside the Hydra Void were identified.

• Publications of The Korean Astronomical Society
• /
• v.11 no.1
• /
• pp.49-55
• /
• 1996

In order to discover the candidates of emission-line galaxies towards Hydra Void, objective-prism observations using U.K. Schmidt Telescope were carried out. To search the emission feature of [0III]${\lambda}{\lambda}4959,5007$ for all objects on the plate, all observed prism plates were scanned with APM at the Royal Observatory and the copied direct R plates were scanned with PDS Microdensitometer operating in the Inter- University Center for National Science Research Facilities. By utilizing the "XIMTOOL" package, both spectral and direct images for the same field were displayed simultaneously on up and down windows separately. In case of distinct emission features for a certain object, corresponding direct object on the other window was examined through eyeballing to see whether this object is a galaxy. Through this procedure, we discovered in total 33 candidates of emission-line galaxies in a single field.

• The Bulletin of The Korean Astronomical Society
• /
• v.39 no.2
• /
• pp.119.1-119.1
• /
• 2014

We present the scanned digital images and their preliminary analysis results of objective-prism plates taken with the Michigan Curtis Schmidt telescope at Cerro Tololo Inter-American Observatory. In order to separate an individual spectrum of a star, it should be required to identify each field star in the plate. Using the PPM(Position and Proper Motion) catalog, we are verifying which star corresponds to the spectrum in a plate. In addition to this, we plan to devise the method for wavelength calibration in each spectrum. Finally we will make them for public use, not only for professional astronomers but also for high school and college students for encouraging them to be interested in the astronomy, especially astronomical spectroscopy and stellar astronomy.