The design of the Near Space Optical Survey-alpha (NSOS-α) telescope, encouraged by Korea Astronomy and Space Science Institute (KASI) aims to discover and catalog near-Earth asteroids, especially Potentially Hazardous Asteroids (PHAs). To achieve this goal, an optical telescope with a 1.5m class primary mirror and a 5 square degree field of view will be installed and operated at Cerro Tololo Inter-American Observatory (CTIO) in Chile. The wide field telescope is under development and being designed by a collaboration between KASI and the NSF’s National Optical-Infrared Astronomy Research Laboratory (NOIRLab). A prime focus configuration was adopted and designed with a seven element wide field corrector (WFC). The main mechanical design philosophy was scaled, modified, and revised based on the Korea Microlensing Telescope Network (KMTNet). The NSOS-α telescope will be the first dedicated observation facility for asteroid survey in the southern hemisphere using a 1.5-meter class telescope. In this paper, a summary of the optical and mechanical assemblies designed for the NSOS-α telescope will be addressed.
The OWL@OUKA is the Optical Wide-field patroL (OWL) facility designed and built by Korea Astronomy and Space Science Institute (KASI) and installed in 2015 at Oukaimeden Observatory. For the first time we used the opportunities offered by this instrument for the detection and monitoring the exoplanets by the transit method. In this work, we present, first, the validation of the OWL@OUKA for the transit method by reporting the observations we have done to calibrate the instrument in order to chose the best exposure time for a given star. We report on the results obtained form the first observations, in V filter, of a known transit event of the planet Qatar-1b, a hot Jupiter orbiting a metal-rich K dwarf star (Teff = 5013.0, Vmag = 12.84). We have used the software AstroImagJ to reduce the data and the software EXOFASTv2 to fit the transit and extract the planetary parameters, where we obtained a transit depth 0.0207+0.0044-0.0040 and a planetary radius of 1.09 ± 0.11 RJ , that are in good consistence with the discovery paper. Given the good results obtained, we moved to the second stage of our program, which consists of tracking TESS candidates.
Access to the requested content is limited to institutions that have purchased or subscribe to SPIE eBooks.
You are receiving this notice because your organization may not have SPIE eBooks access.*
*Shibboleth/Open Athens users─please
sign in
to access your institution's subscriptions.
To obtain this item, you may purchase the complete book in print or electronic format on
SPIE.org.
INSTITUTIONAL Select your institution to access the SPIE Digital Library.
PERSONAL Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.