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초고에너지 우주선과 고층대기 극한방전 현상 관측을 위한 TUS(Tracking Ultraviolet Setup) 및 Pinhole Camera 개발 및 진행상황
김민빈,김지은,김예원,나고운,박일흥,서정은,이직,정애라,Kim, Min-Bin,Kim, Ji-Eun,Kim, Ye-Won,Na, Go-Un,Park, Il-Heung,Seo, Jeong-Eun,Lee, Jik,Jeong, Ae-Ra 한국천문학회 2012 天文學會報 Vol.37 No.2
TUS(Tracking Ultraviolet Setup)는 5x1019 eV 이상의 초고에너지 우주선의 스펙트럼과 그 기원, 그리고 고층대기 극한방전 현상(TLE) 관측을 위한 우주망원경이다. 위성 Lomonosov의 탑재체로 2013년에 발사예정에 있으며 지구로부터 550km 상공에서 지구를 돌며 3년 이상 임무를 수행할 예정이다. TUS는 크게 반사경과 Detector Module 두 부분으로 나뉜다. 7개의 육각형 프레넬 거울을 이용한 $2m^2$ 크기의 반사경과 256개의 PMT(Photo Multiplier Tube)로 구성된 Detector Module을 이용하여 지구 대기에서 초고에너지 우주선에 의해 발생하는 UV fluorescence와 Cherenkov light를 관측한다. TUS Detector Module의 한 부분인 Pinhole Camera는 본 연구단의 기술로 직접 개발한 탑재체로서 TUS 반사경을 통하지 않고 두개의 $8{\times}8$ 어레이 MAPMT (Multi Anode PMT)가 직접 지구를 바라보며 고층대기 극한방전 현상을 관측한다. Pinhole camera는 TUS의 시야각을 포괄하는 넓은 시야각을 가지고 있으며 빠른 트리거 시스템으로 고층대기 극한 방전 현상을 관측하며, 이 방전현상과 TUS가 관측하는 초고에너지 우주선과의 상관 관계를 연구한다. 현재 TUS 및 Pinhole Camera는 러시아에서 조립되어 우주환경 인증 시험 및 인터페이스 테스트가 진행되고 있다. 본 발표에서는 TUS와 Pinhole Camera를 소개하고 현재까지의 진행상황 및 테스트 결과에 대해 보고하고자 한다.
The Slewing Mirror Telescope of the Ultra Fast Flash Observatory Pathfinder
정수민,최지녕,정애라,김민빈,김석환,김예원,김지은,이직,임희진,나고운,남지우,박일흥,서정은,Jeong, Soomin,Choi, Ji Nyeong,Jung, Aera,Kim, Min Bin,Kim, Sug-Whan,Kim, Ye Won,Kim, Jieun,Lee, Jik,Lim, Heuijin,Na, Go Woon,Nam, Jiwoo,Park, Il Hung 한국천문학회 2012 天文學會報 Vol.37 No.2
The Slewing Mirror Telescope (SMT) is a key telescope of Ultra-Fast Flash Observatory (UFFO) space project to explore the first sub-minute or sub-seconds early photons from the Gamma Ray Bursts (GRBs) afterglows. The first realization of UFFO is the 20kg UFFO-Pathfinder (UFFO-P) to be launched on board the Russian Lomonosov satellite in 2013 by the Soyuz-2 rocket. Once the UFFO Burst Alert & Trigger Telescope (UBAT) detects the GRBs, Slewing mirror (SM) will rotate to bring the GRB into the SMT's field of view instead of slewing the entire spacecraft. SMT can image the UV/Optical counterpart with about 4-arcsec accuracy. However it will provide a important understanding of the GRB mechanism by measuring the sub-minute optical photons from GRBs. SMT can respond to the trigger over $35^{\circ}{\times}35^{\circ}$ wide field of view within 1 sec by using Slewing Mirror Stage (SMS). SMT has 10-cm Ritchey-Chretien telescope and $256{\times}256$ pixilated Intensified Charge-Coupled Device (ICCD) on focal plane. In this paper, we discuss the overall design of UFFO-P SMT instrument and payloads development status.
최지녕,최연주,정수민,정애라,김민빈,김지은,김석환,김예원,이직,임희진,민경욱,나고운,남지우,박일흥,서정은,Choi, Ji Nyeong,Choi, Yeon Ju,Jeong, Soomin,Jung, Aera,Kim, Min Bin,Kim, Ji Eun,Kim, Sug-Whan,Kim, Ye Won,Lee, Jik,Lim, Heuijin,Min, Kyung Wo 한국천문학회 2012 天文學會報 Vol.37 No.2
UFFO Burst Alert & Trigger telescope (UBAT) is one of major instruments of UFFO-Pathfinder. The UBAT aims at 10 arcmin resolution localization of Gamma Ray Bursts with X-ray coded mask technique. It has $400mm{\times}400mm$ coded mask aperture, hopper, shielding and detector module with effective area of $191cm^2$. The detector module consists of an assembly of 36 64-ch MAPMTs and $25mm{\times}25mm$ pixellated YSO crystal array, and associated analog and digital electronics of about 2500 channels. We performed a vibration test using a dummy MAPMT with the detector module structure to measure the indused stress applied onto the MAPMT. We designed a sub-structure on the detector module to avoid the resonance that would otherwise deforms the detector module structure. A finite element analysis confirms the reduction of the load acceleration down to 12g. The experimental results are to be reported. Consequently, it proves that the MAPMT arrays of the flight UBAT detector module structure would survive in the space launch environment.
Design and Construction of Detector Module for UFFO Burst Alert & Trigger Telescope
정애라,최지녕,최연주,정수민,김지은,김민빈,김석환,김예원,이직,임희진,민경욱,나고운,남지우,박일흥,Jung, Aera,Ahmad, Salleh,Barrillon, Pierre,Brandt, Soren,Budtz-Jorgensen, Carl,Castro-Tirado, Alberto J.,Chen, Pisin,Choi, Ji Nyeong,Choi, Yeon J 한국천문학회 2012 天文學會報 Vol.37 No.2
One of the key aspects of the upcoming Ultra-Fast Observatory (UFFO) Pathfinder for Gamma-Ray Bursts(GRBs) identification will be the UFFO Burst Alert & Trigger Telescope(UBAT), based on a novel space telescope technique. The UBAT consists of coded mask, hopper, and detector module(DM). The UBAT DM consists of YSO crystal arrays, multi-anode photo mulipliers, and readout electronics. We will present the design and construction of the UBAT DM, and the response of the UBAT DM to X-ray sources.
The Burst Alert and Trigger Telescope for the Ultra Fast Flash Observatory Pathfinder
나고운,최지녕,최연주,정수민,정애라,김지은,김민빈,김석환,김예원,이직,임희진,민경욱,박일흥,서정은,Na, Go Woon,Choi, Ji Nyeong,Choi, Yeon Ju,Jeong, Soomin,Jung, Aera,Kim, Ji Eun,Kim, Min Bin,Kim, Sug-Whan,Kim, Ye Won,Lee, Jik,Lim, Heuijin,Min, 한국천문학회 2012 天文學會報 Vol.37 No.2
The Ultra Fast Flash Observatory (UFFO) pathfinder is a payload system on-board the Russian satellite Lomonosov, scheduled to be launched in 2013. The main purpose of the UFFO pathfinder is to observe the early photons from Gamma-Ray Bursts. It consists of two instruments. The first instrument is the UFFO Burst Alert X-ray Trigger telescope (UBAT) for the fast-trigger and detection of GRB location, and the second is the Slewing Mirror Telescope (SMT) for the observation of the UV/optical afterglow from the GRB located by the UBAT. It will provide the first-ever systematic study of UV/optical emission far earlier than 1 sec after trigger. We will present the design, fabrication and the preliminary performance of the UBAT.
The Electronics system of the Ultra Fast Flash Observatory Pathfinder
김지은,최지녕,최연주,정수민,정애라,김민빈,김석환,김예원,이직,임희진,민경욱,나고운,박일흥,서정은,Kim, Ji Eun,Choi, Ji Nyeong,Choi, Yeon Ju,Jeong, Soomin,Jung, Aera,Kim, Min Bin,Kim, Sug-Whan,Kim, Ye Won,Lee, Jik,Lim, Heuijin,Min, Kyung Wook,N 한국천문학회 2012 天文學會報 Vol.37 No.2
The Ultra Fast Flash Observatory (UFFO) pathfinder consists of the UFFO Burst Alert X-ray Trigger telescope (UBAT) and the Slewing Mirror Telescope (SMT). They are controlled by the UFFO Data Acquisition system (UDAQ). The UBAT triggers Gamma-Ray Bursts(GRBs) and sends the position information to the SMT. The SMT slews the motorized mirror rapidly to the GRB position to take the UV/Optical data within a second after trigger. The UDAQ controls each instrument, communicates with the satellite, collects the data from UBAT and SMT, and transfers them to the satellite. Each instrument uses its own field programmable gates arrays (FPGA) for low power consumption and fast processing, and all functions are implemented in FPGAs without using microprocessors. The entire electronics system of the UFFO pathfinder including architecture, control, and data flow will be presented.