• 천문학회보
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• 제40권2호
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• pp.39.3-40
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• 2015

The NISS (Near-infrared Imaging Spectrometer for Star formation history) onboard NEXTSat-1 is the near-infrared instrument optimized to the first small satellite of NEXTSat series. The capability of both imaging and low spectral resolution spectroscopy in the near-infrared range is a unique function of the NISS. The major scientific mission is to study the cosmic star formation history in local and distant universe. For those purposes, the main targets are nearby galaxies, galaxy clusters, star-forming regions and low background regions. The off-axis optical design of the NISS with two linear variable filters is optimized to have a wide field of view ($2deg.{\times}2deg.$) as well as the wide wavelength range from 0.95 to $3.8{\mu}m$. The mechanical structure is considered to endure the launching condition as well as the space environment. The dewar inside the telescope is designed to operate the infrared detector at 80K stage. From the thermal analysis, we confirmed that the telescope and the dewar can be cooled down to around 200K and 80K, respectively in order to reduce the large amount of thermal noise. The stray light analysis is shown that a light outside a field of view can be reduced below 1%. After the fabrications of the parts of engineering qualification model (EQM), the NSS EQM was successfully assembled and integrated into the satellite. To verify operations of the satellite in space, the space environment tests such as the vibration, shock and thermal-vacuum test were performed. Here, we report the results of the critical design review for the NISS.

• 천문학회보
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• 제39권2호
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• pp.102-102
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• 2014

The NISS (Near-infrared Imaging Spectrometer for Star formation history) onboard NEXTSat-1 is the near-infrared instrument onboard NEXTSat-1 which is being developed by KASI. The main scientific targets are nearby galaxies, galaxy clusters, star-forming regions and low background regions in order to study the cosmic star formation history in local and distant universe. After the Preliminary Design Review, we have fixed major specifications of the NISS. The off-axis optical design with 15cm apertureis optimized to obtain a wide field of view ($2deg.{\times}2deg.$), while minimizing the sensitivity loss. The opto-mechanical structure of the NISS was designed to be safe enough to endure in the launching condition as well as the space environment. The tolerance analysis was performed to cover the wide wavelength range from 0.95 to $3.8{\mu}m$ and to reduce the degradation of optical performance due to thermal variation at the target temperature, 200K. The $1k{\times}1k$ infrared sensor is operated in the dewar at 80K stage. We confirmed that the NISS can be cooled down to below 200K in the nominal orbit through a radiative cooling. Here, we report the preliminary design of the NISS.

• 천문학회보
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• 제41권2호
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• pp.64.3-65
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• 2016

The NISS (Near-infrared Imaging Spectrometer for Star formation history) is the near-infrared instrument optimized to the Next Generation of small satellite series (NEXTSat). The capability of both imaging and low spectral resolution spectroscopy in the near-infrared range is a unique function of the NISS. The major scientific mission is to study the cosmic star formation history in local and distant universe. For those purposes, the main observational targets are nearby galaxies, galaxy clusters, star-forming regions and low background regions. The off-axis optical design is optimized to have a wide field of view ($2deg.{\times}2deg.$) as well as the wide wavelength range from 0.95 to $3.8{\mu}m$. Two linear variable filters are used to realize the imaging spectroscopy with the spectral resolution of ~20. The mechanical structure is considered to endure the launching condition as well as the space environment. The compact dewar is confirmed to operate the infrared detector as well as filters at 80K stage. The electronics is tested to obtain and process the signal from infrared sensor and to communicate with the satellite. After the test and calibration of the engineering qualification model (EQM), the flight model of the NSS is assembled and integrated into the satellite. To verify operations of the satellite in space, the space environment tests such as the vibration, shock and thermal-vacuum test were performed. Here, we report the test results of the flight model of the NISS.

• 천문학회보
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• 제42권1호
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• pp.40.1-40.1
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• 2017

The NISS (Near-infrared Imaging Spectrometer for Star formation history) is the near-infrared spectro-photometric instrument optimized to the Next Generation of small satellite series (NEXTSat). To achieve the major scientific objectives for the study of the cosmic star formation in local and distant universe, the spectro-photometric survey covering more than 100 square degree will be performed. The main observational targets will be nearby galaxies, galaxy clusters, star-forming regions and low background regions. The off-axis optics was developed to cover a wide field of view ($2deg.{\times}2deg.$) as well as the wide wavelength range from 0.95 to $2.5{\mu}m$, which were revised based upon the recent test and evaluation of the NISS instrument. The mechanical structure were tested under the launching condition as well as the space environment. The signal processing from infrared sensor and the communication with the satellite were evaluated after the integration into the satellite. The flight model of the NSS was assembled and integrated into the satellite. To verify operations of the satellite in space, the space environment tests such as the vibration, shock and thermal-vacuum test were performed. The accurate calibration data were obtained in our test facilities. Here, we report the test results of the flight model of the NISS.

• 대한전자공학회논문지TC
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• 제38권6호
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• pp.1-10
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• 2001

이 논문에서는 수동 성형 구조를 이용한 파장 분할 다중화 방식 (Wavelength division multiplexing:WDM) 기반의 근거리 망에서 가변 길이의 메시지를 효율적으로 전송할 수 있는 동기 예약 프로토콜을 제안한다. 제어 채널은 데이터 채널 상의 메시지 전송을 조절하기 위하여 사용되며, 시간은 고정 길이의 슬롯으로 동기화 되어 있다. 망은 가변 수의 노트를 수용할 수 있으며, 또한 노트의 수의 변화에 무관하게 동작한다. 따라서 어떠한 '새로운' 노드도 망의 초기화 없이 언제든지 망에 접속할 수 있다. 제안된 프로토콜을 이용하면 데이터 채널과 목적지 주소 충돌 현상도 피할 수 있다. 제안된 프로토콜의 성능은 한 슬롯 시간에 대한 여러 가지 종단간 전파 지연의 경우에 대하여 균형점 분석 (EPA) 방식을 이용하여 분석하고 모의 시험을 통하여 분석 결과를 검증한다. 분석 결과에 따르면, 전파 지연이 성능에 상당한 영향을 미치는 것을 알 수 있다.

• 한국통신학회논문지
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• 제23권4호
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• pp.1035-1044
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• 1998

본 논문에서는 수동 성형 결합기(Passive Star coupler)를 이용한 단일흡 방식의 파장 분할 다중화 네트워크에서 다중 채널 접근 방안과 이에 따른 망 구조가 연구된다. 제안되는 방안에서는 단일흡 방식의 파장 분할 다중화 네트워크에서 핵심이되는 자둥 사용자의 다중 채널 접근을 위해 집중형 스케쥴링 노드(Central Scheduling Node, CSN)를 두었다. 제안되는 방법은 망 내의 모든 노드에서 분산적인 스케쥴링 알고리듬을 수행하는 기존의 다중 채널 접근 방안에서 제기될 수 있는 제어 오버헤드를 줄일 수 있으며 채널 충돌, 목적지 충돌과 같은 충돌이 발생하지 않는 스케쥴링 노드는 간단한 구조를 가지며 여기서 수행되는 스케쥴링 알고리듬 역시 간단하기 때문에 구현상에 장점을 가진다. 그리고 집중형 노드는 데이터 패킷이 아닌 제어 패킷만을 처리하기 때문에 버퍼 요구량 또한 작다. 제안된 네트워크 구조와 다중 접근 방안은 다중큐 다중서버(Multi-Queue Multi-Server)모델로 성능이 분석되며 아울러 시뮬레이션을 통해 성능이 평가된다.

• 한국학교ㆍ지역보건교육학회지
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• 제17권2호
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• pp.71-81
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• 2016

Objectives: The objective and aim of this research is to cultivate a problem-solving ability by analysing the factors that negatively impact on filming sexual behaviour by adolescent. Methods: This research mainly refer to the secondary reference which is conducted a survey of all over the country by National Youth Policy Institute. 3,963 students on the register who participated in survey between 12th of June in 2014 and 15th of July in 2014 was nominated as final recipient for research. Results: Firstly, it has been shown that students who have watched sexual video have more experienced at filming sexual behaviour. In the area of stimulation(p<0.01) and emulation/sharing(p<0.001) except to violation of human rights, adolescent who has experienced at filming sexual behaviour significantly gains more high score than adolescent who does not have experienced statistically. Secondly, as a result of analysis the factors which negatively impact on filming sexual behaviour by adolescent with Binary logistic regression analysis, the adolescent who have shared sexual video was impacted on having an experience at filming sexual behaviour. and the adolescent who had sexual conversation was impacted on having an experience at filming sexual behaviour. Conclusion: A local autonomous entity and school should enforce systematic health education and practical management of mass media rather than unconditional restriction of adolescent's use of smart phone. To carry out this, the state and a local autonomous entity should urge plan for support for settling the instructive environment about using smart phone.

• 천문학회보
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• 제44권1호
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• pp.38.4-38.4
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• 2019

Ultra-diffuse galaxies (UDGs) are intriguing in the sense that they are much larger than dwarf galaxies but have much lower surface brightness than normal galaxies. To date, UDGs have been found only in the local universe. Taking advantage of deep and high-resolution HST images, we search for UDGs in massive galaxy clusters in the distant universe. In this work, we present our search results of UDGs in three massive clusters of the Hubble Frontier Fields: Abell 2744 (z=0.308), Abell S1063 (z=0.348), and Abell 370 (z=0.375). These clusters are the most distant and massive among the host systems of known UDGs. The color-magnitude diagrams of these clusters show that UDGs are mainly located in the faint end of the red sequence. This means that most UDGs in these clusters consist of old stars. Interestingly, we found a few blue UDGs, which implies that they had recent star formation. The radial number densities of UDGs clearly decrease in the central region of the clusters in contrast to those of bright galaxies which keep rising. This implies that a large fraction of UDGs in the central region were tidally disrupted. These features are consistent with those of UDGs in nearby galaxy clusters. We estimate the total number of UDGs (N(UDG)) in each cluster. The abundance of UDGs shows a tight relation with the virial masses (M_200) of thier host systems: M_200 \propto N(UDG)^(1.01+/-0.05). This slope is found to be very close to one, indicating that efficiency of UDGs does not significantly depend on the host environments. Furthermore, estimation of dynamical masses of UDGs indicates that most UDGs have dwarf-like masses (M_200 < 10^11 M_Sun), but a few UDGs have $L{\ast}$-like masses (M_200 > 10^11 M_Sun). In summary, UDGs in distant massive clusters are found to be similar to those in the local universe.

• 천문학회보
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• 제40권1호
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• pp.48.1-48.1
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• 2015

We investigate the role of small-scale and large-scale environments in triggering nuclear activity of the local galaxies using a volume-limited sample with $M_r$ < -19.5 and 0.02 < z < 0.0685 from the Sloan Digital Sky Survey Data Release 7. To fix the mass of the supermassive black hole in its host galaxy, we limit the central velocity dispersion of the sample galaxies. The active galactic nuclei (AGN) host sample is composed of Type II AGNs identified with flux ratios of narrow emission lines with S/N > 6. In this study, we find that the AGN fraction of late-type host galaxies are commonly larger than of early type galaxies. The AGN fraction of host galaxy with late-type nearest neighbor starts to increase as the host galaxy approaches the virial radius of the nearest neighbor (about a few hundred kpc scale). Our result may support the idea that the hydrodynamic interaction with the nearest neighbor plays an important role in triggering the nuclear activity of galaxy. The early-type galaxies in high density regions show decline of AGN activity compared to ones in lower density regions, whereas the direction of the environmental dependence of AGN activity for late-type galaxies is rather opposite. We also find that the environmental dependence of star formation rate is analogous to one of AGN activity except in the high density region.

• 천문학회보
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• 제40권1호
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• pp.79.3-80
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• 2015

Galaxy overdensities such as galaxy clusters and superclusters are the largest gravitationally bound systems in the Universe. Since they contain many different levels of local densities, they are excellent places to test galaxy evolution models in connection to the environments. The environment studies of galaxies at z ~ 1 are important because the environmental quenching seems to be an important mechanism to reduce star formation activities in galaxies at z < 1. However, there have been not many studies about high redshift galaxy clusters at z ~ 1 because of the lack of wide and deep multi-wavelength data. We have used the multi-wavelength data from the UKIDSS DXS (J and K band), the SWIRE (4 IRAC bands), and the PAN-STARRS (g, r, i, z, y bands) in the ELAIS-N1 field. We identified galaxy cluster candidates at 0.2 < z < 1.6 using the multi-wavelength data. We found several superclusters where cluster candidates are concentrated on few tens of Mpc scale. Interestingly, some of the supercluster candidates consist of galaxy clusters which have high blue galaxy. We will present high redshift galaxy cluster and supercluster candidates in ELAIS-N1 field and galaxy properties in different environments including dense clusters and fields.