안녕하십니까.

오는 수요일(5월 29일) 오후 4:00에 아래와 같이 2024년 상반기 정규 콜로키움이 진행될 예정입니다.

발표 후에는 연사와의 대화시간(5:00-5:40) 및 저녁 식사가 예정되어 있으니 많은 참여 부탁드립니다.

발표자: 안교훈 박사 (KASI, NAOJ)

호스트: 이성호

장소: 장영실홀 331-2 및 원격 연결

일시: 5월 29일 (수) 오후 4:00

접속주소: https://zoom.us/j/92444602963?pwd=VXJzWE1zd3VkYmZ1SjRMeXRFQy9kQT09

교육학점: 천문연 소속 현장참석자의 경우 필수 0.5 학점 부여

제목: Taking the twinkle  out of the Night Sky

초록: 

When you look at the sky on a clear night, you probably enjoy the twinkling of stars. However, if you are an astronomer, you might find it extremely annoying. Almost as soon as telescopes were invented, astronomers realized that the quality of images was limited by atmospheric turbulence, which distorts short exposure and blurs long exposure astronomical images. Even if we have 8-10 meter class telescopes now, without AO, the telescope's angular resolution would be limited by the atmospheric turbulence “seeing” -the size of the blurred image is almost two orders of magnitude worse than what the telescopes could achieve. 
To overcome this limitation, the first concept of adaptive optics (AO) was proposed by H. W. Babcock in 1953 for ground-based telescopes. However, the technology for AO components was not mature enough then. From the late-1980s, astronomers became interested in applying the AO technique to astronomy. As of today, AO has rapidly been developed over the past 70 years and has become a state-of-the-art technique. The wavefront aberration induced by atmospheric turbulence can be measured by a wavefront sensor and compensated for by a wavefront corrector, thereby deblurring the images in part or entirely.
This presentation introduces astronomical science that can be achieved with modern AO technologies. We also present recent technology trends for the AO system, such as types of wavefront sensors (WFSs) and wavefront correctors. In the wavefront sensors section, we present Shack-Hartmann WFS, pyramid WFS, and curvature WFS. In the wavefront corrector section, we introduce wavefront correctors such as deformable mirrors and a spatial liquid modulator.
Lastly, we introduce modern AO systems with multiple laser and nature guide stars for various applications.

진행언어: 한국어

슬라이드언어: 영어

원격 접속 방법 :

A.뚜웹 브라우저: Chrome을 추천하며 아래 주소를 실행시 Zoom 구동을 위한 프로그램이 설치될 수 있음

B. 접속 주소: https://zoom.us/j/92444602963?pwd=VXJzWE1zd3VkYmZ1SjRMeXRFQy9kQT09

C. 유의사항: 접속 후 "마이크는 뮤트로 설정" - 기본설정은 뮤트로 되어있음 > 질의 응답시간에는 마이크를 사용해서 질문 가능함

2024년 상반기 천문연구원 콜로키움 일정

https://www.kasi.re.kr/kor/publication/post/notice/29938

(위 일정은 연사분의 상황에 따라서 변경될 수 있습니다.)

천문연 콜로키움 위원회 (김종수, 선광일, 이창원, 문홍규, 노혜림, 한정열)

운영위원회 (김진호, 송영범, 오재석, 윤용민, 조영수, 홍경수) 

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Dear all,

The KASI's regular colloquium is scheduled at May. 29, as shown below.

A conversation session with speakers and dinner are scheduled after the colloquium.

Speaker: Dr. Kyohoon Ahn (KASI, NAOJ)

Host: Sungho Lee

Place: Jang Yeong-sil Hall 331-2 & Online

Time: May 29 (Wed) 4:00 pm 

Access: https://zoom.us/j/92444602963?pwd=VXJzWE1zd3VkYmZ1SjRMeXRFQy9kQT09

KASI Educational credits: 0.5 educational credits are awarded to off-line attendees.

Title: Taking the twinkle  out of the Night Sky

Abstract: 

When you look at the sky on a clear night, you probably enjoy the twinkling of stars. However, if you are an astronomer, you might find it extremely annoying. Almost as soon as telescopes were invented, astronomers realized that the quality of images was limited by atmospheric turbulence, which distorts short exposure and blurs long exposure astronomical images. Even if we have 8-10 meter class telescopes now, without AO, the telescope's angular resolution would be limited by the atmospheric turbulence “seeing” -the size of the blurred image is almost two orders of magnitude worse than what the telescopes could achieve. 
To overcome this limitation, the first concept of adaptive optics (AO) was proposed by H. W. Babcock in 1953 for ground-based telescopes. However, the technology for AO components was not mature enough then. From the late-1980s, astronomers became interested in applying the AO technique to astronomy. As of today, AO has rapidly been developed over the past 70 years and has become a state-of-the-art technique. The wavefront aberration induced by atmospheric turbulence can be measured by a wavefront sensor and compensated for by a wavefront corrector, thereby deblurring the images in part or entirely.
This presentation introduces astronomical science that can be achieved with modern AO technologies. We also present recent technology trends for the AO system, such as types of wavefront sensors (WFSs) and wavefront correctors. In the wavefront sensors section, we present Shack-Hartmann WFS, pyramid WFS, and curvature WFS. In the wavefront corrector section, we introduce wavefront correctors such as deformable mirrors and a spatial liquid modulator.
Lastly, we introduce modern AO systems with multiple laser and nature guide stars for various applications.

Language: Korean

Slide Language: English

Remote access procedure:

A. Web browser: Chrome - When executing the address below, a program for additional zoom operation can be installed.

B. Access: Go to  https://zoom.us/j/92444602963?pwd=VXJzWE1zd3VkYmZ1SjRMeXRFQy9kQT09

C. Notice: After join, Please mute your microphone. - The default setting is microphone mute. > After the presentation, during the Q&A session, you can use the microphone to ask questions.

2024A KASI Colloquium Schedule

https://www.kasi.re.kr/kor/publication/post/notice/29938

(This schedule may vary depending on the speakers' schedule.)

KASI Colloquium committee (Jongsoo Kim, Kwang-Il Seon, Chang Won Lee, Hong-Kyu Moon, Hyerim Noh, Jeong-Yeol Han)

Working committee (Jinho Kim, Youngbum Song, Jae Sok Oh, Yongmin Yoon, Youngsoo Jo, Kyeongsoo Hong)