• Journal of Astronomy and Space Sciences
• /
• 제29권1호
• /
• pp.69-77
• /
• 2012

This report describes the inception, development and extensive use over 30 years of elliptical polarimeters at the University of Pennsylvania. The initial Mark I polarimeter design utilized oriented retarder plates and a calcite Foster-Clarke prism as the analyzer. The Mark I polarimeter was used on the Kitt Peak 0.9 m in 1969-70 to accomplish a survey of approximately 70 objects before the device was relocated to the 0.72 m reflector at the Flower and Cook Observatory. Successive generations of automation and improvements included the early-80's optical redesign to utilize a photoelastic modulated wave plate and an Ithaco lock-in amplifier-the photoelastic modulating polarimeter. The final design in 2000 concluded with a fully remote operable device. The legacy of the polarimetric programs includes studies of close binaries, pulsating hot stars, and luminous late-type variables.

• Journal of Korean Vacuum Science & Technology
• /
• 제6권3호
• /
• pp.116-119
• /
• 2002

A performance of a new positron polarimeter is investigated by simulation using a charged-particle trajectory program. The results of the ray tracing are presented along with the details of the design parameters and projected system performance. A ray tracing analysis indicates that this design is capable of effectively transmitting positrons at beam energies varying from 0.1 to 30 keV within the beam diameter of 2-6mm. However, the observed reflection of the positrons(lower than 2 keV) at 12 kGauss indicated that further refinement of beam design is needed to produce a better positron polarimeter.

• 한국정보디스플레이학회:학술대회논문집
• /
• 한국정보디스플레이학회 2006년도 6th International Meeting on Information Display
• /
• pp.809-813
• /
• 2006

We have studied the optical properties of the biaxial film such as fast axis, retardance and the change of polarization state between crossed polarizer using dual rotating retarder polarimeter. We have developed a novel simulation model, which could explain well the experimental results, and found that it could be used to optimize the compensation film in LCD for improving wide-viewing property.

• 한국통신학회:학술대회논문집
• /
• 한국통신학회 1998년도 추계종합학술발표회 논문집(상)
• /
• pp.839-842
• /
• 1998

• 한국자기학회:학술대회 개요집
• /
• 한국자기학회 2004년도 동계학술연구발표회 논문개요집
• /
• pp.193-193
• /
• 2004

• 천문학회보
• /
• 제28권2호
• /
• pp.57-57
• /
• 2003

• 한국광학회지
• /
• 제23권6호
• /
• pp.241-245
• /
• 2012

광학 활성의 측정은 고분자, 광통신, 천문학, 물리학 등과 관련된 분야에서 매우 중요한 주제가 되고 있다. 따라서 이와 같은 경향은 이 주제를 학부 실험에 반영되도록 할 필요가 있다. 이 실험에서는 파장이 543 nm인 헬륨-네온 레이저와 학부용으로 시판되는 파스코 사의 검출기, 회전 엔코더 및 자료 수집기를 사용해서 저비용으로 믿을만한 결과를 주는 편광계를 구성하고 관련 이론과 실험식을 제시하였다. 장치 성능을 검증하기 위해 반파장판을 표준 시료로 사용했으며, 그 후 농도가 30 %인 설탕 용액을 측정 시료로 사용해 비회전을 측정해 보았다. 설탕의 비회전 측정 결과는 +76 deg.cc/g.dm로써, 기존의 CRC 자료들의 내삽을 통해 추정된 값과 거의 동일했으므로, 대부분 학부 수준의 실험에서도 충분히 수용 가능하다고 판단되었다.

• 한국광학회지
• /
• 제15권6호
• /
• pp.547-554
• /
• 2004

z-축 방향으로 진행하는 Ti:LiNbO$_3$, 광도파로와 전기광학효과를 이용하여 집적광학형 편광조절기를 구현하였다. 소자는 λ/4-λ/2-λ/4 wave-plate들로 구성되었으며, 각 wave-plate에 인가되는 전압들에 따라 나타나는 위상변화량과 이에 대응되는 편광모드 변환을 정량적으로 검토하고, 폴래리미터 (polarimeter)와 Poincare 구 좌표계를 이용하여 편광 조절기의 동작 상태를 체계적으로 측정하였다. 제작된 편광조절기는 각 wave-plate들의 선택과 인가전압에 따라 어떠한 입력 편광 상태도 특정한 출력 편광상태로 변화시킬 수 있음을 확인하였다.

• 천문학회보
• /
• 제36권2호
• /
• pp.86.1-86.1
• /
• 2011

We are developing a new universal spectropolarimeter on the Domeless Solar Telescope (DST) at the Hida Observatory to realize precise spectropolarimetric observations in a wide range of wavelength in visible and near infrared. The system aims to open a new window of plasma diagnostics by using Zeeman effect, Hanle effect, Stark effect, impact polarization, and atomic polarization for measuring the external magnetic field, electric field, or an anisotropy in the excitation of the atoms. The polarimeter is a successor of formerly developed polarimeter on DST, which make possible to observe a polarization in a photospheric spectral line with polarimetric accuracy of 10-2 (Kiyohara et al. 2004). The new system consists of a 60cm aperture vacuum telescope, a high dispersion vacuum spectrograph, polarization modulator / analyzer composed of a rotating waveplate whose retardation is constant for a wide range of wavelength and Wallaston prism, and a fast and large format CCD camera or IR camera. Spectral images in both orthogonal polarizations are taken simultaneously with a frame rate of ~20Hz while the waveplate rotates continuously in a rate of 1rev./sec. Thus It takes 5 ~ 60 sec to observe polarization with accuracy of 10-3 in a wide wavelength range (400 - 1100nm). We also examined a polarimetric model of the telescope with accuracy of 10-3 to calibrate instrumental polarization on some wavelengths. In this talk, I will focus on the performance of the instrument.

• 천문학회보
• /
• 제36권2호
• /
• pp.85.2-85.2
• /
• 2011

A new infrared spectro-polarimeter was installed in 2008 onto the Solar Flare Telescope of NAOJ in the Mitaka headquarters. The Solar Flare Telescope had been operated previously as a filter-based magnetograph and obtained vector magnetograms of active regions with the Fe I 630.3nm line during 1992 - 2005. The aim of this new instrument is to measure the distribution of magnetic helicity over the whole Sun and for an extended period with high magnetic sensitivity in the infrared wavelengths. This spectro-polarimter is able to obtain polarizations in both photospheric and chromospheric layers. In order to take full Stokes profiles, we observe Fe I 1564.8 nm and He I 1083.0 nm lines (with the neighboring photospheric Si line) for the photospheric and chromospheric magnetic field vectors, respectively. The infrared detector of this instrument is a $640{\times}512$-pixel InGaAs camera produced by a Belgian company Xenics. The frame rate of the camera is 90 frames/sec. The 640-pixel row of this camera is set along the spectrograph slit of the polarimeter. Since the slit only covers the solar hemisphere, a full disk map is obtained by raster scanning the solar disk twice. A magnetic map is made of about $1200{\times}1200$ pixels with a pixel size of 1.8 arcsec. It generally takes 1.5 hours to scan the whole Sun. Although some issues on the instrument calibration still remain, a few maps of the whole Sun at the two wavelengths are now taken daily. In this presentation, we will introduce the instrument and present some observational results.