• 천문학회보
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• 제41권1호
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• pp.67.1-67.1
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• 2016

We observed two star forming regions, N159 and N160, in the Large Magellanic Cloud with SIRPOL, the polarimeter of the Infrared Survey Facility (IRSF) in South Africa. The photometric and polarimetric observations are done in three near-infrared bands, J, H, and Ks. We measured Stokes parameters of point sources and calculated their degrees of polarization and polarization angles. The polarization vector map shows complex features associated with dust and gas structures. Overall features of the magnetic field in N159 and N160 regions are different from each other and appear to be related to local environments, such as interior and boundary of shell structure, existence of star-forming HII regions, and boundaries between HII regions and dense dark clouds. We discuss the relation between the structure of magnetic field and the local properties of dust and gas in N159 and N160 regions by comparing our polarization vector map with images of $H{\alpha}$, mid-infrared, and $^{12}CO$ emissions, respectively by WFI of MPG/ESO telescope, Spitzer IRAC, and NANTEN.

• Journal of Astronomy and Space Sciences
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• 제32권1호
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• pp.91-99
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• 2015

The Korean Solar Radio Burst Locator (KSRBL) is a solar radio spectrograph observing the broad frequency range from 0.245 to 18 GHz with the capability of locating wideband gyrosynchrotron bursts. Due to the characteristics of a spiral feed, the beam center varies in a spiral pattern with frequency, making a modulation pattern over the wideband spectrum. After a calibration process, we obtained dynamic spectra consistent with the Nobeyama Radio Polarimeter (NoRP). We compared and analyzed the locations of bursts observed by KSRBL with results from the Nobeyama Radioheliograph (NoRH) and Atmospheric Imaging Assembly (AIA). As a result, we found that the KSRBL provides the ability to locate flaring sources on the Sun within around 2'.

• 반도체디스플레이기술학회지
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• 제17권3호
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• pp.70-74
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• 2018

In typical spectroscopic ellipsometry, the optical and geometrical properties of thin film and nano pattern can be obtained by measuring the polarization state of light reflected/transmitted from the object by rotating a analyzer or a compensator. We proposed a snapshot spectroscopic ellipsometric system based on a modified Michelson interferometer to overcome the time-consuring measurement principle due to rotating part. The proposed system provides spectral ellipsometric parameters (psi, delta) in real time by using a single spectral interference signal generated in the interferometric polarization module. However, it has a long-term stability problem resulting in delta(k) drift. In this paper, it is experimentally proved that the drift problem is caused by anisotropic refractive index change of the beam intersection layer in beam splitter of interferometer.

• 천문학회보
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• 제40권2호
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• pp.28.3-29
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• 2015

$Ly{\alpha}$ nebulae, or "$Ly{\alpha}$ blobs", are extended (~100 kpc), bright (L[$Ly{\alpha}$] ~ 1044 erg/s) clouds of $Ly{\alpha}$-emitting gas. The origin of the $Ly{\alpha}$ emission remains unknown, but recent theoretical work suggests that measuring the polarization could discriminate among powering mechanisms. we will discuss current status of $Ly{\alpha}$ polarization observations at high-redshift and our on-going survey program. We will present the first narrow-band, imaging polarimetry of a $Ly{\alpha}$ blob, B3 J2330+3927 at z=3.09, with an embedded, radio-loud AGN (C. You et al. in prep.). The AGN lies near the blob's $Ly{\alpha}$ emission peak and its radio lobes align roughly with the blob's semi-major axis. With the SPOL polarimeter on the MMT telescope, we map the polarization in a grid of circular apertures of radius 0.6" (4.4 kpc), detecting a significant (>$2{\sigma}$) polarization fraction P% in 10 apertures and achieving strong upper-limits (as low as 2%) elsewhere. The degree of the polarization map increases from P% ~ 5% at ~5 kpc from the blob center to ~20% at the outer part (~30 kpc). The detections are distributed asymmetrically, roughly along the blob's major axis. The polarization angles (${\Theta}$) are mostly perpendicular to this axis. These results are consistent with the picture that $Ly{\alpha}$ photons produced at the AGN (or the host galaxy) are resonantly scattered away from the center. Higher polarization fraction on the radio jet suggests that the gas is more optically thin along the jet than the off-axis region.

• 천문학회보
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• 제40권2호
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• pp.36.2-36.2
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• 2015

We report the first detection of linearly polarized emission at an observing wavelength of 350 mum from the radio-loud active galactic nucleus 3C 279. We conducted polarization observations for 3C 279 using the SHARP polarimeter in the Caltech Submillimeter Observatory on 2014 March 13 and 14. For the first time, we detected the linear polarization with the degree of polarization of $13.3%{\pm}3.4%$ (3.9sigma) and the electric vector position angle (EVPA) of $34.^{\circ}7{\pm}5.^{\circ}6$. We also observed 3C 279 simultaneously at 13, 7, and 3.5 mm in dual polarization with the Korean very long baseline interferometry (VLBI) Network on 2014 March 6 (single dish) and imaged in milliarcsecond (mas) scales at 13, 7, 3.5, and 2.3 mm on March 22 (VLBI). We found that the degree of linear polarization increases from 10% to 13% at 13 mm to 350 mum and the EVPAs at all observing frequencies are parallel within < $10^{\circ}$ to the direction of the jet at mas scale, implying that the integrated magnetic fields are perpendicular to the jet in the innermost regions. We also found that the Faraday rotation measures RM are in a range of $-6.5{\times}102{\sim}-2.7{\times}103$ rad m-2 between 13 and 3.5 mm, and are scaled as a function of wavelength:| {RM}| ${\backslash}propto$ {lambda }-2.2. These results indicate that the millimeter and sub-millimeter polarization emission are generated in the compact jet within 1 mas scale and affected by a Faraday screen in or in the close proximity of the jet.

• 한국미생물·생명공학회지
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• 제28권6호
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• pp.355-360
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• 2000

Candida rugosa IFO0750의 UV-변이주를 제조하여 butyric acid를 D-$\beta$-hydroxybutyrin acid(이하 D-$\beta$-HBA)로 전환하는 데 이용하였다. 후보 변이주 중 활성이 가장 높은 Candida rugosa CM42를 이용하여 발효를 수행한 후 NMR 분석, polarimeter 분석 등을 통하여 생성된 물질이 D-$\beta$-HBA 임을 확인하였다. Chemostar 배양을 이용하여 D-$\beta$-HBA 발효 생산의 주요 영향인자를 분석하였으며, 균체의 활성을 나타내는 비생산성의 최대치는 균체의 비증식 속도를 0.06, 발효조 내의 glucose와 butyric acid의 농도를 각각 10g/L와 8.7 g/L로 각각 유지 할 때 얻어졌다. 회분식 배양 중에 glucose와 butyric acid를 공급하여 발효조 내의 glucose 및 butyric acid 농도를 최적조건으로 유지하는 fed-batch 발효를 수행하였다. 배양 180 시간 후에 D-$\beta$-HBA 농도가 약 12.4 g/L에 도달하였으며 회분식 발효에 비하여 4.7배 증가하였다.

• 한국미생물·생명공학회지
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• 제15권6호
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• pp.369-374
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• 1987

하상 오니 및 토양으로부터 D-$\alpha$-Amino-$\varepsilon$-Caprolactam(DAC)의 자화능이 우수한 균을 분리하여 Alcaligenes eutrophus로 동정하였다. Alcaligenes eutrophus A52의 생육을 위한 배양조건은 배양 초기 최적 pH가 6.0, 최적온도는 3$0^{\circ}C$, 최적 DAC 농도는 0.2%로서 50시간 배양으로 0.2% DAC를 거의 다 자화하여 정지기에 도달하였다. 본 균은 탄소원으로 glucose와 fructose, 질소원으로는 NH$_4$Cl, NH$_4$NO$_3$, (NH$_4$)$_2$SO$_4$ 및 NaNO$_3$를 잘 자화하였다. 탄소원 및 질소원으로 Iysine, glutamate를 잘 이용하였으나 그 밖의 아미노산 자화능은 낮았다. 균체로부터 추출한 3.1mg의 단백질에 상당하는 무세포 추출 액으로 0.5% DAC를 55%에서 12시간 반응시킨 생성물은 약 98% L-Iysine으로 확인되었다.

• 한국임상약학회지
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• 제8권2호
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• pp.147-158
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• 1998

The purpose of this study was to test the stability of TPN basic solutions containing amino acids and dextrose. Test solutions containing $4.25\%$ amino acids in $25\%$ dextrose (central TPN basic solution) or $4.25\%$ amino acids in $10\%$ dextrose (peripheral TPN basic solution) were prepared. Two different amino acids solutions $(Fravasol^{(R)}\;vs\;Freamine^{(R)})$ were tested. The samples were taken from each admixture and stored in the evacuated, sterile containers at $2{\sim}8^{\circ}C$ and ambient room temperature. Each sample was analyzed at 0, 3, 7, 14 and 30 days of storage. Each amino acid was analyzed by amino acid analyzer. Dextrose content was measured by polarimeter. The pH and chromagen formation were also monitored. The decomposition was measured by the changes in concentration of amino acids and dextroser TPN basic $solution-Freamine^{(R)}$ admixture stored at $2\sim8^{\circ}C$ were stable for 30 days. Central and peripheral TPN basic solutions stored at room temperature were stable for 7 days and 14 days, respectively. There were no changes in color for 30 days by naked eye. Amino acid concentrations in TPN basic $solution-Fravasol^{(R)}$ admixture stored at $2\sim8^{\circ}C$ or room temperature were stable for 30 days. But, significant color change was detected according to passing time. In conclusion, Peripheral TPN basic $solution-Fravasol^{(R)}$ admixture stored at room temperature and in refrigerator were stable for 3 days and 7 days, respectively. However, central TPN basic solution-Fravasol admixtures were unstable. Therefore, it is recommended that it should be admixed right before use.

• 천문학회보
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• 제41권1호
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• pp.31.4-32
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• 2016

Observing the solar atmosphere with ground-based telescopes in the near-infrared has a number of advantages when compared to classical measurements in visible wavelengths. One of them comes from the magnetic sensitivity of spectral lines, which varies as ${\lambda}_g$, where g is the effective $Land{\acute{e}}$ factor of the transition. This wavelength dependence makes the near-infrared range adequate to study subtle spatial or temporal variations of the magnetic field. Spectral lines, such as the photospheric Fe I $1.5648{\mu}m$ spectral line, with a $Land{\acute{e}}$ factor g=3, have often been used in the past for this type of studies. To study the chromosphere, the Ca II IR triplet and the He I $1.0830{\mu}m$ triplet are the most often observed lines. The latter has the additional advantage that the photospheric Si I $1.0827{\mu}m$ is close enough so that photosphere and chromosphere can be simultaneously recorded with a single detector in a spectrograph. The instrument TIP (Tenerife Infrared Polarimeter) has been continuously operating since 1999 at the 70-cm German VTT of the Observatorio del Teide and has been recently moved to the 1.5-m German GREGOR. During all this time, results have been obtained concerning the nature of the weak photospheric magnetic field of the quiet sun, magneto-acoustic wave propagation, evolution with the cycle of sunspot magnetic fields, photospheric and chromospheric magnetic field in emerging regions, magnetic field in chromospheric structures such as filaments, prominences, flares, and spicules, etc. In this talk, I will review the main results obtained after all these observations and mention the main challenges for the future. With its novel polarization-free design and a complete suite of instruments aimed at simultaneous (imaging and spectroscopic) observations of the solar photosphere and chromosphere, the EST (European Solar Telescope) will represent a major world-wide infrastructure to understand the physical nature of all these phenomena.

• 천문학회보
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• 제46권1호
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• pp.45.2-46
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• 2021

The Hayabusa 2 mission target asteroid (162173) Ryugu is a near-Earth, carbonaceous (C-type) asteroid. Before the arrival, this asteroid is expected to be covered with mm- to cm- sized grains through the thermal infrared observations [1]. These grains are widely understood to be formed by past impacts with other celestial bodies and fractures induced by thermal fatigue [2]. However, the close-up images by the MASCOT lander showed lumpy boulders but no abundant fine grains [3]. Morota et al. suggested that there would be submillimeter particles on the top of these boulders but not resolved by Hayabusa 2's onboard instruments [4]. Hence, we conducted polarimetry of Ryugu to investigate microscopic grain sizes on its surface. Polarimetry is a powerful tool to estimate physical properties such as albedo and grain size. Especially, it is known that the maximum polarization degree (Pmax) and the geometric albedo (pV) show an empirical relationship depending on surface grain sizes [5]. We observed Ryugu from UT 2020 November 30 to December 10 at large phase angles (ranging from 78.5 to 89.7 degrees) to derive Pmax. We modified TRIPOL (Triple Range Imager and POLarimeter, [6]) to attach to the 1.8-m telescope at the Bohyunsan Optical Astronomy Observatory (BOAO). With this instrument, we observed the asteroid and determined linear polarization degrees at the Rc-band filter. We obtained sufficient data sets from 7 nights at this observatory to determine the Pmax value, and collaborated with other observatories in Japan (i.e., Hokkaido University, Higashi-Hiroshima, and Nishi-Harima) to acquire linear polarization degrees of the asteroid from total 24 nights observations with large phase angle coverage (From 28 to 104 degrees). The observational results have been published in Kuroda et al. (2021) [7]. We thus found the dominance of submillimeter particles on the surface of Ryugu from the comparison with other meteorite samples from the campaign observation. In this presentation, we report our activity to modify the TRIPOL for the 1.8-m telescope and the polarimetric performance. We also examine the rotational variability of the polarization degree using the TRIPOL data.