• 천문학회지
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• 제33권3호
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• pp.151-158
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• 2000

We conducted a deep CCD observations in V band to obtain stellar density distribution and to determine the distances toward two molecular clouds with anomalous velocity in the Galactic anti-center region. Star count method based on the linear programming technique was applied to the CCD photometric data. We found two prominent peaks at distances of around 1.4 and 2.7 kpc. It is found that the first peak coincides well with stellar density enhancement of B8-A0 stars and the second one with the outer Perseus arm. The effect of the choice of the luminosity function is discussed. The stellar number density distribution is used to derive the distances to the molecular clouds and the visual extinctions caused by the clouds. We found that two molecular clouds are located almost at the same distance of about 1.1 $\pm$ 0.1 kpc, and the peak extinctions caused by the clouds are about 2.2 $\pm$ 0.3 mag in V band.

• 지능정보연구
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• 제22권1호
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• pp.43-61
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• 2016

온라인 쇼핑몰의 상품에 대한 고객 리뷰는 구매자들의 구매 의사결정에 영향을 미치고 있으며 중요한 구전효과의 원천과 의사결정의 정보 원천의 역할을 하고 있다. 한 제품에 대한 리뷰가 무척 많기에 온라인 쇼핑몰들은 고객 리뷰 평가 방안을 도입하였고, 이를 통해 고객들에게 유용하리라고 판단되는 리뷰들을 걸러서 보여주거나 강조할 수 있게 되었다. 리뷰 평가 방안은 해당 리뷰가 도움이 되었는지 혹은 도움이 되지 않았는 지를 리뷰를 읽은 고객이 평가하게 하는 방안이다. Amazon.com은 고객 평가를 바탕으로 총 투표 수 중에서 유용하다는 투표 수의 비율을 리뷰 유용성 지표로 삼고 있으며, Yelp.com은 유용하다는 투표 수 자체를 유용성 지표로 삼고 있다. 본 연구는 고객 리뷰의 감성과 독해 용이성이 리뷰의 유용성에 미치는 영향을 파악하고자 한다. Amazon.com의 고객 리뷰 자료를 활용하여 비율형 유용성 지표를 종속변수로 하는 유사한 연구들이 수행되어 왔다. 본 연구에서는 Yelp.com의 리뷰 자료를 활용하여 가산형 리뷰 유용성 지표인 경우에도 동일한 효과가 존재하는지를 검토하고자 한다. Yelp.com의 음료와 음식 카테고리에 해당하는 업종에 대한 리뷰를 자료로 활용하였으며, 점포의 명성과 인기도 데이터를 파악할 수 있는 170,294개의 리뷰를 분석에 활용하였다. 분석결과는 리뷰의 긍정 정도는 유용 투표수를 늘리는데 음의 영향을 미쳤다. 평가가 긍정적인 리뷰에서는 음의 영향관계가 유의 하였으나, 평가가 부정적인 리뷰에서는 리뷰의 긍정 정도가 유용 투표 수에 미치는 영향은 유의하지 않았다. 독해 용이성은 리뷰가 읽기 어려울 수록 높은 값을 갖으며, 독해의 어려운 정도는 유용 투표수 획득에 음의 영향을 미쳤다. 독해 용이성은 긍정 리뷰, 부정 리뷰 관계없이 모두 음의 영향을 미치는 것으로 분석되었다. 이 결과는 유용 투표수가 0인 리뷰를 포함하여 영과잉 음이항 회귀분석을 수행한 경우와 유용 투표수가 0인 리뷰를 제외하고 음이항 회귀분석을 수행한 경우 모두 동일하게 파악되었다.

• 한국식품과학회지
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• 제42권6호
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• pp.739-742
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• 2010

오미자주 양조에 있어서 중요한 효모 발효의 최적화를 위하여 시중에서 판매되고 있는 다양한 활성건조효모 8종(Lalvin 1116, Lalvin 1118, Lalvin D-47, Lalvin Bourgovin, Parisienne, Fermivin, Red Star Monrachet, Red Star Premier Cuvee)을 선정하여 오미자주의 이화학 및 관능특성을 연구한 결과, pH 및 산도는 각각 3.0-3.3, 1.8-2.4%였으며, 당도는 발효초기 $24^{\circ}Bx$에서 24일 후 $8.4-10.2^{\circ}Bx$이었다. 활성건조효모 8종을 이용하여 제조한 오미자주의 알코올 함량은 10.8-13.0%로 나타났으며 Lalvin D-47과 Red Star Premier Cuvee로 제조한 오미자 발효주의 알코올 함량(13.0%)이 가장 높게 나타났다. 효모수는 Lalvin 1118로 제조한 오미자 발효주가 5.8 log CFU/mL로 가장 낮게 나타났고, 7종의 효모수는 7.0-7.7 log CFU/mL로 비슷하게 나타났다. 색도는 효모의 종류에 따라 L, a, b 값에 모두 변화가 있는 것으로 나타났다. Lalvin 1118을 사용한 오미자 발효주의 맛에 대한 기호도는 6.75로 가장 높았으며, 활성건조효모 8종을 이용한 오미자 발효주의 향과 색의 기호도는 각각 4.90-5.75, 5.25-6.05로 5% 수준에서 유의적 차이를 나타내지 않았고, Lalvin 1118을 사용한 오미자 발효주의 목넘김은 6.65로 가장 높게 나타났다. 위의 결과를 바탕으로, Lalvin 1118을 사용한 오미자 발효주는 알코올 함량(12.0%), 맛($6.75{\pm}1.68$), 목넘김($6.65{\pm}1.50$), 종합적 기호도($6.70{\pm}1.34$)에서 우수한 관능적 특성과 과실주로서의 적절한 알코올 함량을 나타냈으므로 Lalvin 1118은 오미자주 발효에 가장 적합한 것으로 사료된다.

• 천문학회지
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• 제38권2호
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• pp.179-182
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• 2005

We conducted an extremely wide field survey of z ${\~}$ 6 Lyman break galaxies (LBGs) to precisely derive their bright end surface density overcoming the bias due to cosmic variance. We selected out LBG candidates in the Subaru/ XMM-Newton Deep Survey Field (SXDS) over the total of ${\~}1.0\;deg^2$ sky area down to $z_{AB} = 26.0 ({\ge}3{\sigma},\;2'.0 aperture)$ using i' - z' > 1.5 color cut. This sample alone is likely to be contaminated by M/L/T dwarfs, low-z elliptical galaxies, and z ${\~}$ 6 quasars. To eliminate these interlopers, we estimated their numbers using an exponential disk star count model, catalogs of old ellipticals in the SXDS and other field, and a z${\~}$6 quasar luminosity function. The finally derived surface density of z ${\~}$ 6 LBGs was 165 $mag^{-1}\;deg^{-2}$ down to $z_{AB}$ = 26.0 and shows good agreement with previous results from the narrower field survey of HST GOODS.

• 천문학회지
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• 제48권3호
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• pp.177-185
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• 2015

We develop a new auto-guiding system for the Camera for QUasars in the EArly uNiverse (CQUEAN). CQUEAN is an optical CCD camera system attached to the 2.1-m Otto-Struve Telescope (OST) at McDonald Observatory, USA. The new auto-guiding system differs from the original one in the following: instead of the cassegrain focus of the OST, it is attached to the finder scope; it has its own filter system for observation of bright targets; and it is controlled with the CQUEAN Auto-guiding Package, a newly developed auto-guiding program. Finder scope commands a very wide field of view at the expense of poorer light gathering power than that of the OST. Based on the star count data and the limiting magnitude of the system, we estimate there are more than 5.9 observable stars with a single FOV using the new auto-guiding CCD camera. An adapter is made to attach the system to the finder scope. The new auto-guiding system successfully guided the OST to obtain science data with CQUEAN during the test run in 2014 February. The FWHM and ellipticity distributions of stellar profiles on CQUEAN, images guided with the new auto-guiding system, indicate similar guiding capabilities with the original auto-guiding system but with slightly poorer guiding performance at longer exposures, as indicated by the position angle distribution. We conclude that the new auto-guiding system has overall similar guiding performance to the original system. The new auto-guiding system will be used for the second generation CQUEAN, but it can be used for other cassegrain instruments of the OST.

• 한국수산과학회지
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• 제44권1호
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• pp.31-36
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• 2011

This study developed a normal temperature-circulatable retort-sterilized crab analog (RSCA) with a long shelf-life by retort sterilization. We examined the optimum sterilization conditions and quality characteristics of the RSCA. A central composite design for response surface methodology (RSM) was adopted to optimize of the retort sterilization. The central composite design consisted of 11 samples: four factorial points, four star points, and three central points. The sterilization temperature and $F_0$-value for retort sterilization were the independent variables, and the shearing force, whiteness, and sensory score for texture were the dependent variable. The RSM analysis of the multiple response optimization for the RSCA using the Minitap statistical programing gave an $F_0$-value of 3.3 min. at $117.5^{\circ}C$. The RSM analysis also indicated that the sterilization temperature during retort sterilization was the most influential factor, while the $F_0$-value had little effect on the quality of the RSCA. The moisture, pH and volatile basic nitrogen contents of the RSCA product were 73.1%, 7.3 and 17.2 mg/100 g, respectively, and viable cells count was >18 CFU/g. And sensory quality characteristics of this RSCA was similar to those of a commercial crab analog.

• 천문학회지
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• 제50권1호
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• pp.7-20
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• 2017

We carry out the study of $850{\mu}m$ sources in a part of the XMM-LSS field. The $850{\mu}m$ imaging data were obtained by the SCUBA-2 on the James Clerk Maxwell Telescope (JCMT) for three days in July 2015 with an integration time of 6.1 hours, covering a circular area with a radius of 15'. We choose the central area up to a radius of 9'.15 for the study, where the noise distribution is relatively uniform. The root mean square (rms) noise at the center is 2.7 mJy. We identify 17 sources with S/N > 3.5. Differential number count is estimated in flux range between 3.5 and 9.0 mJy after applying various corrections derived by imaging simulations, which is consistent with previous studies. For detailed study on the individual sources, we select three sources with more reliable measurements (S/N > 4.5), and construct their spectral energy distributions (SEDs) from optical to far-infrared band. Redshift distribution of the sources ranges from 0.36 to 3.28, and their physical parameters are extracted using MAGPHYS model, which yield infrared luminosity $L_{IR}=10^{11.3}-10^{13.4}L_{\odot}$, star formation rate $SFR=10^{1.3}-10^{3.2}M_{\odot}yr^{-1}$ and dust temperature $T_D=30-53K$. We investigate the correlation between $L_{IR}$ and $T_D$, which appears to be consistent with previous studies.

• 한국수산과학회지
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• 제54권2호
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• pp.188-193
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• 2021

On March 13, 2018 two postflexion larval specimens (18.28 mm and 16.80 mm in standard length) belonging to the family Cryptacanthodidae, suborder Zoarcoidei were collected from Sokcho and Gangneung in Gangwon Province. The family Cryptacanthodidae comprises 4 species worldwide: 3 in the North Pacific Ocean and 1 in the western North Atlantic Ocean. As a result of analyzing 620 bp of the mtDNA COI region, the two postflexion larvae collected in this study were identified as Cryptacanthodes bergi by 99.5% agreement with C. bergi adult registered in NCBI. Postflexion larvae of C. bergi are compressed with large eyes and radial pectoral fins and the anus located in front of the center of the body. Melanophores were intensively distributed along the dorsal midline, except for caudal peduncle, and sporadically distributed on the back of the anus. In addition, there were limited star-like melanophores on the back of the gut. This species showed 0.058 genetic distance when compared mtDNA COI region of C. aleutensis, and it was well distinguished in the distribution pattern of black vesicles of the head, count and measurement traits. Considering the morphological and ecological characteristics of this species, we suggest a new Korean name, " Gwisin-jang-gaeng-i ".

• 천문학회지
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• 제29권spc1호
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• pp.63-64
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• 1996

The nature of distant faint blue field galaxies remains a mystery, despite the fact that much attention has been devoted to this subject in the last decade. Galaxy counts, particularly those in the optical and near ultraviolet bandpasses, have been demonstrated to be well in excess of those expected in the 'no-evolution' scenario. This has usually been taken to imply that galaxies were brighter in the past, presumably due to a higher rate of star formation. More recently, redshift surveys of galaxies as faint as B$\~$24 have shown that the mean redshift of faint blue galaxies is lower than that predicted by standard evolutionary models (de-signed to fit the galaxy counts). The galaxy number count data and redshift data suggest that evolutionary effects are most prominent at the faint end of the galaxy luminosity function. While these data constrain the form of evolution of the overall luminosity function, they do not constrain evolution in individual galaxies. We are carrying out a series of observations as part of a long-term program aimed at a better understanding of the nature and amount of luminosity evolution in individual galaxies. Our study uses the luminosity-linewidth relation (Tully-Fisher relation) for disk galaxies as a tool to study luminosity evolution. Several studies of a related nature are being carried out by other groups. A specific experiment to test a 'no-evolution' hypothesis is presented here. We have used the AUTOFIB multifibre spectro-graph on the 4-metre Anglo-Australian Telescope (AAT) and the Rutgers Fabry-Perot imager on the Cerro Tolalo lnteramerican Observatory (CTIO) 4-metre tele-scope to measure the internal kinematics of a representative sample of faint blue field galaxies in the red-shift range z = 0.15-0.4. The emission line profiles of [OII] and [OIII] in a typical sample galaxy are significantly broader than the instrumental resolution (100-120 km $s^{-l}$), and it is possible to make a reliable de-termination of the linewidth. Detailed and realistic simulations based on the properties of nearby, low-luminosity spirals are used to convert the measured linewidth into an estimate of the characteristic rotation speed, making statistical corrections for the effects of inclination, non-uniform distribution of ionized gas, rotation curve shape, finite fibre aperture, etc.. The (corrected) mean characteristic rotation speed for our distant galaxy sample is compared to the mean rotation speed of local galaxies of comparable blue luminosity and colour. The typical galaxy in our distant sample has a B-band luminosity of about 0.25 L$\ast$ and a colour that corresponds to the Sb-Sd/Im range of Hub-ble types. Details of the AUTOFIB fibre spectroscopic study are described by Rix et al. (1996). Follow-up deep near infrared imaging with the 10-metre Keck tele-scope+ NIRC combination and high angular resolution imaging with the Hubble Space Telescope's WFPC2 are being used to determine the structural and orientation parameters of galaxies on an individual basis. This information is being combined with the spatially resolved CTIO Fabry-Perot data to study the internal kinematics of distant galaxies (Ing et al. 1996). The two main questions addressed by these (preliminary studies) are: 1. Do galaxies of a given luminosity and colour have the same characteristic rotation speed in the distant and local Universe? The distant galaxies in our AUTOFIB sample have a mean characteristic rotation speed of $\~$70 km $s^{-l}$ after correction for measurement bias (Fig. 1); this is inconsistent with the characteristic rotation speed of local galaxies of comparable photometric proper-ties (105 km $s^{-l}$) at the > $99\%$ significance level (Fig. 2). A straightforward explanation for this discrepancy is that faint blue galaxies were about 1-1.5 mag brighter (in the B band) at z $\~$ 0.25 than their present-day counterparts. 2. What is the nature of the internal kinematics of faint field galaxies? The linewidths of these faint galaxies appear to be dominated by the global disk rotation. The larger galaxies in our sample are about 2"-.5" in diameter so one can get direct insight into the nature of their internal velocity field from the $\~$ I" seeing CTIO Fabry-Perot data. A montage of Fabry-Perot data is shown in Fig. 3. The linewidths are too large (by. $5\sigma$) to be caused by turbulence in giant HII regions.