• 천문학회지
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• 제40권3호
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• pp.61-65
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• 2007

The 2-1 and 5-4 transitions of SiO have been observed toward the Sgr B2 region, including the Principal Cloud(the GMC containing Sgr B2(M)) and its surroundings. The morphology and velocity structure of the SiO emission show a close resemblance with the HNCO Ring feature, identified by Minh & Irvine(2006), of about 10 pc in diameter, which may be expanding and colliding with the Principal Cloud. Three SiO clumps have been found around the Ring, with total column densities $N_{SiO}{\sim}1{\times}10^{14}cm^{-2}$ at the peak positions of these clumps. The fractional SiO abundance relative to $H_2$ has been estimated to be ${\sim}(0.5-1){\times}10^{-9}$, which is about two orders of magnitude larger than the quiet dense cloud values. Our SiO observational result supports the existence of an expanding ring, which may be triggering active star formations in the Principal Cloud.

• 천문학회지
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• 제37권4호
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• pp.131-135
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• 2004

The $H_2S\;(2_{2,0} - 2_{1,1})$ line emission is observed to be strongly localized toward Sgr B2(M), and emissions from other positions in the more extended SgrB2 region are almost negligible. $H_2S$ is thought to form effectively by the passage of the C-type shocks but to be quickly transformed to $SO_2$ or other sulfur species (Pineau des Forets et al. 1993). Such a shock may have enhanced the $H_2S$ abundance in Sgr B2(M), where massive star formation is taking place. But the negligible emission of $H_2S$ from other observed positions may indicate that these positions have not been affected by shocks enough to produce $H_2S$, or if they have experienced shocks, $H_2S$ may have transformed already to other sulfur-containing species. The $SO_2\;22_{2,20} - 22_{1,21}$ line was also observed to be detectable only toward the (M) position. The line intensity ratios of these two molecules appear to be very similar at Sgr B2(M) and IRAS 16239-2422, where the latter is a region of low-mass star formation. This may suggest that the shock environment in these two star-forming regions is similar and that the shock chemistry also proceeds in a similar fashion in these two different regions, if we accept shock formation of these two species.

• Journal of Astronomy and Space Sciences
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• 제21권4호
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• pp.233-242
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• 2004

우리은하중심에 있는 Sgr B2 분자운 지역에 대하여 $HCO^{+}1-0$ 천이선을 관측하여 이 지역의 역학적, 화학적 특성을 연구하였다. 이 지역에는 속도가 ${\sim}50$과 ${\sim}100kms^{-1}$인 가스 구름이 상호작용을 하고 있는 것으로 보이며, 이에 의하여 Sgr B2 분자운의 새로운 별-탄생이 촉진될 수 있다고 여겨진다. 속도성분이 ${\sim}50kms^{-1}$인 지역에서, 뚜렷한 가스 집중을 보이는 'OF38 분자운'('Odenwald & Fazio FIR 38' Cloud)이 새로이 발견되었다. 이 분자운의 $HCO^+$ 칼럼밀도는 $N(HCO^+)=(2-5){\times}10^{14}cm^{-2}$, 크기는 약 15pc이며, 총 질량은 약 $10^6M_{\odot}$으로 계산되었다. 그리고 이 Sgr B2 지역에는 속도 범위가 $100kms^{-1}$에 이르는 큰 규모의 터뷸런트한 컴포넌트가 넓게 퍼져 존재하며, 이 성분의 $N(HCO^+)=1{\times}10^{13}cm^{-2}$으로 상당한 양으로 존재함을 알 수 있다. 그러나 이 지역에서 관측되는 $HCO^+$의 생성반응은, 기존에 제안되었던 $H^{+}_3$와 CO의 반응보다는, 충격파의 영향에 의하여 증가하는 $C^+$와 OH의 반응에서 보다 효과적으로 생성될 것으로 보인다. 새로이 발견된 'OF38 분자운'의 물리 화학적 특성을 밝히는 일은 앞으로의 과제라고 생각한다.

• 대한한방내과학회지
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• 제30권2호
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• pp.288-297
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• 2009

Objective : Inflammatory cytokines have a close relationship to insulin dependent diabetes mellitus (IDDM). The inhibitory effect of Smilacis Glabrae Rhizoma (SGR) were examined on production of nitric oxide (NO), prostaglandin $E_2$ $(PGE_2)$, synthase (iNOS), cyclooxygenase-2 (COX-2), tumor necrosis factor-${\alpha}$ (TNF-${\alpha}$) and NF-${\kappa}$B activation in Raw 264.7 cells. Methods: Raw 264.7 cells were pretreated with SGR(20, 50, 100 ${\mu}g$/ml), and then cultured with lipopolysaccharides (LPS). Cell viability was measured by MTT assay; inhibition of NO, $PGE_2$, and TNF-${\alpha}$ production were measured by Griess reagent and enzyme-linked immunosorbent assay(ELISA). Induction of COX-2 and iNOS were determined by western blotting analysis. Inhibition of NF-${\kappa}$B was measured by immunofluorescence assay (IFA). Results: SGR inactivated NF-${\kappa}$B, and inhibited the production of NO, iNOS, and $PGE_2$. Inhibition of COX-2 and TNF-${\alpha}$ could not be confirmed. Conclusions: From the above result. SGR was found to have an anti-inflammatory effect of inhibition of NO, iNOS, and $PGE_2$ production via inhibition of NF-${\kappa}$B.

• Journal of Astronomy and Space Sciences
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• 제28권1호
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• pp.13-16
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• 2011

The $CH_3OH$ $4_2-5_1$ E transition was observed toward the Sgr B2 region, including the Principal Cloud and its surroundings. This methanol transition shows an extended emission along the 2'N cloud, which is believed to be colliding with the Principal Cloud and may trigger the massive star formation in this cloud. This extended methanol emission may also suggest that the 2'N cloud is under shocks. We derive total methanol column density $N(CH_3OH)\;=\;2.9{\pm}0.3{\times}10^{14}\;cm^{-2}$ toward the peak position of the extended emission. The fractional abundance of methanol is about 10.9, relative to the estimated total $H_2$ abundance, which is similar to the methanol abundances in quiet gas phase.

• 광물과 암석
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• 제35권2호
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• pp.111-123
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• 2022

본 연구는 자연계에서 가장 흔하게 관찰되는 두 그린 러스트(green rust) 광물인 carbonate green rust (CGR)과 sulfate green rust (SGR)을 공침법(co-precipitation)을 통해 각각 합성하고, 이들의 형성 메커니즘 및 이화학적 특성들을 체계적으로 규명하였다. X-선 회절(XRD) 분석 및 리트벨트 정련 수행 결과, 본 합성 조건에서 이차광물상 없이 이중층수산화물로서 CGR과 SGR이 합성됨을 확인하였다. 또한, 각각의 구조 파라미터는 CGR의 경우 a(=b)축 = 3.17 Å, c축 = 22.52 Å이고, SGR의 경우 a(=b)축 = 5.50 Å, c축 = 10.97 Å이며, 이들의 미결정 크기는 각각 (003)면 기준 57.8 nm와 (001)면 기준 40.1 nm로 밝혀졌다. 주사전자현미경/에너지 분산형 분광분석(SEM/EDS) 결과, CGR과 SGR은 모두 육각 판상의 전형적인 이중층수산화물 결정 형상을 보이지만 탄소(C)와 황(S)의 함량은 서로 다르게 나타났다. 퓨리에 변환 적외선(FT-IR) 분광 분석결과, 탄산염(CO₃^2-)와 황산염(SO₄^2-) 이온들이 각각 CGR과 SGR의 층간 음이온으로 밝혀졌고, 이는 XRD를 활용한 광물상 동정 결과와 잘 일치한다. 철 용액으로의 수산화이온(OH^-) 주입 시간에 따른 혼합 용액의 pH와 Eh, 그리고 잔류 철 농도의 비율(Fe(II):Fe(III)) 측정 결과, 시간에 따른 차이는 있지만 두 green rusts 모두 1단계 전구체 형성, 2단계 중간 생성물로의 상변환, 그리고 3단계 green rust로의 상변환과 에이징에 의한 결정성장으로 이어지는 결정 형성 메커니즘을 보이는 것으로 판단된다. 본 연구는 공침법을 통해 CGR과 SGR을 안정적으로 합성하고 이들의 형성 메커니즘과 이화학적 특성을 규명함으로써, green rust를 활용한 응용 연구 및 산업 활용에 원천 기초자료를 제공할 것으로 기대된다.

• Food Science and Biotechnology
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• 제16권2호
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• pp.238-242
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• 2007

Square root models were developed for predicting the kinetics of growth of Listeria monocytogenes in sesame leaves as a function of temperature (4, 10, or $25^{\circ}C$). At these storage temperatures, the primary growth curves fit well ($R^2=0.898$ to 0.980) to a Gompertz equation to obtain lag time (LT) and specific growth rate (SGR). The square root models for natural logarithm transformations of the LT and SGR as a function of temperature were obtained by SAS's regression analysis. As storage temperature ($4-25^{\circ}C$) decreased, LT increased and SGR decreased, respectively. Square root models were identified as appropriate secondary models for LT and SGR on the basis of most statistical indices such as coefficient determination ($R^2=0.961$ for LT, 0.988 for SGR), mean square error (MSE=0.l97 for LT, 0.005 for SGR), and accuracy factor ($A_f=1.356$ for LT, 1.251 for SGR) although the model for LT was partially not appropriate as a secondary model due to the high value of bias factor ($B_f=1.572$). In general, our secondary model supported predictions of the effects of temperature on both LT and SGR for L. monocytogenes in sesame leaves.

• 천문학회보
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• 제40권2호
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• pp.52.2-52.2
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• 2015

SgrA* located in the center of the Milky Way is of great interest to understand the physics of supermassive black hole(SMBH) and the interaction of the G2 cloud around SgrA* with the accretion flow which was expected since 2013. In order to seize this rare opportunity, KVN and VERA Array (so called, KaVA) has started an intensive monitoring program of SgrA* at 22/43 GHz where scatter broadening is reduced compared to lower frequency VLBI observations. We present the results of KaVA SgrA* observation together with Takahagi (32m) and Yamaguchi (32m) telescopes at 22 GHz on March 24, 2013. We have tested both a standard amplitude calibration methods using the Tsys and antenna gain information and a template amplitude calibration method which uses a peak of H2O maser line of nearby maser source (SgrB2), and found that the latter method is useful when an accuracy of Tsys measurement or antenna gain of a telescope is poor. In our comparison, the difference between the two methods is around 20% (~5% for the KVN and ~15% for the VERA when the elevation is above $20^{\circ}$). We also imaged SgrA* with a total flux of ~0.7 Jy at 22GHz, and fitted an elliptical Gaussian model which has a size of ~2.5mas for major axis and ~1.7mas for minor axis, respectively.

• 천문학회지
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• 제31권2호
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• pp.117-125
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• 1998

We have observed the 10-9 transitions of $HC_3N$ and its $^{13}C$ substitutes ($H^{13}CCCN,\;HC^{13}CCN$, and $HCC^{13}CN$), and the vibration ally excited 12-11 ($v_r=1$) $HC_3N$ transition toward the Sgr B2 molecular cloud. The observed $HC_3N$ emission shows an elongated shape around the Principal Cloud ($\~$4.5 pc in R.A. $\times$ 7.4 pc in Decl.). The optically thin $H^{13}CCCN$ line peaks around the (N) core and we derive the total column density $N(H^{13}CCCN) = 4 {\times}10^{13} cm^{-2}$ at this position. Toward the 2' N cloud which shows the peculiar chemistry, the $HC_3N$ lines show enhancements compared to the extended envelope. The shocks of the 2' N may have resulted in the enhancement of $HC_3N$. The hot component of $HC_3N$ is strongly concentrated around the (N) core and its HPW is $\~$0.9 pc in diameter. We derive the lower limit of the abundance ratio $N(HC_3N)/N(H^{13}CCCN)$ to be larger than 40 in most regions except the (M) and (N) cores. The fractionation processes of $^{13}C $at this region may not be as effective as previously reported.

• 천문학회지
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• 제26권1호
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• pp.73-78
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• 1993

We have mapped the $C_3H_2\;2_{12}-1_{01}$ transition line toward the Sgr A molecular cloud on a 1' grid spacing and derived $C_3H_2$ column densities of $3\~7\times10^{14}\;cm^{-2}$ for molecular clouds of Sgr A. The fractional abundances of $C_3H_2$ relative to $H_2$ are obtained to be $3\~6\times10^{-9}$, which are slightly lower than that for the cold dark cloud TMC-1 but are enhanced by factors of 5-60 compared to those for Sgr B2 and the Orion extended ridge. We also estimate from the $C_3H_2$ column densities total masses of $\~10^6\; M_\bigodot$ for two clouds (M - 0.13 - 0.08 and M - 0.02 - 0.07), which are thought to be close to the virial equilibrium. We suggest that the large abundance of $C_3H_2$ in Sgr A may be partly due to the activities of the Galactic center.