• 천문학회지
• /
• 제52권4호
• /
• pp.109-119
• /
• 2019

While the reverberation mapping technique is the best available method for measuring black hole mass in active galactic nuclei (AGNs) beyond the local volume, this method has been mainly applied to relatively low-to-moderate luminosity AGNs at low redshift. We present the strategy of the Seoul National University AGN Monitoring Project, which aims at measuring the time delay of the $H{\beta}$ line emission with respect to AGN continuum, using a sample of relatively high luminosity AGNs out to redshift z ~ 0.5. We present simulated cross correlation results based on a number of mock light curves, in order to optimally determine monitoring duration and cadence. We describe our campaign strategy based on the simulation results and the availability of observing facilities. We present the sample selection, and the properties of the selected 100 AGNs, including the optical luminosity, expected time lag, black hole mass, and Eddington ratio.

• 한국전기전자재료학회:학술대회논문집
• /
• 한국전기전자재료학회 2008년도 추계학술대회 논문집 Vol.21
• /
• pp.145-145
• /
• 2008

High-k materials have been paid much more attention for their characteristics with high permittivity to reduce the leakage current through the scaled gate oxide. Among the high-k materials, $ZrO_2$ is one of the most attractive ones combing such favorable properties as a high dielectric constant (k= 20 ~ 25), wide band gap (5 ~ 7 eV) as well as a close thermal expansion coefficient with Si that results in good thermal stability of the $ZrO_2$/Si structure. During the etching process, plasma etching has been widely used to define fine-line patterns, selectively remove materials over topography, planarize surfaces, and trip photoresist. About the high-k materials etching, the relation between the etch characteristics of high-k dielectric materials and plasma properties is required to be studied more to match standard processing procedure with low damaged removal process. Among several etching techniques, we chose the inductively coupled plasma (ICP) for high-density plasma, easy control of ion energy and flux, low ownership and simple structure. And the $BCl_3$ was included in the gas due to the effective extraction of oxygen in the form of $BCl_xO_y$ compounds. During the etching process, the wafer surface temperature is an important parameter, until now, there is less study on temperature parameter. In this study, the etch mechanism of $ZrO_2$ thin film was investigated in function of $Cl_2$ addition to $BCl_3$/Ar gas mixture ratio, RF power and DC-bias power based on substrate temperature increased from $10^{\circ}C$ to $80^{\circ}C$. The variations of relative volume densities for the particles were measured with optical emission spectroscopy (OES). The surface imagination was measured by scanning emission spectroscope (SEM). The chemical state of film was investigated using energy dispersive X-ray (EDX).

• 한국전기전자재료학회:학술대회논문집
• /
• 한국전기전자재료학회 2009년도 하계학술대회 논문집
• /
• pp.105-105
• /
• 2009

$ZrO_2$ is one of the most attractive high dielectric constant (high-k) materials. As integrated circuit device dimensions continue to be scaled down, high-k materials have been studied more to resolve the problems for replacing the EY31conventional $SiO_2$. $ZrO_2$ has many favorable properties as a high dielectric constant (k= 20~25), wide band gap (5~7 eV) as well as a close thermal expansion coefficient with Si that results in good thermal stability of the $ZrO_2/Si$ structure. In order to get fine-line patterns, plasma etching has been studied more in the fabrication of ultra large-scale integrated circuits. The relation between the etch characteristics of high-k dielectric materials and plasma properties is required to be studied more to match standard processing procedure with low damaged removal process. Due to the easy control of ion energy and flux, low ownership and simple structure of the inductively coupled plasma (ICP), we chose it for high-density plasma in our study. And the $BCl_3$ included in the gas due to the effective extraction of oxygen in the form of $BCl_xO_y$ compound In this study, the surface kinetic properties of $ZrO_2$ thin film was investigated in function of Ch addition to $BCl_3/Ar$ gas mixture ratio, RF power and DC-bias power based on substrate temperature. The figure 1 showed the etch rate of $ZrO_2$ thin film as function of gas mixing ratio of $Cl_2/BCl_3/Ar$ dependent on temperature. The chemical state of film was investigated using x-ray photoelectron spectroscopy (XPS). The characteristics of the plasma were estimated using optical emission spectroscopy (OES). Auger electron spectroscopy (AES) was used for elemental analysis of etched surface.

• 한국지반환경공학회 논문집
• /
• 제12권7호
• /
• pp.23-29
• /
• 2011

산화슬래그는 토목분야에 널리 활용되어 왔으나 전기로 제강 환원슬래그는 거의 활용되지 않고 있는 실정이다. 따라서 토목 분야에서의 재활용 방법을 모색하기 위하여 환원슬래그의 성분을 분석하고 이를 바탕으로 토목현장에서 흔히 볼 수 있는 풍화토와 환원슬래그를 중량비 0% 내지 30%로 혼합한 후, 폐합시스템의 Lysimeter에서 1주, 2주, 4주의 주기로 환원슬래그 혼합토의 환경적 특성을 고찰하기 위한 시험을 수행하였다. 환원슬래그를 XRD, XRF를 이용하여 정성 정량적으로 분석한 결과, calcium silicate의 일종인 $Ca_2(SiO_4)$가 주요 결정 광물로 나타났다. 그리고 ICP-OES에 의한 중금속 분석결과 철강 생산 공정에 의한 영향으로 Al, Fe, Mn이 환원슬래그에 포함된 주요 중금속으로 확인되었다. 이를 폐기물관리법에 의한 오염물질 배출허용기준과 비교한 결과 중금속에 의한 오염가능성은 거의 없을 것으로 사료된다. 또한 환원슬래그 혼합토 침출수는 0% 혼합토에서 pH 6.9로부터 30% 혼합토에서 pH 10으로 측정되어 문제가 없음을 확인하였다. 침출수의 순환주기에 의한 pH 변화는 거의 없는 것으로 나타났다.

• 한국지구과학회지
• /
• 제43권1호
• /
• pp.60-76
• /
• 2022

본 연구는 기상청에서 운용 중인 영국 the United Kingdom Earth System Model (UKESM)을 리눅스 클러스터에 설치하여 과거 28년 기간에 대해 적분을 수행하고, 추가적인 수치 실험을 수행하여 얻은 결과와 비교한다. 설치한 UKESM은 저해상도 버전이지만, 대류권 대기 화학-에어로졸 과정과 성층권 오존 화학 과정을 동시에 모의하는 United Kingdom Chemistry and Aerosol (UKCA) 모듈을 포함하고 있는 최신 버전이다. 본 연구에 사용된 UKCA가 포함된 UKESM (UKESM-UKCA)은 전체 대기에서의 화학, 에어로졸, 구름, 복사 과정이 연동된 모델이다. CMIP5 기존 배출량 자료를 사용하는 UKESM 기준 적분 수치 모의와 함께, 동아시아 지역 이산화황(SO₂) 배출이 기상장에 미치는 영향을 평가하기 위하여 CMIP5 SO2 배출량 대신 최신의 REAS 배출자료로 교체한 실험 적분 수치 모의를 수행하였다. 두 수치 모의의 기간은 모두 1982년 1월 1일부터 2009년 12월 31일까지 총 28년이며, 모델 결과는 동아시아 지역 에어로졸 광학 두께, 2-m 온도, 강수 강도의 시간 평균값과 시간 변화 경향의 공간 분포를 분석하고 관측자료와 비교하였다. 모델에서 얻어진 온도와 강수 강도의 공간 분포 패턴은 관측자료와 전반적으로 유사하였다. 또한 UKESM에서 모의된 오존 농도와 오존전량의 공간 분포도 위성 관측 자료와 분포 패턴이 일치하였다. 두 UKESM 실험 적분 모의 결과로 얻어진 온도와 강수 강도의 선형 변화 경향의 비교를 통해, 동아시아 지역 SO2 지면 배출은 서태평양과 중국 북부지역에 대한 온도와 강수량의 변화 경향에 중요한 요인임을 확인할 수 있었다. 본 연구를 통해 슈퍼컴퓨터에서만 운용되던 UKESM이 리눅스 클러스터 컴퓨팅 환경에도 설치되어 운용이 가능하다는 점을 제시한다. 대기 환경 및 탄소순환을 연구하는 다양한 분야의 연구자들에게도 대기-해양-지면-해빙이 상호작용하는 UKESM와 같은 지구시스템모델이 활용될 가능성과 접근성이 높아졌다.

• 천문학회지
• /
• 제29권spc1호
• /
• pp.63-64
• /
• 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.