• Communications for Statistical Applications and Methods
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• 제7권1호
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• pp.13-22
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• 2000

We consider local likelihood method with a smoothed version of the model density in stead of an original model density. For simplicity a model is assumed as the log-linear density then we were able to show that the proposed local density estimator is less affected by changes among observations but its bias increases little bit more than that of the currently used local density estimator. Hence if we use the existing method and the proposed method in a proper way we would derive the local density estimator fitting the data in a better way.

• 천문학회보
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• 제45권1호
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• pp.65.3-66
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• 2020

We use the IllustrisTNG cosmological hydrodynamical simulation to study the evolution of star formation rate (SFR)-density relation over cosmic time. We construct several samples of galaxies at different redshifts from z=2.0 to z=0.0, which have the same comoving number density. The SFR of galaxies decreases with local density at z=0.0, but its dependence on local density becomes weaker with redshift. At z≳1.0, the SFR of galaxies increases with local density (reversal of the SFR-density relation), and its dependence becomes stronger with redshift. This change of SFR-density relation with redshift still remains even when fixing the stellar masses of galaxies. The dependence of SFR on the distance to a galaxy cluster also shows a change with redshift in a way similar to the case based on local density, but the reversal happens at a higher redshift, z~1.5, in clusters. On the other hand, the molecular gas fraction always decreases with local density regardless of redshift at z=0.0-2.0 even though the dependence becomes weaker when we fix the stellar mass. Our study demonstrates that the observed reversal of the SFR-density relation at z≳1.0 can be successfully reproduced in cosmological simulations. Our results are consistent with the idea that massive, star-forming galaxies are strongly clustered at high redshifts, forming larger structures. These galaxies then consume their gas faster than those in low-density regions through frequent interactions with other galaxies, ending up being quiescent in the local universe.

• 한국수학사학회지
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• 제17권2호
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• pp.15-20
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• 2004

본 논문에서는 밀도 추정에 관한 통계량으로서 불편성과 일치성에 관하여 제시하고 밀도함수에 관한 평활 방법으로서 히스토그램과 커널 밀도 추정 및 극소적응평활(local adaptive smoothing)에 관하여 보이고자 한다. 그리고 과거에서 현재까지 비모수 밀도 추정에 관한 연구에 관하여 조사하고 논하고자 한다.

• Nuclear Engineering and Technology
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• 제36권5호
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• pp.420-429
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• 2004

The local power density should be estimated accurately to prevent fuel rod melting. The local power density at the hottest part of a hot fuel rod, which is described by the power peaking factor, is more important information than the local power density at any other position in a reactor core. Therefore, in this work, the power peaking factor, which is defined as the highest local power density to the average power density in a reactor core, is estimated by fuzzy neural networks using numerous measured signals of the reactor coolant system. The fuzzy neural networks are trained using a training data set and are verified with another test data set. They are then applied to the first fuel cycle of Yonggwang nuclear power plant unit 3. The estimation accuracy of the power peaking factor is 0.45% based on the relative $2_{\sigma}$ error by using the fuzzy neural networks without the in-core neutron flux sensors signals input. A value of 0.23% is obtained with the in-core neutron flux sensors signals, which is sufficiently accurate for use in local power density monitoring.

• 천문학회보
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• 제44권2호
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• pp.53.4-53.4
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• 2019

We reconstruct the underlying dark matter (DM) density distribution of the local universe within 20Mpc/h cubic box by using the galaxy position and peculiar velocity. About 1,000 subboxes in the Illustris-TNG cosmological simulation are used to train the relation between DM density distribution and galaxy properties by using UNet-like convolutional neural network (CNN). The estimated DM density distributions have a good agreement with their truth values in terms of pixel-to-pixel correlation, the probability distribution of DM density, and matter power spectrum. We apply the trained CNN architecture to the galaxy properties from the Cosmicflows-3 catalogue to reconstruct the DM density distribution of the local universe. The reconstructed DM density distribution can be used to understand the evolution and fate of our local environment.

• Journal of the Korean Statistical Society
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• 제30권1호
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• pp.77-87
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• 2001

Some asymptotic results on the local likelihood density estimator of Copas(1995) are derived when the locally parametric model has several parameters. It turns out that it has the same asymptotic mean squared error as that of Hjort and Jones(1996).

• Communications for Statistical Applications and Methods
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• 제10권2호
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• pp.607-617
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• 2003

This paper offers a practical comparison of efficiency between local likelihood approach and conventional kernel approach in density estimation. The local likelihood estimation procedure maximizes a kernel smoothed log-likelihood function with respect to a polynomial approximation of the log likelihood function. We use two types of data driven bandwidths for each method and compare the mean integrated squares for several densities. Numerical results reveal that local log-linear approach with simple plug-in bandwidth shows better performance comparing to the standard kernel approach in heavy tailed distribution. For normal mixture density cases, standard kernel estimator with the bandwidth in Sheather and Jones(1991) dominates the others in moderately large sample size.

• 천문학회지
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• 제18권2호
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• pp.70-78
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• 1985

From the kinematically unbiased sample of halo stars, the local mass density of halo dwarfs is estimated as $6.0{\sim}6.3{\times}10^{-4}m_{\odot}/pc^3$ by adopting a color-magnitude relation and a mass-luminosity relation. The derived halo mass density is not much different from the results of previous studies, which were derived from the kinematically biased sample of halo stars. Therefore it is confirmed that the local mass density of halo stars is far less than that required by Ostriker-Peebles to stabilize the galactic disk against barlike instabilities.

• Progress in Superconductivity
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• 제13권1호
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• pp.28-33
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• 2011

Distribution of the local critical temperature and current density in YBCO coated conductors were analyzed using Low-temperature Scanning Laser and Hall Probe Microscopy (LTSLHPM). We prepared YBCO coated conductors of various bridge types to study the spatial distribution of the critical temperature and the current density in single and multi bridges. LTSLHPM system was modified for detailed linescan or two-dimensional scan both scanning laser and scanning Hall probe method simultaneously. We analyzed the local critical temperature of single and multi bridges from series of several linescans of scanning laser microscopy. We also investigated local current density and hysteresis curve of single bridge from experimental results of scanning Hall probe microscopy.

• 한국언론정보학보
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• 제33권
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• pp.53-86
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• 2006

본 연구는 지역 언론에 내재한 연고 네트워크 구조를 밀도와 지형상의 특성을 분석함으로써 지역 언론에 내재한 연고 네트워크 구조의 지역별 비교 분석을 그 목적으로 한다. 연구 목적을 달성하기 위해 설정한 연구문제는 첫째, 지역 언론사들에 내재한 연고에 따른 밀도 특성, 둘째, 지역 방송사 내의 언론조직과 신문사 조직 간의 연고에 입각한 밀도 비교, 세 번째, 지역 언론사 조직 구성원들의 연고에 따른 지형적 특성이다. 본 연구를 수행하기 위해 문민정부와 국민정부 시기에 지역의 광역시에 소재하고 있는 주요 일간지와 지역 방송사의 뉴스 조직을 분석 대상으로 설정하였으며, 밀도 분석과 교차 분석, 그리고 대응 분석 방법을 병행하여 활용하였다. 분석 결과, 각 지역에 소재하고 있는 언론사 내부 조직 구성원의 집중 경향을 교차분석과 밀도분석을 통해 살펴본 결과, 해당 신문사의 지역적 기반과 근접한 지역 출신 인사들을 중심으로 신문사와 방송사 공히 조밀한 구조를 보이고 있으나, 특히, 신문사가 방송사 내부의 뉴스 조직에 비해 집중 경향이 더욱 높은 것으로 분석되었다. 아울러, 대응 분석을 통해 지역 언론사의 위치상의 특성을 분석한 결과, 출신 지역에 있어서는 직위에 관계없이 위치상의 차이가 명확하게 나타나고 있으며, 출신 대학의 경우 이사진과 실무진 간의 위치적 차이가 드러나고 있다는 점이 특징적이다.