• 한국해양학회지:바다
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• 제4권3호
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• pp.170-179
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• 1999

동해 울릉분지에서 해양내부 수온구조를 파악하기 위하여 폭발성 수중음원(signal underwater sound, SUS)을 이용하여 해양음향 토모그래피 실험을 1997년 6월에 실시하였다. 토모그래피 실험은 $120{\times}120$ km 격자 바깥쪽 경계선에 SUS 21개를 항공기에서 단시간에 투하하였고 그 신호는 관측해역 남쪽에서 수직선배열 수선기로 수신하였다. 수평단면 역산모텔로 얻어진 수온 분포는 150-200 m 수심에서 난수성 소용돌이가 존재함을 보여주어 AXBT에 의한 실측 수온분포와 유사하게 나타났다. 수직모델 역산결과 수직 음속구조 형태는 AXBT 관측결과와 유사하나 250 m 보다 얕은 수심에서는 실제 관측값보다 높은 값을 나타내었다. SUS가 폭발한 수심과 시간이 갖는 불확실성을 고려하여 임의 오류값을 입력한 역산 실험결과는 150-200 m 수심에서 난수성 소용돌이 형태를 보여주나 절대 수온값이 $2^{\circ}C$ 정도 낮게 나타났다. 이러한 결과는 SUS를 음원으로 이용할 때 폭발 위치 및 폭발 시간 측정에 오류가 있음에도 불구하고 잘 발달된 중규모 해양현상을 추적하는데 SUS를 이용한 해양음향 토모그래피 적용 가능성이 매우 높음을 보여준다.

• 천문학회보
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• 제40권1호
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• pp.77.1-77.1
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• 2015

We present our recent work published in the MNRAS (Lee and Kim, 2014). Numerical studies of the imaging and caustic properties of the singular isothermal sphere (SIS) under a wide range of external shear (from 0.0 to 2.0) are presented. Using a direct inverse mapping formula for this lensing system, we investigate various lensing properties for both low-shear (i.e. ${\gamma}$<1.0) and high-shear (i.e. ${\gamma}$ >1.0) cases. We systematically analyse the effective lensing cross-sections of double-lensing and quadruple-lensing systems, based on the radio luminosity function obtained by the Jodrell-VLA Astrometric Survey (JVAS) and the Cosmic Lens All-Sky Survey (CLASS). We find that the limit of a survey selection bias (i.e. between brighter and fainter images) preferentially reduces the effective lensing cross-sections of two-image lensing systems. By considering the effects of survey selection bias, we demonstrate that the long-standing anomaly over the high quads-to-doubles ratios (i.e. 50~70 % for JVAS and CLASS) can be explained by the moderate effective shear of 0.16~0.18, which is half that of previous estimates. The derived inverse-mapping formula could make the SIS + shear lensing model useful for galaxy-lensing simulations.

• 천문학회지
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• 제37권5호
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• pp.381-385
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• 2004

Similarly to other cluster of galaxies previously classified as cooling flow systems, the Chandra observation of MKW 3s reveals that this object has a complex X-ray structure hosting both a X-ray cavity and a X-ray filament. Unlike the other clusters, however, the temperature map of the core of MKW 3s shows the presence of extended regions of gas heated above the radially averaged gas temperature at any radius. As the cluster does not show evidences for ongoing major mergers Mazzotta et al. suggest a connection between the heated gas and the activity of the central AGN. Nevertheless, due to the lack of high quality radio maps, this interpretation was controversial. In this paper we present the results of two new radio observations of MKW 3s at 1.28 GHz and 604 MHz obtained at the GMRT. Together with the Chandra observation and a separate VLA observation at 327 MHz from Young, we show unequivocal evidences for a close connection between the heated gas region and the AGN activity and we briefly summarize possible implications.

• 천문학회보
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• 제40권2호
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• pp.31.3-32
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• 2015

We present the physical properties of star forming regions in IC 10 obtained from Korea VLBI Network (KVN) 22GHz, the Submillimeter Array (SMA) CO, Very Large Array (VLA) HI 21cm, optical (U, B, V and H-alpha), and Spitzer infrared observations. IC 10 is a nearby (~0.7Mpc) irregular blue compact dwarf (BCD) galaxy which is likely to be experiencing an intense and recent burst of star formation. This nearby infant system showing high star formation rate but low metallicity (<20% of that of the Sun) provides critical environment of interstellar medium (ISM) under which current galactic star formation models are challenged. To make quantitative analysis of the ISM in the galaxy, we apply 2D cross-correlation technique to the multi-wavelength data for the first time. By cross-correlating different tracers of star formation, dust and gas phases in IC 10 in a two dimensional way, we discuss the gas properties and star formation history of the galaxy.

• 천문학회보
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• 제39권2호
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• pp.61.1-61.1
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• 2014

IC 10 is one of the most well-known irregular starburst dwarf galaxies in the Local Group. Its low metal and oxygen abundance together with proximity make it an excellent laboratory to test star formation models, especially in low-metallicity systems like galaxies in the early Universe as well as many other local dwarfs. Among a number of active star forming regions, we have detected H2O kilo-maser emission in the south-east region of IC 10(IC 10 SE) using the Korean VLBI Network(KVN). This maser line is likely to be associated with a giant molecular cloud identified in IC 10 SE by former CO studies. Using the HI and CO data from the VLA and SMA archive, we probe the atomic and molecular gas properties of IC 10 SE. We discuss how the cool gas morphology and kinematics are related with maser and star formation activity in IC 10 SE.

• 천문학회보
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• 제41권2호
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• pp.31.3-32
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• 2016

We present the radial variations of the scale heights and the vertical velocity dispersions in a sample of nearby edge-on galaxies using BIMA/CARMA $^{12}CO$ ($J=1{\rightarrow}0$), VLA/EVLA HI, and Spitzer $3.6{\mu}m$ data. Both the disk thicknesses and the velocity dispersions of gas and stars vary with radius, contrary to assumptions of previous studies. We investigate how the interstellar gas pressure and the gravitational instability parameter differ from values derived assuming constant velocity dispersions and scale heights. Using the measurement of the disk thicknesses and the derived radial profiles of gas and stars, we estimate the corresponding volume densities. The gravitational instability parameter Q follows a fairly uniform profile with radius and is ${\geq}1$ across the star-forming disk. The star formation law has a slope that is significantly different from those found in more face-on galaxy studies. The midplane gas pressure appears to roughly hold a power-law correlation with the midplane volume density ratio (${\rho}_{H2}/{\rho}_{HI}$).

• 한국음향학회지
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• 제24권6호
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• pp.325-333
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• 2005

본 논문에서는 2004년 동해에서 수행된 MAPLE 실험의 음향계측 자료를 이용한 지음향학적 인자 역산기법을 제시하고 제안된 기법의 검증을 위해 음원의 위치추적 테스트를 수행하였다. 역산을 위한 목적함수는 예인 음원과 고정된 수직선배열로부터 획득된 음향신호를 이용하여 구한 전달손실과 모의된 전달손실과의 상관관계를 평가하도록 정의하였다. 목적함수의 최적화는 광역 최적화 알고리즘인 VFSA (Very Fast Simulated Annealing)를 사용하여 수행하였다. 본 역산기법을 5개의 주파수 토널 성분 데이터에 적용한 후 이를 바탕으로 실험해역의 지음향 모델을 구성하였다. 끝으로 정합장처리를 통해 예인 음원의 위치를 추적하여 역산된 지음향학적 인자들의 타당성을 검토하였다.

• 한국음향학회지
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• 제20권5호
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• pp.92-99
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• 2001

1999년 10월에 수행한 한국 동해 중북부 해역의 토모그래피 실험은 저주파수음원을 블라디보스톡 부근의 대륙붕 해역에 위치시켰고 수직선배열 수신기를 울릉도 부근에 고정시켜 원거리 음향 신호의 변화특성을 파악코저하였다. 음원은 위상 변조된 신호이며 울릉도 부근해역의 수직선배열 수신기를 이용하여 자료를 수집하였다. 수신된 자료에 대해 도달시간 및 그 변화를 파악하였다. 이를 위해 위상 변조된 신호를 복조하였으며 특성을 파악하기 위해 도달시간 확산 및 상관성 분석을 수행하였다. 분석결과 단주기성 변화가 존재하고 있으며 이는 내부파에 의한 매질의 수직 변동에 의한 영향이라 할 수 있다.

• 천문학논총
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• 제30권2호
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• pp.125-127
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• 2015

We present preliminary results from OH ground state phase referenced observations carried out with the Multi Element Radio Linked Interferometer Network (MERLIN) and e-MERLIN towards the massive star forming region W49A. There are three active SFRs within this complex: W49 North (W49 N), W49 South (W49 S) and W49 South West (W49 SW). The first epoch of observations was obtained in 2005 with MERLIN while the second epoch was obtained in 2013 with the e-MERLIN upgraded system. In this paper, we present 1665 and 1720 MHz maser emission towards W49 S and W49 SW. Overall, both epochs show good agreement with the previous observations of Argon et al. (2000) carried out with the Very Large Array (VLA). The better sensitivity and wider velocity coverage of the MERLIN/e-MERLIN observations allowed us to discover a new 1720 MHz OH maser site in W49 S.

• 천문학회보
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• 제36권1호
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• pp.62.1-62.1
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• 2011

Warp phenomenon seems to be ubiquitous among spiral galaxies, and a a number of mechanisms have been suggested as the origin including cosmic infall and tidal interactions. In this work, we compare warp characteristics of cluster spirals and the ones in the field in order to investigate the influence of environment on warping, in particular of gas disks. We make use of a tilted-ring modeling (TRM) method to VLA HI (21cm) data cubes of carefully selected 20 spiral galaxies in the Virgo cluster. The TRM allows us to probe kinematics, e.g., inclination, position angle, and velocity dispersion of HI disks. We compare the properties of each tilted-ring component to mean properties based on optical images. In this contribution, we present preliminary yet important findings on the warp characteristics of spiral galaxies in dense environment, and discuss possible origins of those kinematical structures.