Prof. K.C. Freeman will shortly visit KASI in the morning of November 16th to talk about what can be done with the Wide-Field Multi-Object Spectrograph (WFMOS) possibly on Gemini/ Subaru/AAT. In addition, as ANU is currently a partner in GMT, he will also talk about what they are planning with the GMT project.

고대로부터 현재에 이르기까지 우리 문화생활과 가장 밀접한 관련성이 있는 것이 시간과 공간에 대한 생각이다. 이는 철학적인 연구의 대상일 뿐만 아니라 20세기 들어서 과학적적으로도 많은 논쟁의 대상으로 연구를 해온 대상이다. 조선시대에는 시간의 흐름과 공간상의 위치를 대단히 중요시 여겨서 모든 우리의 생활 속에서 중요한 요소로 자리를 잡았다.
이러한 시간과 공간에 대한 기본 관념이 조선시대 국가 기관인 관상감에서 매년 간행된 책력에 잘 나타나있다. 책력에는 천체 운행의 천문학적 계산을 바탕으로 하는 역산(曆算)과 전통 문화 속에 숨겨진 미신적 요소인 역주(曆注)라는 두 종류가 포함되어 있다. 본 내용에서는 책력 속에서 이 두 요소가 어떻게 시간과 공간 문제와 관련을 짓고 어떻게 표현 했는지 알아보기로 한다.
책력에서 제시하고 있는 천체의 운행은 시간과 공간을 서로 독립적인 관계로서 설명하지 않고, 서로 끊임없이 인간 생활과 관련을 짓고 있는 것으로 보고 있다. 그 중에서 태양, 달 및 오행성(五行星) 등 칠정(七政)의 운행은 시간과 계절을 결정하는 중요한 천체들이다. 본 내용에서는 주로 천체의 위치와 운동과 관련한 천문학적 계산을 중심으로 설명하고자 한다. 우선 시간과 공간과 관련된 시각과 계절의 결정 방법, 공간 속에서의 방위와 위치를 계산하는 원리, 계산의 실제 등에 대하여 알아보기로 한다.

Firstly, I will simply introduce the different accretion processes in both supermassive black holes and X-ray binaries. Then I would like to talk about my recent work on the accretion and jet physics in radio galaxy FR Is and its possible relation to large scale surroundings.

The Earth upper atmosphere is a strongly forced and coupled system. Because the major external energy sources are the solar radiation in the range of extreme ultraviolet (EUV) and far ultraviolet (FUV), and the solar wind energy, a flow of charged particles (plasma) from the sun, the state of the upper atmosphere depends strongly on the solar activity. When the solar activity is high, magnetic storms occur as a results of increased magnetospheric energy inflow, mainly in the form of electric fields and auroral plasma particle precipitation. During magnetic storms, the energy is transferred from the magnetosphere to the polar atmosphere and distributed among kinetic, internal, and chemical energy of the thermosphere and ionosphere via a number of neutral-plasma interactions. During geomagnetically disturbed periods the ensuing high-latitude ionization, Joule heating, and ion-drag forcing of the upper atmosphere, along with penetration of the electric fields to low latitudes, affect the global dynamics and structure of the thermosphere and ionosphere, and can influence the performance and reliability of space-borne and ground-based technological systems and can endanger human life or health. Thus, as the nearest space environment to us, it is important to understand the Earth\\\\\\\\/s upper atmosphere. In this study, the physical processes responsible for maintaining the coupled thermosphere-ionosphere\\\\\\\\/s dynamical system with respect with the solar activity will be presented.

Callisto is a frequency-agile spectrometer that is easily transportable and hence can be used in many locations around the globe. Deployment at different longitudes will help observing the Sun 24 hours per day, thus capturing solar events that affect the heliosphere. The total frequency range is from 45 to 870 MHz, which is optimal for detecting the earliest stages of solar eruptions. The timing of CALLISTO can be controlled by a GPS or atomic clock. Thus the relative timing is accurate to within less than one millisecond. The digital output of the spectrometer is files in FITS format which easily can be examined by existing astronomical software.


CALLISTO has been installed in Ooty, India. It has successfully captured a first light event of solar radio flare on 2006 November 14. A second one has been installed in Gauribidanur, India and has also captured useful data on 2nd of Januar 2007. CALLISTO has been delivered to Russia (Badary near Irkutsk) in December 2007 and it has already delivered wonderful data. CALLISTO has been shipped to Costa Rica. Hosts: Jorge Paez and Marco Barrantes (university of Costa Rica) CALLISTO has also been shipped to Mexico. Host: Alejandro Lara (UNAM).Now we hope to get another CALLISTO successfully installed in South Korea by the help of local people.


This project utilizes the advanced web communication available today (e-CALLISTO).


All the data can be pooled together from Zurich by software. By IHY kick-off in February 2007, we are able to present dynamic spectrum of the Sun using DiRaC-Software.

Astronomical objects emit many forms of energy, which neither the human eye nor ordinary telescopes can detect. Infrared is one form of this invisible energy. SOFIA is an airborne observatory that will study the universe in the infrared spectrum. Besides this contribution to science progress, SOFIA will be a major factor in the development of observational techniques, of new instrumentations and in the education of young scientists and teachers in the discipline of infrared astronomy.









In the talk, I would like to give a brief introduction to the SOFIA project .

I present a kinematic analysis of the globular cluster (GC) system in the giant elliptical galaxy (gE) M60 in the Virgo cluster.
Using the photometric and spectroscopic database of M60 GCs, we have investigated the kinematics of the GC system: the rotation, the velocity dispersion, and the velocity anisotropy. Similar analysis is carried out for other gEs (M49, M87, NGC 1399, NGC 5128, and NGC 4636) using the data in the literature. We compare the kinematic properties of these GC systems and discuss the implication of these results for the formation models of the GC system in gEs.

The CCAT is a 25 meter diameter submillimeter wave telescope, currently in



the planning phase for construction and operation in the Atacama Desert,



Chile. When it is operational, it will be the premier ground based



facility for submillimeter wave astrophysics with an unmatched wide field



survey capability and will host leading edge submillimeter imaging and



spectroscopic focal plane arrays. The CCAT wide field survey will



complement the high resolution capabilities of the nearby ALMA



facility. I will describe the current plans, highlight the capabilities



and present an opportunity for partnership in the consortium.

Understanding the environment of a supernova explosion and its


consequent evolution is crucial in understanding the Galactic


ecology. The diverse characteristics of supernova remnants (SNRs)


reflect the nature of the progenitor star, of the explosion itself,


and of the ambient medium. In this talk, I will present observational


studies of two Galactic SNRs, Tycho and IC 443, focusing on


their interaction with the ambient medium.


From observations of Tycho, we discovered a thin (<10^17 cm)


shock precursor, whose primary candidate is a cosmic ray (CR) precursor.


The observed properties of the precursor suggest efficient


CR acceleration in Tycho. IC 443 is the first and most studied SNR


interacting with molecular clouds. Our results indicate that the remnant


is interacting with small (~1arc min) isolated molecular clouds, which are likely to be


remnants of the parental molecular clouds destroyed during the pre-SN evolution.


From the line characteristics of shocked molecular clumps, we study


an evolution of shocked molecular clumps.

지구환경변화를 주도하는 대표적 이슈는 (1). 지구온난화 기후변화와 (2). 오존층 파괴에 따른 생태계 영향과 (3). 국가간 대기오염 및 해양오염 등의 월경 문제이며 (4). 산업 발달과 도시화에 따른 자연환경 파괴의 광역화 이다. 이들 중 지구온난화는 국제적 감시와 저감을 위한 노력이 동반되지 않고는 달성될 수 없다. 동북아시아 기후구역의 온난화 감시에는 기상청의 안면도와 제주도 고산 지구대기감시관측소 등에서 온실기체 측정으로 적극 수행하고 있어 지구환경 연구에 대한 우리나라의 미래는 비교적 밝다.
동북아시아 지구환경 지역을 대표하는 한반도지역 대기(일명 배경대기)의 온실기체 이산화탄소의 연평균 농도는 2005년 제주도 고산 관측소 (환경부, 기상청)에서 관측한 결과 년 평균 381.6 ppm을 나타내었다(그림). 기상청 안면도 지구대기감시관측소에서는 385.3 ppm를 보였다. 연평균 증가율은 지난 13년간 (1990-2002년) 제주도 고산관측소에서 1.17 ppm - 2.02 ppm을 보였고 안면도에서는 1999년에서 2002년까지 4년 기간동안 2.30 - 4.07 ppm을 나타냈다. 한반도에서 관측된 이산화탄소 농도의 계절적 특징은 여름철에 일변화 폭이 크고 겨울철 일변화 폭이 작음을 보였다. 또한 우리나라 지역에 배출된 이산화탄소는 좁은 지역에 충분히 혼합되지 못한 상태로 존재하고 특히 중국으로부터의 영향이 있는 것으로 조사되었다. 또한 단순 선형 회귀모형과 2차 다항 회귀모형을 통해 향후 대기 중 이산화탄소 변동에 관한 4가지 시나리오가 계산되었다. 제주 고산관측소의 경우 2010년에 390.9 pp의 농도로 증가될 것이며 2015년에는 396.4-399.7 ppm에 도달할 것으로 나타났다. 안면도 지구대기감시관측소의 경우 2010년에 408.2 ppm 에 이르러 2015년에는 420 ppm을 넘을 것으로 추산된다.
제2의 온실가스 명명되는 메탄의 경우 근래 한반도에서 관측되어지는 메탄 농도는 1.9 ppm을 중심으로 이산화탄소에 비해서는 상당히 안정되어 있다. 계절별 대기의 메탄 농도는 가을철에 가장 높게 그리고 여름과 겨울 및 봄철의 순서로 농도가 나타났다.
N2O의 경우 메탄과 달리 지난 4년간 약간의 상승 경향을 나타내었다. 세계기후자료센터(WDCGG)의 발간 28호에 의하면 현재 대기 중 N2O 의 농도는 연 평균 0.25%의 상승률로서 점차 상승하고 있는 것으로 보고되고 있다.
CFC-11의 경우 1999년에서 2000년 사이 급격한 감소를 나타내었다가 이후 지금까지 안정적 감소 추세를 유지하고 있어 몬트리올 협약에 의한 정부의 사용규제에 대한 정책이 중요함을 보였다. 반면 CFC-12의 경우 지난 4년간 적은 감소 경향을 보였다.

What is the origin and nature of the cosmic X-ray background (here after CXRB)? Can detected discrete X-ray sources account for the CXRB? Since Giacconi et al. (1962) discovered homogeneous and isotropic cosmic X-ray background (here after CXRB), these questions have been investigated using data from several X-ray satellites but still remain technical issues such as the incompleteness of the used data. The CXRB consists of resolved and unresolved components. The resolved CXRB originates in discrete sources, while the unresolved CXRB originates in diffuse components and faint sources that are below current observational flux limits. The resolved CXRB can be directly measured from number counts of the discrete X-ray sources.

In this talk, we will present the total CXRB flux density and the resolved fraction of the total CXRB using the Chandra multivelength project (ChaMP) X-ray point source catalog and the Chandra Deep Fields (CDFs) data. The ChaMP X-ray point source catalog contains ~6,800 X-ray sources detected in 149 Chandra observations covering wide sky area (~10 deg2) and provides X-ray photometric data in 8 different energy bands as well as X-ray spectral hardness ratios and colors. To quantitatively characterize the sensitivity and completeness of the ChaMP sample, we performed extensive simulations. In addition, the origin and cause of the break in the X-ray point source number counts will be discussed in this talk.

The recent development and ongoing observations of the Galaxy
Evolution Explorer (GALEX) UV space telescope provide a better
understanding of the star formation history in early-type galaxies.
Here I will present the recent results of the GALEX observations for
the early-type galaxies at 0 < z < 0.2, and discuss the UV upturn
phenomenon, recent star formation, and AGN connection.

The VERA (VLBI Exploration of Radio Astrometry) project is the only
10-micro-arcsec scale astrometry observation running
currently. Observation series in radio wavelength in 22GHz and 43GHz
are performed with 4 radio telescopes in Japan. The aim of VERA is to
measure accurate distances, their proper motions and internal motions
of radio sources in Galactic star-forming regions and late-type stars.
To achieve 10-micro-arcsec accuracy stably the new software with
enough numerical accuracy is needed. VEDA (VERA Data Analyzer) is
under development for this purpose and the fundamental library for
VEDA \"CCcoda\" have been developed. In this seminar current results of
VERA are introduced and the structure of CCcoda is described.

지난 5년간 국가그리드사업의 주관기관으로 그리드컴퓨팅 기술개발에
선도적 역할을 수행해 온 한국과학기술정보연구원의 그리드사업 성과 소개 및
고성능컴퓨팅 분야의 대표응용인 기후연구 분야의 연구성과와 향후 계획에 대한 소개

According to the present knowledge, a composition of interstellar
absorbing matter is very complex: e.g., the already
detected molecules consist of up to 13 atoms and some larger
species have already been suggested. Another, perhaps most
prominent, evidence of intricate processes of molecular synthesis
and destruction taking place in interstellar medium is the
existence of diffuse interstellar bands (DIBs) - the longest
standing unsolved problem in all of spectroscopy. DIBs were
discovered as long ago as in 1921 (Heger) but their carriers
remain unknown despite considerable efforts of astronomers and
despite a progress in observational astronomy during last 10-15
years. The list of these spectral lines or bands continues to
grow, including more and more weak DIBs and reached now ~300 features.
I will tell about the current state of the problem of DIBs
identification.

Generation of local oscillator power at Terahertz frequencies with conventional techniques is difficult and expensive. In this thesis, I demonstrate steps towards a THz source using the photonic local oscillator technique for submillimeter astronomy. An LT-GaAs photomixer illuminated by two laser signals generates a beat frequency through photoconductive mixing, equal to the difference of two laser frequencies which can be tuned from a few hundred GHz to around a few THz. To generate two frequencies in the same laser for a photonic LO, I have investigated the use of a Ti:Sapphire ring cavity laser. To generate dual-mode operation in the multi-mode laser, two intracavity solid Fabry- Perot etalons were installed. To characterize the spectral width of the photomixing product, the beat frequency was monitored with a commercial photodetector at 34 GHz. The spectral width of the beat frequency was less than 10 kHz. The output power from the LT-GaAs photomixer was found to increase linearly with the applied bias voltage. Unexpectedly large fluctuations in the output power were measured, due to dual-mode intensity variations from the Ti:Sapphire ring cavity laser. The reasons for these power fluctuations are thermal variations of the resonator cavity, mechanical variations, dust particles, air fluctuations, and mode competition. To reduce these power fluctuations, a power stabilization system using volume holographic gratings (VHGs) was developed, which greatly reduced the power fluctuations.



I helped develop a 460/810 GHz dual-channel receiver, called the First Light APEX Submillimeter Heterodyne instrument (FLASH), for the Atacama Pathfinder Experiment (APEX) telescope located at Llano de Chajnantor in Chile0s Atacama desert. Using FLASH and the APEX-2A receivers, a large number of molecular transitions toward the Long Period Variable (LPV) star IK Tau were observed. Thirty four transitions of 12 molecular species, including maser lines, were detected. To determine the spatial distribution of the 12CO(3−2) emission, mapping observations were performed. Assuming local thermodynamic equilibrium (LTE), the rotational temperatures of molecules and the molecular abundances were obtained. By comparing the abundance of the individual molecules to those reported in the literature, we found an improvement over previously available observed abundances. To constrain the physical conditions in the circumstellar envelope, emission from the SO2 and CO molecules was modeled using a Monte Carlo method. From the model fits we could estimate the molecular column density and the kinetic temperature of the envelope.

In this talk, I would like to summarize recent works on the spin of the stellar



mass black holes. The possible connection between the spin of black holes



and explosive phenomena, such as Gamma-ray Bursts and Hypernovae, will be



discussed. Ironically, spinning black holes are the sources of the most energetic



explosions in the Universe after Big-Bang.

High resolution imaging observations using Chandra X-ray Observatory
revealed that there is a large population of point sources in external galaxies.
Most of them are believed to be X-ray binaries in galaxies. Low Mass X-ray Binaries
(LMXBs) are the subsef of X-ray binary population with low-mass (typically < 1Msun)
companions indicating old stellar populations in galaxies.
A study of globular clusters (GCs) in external galaxies highlighted
extragalactic astronomy for
last a few decades. Color distribution, radial/spatial distribution and
metallicity distributition of GCs in a galaxy have been used to understand the formation and evolution of a galaxy.
In a dynamical point of view GCs are probable birth-place of compact
binary later to be observed as X-ray binary.
I will present recent studies based on both X-ray and optical observations
regarding the LMXBs in external galaxies with a particular interest on
theirs connection to globular cluster system in galaxies. The possible
formation process for LMXBs will be discussed.

Magnetic reconnection at the dayside magnetopause is dominantly affected by the relative orientation of the magnetic fields in the magnetosheath and magnetosphere, the relative perpendicular velocities of field lines both before and after reconnection, and the location of the minimum geomagnetic field. We have performed a high-resolution and time-dependent three dimensional MHD simulation of interaction between the solar wind and the Earth’s magnetosphere when the dipole tilt, and By and Bz components of the IMF are simultaneously included in the whole volume of the simulation box. In the recent study of Park et al. (2006) found that for positive dipole tilt (northern hemisphere is summer) and southward IMF (Bz = 5 nT, By = 5nT), the reconnection site shifts sunward and equatorward in the summer hemisphere, and moves tailward and away from equator in the winter hemisphere. The dipole tilt creates asymmetry that strongly affects the direction of the plasma flow due to reconnection. Moreover, the electric field in the northern \\\"reconnection\\\" region (antiparallel region) is 50% larger than that at the magnetic equator and twice that at the subsolar point.



In present study, for the case of positive dipole tilt, and during the northward IMF (Bz = 5 nT, By = 5nT), magnetic reconnection occurs at high latitudes in the northern dusk due to antiparallel field condition in the summer hemisphere for By > 0 and creates open field lines. The open field lines which are generated in the dusk sector and their feet are on the northern ionosphere, move from dusk to dawn in the dayside magnetopause and then come back to dusk in the tail. Tail reconnection successively occurs in the slant and elevated plasma sheet. The polar cap potential in dusk cell is larger than that the dawn cell in summer hemisphere. Moreover three-cell pattern appears in the northern ionosphere. On the other hand, the negative potential is comparable to the positive potential in winter hemisphere and the distorted three-cell pattern appears in the southern ionosphere. The open-closed boundary in the winter hemisphere appears at higher latitude than that in the summer hemisphere.

In galactic disks, the one dimensional velocity dispersion of
interstellar gas is observed to vary between 12-15 km/s in the central
parts down to 4-6 km/s in the outer regions. Many physical mechanisms
are responsible for generating interstellar turbulence. A prominent one is related to energy feedback from stars particularly in the form of supernova explosions. In this talk, I shall review a number of those mechanisms and using three-dimensional numerical simulations assess the contribution of stellar feedback in the form of supernova explosions to the observed levels of interstellar turbulence at different radii in galactic disks.

High time resolution (> 5 Hz) observations recently opened new opportunities to investigate the tiny space rocks beyond Neptune known as Kuiper Belt Objects. Extensions of such technique will become a valuable tool to discover and characterize rapid optical transients, which have never been properly studied. Another very exciting application of high speed observation is in the area of seeing-damaged image restoration. Digital image signal processing techniques combined with recently developed zero read noise imaging devices can together deliver so called super-resolution images, previously available only through space telescopes. Compared to adaptive optics of high cost and very small field of view, this approach can be an inexpensive alternative and yet cover much larger field of view, making it possible to study dense star fields and detailed galaxy structures from ground observatories.

Dark energy is one of the most mysterious objects in both cosmology and astrophysics today. We introduce and review the current dark energy projects in experimental and theoretical point of view. We also show the future projects to investigate the properties of dark energy.

None

The Hayabusa (the original code name is MUSES-C) spacecraft was designed to obtain samples from the surface of an asteroid 25143 Itokawa (1998 SF36) and return them to Earth. Itokawa is classified with S-type asteroid, and its size is 535×294×209 meters. The main objectives of the mission were to demonstrate the performance of various technical items such as autonomous navigation, sampling devices and ion engines. On 12 September 2005, the Hayabusa spacecraft successfully rendezvoused with the target asteroid Itokawa. For nearly two month before the sampling, the remote sensing observations were performed not only for the sampling site selection but also for scientific purposes.
In this colloquium, we show the initial scientific results obtained by the multi-band imaging camera (AMICA) [1] [2], that is, its shape, surface topography and mineralogical composition. Unlike previously explored asteroids, this tiny asteroid is covered with numerous boulders instead of fine regolith, and shows large variations in both color and albedo [3]. In addition, we briefly recount a story we experienced in this project.

Reference
[1] Saito et al. 2006, Science 312, 1341-1344
[2] Yano et al. 2006, Science 312, 1350-1353
[2] Ishiguro et al. 2006, LPSC XXXVII abstract no.1533