The Bulletin of The Korean Astronomical Society (천문학회보)
The Korean Astronomical Society (KAS)
- Semi Annual
- /
- 1226-2692(pISSN)
Domain
- Earth Science(Earth/Atmosphere/Marine/Astronomy) > Astronomy
Volume 35 Issue 1
-
The spectroscopy over a region from 3 to 17
${\mu}m$ based on the tuneable diode lasers (TDLAS) is the most powerful technique for in situ studies of the diagnostics of small molecules. The increasing interest in small molecules especially containing carbon, oxygen, hydrogen, and fluorine containing ones can be fulfilled by TDLAS at 0.0001 cm-1 resolution, because most of these compounds are infrared active. TDLAS provides a means of determining the absolute concentrations of the ground states of stable and transient molecular species, which can be employed for the time dependent studies in sub micro second scale. Information about gas temperature and population densities can also be derived from TDLAS measurements. Collisional energy transfer between the small molecules can be studied with TDLAS. Also, a variety of free radicals and molecular ions have been detected by TDLAS. Since plasmas with molecular feed gases are used in many applications, there are new applications in industrial field. Recently, the development of quantum cascade lasers (QCLs) offers an attractive new option for TDLAS. -
Chung, Hyun-Soo;Oh, Se-Jin;Je, Do-Heung;Roh, Duk-Gyoo;Sohn, Bong-Won;Lee, Sang-Sung;Kim, Hyo-Ryoung 47
APT(Asian-Pacific Telecommunity)는 아시아-태평양지역 국가의 공동이익을 도모하기 위하여 결성된 아-태지역 전파협의체 조직으로, WRC(세계전파통신회의)회의에서의 아-태지역 주관청의 공동이익을 얻기 위해 APG(APT Conference Preparatory Group for WRC)회의를 연간 1회의 비율로 개최하고 있다. WRC-12회의에 대비하여 결성된 APG-12 회의가 2010년 3월 태국 방콕에서 개최되었으며, 전파천문업무 보호 및 22 GHz 대역 달탐사, 38 GHz 대역 Space-VLBI운용대역과 관련된 WRC-11 의제 1.6, 1.11, 1.12 등에 대해 활발한 토론이 있었다. WRC-12 의제 1.12는 항공이동국이 ASTRO-G와 같은 차세대 space-VLBI의 우주연구업무에 유해한 간섭을 줄 수 있으므로, 항공이동업무의 간섭으로부터 37-38GHz대역의 우주연구업무를 보호하기 위한 연구의제이다. 따라서 한국천문연구원에서는 KVN과 일본국립천문대(ASTRO-G)간의 원활한 국제 공동VLBI연구를 위해, WRC회의에서 최종적인 규정개정을 함에 있어서 필요한 아-태지역 국가의 공동의견을 창출하기 위한 APT회의에서 주도적인 역할을 담당하고 있다. 본 발표에서는 APG-12 3차 회의에 제출한 우리나라의 기고서 제출 결과 및 동 회의에서의 최종결과 및 향후 대응책에 대해서도 알아보고자 한다. -
Koo, Bon-Chul;McKee, Christopher F.;Suh, Kyung-Won;Moon, Dae-Sik;Burton, Michael, G.;Hiramatsu, Masaaki;Bessel, Michael S.;Onaka, Takashi;Kim, Hyun-Jeong;Jeong, Woong-Seob;Gaensler, Bryan;Im, Myung-Shin;Lee, Ho-Gyu;Lee, Jae-Joon;Tatematsu, Ken'ichi;Kohno, Kotaro;Ezawa, Ryohei;Ezawa, Hajime;Yun, Min-S.;Hughes, David H. 57
We report the discovery of a bright mid-infrared (MIR) source with prominent crystalline silicate emission using the space telescope AKARI and Spitzer. This source, IRAS 15099-5856, has a spectacular morphology with a bright central compact source (CCS) surrounded by knots, spurs, and several extended (~4') arc-like filaments. The source is seen only in infrared at${\geq}10{\mu}m$ . The Spitzer MIR spectrum of the CCS shows prominent emission features from Mg-rich crystalline silicates and strong [Ne II] 12.88${\mu}m$ and several other faint ionic lines. We model the MIR spectrum as thermal emission from several independent dust components and compare their properties to those of the Herbig Be star HD 100546 which shows very similar MIR spectrum. Our molecular line observations reveal two molecular clouds around the source, but no associated dense molecular cores. We discuss two possible origins for IRAS 15099-5856; a deeply embedded massive young stellar object on the other side of the Galaxy and a disrupted, protoplanetary disk being photoevaporated by the UV radiation from the nearby O star Muzzio 10. -
To investigate whether the present-day active galaxies follow the same black hole mass vs. stellar velocity dispersion (MBH-
$\sigma*$ ) relation as quiescent galaxies, we measured the velocity dispersions of a sample of local Seyfert 1 galaxies, for which black hole masses were measured via reverberation mapping. We measured stellar velocity dispersions from high S/N optical spectra centered on the Ca II triplet region (${\sim}8500^{\circ}A$ ), obtained at the Keck, Palomar, and Lick Observatories. For two objects, in which the Ca II triplet region was contaminated by nuclear emission, we used high-quality H-band spectra obtained with the OH-Suppressing Infrared Imaging Spectrograph and laser-guide star adaptive optics at the Keck-II Telescope. Combining our new measurements with data from the literature, we assemble a sample of 24 active galaxies with stellar velocity dispersions and reverberation MBH in the range of black hole mass 106< MBH /$M{\odot}$ < 109,toobtainthefirstreverberationmappingconstraintsontheslopeandintrinsicscatteroftheMBH-$\sigma*$ relation of active galaxies. Assuming a constant virial coefficient f for the reverberation MBH, we find a slope${\beta}=3.55{\pm}0.60$ and the intrinsic scatter${\sigma}int=0.43{\pm}0.08$ dex in the relation log (MBH/M${\odot}$ )=$\alpha+\beta$ log(${\sigma}*$ /200 km s-1), which are consistent with those found for quiescent galaxies. We derive an updated value of the virial coefficient f by finding the value which places the reverberation masses in best agreement with the MBH -$\sigma*$ relation of quiescent galaxies; using the quiescent MBH -$\sigma*$ relation determined by Gultekin et al. we find log f=0.72+0.09 (or$0.71{\pm}0.10$ ) with an intrinsic scatter of$0.44{\pm}0.07$ (or 0.46+0.07) dex. No correlations between f and parameters connected to the physics of accretion (such as the Eddington ratio or line-shape measurements) are found. The uncertainty of the virial coefficient remains one of the main sources of the uncertainty in black hole mass determination using reverberation mapping, and therefore also in single-epoch spectroscopic estimates of black hole masses in active galaxies. -
About 50% of Active Galactic Nuclei(AGNs) are found to be red and dust-obscured. They are believed to be in an early dusty stage of AGNs evolution or affected by dust torus in the direction of line of sight. However, optical spectrum is affected by dust extinction, making it difficult to study their properties, such as FWHM and luminosity. In order to reveal the mass of central Black Hole(BH) in red AGN, we establish a new BH mass estimator for typical type1 AGNs using Near InfraRed(NIR) hydrogen line(
$P_{\alpha}$ and$P_{\beta}$ ), since these lines are at longer wavelength, less affected by dust extinction than optical hydrogen lines, such as$H_{\alpha}$ and$H_{\alpha}$ . To derive the new empirical formula, we use a sample of well-known 36 AGN with a wide BH mass range of$10^6-10^9\;M_{\odot}$ , where$M_{BH}s$ are estimated by reverberation mapping method and single epoch method. The$P_{\alpha}/P_{\beta}$ luminosities and FWHMs are derived by analyzing IRTF NIR spectra or taken from literature values. We show that luminosities and FWHMs of these lines correlate well with those of Balmer lines. Suggesting that Paschen and Balmer broad lines are originated from same region. Finally, we present the new$M_{BH}$ formula that are based on$P_{\alpha}/P_{\beta}$ luminosity and FWHM. We hope that our result will be used for investigating red AGNs. -
Choi, Yun-Young;Park, Chang-Bom;Kim, Ju-Han;Weinberg, David H.;Kim, Sung-Soo S.;Gott III, J. Richard;Vogeley, Michael S. 82
We measure the topology of the galaxy distribution using the Seventh Data Release of the Sloan Digital Sky Survey (SDSS DR7), examining the dependence of galaxy clustering topology on galaxy properties. The observational results are used to test galaxy formation models. A volume-limited sample defined by Mr<-20.19 enables us to measure the genus curve with amplitude of G=378 at 6h-1Mpc smoothing scale, with 4.8% uncertainty including all systematics and cosmic variance. The clustering topology over the smoothing length interval from 6 to 10h-1Mpc reveals a mild scale-dependence for the shift and void abundance (A_V) parameters of the genus curve. We find strong bias in the topology of galaxy clustering with respect to the predicted topology of the matter distribution, which is also scale-dependent. The luminosity dependence of galaxy clustering topology discovered by Park et al. (2005) is confirmed: the distribution of relatively brighter galaxies shows a greater prevalence of isolated clusters and more percolated voids. We find that galaxy clustering topology depends also on morphology and color. Even though early (late)-type galaxies show topology similar to that of red (blue) galaxies, the morphology dependence of topology is not identical to the color dependence. In particular, the void abundance parameter A_V depends on morphology more strongly than on color. We test five galaxy assignment schemes applied to cosmological N-body simulations to generate mock galaxies: the Halo-Galaxy one-to-one Correspondence (HGC) model, the Halo Occupation Distribution (HOD) model, and three implementations of Semi-Analytic Models (SAMs). None of the models reproduces all aspects of the observed clustering topology; the deviations vary from one model to another but include statistically significant discrepancies in the abundance of isolated voids or isolated clusters and the amplitude and overall shift of the genus curve. SAM predictions of the topology color-dependence are usually correct in sign but incorrect in magnitude. -
A short-period comet, 17P/Holmes, is one of the most outstanding comets because of the outburs in 2007. It orbits the sun at the distance between 2.1AU and 5.2 AU with the orbital period of 6.9 year. On 2007 October 23, its brightness was suddenly increased by about a million times from 17 mag to 2.5 mag. We made observations of 17P/Holmes soon after the outburst on October 25, 27 and 28, using a 105cm telescope at the Ishigakijima Astronomical observatory, Japan. We took the images with V, R and I-band filters simultaneously. Total exposure times are 15 (October 25), 69 (October 27), and 37 (October 28) minute in each filter. The composite images provide good signal to noise ratio and help us to recognize faint structures embedded in the dust cloud. We examined a sequence of images using a digital filter that enhances the small-scale structures. As the result of the data analysis, we confirm (1) the radial expanded structure coming out from the nucleus of comet, and (2) dozens of blobs that moved radially away from the nucleus. In this presentation, we introduce the observations and the data reductions, and consider the origins of these fine structure.
-
In this talk we outline the current understanding of solar flares, mainly focusing on magnetohydrodynamic (MHD) processes. A flare causes plasma heating, mass ejection, and particle acceleration which generates high-energy particles. The key physical processes producing a flare are: the emergence of magnetic field from the solar interior to the solar atmosphere (flux emergence), formation of current-concentrated areas (current sheets) in the corona, and magnetic reconnection proceeding in a current sheet to cause shock heating, mass ejection, and particle acceleration. A flare starts with the dissipation of electric currents in the corona, followed by various dynamic processes that affect lower atmosphere such as the chromosphere and photosphere. In order to understand the physical mechanism for producing a flare, theoretical modeling has been develops, where numerical simulation is a strong tool in that it can reproduce the time-dependent, nonlinear evolution of a flare. In this talk we review various models of a flare proposed so far, explaining key features of individual models. We introduce the general properties of flares by referring observational results, then discuss the processes of energy build-up, release, and transport, all of which are responsible for a flare. We will come to a concluding viewpoint that flares are the manifestation of the recovering and ejecting processes of a global magnetic flux tube in the solar atmosphere, which has been disrupted via interaction with convective plasma while rising through the convection zone.
-
It has been a puzzle in solar physics how a low-lying magnetic structure such as a solar prominence surrounded by a strongly line-tied overlying field sometimes intrudes through the latter and goes into eruption. A numerical simulation study of the solar coronal plasma reveals that a ballooning instability can explain this type of eruptive process. We consider an idealized situation with two flux ropes merging. When magnetic field lines from different flux ropes reconnect, a new field line connecting farther footpoints is generated. Since the field line length abruptly increases, the field line expands outward. If the plasma beta is low, this expansion takes place more or less evenly over the whole field line. If, on the other hand, the plasma beta is high enough somewhere in this field line, the outward expansion is not even, but is localized as in a bulging balloon. This ballooning section of the magnetic field penetrates out of the overlying field, and eventually the originally underlying field and the overlying field come to interchange their apex positions. This process may explain how a field structure that has stably been confined by an overlying field can occasionally show a localized eruptive behavior.
-
We examined variations of the solar wind magnetic fields which are characterized by smooth field rotations with time scales of 2-7 hours, and identified the existence of two classes of structures. One is a small-scale magnetic flux rope, and the other shows clear characteristics of Alfven waves. In this study, we attempted to clarify fundamental characteristics of the structure of the second class. We have found that the observed features are basically described by the cylindrical structure consisting of the uniform background field and the circular torsional wave field propagating along the background field. We performed the least-squares fitting analysis for the observed rotational variations with a simple model of the torsional Alfven wave as described above. The fitted results show satisfactory agreement with observations and thus allow us to determine the structure of the region occupied by the torsional Alfven wave. Furthermore, the examination of ACE and WIND observations reveals several cases in which two spacecrafts encountered the same structure at different position and different times. Comparison of such cases provides further evidence that the observed rotational field variations are due to the torsional Alfven waves, and not due to elliptically-polarized Alfven waves.
-
We have studied the formation of coronal holes (CHs) associated with halo CMEs. For this study, we used multi-wavelength data from Yohkoh Soft X-ray Telescope (SXT), GOES Soft X-ray Imager (SXI), SOHO EIT 195
${\AA}$ , SOHO MDI magnetogram, MLSO He I 10830${\AA}$ , and BBSO H-alpha. The CHs are characterized by open magentic field regions with low emission, density, and temperature and their open fields drive high speed solar winds which cause geomagnetic storms. So far, the formation and the evolution of CHs are not well understood. The formation of the dark region associated with the eruption of a CME is well known as "coronal dimming" which may be caused by the mass depletion near the CME footpoint. It is different from a typical CH since it persists for only one or two days. In this study, we present three cases that show the formation of coronal holes which are associated with three halo CMEs: 1) 2000 Jul 14, 2) 2003 Oct 28, 3) 2005 May 13. In the first case, hot plasma was ejected during a weak eruption and then filled out the pre-existing CH. After the halo CME occurred, the hot plasma region becomes a CH again. In the second and the third cases, we found newly formed CHs just after their associated CMEs. All three coronal holes are associated with strong flares and persist over 3 days until they disappeared by the solar rotation. Examining the MDI magnetograms, we found that the magnetic polarity of each CH region has one polarity. Based on these results, we suggest that the coronal holes can be formed by the CMEs and they should be distinguished from the coronal dimming. -
Ground-based solar observations have several merits such as wider field of view and higher time cadence than those of satellite observations. The Domeless Solar Telescope of Hida Observatory is designed to acquire solar surface images at the highest possible spatial resolution using two types of spectrographs: a vertical spectrograph with the highest wavelength resolution in the world, and a horizontal spectrograph that can take images of the sun in multi-wavelength over the entire visible solar spectrum. The temporal variation of fine features such as chromospheric grains in the supergranulation cells and facular points in the network region has been obtained using DST Ca II K lines compared with Hinode Ca II H lines. This analysis is expected to provide a fundamental tool for research of diverse phenomena on the solar surface.
-
We have investigated seven Extreme-Ultraviolet (EUV) bright points in the active region (AR 10926) on 2006 December 2 by the EUV imaging spectrometer (EIS) onboard Hinode spacecraft. We determined their Doppler velocities and non-thermal velocities from 15 EUV spectral lines (log T=4.7-7.2) by fitting each line profile to a Gaussian function. We present the Doppler velocity map as a function of temperature which corresponds to a different height. As a result, these active region bright points show two different types of characteristics. Type 1 bright point shows a systematic increase of Doppler velocity from -68 km/s (blue shift) at log T=4.7 to 27 km/s (red shift) at log T=6.7, while type 2 bright points have Doppler velocities in the range of -20 km/s and 20 km/s. Using MDI magnetograms, we found that only type 1 bright point was associated with the canceling magnetic feature at the rate of
$2.4{\times}10^{18}$ Mx/hour. When assuming that these bright points are caused by magnetic reconnection and the Doppler shift indicates reconnection out flow, the pattern of the Doppler shift implies that type 1 bright point should be related to low atmosphere magnetic reconnection. We also determined electron densities from line ratio as well as temperatures from emission measure loci using CHIANTI atomic database. The electron densities of all bright points are comparable to typical values of active regions (log Ne=9.9-10.4). For the temperature analysis, the emission loci plots indicate that these bright points should not be isothermal though background is isothermal. The DEM analysis also show that while the background has a single peak distribution (isothermal), the EUV bright points, double peak distributions. -
We report three types of evolutions of EUV bright points (EBPs) which are characterized by their height variations. We analyzed three EBPs during their lifetimes observed by STEREO/SECCHI/EUVI and we obtained heights, sizes, and intensities. Moreover, we investigated their underlying magnetic bipoles observed by SOHO/MDI and we measured distances and fluxes of the two opposite fragments. We found three distinct changes in the heights of the EBPs: upward, downward, and flat. In the upward case, the EBP showed a small and dark structure first, and then changed to a large and bright loop. In the downward case, the EBP first appeared as a large and dark loop structure, and then evolved to a compact and bright loop system. Finally, in the flat case, the height and the size of the EBP didn't change significantly. We found that those EBPs were associated with three distinct contact types of their underlying magnetic fragments, emerging, cancelling, and shearing, respectively. In all cases, both flux emergences and flux cancellations were observed during the lifetimes of the BPs. The flux emergence was dominant in the initial phase and the flux cancellation was significant when the intensity reached its maximum. In addition, we found a remarkable correlation between the heights of the EBPs and the distance of the opposite magnetic fragments.
-
The Extreme ultraviolet Imaging Spectrometer (EIS) on board Hinode provide us with excellent imaging spectroscopic data with very good spatial and spectral resolutions, which can be used for detecting Doppler flows in transition region and coronal lines as well as diagnosing plasma properties such as temperature, density, and non-thermal velocity. In this study we have made an EUV-imaging spectroscopic study of the source region of a partial halo coronal mass ejection (CME) that occurred on 2007 July 9 in NOAA 10961. Dopplergrams are obtained before and after the CME eruption using 12 EIS spectral lines (Log T= 4.9~7.2). Major results are summarized as follows. First, it is noted that either red shifts disappeared or blue shifts newly appeared for all spectral lines lower than Log T =6.0. Second, there were significant intensity increases for all wavelengths. Third, there were no significant variations in non-thermal motions for all wavelengths. We found one interesting bright point that newly appeared after the CME eruption. We discuss the implication on the results in terms of the CME eruption.
-
오늘날 태양의 흑점과 흑점군의 개수는 각 국의 천문대에서 관측자가 태양을 스케치하여 직접 산출하고 있다. 이렇게 산출된 자료는 해당 천문대의 관측 특성을 나타내는 상수를 사용하여 국제 흑점 상대수로 변환되고, 이는 태양의 활동성을 나타내는 중요한 지표로 사용된다. 하지만 이들의 수를 직접 산출하는 것은 인력과 시간을 필요로 하고, 관측자의 주관적인 판단이 개입될 수 있다. 우리는 이러한 점을 개선하기 위하여 컴퓨터 프로그래밍을 통한 흑점과 흑점군의 개수를 산출하는 방법을 연구하였다. 우선 태양 백색광 영상에서 광도 히스토그램를 통해 경계값을 찾아 이진화하고, 흑점을 분리하기 위해 경계검출기법과 채움기법을 사용하였다. 그리고 분리된 흑점들의 거리를 계산하여 이들의 거리가 경험적 기준거리보다 가까운 흑점을 군집화하였다. 이 방법을 20개의 영상에 적용한 결과, 관측자가 직접 산출한 흑점수와 컴퓨터 프로그램을 사용하여 얻은 흑점수가 서로 매우 좋은 상관관계(r=0.91)를 보였다. 이 연구 결과를 토대로 흑점수 자동 산출 프로그램의 발전방향과 활용방안에 대해 논의하고자 한다.
-
Numerous operational anomalies and satellite failures have been reported since the beginnings of the "space age". Space weather effects on modern spacecraft systems have been emphasized more and more as increasing their complexity and capability. Energetic particles potentially can destroy and degrade electronic components in satellites. We analyzed the geostationary (GEO) satellite anomalies during 1997-2009 to search possible influences of space weather on the satellite anomalies like power problem, control processor problem, attitude control problem, etc. For this we use particle data from GOES and LANL satellites to investigate space weather effects on the GEO satellites' anomalies depending on Kp index, local time, seasonal variation, and high-energy electron contribution. As results, we obtained following results: (1) there is a good correlation between geomagnetic index(Kp) and anomaly occurrences of the GEO satellite; (2) especially during the solar minimum, occurrence of the satellite anomalies are related to electron flux increase due to high speed solar wind; (3) satellite anomalies occurred more preferentially in the midnight and dawn sector than noon and dusk sector; (4) and the anomalies occurred twice more in Spring and Fall than Summer and Winter; (5) the electron with the lowest energy channel (50-75keV) has the highest correlation (cc=0.758) with the anomalies. High association between the anomalies and the low energy electrons could be understand by the facts that electron fluxes in the spring and fall are stronger than those in the summer and winter, and low-energy electron flux is more concentrated in the dawn sector where the GEO satellite anomalies occurred more frequently than high-energy electron flux. While we could not identify what cause such local time dependences, our results shows that low-energy electrons (~100keV) could be main source of the satellite anomaly, which should be carefully taken into account of operating satellites.
-
본 연구에서는 IDL(Interactive Data Language)의 여러가지 영상처리기법을 SOHO EIT 영상에 적용하여 세부적인 코로나 구조를 파악하고자 한다. 이를 위하여 우리는 히스토그램 평활화(Equalization), 2차 미분을 이용한 경계선 추출 방법인 라플라시안 필터링, 공간 주파수 영역의 웨이블릿 변환 등의 영상 처리 기법을 사용하였다. 히스토그램 평활화는 1차 처리과정으로 모든 영상에 동일하게 사용되었고, 나머지 방법은 2차 처리과정으로 사용하였다. 처리 결과 웨이블릿 변환 보다는 라플라시안 필터링 영상처리 방법이 더 구체적인 구조를 보여주는 것을 알 수 있었다. 다만 웨이블릿 변환의 경우 IDL에 내장된 노이즈 제거용 웨이블릿 변환 함수를 사용한 것으로, 다른 다양한 방법의 적용이 필요한 것으로 판단된다. 본 연구를 통해 얻은 영상처리 기법이 태양 코로나 구조 연구에 유용하게 사용될 수 있기를 기대한다.
-
본 연구의 목적은 태양 코로나 구조를 분석하기에 적합한 영상처리 기법을 찾는 것이다. 이를 위하여 우리는 IDL(Interactive Data Language)에 내장된 여러 가지 영상처리방법을 SOHO EIT 영상에 적용하였다. 우리는 영상처리를 위하여 단일 영상처리 방법과 2단계 영상 처리 방법을 사용하였다. 단일 영상처리 방법으로 히스토그램 평활화(Equalization), 주파수 필터링, 경계선 강화기법(Sobel, Robert) 등을 사용하였다. 2단계 영상처리 방법은 단일 영상 처리 방법에서 효과적이었던 방법들을 두 가지 이상 순차적으로 적용하는 것이다. 본 연구를 통하여 우리는 2단계 영상처리 방법(예, 저주파 필터 + Sobel + 히스토그램 평활화)이 단일 영상처리 방법 보다 코로나 루프 구조를 잘 보여주는 것을 확인하였다. 이 연구 결과가 태양 코로나 구조 연구에 유용하게 사용될 수 있을 것으로 기대된다.
-
Cho, Kyung-Suk;Park, Young-Deuk;Lee, Jae-Jin;Bong, Su-Chan;Kim, Yeon-Han;Hwang, Jung-A;Choi, Seong-Hwan 32.1
KASI's Solar and Space Weather Research Group (SSWRG) is actively involved in solar and space weather research. Since its inception, the SSWRG has been utilizing ground-based assets for its research, such as the Solar Flare Telescope, Solar Imaging Spectrograph, and Sunspot Telescope. In 2007 SSWRG initiated the Korean Space Weather Prediction Center (KSWPC). The goal of KSWPC is to extend the current ground observation capabilities, construct space weather database and networking, develop prediction models, and expand space weather research. Beginning in 2010, SSWRG plans to expand its research activities by collaborating with new international partners, continuing the development of space weather prediction models and forecast system, and phasing into developing and launching space-based assets. In this talk, we will report on KASI's recent activities of international collaborations with NASA for STEREO (Solar Terrestrial Relations Observatory), SDO (Solar Dynamic Observatory), and Radiation Belt Storm Probe (RBSP). -
Bong, Su-Chan;HwangBo, Jung-Eun;Lee, Chang-Hoon;Cho, Kyung-Suk;Park, Young-Deuk;Gary, Dale E.;Lee, Dae-Young 32.2
The Korean Solar Radio Burst Locator (KSRBL) is a single dish radio spectrograph, which is designed to record the spectra of microwave (0.5 - 18 GHz) bursts with 1 MHz spectral resolution and 1 s time cadence, and locate their positions on the solar disk within 2 arcmin. It was installed at KASI in 2009 August, and operational thereafter. The antenna pointing coefficients were initially determined during the installation and refined later using a series of antenna pointing calibrations. The filter to prevent the radio frequency interference around 2 GHz was designed and is to be installed. After the installation, the full frequency coverage will be recovered from the temporarily restricted frequency coverage (5 - 14 GHz). Also an effort to solve a couple of minor problems for the full performance of the system is in progress. -
HwangBo, Jung-Eun;Bong, Su-Chan;Choi, Seong-Hwan;Baek, Ji-Hye;Cho, Kyung-Suk;Lee, Dae-Young;Park, Young-Deuk 33.1
태양전파폭발위치관측기(KSRBL)는 단일 안테나 전파분광기로써 미 뉴저지공과대학과의 협력으로 2009년 8월에 한국천문연구원에 개발 설치되었다. 1 MHz 스펙트럼 분해능과 1초의 시간 분해능을 가지고 있고 관측할 수 있는 주파수 대역은 245, 410 MHz 와 0.5-18 GHz에 이르는 광대역이다. 또한 태양 전면$0.03^{\circ}$ 각거리 안의 오차 범위 내에 태양 폭발 위치를 감지할 수 있다. 전파 관측은 LabVIEW와 IDL 프로그램에 의해 미리 짜여진 관측 스케줄에 따라 매일 자동으로 진행된다. 하루에 생성되는 원시데이터는 90 GB 정도이며, 태양이 지고나면 원시데이터는 적분과정을 통해 용량이 6 GB 정도로 줄어들게 된다. 이렇게 처리된 파일은 바로 데이터 서버에 자동 전송된다. 또한 KSRBL 관측일지 홈페이지를 웹기반으로 개발하였으며 조만간 이를 데이터 전송과 연계하여 전파 폭발이 감지될 경우 원시데이터도 데이터 서버에 자동 전송되도록 할 예정이다. 2010년 1월에서 2월 8일 사이 5개의 전파 폭발이 관측되었고 태양활동이 점차 활발해짐에 따라 관측횟수는 더욱 늘어날 전망이다. 관측된 사례들에 대해 다른 전파 및 X선 관측과 비교분석하였다. -
We have investigated a relationship among the solar proton events (SPEs), coronal mass ejections (CMEs) and solar flares during the solar cycle 23 (1997-2006). Using 63 SPE dataset, we found that SPE rise time, duration time, and decrease times depend on CME speed and SPE peak intensity depends on the CME earthward direction parameter as well as CME speed and x-ray flare intensity. While inspecting the relation between SPE peak intensity and the CME earthward direction parameter, we found that there are two groups: first group consists of large 6 SPEs (> 10,000 pfu at >10 MeV proton channel of GOES satellite) and shows a very good correlation (cc=0.65) between SPE peak intensity and CME earthward direction parameter. The second group has a relatively weak SPE peak intensity and shows poor correlation between SPE peak intensity and the CME earthward direction parameter (cc=0.01). By investigating characteristics of 6 SPEs in the first group, we found that there are special common conditions of the extremely large proton events (group 1); (1) all the SPEs are associated with very fast halo CME (>1400km/s), (2) they are almost located at disk region, (3) they also accompany large flare (>M7), (4) all they are preceded by another wide CMEs, and (5) they all show helmet streamer nearby the main CME. In this presentation, we will give details of the energy spectra of the 6 SPE events from the ERNE/HED aboard the Solar and Heliospheric Observatory (SOHO), and onset time comparison among the SPE, flare, type II burst, and CME.
-
Solar proton events, whose fluxes are larger than 10 particles cm-2 sec-1 ster-1 for >10 MeV protons, have been observed since 1976. NOAA proton event list from 1997 to 2006 shows that most of the events are related to both flares and CMEs but a few fraction of events (5/93) are only related with CMEs. In this study, we carefully identified the sources of these events. For this, we used LASCO CME catalog and SOHO MDI data. First, we examined the directions of CMEs related with the events and the CMEs are found to eject from the western hemisphere. Second, we searched a major active region in the front solar disk for several days before the proton events occurred by taking into account two facts: (1) The location of the active region is consistent with the position angle of a given CME and (2) there were several flares in the active region or the active region is the largest among several candidates. As a result, we were able to determine active regions which are likely to produce proton events without ambiguity as well as their longitudes at the time of proton events by considering solar rotation rate,
$13.2^{\circ}$ per day. From this study, we found that the longitudes of five active regions are all between$90^{\circ}W$ and$120^{\circ}W$ . When the flare peak time is assume to be the CME event time, we confirmed that the dependence of their rise times (proton peak time - flare peak time) on longitude are consistent with the previous empirical formula. These results imply that five events should be also associated with flares which were not observed because they occurred from back-side. -
Cosmic rays registered by Neutron Monitors on the surface of the Earth are believed to be coming from outer space, and sometimes also from the exotic objects of the Sun. Ground level enhancement (GLE) is the sudden, sharp and short-lived increase in cosmic rays originated from the Sun. Since GLE is the signature in solar cosmic ray intensity, different solar factors erupted from the Sun can be responsible for causing it. In this context, an attempt has been made to determine quantitative relationships of GLEs > 5% with simultaneous solar, interplanetary and geophysical factors from 1997 through 2006 thereby searching the perpetrators which seem to be causing them. The study has revealed that solar flares are stronger (
$0.71{\times}10-4$ w/m2) during GLE peaks than the solar flares ($1.10{\times}10-5$ w/m2) during GLE non-peaks and backgrounds. On the average, the solar wind plasma velocity and interplanetary magnetic field are found stronger during the GLE peaks than the GLE non-peaks and backgrounds indicating that the solar flares, in conjunction with interplanetary shocks, sometimes may cause GLE peaks. Direct proportionality of GLE peaks to simultaneous solar energetic particle (SEP) fluxes imply that the GLE peaks may often be caused by SEP fluxes. Although the high intensity of SEP fluxes are also seen extended few minutes even after GLE peaks, the mean (373.62 MeV) of the GLE associated SEP fluxes is much stronger than the mean (10.35 MeV) of the non-GLE associated SEP fluxes. Evidences are also supported by corresponding SEP fluences that the the mean fluence (${\sim}5.32{\times}107/cm2$ ) across GLE event was more intense than the mean fluence (${\sim}2.53{\times}106/cm2$ ) of SEP fluxes across non-GLE event. -
Kim, Gwang-Dong;Na, Ja-Gyeong;O, Se-Jin;Im, In-Seong;Gang, Yong-U;Jang, Bi-Ho;Jang, Jeong-Gyun 35.1
천체는 천구의 북극을 중심으로 지구자전에 의하여 반시계방향으로 일주 운동을 한다. 적도의식 망원경의 최대 장점은 극축이 정확히 맞추어졌다면 접안렌즈 중앙에 적위축 조정으로 정확히 원하는 천체를 위치시키고, 적경축을 지구자전축에 동기 시켜 회전시키면 어떠한 대상이라도 추적이 가능하다. 본 연구에서는 Hardware적으로 적경축 구동을 지구 자전속도에 동기 시키는 제어회로를 설계하였다. -
Na, Ja-Gyeong;Chae, Jong-Cheol;Park, Hyeong-Min;An, Gwang-Su;Jang, Bi-Ho;Park, Yeong-Deuk;Yang, Hui-Su;Kim, Gwang-Dong 35.2
한국천문연구원은 미국 BBSO(Big Bear Solar Observatory)에 건설 중인 1.6 m NST(New Solar Telescope) 개발사업에 참여하고 있다. 고속태양영상분광기, FISS(Fast Imaging Solar Spectrograph)는 한국천문연구원과 서울대학교가 공동으로 개발하는 태양관측용 영상분광기로서, Echelle 회절격자를 분광소자로 사용하고 있다. FISS는 빠른 영상 스캐닝과 고속 CCD 카메라를 이용하여 동시에 두 파장을 관측할 수 있으며, NST의 적응광학계로부터 영상을 입력받기 때문에 회절한계에 가까운 분광영상을 얻을 수 있다. 본 연구에서는 FISS 제작을 위한 요구사항 분석, 분광기 구성과 광학설계, 구성품의 제작, 그리고 분광기의 성능검증을 위한 태양 시험관측 결과에 대해 소개한다. -
OFC (Optical Frequency Comb) is an optical spectrum which consists of equidistant lines in frequency space. OFC can thus be used as an optical ruler. Since it was demonstrated in late 1990s, it is revolutionizing many fields in frequency metrology such as the measurement of absolute optical frequencies, the measure ratios of optical frequencies with extremely high precision. It is also used in high-precision spectroscopy. In astronomy, OFC can be used as a very accurate and stable wavelength standard for a high resolution spectrograph to measure the radial velocity of celestial bodies with extremely high accuracy of about several tens cm/s. In our presentation, we will introduce some basic concepts of OFC and some issues to use it in astronomical spectrograph. We will also present our plan to develop a high resolution spectrograph with OFC.
-
Lim, Ju-Hee;Kim, Young-Ju;Park, Won-Kee;Kim, Jin-Young;Chang, Seung-Hyuk;Pak, Soo-Jong;Im, Myung-Shin 36.2
The CQUEAN (Camera for QUasars in EArly uNiverse) is an optical CCD camera optimized for observation of high redshift objects. It is going to be attached to the cassegrain focus of 2.1m telescope at McDonald Observatory, USA. We are making a focal reducer for CQUEAN to secure a larger field of view. The focal reducer is composed of four spherical lens, and it reduces the focal length of telescope by one third. We designed the lens configuration, performed tolerance analysis, and estimated the optical performance with ZEMAX. The differences in optical performace with/without filters were also investigated. The result from ZEMAX shows that the system has ample margin of errors for median seeing of 1.2" at McDonald observatory. Even with aberration and alignment tolerance, the performance is better than the original requirement. The lenses are now being made, and the lens barrel and an adapter for assembly of the Andor CCD camera and the filter wheel is now under designing process. We expect that the manufacturing of the focal reducer system as well as its optical test will be finished by April 2010. -
망원경을 사용하여 천체를 관측할 때, 관측할 천체가 있는 위치로 망원경을 정확히 구동하여야 하고, 관측하는 시간 동안 충분히 정확히 추적하여야 한다. 그러나, 망원경은 다양한 재질의 많은 종류의 기계적인 부품들을 조립하여 만들어져 있기에, 필연적으로 기계적인 오차를 가지고 있다. 망원경 구동제어 장치는 수학 연산과 다양한 펄스 특성에 기인한 제어 오차를 가지고 있다. 그리고, 영상을 획득하는 부분은 시간 지연과 상의 왜곡이나 전자적인 잡음의 영향을 받는다. 또한, 바람이나 진동 등 예기치 않은 외부적인 요인에 의한 오차가 유발되기도 한다. 이러한 다양한 요인들로 인하여, 망원경이 천체를 정확히 찾아가고 추적하는 것을 어렵게 만든다. 우리는 자동제어공학에서 사용하는 제어해석 기법을 사용하여 망원경 제어 모형을 만들어 나가고자 한다. 특정 망원경에 있어, 오차 유발에 어느 요인이 가장 큰 영향을 주는지, 또한, 어떤 특성을 조절하고, 어느 정도의 제어 시간 간격을 주어야 하는지 등, 추적오차에 주는 영향들을 정량적으로 분석하고 제어에 반영하여 가장 최적의 제어를 할 수 있도록 하고자 한다. 그 첫번째 시도로, 김해천문대 독일식 적도의 방식 200mm 망원경과 이전 연구에서 개발한 PLC 기반의 망원경 제어 장치(강용우 외, 2008) 및 AP8 CCD 카메라를 사용하여, 지향 및 추적 관측 실험을 하였다. 그 결과를 분석하여 경험적 제어 모형을 만들고, 그 해석을 수행한 내용을 소개하고자 한다.
-
한국천문연구원에서는 이동형 레이저위성추적(SLR) 시스템을 개발하고 있다. 이동형 레이저위성추적 시스템의 광학부는 송신광학계, 수신광학계, 광신호유도계로 구성되어 있으며, 주야간에 운영되는 시스템의 특성상 광신호유도계는 특별한 구성과 기능을 갖는다. 본 연구에서는 주야간 위성추적을 위해 요구되는 광신호유도계의 구성과 기능을 소개하며, 또한 광신호유도 광학계의 광학설계에 대해서도 논한다.
-
Kim, Eun-Bin;Park, Won-Kee;Kim, Jin-Young;Oh, Hee-Young;Choi, Chang-Su;Pak, Soo-Jong;Im, Myung-Shin;Kuehne, John 38.1
McDonald 2.1m Otto Struve Telescope is located in the Davis Mountains, 450 miles west of Austin, Texas. The telescope was built in 1938, but it is still in demand today. CQUEAN (Camera for QUasar in Early uNiverse) will be attached on this telescope and perform Y-band imaging observations. Dynamics study of the telescope shows that tracking errors are 0.1 arcsec/100sec in declination direction and 0.4 arcsec/100sec in R.A. direction. In order to allow a long exposure (> a few minutes) of a target field, we are making auto-guiding system for the 2.1m telescope. The auto-guiding system of CQUEAN will be connected with TCS of the telescope. The expected number of stars on the CCD field (2.97 square arcminutes) is about 1.2 stars which are brighter than magnitude 17.5 in 2.97 square arcminutes. For more effective observation, we plan to implement moving mechanism in guiding system so that guide CCD camera can see wider off-axis fields. -
Park, Won-Kee;Kim, Eun-Bin;Choi, Chang-Su;Lim, Ju-Hee;Kim, Jin-Oung;Jeong, Hyeon-Ju;Oh, Hee-Young;Pak, Soo-Jong;Im, Myung-Shin 38.2
We report the current status of CQUEAN (Camera for QUasars in EArly uNiverse) development. CQUEAN is an optical CCD camera which uses a 1024*1024 pixel deep-depletion CCD. It has an enhanced QE than conventional CCD at wavelength band around 1${\mu}m$ , thus it will be an efficient tool for observation of quasars at z > 7. It will be attached to the 2.1m telescope at McDonald Observatory, USA. A telescope interface containing a focal reducer is being designed to secure a larger field of view at the cassegrain focus of 2.1m telescope. Instrument control software will be written with python on linux platform. We are carrying out lab tests to investigate the characteristics of the system components in order to maximize the observational efficiency. Preliminary results of the tests will be presented. CQUEAN is expected to see the first light during summer season of 2010. -
Jeong, Hyeon-Ju;Park, Won-Kee;Kim, Eun-Bin;Choi, Chang-Su;Pak, Soo-Jong;Im, Myung-Shin;Kim, Jung-Hoon 39.1
We are developing a CCD camera named CQUEAN (Camera for Quasars in Early Universe) to search for quasars at z > 7. CQUEAN has a 1024*1024 deep depletion CCD chip and will be attached to 2.1m Otto-Struve Telescope at McDonald Observatory, USA. Although commercial software for the CCD camera is provided by the vendor, we are going to develop our own software to control the other instruments as well, to carry out efficient observation. There are four major parts in our software: Instrument control part controls the camera and filter wheel to obtain imaging data. Quick look window is to display acquired imaging data for quick inspection. Telescope control part interfaces with Telescope Control System (TCS) to move the telescope and to get time or coordinate information. Finally, Observation scripting facility part carries out a series of short exposures in a batch. The whole software will be written in python on linux platform, using the instrument control software libraries provided by the vendors. -
In this paper, I present the domestic development of near infrared camera systems for the ground telescope and the space satellite. These systems are the first infrared instruments made for astronomical observation in Korea. KASINICS (KASI Near Infrared Camera System) was developed to be installed on the 1.8m telescope of the Bohyunsan Optical Astronomy Observatory (BOAO) in Korea. KASINICS is equipped with a
$512{\times}512$ InSb array enable L band observations as well as J, H, and Ks bands. The field-of-view of the array is$3.3'{\times}3.3'$ with a resolution of 0.39"/pixel. It employs an Offner relay optical system providing a cold stop to eliminate thermal background emission from the telescope structures. From the test observation, limiting magnitudes are J=17.6, H=17.5, Ks=16.1 and L(narrow)=10.0 mag at a signal-to-noise ratio of 10 in an integration time of 100 s. MIRIS (Multi-purpose InfraRed Imaging System) is the main payload of the STSAT-3 in Korea. MIRIS Space Observation Camera (SOC) covers the observation wavelength from$0.9{\mu}m$ to$2.0{\mu}m$ with a wide field of view$3.67^{\circ}{\times}3.67^{\circ}$ . The PICNIC HgCdTe detector in a cold box is cooled down below 100K by a micro Stirling cooler of which cooling capacity is 220mW at 77K. MIRIS SOC adopts passive cooling technique to chill the telescope below 200K by pointing to the deep space (3K). The cooling mechanism employs a radiator, a Winston cone baffle, a thermal shield, MLI of 30 layers, and GFRP pipe support in the system. Opto-mechanical analysis was made in order to estimate and compensate possible stresses from the thermal contraction of mounting parts at cryogenic temperatures. Finite Element Analysis (FEA) of mechanical structure was also conducted to ensure safety and stability in launching environments and in orbit. MIRIS SOC will mainly perform the Galactic plane survey with narrow band filters (Pa$\alpha$ and Pa$\alpha$ continuum) and CIB (Cosmic Infrared Background) observation with wide band filters (I and H) driven by a cryogenic stepping motor. -
Han, Won-Yong;Lee, Dae-Hee;Park, Young-Sik;Jeong, Woong-Seob;Ree, Chang-Hee;Moon, Bong-Kon;Park, Sung-Joon;Cha, Sang-Mok;Nam, Uk-Won;Park, Jang-Hyun;Lee, Duk-Hang;Ka, Nung-Hyun;Seon, Kwang-Il;Yang, Sun-Choel;Park, Jong-Oh;Rhee, Seung-Wu;Lee, Hyung-Mok;Matsumoto, Toshio 40.1
The Main payload of the STSAT-3 (Korea Science & Technology Satellite-3), MIRIS (Multipurpose Infra-Red Imaging System) has been developed for last 3 years by KASI, and its Flight Model (FM) is now being developed as the final stage. All optical lenses and the opto-mechanical components of the FM have been completely fabricated with slight modifications that have been made to some components based on the Engineering Qualification Model (EQM) performances. The components of the telescope have been assembled and the test results show its optical performances are acceptable for required specifications in visual wavelength (@633 nm) at room temperature. The ensuing focal plane integration and focus test will be made soon using the vacuum chamber. The MIRIS mechanical structure of the EQM has been modified to develop FM according to the performance and environment test results. The filter-wheel module in the cryostat was newly designed with Finite Element Analysis (FEM) in order to compensate for the vibration stress in the launching conditions. Surface finishing of all components were also modified to implement the thermal model for the passive cooling technique. The FM electronics design has been completed for final fabrication process. Some minor modifications of the electronics boards were made based on EQM test performances. The ground calibration tests of MIRIS FM will be made with the science grade Teledyne PICNIC IR-array. -
Cha, Sang-Mok;Mun, Bong-Gon;Jeong, Ung-Seop;Lee, Dae-Hui;Nam, Uk-Won;Park, Yeong-Sik;Lee, Chang-Hui;Park, Seong-Jun;Lee, Deok-Haeng;Ga, Neung-Hyeon;Han, Won-Yong;Park, Jang-Hyeon;Seon, Gwang-Il;Yang, Sun-Cheol;Park, Jong-O;Lee, Seung-U;Lee, Hyung-Mok;Matsumoto, Toshio 40.2
MIRIS 우주관측카메라는 과학기술위성 3호의 주탑재체로서$0.8{\sim}2.0{\mu}m$ 의 근적외선영역에서 우주배경복사와 우리은하 평면의 Pa-$\alpha$ survey 관측을 목적으로 한다. 이러한 임무를 수행하기 위해 MIRIS 우주관측카메라에는 MCT(HgCdTe) IR 검출기가 사용되고 6개의 필터를 장착할 수 있는 필터휠이 설계되었으며, 열잡음을 줄이고 원하는 SNR을 얻기 위해 모두 100K 이하로 냉각이 요구된다. 효과적인 냉각 및 저온유지를 위해서 외부의 열을 1차적으로 차단하는 Cryostat 외부용기와 100K 이하로 냉각되는 내부 Cold Box의 이중구조를 가지는 Dewar가 설계 되었다. 내부 Cold Box의 냉각은 소형 stirling cooler로 이루어지고 외부의 열 유입량이 Cooler의 냉각용량을 넘지 않도록 설계하였다. Cryostat 외부용기는 radiation cooling으로 냉각되어 200K 이하의 온도를 유지하며 내부 Cold Box로의 열유입을 최소화하기 위해 GFRP(Glass Fiber Reinforced Plastic) 단열 지지대와 MLI(Multi Layer Insulation)가 사용된다. 또한 100K으로 냉각시 필터고정부와 Cold Box 구조에서 일어날 수 있는 구조적인 피로도를 줄이고 열변형에 의한 문제를 방지하기 위한 고려가 설계에 포함되었다. FM(Flight Model)은 고진공 환경의 우주공간에서 문제가 발생하지 않도록 설계되었다. 또한 EQM 진동시험결과를 토대로 발사환경에서 발생하는 강한 진동을 견딜 수 있도록 FEM(Finite Elements Method) 구조해석을 통하여 필터고정부에 flexible structure 설계와 완충제를 추가하고 필터휠 구동부와 harness 고정부 및 cooler 지지부를 비롯한 전체 구조물에서 충분히 진동을 극복할 수 있도록 설계하였다. -
Oh, Hee-Young;Pak, Soo-Jong;Yuk, In-Soo;Park, Chan;Lee, Sang-On;Chun, Moo-Young;Kim, Kang-Min;Lee, Sung-Ho;Pyo, Tae-Soo;Jaffe, Daniel T. 41.1
IGRINS (the Immersion GRating Infrared Spectrograph) is a high resolution infrared spectrograph which is being developed by a collaboration of the University of Texas, the Korea Astronomy and Space Science Institute, and Kyung Hee University. The wavelength calibration unit of IGRINS will be situated between the telescope flange and IGRINS dewar. It will include Th-Ar hallow cathode lamp, optical elements, and gas absorption cell for the case that requires precise calibration (e.g., radial velocity observation). The system will also use a tungsten halogen lamp in an integrating sphere as a blackbody source for the flat-field imaging. IGRINS will be placed initially on the McDonald 2.7m Harlan J. Smith telescope and later on 4-8m class telescopes. We present an overview of the plan for the wavelength calibration sources and of the development process for the optical and mechanical design of the IGRINS calibration system. -
The infrared astronomy satellite AKARI/FIS (Far-Infrared Surveyor) performed all-sky survey in 4 Far-IR bands (50 - 200
${\mu}m$ range). It observed around 94% of the whole sky twice or more with a higher spatial resolution and a wider wavelength coverage than that of previous all-sky mission, IRAS. The AKARI/FIS bright source catalogue${\beta}-2$ is the second released version which included around 290,000 point sources. It provides us with more reliable position and flux information, and around 4 times larger number of sources compared with the first version of catalogue. The sensitivity limit at$90{\mu}m$ band is 0.6 Jy and the estimated flux uncertainty is 20-35% for bright sources. The catalogue will be open to public in this year after the improvement of accuracy, reliability and completeness. -
Son, Bong-Won;Miyazaki, A.;Byeon, Do-Yeong;Lee, Sang-Seong;Jeong, Tae-Hyeon;O, Chung-Sik;Kobayashi, H. 42.1
한국천문연구원 한국우주전파관측망(KVN)은 2008년 KVN연세-VERA 간의 프린지 검출에 이어, 2009년 10월 KVN 모든 기선 간의 22GHz와 43GHz 프린지 검출에 성공하였다. 본 발표에서는 KVN 프린지 검출 시험의 과정과 결과를 요약하고, 또한 현재 수행 중인 KVN의 두 주파수 동시 VLBI 시험관측의 진행과정을 보고 하고자 한다. -
2009년부터 2010년에 걸쳐 22 및 43GHz 대역에서의 KVN 단일경 시험관측이 이루어졌다. KVN 관측소는 연세대학교, 울산대학교, 탐라대학교에 위치하고 있으며, 시험관측의 주된 내용은 안테나 지향모델 구축, 22/43 GHz 빔 정렬, 이득곡선 측정 및 안테나 효율측정 등이다. 구축된 지향오차의 정밀도는 세 곳의 관측소 모두 rms가 5초 이내였으며, 두 빔도 5초 이내로 정렬되어 있음이 확인되었다. 안테나 효율은 22 및 43GHz에서 모두 60%를 넘는 값을 얻을 수 있었다.
-
Lee, Sang-Sung;Oh, Chung-Sik;Sohn, Bong-Won;Byun, Do-Young;Jung, Tae-Hyun;Kim, Kee-Tae;Miyazaki, Atsushi;Kobayashi, Hideyuki;Han, Seog-Tae;Je, Do-Heung;KVN team, KVN team 43.1
We have carried out 43-GHz VLBI test observations of the Korean VLBI Network (KVN), which has obtained the first fringes at 22/43-GHz in 2009 (a talk by Sohn, Bong Won). In collaboration with VERA (VLBI Exploration of Radio Astrometry) in Japan, we have observed Active Galactic Nuclei (AGNs) and Orion-KL at 43GHz on 22nd and 23rd December, 2009, in order to evaluate the baseline- and image-sensitivity of KVN and KVN+VERA. In this talk we report the preliminary results of the VLBI test observations of the Korean VLBI Network at 43GHz. -
Following the success of detecting fringes on KVN (Korean VLBI Network), a phase referencing observation is currently planned in order to achieve a better sensitivity in mm-VLBI. The high frequency observation (
$\geq$ 22 GHz), wide bandwidths (~512 MHz) and high speed data recording (~1 Gbps, Mark5B) will result in resolution and sensitivity improvement on KVN. In particular, two powerful techniques of VLBI phase correction by fast-antenna switching and multi-frequency phase referencing are also introduced in KVN, hoping to resolve the problem of atmospheric delay errors which degrade the coherence significantly. In this study, we have compared the expected performance of phase referencing between fast antenna switching and multi-frequency phase referencing and discussed the essential condition and postulates of phase referencing for KVN. -
O, Se-Jin;Yeom, Jae-Hwan;No, Deok-Gyu;Park, Seon-Yeop;Kawaguchi, Noriyuki;Kobayashi, Hideyuki 44.1
한국천문연구원에서는 2009년 1단계 한일공동VLBI상관기(Korea-Japan Joint VLBI Correlator, KJJVC)의 개발과 설치를 완료하였다. KJJVC는 한국우주전파관측망(Korean VLBI Network, KVN), KVN과 일본 내의 VLBI 관측망을 포함하는 한일공동VLBI관측망(Korea-Japan Joint VLBI Network, KJJVN), 그리고 한중일의 VLBI관측망인 동아시아 VLBI관측망(East Asian VLBI Network, EAVN)으로 관측한 VLBI 데이터를 상관처리할 수 있도록 설계 제작되었다. 그리고 고속재생기, 데이터 동기재생처리시스템(Raw VLBI Data Buffer, RVDB), VLBI상관서브시스템(VLBI Correlation Subsystem, VCS), 데이터 아카이브 시스템(Peta-scale Epoch Data Archive, PEDA)로 구성된다. 특히 일본국립천문대 VERA에서는 테이프 형태의 DIR2000 고속기록기를 사용하고 있는데, DIR2000의 제품단종으로 인해 이 데이터를 VCS에 재생하기 위해 DIR1000을 개량한 VERA2000 고속재생기를 개발하였다. 즉, VSI 형태의 데이터를 1Gbps 속도로 재생만 하기 위해 기존의 시스템을 개량하였으며, 2009년 10월에 VLBI상관기실에 설치되었다. 본 논문에서는 VERA2000 시스템의 구성 및 개발, 시험운영 등에 대해 간략히 소개하고자 한다. -
Recently, SRAO has upgraded from one-pole system software to dual-pole system software. We present the new dual-pole system software and how it works in detail. Dual-pole observation is enabled with just some commands. To do so, backend-system controls two different hardwares, proceeds two different data and make two files at one observation.
-
한국천문연구원과 일본 국립천문대는 공동으로 한일공동VLBI상관기(Korea-Japan VLBI Correlator, KJJVC)를 개발하였다. 이 상관기는 최대 16 관측국에 대하여 16 세트의 자기상관 및 120 세트의 상호상관을 계산할 수 있다. 각 관측국당 최대 8,192 Mbits/sec의 입력 데이터를 처리할 수 있으며, 8,192개의 주파수채널을 갖는 상관 스펙트럼을 약 25.4 밀리초~수초의 적분 시간으로 출력할 수 있는데, 최대 상관 출력 속도는 1.4GB/sec이다. 한편, 이 상관기는 한국우주전파관측망(KVN) 뿐만 아니라 동아시아VLBI관측망 및 우주공간VLBI관측망의 관측 데이터도 처리할 수 있도록 설계 제작되었으며, 최대 지연 추적 범위는
${\pm}35,000km$ 이며, 보상 가능한 최대 기선 속도는 7.5km/sec이다. 현재 다른 VLBI관측망에서 사용하고 있는 타 상관기의 경우 지연은 2차 미분까지 보상하고, 프린지 위상은 3 단계로 보상하고 있는 것에 비하여, 한일공동VLBI상관기에서는 지연은 3차 미분까지 보상하여 지연 잔차를 최소화하고 프린지 위상은 16 단계로 세분하여 보상 수준의 정밀도를 최대화하였다. 이러한 지연 보상 및 프린지 멈춤 알고리즘을 상세히 소개하고 그 특성 및 장점을 보고한다. -
한국천문연구원은 한국우주전파관측망(Korean VLBI Network, KVN)에서 시험 운영 중인 한일공동VLBI상관기(Korea-Japan VLBI Correlator, KJJVC)의 핵심인 VLBI상관 서브시스템(VLBI Correlation Subsystem, VCS)을 제어하기 위해 CCS(Correlation Control Software)를 개발하였다. CCS는 명령어의 문법 검사를 하고, VCS와 TCP/IP 소켓으로 통신하여 명령어와 응답(reply)을 주고받으며, VCS의 실시간 요청에 대응하여 입력 지연 파라미터(delay parameter)를 자동으로 전달하는 소프트웨어이다. CCS는 사용자의 명령어를 local UNX FIFO를 통하여, 명령줄(Command Line)로 전달받고, 이러한 명령어들의 조합을 쉘 스크립트로 묶는 형태로 구성 되어있다. 그러나, 이렇게 명령어의 조합을 직접 편집하여 구성할 때, 입력할 명령어나 지연 파라미터의 구성이 복잡해지면, 스크립트에 필요한 명령이 문법에 맞지 않게 사용되거나, 일부 명령어가 누락될 수 있는 위험이 있다. 이러한 오류를 차단하고 작업 효율을 높이기 위하여, 상관 처리의 전체 운용 및 제어를 통합적으로 할 수 있는 사용자 인터페이스가 필요하다. 이를 위하여 KJJVC의 운용 및 제어를 위한 GUI를 설계하고 제작하였다. 개발된 GUI는 Python 언어를 기반으로 하는 wxPython 패키지를 사용하였으며, 사용자(Operator)가 명령어 문법이나 순서를 확인할 필요 없이, 관측 정보와 관측국 정보, 기록 매체 정보만 가지고 손쉽게 명령어의 조합을 생성해 주며, 시스템 초기화와 각종 정보의 입력이 직관적으로 이루어질 수 있도록 해 준다. 본 연구에서는 개발된 GUI의 설계 및 개발 과정과 시험운영에 대해 소개한다.
-
Chung, Hyun-Soo;Je, Do-Heung;Oh, Se-Jin;Roh, Duk-Gyoo;Sohn, Bong-Won;Lee, Sang-Sung;Kim, Hyo-Ryoung 46.1
APT(Asian-Pacific Telecommunity)는 아시아-태평양지역 국가의 공동이익을 도모하기 위하여 결성된 아-태지역 전파협의체 조직으로, WRC(세계전파통신회의)회의에서의 아-태지역 주관청의 공동이익을 얻기 위해 APG(APT Conference Preparatory Group for WRC)회의를 연간 1회의 비율로 개최하고 있다. WRC-12회의에 대비하여 결성된 APG-12 회의가 2010년 3월 태국 방콕에서 개최되었으며, 전파천문업무 보호 및 22 GHz 대역 달탐사, 38 GHz 대역 Space-VLBI운용대역과 관련된 WRC-12 의제 1.6, 1.11, 1.12 등에 대해 활발한 토론이 있었다. WRC-12 의제 1.6은 수동업무(전파천문업무, 지구탐사위성 및 우주연구업무)를 능동업무의 유해혼신으로부터 보호하기 위하여 제정한 전파규칙 각주 5.565조의 개정 검토와 관련된 의제이다. 따라서 한국천문연구원에서는 275 GHz 이상 대역에서의 전파천문업무의 원활한 운용을 위해, WRC회의에서 최종적인 규정개정을 함에 있어서 필요한 아-태지역 국가의 공동의견을 창출하기 위한 APT회의에서 주도적인 역할을 담당하고 있다. 본 발표에서는 APG-12 3차 회의에 제출한 우리나라의 기고서 제출 결과 및 동 회의에서의 최종결과 및 향후 대응책에 대해서도 알아보고자 한다. -
Chung, Hyun-Soo;Roh, Duk-Gyoo;Oh, Se-Jin;Je, Do-Heung;Sohn, Bong-Won;Lee, Sang-Sung;Kim, Hyo-Ryoung 46.2
APT(Asian-Pacific Telecommunity)는 아시아-태평양지역 국가의 공동이익을 도모하기 위하여 결성된 아-태지역 전파협의체 조직으로, WRC(세계전파통신회의)회의에서의 아-태지역 주관청의 공동이익을 얻기 위해 APG(APT Conference Preparatory Group for WRC)회의를 연간 1회의 비율로 개최하고 있다. WRC-12회의에 대비하여 결성된 APG-12 회의가 2010년 3월 태국 방콕에서 개최되었으며, 전파천문업무 보호 및 22 GHz 대역 달탐사, 38 GHz 대역 Space-VLBI운용대역과 관련된 WRC-11 의제 1.6, 1.11, 1.12 등에 대해 활발한 토론이 있었다. WRC-12 의제 1.11은 22.55-23.15GHz 대역을 달탐사의 관측자료 전송, 명령 및 제어링크 등을 위한 우주연구업무(지구대우주) 용도로 분배 검토하기 위한 의제이다. 따라서 한국천문연구원에서는 국가정책의 일환으로 추진되는 달탐사계획의 향후 원활한 자료전송, 자세링크, 명령을 원활히 수행하기 위해, WRC회의에서 최종적인 규정개정을 함에 있어서 필요한 아-태지역 국가의 공동의견을 창출하기 위한 APT회의에서 주도적인 역할을 담당하고 있다. 본 발표에서는 APG-12 3차 회의에 제출한 우리나라의 기고서 제출 결과 및 동 회의에서의 최종결과 및 향후 대응책에 대해서도 알아보고자 한다. -
Four of nine exoplanets found by microlensing were detected by the resonant caustic, which represents the merging of the planetary and central caustics at the position when the projected separation of a host star and a bounded planet is s~1. One of the resonant caustic lensing events, OGLE-2005-BLG-169, was a caustic-crossing high-magnification event with A_max ~800 and the source star was much smaller than the caustic, nevertheless the perturbation was not obviously apparent on the light curve of the event. In this paper, we investigate the perturbation pattern of the resonant caustic to understand why the perturbations induced by the caustic do not leave strong traces on the light curves of high-magnification events despite a small source/caustic size ratio. From this study, we find that the regions with small magnification excess around the center of the resonant caustic are rather widely formed, and the event passing the small-excess region produces a high-magnification event with a weak perturbation that is small relative to the amplification caused by the star and thus does not noticeably appear on the light curve of the event. We also find that the positive excess of the inside edge of the resonant caustic and the negative excess inside the caustic become stronger and wider as q increases, and thus the resonant caustic-crossing high-magnification events with the weak perturbation occur in the range of q
$\leq$ 10-4. We determine the probability of the occurrence of events with the small excess$|\varepsilon|{\leq}3%$ in high-magnification events induced by a resonant caustic. As a result, we find that for the Earth-mass planets with a separation of ~2.5 AU the resonant caustic high-magnification events with the weak perturbation can occur with a significant frequen. -
Omiya, Masashi;Han, In-Woo;Izumiura, Hideyuki;Lee, Byeong-Cheol;Sato, Bun'ei;Kim, Kang-Min;Yoon, Tae-Seog;Kambe, Eiji;Yoshida, Michitoshi;Masuda, Seiji;Toyota, Eri;Urakawa, Seitaro;Takada-Hidai, Masahide 48.2
Korean-Japanese Planet Search Program has been carried out since 2005 to search for planets around intermediate-mass giant stars (1.5-5.0 solar masses) by an international collaboration between Korean and Japanese researchers. In this program, we have been carrying out a precise radial velocity survey of about 190 G-type giant stars (6.21.9 solar masses) giant stars. These results extend the planet mass distribution of massive intermediate-mass stars to higher and lower mass region, and may further constrain substellar system formation mechanisms. We report the recent results and current status of Korean-Japanese Planet Search Program. -
The optical lightcurves of flare events can be regarded as a direct indicator about the existence of magnetic activity in low-mass stars. Stellar flares are generated by magnetodynamic processes in the stellar interiors as on the Sun and indicate that the locally intensified active regions still exist on the photosphere. However previous photometric observations are limited to a few selected active objects because of their faintness and randomness of the flare occurrence. Based on dedicated deep (r~23), long-term (24 night) time-series monitoring of the open cluster M37 from MMT 6.5m transit survey program, we searched for flare-like transient phenomena in the 3,052 M-dwarf lightcurves with relatively high-temporal resolution (30s-90s). In order to collect all statistical significant events, we applied the change-point analysis with filtering algorithm using local statistics. We found a number of flares from 412 M-dwarf stars that are probable cluster members. Nearly half of them have periodic brightness variations with a near or distorted sinusoidal shape. With a small exception of binary cases, most of these variations appear to reflect the presence of large starspots resulting in rotational brightness modulations. We will discuss the relationship among magnetic activity indicators and dependence on spectral type.
-
We have presented the evolutionary status of four detached double line spectroscopic eclipsing binaries which are CD Tau, CM Lac, HS Hya and ZZ Boo because the component stars of these binary systems still act as a single star. We determined the absolute dimensions of these binary systems using photometric and spectroscopic solutions from analysis of light curves and radial velocity curves. Using the luminosities, effective temperatures and masses we choose evolutionary tracks of these binary systems. Finally we obtained ages and metallicity of the stars. We found that CM Lac and HS Hya are very young stars and their ages are in range of 0.15-1.05 and 0.22-1.14 Gyrs. For CD Tau and ZZ Boo, they are older than the others and their age in range of 1.95-2.95 and 1.48-1.73 Gyrs.
-
We have analyzed times of minima for of 6 binary systems. Three binary systems show period decrease at rate
$3.19{\times}10-5$ yr -1 for SV Cen,$1.35{\times}10-7$ yr -1 for RT Scl and$1.14{\times}10-7$ yr -1 for AD Phe. Two systems show period increase$5.696{\times}10-8$ yr -1 for SX Aur and$6.93{\times}10-8$ yr -1 for GO Cyg. One system shows cyclic period variation. We estimated the mass transfer rate for 5 binary systems. Four systems show asymmetric light curves. Two asymmetric light curves (SV Cen and RT Scl) are due to hot spot caused by mass transfer. And two asymmetric light curves (AD Phe and TY Boo) are due to cool spot caused by magnetic activities on the cooler component. We also obtain absolute dimensions from photometric solution and spectroscopic solution by analyzing their light curves and radial velocity curves, which are collected from literatures, using 2007 version Wilson and Deviney computer code. -
We present the explicit expressions for the matrix elements associated with the interaction of photons with atomic hydrogen. These expressions are applied to compute the scattering cross section for the Raman scattering operating blueward of Lyman epsilon and H gamma. A brief discussion that re relevant to some symbiotic stars and young planetary nebulae is also presented.
-
We present the interim results of simultaneous observations of SiO and H2O masers toward 401 known stellar SiO and/or H2O maser sources (166 both SiO and H2O maser sources, 83 only SiO maser sources, and 152 only H2O maser sources) using KVN_Yonsei telescope. The results of 166 known SiO/H2O maser sources will be presented by Kim et al. and the results of 83 only SiO maser sources and 152 only H2O maser sources presented here. Both SiO and H2O maser emission were detected from 30 sources giving a detection rate of 36 % toward known 83 only SiO maser sources, while they were detected from 66 sources giving a detection rate of 43 % toward known 152 only H2O maser sources at one epoch observation. Only SiO masers were detected from 42 sources toward 83 only SiO sources, while they were detected from 28 sources toward 152 only H2O sources. Characteristics of these observed sources in the IRAS two-color diagram is investigated including mutual relations between SiO and H2O maser emission. In addition, these results will be useful for statistical study of late-type stars and future VLBI observations.
-
We have carried out an extensive statistical analysis based on the results of simultaneous observations of SiO and
$H_2O$ masers toward 166 known SiO and$H_2O$ maser sources using KVN_Yonsei radio telescope (Kim et al.2010, ApJS submitted). We investigate the distributions of the mean velocities and the intensity ratios between SiO and$H_2O$ maser emission including those between SiO v=1 and v=2,J=1-0 transitions according to type of evolved stars. We also investigate mutual relations between SiO and$H_2O$ maser properties(total flux densities and velocity structures etc.) according to stellar pulsation phases. Most of SiO masers appear around the stellar velocity (80 % within${\pm}5km\;s^{-1}$ ), while$H_2O$ masers show a different characteristic compared with SiO masers (69% within${\pm}5km\;s^{-1}$ ). In addition, we investigate a correlation between$SiO/H_2O$ maser emission and AKARIFIS flux density as well as the AKARI color characteristics of SiO and$H_2O$ observational results in the AKARIFIS two-color diagram. -
The relationship between orbital periods of cataclysmic variables (CV) and mass-loss rates of their donor stars is an important subject of theoretical researches. The observed donor's radii are oversized in comparison with those of isolated unperturbed stars of the same mass, which is thought to be a consequence of the mass-loss. Using the empirical mass-radius relation of CVs and the Hayashi theory for changes in effective temperature, orbital period, and luminosity of the donor with the stellar radius, we find the mass-loss rate of CVs as a function of the orbital period P. The derived mass-loss rate is more or less constant at 10-9.6-10-10M
$\odot$ yr-1 with P above 90 minutes and declines very rapidly with P below 90 minutes, reaching 10-10.3-10-11.7M$\odot$ yr-1 when P is close to the minimum period. The turnaround behavior of the mass-loss rate shape with P near the minimal period is much less pronounced than suggested by earlier numerical models, making observational detection of the turnaround highly unlikely. When applied to our new results, SDSS 1035, 1507, 1501 and 1433 systems, previously known as post-bounce CVs, are more likely to be systems that have yet to reach the minimal period. -
In search of the intracluster dusts, we have made a survey of globular clusters (GCs) with the Far-Infrared Surveyor (FIS) aboard AKARI, the Japanese infrared space satellite. The GCs are thought to host dust particles that are condensed from the material injected by the cluster asymptotic giant branch (AGB) stars. However, attempts to detect dust emission from GCs had not been successful until a significant amount of far-infrared (FIR) emission was detected close to the NGC 7078 center by the ISO observations (Evans et al. 2003). Recent FIR observations by the AKARI (Matsunaga et al. 2008) and the Spitzer Space Telescope (Boyer et al. 2006; Barmpy et al. 2009) reported a tentative detection of the dusts in NGC 5024 and NGC 6341, and also confirmed the previous ISO dust detection from NGC 7078. We have observed 17 selected GCs in four FIS wavebands at 65, 90, 140, and 160 micrometers. Each observation covers about
$10'{\times}10'$ area centered at each GC. The resulting images show extended structures and/or blobs around the GCs. The extended structures are very suggestive of the Galactic cirrus, while the blobs around NGC 288 and NGC 4833 seem to be related to the two clusters. In this presentation, we will report four representative cases of our survey results and discuss the properties of newly detected sources. -
Im, Dong-Uk;Han, Sang-Il;Cheon, Sang-Hyeon;Jeong, Mi-Yeong;Jang, Cho-Rong;Han, Mi-Hwa;Kim, Myo-Jin;Son, Yeong-Jong 53.1
$Y^2$ (Yonsei-Yale) Isochrones은 Yale의 항성 진화 계산을 이용한 정밀한 등연령곡선으로 구상성단의 연구에 널리 사용되고 있다. 이번 연구에서는$Y^2$ -Isochrones를 Kurucz 모형을 이용한 색변환을 통해서 SDSS로 널리 알려진 ugriz 필터 체계에 대해 적용하고 실제 관측 결과와 비교함으로써 타당성을 검증하고자 한다. 우선 ugriz 필터의 등연령곡선을 제공하는 BaSTI와 DSEP, Padova 모델간의 비교를 통해$Y^2$ -Isochorones이 MSTO에서 g-r값이 다른 모델에 비해 0.05정도 큼을 확인하였다. 또한 CFHT 3.6m 망원경의 가시광 카메라 MegaCam으로부터 얻은 중원소 함량이 낮은 다섯 개의 구상성단 M15, M30, M53, NGC 5053, NGC 5466에 대한 g, r, i 필터의 색등급도에 각각의 등연령곡선을 적용하여 모델에 따른 구상성단의 특성을 분석하였다.$Y^2$ -isochrones를 이용한 (g-r, r) CMD의 분석 결과, BaSTI와 DSEP 모델에 비해 0.1~0.3만큼 거리지수가 크고, 성단의 나이는 1~3Gyr 정도 어리게 측정됨을 확인할 수 있었다. 더불어 SDSS 관측으로부터 얻어진 구상성단에 대한 색등급도와 비교 분석과정을 수행하여, 다른 망원경에서의 사용가능 여부를 확인하였다. 이 연구를 통하여 각 모델에 따른 등연령곡선의 차이를 확인하고, 현재 여러 망원경에서 사용되고, 앞으로 여러 대형망원경에서 사용될 ugriz 필터 체계에$Y^2$ -Isochrones를 적용할 수 있는 타당성을 제시하고자 한다. -
Using the JHK 2MASS near-infrared data, we present photometry results for the old open cluster (OC) Trumpler 5 (Tr 5). From the near-infrared color-magnitude diagrams of Tr 5, we have located the position of the red giant clump (RGC) stars, and used the mean magnitude of the RGC stars in K-band to estimate the distance to Tr 5. From the Padova isochrone fittings, we have estimated the reddening, metallicity, and age of Tr 5. These parameters generally agree well with those obtained from the previous studies on Tr 5 and confirms that this cluster is an old OC with metallicity being metal-poorer than solar abundance, located in the anti-Galactic center region.
-
최근 이루어진 구상성단내 다중항성종족의 발견은 항성계의 형성 및 진화, 더 나아가 우리 은하의 형성 등에 획기적인 변혁을 필요로 하는 중요한 사건이다. 본 발표에서는 항성종족이론이 현재 직면한 문제점들과 해결 방안들을 대한 검토와 KGMT시대에 대비한 전망을 토의할 것이다.
-
The most massive galactic globular cluster,
$\omega$ Cen has been observed using recently mounted WFC3/UVIS cameras of Hubble Space Telescope at both near-UV and optical bands. We present the photometry of stars in the central region of$\omega$ Cen in F225W, F275W and F336W bands. The near-UV color-magnitude diagrams and color-color diagrams of stars in$\omega$ Cen show multiple red giant branches and main sequences as already discovered in both ground-based and HST/ACS observations in the optical bands. We modelled the stellar populations of$\omega$ Cen using Yonsei Isochrone, where$\alpha$ -particles and helium enhancement processes have been included properly. We compare the best-fit stellar populations obtained from the current near-UV observations to the suggested stellar population models based on optical band data. We also discuss the methodological issues arising when dealing with the near-UV observations; red-leak in near-UV filters and the huge interstellar extinction in near-UV bands compared to the optical bands and its non-linear effect in color-magnitude diagrams. -
대마젤란 은하에 속한 식쌍성의 시선속도 곡선을 완성하기 위하여 2009년 11월 칠레에 위치한 Cerro Tololo Inter-American Observatory (CTIO)의 1.5m 망원경과 R-C Spectrograph를 사용하여 중 분산 분광관측을 수행하였다. 분광관측은 380nm - 540nm 영역에서
$H_8,\;H_{\varepsilon},\;H_{\delta},\;H_{\Gamma},\;H_{\beta}$ 등의 흡수선을 관측하였다. 중분산으로 관측된 식쌍성의 각 구성원별에서 나오는 흡수선들은 구별되지 않으므로 이를 구별하기 위하여 구성원들의 Flux 비와 함께 gauss curves fitting 방법으로 각 흡수선들을 2개의 성분으로 분해하여 시선속도를 측정하고, 시선속도곡선을 완성하였다. 완성된 이중 시선속도 곡선은 Wilson & Devinney 차등 보정법으로 분석하여, 궤도 장반경, 질량비, 계의 시선속도 등을 구하였다. 또한 각 식쌍성들의 광도곡선을 분석하여 측광학적인 해를 구하고, 최종적으로 분광 및 측광관측의 해를 혼합하여 대마젤란은하 식쌍성들의 절대량을 구하였다. 이후 이를 바탕으로 거리를 구하여 기존에 발표된 마젤란은하의 거리와 비교하였다. -
We present a photometric and spectroscopic study of the globular clusters (GCs) in the giant elliptical galaxy NGC 4636 in the Virgo cluster. The photometry of the GCs is based on HST/WFPC2 images for the inner region and deep, wide field Washington
$CT_1$ CCD images for the outer region. We investigated the color distribution, the radial number density profile, the spatial distribution, and the mean color of the bright blue GCs about the GCs in NGC 4636. We obtained spectra of the GC candidates in NGC 4636 using the Multi-Object Spectroscopy (MOS) mode of Faint Object Camera and Spectrograph (FOCAS) on the SUBARU 8.2m Telescope. We measured the velocities for 105 GCs in NGC 4636. Using the 238 GCs obtained from combining our results with data in the literature, we investigated the kinematics of the GC system of NGC 4636: the rotation, the velocity dispersion, the radial variation, and the orbit. We also investigated the distribution and the radial variation of the metallicities, ages, and alpha-elements of the GCs in NGC 4636 derived using the absorption lines. We compared the GC kinematics of NGC 4636 with those of other six gEs, finding that the kinematic properties of the GCs are diverse among gEs. We found several correlations between the kinematics of the GCs and the global parameters of their host galaxies. Finally we discuss the implication of the results for the formation models of the GC system in gEs, and suggest a mixture scenario for the origin of the GCs in gEs. -
We present JHK photometry of star clusters in the dwarf irregular/dwarf starburst galaxy NGC 1569. Adopting several criteria to exclude other sources like foreground stars, background galaxies, etc., ~150 star cluster candidates are identified in the near-infrared images of NGC 1569, which include very young star clusters. From analysis based on theoretical background, we find ten very young star clusters near the center of this galaxy. The total reddening values toward these clusters are estimated from comparison with the theoretical estimates given by star cluster mode.
-
M87, a cD galaxy in the Virgo cluster, has 3-10 times larger enclosed mass than the Milky Way at any given galactocentric radius. Thus the globular cluster (GC) system in M87 is expected to have undergone a more significant dynamical evolution than that of the Milky Way if it had started from the same initial mass function (MF) and radial distribution (RD) as the Milky Way. The evolution of MF and RD of the M87 GC system has been calculated using an advanced, realistic Fokker-Planck (FP) model that considers dynamical friction, disk/bulge shocks, and eccentric cluster orbits. We perform hundreds of FP calculations with different initial cluster conditions, and then search a wide parameter space for the best-fit initial GC MF and RD that evolves into the observed present-day GC MF and RD. We also find best-fit initial MFs and RDs for blue and red GC groups, separately.
-
Kim, Kee-Tae;Byun, Do-Young;Oh, Chung-Sik;Kang, Hyun-Woo;Bae, Jae-Han;Youn, So-Young;Kim, Won-Joo 58.1
We carried out simultaneous 22GHz$H_2O$ and 44GHz$CH_3OH$ maser line surveys of about 1000 galactic YSOs using KVN 21m telescopes. The sources consist of low-mass, intermediate-mass, high-mass YSOs in different evolutionary stages. We will present the preliminary results. -
L1251B, which was revealed as a small group of protostars by the Spitzer Space Telescope (SST), presents a great site of studying chemical evolution in gas and ice as well as various dynamical processes associated with star formation (infall, rotation, and outflow). We have mapped L1251B with the Infrared Spectrograph (IRS) aboard the SST to study the chemical distribution in the phases of gas and ice and the dynamical feature related to shock in the region. Various atomic lines and the
$H_2$ pure rotational lines, which trace different shock velocities, were detected. In addition, the distribution of the water and$CO_2$ ices hints variety of the ice desorption mechanism in L1251B. -
Kim, Jae-Yeong;Pak, Soo-Jong;Choi, Min-Ho;Kwon, Jung-Mi;Kandori, Ryo;Nakajima, Yasushi;Tamura, M.;Nagata, T.;Sato, S. 59.1
We present wide-field near-IR imaging polarimetry of 30 Doradus, using the InfraRed Survey Facility(IRSF) 1.4 m telescope at the South African Astronomical Observatory. We obtained polarimetry data in J, H, and Ks bands using the JHKs-simultaneous imaging polarimeter SIRPOL. 30 Doradus is located in the Large Magellanic Cloud(LMC) and it is the most active starburst region known in the Local group of galaxies. 30 Doradus is one of the best field to examine the behavior of the interstellar medium and star-formation mechanism under different conditions. We will investigate the structure of magnetic field in 30 Doradus region. -
The structures of the protoplanetary nebula have been examined under various conditions of the stellar wind and the mass distribution of the nebula by assuming that the nebula is steady and geometrically thick. T Tauri stars commonly accompany with disks as well as the stellar wind. Therefore, the nebula around T Tauri stars should be influenced by the stellar wind. The results are summarized as follows ; The height of the geometrical surface of the nebula is suppressed by the dynamical pressure of the wind but depends very weakly on the wind strength. The surface becomes higher slightly when the wind strength becomes weaker. Furthermore, the dependency of the nebular height on the mass distribution of the nebula is also weak. As a natural result of the above, the temperature distribution in the nebula is insensitive to the wind strength and the mass distribution of the nebula, too. Thus, we can conclude that the temperature and geometrical surface height of the nebula under the stellar wind does not depend on neither the wind properties nor the mass distribution of nebula.
-
Methanol maser sources are believed to represent the earliest evolutionary stage of massive star formation. Pandian et al. (2007) recently made a very sensitive blind survey of 6.7GHz ClassII methanol maser towards the Galacitic midplane (
$35^{\circ}$ <1<$55^{\circ}$ & |b|<$0.5^{\circ}$ ) and found 86 maser sources. We carried out 22GHz$H_2O$ and 44.0 GHz$CH_3OH$ maser line surveys of them with KVN 21m and various (CO (2-1),$^{13}CO$ (2-1),$^{13}CO$ (1-0),$C^{18}O$ (2-1), CS (2-1),$HCO^+$ (3-2) and HCN (3-2)) molecular line surveys with SRAO 6m and TRAO 14m. we will present the preliminary results and discuss the implications for massive star formation. -
We have studied the abundance ratio of HNC and HCN toward the Red MSX Sources (RMS) using HCN (J=1-0), HNC (J=1-0),
$H^{13}CN$ (J=1-0),$HN^{13}C$ (J=1-0),and$N_2H^+$ (J=1-0) lines observed with the Mopra 22 m radio telescope. The RMS are massive young stellar objects identified by the MSX satellite data combined with the 2MASS data. HCN and HNC (a geometrical isomer of HCN) are among the most basic interstellar molecules. According to our analysis, the column density of HCN is found to be correlated with that of HNC. Additionally, the [HNC]/[HCN] abundance ratio is sensitive to the core temperature because HNC is depleted in high temperature regions. This result is consistent with the previous results seen in low mass starless or protostellar cores. -
Park, Byeong-Gon;Kim, Yeong-Su;Gyeong, Jae-Man;Yuk, In-Su;Cheon, Mu-Yeong;Kim, Sang-Cheol;Yeo, A-Ran;Park, Gwi-Jong;Kim, Gang-Min;Lee, Seong-Ho;Parkt, Chan;O, Hui-Yeong;An, Gi-Beom;Choe, Ji-Hye;Go, Ju-Heon;Kim, Eun-Gyeong 61.1
한국천문연구원의 대형광학망원경 개발사업(K-GMT)은 거대마젤란망원경(GMT; Giant Magellan Telescope)의 지분 10% 확보를 목표로 2009년부터 2018년까지 수행하고 있는 사업이다. 2009년 GMT사업에 공식 참여한 한국천문연구원은 GMT 이사회와 과학자문위원회 등에 적극적으로 참여하여 활동하였다. 본 사업의 2차년도에 해당하는 2010년에는 K-GMT 과학기기워킹그룹을 중심으로 거대망원경 여름학교와 국제워크숍을 개최할 예정이며 GMT 이사회 한국 개최, GMT 부경 시험 모델 개발, GMT 1세대 관측기기 후보로 선정된 GMTNIRS 개념설계연구 등이 수행될 예정이다. 본 발표에서는 GMT 및 K-GMT의 2010년 주요 활동 계획을 보고한다. -
Yuk, In-Soo;Lee, Sung-Ho;Chun, Moo-Young;Kim, Kang-Min;Park, Chan;Pak, Soo-Jong;Oh, Hee-Young;Lee, Sang-On;Lee, Han-Shin;Jaffe, Daniel T.;Pyo, Tae-Soo;Park, Byeong-Gon;Kim, Young-Soo;Kyeong, Jae-Mann 61.2
GMTNIRS (the GMT Near Infrared Spectrograph) is one of the first generation instrument candidates for GMT (Giant Magellan Telescope). Conceptual design studies for nine instruments were proposed last year, and the GMT organization selected 6 instruments including GMTNIRS for the next phase. GMTNIRS will be developed by an international collaboration between KASI and UT(University of Texas). KASI and UT have been also developing IGRINS (the Immersion Grating Infrared Spectrometer) which is a fore-runner instrument of GMTNIRS since 2009. In this talk, we will present the instrument details and development plan, and discuss the science case for GMTNIRS. -
Kyeong, Jae-Mann;Kim, Young-Soo;Park, Byeong-Gon;Yuk, In-Soo;Kim, Sang-Chul;Lyo, A-Ran;Chun, Moo-Young 62.1
GMTO(Giant Magellan Telescope Organization) 이사회(Board Meeting)는 GMT의 1세대관측기기 1차 선정을 하였다. 의향서(Letter of Intent)를 제출한 12개 기기 중 9개 기기에 대해 제안서를 받아 과학자문위원회(Science Advisory Committee)에서 과학적 측면(Science), 기술적 측면(Technical), 비용 및 작업범위측면(Cost, scope & management)에서 심사한 결과 6개를 추천하였고 이사회에서 이를 승인하였다. 한국이 참여하는 GMTNIRS를 포함하여 G-CLEF, GMACS, GMTIFS, NIRMOS, TIGER가 선정되었다. 이 기기들은 2010년 4월부터 14개월 동안의 Conceptual Design Study를 거쳐 2011년 하반기에 이중에서 다시 3~4개가 GMT 1세대 관측기기로 최종 선정되어 제작될 예정이다. -
Kim, Yeong-Su;Park, Gwi-Jong;Yang, Ho-Sun;Song, Jae-Bong;Kim, Hak-Yong;An, Hyo-Seong;An, Gi-Beom;Jang, Jeong-Gyun;Go, Ju-Heon;Kim, Eun-Gyeong;Choe, Ji-Hye;Park, Byeong-Gon;Gyeong, Jae-Man;Yuk, In-Su 62.2
한국천문연구원은 GMT (Giant Magellan Telescope)의 부경 중의 하나인 FSM (Fast Steering Mirror)의 시험모델을 한국표준과학연구원, 광주과학기술원, 미국 NOAO와 협력하여 개발 중이다. FSM은 주로 반사경과 지지부, tip-tilt 부분으로 나누어질 수 있는데, 개념설계 이후 광축 지지부가 tip-tilt 기능도 겸하여 수행하는 것으로 설계변경되었다. 이 논문에서는 변경된 FSM의 구조를 파악하고 이에따른 시험모델의 개발 현황에 대하여 논한다. -
Over its 30-year lifetime, UKIRT has been the world's leading telescope devoted exclusively to observations in the infrared. Its outstanding success over this period is attributable to a number of factors, foremost among which are the size (3.6m) and high quality of the mirror, the excellent site at the summit of Mauna Kea, and the deployment of unique, world-beating instrumentation. In recent years, as the UK has re-directed its investment in astronomical facilities towards ESO, UKIRT has focussed on wide-field imaging in the near infrared, and we are currently conducting a definitive programme known as the UKIRT Infrared Deep Sky Survey (UKIDSS). In this presentation I will describe UKIRT's current capabilities, its evolving operation, opportunities for Korean participation, and possibilities for its future development.
-
2010년대 후반에 완성될 거대마젤란 망원경을 비롯한 차세대 망원경들의 개발을 앞두고 한국천문학의 현재를 짚어보기 위해, 본 연구에서는 대형망원경을 이용한 연구현황을 조사하여 발표한다. 4미터급 이상의 대형망원경을 사용하여 개인/공동 연구 등을 통해 수행되고 있는 관측 연구들을 파악하고 연구 주제들 및 사용되고 있는 관측기기들의 범위를 조사하여 국내연구진의 관측연구 현황 및 역량을 보고 한다.
-
연세대학교 천문우주학과는 미국 국립천문대가 지난 2005년 공모한 CTIO 4m 광학망원경에 대한 운영협력기관(Operations Partnership)으로 선정되어 2006년부터 2009년까지 3년간 년 14일의 관측을 수행하였다. 이 프로젝트를 통해 구상성단과 타원은하의 항성종족에 대한 다양한 관측연구가 수행되었고, 관측자료 분석은 앞으로도 계속될 예정이다. 이를 통해 많은 대학원생들이 중대형 광학망원경의 관측 경험을 축적할 수 있었고, 앞으로도 유사한 프로젝트를 계속 수행할 예정이다.
-
From 2009, CEOU of Seoul National University has been utilizing the United Kingdom Infrared Telescope (UKIRT) at Mauna Kea, Hawaii, as one of its research facilities. UKIRT is a telescope with 3.8m primary mirror, and it is currently the largest telescope specialized for infrared observations. We will summarize our research activities using UKIRT, which include Infrared Medium-deep Survey (IMS) of proto-clusters and high redshift quasars, NIR imaging programs of Gamma Ray Bursts (GRBs), Gamma Ray sources, and SNUQSO quasars. Our research programs include international collaboration with the UK GRB team, the NASA/Swift team, Pomona College, and National Central University of Taiwan. We will also touch on our future plan of using UKIRT.
-
성간난류에 대해 간략히 소개하고 최근의 관측결과를 살펴본다. 최근 연구 결과에 의하면 성간난류는 은하자기장의 생성에 기여하며 별 생성에 결정적인 역할을 한다. 성간난류는 다양한 형태로 나타날 수 있다. 예를 들어 성간매질에는 여러 가지 상(phase)이 존재하며 상이 달라지면 난류의 성질이 달라지며 난류의 구조도 달라진다. 매질이 달라지면 난류를 관측하는 방법도 달라질 수밖에 없다. 본 발표에서는 성간매질의 상(phase)에 따라 어떤 종류의 난류가 존재하며 어떤 관측을 통해 연구하는 지를 알아본다. 또한 성간공간에 실재하는 3차원 난류의 물리량과 천구면에 투영된 2차원 물리량 사이에는 어떤 관계가 있는지를 살펴본다.
-
Lee, Young-Ung;Kim, Young-Sik;Kang, Hyun-Woo;Jung, Jae-Hoon;Kim, Hyun-Goo;Lee, Chang-Hoon;Yim, In-Sung;Kim, Bong-Gyu;Kim, Kwang-Tae 65.2
We present a result of$^{13}CO$ (1-0) survey toward the Outer Galactic Plane using the multi-beam receiver system recently installed on the 14 m telescope at Taeduk Radio Astronomy Observatory(TRAO). Our first target region is from$l=108^{\circ}$ to$113^{\circ}$ and$b=-1^{\circ}$ to$+1^{\circ}$ , and some extended regions are included where emission is still arising. All data are on 50" grid. Velocity resolution is 0.63 km/sec, and the total velocity range is from -150 km/sec to 100 km/sec. A total of 40,000 spectra were obtained. The rms noise is about 0.2 K per channel for unsmoothed raw data. We will present a few initial results of the survey database. -
Using two-dimensional numerical hydrodynamic simulations, we investigate the star formation rate (SFR) in turbulent, multiphase, galactic gaseous disks. Our simulation domain is axisymmetric, and local in the radial direction and global in the vertical direction. Our models include galactic rotation, vertical density stratification, self-gravity, radiative heating and cooling, and thermal conduction, but do not include spiral-arm features. Turbulence in our models is driven by momentum feedback from supernova explosion events occurring in localized dense regions formed by thermal and gravitational instabilities. Self-consistent radiative heating, representing enhanced/reduced FUV photons from the star formation, is also taken into account. By controlling three parameters (the gas surface density, the stellar disk density, and the angular rotation rate) that characterize local galactic disks, we explore how the SFR depends on the background environmental state. We also discuss the relation between the SFR and the gas surface density found in our numerical models in comparison with observations.
-
We have studied the properties of interstellar turbulence as observed by Boston University-Five College Radio Astronomy Observatory (BU-FCRAO) Galactic Ring Survey (GRS). This observation uses 13CO J=
$1{\rightarrow}0$ emission with high spectral resolution of 0.21 kms-1 and covers wide galactic plane regions ($18^{\circ}$ < 1 <$55.7^{\circ}$ and -1 < b <$1^{\circ}$ ). Firstly, we measured the one dimensional power spectrum of 13CO intensity along the galactic longitude and along the galactic latitude. We found the slope of the power spectrum changes around the molecular ring structure and the center of the galactic plane. Secondly, we explored how the power spectral slope is related with the velocity dispersion of supersonic giant molecular clouds in the GRS. Finally, we suggest the turbulent nature of the interstellar medium is connected with star formation activities in spiral arms. -
Understanding the nature of MHD turbulence is of fundamental importance in astrophysics. The results of these studies can be used to develop the star formation theory. While most of previous studies have considered turbulence in uniform media, the stratification of media can play an important role. We performed three-dimensional numerical simulations of isothermal, compressible, MHD turbulence with different plasma beta's and different flow Mach numbers in stratified media to study the effects of stratification on turbulence. We found Statistics of turbulent flow in stratified media is different from in uniform media. In this talk, we present the statistical properties of the MHD turbulence, such as the PDF, power spectrum, and structure function.
-
구형 분자운에서의 복사전달문제를 탈출확률방법에 기초하여 non-local method로 풀었다. 매질을 여러 개의 구간으로 나누고 각 구간에서 물리량이 일정하다고 가정하여 복사전달식을 전개하였고 뉴턴방법을 채택하여 수렴속도를 빠르게 하였다. 이번 연구에서는 분자운 내부의 속도구배가 작든 크든 상관없이 복사전달식을 풀 수 있도록 수치코드를 개발하였다. 우리의 계산 결과는 속도구배가 큰 경우에는 LVG방법을 사용한 결과와 일치하고, 분자운이 정적인 경우에도 이전 연구의 결과와 일치한다. 앞으로 이 방법에 line-overlap과 saturation효과를 추가하여 만기형 별에서의 SiO메이저 연구에 활용할 계획이다.
-
Park, Sung-Joon;Min, Kyoung-Wook;Seon, Kwang-Il;Han, Won-Yong;Lee, Dae-Hee;Edelstein, Jerry;Korpela, Eric;Sankrit, Ravi 68.1
We focus on two Galactic molecular clouds that are located in wholly different environments and both are observed by FIMS instrument onboard STSAT-1. The Draco cloud is known as a translucent molecular cloud at high Galactic latitude. The FUV spectra show important ionic lines of C IV, Si IV+O IV], Si II* and Al II, indicating the existence of hot and warm interstellar gases in the region. The enhanced C IV emission inside the Draco cloud region is attributable to the turbulent mixing of the interacting cold and warm/hot media, which is supported by the detection of the O III] emission line and the$H{\alpha}$ feature in this region. The Si II* emission covers the remainder of the region outside the Draco cloud, in agreement with previous observations of Galactic halos. Additionally, the H2 fluorescent map is consistent with the morphology of the atomic neutral hydrogen and dust emission of the Draco cloud. In the Aquila Rift region near Galactic plane, FIMS observed that the FUV continuum emission from the core of the Aquila Rift suffers heavy dust extinction. The entire field is divided into three sub-regions that are known as the- "halo," "diffuse," and "star-forming" regions. The "diffuse" and "star-forming" regions show various prominent H2 fluorescent emission lines, while the "halo" region indicates the general ubiquitous characteristics of H2. The CLOUD model and the FUV line ratio are included here to investigate the physical conditions of each sub-region. Finally, the development of an infrared imaging system known as the MIRIS instrument onboard STSAT-3 is briefly introduced. It can be used in WIM studies through$Pa{\alpha}$ observations. -
We present near-infrared (NIR) spectra of 6 young stellar objects (YSOs) around the supernova remnant G54.1+0.3 obtained with TripleSpec, a slit-based NIR cross-dispersion echelle spectrograph on th 5-m Palomar Hale telescope covering the entire NIR atmospheric window of 1-2.4 micron. These YSOs, whose formation was possibly triggered by the progenitor of G54.1+0.3, show significant mid-infrared (MIR) excess and have been proposed to be late O- and early B-type YSOs based on their spectral energy distribution. Our TripleSpec observations reveal the existence of strong H and He I lines, consistent with the previous interpretation of their spectral types, while the absence of Br-gamma emission line indicates that the YSOs do not have a nearby circumstellar disk. We discuss the relation between these YSOs and G54.1+0.3 based on the TripleSpec data and previous photometric data as well.
-
IC 443 is famous for its interaction with nearby molecular clouds and intense H2 emission lines in infrared. Therefore, it has been studied extensively for the understanding of molecular shocks. We observed H2 mission lines toward the shock-cloud interaction regions of IC 443, known as clumps B, C, and G. The observations were performed with the InfraRed Camera (IRC) onboard a satellite AKARI over 2.5-5.0 um, where previous space observations, e.g. Infrared Space Observatory (ISO) and Spitzer, do not cover. Our AKARI observations provide spectra of sequential pure-rotational and ro-vibrational H2 emission lines. For the clumps C and G, combining with previous mid-infrared observational results, we found that the H2 level populations show a significant separation between v=0 and v=1 levels; v=1 levels are under-populated than v=0 levels, therefore, the population cannot be described by two temperature LTE model, as many people have analyzed for the shocked H2 gas. We also applied the thermal admixture model, dN(H2; T)~T^(-b) dT, with varying ortho-to-para ratios according to the temperature, to describe the level population, and obtained plausible ranges of the H2 gas density and power-law index b.
-
The far-ultraviolet (FUV) H2 and C IV emission images and spectra of Orion Eridanus Superbubble (OES) is hereby presented. The OES seems to consists of multiple phase through the detection of highly-ionized gas and pervasive neutral hydrogen. The former is traced by hot gas while the latter is traced by cold medium. A spectral image made with H2 fluorescent emission shows that the spatial distribution of hydrogen molecule is well correlated with the dust map. The model spectra was taken from a photodissociation region (PDR) radiation code which find a best suitable parameter such as hydrogen density, gas temperature and incident uv intensity of the radiation field. C IV emission is caused by intermediate temperature ISM about 10^4.5 K~10^6 K. Therefore we could get more clear evidence to reveal the structure of OES. Feature of spectra for the each sub region is also presented and discussed. The data were obtained with the Far-Ultraviolet Imaging Spectrograph (FIMS) and the whole data handling were followed by previous FIMS analysis.
-
We present the far-ultraviolet (FUV) emission line morphologies in the whole region of the supernova remnant G65.3+5.7 using the FIMS/SPEAR data. The morphologies of the C IV
${\lambda}{\lambda}1548$ , 1551,$H2{\lambda}1608 $ , He II${\lambda}1640$ , and O III]${\lambda}{\lambda}1661$ , 1666 lines appear to correlate clearly with the optical emission line images or the ROSAT X-ray (0.11-0.284 keV) image obtained in some of the previous studies. We found that a foreground dust cloud, resonant scattering, and incompleteness of radiative shocks have made the definite differences between the morphologies of the above FUV emission lines. We also present the FUV spectra and line intensities from a few sub-regions. -
We present near- and mid-infrared images of the Crab Nebula, taken with the Infrared Camera (IRC) onboard the AKARI infrared space telescope. These images have a field-of-view of 10'*10' and show the full extent of the nebula at 3, 4, 7, 11, 15, and 24 um. The Crab nebula in near infrared is dominated by synchrotron emission while, in mid infrared, the ionic forbidden lines of Ar, Ne, S, and Fe makes significant contribution. We separate the line emission from synchrotron emission in 3-15 um AKARI bands using the ISOCAM CVF data, and present separate images for the line and synchrotron emissions in each band. We derive the total synchrotron fluxes of the Crab nebula in these bands, which are used to complete the synchrotron spectral energy distribution of the Crab nebula from radio to X-rays. We discuss the spectral variations of the Crab nebula.
-
Lim, Tae-Ho;Min, Kyung-Wook;Park, Jae-Woo;Kim, Il-Joong;Park, Sung-Joon;Lim, Yeo-Myung;Lee, Dae-Hee;Seon, Kwang-Il 71.1
We present the FUV continuum map of The Taurus-Auriga-Perseus complex, which is one of the largest local association of dark clouds. The map is well consistent with the dust extinction and the CO emission map of the T-P-A region. The region is divided into 3 sub-regions by diffuse FUV intensities and the spectra of each region imply that the radiation field due to the Per OB2-association can be a main source of the H2 fluorescent emission of the nearby cloud region. We used the PDR H2 model, named CLOUD, developed by van Dishoeck &Black for the sake of comparing our results to the H2 model. -
Cooling hot gas sets a floor on the ionization level for diffuse gas in the ISM in general and the galactic halo. Many high galactic latitude sight lines, cooling hot gas is the dominant source of the ionization. Such sites are prime regions for the formation of both C IV and Si IV ions at a temperature of T~105K. To study of the ISM that have the 104.5~6K ionization state by ionization or photoionization by the collision, searching for the radiation energy that is emitted at far ultra violet range is required. In this paper, we report the analysis of NGP( North Galactic Pole,
$l:270^{\circ},b:90^{\circ},rad:40^{\circ}$ ) region by fuv($1350{\sim}1750{\AA}$ ) data that are surveyed with FIMS. After making the FIMS FUV image of the NGP region, we divided up into 50 small regions for that and got the spectrum emission lines from each one. -
Kim, Sung-Soo S.;Saitoh, Takayuki;Jeon, Myoung-Won;Merritt, David;Figer, Donal F.;Wada, Keiich 72.1
Gas materials in the inner Galactic disk continuously migrate toward the Galactic center (GC) due to interactions with the bar potential, magnetic fields, stars, and other gaseous materials. In case of the Milky Way, those in forms of molecules appear to accumulate around 200 pc from the center (the central molecular zone, CMZ) to form stars there and further inside. The bar potential in the GC is thought to be responsible for such acculmulation of molecules and subsequent star formation, which is believed to have been continous throughout the lifetime of the Galaxy. We present 3-D hydrodynamic simulations of the CMZ that consider self-gravity, radiative cooling, and supernova feedback, and discuss the efficiency and role of the star formation in that region. We find that the gas accumulated in the CMZ by a bar potential of the inner bulge effectively turns into stars, supporting the idea that the stellar cusp inside the central 200 pc is a result of the sustained star formation in the CMZ. The obtained star formation rate in the CMZ, 0.03-0.1 Msun, is consistent with the recent estimate based on the mid-infrared observations by Yusef-Zadeh et al. We discuss the secular evolution of nuclear bulges in general, based on our results. -
We use three-dimensional hydrodynamic simulations to investigate nonlinear gravitational responses of gas to, and the resulting drag force on, a massive perturber moving on a circular orbit through a uniform gaseous medium. We assume that the background medium is non-rotating and adiabatic with index 5/3, and represent the perturber using a Plummer potential with softening radius a. This work extends our previous study where we showed that the drag force on a straight-line trajectory is proportional to a0.45 if the perturber is massive enough. This indicates that the orbital decay of supermassive black holes (SMBHs) near galaxy centers may take much longer than the prediction of the linear force formula applicable for low-mass perturbers. For the circular orbits are considered, however, we find that the nonlinear drag force becomes independent of a, but dependent instead on the orbital radius R as
$\varpropto$ R0.5. This suggests not only that the choices of large values of a, for resolution issues, in recent numerical experiments for mergers of SMBH, are marginally acceptable, but also that the gaseous drag indeed provides an efficient mean for the orbtial decay of SMBHs. -
We use three-dimensional hydrodynamic simulations to investigate the characteristics of turbulence driven in rotating, vertically-stratified disk. Our models are isothermal, and local in the in-plane direction while global in the vertical direction. We allow localized regions with density larger than the threshold value to explode and inject kinetic energy to the surrounding medium in the real space rather than Fourier space, mimicking supernova explosions thought to be the dominant turbulence source. This work extends our previous study where we studied turbulence in a non-rotating, uniform environment. We find that the galaxy rotation does not make a significant difference in the turbulence level at saturation, since the associated shear velocity is much smaller than the explosion velocity. We analyze the properties of turbulence in our models and compare them with those from the uniform-density models. We also discuss the astrophysical implication of our findings.
-
암흑에너지는 우주상수만으로 여러 우주론 관측 자료들을 잘 설명하고 있지만, 최근 SN Ia 자료가 축적됨에 따라 암흑에너지의 상태방정식 파라미터
$\omega$ 가 우주상수에서와 같이 -1인 상수인지, 시간에 따라 변하는지를 알아내기 위한 연구가 진행되고 있다. 본 연구에서는$\omega$ 가 시간에 따라 갑자기 변하는(sudden jump) transition-$\omega$ CDM 모형을 이용하여 SN Ia 자료를 Markov Chain Monte Carlo(MCMC) 방법을 통해 분석했다. Transition-$\omega$ CDM 모형에서는 상수인$\omega$ 의 값이 임의의 적색이동에서 변한다고 가정하였다. 분석에 사용된 SN Ia 데이터는 307개의 Union 자료와 90개의 CfA3 SN Ia가 추가된 Constitution 자료이며 개별적으로 분석됐다. 그 결과 transition 시기 전후$\omega$ 값들의 확률밀도분포를 얻어내었고, 이를 통해 SN Ia의 특성을 조사하였다. -
Suh, Hye-Won;Jeong, Hyun-Jin;Oh, Kyu-Seok;Yi, Suk-Young K.;Ferreras, Ignacio;Schawinski, Kevin 74.1
We have investigated the radial g-r color gradients of early-type galaxies in the Sloan Digital Sky Survey (SDSS) DR6 in the redshift range 0.00$H{\beta}$ absorption-line strengths and/or emission-line ratios that are indicative of the presence of young stellar populations. This implies that most of the residual star formation in early-type galaxies is centrally concentrated. Blue-cored galaxies are predominantly low-velocity dispersion systems. A simple model shows that the observed positive color gradients are visible only for a billion years after a star formation episode for the typical strength of recent star formation. The observed effective radius decreases and the mean surface brightness increases due to this centrally concentrated star formation episode. As a result, the majority of blue-cored galaxies may lie on different regions in the fundamental plane (FP) from red-cored ellipticals. However, the position of the blue-cored galaxies on the FP cannot be solely attributed to recent star formation but requires substantially lower velocity dispersion. We conclude that a low-level of residual star formation persists at the centers of most of low-mass early-type galaxies, whereas massive ones are mostly quiescent systems with metallicity-driven red cores. -
We present a multi-wavelength study of a supercluster in the NEP region at z=0.087, using AKARI (Infrared space telescope) NEP-Wide (5.8 deg2) survey which has obtained an unique IR imaging dataset with contiguous wavelength coverage from 2 to
$24{\mu}m$ , overcoming the Spitzer limitation of imaging capability at$10-20{\mu}m$ . The NEP-Wide survey is also covered in other wavelength such as X-ray, Radio, GALEX UV in the archive, optical (BRI from Maidanak 1.5m and CFHT's MegaPrime), and NIR imaging data (JH from KPNO 2.1m), with nearly 1900 optical spectra, mostly obtained by our group using MMT/Hectospec and WIYN/Hydra. Armed with the multiwavelength datasets, we investigate the connection between IR properties of galaxies and their environments as a tool to understand the evolution of galaxies in a supercluster environment. Specific attention will be given to MIR emission which can trace star formation activities and passive phases right after post-starbursts, and its relation to other wavelength data. -
The first near-infrared (NIR) spectroscopic survey of SDSS-selected blue early-type galaxies (BEGs) has been conducted using the AKARI/IRC. The NIR spectra of 36 BEGs are successfully secured, which are well balanced in their SF/Seyfert/LINER type composition. For high signal-to-noise ratio, we stack the BEG spectra all and in bins of several properties: color, specific star formation rate and optically-determined spectral type. We estimate the NIR continuum slope and the 3.3 micron PAH emission equivalent width in the stacked BEG spectra, and compare them with those of SSP model galaxies and known ULIRGs. We first report the NIR spectral features of BEGs and discuss the nature of BEGs based on the comparison with other objects.
-
We investigate the dependence of occurrence of bar in galaxies on galaxy properties and environment. The environmental conditions considered include the large-scale background density and distance to the nearest neighbor galaxy. We use a volume-limited sample of 33,296 galaxies brighter than
$M_r$ =-19.5+5logh at$0.02{\leqq}z{\leqq}0.05489$ , drawn from the Sloan Digital Sky Survey Data Release 7. We classify the galaxies into early and late types, and identify bars by visual inspection. We find that the fraction of barred galaxies ($f_{bar}$ ) is 18.2% on average in the case of late-type galaxies, and depends on both u-r color and central velocity dispersion$(\sigma);f_{bar}$ is a monotonically increasing function of u-r color, and has a maximum value at intermediate velocity dispersion (${\sigma}{\simeq}170km\;s^{-1}$ ). This trend suggests that bars are dominantly hosted by systems having intermediate-mass with no recent interaction or merger history. We also find that$f_{bar}$ does not directly depend on the large-scale background density as its dependence disappears when other physical parameters are fixed. We discover the bar fraction decreases as the separation to the nearest neighbor galaxy becomes smaller than 0.1 times the virial radius of the neighbor regardless of neighbor's morphology. These results imply that it is difficult for bars to be maintained during strong tidal interactions, and that the source for this phenomenon is gravitational and not hydrodynamical. -
With advancement of infrared space telescopes during the past decade, infrared wavelength regime has been a focal point to study various properties of galaxies, such as stellar mass, dust contents and dust-hidden star formation with respect to evolution of galaxies. Polycyclic Aromatic Hydrocarbons (PAHs) have emerged as one of the most important features since these features dominate mid-infrared spectra of galaxies. These PAH features provide a great handle to calibrate star formation rates and diagnose ionized states of grains. However, PAH
$3.3{\mu}m$ feature has not been studied as much as other PAH features since it is weaker than others and resides outside of Spitzer's capability. Still its calibration and characterization are important since it will be the only PAH feature accessible by JWST for high-z galaxies. AKARI mJy Unbiased Survey of Extragalactic Sources in 5MUSES (AMUSES) intends to take advantage of AKARI's capability of spectroscopy on 2 to 5${\mu}m$ to provide an unbiased library of 44 sample galaxies selected from a parent sample of 5MUSES, one of Spitzer legacy projects. For these 3.3mm flux limited sample galaxies whose redshifts range between 0 < z <1, AMUSES will calibrate PAH$3.3{\mu}m$ as a SFR while measuring ratios between PAH features and investigating Bra's potential as a SFR indicator. We present preliminary results of AMUSES. -
We report the extended far-ultraviolet (FUV) halo of NGC 891 above the galactic plane. The FUV intensity distribution is well described by two exponential components, one with the scale height of ~0.34 kpc and the other of ~2.3 kpc. The extraplanar FUV halo is traceable up to > 5 kpc. The FUV halo is attributable to scattered-off starlight by extraplanar dust. Using Monte-Carlo radiative transfer simulations, the FUV intensity distribution along the minor axis is found to be well modeled with two dust comonents. Its implications are discussed.
-
Extragalactic Research Highlights of AKARI - From Nearby Galaxies to Quasars in the Early Universe -I summarize highlights from extragalactic research activities performed with AKARI infrared space telescope. The main emphasis will be given to the works carried out by Korean astronomers. The activities span a wide range of topics, such as MIR properties of nearby galaxies in cluster environment, MIR diagnosis of star-forming galaxies at z=0 through z=2 in the North Ecliptic Pole (NEP) survey field, the Extended Groth Strip (EGS), and the First Look Survey (FLS) field, and the NIR spectroscopy of Luminous Infrared Galaxies (LIRGs) and Active Galactic Nuclei/Super-massive Black Holes at low redshift as well as near the re-ionization epoch of z~6. I describe FIR and MIR all sky data which can be used as a precious resource for extragalactic research, and other future and ongoing works with AKARI. These AKARI results will form a strong basis for future studies using other facilities, such as infrared surveys with UKIRT, FIR study of dusty universe with Herschel, and the SPICA mission.
-
A high redshift quasar is useful to investigate the early part of our universe. Since they are one of the brightest objects in the early universe, they can provide us with clues of the growth of super massive black holes and the early metal enrichment history. To discover the high redshift quasars, we designed a survey of wide area and moderate depth; Infrared Medium-deep Survey (IMS), a J-band imaging survey of ~200
$deg^2$ area where the multi-wavelength data sets exist. To obtain the J-band data, we are using the United Kingdom Infra-Red Telescope (UKIRT), and so far we have covered ~20$deg^2$ with Y- or J-bands over three observing runs during 2009. We used color-color diagrams of multi-wavelength bands including i, z, Y, J, K,$3.6{\mu}m$ and$4.5{\mu}m$ to select high redshift quasars. The major challenge in the selection is many M/L/T dwarfs, low redshift galaxies, and instrumental defects that can be mistaken as a high redshift quasar. We describe how such contaminating sources can be excluded by adopting multiple color-color diagrams and eye-ball inspections. So far, our selection reveals two quasar candidates at z~7. -
We present the initial results of rest-frame optical spectroscopy of quasars at 3 < z < 5 from the AKARI space telescope mission program QSONG (Quasar Spectroscopic Observation with NIR Grism). QSONG is an AKARI phase-3 mission program which utilizes the unique capability of spectroscopy at 2.5-5 microns, and is adequate for detecting redshifted Balmer lines. We focus on how to overcome the noise induced from instrumental degradation, and report our measurements of supermassive black hole (SMBH) masses with well calibrated optical mass estimators.
-
Ionization of hydrogen occurs globally in our universe. The epoch of this cosmic reionization may be probed by various observations, among which the 21cm observation of neutral hydrogen at high redshift is the most promising candidate. In order to provide a mock data, we have performed the first, self-consistent simulation of cosmic reionization. We account for all possible UV-radiating sources which reside in halos ranging from minihalos to atomically-cooling halos. In order to simulate the contribution from Pop III objects, we also calculate the radiative transfer of Lyman-Werner radiation and apply a suppression criterion for Pop III objects. Our priliminary result indicates that Pop III objects ionize the universe at very high redshift and create rich, small-scale bubble structure, while sources in atomically-cooling halos ionize the universe at relatively low redshift and create large-scale bubble structure. We discuss how these two different scales and epoch may be probed by future 21cm observations.
-
We present a detailed description of the blast-wave modeling technique for a very general class of GRB explosions. Providing a simple method of evaluating the blast energy, we demonstrate that a common approximation of pressure balance for the blast wave violates the energy-conservation law significantly for adiabatic blast waves. We show that the energy-violation problem is successfully resolved by the "mechanical model" that we developed. GRB afterglow lightcurves that are produced by the forward and reverse shock waves of the blast wave are presented.
-
The origin of galactic angular momentum is commonly explained as a result of tidal torques of neighbouring protogalaxies on the forming galactic halo. In this context, the environment plays a preponderant role establishing the total angular momentum of present day galaxies. For the last four decades, most of the observational studies focused their attention on the spatial orientation of galaxies in filaments, groups or clusters, leaving behind the magnitude of the angular momentum. We have implemented a simple model to account for the spin of disk galaxies that allow us to obtain an estimate for any galaxy requiring a minimum of information. Applying this method to a sample of galaxies extracted from the Sloan Digital Sky Survey, we have been studying angular momentum distributions of galaxies in different environments. In this talk I will present some results for galaxies immersed in different environments, spanning three orders of magnitude in environmental density, galaxies having nearby companions and clustered galaxies.
-
In the last meeting of KAS, we reported the first statistical study of Faraday rotation measure (RM) in the large-scale structure of the universe using the data of cosmological structure formation simulations. With a turbulence dynamo model for the intergalactic magnetic field (IGMF), we predicted that the root mean square of RM through filaments is \sim 1 rad/m^2. Future radio observatories such as the Square Kilometer Array (SKA) could detect this signal level. However, it is known that the typical foreground galactic RM is a few tens and less than ten rad/m^2 in the low and high galactic latitudes, respectively. So the RM in the large-scale structure could be detected only after the foreground galactic RM is removed. In this talk, we show how we remove the foreground galactic RM and what we obtain from the masked data, by using some noise models and masking techniques. Our results can be used to simulate future RM observations by SKA, and eventually to constrain the origin and evolution of the IGMF in the large-scale structure.
-
During the formation of cosmic web, collisionless shock waves are produced around and inside the substructures. In these shock waves electrons and ions are accelerated to such high energies that they can produce gamma rays in several ways. Many authors have studied the contribution of shock-induced radiation to the cosmic gamma-ray background. However not all the important physical processes are included in their calculation. By considering more complete physical process, we re-investigate the problem. In our model, the energy distribution of the cosmic rays (CRs) are calculated by widely accepted diffusive shock acceleration model, both primary and secondary CR electrons are included, both inverse Compton scattering and bremsstrahlung process are considered. The difference of the results are discussed.
-
Mun, Hong-Gyu;Chae, Jong-Cheol;Lee, Myeong-Hyeon;Lee, Hui-Won;Jeong, Hyeon-Su;Kim, Ung-Tae;Lee, Gyeong-Suk;Lee, Seo-Gu;Lee, Dong-Ju;Hong, Dae-Gil;Lee, Gang-Hwan;Kim, Cheon-Hwi;Min, Yeong-Cheol;Lee, Gyeong-Suk;Hyeon, Seong-Gyeong;Kim, Ji-Hye;Yun, Seon-Hye;Gang, Yeong-Un;Yang, Jong-Man;Park, Seok-Jae 84.1
2009 세계 천문의 해(International Year of Astronomy 2009, IYA2009) 한국조직위원회는 지난 1년간 148개 참가국의 일원으로 다양한 활동을 펼쳤다. IYA2009 활동은 강연, 별 축제와 같은 고전적인 이벤트로부터 시, 수필, 에세이, 음악, 미술, 만화, 영화, 대회, 인터넷 생중계, 플래시 동영상과 같이 새롭게 시도된 프로그램에 이르기까지 다양하게 기획, 운영되었다. 또한 우리는 시민천문대와 과학관, 미술관은 물론, 지하철, 기차역, 시청, 놀이공원, 쇼핑몰, 백화점, 병원, 그리고 경찰서에 이르기까지, 기존의 전통적인 전시공간을 벗어나 다양한 장소에서 전시회와 동영상 상영을 시도했다. 우리는 지난 1년간 90여 종의 행사를 410여 회에 걸쳐 진행했으며, 총 11,700,000여 명의 일반 시민과 학생들이 2009 세계 천문의 해에 참여한 것으로 추산하고 있다. IYA2009는 강연 200여 회, 전시 80여 회, 공연 15회, 학회 7회 등으로 요약할 수 있으며, 공식책자 4종, 도록 3종이 발간되었다. 관련 보도자료는 40 차례 배포했으며, 그 결과 2,500여 건이 언론을 통해 보도되었고, 총 248편의 연재기사가 실렸다. 2009 세계 천문의 해 한국조직위원회 공식 웹진 '이야진' 접속자는 999,890명, 총 페이지 뷰 건수는 131,963,473을 기록했다. -
현재 국내에는 약 30여 개의 천문관련 시설이 운영 중에 있으며 매년 2-3개의 시설이 추가로 건설 되고 있다. 대부분의 시설은 천체투영관과 천체망원경을 중심으로 건설, 운영되고 있지만 일부 천문관련 전시물을 포함하고 있는 곳들도 많이 있다. 하지만 천문관련 전시는 대부분 형식적인 설명패널이나 단순한 원리를 보여주는 전시물들로 이루어져 있어 실질적으로 천문교육에 활용되고 있는 곳은 거의 없는 실정이다. 본 연구에서는 현재 국내외 천문관련 시설에서 이루어지고 있는 전시물의 현황을 분석하고, 최신 연구 결과를 쉽게 전달하고 교육 효과를 높일 수 있는 새로운 형태의 전시물 개발 가능성에 대해 논의해 보고자 한다. 본 연구의 결과는 향후 국립과천과학관 및 국립대구 광주과학관의 천문관련 전시물 제작에 이용될 예정이다.
-
2010년 현재 국내에는 약 30여 개의 천체투영관(Planetarium)이 운영 중에 있으며 매년 2-3개의 천체투영관이 건설 되고 있다. 국내 다수의 천체교육시설은 천문학전공자가 아닌 비전문가들의 건설기획 운영으로 천체투영관의 근본적 역할과 기능을 다하고 있지 못한 실정이다. 천체투영관의 긍정적 운영과 교육적 활용을 높이기 위하여 1)현재 운영 중인 천체투영관의 운영실무자들에게 설문지를 배포하여 각 천체투영관 시설 현황과 운영 교육 프로그램을 조사하고, 2)설문조사 결과와 학년별 과학과 교육과정을 분석하여 천체투영관을 활용한 천문교육 프로그램을 개발하려 한다. 본 발표에서는 설문조사 결과와 교육프로그램 개발 계획에 대해 이야기 하고자 한다. 향후 개발된 교육프로그램은 국립과천과학관에서 시범운영하고 설문결과를 얻어 발표할 예정이다.
-
국립과천과학관은 2008년 11월에 개관하였고, 천체관측소에는 직경 1-m 반사망원경과 4k CCD카메라, UBVRI Filter system이 설치되어있다. 국립과천과학관 관측시스템의 시야는 28.16각분이고, CCD카메라는 Cryogenic 방식의 냉각으로
$-110^{\circ}C$ 정도로 냉각할 수 있다. 또한 CCD카메라는 4개의 증폭기(Amplifier)를 이용하여 읽기 시간을 줄일 수 있도록 설계되어 있다. 이 연구는 국립과천과학관 관측시스템을 과학적인 목적으로 사용하기 위해 기기적인 특성을 먼저 알아보기 위함이며 진행 중에 있다. 현재까지 관측한 자료를 바탕으로 시간에 따른 영점영상의 변화, 노출시간에 따른 암전류 영상의 변화, 증폭기 에 따른 영점영상의 차이 등을 분석하였다. -
2000년대 초에 일반인들을 위한 천문대인 대전, 영월, 김해에 시민천문대가 개관하던 당시 우리나라에는 시민천문대를 운영했던 전례가 없었다. 당시 시민천문대는 중소도시에서 지방과학관 사업의 일환으로 국비지원을 받아 건립하였기 때문에 입장료를 내고 관람을 하는 과학관 개념으로 운영되는 것이 자연스러웠다. 그러나 천체관측을 중심으로 진행하는 천문대는 운영자의 조작과 설명을 필요로 하기 때문에 단순히 전시물을 관람하는 기존의 과학관 운영과는 많은 차이가 있었다. 이러한 문제를 해결하기 위하여 2008년부터 김해천문대에서 관람중심의 운영을 탈피, 프로그램 중심의 운영을 시도하여 다양한 프로그램을 개발, 운영을 통해 많은 발전을 이루었다. 본 발표에서는 김해천문대에서 그동안 추진해 온 프로그램 중심으로의 운영 변화 과정과 그 결과를 보고하고 향후 발전시켜 나아갈 방향에 대해 소개할 예정이다.
-
한국천문연구원(이하 천문연)은 지식경제부에서 주관하고 행정안전부와 한국정보화 진흥원에서 시행한 '2009년도 지식정보화 사업'의 일환으로 우리나라 역서에 대한 데이터베이스를 구축하여 운영 중이다. 현재 1607년부터 2009년까지의 기간중 자료를 구할 수 있는 약 220년간의 역서에 대해 원문이미지와 텍스트(일부 연도 제외) 자료를 서비스 하고 있다. 본 연구에서는 시대별 한국에서 사용된 역법과 역서의 변천에 대해 간단히 언급하고, 역서 데이터베이스 구축과정에 대해서 소개하고자 한다. 그리고 현재 천문연에서 구축한 역서 데이터베이스 목록과 더불어 1830년 시헌력 역서를 예로 역서에 포함된 내용에 대해서도 간략히 소개 하고자 한다.
-
Main-belt comets (hereafter MBCs) are one of the hottest topics in the solar system astronomy. They are objects orbiting in the main asteroid belt which show cometary activity. Unlike most comets, which spend most of their orbit beyond 5AU from the Sun, MBCs follow near-circular orbits within the asteroid belt that are indistinguishable from the orbits of major population of the asteroids. P/2010 A2, the fifth MBC, was discovered by on January 6, 2010 by Lincoln Near-Earth Asteroid Research. It passed its perihelion at 2.01AU on December 3, 2009, about a month before it was discovered. With an aphelion of only 2.6 AU, P/2010 A2 spends all of its time inside of the frostline ~2.7 AU. We made observations of P/2010 A2 with Nishi-Harima Astronomical Observatory 2-m telescope only a week after the discovery. From the observed images, we found that the dust cloud was composed of large particles (>1mm) impulsively ejected between March and June, 2009. No coma was detected by our observations, suggesting that this object was no longer active. Consequently, we conjecture that these dust particles could be released by the impact collision among asteroids.
-
Near-Earth asteroid-comet transition object 4015 Wilson-Harrington is a possible target of the joint European Space Agency (ESA) and Japanese Aerospace Exploration Agency (JAXA) Marco Polo sample return mission. 4015 W-H was discovered showing cometary activity by Albert G. Wilson and Robert G. Harrington at Palomar Observatory in 1949. After recovered in 1979, 4015 W-H has been observed at every apparition, it always was seen as a point source. We made time series observations for 4015 W-H using the 1.8m telescope with 2K CCD at Bohyunsan Observatory, on the nights of 2009 November 17-19. The geocentric distance of 4015 H-W was about 0.38 AU at that time. No trace of cometary activity is seen from our images. From the light curve analysis, we find a double-peaked rotational period of 2.2 hours with amplitude of 0.4 magnitude. Our result is much shorter than previous measurements of 3.6 hours (Harris & Young 1983) and 6.1 hours (Osip et al 1995). We will discuss possible origin of the period variations.
-
2001년부터 목성, 토성, 타이탄을 관측하여 얻은 근적외선 고분산 분광선에 대한 자료들을 요약하고, 이들 데이터에서 도출된 연구 결과들을 정리하였다. 특히 3 마이크론 근처에서 혜성이나 성간물질 등에서 종종 나타나는 C-H stretching band와 비슷한 분광구조를 확인하였다. 이 분광구조는 행성계 물체의 연무나 구름 입자 속에 포함하고 있는 유기분자 때문이라고 유추된다. 이 파장 영역은 강한 대기 흡수 때문에 많은 관측자들이 기피하던 영역이었는데, 근래에 들어 고분산 분광기의 발달로 대기흡수선 사이를 통해 이들 천체들의 자세한 분광구조를 알 수 있게 되었다. 이번 발표에서 목성, 토성, 타이탄 분광 구조의 다른 점과 같은 점을 보여주고, 이 파장 영역에서만 도출할 수 있는 유용한 과학적 결과를 강조하고자 한다.
-
2006년 2월 7일, Gemini North Observatory의 Near-Infrared Integral Field Spectrometer (NIFS)를 사용해 타이탄의 K-band 분광영상을 얻었다. NIFS의 파장분해능은 R~5,000이었고, 타이탄 disk의 적도부분은 약 16 pixel로 분해되었다. 2.0 - 2.1 micron 영역에서 미지의 분광선이 관측됐는데, 그 분광 구조는 전형적인 slightly asymmetric-top molecule의 rotational-vibrational 밴드 구조와 유사하게 나타났다. 또한 N2-N2 Collision-Induced Absorption (CIA)과 H2-N2 dimer에 의한 흡수와 메탄(CH4)가스 흡수를 포함한 분광모델을 만들어 비교한 결과 이 파장영역에는 이러한 흡수선들의 영향이 적은 것으로 확인됐다. 따라서 해당 영역의 저분산 (R~2,000 - 3,400) 스펙트럼을 토대로 액체 또는 고체 상태의 탄화수소가 타이탄에 존재한다고 보는 최근 발표된 주장들은 (e.g., Brown et al. 2008, Nature, v. 454, p. 607; Adamkovics et al. 2009, Planetary and Space Science, v. 57, p. 1586) 보다 신중히 고려돼야 한다.
-
Cassini/VIMS 관측에 의하면 타이탄의 3 마이크론 파장영역에서 다른 파장 대와 달리 메탄 분자만으로는 관측 값에 맞는 모델을 만들기 힘든 특이한 형태의 흡수 밴드 영역이 발견되었다 (Bellucci et al. 2009, Icarus, v. 201, p. 198). 이 파장영역은 행성뿐만 아니라 ISM (Interstellar Medium)과 혜성 등에서 연구 되고 있는 C-H stretching band와 흡사한 구조를 가지고 있다. 이러한 구조는 타이탄 연무 속에 포함된 유기물질에 의한 것으로 추정된다. 본 연구는 최근까진 개발된 복사방정식 모델과 2006년 Cassini/VIMS가 관측한 고도에 따른 solar occultation 데이터를 비교하여 밴드구조의 실체를 알아보는 것이 주 목적이다. 우리는 고도 별로 다르게 나타나는 흡수밴드의 파장 영역을 세밀히 나눈 후 메탄과 함께 유기물질의 연무가 더해진 모델을 만들었다. 도출된 유기물질의 구조가 관측된 밴드 구조에 미치는 영향을 알아보고 앞으로의 연구 방향을 제시 할 것이다.
-
우리는 목성의 emission과 absorption 스펙트럼에 영향을 미치는 인자를 알아보고 목성의 대기구조를 연구하기 위하여 2006년 4월 18일부터 8월22일 사이 중 7일간 United Kingdom Infrared Telescope(UKIRT)의 고분산분광기 CGS4(R=37,000)를 이용하여 관측한 목성의
$2.86-3.53{\mu}m$ 분광관측 자료를 분석하였다. 관측자료의 분석에는$CH_4,\;CH_3D,\;NH_3,\;C_2H_2,\;C_2H_6,\;PH_3$ , HCN의 분광선 뿐만 아니라 구름과 Haze의 영향도 포함하는 대기모델을 사용하였다. 대부분의 관측된 분광선은 모델링을 통하여 얻은 synthetic spectrum과 일치하였으나 3.00 에서$3.10{\mu}m$ 사이에서 일치하지 않는 다섯 개의 미확인 분광선을 발견하였다. 이들은 각각$3.003{\mu}m$ 근처와 3.0505, 3.0735,$3.0865{\mu}m$ 그리고$3.0935{\mu}m$ 에서 나타나며, 미확인 분광선들이 Seo et al.(2007)이 언급한 태양의 적외선 흡수선에 의해서 나타나는 분광선이 아님을 보였다. 우리는 이 미확인 분광선들을 설명할 수 있는 가능한 분자들을 제시 하고자 한다. -
Hwang, Seong-Won;Han, Je-Hui;Sim, Chae-Gyeong;Kim, Sang-Jun;Jin, Ho;Im, Myeong-Sin;Kim, Gang-Min 90.1
우리는 Machholz 혜성(C/2004Q2)의 가시광선 영역 스펙트럼 (황성원 외, 2009, JASS, v. 26, p. 279)과 기존의 연구 문헌에 나오는 Austin, Swift-Tuttle, Brorsen-Metcalf 및 de Vico 혜성의 가시광선 영역 고분산 분광 자료와 비교 분석해 방출선의 파장 및 그 원인이 되는 물질을 확인했다. 그 결과 Machholz 혜성의 방출선은 대부분$C_2,\;NH_2,\;CN,\;H_2O^+$ 에 의한 것으로 나타났으며, 기존의 혜성 자료에서 알려지지 않은 미확인 방출선도 발견됐다. 또한, 주로 장파장 영역에서 나타나는 OH 방출선을 지구대기의 OH 방출선 자료와 비교 분석한 결과, Maccholz 혜성 고유의 OH일 가능성이 있는 방출선도 확인됐다. 본 연구에서 정리한 Machholz 혜성 및 다른 혜성들과의 비교 자료는 데이터베이스화하여 공개한다. -
Lunar sodium observations are being prepared by a group of WCU scientists at the Kyung-Hee Observatory. We have been working on 3-D Monte Carlo simulations of the lunar sodium exosphere since 2009, and we need to obtain additional sodium images in order to constrain our models. Using a newly-designed simple coronagraph which is optimized for lunar observations, we plan to make direct sodium image observations. We present the structure of the planned coronagraph, optical-image observation plans, and spectroscopic observation plans of the lunar tail. We will also present updated results from the 3-D Monte Carlo simulations.
-
Despite a surface dominated by carbon-based life, the bulk composition of the Earth is dramatically carbon poor when compared to the material available at formation. Bulk carbon deficiency extends into the asteroid belt representing a fossil record of the conditions under which planets are born. The initial steps of planet formation involve the growth of primitive sub-micron silicate and carbon grains in the Solar Nebula. We present a solution wherein primordial carbon grains are preferentially destroyed by oxygen atoms ignited by heating due to stellar accretion at radii < 5 AU. This solution can account for the bulk carbon deficiency in the Earth and meteorites, the compositional gradient within the asteroid belt, and for growing evidence for similar carbon deficiency in rocks surrounding other stars.
-
We present far-ultraviolet (FUV) observations of comet C/2001 Q4 (NEAT) obtained with Far-ultraviolet Imaging Spectrograph (FIMS, also called SPEAR) around perihelion between 8 and 15 May 2004. Several important emission lines, including S I (1425, 1474
${\AA}$ ), C I (1561, 1657${\AA}$ ), CO (1087.9, 1340-1680${\AA}$ ) were detected. Especially, the spectral features of CO are its electronic transitions belongings to the A-X, C-X systems. We also obtained radial profile of S I, C I, H I$Ly{\beta}$ with line fitting from central coma. The production rate of several spectral lines calculated from observed FUV photon flux. FUV spectral images of S I, C I, H I$Ly{\beta}$ emission lines were obtained.