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 38 Issue 1
-
Review briefly results of the solar and stellar chemical abundances from the high resolution spectroscopy and discuss the solar composition problem and puzzles of the astronomical spectroscopic results.
-
The high Antarctic plateau is the driest and coldest environment on the surface of the Earth and offers superlative conditions for the conduct of a wide range of astronomical observations, from optical to millimetre wavebands. This includes, especially, the infrared - where the sky background is greatly reduced from temperate sites - and the sub-millimetre / THz bands - where new or cleaner atmospheric windows can be viewed through. Astronomical observations have now been conducted from five locations on the Antarctic plateau - the South Pole, Domes A, C and F, and Ridge A. Ambitious plans for the construction of observatories there have been announced. An IAU Symposium on "Astrophysics from Antarctica" featured as part of last year's IAU General Assembly in Beijing. This talk will provide an overview of astronomy in Antarctica, describing the special conditions that make some forms of observation particularly favourable there, and discuss the development of observatories on the Antarctic plateau and the plans for their future development.
-
Development of bolometer array and camera at millimeter and submillimeter wavelengths plays an important role for detecting submillimeter galaxies (SMGs) which appear to be very bright at the submillimeter and millimeter wavelengths. These SMGs, luminous infrared galaxies detected at mm/submm wavelengths seem to be progenitors of present-day massive galaxies and account for their considerable contributions to the light from the early universe and their expected high star formation rates (SFRs) if there is a close link between the SMG phenomena and the star formation activities and the interstellar dust in galaxies is mainly heated by the star light. In this talk, we review assembly of SMGs compiled with observations using the bolometer arrays and cameras and investigate their spectral energy distribution fits including the data at other wavelengths which trace the photometric properties and the red-shift distribution of galaxies. We find that these bright SMGs significantly contribute to the cosmic star formation rate density at red-shifts of 2-3 (about 8 %) for the spatial distribution of these galaxies.
-
1990년대 중반 처음으로 행성이 발견되기 이전에는 우리의 행성에 대한 지식은 태양계에 존재하는 행성들에 국한되었다. 이후 행성 발견을 위해 여러 방법이 개발되고, 이어진 관측실험을 통해 행성 발견이 가히 폭발적으로 증가함으로써 외계 행성에 대한 연구는 천문학에서 가장 활발한 연구가 이루어지는 분야가 되었다. 한국 천문학계에서도 외계행성에 대한 연구가 지속적으로 행해져 오고 있다. 특히 중력렌즈 방법을 사용한 외계행성 검출 분야에서 많은 연구가 이루어지고 있다. 본 연설에서는 중력렌즈 현상을 이용하여 행성을 발견할 수 있는 원리, 관측실험, 발견된 행성, 과학적 중요성에 대해 발표한다. 그리고 2014년부터 시행할 대규모 관측실험에 대해서도 설명한다.
-
Chung, Jiwon;Rey, Soo-Chang;Sung, Eon-Chang;Yeom, Bum-Suk;Humphrey, Andrew;Yi, Wonhyeong;Kyeong, Jaemann 39
We present a study of correlations between the elemental abundances and galaxy morphologies of 91 blue compact galaxies (BCGs) at z=0.20-0.35 with Sloan Digital Sky Survey (SDSS) DR7 data. We classify the morphologies of the galaxies as either 'disturbed' or 'undisturbed', by visual inspection of the SDSS images, and using the Gini coefficient and M20. We derive oxygen and nitrogen abundances using the Te method. We find that a substantial fraction of BCGs with disturbed morphologies, indicative of merger remnants, show relatively high N/O and low O/H abundance ratios. The majority of the disturbed BCGs exhibit higher N/O values at a given O/H value compared to the morphologically undisturbed galaxies, implying more efficient nitrogen enrichment in disturbed BCGs. We detect Wolf-Rayet (WR) features in only a handful of the disturbed BCGs, which appears to contradict the idea that WR stars are responsible for high nitrogen abundance. Combining these results with Galaxy Evolution Explorer (GALEX) GR6 ultraviolet (UV) data, we find that the majority of the disturbed BCGs show systematically lower values of the$H{\alpha}$ to near-UV star formation rate ratio. The equivalent width of the$H{\beta}$ emission line is also systematically lower in the disturbed BCGs. Based on these results, we infer that disturbed BCGs have undergone star formation over relatively longer time scales, resulting in a more continuous enrichment of nitrogen. We suggest that this correlation between morphology and chemical abundances in BCGs is due to a difference in their recent star formation histories. -
We present a test of the emission statistics of active galactic nuclei (AGN), probing the connection between the red-noise temporal power spectra and multi-modal flux distributions known from observations. We simulate AGN lightcurves under the assumption of uniform stochastic emission processes for different power-law indices of their respective power spectra. For sufficiently shallow slopes (power-law indices beta
${\leq}$ 1.0), the flux distributions (histograms) of the resulting lightcurves are approximately Gaussian. For indices corresponding to steeper slopes (beta${\geq}$ 1.0), the flux distributions become multi-modal. This finding disagrees systematically with result of recent mm/radio observations. Accordingly, we conclude that the emission from AGN does not necessarily originate from uniform stochastic processes even if their power spectra suggest otherwise. Possible mechanisms include transitions between different activity states and/or the presence of multiple, spatially disconnected, emission regions. -
We present preliminary results of far-infrared(FIR) study of the supernova remnant(SNR)s in the Large Magellanic Cloud using the Herschel HERITAGE (HERschel Inventory of The Agents of Galaxy Evolution) data set. HERITAGE provides FIR data covering the entire LMC at 100,160, 250, 350, and 500 um. In order to confirm FIR emission associated with SNRs, we refer to Magellanic Cloud Emission-Line Survey (MCELS) H-alpha & SII data, Spitzer surveying the Agents of a Galaxy's Evolution (SAGE) Multiband Imaging Photometer (MIPS) 24um & 70um data, Chandra Supernova Remnants Catalog, and ATCA 4.8GHz continuum images of Dickel et al. (2005). Among 47 SNRs in the LMC, 7 SNRs show associated FIR emission. We present multi-wavelength view of 5 SNRs; DEM L249, N49, N63A, N132D, and the SNR in N4. N49 and N132D show morphological correlation in FIR and X-ray, suggesting that the FIR emission is from dust grains collisionally heated by X-ray emitting plasma. The FIR emission of N63A resembles H-alpha emission, which implies that the FIR line radiation could be dominant. The FIR images of the rest two objects, DEM L249 and SNR in N4, show no correlation to the other-waveband images.
-
Pyo, Jeonghyun;Kim, Il-Joong;Park, Won-Kee;Jeong, Woong-Seob;Lee, Dae-Hee;Moon, Bongkon;Park, Youngsik;Park, Sung-Joon;Park, Kwijong;Lee, Duk-Hang;Nam, Uk-won;Han, Wonyong 74
Multi-purpose Infra-Red Imaging System (MIRIS) is the main payload of the Science and Technology Satellite-3 (STSAT-3) to be launched in the late half of this year. For the Space Observation Camera (SOC) of MIRIS, we developed the data reduction pipeline with Python powered by Astropy, a community Python library for astronomy. The pipeline features the following functionalities: i) to retrieve the raw observation data from database and convert it to a FITS format, ii) to mask bad pixels, iii) to correct the non-linearity, iv) to differentiate the frames, v) to correct the flat-field, vi) to correct focal-plane distortion, vii) to improve the world coordinate system (WCS) information using known point-source catalog, and viii) to combine the sequentially taken frames. The pipeline is well modularized and has flexibility for later update. In this poster, we introduce the details of the pipeline's features and the future maintenance plan. -
We investigate the direct determination of expansion history using redshift distortions without plugging into detailed cosmological parameters. The observed spectra in redshift space include a mixture of information: fluctuations of density-density and velocity-velocity spectra, and distance measures of perpendicular and parallel components to the line of sight. Unfortunately it is hard to measure all the components simultaneously without any specific prior assumption. The degeneracy breaking, between the effect of cosmic distances and redshift distortions for example, depends on the prior we assume. An alternative approach is to utilize the cosmological principle inscribed in the heart of the Friedmann-Lematre-Robertson-Walker (hereafter FLRW) universe, that is, the specific relation between the angular diameter distance and the Hubble parameter, in this degeneracy breaking.
-
The presence of dark energy, suggested from Type Ia supernovae (SNe) cosmology, is the most pronounced astronomical discovery made during the past decade. The basic assumption of this discovery is that the look-back time evolution of SNe luminosity would be negligible after light-curve correction. Several recent works, however, show that there are some differences in Hubble residual among host galaxies having different morphology and mass, indicating that SNe luminosity might be affected by population age. In order to investigate this more directly, we are continuing the YONSEI (YOnsei Nearby Supernovae Evolution Investigation) project, where we are obtaining low-resolution spectra of some 60 nearby early-type host galaxies. The early-type galaxies are preferred because the mean population ages and metallicities can be estimated from the absorption lines, and they are less affected by dust extinction. In this talk, we will report our progress in determining the ages and metallicities of host galaxies to investigate their correlation with the Hubble residual.
-
Lee, Joon Hyeop;Kim, Minjin;Ree, Chang Hee;Kim, Sang Chul;Lee, Jong Chul;Lee, Hye-Ran;Jeong, Hyunjin;Seon, Kwang-Il;Kyeong, Jaemann;Oh, Kyuseok 30.1
The sizes of galaxies are known to be closely related with their masses, luminosities, redshifts and morphologies. However, when we fix these quantities and morphology, we still find large dispersions in the galaxy size distribution. We investigate the origin of these dispersions for red early-type galaxies, using two SDSS-based catalogs. We find that the sizes of faint galaxies (${\log}(M_{dyn}/M_{\odot})$ < 10.3 or$M_r$ >-19.5) are affected more significantly by luminosity, while the sizes of bright galaxies (${\log}(M_{dyn}/M_{\odot})$ > 11.4 or$M_r$ <-21.4) are by dynamical mass. At fixed mass and luminosity, the sizes of low-mass galaxies (${\log}(M_{dyn}/M_{\odot})$ ~ 10.45 and$M_r$ ~-19.8) are relatively less sensitive to their colors, color gradients and axis ratios. On the other hand, the sizes of intermediate-mass (${\log}(M_{dyn}/M_{\odot})$ ~ 10.85 and$M_r$ ~-20.4) and high-mass (${\log}(M_{dyn}/M_{\odot})$ ~ 11.25 and$M_r$ ~-21.0) galaxies significantly depend on those parameters, in the sense that larger red early-type galaxies have bluer colors, more negative color gradients (bluer outskirts) and smaller axis ratios. These results indicate that the sizes of intermediate- and high-mass red early-type galaxies are significantly affected by their recent minor mergers or rotations. Major dry mergers also may have influenced on the size growth of high-mass red early-type galaxies. -
The mean color of globular cluster (GCs) systems in early-type galaxies (ETGs) is, in general, bluer than the integrated color of field stars in their host galaxies. Recently, Goudfrooij & Kruijssen (2013) reported that even red GCs in the ETGs show bluer colors than their host field stars and suggested the different initial mass function (IMF) for red GCs and field stars to explain the observed offset in color. Here we suggest an alternative scenario that explains the observed color offsets between red GCs in ETGs and the field stars in the parent galaxies without invoking to the variation of the IMF. We find that the inclusion of second-generation (SG) helium-enhanced populations in the model fully explains the observed color offset between red GCs and field stars in the host galaxies. We have also tested the effect of the IMF slope on our models, but the effect is relatively small compared to the effect of the SG population. Our new model suggests that, in order to explain far-UV strong metal-rich GCs in M87 and the observed color offset between metal-rich GCs and the field stars in ETGs simultaneously, the inclusion of the SG populations with enhanced helium abundance is a more natural solution than the model that only adopted variations in the IMF.
-
Barred-spiral galaxies possess double patterns: a bar and spiral arms. While their angular speeds play an important role in governing gas dynamical evolution of barred spiral galaxies, there is no direct way to observe them. The Tremaine-Weinberg (TW) method has been one of the most reliable indirect methods to estimate pattern speeds, although it requires a few strict assumptions, notably one that the gas tracer is in a quasi-steady state. In barred-spiral galaxies, however, non-steady gas flows are significant especially when the double patterns have different angular speeds. Using numerical models, we explore the effect of non-steady gas motions on the determination of double pattern speeds based on the TW method. We find that the TW method is accurate within 15% when there is only a single pattern or when double patterns have the same angular speed. When double patterns have different speeds, on the other hand, neglecting the non-steady flows leads to quite large errors (> 30%) in the derived pattern speeds, and severely underestimate the real values for the viewing angle parallel to the bar minor axis. This suggests that one should be cautious when applying the TW method to galaxies with double patterns with different speeds.
-
We use grid-based hydrodynamic simulations to study star formation in nuclear rings in barred galaxies. The gaseous medium is assumed to be infinitesimally thin, isothermal, and unmagnetized. To investigate various situations, we vary the total gas content in the bar regions and the bar growth time. We find that star formation rate (SFR) in a nuclear ring is determined by the mass inflow rate to the ring rather than the total gas mass in the ring. The SFR shows a strong primary burst and weak secondary bursts at early time, and declines to small values at late time. The primary burst is caused by the rapid gas infall to the ring due to the bar growth, with its duration and peak depending on the bar growth time. The secondary bursts result from re-infall of the ejected gas by star formation feedback of the primary burst. When the SFR is low, ages of young star clusters exhibit an azimuthal gradient along the ring since star formation takes place mostly near the contact points between the dust lanes and the nuclear ring. When the SFR is large, on the other hand, star formation is widely distributed throughout the whole length of the ring, with no apparent age gradient of star clusters. Regardless of SFR, star clusters have a positive radial age gradient, with younger clusters located closer to the ring, since the ring shrinks in size over time.
-
We use numerical simulations to investigate the evolution of both the star formation rate (SFR) and the observable properties of equal-mass disk merger remnants for 18 different orbital configurations. In our analysis, the photometric properties of the remnants have been constructed by considering dust reddening effect in order to facilitate the comparison with observational data of large surveys such as the Sloan Digital Sky Survey (SDSS). First, we found that the detailed evolutions of merging galaxies are different between the merging characteristics such as merging time scale, SFR history, and burst efficiency. Around
$70{\pm}5$ percent of gas turns into stars until the merger-induced starburst ends regardless of merger types. Our study also suggests that merger features involve a small fraction of stars. Merger features last roughly 3 times the final coalescence time of galaxy mergers. For a shallower surface brightness limit, the features seem to survive in a shorter time, which is the reason why detecting merger features by using shallow surveys were difficult in the past. -
We examine large-scale environmental effects on the formation and the mass growth of dark matter halos. To facilitate this, we constructed dark matter halo merger trees from a cosmological N-body simulation, which enabled us to trace the merger information and the assembly history of individual halos. In fact, since the massive halos are more likely to be distributed in denser regions than in less dense regions (Mo & White, 1996), the large-scale environment dependence of the properties of halos can be partly originated from the halo mass effect. In order to avoid such contamination, caused by the mass dependence of halo properties, we carefully measured the local overdensity as the indicator of large-scale environment, which was calculated to be as independent of halo mass as possible. Small halos (
${\sim}10^{11-12}M_{\odot}$ ), which usually host isolated single galaxies, show a notable difference on the formation time of galaxies depending on their large-scale environments, which reconfirms halo assembly bias (Gao & White, 2007). Furthermore, we investigate how this environmental effect on small halos is correlated with the mass assembly history of galaxies by using our semi-analytic model. We found that assembly bias in small halos does not have significant effects on the formation time or on the star formation history of galaxies residing in those halos except for the individual stellar mass of galaxies at z = 0. On average, isolated galaxies in high-density regions tend to be slightly more massive than those in low-density regions. Although the observational data from the current galaxy surveys is not yet sufficient for testing this prediction, future galaxy surveys will be able to explore these small galaxies more thoroughly. -
The ISM properties under ICM pressure in the cluster environment: NGC4330, NGC4402, NGC4522, NGC4569Galaxies undergo various processes in the cluster environment, which could affect their evolution. In particular, ram pressure due to intracluster medium (ICM) can effectively remove HI gas, which is a relatively diffuse form of interstellar medium (ISM). On the other hand, molecular gas is not expected to get easily stripped as atomic gas since it is denser and sitting well within the stellar disk in a deeper potential well. However, cluster galaxies are found to be redder and more passive in star formation activity compared to their field counterpart. This implies that molecular gas may also get affected somehow in dense environments. In this work, we investigate molecular gas properties of a sample of galaxies undergoing HI stripping due to the ICM. We present the 12/13 CO (2-1) data of four spiral galaxies in the Virgo cluster at different ram pressure stripping stages, obtained using the Sub Millimeter Array (SMA). CO morphology of the sample appears to be highly asymmetric and disturbed. Using the ratio of different lines, we probe the molecular gas temperature in different regions. We find higher gas temperature than the range normally found among field galaxies. We discuss how these distinct molecular gas properties may affect star formation and hence the evolution of the cluster galaxy population.
-
We present 12CO (
$J=1{\rightarrow}0$ ) observations of a set of local galaxies (0.04 < z < 0.08) with a large cool gas reservoir, dubbed "HI Monsters". The data were obtained using the Redshift Search Receiver (RSR) on the Five College Radio Astronomy Observatory (FCRAO) 14 m telescope. The sample consists of 20 galaxies with$M_{HI}$ >$3{\times}10^{10}M_{\odot}$ identified by the ALFALFA survey and 8 additional objects with comparable HI mass from a separate LSB galaxy study ($M_{HI}$ >$1.5{\times}10^{10}M_{\odot}$ ). Our sample selection is purely based on the amount of neutral hydrogen in galaxies, thereby providing a chance to study how atomic and molecular gas relate to each other in these extremely HI-rich systems. We have detected CO in 15 out of 20 ALFALFA selected HI Monsters and 4 out of 8 LSB HI Monsters. We present the global molecular gas properties of the sample and discuss how their molecular gas properties correlate with their star formation activities. -
Seo, Hyun Jong;Matsumoto, Toshio;Jeong, Woong-Seob;Lee, Hyung Mok;Matsuura, Shuji;Matsuhara, Hideo;Oyabu, Shinki;Pyo, Jeonghyun;Wada, Takehiko 34.1
The first generation stars in the universe are not observed as discrete objects by using current observational facilities, but their contributions are redshifted to the near infrared wavelength bands at present universe. Therefore, investigation of background radiation at near infrared is important for the study of the first stars. In this study, we present new observations of spatial fluctuations in sky brightness toward the north ecliptic pole using data from AKARI. Among pointed observation program of AKARI, we used two pointing surveys named Monitor field and NEP wide field at three wavelength bands 2.4, 3.2, and 4.1${\mu}m$ . To obtain spatial fluctuations from observed images, first of all, we exclude pixels affected by resolved foreground objects and then obtain diffuse map which consists of diffused radiation only. Because the diffuse map contains not only cosmological components but also various foreground components, in order to detect cosmological components, we estimate the contributions of foreground components separately. The results of this study show that there remains excess spatial fluctuation that cannot be explained by known foreground sources. This work is based on observations with AKARI, a JAXA project with the participation of ESA. -
Spin distribution of dark matter halos in a cosmological N-body simulation is well fitted by a log-normal distribution, but the origin of the log-normal like shape is still unknown. To understand the evolution of spin and the origin of spin distribution, we have studied the change of the angular momentum of simulated halos through their merging histories. First, we traced merging histories of the dark matter halos and measured the probability distribution of the angular momentum changes from a series of simulations. We were able to fit the angular momentum changes with the Gaussian distribution in spaces of M, spin,
${\Delta}M$ . Using the simulated merging trees and the distribution of angular momentum changes during the merging events, we can recover the spin distribution of halos over the various mass scales. -
Seo, Hyun Jong;Matsumoto, Toshio;Jeong, Woong-Seob;Lee, Hyung Mok;Matsuura, Shuji;Matsuhara, Hideo;Oyabu, Shinki;Pyo, Jeonghyun;Wada, Takehiko 35.1
The first generation stars in the universe are not observed as discrete objects by using current observational facilities, but their contributions are redshifted to the near infrared wavelength bands at present universe. Therefore, investigation of background radiation at near infrared is important for the study of the first stars. In this study, we present new observations of spatial fluctuations in sky brightness toward the north ecliptic pole using data from AKARI. Among pointed observation program of AKARI, we used two pointing surveys named Monitor field and NEP wide field at three wavelength bands 2.4, 3.2, and 4.1${\mu}$ . To obtain spatial fluctuations from observed images, first of all, we exclude pixels affected by resolved foreground objects and then obtain diffuse map which consists of diffused radiation only. Because the diffuse map contains not only cosmological components but also various foreground components, in order to detect cosmological components, we estimate the contributions of foreground components separately. The results of this study show that there remains excess spatial fluctuation that cannot be explained by known foreground sources. This work is based on observations with AKARI, a JAXA project with the participation of ESA. -
초은하단을 구성하고 있는 은하단들의 분포를 통해 선형지수를 구하고 이를 이용하여 초은하단 규모에서 다양한 중력 모델을 검증한다.
-
I present a simple scheme for the treatment of gravitational interactions on galactic scales. In analogy with known mechanisms of quantum field theory, I assume ad hoc that gravitation is mediated by virtual exchange particles - gravitons - with very small but non-zero masses. The scheme predicts the asymptotic flattening of galactic rotation curves, the Tully-Fisher/Faber-Jackson relations, the mass discrepancy-acceleration relation of galaxies, and the surface brightness-acceleration relation of galaxies correctly; additional (dark) mass components are not required. The well-established empirical scaling laws of Modified Newtonian Dynamics follow naturally from the model. The scheme I present is not a consistent theory of gravitation; rather, it is a toy model providing a convenient scaling law that simplifies the description of gravity on galactic scales.
-
Jeong, Woong-Seob;Matsumoto, Toshio;Im, Myungshin;Lee, Hyung Mok;Lee, Jeong-Eun;Tsumura, Kohji;Tanaka, Masayuki;Shimonishi, Takashi;Lee, Dae-Hee;Pyo, Jeonghyun;Park, Sung-Joon;Moon, Bongkon;Park, Kwijong;Park, Youngsik;Han, Wonyong;Nam, Ukwon 36.2
The SPICA (SPace Infrared Telescope for Cosmology & Astrophysics) project is a next-generation infrared space telescope optimized for mid- and far-infrared observation with a cryogenically cooled 3m-class telescope. The focal plane instruments onboard SPICA will enable us to resolve many astronomical key issues from the formation and evolution of galaxies to the planetary formation. The FPC-S (Focal Plane Camera - Sciecne) is a near-infrared instrument proposed by Korea as an international collaboration. Owing to the capability of both low-resolution imaging spectroscopy and wide-band imaging with a field of view of$5^{\prime}{\times}5^{\prime}$ , it has large throughput as well as high sensitivity for diffuse light compared with JWST. In order to strengthen advantages of the FPC-S, we propose the studies of probing population III stars by the measurement of cosmic near-infrared background radiation and the star formation history at high redshift by the discoveries of active star-forming galaxies. In addition to the major scientific targets, to survey large area opens a new parameter space to investigate the deep Universe. The good survey capability in the parallel imaging mode allows us to study the rare, bright objects such as quasars, bright star-forming galaxies in the early Universe as a way to understand the formation of the first objects in the Universe, and ultra-cool brown dwarfs. Observations in the warm mission will give us a unique chance to detect high-z supernovae, ices in young stellar objects (YSOs) even with low mass, the$3.3{\mu}$ feature of shocked circumstance in supernova remnants. Here, we report the current status of SPICA/FPC project and its extragalactic sciences. -
We present a result of a statistical studies on nuclear activities of compact group galaxies. It is suggested that the galaxy interaction can trigger the nuclear activity by producing the gas inflow to the center of galaxies. To understand the connection between galaxy interaction and nuclear activity, we study the fraction of Active Galactic Nuclei (AGN) host galaxies in compact groups, known as the most favored environment for galaxy interaction. We select 59 spectroscopically confirmed compact groups in the SDSS DR6. Using the emission line ratio, we determine the spectral types of compact group galaxies and obtain the fraction of AGN-host galaxies. We compare this fraction with those in other galaxy environments. For the early type galaxies, we find that the AGN fraction of compact group galaxies are lower than field galaxies, but higher than cluster galaxies. On the other hand, the AGN fraction of compact group galaxies is similar to those for field and cluster environment for the late type galaxies. Implications of this result will be discussed.
-
We present the galaxy luminosity function (LF) of the Abell 119 cluster. Deep images in u, g, r bands were taken using MOSAIC 2 CCD on a Blanco 4-m telescope at CTIO. Based on scaling relations at faint magnitudes and spectroscopy at bright magnitudes, accurate membership of galaxies is determined. The LF is fitted by a single Schechter function and a two components (Gauss + Schechter) function. Blue galaxies are well fitted by a single Schechter function with steep slope
${\alpha}$ ~ -1.55). Red galaxies in the inner, high density region are fitted by single Schechter function with shallow slope (${\alpha}$ ~ -1.30), while red galaxies in the outer, low density region are well fitted by a two components function. The different slope of LFs between the inner and outer seems to stem from the luminosity segregation of A119 indicating larger number ratio of luminous to faint ratio towards the cluster center. The different shape of LFs seems to be resulted from the different composition of luminous and faint galaxies among main-cluster, sub-cluster, and infall region. -
We present observational estimation of the infrared (IR) luminosity function (LF) of local (z < 0.3) star-forming (SF) galaxies derived from the AKARI NEP-Wide samples. We made an analysis of the NEP-Wide data with optical spectroscopic information allowing an accurate determination of luminosity function. Spectroscopic redshifts for about 1650 objects were obtained with MMT/Hectospec and WIYN/Hydra, and the median redshifts is about 0.22. To measure the contribution of SF galaxies to the luminosity function, we excluded AGN sample by comparing their SEDs with various model template. Spectroscopic redshifts and the AKARI's continuous filter coverage in the mid-IR (MIR) wavelength (2 ~ 25 micron) enable us to avoid large uncertainties from the mid-IR SED of galaxies and corresponding k-corrections. The 8-micron luminosity function shows a good agreement with the previous works in the bright-end, whereas it seems not easy to constrain the faint-end slope. The comparison with the results of the NEP-Deep data (Goto et al. 2010) suggests the luminosity evolution to the higher redshifts, which is consistent with the down-sizing evolutionary pattern of galaxies.
-
Galaxy clusters, the largest gravitationally bound systems, are an important means to place constraints on cosmological models and study the evolution and formation of galaxies and their large scale distribution. We report results from our study of galaxy clusters in the European Large Area ISO Survey North1(ELAIS-N1) field, covering a sky area of 8.75
$deg^2$ . We combine multi-wavelength data from the UKIRT Infrared Deep Sky Survey Deep Extragalactic Survey (UKIDSS DXS, JK bands), Spitzer Wise-area InfraRed Extragalactic survey (SWIRE, Optical-Infrared bands), and CFHT (z band). The photometric redshifts are derived from these datasets and are used to search for high redshift galaxy cluster candidates. Finally, we provide new candidates of galaxy clusters at redshifts 1.0Kim, Myo Jin;Chung, Aeree;Lee, Joon Hyeop;Lim, Sungsoon;Kim, Minjin;Lee, Jong Chul;Ko, Jongwan;Yang, Soung-Chul 40.1
The HI ring serendipitously found in the Leo I galaxy group is unique in size in the Local Universe. It is ~200kpc in diameter with MHI~$1.67{\times}109M{\odot}$ , surrounding a pair of early type galaxies M105 and NGC 3384. Its origin is still under debate whether it is the remnant of formation of a galaxy group (primordial) or formed from stripped material during galaxy-galaxy interaction (tidal origin). Intriguingly a number of dwarf galaxies have been identified along the gas ring (with or without optical counterpart). Various properties of these dwarf galaxies such as dark matter content, color, and/or metallicity will allow us to pin down the origin of this large scale HI ring. We have obtained a mosaicked CFHT MegaCam image and the EVLA HI cube of the large scale gas ring. In this work we present optical and gas properties of dwarf galaxies identified in the CFHT data.Lee, Hye-Ran;Lee, Joon Hyeop;Kim, Minjin;Oh, Seulhee;Ree, Chang Hee;Jeong, Hyunjin;Kyeong, Jaemann;Kim, Sang Chul;Lee, Jong Chul;Ko, Jongwan;Park, Byeong-Gon;Sung, Eon-Chang;Sheen, Yun-Kyeong 40.2
The properties of bright galaxies are closely related to those of their nearby neighbors and satellite galaxies. In addition, the properties of galaxies in clusters are known to be strongly affected by the cluster environment. These two environmental effects raise a question: how significantly do nearby neighbors and satellite galaxies affect the properties of bright galaxies in a cluster? To address this issue, we reduce and analyze the deep and wide-field images of Abell 3659 (z ~ 0.0907) in the g' and r' bands obtained using IMACS on the Magellan (Baade) 6.5m telescope. The main goal of this study is to find out the relationship between the properties of bright galaxies and those of fainter companion galaxies in a cluster. This poster is a progress report, in which we present the sample selection and the preliminary results.우주 자기장의 기원은 잘 알려져 있지 않다. 크게 나누어서 우주론적인 기원과 천문학적인 기원을 고려할 수 있다. 자기장의 기원이 무엇이든지 간에, 난류는 씨앗자기장을 증폭시키는데 큰 역할을 한다. 본 발표에서는 천문학적인 기원을 가지는 씨앗자기장이 난류 내에서 어떻게 성장하는 지를 논의한다. 또한 과연 관측을 통해서 천문학적 기원과 우주론적 기원을 구분할 수 있는 지를 논의한다.We present the statistical properties of a volume-limited sample of 7,429 nearby (z = 0.033-0.044) galaxies from the Sloan Digital Sky Survey Data Release 7. By performing a visual inspection, we classified our sample galaxies according to the Hubble sequence (Hubble 1926, 1936). Then we excluded apparently smaller and flatter galaxies from our database because morphology classification on them turned out to be difficult. Our results cover structural (e.g. concentration index, color, magnitude, stellar mass, etc.), spectroscopic (e.g. velocity dispersion,$H{\beta}$ absorption line, Fe absorption line, Mg absorption line, accretion rate,$H{\alpha}$ emission line, etc.), and environmental (e.g. density, etc.) properties of each morphology type based on morphology distribution. For this analysis, we used the recent re-measurements of spectral line strengths by Oh and collaborators (2011). Our statistics confirm the up-to-date understanding on galaxy populations, e.g., correlations between morphology and line strengths and in turn derived ages and so on.Oh, Seulhee;Yi, Sukyoung K.;Sheen, Yun-Kyeong;Kyeong, Jaemann;Sung, Eon-Chang;Ho, Luis C.;Kim, Minjin;Park, Byeong-Gon 42.1
In the LCDM paradigm, hierarchical merging is thought to play a key role in the formation and evolution of massive galaxies. Theoretical and observational studies suggest that massive galaxies started forming at high redshifts and were assembled via numerous mergers. Galaxy clusters are the sites where the most massive galaxies are found and the most dramatic merger histories are embedded. The previous work of Sheen et al. (2012) identified via visual inspection many massive galaxies with merger features in clusters, which surprised the community. In this study we aim to quantify peculiarity of galaxies to pin down the merger frequency in cluster environments more objectively. We have performed optical deep imaging of 4 Abell clusters by using IMACS f/2 on a Magellan Badde 6.5-m telescope. For the galaxies in our data, we applied GALFIT algorithm, which fits analytic models to galaxy data, and we analyzed their residuals. We present the preliminary results of our sample galaxies.The F-GAMMA (FERMI-GST AGN Multi-frequency Monitoring Alliance) project is a program for the monthly monitoring of the broad-band spectra of currently about 90 selected Fermi-GST AGNs. F-GAMMA utilizes several facilities in cm, mm, sub-mm, infrared and optical bands, achieving an unprecedented coverage for the study of the spectral evolution of powerful relativistic jets in AGNs. The KVN joined the F-GAMMA project in May 2011, aiming to monitor flux density at 22 and 43 GHz. We present the preliminary results of flux density variability, evolution of spectral index, and modulation index.We present here the preliminary results of the fast variability of AGN radio light curves. The shortest time scale of minute in AGN light curves is needed to probe the AGN activity for a few reasons; First, to check if there is any kind of shortest time scale activity. Secondly, to find out what high frequency end of AGN spectra look like. For the last, to see the time delay at several wavelength bands and the change of the spectral index with time. The observation was conducted with three KVN(Korea VLBI Network) antennas with single dish cross scan mode. In order not to lose the target at any given time, whenever one station needs to observe the calibrator, the other station is on the target. Though the detailed data reduction is still going on, there might exist varying feature in the radio light curve. The more fine calibration will be done in near future and another good data set is ready for the reduction.The local environmental effects on the triggering of active galactic nucleus(AGN) activity has been studied with many authors, but there still be controversy. We perform statistical analysis for nearby(0.01 < z < 0.05) volume limited(Mr < -19) samples with visual inspection based on Sloan Digital Sky Survey Data Release7. We inspect ~60,000 galaxy images visually to find peculiar objects which show not only ongoing merging features and tidal features, but also post merging features like ring or shell structures. We found that these peculiar features were shown at least 2 times more frequently among AGN host galaxies than non AGN galaxies, and this trend was still visible when galaxy properties such as color or stellar mass are fixed. Furthermore, L[OIII] and L(Ha) of peculiar galaxies are found to be more increased than those of normal galaxies. In order to ensure this results, we also checked it for a smaller subsample with ~2mag deeper monochromatic images provided from SDSS Stripe82 database, and found consistent results. At last, we perform the same work for pair(r_p<80kpc/h, delta_v<200km/s) systems. Because of some pair systems which do not interact gravitationally in actuality but fulfill the criteria for identification of pair system, the trends are found to be slightly weaker. We also found that line luminosities are increased consistently as projected distance between central and companion galaxy decreased, and as companion color gets bluer. Overall, the results of this study tell us that the local environment of galaxies affect the frequency as well as the strength of AGN activity. Local environmental effects, however, may not be the dominant triggering mechanism for AGN activity since the majority of peculiar galaxies are non AGN galaxies.We present the preliminary results from 86 GHz GMVA observations on 2 AGN - 0954+658 and 0716+714. The observation was taken with the Global mm-VLBI Array in Oct. 2010, with dual polarization mode. The aim of the observation is to produce the polarization maps of the sources, with the Stokes parameters - I, Q, U and V. The final results will be used for estimating the strength of the intrinsic magnetic field and the geometries of AGN jets.We probe the feasibility of high-frequency radio observations of very rapid flux variations in compact active galactic nuclei (AGN). Our study assumes observations at 230 GHz with a small 6-meter class observatory, using the SNU Radio Astronomical Observatory (SRAO) as example. We find that 33 radio-bright sources are observable with signal-to-noise ratios larger than ten. We derive statistical detection limits via exhaustive Monte Carlo simulations assuming (a) periodic, and (b) episodic flaring flux variations on time-scales as small as tens of minutes. We conclude that a wide range of flux variations is observable. This makes high-frequency radio observations - even with small observatories - a powerful probe of AGN intra-day variability; especially, those observations complement observations at lower radio frequencies with larger observatories like the Korean VLBI Network (KVN).High velocity clouds (HVCs) are H I clouds that move with large speed (${\mid}V_{LSR}{\mid}$ >100 km/s) in the halo of the Milky Way. It is now evident that at least some populations of HVCs originated from extragalactic sources, either primordial gas left over from the galaxy formation or gaseous material stripped off from other galaxies closely passing by the Milky Way. HVCs with extragalactic origin play an important role in the star formation of the Milky Way when they eventually collide with the disk of the Milky Way. Although it is still observationally controversial whether HVCs are surrounded by dark matter or not, it is theoretically interesting to investigate the effect of dark matter on the collision of HVCs with the disk of the Milky Way. We model this scenario by using hydrodynamic simulations and search for proper parameters that explain the currently available observations such as the Smith Cloud that is thought to have collided with the Galactic disk already.The neutral component of the interstellar medium (ISM) is segregated into the cold neutral medium (CNM) and warm neutral medium (WNM) as a result of thermal instability. It was found that the CNM--WNM evaporation interface, across which the CNM undergoes thermal expansion, is linearly unstable to corrugational disturbances, in complete analogy with the Darrieus-Landau instability (DLI) in terrestrial flames. To explore dynamical consequences of the DLI in the ISM, we perform a linear stability analysis of the DLI including the effect of thermal conduction as well as nonlinear hydrodynamic simulations. We find that the DLI is suppressed at short length scales via heat transport. The linear growth time of the fastest growing mode is proportional to the square of the evaporation flow speed of the CNM relative to the interface and is typically >10 Myr. In the nonlinear stage, perturbations grow into cusp-like structure protruding toward the WNM, and soon reach a steady state where the evaporation rate is increased by a factor of 2 compared to the initial state. We demonstrate that the amplitude of the interface distortion and enhancement in evaporation rate are determined primarily by the density ratio between the CNM and WNM. Given quite a long growth time and highly subsonic velocities at saturation, the DLI is unlikely to play an important role in the ISM dynamics.Supersonic turbulence is believed to decay rapidly within a flow crossing time irrespective of the degree of magnetization. However, this consensus of decaying magnetohydrodynamic (MHD) turbulence relies on local isothermal simulations, which are unable to investigate the role of global magnetic fields and structures. Utilizing three-dimensional MHD simulations including interstellar cooling and heating, we investigate decaying MHD turbulence within cold neutral medium sheets embedded in warm neutral medium. Early evolution is consistent with previous studies characterized rapid decay of turbulence with the decaying time shorter than a flow crossing time and power-law temporal decay of turbulent kinetic energy with slope of -1. If initial magnetic fields are strong and perpendicular to the sheet, however long term evolutions of kinetic energy shows that a significant amount of turbulent energy still remains even after ten flow crossing times, and decaying rate is reduced as field strengths increase. We analyse power spectra of remaining turbulence to show that incompressible, in-plane motions dominate.We have performed a set of high-resolution simulations of nuclear star-forming ring that results in an inward gas migration from the galactic disk. Our simulations consider gas heating/cooling, star formation, and supernova feedback. The galactic potential was obtained from a snapshot of a 6.3 million particle simulation of a galactic disk at 1 Gyr, which manifests spiral arms and pseudo-bulge. The potential was modeled with a combination of 3-dimensional spherical (for the pseudo-bulge) and 2-dimensional cylindrical (for the disk) multipole expansion technique. With such a potential model, one can easily set up various realistic 3-dimensional potential models by slightly changing the expansion coefficients. We have performed a set of simulations with a few million gas particles covering the central ~6 kpc of the disk for different pseudo-bulge sizes and non-axisymmetry, and we report the dependence of the gas inflow rate, size of the star-forming ring, and star-formation rate in the ring on the size and strength of the non-axisymmetry in the bulge.It is known that the diffuse$H{\alpha}$ emission outside of bright H II regions not only are very extended, but also can occur in distinct patches or filaments far from H II regions, and the line ratios of [S II]${\lambda}6716/H{\alpha}$ and [N II]${\lambda}6583/H{\alpha}$ observed far from bright H II regions are generally higher than those in the H II regions. These observations have been regarded as evidence against the dust-scattering origin of the diffuse$H{\alpha}$ emission (including other optical lines), and the effect of dust scattering has been neglected in studies on the diffuse$H{\alpha}$ emission. However, as opposed to the previous contention, the expected dust-scattered$H{\alpha}$ halos surrounding H II regions are, in fact, in good agreement with the observed$H{\alpha}$ morphology. We find that the observed line ratios of [S II]/$H{\alpha}$ , [N II]/$H{\alpha}$ , and He I${\lambda}5876/H{\alpha}$ in the diffuse ISM accord well with the dust-scattered halos around H II regions, which are photoionized by late O- and/or early B-type stars. We also demonstrate that the$H{\alpha}$ absorption feature in the underlying continuum from the dust-scattered starlight ("diffuse galactic light") and unresolved stars is able to substantially increase the [S II]/$H{\alpha}$ and [N II]/$H{\alpha}$ line ratios in the diffuse ISM.We present the near-infrared spectra (2.5-5.0 um) of shocked$H_2$ gas, observed with the Infrared Camera onboard the satellite AKARI. Two supernova remnants, IC 443 and HB 21, were observed. IC 443 shows a hint of non-equilibrium ortho-to-para ratio (OPR): 2.4 (-0.2, +0.3). HB 21 also shows an indication of a potential non-equilibrium OPR: 1.8-2.0. These non-equilibrium OPRs are first reported for shocked$H_2$ gas at E(v,J) > 7000 K, as far as we are aware. We concluded that the non-equilibrium OPR probably originates from dissociative J-shocks, considering several factors such as the shock combination requirement, the line ratios, and the possibility that$H_2$ gas can form on grains with a non-equilibrium OPR. The difference in the collision energy of H atoms on grain surfaces would give rise to the observed difference between the OPRs of IC 443 and HB 21, if dissociative J-shocks are responsible for the$H_2$ emission. Our study suggests that shocked-then-cooled$H_2$ gas may play as a heat reservoir with the non-equilibrium OPR.We have been carrying out near-infrared (NIR) spectroscopy as well as [Fe II] narrow band imaging observations of Cassiopeia A supernova remnant (SNR). In this presentation, we describe the spectral classification of the iron knots around the SNR. From eight long-slit spectroscopic observations for the iron-bright shell, we identified a total of 61 iron knots making use of a clump-finding algorithm, and performed principal component analysis in an attempt to spectrally classify the iron knots. Three major components have emerged from the analysis; (1) Iron-rich, (2) Helium-rich, and (3) Sulfur-rich groups. The Helium-rich knots have low radial velocities (${\mid}v_r{\mid}$ < 100 km/s) and radiate strong He I and [Fe II] lines, that match well with Quasi-Stationary Flocculi (QSFs) of circumstellar medium, while the Sulfur-rich knots show strong lines of oxygen burning materials with large radial velocity up to +2000 km/s, which imply that they are supernova ejecta (i.e. Fast-Moving Knots). The Iron-rich knots have intermediate characteristics; large velocity with QSF-like spectra. We suggest that the Iron-rich knots are missing "pure" iron materials ejected from the inner most region of the progenitor and now encountering the reverse shock.Lee, Youngung;Kim, Youngsik;Yim, Insung;Kim, Bong-Gyu;Kang, Hyun-Woo;Jung, Jae-Hoon;Lee, Chang-Hoon;Kim, Kwang-Tae 49.2
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 target region is from l=$120^{\circ}$ to$133^{\circ}$ 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 140,000 spectra were obtained. The rms noise is about 0.18 K per channel for unsmoothed raw data. We will present a few initial results of the survey database.As part of the DIGIT key program, we observed GSS30-IRS1, a Class I object located in Ophiuchus (d=125 pc), with Herschel-PACS. More than 70 lines were detected: CO lines of$J=14{\rightarrow}13$ to$41{\rightarrow}40$ , several$H_2O$ lines of Eu=100 to 1500 K, 16 OH lines, and two atomic [OI] lines at 63 and 145${\mu}m$ . All lines, except for [OI], were detected only at the central spaxel of$9.4^{\prime\prime}{\times}9.4^{\prime\prime}$ while the [OI] emission is extended along the NE-SW direction. One interesting feature in GSS30-IRS1 is that the continuum is extended beyond PSF, unlike the line emission. For detail analysis, we apply the non-LTE LVG model, RADEX as well as simple rotational diagrams to the detected line fluxes. We will discuss about the physical conditions around GSS30-IRS1, learned by the line flux analysis.In the process of star formation, the density and temperature of associated material, which are the physical conditions for the molecular chemistry, vary dramatically. As a result, the connection between physical and chemical conditions has been used to trace the evolutionary stages in star formation. One chemical tracer for the physical conditions in star forming material is the [HCN]/[HNC] abundance ratio since the ratio strongly depends on the kinetic temperature in molecular clouds. Here we investigate the [HCN]/[HNC] abundance ratios in objects related to the massive star formation. For the investigation, we carried out$H^{13}CN$ and$HN^{13}C$ line observation toward objects in three different evolutionary stages of massive star formation: Infrared dark clouds (IRDCs), High-mass protostellar object (HMPOs), and Ultra-compact HII regions (UCHIIs). According to our observational results, both$H^{13}CN$ and$HN^{13}C$ lines have been detected toward 19 IRDCs, 25 HMPOs, and 31 UCHIIs. We will discuss about the [HCN]/[HNC] abundance ratios in different evolutionary stages of massive star formation and associate the results with the physical conditions of the targets.We present molecular line observations of a small group of Young Stellar Objects (YSOs), L1251C. Observations by Spitzer Space Telescope legacy program "From Molecular Cores to Planet Forming Disks"(c2d; Evans et al. 2003) revealed that there are three YSOs within ~15" in L1251C: IRS1 (Class I), IRS2 (Class II), and IRS3 (Class II). In order to understand the molecular environment around these YSOs, we carried out the KVN single-dish observations in$HCO^+$ J=1-0,$H^{13}CO^+$ J=1-0,$N_2H^+$ J=1-0 and HCN J=1-0. CO J=1-0 was also mapped in L1251C with the TRAO 14m telescope. Integrated intensity maps of high density tracers such as$H^{13}CO^+$ J=1-0,$N_2H^+$ J=1-0 and HCN J=1-0 show similar emission distributions, whose peaks are off from the positions of YSOs. However,$HCO^+$ J=1-0, which is believed to trace both infall and outflow, presents its emission distribution different from those of other molecular transitions. The line profile of$HCO^+$ J=1-0 is superimposed by two velocity (narrow and broad) components. The$HCO^+$ outflow map reveals multiple structures while the CO outflow map elongates mainly along the EW direction. With the KVN single dish, the 22 GHz$H_2O$ maser emission has been also monitored toward L1251C to find variations of the systemic velocity and intensity with time.We present observational results of CO outflows towards 24 embedded young stellar objects (YSOs), which are selected from the targets of the Herschel key program, "Dust, Ice, and Gas in Time" (DIGIT). Molecular outflow activity, which is believed to have strong dependence on accretion process, is the most powerful in the early embedded phase of star formation and declines as the central protostars evolve to the main sequence stage. In order to study the relation between the CO outflows observed in low J transitions and the properties of protostars, we mapped the CO outflows of the selected targets in J=1-0 and J=2-1 with the 14-m TRAO telescope and the 6-m SRAO telescope, respectively. We also compare the CO outflow momentum fluxes with the FIR molecular line luminosities of CO,$H_2O$ , OH, and OI, which were detected by the Herschel-PACS observations.Baek, Giseon;Pak, Soojong;Green, Joel D.;Jeon, Yiseul;Choi, Changsu;Lee, Jeong-Eun;Im, Myungshin;Meschiari, Stefano 52.1
We present preliminary results of the photometric variability analysis in SDSS r, i and z bands for a newly confirmed FU Orionis-type object, HBC 722. We observed HBC 722 from 2011 April to 2012 November, with Camera for Quasars in Early uNiverse (CQUEAN) attached to the 2.1m Otto Struve telescope at McDonald Observatory, USA. The rapid cadence monitoring observations (minute timescale) were conducted in chosen photometric nights during observation campaigns to get adequate number of samples for short term period analysis. As this object is in active state, temperature at the inner disk/stellar surface can be characterized by the colors between r, i and z bands. Also, It is theorized that a sudden cataclysmic accretion associated with FU Orionis-type outburst can give rise to detectable "hot spots" on the central star and rotational asymmetries in the disk instability region. Thus the periodic variabilities of three bands would trace the stellar rotation or Keplerian rotation at the instability region of the inner accretion disk. Additionally, the range of instabilities could be estimated on the assumption of a temperature distribution for the HBC 722 disk. This analysis can provide a clue for understanding enhanced disk accretion of Class II young stellar object.We compile a near-infrared photometric and polarimetric catalog for the$5{\times}9$ fields (${\sim}39^{\prime}{\times}69^{\prime}$ ) in the eastern side of the Large Magellanic Cloud (LMC). The photometric and the polarimetric data were obtained in J, H, and Ks bands using JHKs-simultaneous imaging polarimeter SIRPOL of the InfraRed Survey Facility (IRSF) in 2008 December and 2011 December. We estimate quality of the data using the method and the result from the IRSF Magellanic Clouds point source catalog which was published on 2007 June. In this poster, we present configuration of the catalog and the results of the verification.이 연구는 질량이 낮은 별탄생 지역에서 '에피소딕 질량수축 이론'을 관측과 수치모델로 테스트하였다. 스피쳐 우주망원경을 비롯한 여러 망원경으로 별 탄생 지역을 관측한 결과, 어린 별의 광도는 0.01 태양광도에 불과한 매우 낮은 값에서부터 높은 값까지 넓은 영역에 걸쳐 분포한다는 것이 알려졌다. 이 관측 결과는 70년대부터 있어 온 소위 표준 별탄생 모델의 예측과는 다른 결과이다. 관측과 표준 별탄생 모델의 차이를 풀기 위해서 에피소딕 질량수축 모델이 제안되었다. 테스트를 통하여 광도가 낮은 어린 별의 관측적 특성이 에피소딕 질량수축 모델로 한꺼번에 설명될 수 있음을 보였다. 우선, 카르마 전파 간섭계를 사용하여 전체 어린 별의 광도 분포에 해당하는 별 샘플을 선택하여 관측하였다. 표준 별탄생 모형은 중력수축이 진행됨에 따라 디스크 질량이 점진적으로 증가하지만 에피소딕 중력수축 모델은 디스크 질량과 별의 진화상태 사이에 특별한 연관관계가 없음을 예측한다. 여섯 개의 측정된 디스크 질량은 별의 진화상태와 상관없음을 보여주었다. 다음으로, 열아홉 개 어린 별의 이산화탄소 얼음을 적외선으로 분광 관측하고 분석하였다. 관측대상별 중 절반은 다른 분자와 섞이지 않은 순수한 이산화탄소 얼음이 존재한다는 증거를 보였고, 그 중 여섯 개는 순수 이산화탄소 얼음 존재의 강력한 증거인 두개의 픽이 나온 흡수선 형태를 보였다. 순수 이산화탄소 얼음 성분이 현재 광도가 낮은 별에서 존재한다는 것은 과거에 광도가 밝았던 시기, 즉 중력수축속도가 높았던 시기가 있었다는 것을 뒷받침한다. 화학진화모델에 에피소딕 중력수축 모델과, 일산화탄소 얼음이 이산화탄소 얼음으로 전환될 수 있다는 새로운 화학 네트워크를 포함한 모델로 광도가 낮은 어린 별에서의 순수 이산화탄소의 존재, 총 이산화탄소의 양, 그리고 관측된 일산화탄소 가스의 양을 모두 설명할 수 있었다.FUors are believed in the outburst phase of the episodic accretion model with accretion mass rates enhanced by 2-3 orders of magnitude compared to the normal classical T-Tauri stars. We have been monitoring HBC 722, which was brightened by ~5 mag in the V band in 2010 and thus became a new FUor, with BOES. We also observed two other FUors, FU Ori and V1057 Cyg with BOES. V1057 Cyg has been monitored in the optical spectroscopy for decades since its outburst. We present the results of our 2-year monitoring observations of HBC 722 in comparison with FU Ori and V1057 Cyg.We analyze the behaviors of reddening vectors in the Spitzer/IRAC photometric system for young stellar objects (YSOs) of different evolutionary stages, masses, and inclinations using the model spectral energy distributions (SED) by Robitaille et al. As reported in visible and near-infrared photometric systems, the magnitudes and colors of YSOs show strong SED dependence and non-linearity. In the [8.0] band where the 9.7${\mu}m$ interstellar silicate feature plays a significant role in extinction, the effective wavelength shifts "bluewards", not "redwards" as in most, if not all, optical and infrared bands including the other three IRAC bands, as the extinction in Ks increases up to ~2 mag, and then asymptotically reaches a constant value as the extinction further increases. This "bluening" is seen when the YSO is in later evolutionary stage and/or has a stellar mass of ~2$M_{\odot}$ or greater. In many cases, the reddening vectors in the IRAC color-color diagrams are prominently curved, and in some extreme cases, the colors involving the [8.0] band becomes bluer in the beginning and then becomes redder later as the amount of extinction increases. We also present our "suggested" extinction laws employing the combination of a broken-power law and the 9.7${\mu}m$ silicate feature, which well reproduce the extinction behaviors observed in the IRAC bands.We present the observational study of parsec-scale jets from YSOs reaching lengths of several arc-minutes. The medium-resolution spectroscopic data were obtained between 6000 -$7000{\AA}$ with BOAO long-slit spectrograph. By performing multi-position observation, we investigated the physical variation of the jets and the ambient gas along the whole path of the jets. The flux, electron density, ionization fraction, and electron temperature are discussed with the estimated line ratios between from [OI], [NII],$H{\alpha}$ and [SII] emission lines. This study carried out with more than 8 jets of YSOs including low- to intermediate-mass stars. We also briefly discuss the kinematics of the outflows using spatial and spectroscopic data.Hinse, Tobias C.;Han, Wonyong;Yoon, Joh-Na;Lee, Jae Woo;Lee, Chung-Uk;Park, Jang-Ho;Kim, Chun-Hwey 56.1
We have carried out follow-up observations of transiting extrasolar planets using small- to medium-sized reflectors located in Korea. Using the 0.60m telescope stationed at CbNUO (Chungbuk National University Observatory) we have achieved a photometric precision of 1.48 milli-magnitudes (root-mean-square scatter of data) of a HAT-P-09b (transit duration of 3.43 hrs) transit light curve (transit depth ~ 1.3%) with V=12.3 mag for the host star. We expect a photometric precision of 1.0 - 1.2 milli-magnitude for brighter targets (V ~ 10 - 11 mag). The transit technique and its application will be outlined. The results of test observations will be presented and the defocus technique will be discussed.Compact binaries are important sources of gravitational waves. They are also prime targets for long baseline laser interferometers. In this talk, we present latest progresses made in the Galactic merger rate calculations for compact binaries in the Galactic disk, with an emphasis on NS-NS binaries. For the first time, the non-recycled pulsar found in the Double Pulsar system (PSR J0737-3039B) is included in the rate calculation. We then discuss the prospects of detecting gravitational waves for Earth-based detectors such as advanced LIGO (Laser Interferometer Gravitational-wave Observatory) in US and advanced Virgo in Europe, extrapolating the Galactic rate estimates up to the detection volume of the advanced LIGO-Virgo network, Our results support the expectation that gravitational waves emitted from compact binary mergers will be detected within a decade. However, the detection rate of gravitational waves associated with NS-NS mergers is most likely to be several per year that is much smaller than what has been previously known.Non-LTE 항성대기모형인 Tlusty 모형의 합성색지수와 성간소광을 매우 적게 받은 산개성단에 있는 별들의 색지수를 바탕으로 O와 B형 별의 고유색지수 관계를 채택하였다. 태양인근 3kpc 내에 있는 약 190개 젊은 산개성단의 가시광 및 근적외선 2MASS JHKs 관측자료와 위에서 채택한 고유 색지수 관계를 적용하여 색 초과비 E(V-I)/E(B-V), E(V-J)/E(B-V), E(V-H)/E(B-V), 및 E(V-Ks)/E(B-V)를 얻고, 색 초과비와$R_V$ 의 관계를 사용하여, 각 성단의 성간소광법칙$R_V$ 를 결정하였다. 국부 나선팔의 백조자리 방향과 Per 나선팔에 있는 산개성단들은 약간 작은$R_V$ 를 보이며, 큰개자리 방향의 국부 나선팔에 있는 산개성단은 정상적인$R_V$ 를, 그리고 Sgr-Car 나선팔에 있는 산개성단들은 약간 큰 값을 보였다. 이 결과는 최대 편광도를 보이는 파장과$R_V$ 의 관계로 얻을 수 있는 양상과 잘 일치한다.Based on N-body simulations, we find out that significant fraction of dynamically formed BH-BH (10$M_{\odot}$ and NS-NS (1.4$M_{\odot$ ecah) binaries are ejected from globular clusters. About 30 percent of compact stars are ejected in the form of binary. The merging time of ejected binary depends on the velocity dispersion of globular cluster. Some of ejected binaries have merging time-scales shorter than Hubble time and are expected to produce gravitational waves that can be detectable by the advanced ground-based interferometers. The merger rates of ejected BH-BH and NS-NS binaries per globular cluster are estimated to be 3.5 and 17 per Gyr, respectively. Assuming the spatial density of globular clusters as 8.4$h^3$ clusters$Mpc^{-3}$ and extrapolating to the horizon distance of the advanced LIGO-Virgo network, we expect the detection rates solely attributed to BH-BH and NS-NS with cluster origin are to be 42 and 1.7$yr^{-1}$ , respectively. Besides, we find out that BH-NS binary ejection hardly occurs in globular clusters and dynamically formed compact binaries may possibly be the source of short GRBs whose locations are far from host galaxies.We present$10{\mu}m-35{\mu}m$ Spitzer spectra of the interstellar medium in the Central Molecular Zone (CMZ), the central 210 pc${\times}$ 60 pc of the Galactic center (GC). We present maps of the CMZ in ionic and$H_2$ emission, covering a more extensive area than earlier spectroscopic surveys in this region. The radial velocities and intensities of ionic lines and$H_2$ suggest that most of the$H_2$ 0-0 S(0) emission comes from gas along the line-of-sight, as found by previous work. We compare diagnostic line ratios measured in the Spitzer Infrared Nearby Galaxies Survey (SINGS) to our data. Previous work shows that forbidden line ratios can distinguish star-forming galaxies from LINERs and AGNs. Our GC line ratios agree with star-forming galaxies and not with LINERs or AGNs.We present a photometric study of the globular clusters (GCs) in the giant elliptical galaxy M86 in the Virgo Cluster, using the Washington$CT_1$ images taken at the KPNO 4 m telescope. The color distribution of the GCs in M86 is bimodal. The radial number density profile of the blue GCs decreases more slowly as the galactocentric distance increases than that of the red GCs. The density profile of the red GCs is similar to the surface brightness profile of M86 stellar halo. The blue GCs have a roughly circular spatial distribution, while the red GCs have a spatial distribution somewhat elongated, which is consistent with the distribution of the galaxy stellar light. M86 GCs have the negative radial color gradient because the number ratio of the blue GCs to the red GCs increases as galactocentric radius increases. The mean color of the red GCs is similar to that of the stellar halo. The bright blue GCs in the outer region of M86 reveal a blue tilt that the mean colors of the blue GCs get redder as they get brighter. We discuss these results in comparison with other giant elliptical galaxies in the Virgo Cluster.Yang, Yuna;Park, Won-Kee;Sung, Hyunil;Lee, Sanggak;Yoon, Tae-Seog;Lee, Jeongeun;Kang, Wonseok;Park, Keunhong;Cho, Dong-Hwan 59.1
HBC722 (also known as LkHa 188-G4 and PTF 10qpf; A. Miller et al., 2011) is one of the FU Orionis-like young stellar objects which outbursted in August 2010 (Semkov et al., 2010). We have been monitoring the post-outburst phase of this object since November 2010 with Korean Astronomy and Space Science Institute Near Infrared Camera System (KASINICS), at Bohyunsan Optical Astronomy Observatory (BOAO). Four filters, J, H, Ks, and H2 band, were used for this observation. We did aperture photometry to find photometric variation. The light curve shows a long period brightness change. After decrease of the brightness, which was reported at the KAS 2011 fall meeting, HBC722 brightens up slowly now. However we cannot confirm any short period variations, previously reported by Green et al (2013), due to large scatters in the obtained light curve.Wilson and Bappu found a tight correlation between the stellar absolute visual magnitude (MV) and the width of the Ca II K emission line for late-type stars in 1957. Here, we revisit the Wilson-Bappu relationship (hereafter, WBR) to claim that WBR can be an excellent indicator of stellar surface gravity of late-type stars as well as a distance indicator. We have measured the width (W) of the Ca II K emission line in high resolution spectra of 125 late-type stars, which were obtained with Bohyunsan Optical Echelle Spectrograph (BOES) and adopted from the UVES archive. Based on our measurement of the emission line width (W), we have obtained a WBR of$M_V=33.76-18.00{\log}W$ . In order to extend the WBR to be a surface gravity indicator, the stellar atmospheric parameters such as effective temperature ($T_{eff}$ ), surface gravity (logg), metallicity ([Fe/H]), and micro-turbulence (${\xi}_{tur}$ ) have been derived from the self-consistent detailed analysis using the Kurucz stellar atmospheric model and the abundance analysis code, MOOG. Using these stellar parameters and logW, we found that${\log}g=-5.85\;{\log}W+9.97\;{\log}T_{eff}-23.48$ for late-type stars.Numerous dust particles are scattered in the interplanetary space of the solar system (Interplanetary Dust Particles; IDPs). The origin of the IDPs is one of the major questions in the solar system astronomy because IDPs are being removed from the solar system within a few million years by photon drag. Comets and asteroids were pointed out as the possible sources of IDPs. Although several dust supplying mechanisms from comets and asteroids have been revealed, amount of contribution from each sources are still not clear. Zodiacal light is sunlight scattered by IDPs. Spectra of zodiacal light can supply important observational clue to reveal the origin of the IDPs, because comets and each type of asteroids have different kind of spectra. However, reflectance spectrum of zodiacal light was not measured at the wavelength of weak atmospheric contamination. We measured the reflectance spectra of zodiacal light from$5000{\AA}$ to$7000{\AA}$ . We used open data obtained by the Subaru/FOCAS instruments archived in the SMOKA database. From the longslit spectrum data, we measured spectrum of sky background and estimated flux from the sources other than the zodiacal light. We compared it with the spectra of each type of minor bodies in the solar system, and meteorites originated from these bodies.We investigate several eruptive hot plasma observations by Hinode/XRT. Their corresponding EUV and/or white light CME features are visible in some events. Using those observations, we determine the mass constraints of eruptive plasma by assuming simplified geometrical structures of the plasma. In some events, their associated prominence eruptions and eruptive plasma were observed in EUV observations as absorption or emission features. The absorption feature provides the lower limit to the cold mass while the emission feature provides the upper limit to the mass of observed eruptive plasma in X-ray and EUV passbands. We compare the mass constraints for each temperature responses and find that the mass in EUV and XRT are smaller in their upper or lower limit than total mass in coronagraph. About half eruptive events in XRT have no corresponding CME, which may be due to failed eruptions or low plasma density. In addition, some events were observed by a few passbands in X-ray, which allows the determination of the eruptive plasma temperature using a filter ratio method. We present the isothermal plasma temperatures by the filter ratio method. These are possibly an average temperature for higher temperature plasma because the XRT is more sensitive in higher temperature.In this study we apply Support Vector Machine (SVM) to the prediction of geo-effective halo coronal mass ejections (CMEs). The SVM, which is one of machine learning algorithms, is used for the purpose of classification and regression analysis. We use halo and partial halo CMEs from January 1996 to April 2010 in the SOHO/LASCO CME Catalog for training and prediction. And we also use their associated X-ray flare classes to identify front-side halo CMEs (stronger than B1 class), and the Dst index to determine geo-effective halo CMEs (stronger than -50 nT). The combinations of the speed and the angular width of CMEs, and their associated X-ray classes are used for input features of the SVM. We make an attempt to find the best model by using cross-validation which is processed by changing kernel functions of the SVM and their parameters. As a result we obtain statistical parameters for the best model by using the speed of CME and its associated X-ray flare class as input features of the SVM: Accuracy=0.66, PODy=0.76, PODn=0.49, FAR=0.72, Bias=1.06, CSI=0.59, TSS=0.25. The performance of the statistical parameters by applying the SVM is much better than those from the simple classifications based on constant classifiers.We study chromospheric oscillations including umbral flashes and running penumbral waves in a sunspot using scanning spectroscopy in H-alpha and Ca II 8542A, with the Fast Imaging Solar Spectrograph (FISS) at the 1.6 meter New Solar Telescope at Big Bear Solar Observatory. A bisector method is applied to spectral observations to construct chromospheric Doppler velocity maps. Temporal sequence analysis of these shows enhanced high-frequency oscillations inside the sunspot umbra in both lines. Their peak frequency gradually decreases outward from the umbra. The oscillation power is found to be associated with magnetic-field strength and inclination, with different relationships in different frequency bands.The Cassini/Visual Infrared Mapping Spectrometer (VIMS) observed the sun through the atmosphere of Titan, and provided vertically-resolved 63 spectra from 49 km to 987 km for the 1 - 5 micron range (Bellucci, 2008). Bellucci et al. (2009) analyzed selected spectral ranges where the band absorptions of$CH_4$ and CO are strong by constructing synthetic spectra including$CH_4$ and CO lines, but without including haze absorptions in their synthetic spectra. Kim et al. (2011) and Sim et al. (2013) were able to extract detailed spectral features of fundamental (Dv = 1) and overtone (Dv = 2) bands of the haze from the VIMS spectra by excluding the adjacent influences of strong$CH_4$ absorptions using a radiative transfer program, which includes effects of absorption and emission of lines of these molecules, and absorption and scattering of haze particles. In this presentation, we extend our detailed analyses to other remaining wavelengths in order to provide the spectral characteristics of the Titanian haze for the entire 1 - 5 micron range and to identify any additional haze spectral features and an unidentified feature near 4.3 microns reported by Bellucci et al. (2009).It is considered that comets near the ecliptic plane have been injected into inner solar system from Kuiper-belt. Some of them are still active while others are dormant with no detectable tails and comae. These dormant comets have eccentric and/or inclined orbits, which are parameterized by Tisserand parameter TJ<3. In addition, dormant comets can be differentiated from asteroids based on the albedo, because they have low albedo (the geometrical albedos pv<0.1). The conditions of TJ<3 and pv<0.1 have been used as a criteria to discriminate dormant comets from asteroids. However, we must be more careful because there are 'contaminations' from the outer region, i.e. Jovian Trojans (5.05To improve the forecast capability of geomagnetic storms, we consider the real time solar and near Earth conditions together, since the characteristics of CMEs can be modified during their transit from the Sun to the Earth, and the geomagnetic storms may be directly affected by not only solar events but also near Earth interplanetary conditions. Using 55 CME-Dst pairs associated with M- and X-class solar flares, which have clearly identifiable source regions during 1997 to 2003, we confirm that the peak values of negative magnetic field Bz and duskward electric field Ey prior to Dst minimum are strongly related with Dst index. We suggest the solar wind criteria (Bz<-5 nT or Ey>3 mV/m for t>2 hr) for moderate storm less than -50 nT by modifying the criteria for intense storms less than -100 nT proposed by Gonzalez and Tsurutani (GT, 1987). As the results, 90% (28/31) of the storms are correctly forecasted by our criteria. For 15 exceptional events that are incorrectly forecasted by only CME parameters, 12 cases (80%) can be properly forecasted by solar wind criteria. When we applying CME and solar wind conditions together, all geomagnetic storms (Dst<-50 nT) are correctly forecasted. Our results show that, the storm forecast capability of the 2~3 days advanced warning based on CME parameters can be improved by combining with the urgent warning based on the near Earth solar wind condition.We have investigated the EUV coronal jets observed by Solar Dynamic Observatory (SDO) / Atmospheric Imaging Assembly (AIA). From the Heliophysics Events Knowledgebase (HEK), we consider all recorded 40 EUV jets in$171{\AA}$ from May 2010 to July 2011 and use 19 jets whose location can be clearly identified, excluding limb events because of the ambiguity of their positions. According to the positions of their roots, these coronal jets are classified into two types: bright point jet (BPJ, 9 jets) and active region boundary jet (ABJ, 10 jets). BPJs are located at the top of bright points and ABJs at the boundaries of active regions. There are significant differences in speed and size between two types. Here the speed and size of a jet are assumed to be its maximum values in the case that the jet has several ejections. The average speed and size of 9 BPJs are about 110 km/s and 69,000km, respectively. The average speed and size of 10 ABJs are about 660 km/s and 194,000 km, respectively. The speed distribution of ABJs has two peaks at about 270 km/s and 1700 km/s. It is very interesting to note that three ABJs have very high speeds larger than 1600 km/s and they are all composed of a group of recurrent jets with low and high speed at the same location. In addition, we are investigating these events in other wavelengths and compare their characteristics.The point spread function (PSF) of an optical system is in general defined as a two-dimensional intensity distribution which results from a single point source at infinity. It is an important key for the evaluation of the optical performance of an astronomical telescope. The PSFs of the soft X-ray telescope (SXT) aboard Yohkoh were measured in a wide range of the field-of-view under the in-flight configuration at White Sands Missile Range prior to launching the satellite. It has been known that the SXT PSF has a sharp peak at the core and the intensity drops very fast as it goes distant from the center. Due to the combination of this sharp peak at the PSF core and the effect of undersampling by a large pixel size, a carefully designed method is requested in the examination of the PSF data. The pattern of the SXT PSF is determined by the fitting of a mathematical functional form to the pre-launch experimental data. The elliptical Moffat function has been adopted for the evaluation of the SXT PSF. It is revealed from our study that the SXT PSF shows a peculiar characteristics, and thus a careful consideration on the undersampling effect and also a proper choice of statistics are necessary for the determination of the best fit function of the PSF. Details on the on- and off-axis SXT PSF in the field-of-view will be introduced and discussed in our presentation.Bong, Su-Chan;Hwangbo, Jung-Eun;Park, Sung-Hong;Park, Jongyeob;Park, Young Deuk;Lee, Dae-Young 64.2
Korea Astnonomy and Space Science Institute (KASI) operates two solar radio observing facilities, the Korean station of the e-CALLISTO and the Korean Solar Radio Burst Locator (KSRBL). The e-CALLISTO station had suffered from tracking problem for past several years. Since 2011, KASI has developed a new tracking system, and recently the antenna has regained the its sun-tracking capability and full day-time coverage. The KSRBL also suffered from the control computer breakdown last year. After one year of operational gap, the KSRBL restored its normal daily observation. We also expanded the data server storage capacity, to store the full original data of 25 ms integration time and 0.25 MHz frequency resolution, amounting to about 80 GB per day.Hwangbo, Jung-Eun;Bong, Su-Chan;Lee, Jeongwoo;Lee, Dae-Young;Park, Seong-Hong;Park, Young-Deuk 65.1
The 2011 August 09 Flare is one of the largest X-ray flares of Sunspot Cycle 24 to attract a lot of attention for its various activities detected in coronal images. In this study we concern ourselves mostly on information of high energy electrons produced during this flare provided by hard X ray data from the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) and radio data from the Korean Solar Radio Burst Locator (KSRBL) and Ondrejov. EUV images obtained by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory are used to provide the context of magnetic reconnection. In our results, (1) HXR spectra have a rich spectral morphology. Initially it could be fit by one thermal component (T~30MK) and one single power law nonthermal spectrum, but later a better fit could be made by introducing an additional thermal component (T~55 MK). (2) Time delays between the KSRBL burst and the RHESSI hard X-ray emission were found which are more obvious at low frequencies and insignificant at high frequencies. (3) The HXR source lies in the core of the quadrupolar active region. In our interpretation based on AIA 94 A images, the outer part of the active region erupted to be blown out, leaving the intense hard X-ray emission concentrated in the core. We relate the appearance of the second thermal component to the evolution of the AIA 171 and 94 A images. The time delays of microwave peaks to HXR peaks are interpreted as indicating presence of trapped electrons in larger closed magnetic loops. With these result we conclude that the hard X ray and microwaves are due to impulsive acceleration in the low and high heights and a sigmoidal reconnection scenario.A presence of a penumbra is one of the main properties of a mature sunspot, and its formation mechanism has been elusive due to a lack of observations that fully cover the formation process. Utilizing the New Solar Telescope at the Big Bear Solar Observatory, we observed the formation of a partial penumbra for about 7 hours simultaneously at the photospheric (TiO;$7057{\AA}$ ) and the chromospheric ($H{\alpha}$ ,$-1{\AA}$ ) spectral lines with high spatial and temporal resolution. From this uninterrupted, long observational sequence, we found that flux emergence under the stable chromospheric canopy fields resulted in penumbra formation, while emerging flux under the expanding chromospheric fields appeared as transient elongated granules. Based on these findings, we suggest a possible scenario for penumbra formation in which a penumbra forms when the emerging flux is constrained from continuing to emerge, but rather is trapped at the photospheric level by the overlying chromospheric canopy fields.Six universities, four institutes and agencies, and two vendors are working for space weather in South Korea. Along with education and research activities, they have been extending ground-based observation system and upgrading space weather service, and participating in international space weather programs. Recently, several space missions for space weather have been proposed in accordance with the national space program of Korea. Here, we report and discuss the current status and future perspective of Korean community for space weather.In this study, we present a pore-selection technique to estimate the size of pore. The estimation of the size of pore is important to examine the temporal evolution of size itself and corresponding intensity. The size of pore is typically estimated by applying the intensity threshold technique to the fixed box which contains the entire pore. The typical method has disadvantages in the following circumstances; there are small features near the pore or the image has low spatial resolution. In the former, it is difficult to define a box containing the pore only, excluding the small features near the pore. In the latter, the background and threshold intensity are insignificant due to the insufficient number of pixel in the box. To avoid these difficulties, we use a pore-selection technique which is simply based on the measurement of distances from the pore center. In addition, we will discuss the advantage of the technique for the imaging spectrograph data like the NST FISS.The CFHT currently has three instruments running in QSO mode and one in Classical mode. I will touch on the capabilities of these instruments and give an update on the future instrumentation at CFHT. One new instrument, SITELLE, is scheduled to be delivered to CFHT at the end of the year. Another instrument which is a proof of concept is GRACES which should see first light during the summer. I will also give an update on the Dome Venting project and the Next generation CFHT.Park, Byeong-Gon;Seo, Yoon-Kyung;Yoon, Yang-Noh;Hwang, Narae;Kim, Young-Soo;Yuk, In-Soo;Lee, Jae-Joon 67.2
The GMT project is in its final stage of Design Development Phase in 2013, moving toward the Construction Phase planned to begin on Jan. 1st, 2014. In this contribution, we present the current status and progress of the GMT project including selection of the first generation instruments, development of primary mirror segments, site preparation, and science case revision along with plans for 2013 when the preparation of construction phase will be made.The K-GMT group launches a new science program designed to promote the observational research capabilities of Korean Astronomical Society. The science program (SP, hereafter) will provide the access to the observational facilities that is required for the completion of science proposals selected based on their scientific merits. The SP will invite the submission of proposals from all members of Korean Astronomical Society annually starting from mid-2013. We will introduce the rationale, action plan, and major timelines for the new K-GMT SP to the Korean astronomical community members.The Giant Magellan Telescope Integral-Field Spectrograph (GMTIFS) is a near-infrared imager and integral-field spectrograph, which will be the workhorse adaptive-optics (AO) instrument on the GMT when AO operations begin. We will describe the current design and proposed capabilities of the GMTIFS. We will also present a brief overview of GMTIFS science cases that include first-light objects, galaxy feedback and assembly, the nature of compact massive objects as well as the formation and evolution of stars and planets.We are developing Adaptive Optics (AO) system for 1m telescope at Gwacheon National Science Museum Observatory. The beam spot of the Gwacheon 1m telescope. The tip-tilt correction system consists of a CMOS sensor, a tip-tilt mirror and a feed back loop. The beam spot location at the CMOS sensor indicates the tip-tilt components of the incoming light. The tip-tilt mirror is controlled by DAC output voltage calculated by proportional-integral-derivative (PID) controller. This system successfully corrects the tip-tilt motion of the spot.The direct detection of gravitational wave has a very important meaning as a basis for verification of the theory of relativity. Several laser interferometer detectors have attempted to detect GW directly (e.g. LIGO, VIRGO), but positional accuracy of GW detector is too wide (about 10~100sq deg) to find which objects emit GW. One of the main sources of GW is gamma-ray burst which can be detected even in electromagnetic wave. Then to verify Gamma-ray burst object as a GW source, we proceed EM follow-up observation with wide field of view. A first program initiating EM follow-ups to possible transients GW events has been developed and exercised by LIGO and VIRGO community in association with several partners. Using QUEST optical data, we tested the method of cross-convolution recommended by EM follow-up community. We will describe the results of that test.Jeong, Woong-Seob;Lee, Dae Hee;Moon, Bongkon;Park, Kwijong;Park, Sung-Joon;Pyo, Jeonghyun;Park, Youngsik;Kim, Il-Joong;Park, Won-Kee;Kim, Mingyu;Lee, Duk-Hang;Nam, Ukwon;Han, Wonyong;Im, Myungshin;Lee, Hyung Mok;Lee, Jeong-Eun;Shin, Goo-Hwan;Chae, Jangsoo 70.1
New space program for "Next-Generation Small Satellite (NEXTSat)" launched last year after the success of the series of Science & Technology Satellite (STSAT). KASI proposed the near-infrared imaging spectrometer as a scientific payload onboard NEXTSat-1. It was selected as one of two scientific payloads. The approved scientific payload is the near-infrared imaging spectrometer for the study of star formation history (NISS). The efficient near-infrared observation can be performed in space by evading the atmospheric emission as well as other thermal noise. The observation of cosmic near-infrared background enables us to reveal the early Universe in an indirect way through the measurement of absolute brightness and spatial fluctuation. The detection of near-infrared spectral lines in nearby galaxies, cluster of galaxies and star forming regions give us less biased information on the star formation. In addition, the NISS will be expected to demonstrate our technologies related to the development of the Korea's leading near-infrared instrument for the future large infrared telescope, SPICA.O, Se-Jin;Yeom, Jae-Hwan;No, Deok-Gyu;O, Chung-Sik;Jeong, Jin-Seung;Jeong, Dong-Gyu;Atsushi, Miyazaki;Tomoaki, Oyama;Noriyuki, Kawaguchi;Hideyuki, Kobayashi;Katsunori, Shibata M. 70.2
한국천문연구원은 일본국립천문대와 한일공동으로 개발한 한일공동VLBI상관기(KJJVC)의 VLBI 관측자들에게 연구결과를 제공할 수 있는 정상운영을 2013년부터 수행하였다. 한일상관센터(KJCC)에서는 평균 8시간정도 관측한 VLBI 관측자료의 상관처리에 소요되는 시간은 약 2주 정도이며, 데이터 분석가의 확인을 거친 후 담당 PI에게 상관결과를 전달하고 있다. 현재 상관처리는 다양한 관측모드 중에서 연구관측에서 많은 비중으로 차지하고 있는 C5(16MHz 대역폭에 16stream) 모드를 지원하고 있으며, 2013년도에 여러 연구자들의 요구에 대응하기 위해 Wideband(512MHz 대역폭), C1(256MHz 대역폭, 1stream), C2(128MHz 대역폭, 2stream) 모드를 지원할 수 있도록 시스템의 성능을 개선할 예정이다. 또한 일본국립천문대에서는 자기테이프를 사용하고 있는 VERA 관측망에 대해 관측자료의 복사시간 단축, 운영효율을 향상시키기 위해 하드디스크를 채용한 OCTADISK 시스템을 개발하였으며, 한일상관센터에도 동기재생처리장치에 장착된 2대의 OCTADDB를 OCTADISK로 수정작업을 추진하였다. 본 보고에서는 이상에 기술한 것과 같이 한일상관센터의 운영현황과 향후 계획에 대해 자세히 기술한다.Park, Yeong-Sik;Park, Seon-Yeop;Im, Hong-Seo;Choe, Jin;Jo, Jung-Hyeon;Lee, Jeong-Ho;Jin, Ho;Bae, Yeong-Ho;Mun, Hong-Gyu;Choe, Yeong-Jun;Park, Jang-Hyeon 71.1
한국천문연구원은 우주물체 전자광학 감시체계 기술개발 사업을 통해 자국위성의 추적감시를 위해 0.5m 광시야 감시관측소 국제 네트워크(OWL : Optical Wide-Field patroL)를 구축할 예정이다. OWL 시스템의 설계 검증을 위해 시험모델을 개발하였고, 연구소 내에 테스트베드에 설치하여 종합적인 테스트를 수행하고 있다. 2012년 11월 상세설계 검토회의(CDR)를 수행하여 해외 설치할 서브시스템들의 설계를 확정 하였다. 현재 테스트 베드에서는 마운트와 컨트롤 시스템의 성능을 시험하기위해 10인치 RC 대체 경통으로 테스트 관측을 수행하였고, 3월에 납품한 proto-type 경통을 부착하여 시험관측 중에 있다. 시험 관측으로 획득한 영상들과 시스템의 개발 진행사항을 논의 하고자 한다.1 m 천체망원경에 대한 초기 광기계 구조해석이 진행되었다. 3개의 반사경으로 구성되는 광학계는 Richey-Cretien 방식으로써 두 개의 Nasmyth 초점을 제공하고, 초점비는 F/8이다. 결정된 반사경 마운트 방법에 의해 반사경면의 표면 RMS(Root Mean Square) 변형량은 모두 20 nm보다 작다. 전체 구조물에 대한 구조해석을 수행하기 위해 솔리드, 쉘, 빔 요소 등으로 구성된 정밀유한요소 모델이 NX 소프트웨어로 설계되었다. 전체 구조물은 첫 번째 고유모드는 68 Hz에서 병진모드가 발생했다. 중력에 대해서는 최대 응력이 18.2 MPa로써 미비하였고, 전체 최대 변위는 50.3${\mu}m$ 로써 계산되었다. 이 변위값은 광학설계 소프트웨어에 재입력되어 광학계의 성능이 재분석 될 것이다.Camera for QUasars in EArly uNiverse (CQUEAN) is an optical CCD camera, developed by Center for Exploration of Origin of the Universe (CEOU), which is now searching for high red shift quasar candidates. It has been operated since 2010, attached to the 2.1m Otto Struve telescope at the McDonald Observatory, USA. Based on the previous operation experiences, we present CQUEAN II system design which has a new filter wheel allowing with 20 narrow band filters. In addition, the auto guiding system will be rearranged and the interfacing units between the telescope and the instrument will become stabilized.Kim, Sanghyuk;Pak, Soojong;Chang, Seunghyuk;Kim, Geon Hee;Yang, Sun Choel;Lee, Sang Yong;Huh, Myung Sang;Im, Myungshin 72.2
An off-axis telescope has several advantages in optical performance comparing with a conventional on-axis telescope. However, in general, an off-axis telescope has a narrow field of view due to the linear astigmatism caused by the asymmetric structure. It was shown in the previous work that the linear astigmatism can be eliminated by properly configuring parameters in a confocal off-axis reflector system. Furthermore, the third order aberrations of a confocal off-axis telescope can be minimized by optimizing the shape of the mirrors. Despite many advantages, the confocal off-axis telescopes have been evaded because of difficulties of off-axis mirror fabrication, alignment process and unaccustomed off-axis baffle design. The baffle for the off-axis telescope should be designed considering that the effects of stray lights are different because of the asymmetry of off-axis system. In this poster, the design, manufacturing, and test for the baffle and housing of an off-axis telescope are presented.Gang, Yong-U;Song, Min-Gyu;Wi, Seok-O;Lee, Seong-Mo;Je, Do-Heung;Lee, Jeong-Won;Jeong, Mun-Hui;Gang, Ji-Man 73.1
전파자료처리를 위한 전파분광기는 전파망원경으로 얻어진 우주전파자료를 최종 처리하는 장비이다. 현재, 전파관측에서는 우주의 미세구조를 밝혀내기 위해 관측자료의 대량화와 고속화가 진행되고 있는데, 이러한 초고속 대용량 자료를 처리하기 위해서 FPGA나 ASIC 등으로 구성된 하드웨어 기반의 전파분광기를 주로 사용하고 있다. 그러나, 하드웨어 기반의 전파분광기는 개발에 시일이 많이 소요되고 고가이며 수정 변경이 쉽지 않다. 한편, 관측자료는 더 대량화되고 고속처리가 필요한 추세로 가고 있다. 이러한 한계를 극복할 수 있는 방법 중 하나가 고속 계산 플랫폼을 기반으로 구현되는 소프트웨어 전파분광기이다. 미국, EU, 일본 등은 이러한 전파분광기 개발을 이미 진행하고 있다. 특히, THz 대역에서 관측시스템 개발을 이제 막 시작하는 우리나라로서는 경쟁력을 갖추려면 외국의 기술의존성을 탈피하고 첨단의 초고속 관측자료처리 기술을 확보해야 한다. 이를 위해 국내의 우수한 IT기술을 전파관측기술에 활용하여 단계적으로 기술을 발전시킬 필요가 있다. 본 연구는 고속 계산 플랫폼을 기반으로 구현되는 소프트웨어 광대역 전파분광기의 기술개발에 관한 것으로 전파관측에 적용할 수 있는 x-엔진 개발과 기술 결합에 중점을 두고자 한다. 이에 소프트웨어 광대역 전파분광기의 기본 설계 및 향후 계획을 소개한다.Lee, Hye-in;Kang, Wonseok;Pak, Soojong;Kwon, Bong-Yong;Lee, Sungwon;Chun, Moo-Young;Jeong, Ueejeong;Yuk, In-Soo;Kim, Kangmin;Park, Chan 73.2
An autoguiding system for astronomical observations should be accurate and stable for efficient data taking. IGRINS (Immersion Grating Infrared Spectrograph) is a high resolution near-IR spectrograph which is now developed by Korea Astronomy and Space Science Institute and the University of Texas. We plan to attach this instrument on the 2.7m telescope at the McDonald observatory in 2013. IGRINS consists on three detector modules, i. e., H and K band spectrograph modules and a K band slit camera module. We use the slit camera for autoguiding of the telescope. In this poster, we describe the system architecture of the hardware and software of the autoguiding system, and the algorithm which would effectively find centers of stellar images on or outside of the slit of the infrared array.자체의 중력 효과를 고려하는 구대칭 완전 유체 전산모사 연구를 위해 일반상대론적 유체역학 코드를 이 분야 연구자들을 위한 공개용으로 개발하였다. 이 코드는 3+1 ADM(Arnowitt-Deser-Misner) 공식과 등방 공간 좌표를 사용하였다. 시공간 기하를 구하기 위해 극한값 썰기 (maximal slicing) 조건과 함께 세 개의 제한 방정식을 풀었고, 시공간을 채우는 물질인 유체는 근사 리만 해법을 사용한 HRSC (high resolution shock capturing) 기법으로 오일러 관찰자 시점에서 풀었다. 이 코드의 수렴성과 정확성을 검증하기 위해 상대론적인 구대칭 충격파 비교 분석, 블랙홀로 빨려 들어가는 상대론적 구대칭 강착, TOV(Tolman-Oppenheimer-Volkoff) 별 및 OS (Oppenheimer-Snyder) 붕괴 코드 테스트를 수행하였다. 특히, 이 코드의 동적 진화 테스트인 OS 붕괴의 경우 해석적인 해와 결과를 비교하기 위하여 좌표변환을 수치 계산으로 수행하였다. 아인슈타인의 일반상대성 이론을 넘어서는 변형된 중력이론 중 하나로 최근 제시된 EiBI(Eddington-inspired Born-Infeld) 이론에서 TOV 별의 해가 일반상대성 이론과 어떠한 차이를 보이는지 살펴 보았고, 그 이론에서도 물질이 붕괴하여 블랙홀을 만드는 경우 특이점이 형성되는지 고찰해 보았다.2008년 11월에 개관한 국립과천과학관은 매년 약 150만 명의 관람객이 방문하고 있으며, 천체투영관과 천체관측소에도 매년 20만 명 이상이 방문하고 있어 지금까지 방문한 총 누적 인원은 100만 명이 넘는다. 그리고 그동안 국립과천과학관에서는 일식, 월식, 유성우와 같은 특별한 천문현상 관측행사, 국제천체투영관영화제, 천체투영관 음악회와 과학 토크콘서트, 천문학 교실 등 다양한 천문 행사와 교육프로그램이 진행되어 천문학 대중화의 대표적인 기관으로 자리 잡았다. 하지만 점점 높아지고 있는 관람객들의 눈높이와 요구수준을 맞추기 위해서는 더욱 창의적이고 새로운 행사와 교육프로그램을 개발하여야 한다. 이것은 현재 천문시설을 운영하고 있거나 앞으로 운영할 계획인 다른 기관들도 모두 공통적으로 직면하고 있는 현실일 것이다. 이번 발표에서는 그동안의 국립과천과학관 천문시설의 운영 경험을 공유하고 향후 발전 방향을 함께 논의하는 기회를 가져보고자 한다.고대 천문기록을 연구하는 과정에서 기록의 사실 여부와 함께 천문기록에 영향을 미치는 요소를 확인하는 것은 중요하다. 본 연구에서는 고대의 천문기록 중에서 관측 빈도수가 높은 유성과 유성우 기록을 통해 이들의 분포와 역사적 환경 요소와의 관련성을 알아보았다. 유성과 유성우 기록을 분석한 선행연구에 의하면 한국과 중국 일본의 고대 유성과 유성우 기록은 잘 알려진 주기 유성우의 특성을 잘 보여준다. 그러나 인접한 세 나라의 관측 기록은 시대별로 일부 다른 분포를 보이는데 이러한 이유를 알아보기 위해 세 나라의 역사적 환경과 천문기록 분포와의 상관관계를 조사하였다. 본 연구에서는 1200년부터 1700년까지 500년 동안의 왕조-왕위교체, 외부침략, 내란과 같은 역사 사건을 조사하여 중요도에 따라 세 등급으로 나누고 이들을 유성과 유성우 기록 분포와 비교하였다. 연구 결과, 한국과 중국 일본의 고대 유성과 유성우의 기록 분포와 역사적 사건과는 서로 관련성이 없는 것으로 나타났다. 이것은 세 나라의 고대 천문관측 기록이 정치적 사건의 영향을 받지 않았음을 의미한다. 고대 천문기록을 분석할 경우 역사적 사건이나 왕위교체 등의 사회적 영향보다는 시대별 천문기록의 분포개수를 고려한 가중치가 중요하게 고려되어야 할 것이다.SPICA(SPace Infrared Telescope for Cosmology and Astrophysics) is an infrared space observatory with cooled telescope of 3 m aperture. Because of its large aperture, near- and mid-infrared instruments onboard SPICA require fine guidance with attitude accuracy less than 0.1 arcsecond. The FPC-G is a focal plane camera to achieve this high attitude accuracy and KASI is leading its development. The SPICA project is now under the Risk Mitigation Phase 2 (RMP2) and one of major risks is to satisfy the requirement of pointing and attitude control. To assess the impacts of disturbance sources on the attitude control and devise methods to mitigate possible risks, a software simulator of the FPC-G is under the development. In this presentation, we report the status of development of the simulator and the development plan during the RMP2.Kim, Jeong-Hwan;Ji, Ung-Bae;Yu, Tae-Hwa;Lee, Eun-Ji;Kim, Dong-Hyeon;Choe, Su-Hyeon;Bang, Jeong-Hun;Gang, Hyeok-Mo;Jang, Jang-Gun;Hong, Seung-Su;Jeong, Seo-Yeong;Lee, Ju-Heon;Gang, Hyeon-Jin;Yu, Da-In 77.1
WouldYouLike[우주:라이크]는 연세대학교 천문우주학과와 생활디자인과 학생들을 중심으로 천문우주학 대중화를 위해 활동하는 단체이다. 비영리 학생 단체인 만큼 학생들 스스로가 학습한 내용을 직접 요약하고 이를 바탕으로 일반 대중들이 쉽게 접하고 읽을 수 있는 천문우주학 콘텐츠를 제작하는 것을 목표로 하고 있다. 지난 해 봄 약 500여명의 연세대와 이화여대 학생들에게 시행한 관련 설문조사를 시작으로 6월과 12월에 약 30여 페이지 분량의 천문우주관련 소식을 담은 잡지를 발간하였다. 창간호 1300여부와 2호 550부는 연세대를 중심으로 주변 대학교에 배부되었으며 SNS를 이용한 온라인 버전도 약 1900여명의 사람들에게 공개되었다. 천문우주과학의 최신 소식을 전하고 천체사진을 찍는 방법을 소개하는 등 대중의 관심을 끌 내용부터 명왕성의 행성 직위 박탁, 천문대 탐방, IAU 탐방 등 다양한 관련 내용을 담았다. 현재는 3호를 제작중이며 4월말 발간을 목표로 하고 있다. 여기서는 지금까지의 활동 및 앞으로의 계획을 소개하고 천문우주학 전공자들의 의견을 받아 추후의 활동에 반영할 수 있도록 한다.xIn the present work, we explored the effect of the radiation on the effective impact parameter for capture in a fully general relativistic manner. To summarize our results, evidently due to the radiation drag (the Poynting-Robertson effect), critical impact parameter of point particle gets larger by the factor of two, thus, the effective cross section of the luminous relativistic star becomes 4 times larger than that of the star without radiation emission. In addition, the finite size effect of the star adds up to this growth of the effective cross section.
이메일무단수집거부
- 본 웹사이트에 게시된 이메일 주소가 전자우편 수집 프로그램이나 그 밖의 기술적 장치를 이용하여 무단으로 수집되는 것을 거부하며, 이를 위반시 정보통신망법에 의해 형사 처벌됨을 유념하시기 바랍니다.
- [게시일 2004년 10월 1일]
이용약관
-
제 1 장 총칙
- 제 1 조 (목적) 이 이용약관은 KoreaScience 홈페이지(이하 “당 사이트”)에서 제공하는 인터넷 서비스(이하 '서비스')의 가입조건 및 이용에 관한 제반 사항과 기타 필요한 사항을 구체적으로 규정함을 목적으로 합니다.
- 제 2 조 (용어의 정의) ① "이용자"라 함은 당 사이트에 접속하여 이 약관에 따라 당 사이트가 제공하는 서비스를 받는 회원 및 비회원을 말합니다. ② "회원"이라 함은 서비스를 이용하기 위하여 당 사이트에 개인정보를 제공하여 아이디(ID)와 비밀번호를 부여 받은 자를 말합니다. ③ "회원 아이디(ID)"라 함은 회원의 식별 및 서비스 이용을 위하여 자신이 선정한 문자 및 숫자의 조합을 말합니다. ④ "비밀번호(패스워드)"라 함은 회원이 자신의 비밀보호를 위하여 선정한 문자 및 숫자의 조합을 말합니다.
- 제 3 조 (이용약관의 효력 및 변경) ① 이 약관은 당 사이트에 게시하거나 기타의 방법으로 회원에게 공지함으로써 효력이 발생합니다. ② 당 사이트는 이 약관을 개정할 경우에 적용일자 및 개정사유를 명시하여 현행 약관과 함께 당 사이트의 초기화면에 그 적용일자 7일 이전부터 적용일자 전일까지 공지합니다. 다만, 회원에게 불리하게 약관내용을 변경하는 경우에는 최소한 30일 이상의 사전 유예기간을 두고 공지합니다. 이 경우 당 사이트는 개정 전 내용과 개정 후 내용을 명확하게 비교하여 이용자가 알기 쉽도록 표시합니다.
- 제 4 조(약관 외 준칙) ① 이 약관은 당 사이트가 제공하는 서비스에 관한 이용안내와 함께 적용됩니다. ② 이 약관에 명시되지 아니한 사항은 관계법령의 규정이 적용됩니다.
-
제 2 장 이용계약의 체결
- 제 5 조 (이용계약의 성립 등) ① 이용계약은 이용고객이 당 사이트가 정한 약관에 「동의합니다」를 선택하고, 당 사이트가 정한 온라인신청양식을 작성하여 서비스 이용을 신청한 후, 당 사이트가 이를 승낙함으로써 성립합니다. ② 제1항의 승낙은 당 사이트가 제공하는 과학기술정보검색, 맞춤정보, 서지정보 등 다른 서비스의 이용승낙을 포함합니다.
- 제 6 조 (회원가입) 서비스를 이용하고자 하는 고객은 당 사이트에서 정한 회원가입양식에 개인정보를 기재하여 가입을 하여야 합니다.
- 제 7 조 (개인정보의 보호 및 사용) 당 사이트는 관계법령이 정하는 바에 따라 회원 등록정보를 포함한 회원의 개인정보를 보호하기 위해 노력합니다. 회원 개인정보의 보호 및 사용에 대해서는 관련법령 및 당 사이트의 개인정보 보호정책이 적용됩니다.
- 제 8 조 (이용 신청의 승낙과 제한) ① 당 사이트는 제6조의 규정에 의한 이용신청고객에 대하여 서비스 이용을 승낙합니다. ② 당 사이트는 아래사항에 해당하는 경우에 대해서 승낙하지 아니 합니다. - 이용계약 신청서의 내용을 허위로 기재한 경우 - 기타 규정한 제반사항을 위반하며 신청하는 경우
- 제 9 조 (회원 ID 부여 및 변경 등) ① 당 사이트는 이용고객에 대하여 약관에 정하는 바에 따라 자신이 선정한 회원 ID를 부여합니다. ② 회원 ID는 원칙적으로 변경이 불가하며 부득이한 사유로 인하여 변경 하고자 하는 경우에는 해당 ID를 해지하고 재가입해야 합니다. ③ 기타 회원 개인정보 관리 및 변경 등에 관한 사항은 서비스별 안내에 정하는 바에 의합니다.
-
제 3 장 계약 당사자의 의무
- 제 10 조 (KISTI의 의무) ① 당 사이트는 이용고객이 희망한 서비스 제공 개시일에 특별한 사정이 없는 한 서비스를 이용할 수 있도록 하여야 합니다. ② 당 사이트는 개인정보 보호를 위해 보안시스템을 구축하며 개인정보 보호정책을 공시하고 준수합니다. ③ 당 사이트는 회원으로부터 제기되는 의견이나 불만이 정당하다고 객관적으로 인정될 경우에는 적절한 절차를 거쳐 즉시 처리하여야 합니다. 다만, 즉시 처리가 곤란한 경우는 회원에게 그 사유와 처리일정을 통보하여야 합니다.
- 제 11 조 (회원의 의무) ① 이용자는 회원가입 신청 또는 회원정보 변경 시 실명으로 모든 사항을 사실에 근거하여 작성하여야 하며, 허위 또는 타인의 정보를 등록할 경우 일체의 권리를 주장할 수 없습니다. ② 당 사이트가 관계법령 및 개인정보 보호정책에 의거하여 그 책임을 지는 경우를 제외하고 회원에게 부여된 ID의 비밀번호 관리소홀, 부정사용에 의하여 발생하는 모든 결과에 대한 책임은 회원에게 있습니다. ③ 회원은 당 사이트 및 제 3자의 지적 재산권을 침해해서는 안 됩니다.
-
제 4 장 서비스의 이용
- 제 12 조 (서비스 이용 시간) ① 서비스 이용은 당 사이트의 업무상 또는 기술상 특별한 지장이 없는 한 연중무휴, 1일 24시간 운영을 원칙으로 합니다. 단, 당 사이트는 시스템 정기점검, 증설 및 교체를 위해 당 사이트가 정한 날이나 시간에 서비스를 일시 중단할 수 있으며, 예정되어 있는 작업으로 인한 서비스 일시중단은 당 사이트 홈페이지를 통해 사전에 공지합니다. ② 당 사이트는 서비스를 특정범위로 분할하여 각 범위별로 이용가능시간을 별도로 지정할 수 있습니다. 다만 이 경우 그 내용을 공지합니다.
- 제 13 조 (홈페이지 저작권) ① NDSL에서 제공하는 모든 저작물의 저작권은 원저작자에게 있으며, KISTI는 복제/배포/전송권을 확보하고 있습니다. ② NDSL에서 제공하는 콘텐츠를 상업적 및 기타 영리목적으로 복제/배포/전송할 경우 사전에 KISTI의 허락을 받아야 합니다. ③ NDSL에서 제공하는 콘텐츠를 보도, 비평, 교육, 연구 등을 위하여 정당한 범위 안에서 공정한 관행에 합치되게 인용할 수 있습니다. ④ NDSL에서 제공하는 콘텐츠를 무단 복제, 전송, 배포 기타 저작권법에 위반되는 방법으로 이용할 경우 저작권법 제136조에 따라 5년 이하의 징역 또는 5천만 원 이하의 벌금에 처해질 수 있습니다.
- 제 14 조 (유료서비스) ① 당 사이트 및 협력기관이 정한 유료서비스(원문복사 등)는 별도로 정해진 바에 따르며, 변경사항은 시행 전에 당 사이트 홈페이지를 통하여 회원에게 공지합니다. ② 유료서비스를 이용하려는 회원은 정해진 요금체계에 따라 요금을 납부해야 합니다.
-
제 5 장 계약 해지 및 이용 제한
- 제 15 조 (계약 해지) 회원이 이용계약을 해지하고자 하는 때에는 [가입해지] 메뉴를 이용해 직접 해지해야 합니다.
- 제 16 조 (서비스 이용제한) ① 당 사이트는 회원이 서비스 이용내용에 있어서 본 약관 제 11조 내용을 위반하거나, 다음 각 호에 해당하는 경우 서비스 이용을 제한할 수 있습니다. - 2년 이상 서비스를 이용한 적이 없는 경우 - 기타 정상적인 서비스 운영에 방해가 될 경우 ② 상기 이용제한 규정에 따라 서비스를 이용하는 회원에게 서비스 이용에 대하여 별도 공지 없이 서비스 이용의 일시정지, 이용계약 해지 할 수 있습니다.
- 제 17 조 (전자우편주소 수집 금지) 회원은 전자우편주소 추출기 등을 이용하여 전자우편주소를 수집 또는 제3자에게 제공할 수 없습니다.
-
제 6 장 손해배상 및 기타사항
- 제 18 조 (손해배상) 당 사이트는 무료로 제공되는 서비스와 관련하여 회원에게 어떠한 손해가 발생하더라도 당 사이트가 고의 또는 과실로 인한 손해발생을 제외하고는 이에 대하여 책임을 부담하지 아니합니다.
- 제 19 조 (관할 법원) 서비스 이용으로 발생한 분쟁에 대해 소송이 제기되는 경우 민사 소송법상의 관할 법원에 제기합니다.
- [부 칙] 1. (시행일) 이 약관은 2016년 9월 5일부터 적용되며, 종전 약관은 본 약관으로 대체되며, 개정된 약관의 적용일 이전 가입자도 개정된 약관의 적용을 받습니다.