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 39 Issue 2
-
Magnetic fields appear to be ubiquitous in astrophysical environments. The existence of magnetic fields in the large-scale structure of the universe has been established through observations of Faraday rotation and synchrotron emission, as well as through recent gamma-ray observations. Yet, the nature and origin of the magnetic fields remains controversial and largely unknown. In this talk, I briefly summarize recent developments in our understanding of the nature and origin of magnetic fields. I also describe a plausible scenario for the origin of the magnetic fields; seed fields were created in the early universe and subsequently amplified during the formation of the large-scale structure of the universe. I then discuss the prospect of observation of magnetic fields in the large-scale structure of the universe.
-
Despite the great success that stellar evolution theory have enjoyed during the last 50 years, new challenges are emerging with recent observations of supernovae: many aspects of supernovae cannot be easily explained by the standard scenarios on supernova progenitors. A few examples include the red supergiant problem - the dearth of Type IIP supernova progenitors with masses higher than about 16 Msun, the non-detection of Type Ib/c supernova progenitors despite very deep searches in pre-supernova optical images, the unexpected blue colors of some Type IIn supernova progenitors, and the exotic stellar explosions of both ultra-faint and super-luminous types that have been only recently discovered. By confronting these observations with new stellar evolution models, we are making significnt progress in better understanding the role of metallicity, rotation and binary interactions for the pre-supernova evolution of massive stars. In this talk, I will give a brief review on the recent observational constraints on supernova progenitors and a progress report on several research projects that deal with pair-instability supernovae from the local Universe, type Ib/c supernovae from massive binary systems, and some peculiar stellar explosions like SN2012Z.
-
Studies of compact radio sources since the discovery of quasars have revealed a variety of physical properties: both in morphology and kinematics from sub-parsec to Mega-parsec scales, radiation mechanisms at frequencies from the radio to
${\gamma}$ -rays, theoretical models for relativistic jets, etc. The frontier discovery of Very Long Baseline Interferometry (VLBI) observations for the compact extragalactic radio sources have triggered the extensive studies to investigate the underlying physics of the relativistic jets. In this context, the highest resolution VLBI surveys of ultra-compact radio sources provide the potentially important statistical basis for future study. As a tool of this study, a new millimeter VLBI network in Korea, the Korean VLBI Network (KVN) will paly an important role. We present results from large VLBI surveys of compact radio sources at millimeter wavelengths and discuss the prospects with the KVN on this study. -
Through KASI, Korean astronomers will have access to the Gemini Observatory starting in 2015. Gemini operates two optical/infrared 8m-class telescopes: one on the northern hemisphere in Hawaii, one on the southern hemisphere in Chile. Both are equipped with state of the art instruments and adaptive optics systems that will be presented. Gemini also offers the opportunity for instrument development and welcomes visiting instruments. In terms of operations, Gemini offers to its partners three ways of applying for time: through semester-basis calls for standard programs, through yearly calls for Large and Long Programs, and through monthly calls for fast turnaround programs. Gemini operates in queue mode (observing for the principal investigators and allowing flexibility in the time domain), as well as in the classical visitor mode (where principal investigators come to the telescope). I will explain the requirements and advantages of all these modes as well as a full update on the Gemini Observatory.
-
Interactions such as mergers and flybys play a fundamental role in shaping galaxy morphology. We used the Horizon Run 4 cosmological N-body simulations to study the frequency and the type of halo interactions as a function of the environment, the separation p, the mass ratio q, and the target halo mass. We defined targets as haloes more massive than 10^11 Msun/h, and a target is interacting if it is located within the virial radius of a neighbour halo more massive than 0.4 times the target mass. We find that the interaction rate as a function of time has a universal shape for different halo mass and large-scale density, with an increase and saturation. Larger density yield steeper slopes and larger final interaction rates, while larger masses saturate later. Most interactions happen at large-scale density contrast
${\delta}$ about 10^3, regardless of the redshift. We also report the existence of two modes of interactions in the (p,q) plane, reflecting the nature (satellite or main halo) of the target halo. These two trends strongly evolve with redshift, target mass, and large-scale density. Interacting pairs have similar spins parameters and aligned spins, with radial trajectories, and prograde encounters for non-radial trajectories. The satellite trajectories become less and less radial as time proceed. This effect is stronger for higher-mass target, but independent of the large-scale density. -
Blue Compact Dwarf galaxies (BCDs) are low-mass galaxies with recently enhanced star formation activity. Since the discovery of old stellar population in the BCDs, a number of hypotheses have been suggested as the origin of the current active star formation. One theory is tidal interactions such as fly-by and merger. In this study we test this hypothesis using a pair of BCDs, ESO 435-IG20 and ESO 435-IG16 that are separate by only ~80 kpc in projection at a similar redshift (at a ~9 Mpc distance). In the HIPASS survey, intergalactic atomic hydrogen envelope has been found to be covering both galaxies, making the pair a good candidate for the case where the star formation has been triggered by tidal interaction. We probe the gas morphology and kinematics of the BCD pair using ATCA HI data in order to find the evidence of tidal interaction. We also estimate star formation rates in the pair based on Ha emission and UV continuum, and compare with other dwarf galaxies to investigate how responsible the tidal interaction is for the enhanced star formation in this case.
-
Kim, Suk;Rey, Soo-Chang;Jerjen, Helmut;Lisker, Thorsten;Sung, Eon-Chang;Lee, Youngdae;Chung, Jiwon;Pak, Mina;Yi, Wonhyeong;Lee, Woong 50
We present a new catalog of galaxies in the wider region of the Virgo cluster, based on the Sloan Digital Sky Survey (SDSS) Data Release 7. The Extended Virgo Cluster Catalog (EVCC) covers an area of 725 deg2 or 60.1 Mpc2. It is 5.2 times larger than the footprint of the classical Virgo Cluster Catalog (VCC) and reaches out to 3.5 times the virial radius of the Virgo cluster. We selected 1324 spectroscopically targeted galaxies with radial velocities less than 3000 km s-1. In addition, 265 galaxies that have been missed in the SDSS spectroscopic survey but have available redshifts in the NASA Extragalactic Database are also included. Our selection process secured a total of 1589 galaxies of which 676 galaxies are not included in the VCC. The certain and possible cluster members are defined by means of redshift comparison with a cluster infall model. We employed two independent and complementary galaxy classification schemes: the traditional morphological classification based on the visual inspection of optical images and a characterization of galaxies from their spectroscopic features. SDSS u, g, r, i, and z passband photometry of all EVCC galaxies was performed using Source Extractor. We compare the EVCC galaxies with the VCC in terms of morphology, spatial distribution, and luminosity function. The EVCC defines a comprehensive galaxy sample covering a wider range in galaxy density that is significantly different from the inner region of the Virgo cluster. It will be the foundation for forthcoming galaxy evolution studies in the extended Virgo cluster region, complementing ongoing and planned Virgo cluster surveys at various wavelengths. -
Lee, Hye-Ran;Lee, Joon Hyeop;Kim, Minjin;Ree, Chang Hee;Jeong, Hyunjin;Kyeong, Jaemann;Kim, Sang Chul;Lee, Jong Chul;Ko, Jongwan;Park, Byeong-Gon 52
It is widely accepted that the evolution of galaxies is accelerated in dense environments. According to recent studies, however, the evolution by direct interactions between galaxies is known to be most active in a galaxy group rather than in a galaxy cluster. In particular, the central galaxy in a group is closely related to its satellites in the properties such as morphology, color and star formation rate, because those galaxies evolve together in a small-scale environment. Currently, however, it is not yet studied well whether such conformity between bright galaxies and their faint companions remains after a galaxy group falls into a galaxy cluster. Recently, Lee et al. (2014) have found that the colors of bright galaxies show a measurable correlation with the mean colors of faint companions around them in WHL J085910.0+294957, a galaxy cluster at z = 0.3, which may be the vestige of infallen groups in the cluster. As a follow-up study, we study Abell 2744, an ongoing cluster-cluster merger at z = 0.308, using the HST Frontier Fields Survey data. The cluster members are selected based on the distributions of color, size and concentration along magnitude. The correlation in color between bright galaxies and their companions is not found in the full area of Abell 2744. However, when the area is limited to the southeastern part of the Abell 2744 image, the mean color of faint companions shows marginal dependence (>$2{\sigma}$ to Bootstrap uncertainties) on the color of their adjacent bright galaxy. We discuss the implication of these results, focusing on their dependence on local environments. -
We use dense redshift surveys of nine galaxy clusters at z ~ 0.2 to compare the galaxy distribution in each system with the projected matter distribution from weak lensing. By combining 2087 new MMT/Hectospec redshifts and the data in the literature, we construct spectroscopic samples within the region of weak-lensing maps of high (70-89%) and uniform completeness. With these dense redshift surveys, we construct galaxy number density maps using several galaxy subsamples. The shape of the main cluster concentration in the weak-lensing maps is similar to the global morphology of the number density maps based on cluster members alone, mainly dominated by red members. We cross correlate the galaxy number density maps with the weak-lensing maps. The cross correlation signal when we include foreground and background galaxies at 0.5zcl < z < 2 zcl is 10 - 23% larger than for cluster members alone at the cluster virial radius. The excess can be as high as 30% depending on the cluster. Cross correlating the galaxy number density and weak-lensing maps suggests that superimposed structures close to the cluster in redshift space contribute more significantly to the excess cross correlation signal than unrelated large-scale structure along the line of sight. Interestingly, the weak-lensing mass profiles are not well constrained for the clusters with the largest cross correlation signal excesses (>20% for A383, A689 and A750). The fractional excess in the cross correlation signal including foreground and background structures could be a useful proxy for assessing the reliability of weak-lensing cluster mass estimates.
-
One of the subjects in clouds' structure and development is small scale structure of interstellar cloud. The possibility of AU scale structure (Marscher et al. 1993; Moore & Marscher 1995; Roy et al. 2012) is discussed, and this small scale structure is considered as the result of hydrogen volume density (Moore & Marscher 1995), or small-scale chemical and other inhomogeneities (Liszt & Lucas 2000). In order to study this subject with emission line, extremely high resolution is mandatory by VLBI system. However, the alternative method could be observing the absorption line of interstellar cloud on the continuum object. In this case, the resolution would be restricted to the size of the continuum object, if the size of the object is smaller than the resolution of a used telescope. We observed the previous researchers' three objects (BLLAC, NRAO150, B0528+138), whose spectrums are changed from 1993 to 1998 (Liszt & Lucas 2000), with KVN. Through KVN observation, we found the changes of optical depth spectrum compared with the previous spectrums. We will discuss the optical depth spectrum variation by time variation and the meaning of it.
-
While the current consensus view holds that galaxy mergers are commonplace, it is sometimes speculated that Globular Clusters (GCs) may also have undergone merging events, possibly resulting in massive objects with a strong metallicity spread such as Omega Centauri. Galaxies are mostly far, unresolved systems whose mergers are most likely wet, resulting in observational as well as modeling difficulties, but GCs are resolved into stars that can be used as discrete dynamical tracers, and their mergers might have been dry, therefore easily simulated with an N-body code. It is however difficult to determine the observational parameters best suited to reveal a history of merging based on the positions and kinematics of GC stars, if evidence of merging is at all observable. To overcome this difficulty, we investigate the applicability of supervised and unsupervised machine learning to the automatic reconstruction of the dynamical history of a stellar system. In particular we test whether statistical clustering methods can classify simulated systems into monolithic versus merger products. We run direct N-body simulations of two identical King-model clusters undergoing a head-on collision resulting in a merged system, and other simulations of isolated King models with the same total number of particles as the merged system. After several relaxation times elapse, we extract a sample of snapshots of the sky-projected positions of particles from each simulation at different dynamical times, and we run a variety of clustering and classification algorithms to classify the snapshots into two subsets in a relevant feature space.
-
Park, Chan;Jaffe, Daniel T.;Yuk, In-Soo;Chun, Moo-Young;Pak, Soojong;Kim, Kang-Min;Pavel, Michael;Lee, Hanshin;Oh, Heeyoung;Jeong, Ueejeong;Sim, Chae Kyung;Lee, Hye-In;Le, Huynh Anh Nguyen;Strubhar, Joseph;Gully-Santiago, Michael;Oh, Jae Sok;Cha, Sang-Mok;Moon, Bongkon;Park, Kwijong;Brooks, Cynthia;Ko, Kyeongyeon;Han, Jeong-Yeol;Nah, Jakyuong;Hill, Peter C.;Lee, Sungho;Barnes, Stuart;Yu, Young Sam;Kaplan, Kyle;Mace, Gregory;Kim, Hwihyun;Lee, Jae-Joon;Hwang, Narae;Kang, Wonseok;Park, Byeong-Gon 90
The Immersion Grating Infrared Spectrometer (IGRINS) is the first astronomical spectrograph that uses a silicon immersion grating as its dispersive element. IGRINS fully covers the H and K band atmospheric transmission windows in a single exposure. It is a compact high-resolution cross-dispersion spectrometer whose resolving power R is 40,000. An individual volume phase holographic grating serves as a secondary dispersing element for each of the H and K spectrograph arms. On the 2.7m Harlan J. Smith telescope at the McDonald Observatory, the slit size is$1^{{\prime}{\prime}}{\times}15^{{\prime}{\prime}}$ . IGRINS has a plate scale of 0.27" pixel-1 on a$2048{\times}2048$ pixel Teledyne Scientific & Imaging HAWAII-2RG detector with a SIDECAR ASIC cryogenic controller. The instrument includes four subsystems; a calibration unit, an input relay optics module, a slit-viewing camera, and nearly identical H and K spectrograph modules. The use of a silicon immersion grating and a compact white pupil design allows the spectrograph collimated beam size to be 25mm, which permits the entire cryogenic system to be contained in a moderately sized ($0.96m{\times}0.6m{\times}0.38m$ ) rectangular Dewar. The fabrication and assembly of the optical and mechanical components were completed in 2013. From January to July of this year, we completed the system optical alignment and carried out commissioning observations on three runs to improve the efficiency of the instrument software and hardware. We describe the major design characteristics of the instrument including the system requirements and the technical strategy to meet them. We also present the instrumental performance test results derived from the commissioning runs at the McDonald Observatory. -
The mass measurement of neutron stars or black holes is of fundamental importance in our understanding of the evolution of massive stars and core-collapse supernova explosions as well as some exotic physics of the extreme conditions. Despite the importance, however, it's very difficult to measure mass of these objects directly. One way to do this, if they are in binary systems, to measure their binary motions (i.e., Doppler shifts) which can give us direct information on their mass. Recently many new highly-obscured massive X-ray binaries have been discovered by new hard X-ray satellites such as INTEGRAL and NuSTAR. The new highly-obscured massive X-ray binaries are faint in the optical, but bright in the infrared with many emission lines. Based on the near-infrared spectroscopy, one can first understand the nature of stellar companions to the compact objects, determining its spectral types and luminosity classes as well as mass losses and conditions of (potential) circumstellar material. Next, spectroscopic monitoring of these objects can be used to estimate the mass of compact objects via measuring the Doppler shifts of the lines. For the former, broad-band spectroscopy is essential; for the latter, high-resolution spectroscopy is critical. Therefore, IGRINS appears to be an ideal instrument to study them. An IGRINS survey of these new highly-obscured massive X-ray binaries can give us a rare opportunity to carry out population analyses for understanding the evolution of massive binary systems and formation of compact objects and their mass ranges. In this talk, we will present a sample near-infrared high resolution spectra of HMXB, IGR J19140+0951 and discuss about its spectral feature. These spectra are obtained on 13th July, 2014 from IGRINS commissioning run at McDonald 2.7m telescope. And at final, we will introduce the upgrade plan of IGRINS Operation Software (IGOS), to gather the input from IGRINS observer.
-
Cho, Kyung-Suk;Bong, Su-Chan;Nakariakov, Valery;Lim, Eun-Kyung;Park, Young-Deuk;Chae, Jongchul;Yang, Heesu;Park, Hyung-Min;Yurchyshyn, Vasyl 98
Due to the simple vertical structure of magnetic field, pores can be exploited to study the transport of mechanical energy by waves along the magnetic field to the chromosphere and corona. For a better understanding of physics of pores, we have investigated chromospheric traveling features running across two merged pores from their centers at the speed about 55 km s-1, in the active region AR 11828. The pores were observed on 2013 August 24 by using high time, spatial, and spectral resolution data from the Fast Imaging Solar Spectrograph (FISS) of the 1.6 meter New Solar Telescope (NST). We infer a LOS velocity by applying the bisector method to the Ca II$8542{\AA}$ band and$H{\alpha}$ band, and investigate intensity and the line-of-sight velocity changes at different wavelengths and different positions at the pores. We find that they have 3 minutes oscillations, and the intensity oscillation from the line center is preceded by that from the core ($-0.3{\AA}$ ) of the bands. There is no phase difference between the intensity and the LOS velocity oscillations at a given wavelength. The amplitude of LOS velocity from near the core spectra is greater than that from the far core spectra. These results support the interpretation of the observed wave as a slow magnetoacoustic wave propagating along the magnetic field lines in the pores. The apparent horizontal motion and a sudden decrease of its speed beyond the pores can be explained by the projection effect caused by inclination of the magnetic field with a canopy. -
Jeong, Woong-Seob;Park, Sung-Joon;Moon, Bongkon;Lee, Dae-Hee;Park, Won-Kee;Lee, Duk-Hang;Ko, Kyeongyeon;Pyo, Jeonghyun;Kim, Il-Joong;Park, Youngsik;Nam, Ukwon;Park, Chan;Im, Myungshin;Lee, Hyung Mok;Lee, Jeong-Eun;Shin, Goo-Hwan;Chae, Jangsoo;Matsumoto, Toshio 102
The NISS (Near-infrared Imaging Spectrometer for Star formation history) onboard NEXTSat-1 is the near-infrared instrument onboard NEXTSat-1 which is being developed by KASI. The main scientific targets are nearby galaxies, galaxy clusters, star-forming regions and low background regions in order to study the cosmic star formation history in local and distant universe. After the Preliminary Design Review, we have fixed major specifications of the NISS. The off-axis optical design with 15cm apertureis optimized to obtain a wide field of view ($2deg.{\times}2deg.$ ), while minimizing the sensitivity loss. The opto-mechanical structure of the NISS was designed to be safe enough to endure in the launching condition as well as the space environment. The tolerance analysis was performed to cover the wide wavelength range from 0.95 to$3.8{\mu}m$ and to reduce the degradation of optical performance due to thermal variation at the target temperature, 200K. The$1k{\times}1k$ infrared sensor is operated in the dewar at 80K stage. We confirmed that the NISS can be cooled down to below 200K in the nominal orbit through a radiative cooling. Here, we report the preliminary design of the NISS. -
Kim, Sanghyuk;Pak, Soojong;Jeong, Byeongjoon;Shin, Sangkyo;Kim, Geon Hee;Lee, Gil Jae;Chang, Seunghyuk;Yoo, Song Min;Lee, Kwang Jo;Lee, Hyuckee 103
Manufacturing of lens and mirror using Diamond Turning Machine (DTM) offers distinct advantages including short fabrication time and low cost as compared to grinding or polishing process. However, the DTM process can leave mid-frequency error in the optical surface which generates an undesirable diffraction effect and stray light. The mid-frequency error is expected to be eliminated by mechanical polishing after the DTM process, but polishing of soft surface of ductile aluminum is extremely difficult because the polishing process inevitably degrades the surface form accuracy. In order to increase its surface hardness, we performed electroless nickel plating on the surface of diamond-turned aluminum (Al-6061T6) off-axis mirrors, which was followed by the 6-hour-long baking process at$200^{\circ}C$ for improving its hardness. Then we polished the nickel plated off-axis mirrors to remove the mid-frequency error and measured polished mirror surfaces using the optical surface profilometer (NT 2000, Wyko Inc.). Finally, we ascertained that the mid-frequency error on the mirror surface was successfully removed. During the whole processes of nickel plating and polishing, we monitored the form accuracy using the ultra-high accurate 3-D profilometer (UA3P, Panasonic Corp.) to maintain it within the allowable tolerance range (< tens of nm). The polished off-axis mirror was optically tested using a visible laser source and a pinhole, and the airy pattern obtained from the polished mirror was compared with the unpolished case to check the influence of mid-frequency error on optical images. -
Shin, Jehyuck;Lee, Seongwhan;Lee, Jung-Kyu;Lee, Hyojeong;Lee, Jeongho;Seo, Junwon;Shin, Youra;Jeong, Seonyeong;Cheon, Junghoon;Kim, Hanjun;Lim, Jeonghyun;Lee, Junmin;Jin, Ho;Nam, Uk-Won;Kim, Sunghwan;Lee, Regina;Kim, Hyomin;Lessard, Marc R. 106
SIGMA (Scientific cubesat with Instrument for Global Magnetic field and rAdiation)는 근 지구공간에서 우주방사선량 측정과 자기장 변화 검출의 과학적 목적과 교육적 목적을 가지고 개발하고 있는 초소형 큐브위성이다.$100mm{\times}100mm{\times}340.5mm$ 의 크기로 약 3.6 kg의 무게를 가지며, 탑재체는 방사선에 대하여 인체와 동일한 산란 흡수 특성을 가진 Tissue Equivalent Proportional Counter (TEPC)와 자기장 측정을 위한 Magnetometer (Mag)이다. 위성체는 구조계, 자세제어계, 전력계, 명령 및 데이터처리계, 통신계로 구성되어있다. 구조계는 위성의 뼈대인 Chassis와 Mag deployer로 이루어져있고, 위성의 안정적인 자세유지를 목적으로 Attitude Control System (ACS) Board와 Torque Coil이 자세제어계로 구성된다. 전력의 생산과 공급 및 충전은 태양전지판과 Electrical Power System (EPS), 리튬 배터리로 구성된 전력계에서 이뤄지며, 명령 및 데이터처리계는 On Board Computer (OBC)와 Instrument Interface board (IIB)를 중심으로 서브시스템의 명령체계와 데이터처리를 다룬다. 통신계는 Uplink인 VHF 안테나와 Downlink인 UHF, S-band 안테나로 구성되며 지상과 명령을 송수신한다. SIGMA는 타임인터럽트 기능을 활용한 Flight Software (FSW)로 운용되며 임무에 따른 6가지 모드의 시나리오로 위성을 운용한다. 이에 SIGMA의 개발과 테스트 결과를 소개한다. 본 큐브위성 개발기술을 바탕으로 향후 천문관측용 위성에도 활용할 예정이다. -
Optical Multi-Channel Intensity Interferometry - or: How To Resolve O-Stars in the Magellanic CloudsTrippe, Sascha;Kim, Jae-Young;Lee, Bangwon;Choi, Changsu;Oh, Junghwan;Lee, Taeseok;Yoon, Sung-Chul;Im, Myungshin;Park, Yong-Sun 111
Intensity interferometry, based on the Hanbury Brown--Twiss effect, is a simple and inexpensive method for optical interferometry at microarcsecond angular resolutions. Motivated by recent technical developments, we argue that the sensitivity of large modern intensity interferometers can be improved by factors up to approximately 25,000, corresponding to 11 photometric magnitudes, compared to the pioneering Narrabri Stellar Interferometer of the 1970s when resolving. Our approach, based on spectrally resolved light, permits the construction of large optical interferometers at the cost of (very) long-baseline radio interferometers. Realistic intensity interferometers are able to spatially resolve main-sequence O-type stars in the Magellanic Clouds. Multi-channel intensity interferometers can address a wide variety of science cases: (i) linear radii, effective temperatures, and luminosities of stars; (ii) mass-radius relationships of compact stellar remnants; (iii) stellar rotation; (iv) stellar convection and the interaction of stellar photospheres and magnetic fields; (v) the structure and evolution of multiple stars; (vi) direct measurements of interstellar distances; (vii) the physics of gas accretion onto supermassive black holes; and (viii) calibration of amplitude interferometers by providing a sample of calibrator stars. -
We present our activities linking to planning of possible forms of large program to study on circumstellar H2O and SiO maser sources with KaVA. A great advantage of KaVA for the stellar maser observations is the combination of the unique capability of the multi-frequency phase referencing technique of KVN and the dual-beam astrometry of VERA with the KaVA's relative dense antenna configuration. We have demonstrated this advantage through the test observations conducted by the KaVA Evolved Stars Sub-working Group since 2012 March. Snapshot KaVA imaging is confirmed to be possible in integration time of 0.5 hour at the 22 GHz band and 1.0 hour at the 43 GHz band in typical cases. This implies that large snapshot imaging surveys towards many H2O and SiO stellar masers are possible within a reasonable machine time (e.g., scans on ~100 maser sources within 200 hours). This possibility enables us to select the maser sources, which are suitable for future long-term (10 years) intensive (biweekly-monthly) monitoring observations, from 1000 potential target candidates selected from dual-frequency band (K/Q-bands) KVN single-dish observations. The output of the survey programs will be used for statistical analysis of the structures of individual stellar maser clumps and the spatio-kinematical structures of circumstellar envelopes with accelerating outflows. The combination of astrometry in milliarcsecond(mas) level and the multi-phase referencing technique yields not only trigonometric parallax distances to the masers but also precise position reference for registration of different maser lines. The accuracy of the map registration affects interpretation of the excitation mechanism of the SiO maser lines and the origin of the variety of the maser actions, which are expected to reflect periodic behaviors of the circumstellar envelope with stellar pulsation. Currently we are checking the technical feasibility of KaVA operations for this combination. After this feasibility test, the long-term monitoring campaign program will run as one of KaVA's legacy projects.
-
First, We will briefly introduce early science results of AGN observations with KVN and KaVA. KaVA is the combined array of the Korean VLBI network (KVN) and VLBI Exploration of Radio Astronomy (VERA). These include KaVA monitoring of M87, Sgr A* and a few bright blazars and KVN Search for circular polarized Blazars. Furthermore, we will present our future plan of monitoring observation of Sgr A* and M87 with KaVA and Low Radio Power AGN multi frequency polarization survey with KVN. Because of the largeness of their centralsuper-massive black holes, we select them as top-priority sources of our key science program (KSP). The main science goals of the KaVA KSP are (1) mapping the velocity field of the M87 jet and testing magnetically-driven-jet paradigm, and (2) obtaining tightest constraints on physical properties of radio emitting region in Sgr A. High sensitivity achieved through simultaneous multifrequency phase referencing technique of KVN will allow us to explore Low Radio Power AGN cores which build majority of AGNs and therefore are important for undestanding the evolution of AGNs and of their hosts.
-
Clusters of galaxies provide unique laboratories to study astrophysical processes on large scales, and are also important probes for cosmology. X-ray observations are still the best way to find and characterise clusters. The extended ROSAT-ESO flux-limited X-ray (REFLEX II) galaxy clusters form currently the largest well-defined and tested X-ray galaxy cluster sample, providing a census of the large-scale structure of the Universe out to redshifts of z-0.4. I will describe the properties of the survey and the X-ray luminosity function, which led to our recent cosmological constraints on omegaM-sigma8. They tighten the previous constraints from other X-ray experiments, showing good agreements with those from the Planck clusters, but some tension exists with the Planck CMB constraints. The second part of my talk will concern the structure of the local Universe, and the study of the first X-ray superclusters. The density of the clusters reveals an under-dense region in the nearby Universe, which has an interesting implication for the cosmological parameters. Using the X-ray superclusters, that are constructed with a physically motivated procedure, I will show environmental aspects that X-ray superclusters provide, and compare to cosmological N-body simulations.
-
고립된 은하주위의 위은하들의 편향된 낙하 운동을 보인다. 이 편향성을 결정하는 요소는 속도가위장의 비등방성인데 속도가위장의 단축으로 위은하들의 낙하가 일어나는 관측적 증거를 제시하고 이 편향성을 측정하여 은하단과 은하의 동력학적 질량을 결정한 후 궁극적으로 중력 법칙을 검증한다.
-
Neutrino science has received a boost of attention quite recently in cosmology, since the outstanding discovery in particle physics over the last decade that neutrinos are massive: pinpointing the neutrino masses is one of the greatest challenges in science today, at the cross-road between particle-physics, astrophysics, and cosmology. Cosmology offers a unique 'laboratory' with the best sensitivity to the neutrino mass, as primordial massive neutrinos comprise a small portion of the dark matter and are known to significantly alter structure formation. I will first introduce a new suite of state-of-the-art hydrodynamical simulations with cold dark matter, baryons and massive neutrinos, specifically targeted for modeling the low-density regions of the intergalactic medium as probed by the Lyman-Alpha forest at high-redshift. I will then present and discuss how these simulations are used to constrain the parameters of the LCDM cosmological model in presence of massive neutrinos, in combination with BOSS data and other cosmological probes, leading to the strongest bound to date on the total neutrino mass.
-
We investigate the history of formation of ~400 galaxies in four Abell clusters at 0.04We report on the optical spectroscopic analysis of a Low Luminosity Quasi Stellar Objects (LLQSOs) sample at
$z{\leq}0.06$ based on the Hamburg/ESO QSO survey (HES). To better relate the low-redshift Active Galactic Nucleus (AGN) to the QSO population it is important to study samples of the latter type at a level of detail similar to that of the low-redshift AGN. Powerful QSOs, however, are absent at low redshifts due to evolutionary effects and their small space density. Our understanding of the (distant) QSO population is, therefore, significantly limited by angular resolution and sensitivity. The LLQSOs presented here offer the possibility to study the faint end of this population at smaller cosmological distances and, therefore, in greater detail. This, in turn, provides information about the key ingredients with respect to fueling and feedback of QSOs, and their relative importance/strength. Here, we present results of the analysis of visible wavelength spectroscopy provided by the HES and the 6 Degree Field Galaxy Survey (6dFGS). Interesting differences in the taxonomy of the sources having both types of spectra have been noticed and will be discussed.We present the three-dimensional genus topology of large-scale structure using the CMASS sample of the Final SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS) data. To estimate the uncertainties in the measured genus, we very carefully construct mock CMASS surveys along the past light cone from the Horizon Run 3. We find that the shape of the observed genus curve agrees very well with the prediction of perturbation theory and with the mean topology of the mock surveys. However, comparison with simulations show that the observed genus curve slightly deviates from the theoretical Gaussian expectation. From the deviation, we further quantify the primordial non-Gaussian contribution.최근 연구에서 발디 등은 우주론적 축퇴라는 이슈를 부각시켰다. 우주론적 축퇴는 실제 우주가 다수의 대안 우주론을 동시에 복합적으로 가질 때 거대 구조를 이용한 기존의 통계적인 방법만으로 우주론을 단정적으로 구별해 내기 충분치 않다는 것을 의미한다. 이 연구에서는 초은하단 스파인(spine)의 비크기(specific size)가 우주론적 축퇴를 완화할 수 있는지 조사하였다. f(R) 중력과 무거운 중성미자가 동시에 복합적으로 적용되는 다체 수치실험의 헤일로들을 분석한 결과, f(R) 중력이 비크기에 미치는 영향을 최대한으로 억제하는${\sum}_im_{{\nu}_i}$ 의 값이 기존의 통계적인 방법들에서 얻은 값과 다름을 확인하였다. 더 나아가 z=0.3 이상의 높은 적색편이에서는 f(R) 중력과${\sum}_im_{{\nu}_i}$ 조합한 모든 우주에서의 초은하단 평균 비크기가 표준 우주론인${\Lambda}$ CDM과 통계적으로 유의미하게 달라지는 것을 확인하였다. (arXiv:1404.3639v1)우주론의 표준모형에서는 어느 정도 큰 규모에서 물질의 분포가 균일하고 등방하다고 가정한다. 본 연구는 어떤 규모에서 물질의 분포가 균일한지 은하의 관측 자료를 이용하여 조사하였다. 관측 자료로는 SDSS Data Release 7의 적색편이 값이 0.16에서 0.47사이에 있는 105,831개의 LRGs의 목록을 사용하였다. LRGs의 목록을 이용해서 일정한 적색편이 구간에 있는 은하들을 택하여, 이를 2차원 면으로 간주하고, 각 은하를 중심으로 원을 만들어 원의 면적에 대한 원 내부에 있는 은하들의 개수의 증감을 이용하여 균일성을 조사하였다. 정확한 비교를 위해 LRGs의 목록과 동일한 수의 은하를 무작위적으로 뿌린 Random catalog와 표준모형을 기반으로 만들어진 Horizon Run 3의 N-body simulation 의 결과로부터 얻어낸 halo mock catalog를 각각 비교하였다.structure of matters of Lambda cold dark matter (CDM) cosmology on detailed numerical simulations. To accomplish our research goal, we have added the following baryonic physics on the existing cosmological hydrodynamic code, Gadget-2: 1) radiative heating and cooling, 2) reionization of the Universe and UV shielding, 3) star formation, 4) energy and metallicity feedback by supernova. In addition, we included cluster formation to distinguish clustered star formation inside the very high density gas clumps from the field star formation. Our simulations cover a cubic box of a side length 4Mpc/h with 130 million particles. The mass of each particles is$3.4{\times}104Msun$ , thus the GCs can be resolved with more than hundreds particles. We discuss various properties of the GCs such as mass function, specific frequency, baryon-to-dark matter ratio, metallicity, spatial distribution, and orbit eccentricity distribution as functions of redshift. We also discuss how the formation and evolution of the GCs are affected by UV shielding.Ko, Jongwan;Utsumi, Yousuke;Hwang, Ho Seong;Dell'Antonio, Ian P.;Geller, Margaret J.;Yang, Soung-Chul;Kyeong, Jaemann 45.2
To measure the mass distribution of galaxy systems weak-lensing analysis has been widely used because it directly measures the total mass of a system regardless of its baryon content and dynamical state. However, the weak-lensing only provides a map of projected surface mass density. On the other hand, galaxy redshift surveys provide a map of the three-dimensional galaxy distribution. It thus can resolve the structures along the line of sight projected in the weak-lensing map. Therefore, the comparison of structures identified in the weak-lensing maps and in the redshift surveys is an important test of the issues limiting applications of weak-lensing to the identification of galaxy clusters. Geller et al. (2010) and Kurtz et al. (2012) compared massive clusters identified in a dense redshift survey with significant weak-lensing map convergence peaks. Both assessments of the efficiency of weak-lensing map for cluster identification did not draw a general conclusion, because the sample is so small. Thus, we additionally perform deep imaging observations of fields in a dense galaxy redshift survey that contain galaxy clusters at z~0.2-0.5, using CFHT Megacam.The calcium infrared triplet (CaT) is one of the prominent absorption features in the infrared wavelength regime. Recently, this absorption feature has been getting attention in the prediction of metallicity of stellar populations because of its strong sensitivity to the calcium abundance and metallicity of a star. However, we find that measuring metallicity directly from CaT is very dangerous because the formation mechanism of CaT is very inefficient in the cool stars which are abundant in metal-rich populations. This characteristics of CaT make the CaT-metallicity relation to converge around ~$8{\AA}$ in the metal-rich regime. Our results suggest that, because of the converging CaT-metallicity relation in the metal-rich regime, the metallicity of simple stellar populations greater than [Fe/H]~-0.5 is unreliable when the linear conversion between CaT and metallicity is applied to derive metallicity. Based on these results, we suggest that CaT is not a good metallicity indicator for the metal-rich stellar populations.Bulges of galaxies are thought to have formed and grown at least in part through galaxy mergers, and thus an accurate derivation of their properties can be an effective course to test/confirm our understanding on their formation and evolution in the standard hierarchical merger paradigm. We have generated a sample of galaxy bulges (n = 15,423) in the nearby (0.005 < z < 0.05) universe from the SDSS DR7 and GALEX GR6plus7 databases and derived their structural and photometric properties by means of SExtractor and GALFIT application. Most notable properties include bulge-to-total luminosity ratio, effective radius, disk scale length, ellipticity, and position angle. The UV properties of the bulges have also been analyzed to infer their recent star formation history. A spectroscopic analysis has been performed using their absorption and emission line strengths measured and released by the OSSY team. We present our preliminary results from our investigation mainly focused on stellar population properties and discuss their implications on the formation of bulges.We investigate the evolution of galaxies in mid-infrared (MIR)$[3.4{\mu}m]-[12{\mu}m]$ color versus$12{\mu}$ luminosity diagram using Wide-field Infrared Survey Explorer data for member galaxies of the A2199 supercluster at$z{\simeq}0.03$ . In the MIR color-luminosity diagram, we classify galaxies into three MIR classes: MIR blue cloud (massive, quiescent and mostly early-type), MIR star-forming sequence (mostly late-type), and MIR green valley galaxies. Both MIR green valley galaxies and MIR blue cloud galaxies are optically red sequence populations, and there is no significant difference in star formation rates and stellar masses between them. We compare cumulative distribution functions of surface galaxy number density and of cluster/group-centric distance between three MIR classes. However, when considering only early-type galaxies, the difference between MIR blue cloud galaxies and MIR green valley galaxies disappears. In contrast, the intermediate trend of MIR green valley galaxies is still found for late-type galaxies. We discuss our results concerning the difference of evolution between early- and late-type galaxies and the connection to environment.We study the resolved stellar populations of ESO149-G003, a nearby dwarf irregular galaxy in the vicinity of the Sculptor group. We present F606W-F814W vs. F814W colour-magnitude diagrams (CMDs) obtained from HST/ACS archival data. We analyze the stellar content of ESO149-G003, as well as the spatial distribution of stars selected from stellar isochrone fitting analysis. Distance measurement using the tip of the red giant branch method, age measurement of various populations seen in the CMD, and isochrone fitting result will be shown and discussed.The Virgo cluster, the nearest galaxy cluster, is dynamically young, hosting numerous globular clusters in galaxies as well as intracluster globular clusters (IGCs). We obtained spectra of globular cluster candidates in the core region of the Virgo cluster using Hectospec at MMT to study the kinematics of the globular clusters. The targets are located at a large range (50 kpc < d < 500 kpc) from M87, the most massive galaxy in Virgo. We distinguish the genuine globular cluster population in the targets by inspecting their spectral features and radial velocities. As a result, a significant number of IGCs are found. We present preliminary results of the kinematics of globular clusters in the Virgo core region.Ultra faint dwarf galaxies (UFDs) are larger but fainter than globular clusters, being the faintest galaxies in the universe. They have been found only in the Local Group. We report the discovery of an UFD in the intracluster field of the Virgo cluster (Virgo UFD1). It is located near the core of Virgo cluster, and far from any massive galaxies. The color magnitude diagram of resolved stars in Virgo UFD1 shows narrow, metal poor red giant branch (RGB), which is very similar to the UFDs in the Local Group. by comparing RGB in this galaxy with 12 Gyr stellar isochrones, we estimate its distance,$d=16.4{\pm}0.4$ Mpc and mean metallicity,$[Fe/H]=-2.4{\pm}0.4$ . We derive its integrated photometric properties and structural parameters : V-band absolute magnitude of$MV=-6.3{\pm}0.2$ , effective radius of$84{\pm}7pc$ , and central surface brightness of${\mu}V,0=26.49{\pm}0.09$ mag arcsec-2. These properties are similar to these of Local Group UFDs. Virgo UFD1 is the first UFD discovered beyond the Local Group. These results indicate that it may be a fossil remnant of the first galaxies.Sohn, Jubee;Ko, Youkyung;Lim, Sungsoon;Jang, In Sung;Lee, Myung Gyoon;Hwang, Narae;Kim, Sang Chul;Park, Hong Soo 53.1
The M81 group is a nearby galaxy group hosted by M81, a twin galaxy of Milky Way. This galaxy group is considered as an ideal laboratory for near-field cosmology to understand mass assembly and evolution of galaxies in the group environment. We designed a project to investigate spectroscopic properties of globular cluster candidates in this group. We obtained spectra of globular cluster candidates using the MMT/Hectospec as a part of the K-GMT Science Program. Our main targets include globular cluster candidates of the M81 group member galaxies and those wandering in the intragroup region. We also observed supernova remnants and some background galaxies. Observing fields covered about 2 square degrees including three main galaxies of the M81 group. Using these spectra, we will identify globular clusters in the M81 group, and investigate their properties including age and metallicity. We will discuss the MMT/Hectospec data reduction processes, and future plan for this project.Radial color gradient of early type galaxies (ETGs) is a key tool for studying the evolution of these galaxies. In this work, we investigated whether ETGs having negative or positive color gradients show any distinguishable characteristics in the galaxy properties. We selected sample of 211 ETGs at 0.01 < z < 0.5 in the Spitzer FLS field, then we constructed u-R color gradients. We obtained the stellar mass, specific star formation rate and fluxes of emission lines of each ETG from MPA-JHU DR7 catalog. Spitzer IRAC and MIPS 24 micron data were used to detect dust emission from the ETGs. Preliminary result shows that less massive galaxies are likely to have positive color gradients, which is probably due to the ongoing star formation in the galaxy core. Almost all AGNs have negative color gradients. This probably is because AGNs are located in relatively massive galaxies with little ongoing star formation. There exists a marginal difference in the percentage of galaxies with PAH emission between ETGs having positive color gradient and negative color gradient. This also supports that ETGs with positive color gradient are galaxies having enhanced star formation.Hwang, Narae;Park, Hong Soo;Lee, Myung Gyoon;Lim, Sungsoon;Hodge, Paul W.;Kim, Sang Chul;Miller, Bryan;Weisz, Daniel 55.1
on the observation with the Gemini Multi-Object Spectrograph on the Gemini-South 8.1 m telescope. The radial velocities of four ESCs do not display any sign of systematic motion, unlike the intermediate age carbon stars in NGC 6822. The ages and metallicities derived using the Lick indices show that the ESCs are old (>=8 Gyr) and metal poor ([Fe/H] <= -1.5). NGC 6822 is found to have both metal poor ($[Fe/H]{\approx}-2.0$ ) and metal rich ($[Fe/H]{\approx}-0.9$ ) star clusters within 15' (2 kpc) from the center, whereas only metal poor clusters are observed in the outer halo with r >= 20'(2.6 kpc). Based on the kinematics, old ages, and low metallicities of ESCs, we discuss the possible origin of ESCs and the formation of the outer halo of a small dwarf irregular galaxy NGC6822.Role of environments is one of today's most widely discussed and debated topic in the field of extra-galactic astronomy. Extreme morphology-density relations found in low-mass galaxies are considered to be the result of an effective role played by environment in the evolution of these galaxies. I will present the results from our dedicated study of early-type dwarf galaxies (dEs) in different environments using imaging and spectroscopic data. We find that Virgo cluster dEs have a variety of structural and kinematic properties. A significant fraction of dEs possesses disk features, such as spiral arm and bar, while a central nucleus seems to be universal in these low mass galaxies. We also find that a majority of dEs are fast rotator and their rotation curves are much steeper than that of spiral galaxies of similar mass. Finally I will discuss how the different environmental mechanisms, i.e., gas-stripping or tidal interaction, can contribute to form heterogeneous dEs in Virgo cluster.Although the growth of structure, as traced by galaxy clusters, has been extensively studied through cosmological simulations and large-scale surveys, the early formation and evolution of their galaxy content, and its relation to the transformation of the host environment, are still somewhat poorly understood. This is particularly true of the processes that give rise to the quiescent galaxy population between z=3 and z=2. Recent discoveries at z~2 are now bridging the gap between the well-established massive clusters of the last 9 Gyr and the high-redshift universe, and new datasets are now giving us access to statistical populations of intermediate-mass structures at this epoch. I will discuss the properties of quiescent galaxies in the most distant confirmed X-ray detected galaxy clusters, their implications for galaxy quenching at high-redshift as well as the regulation of star formation at group scales at z~2.We present an extensive study of the environment of galaxies with bars in the low-redshift Uni-verse, using a volume-limited sample of over 30,000 galaxies drawn from the Sloan Digital Sky Survey, with visually-determined morphological classifications and bar identifications. We use four different statistics to quantify the environment of our galaxies: the projected two-point cross-correlation function with respect to a spectroscopic sample of reference galaxies, the background-subtracted number count of galaxies in a deep photometric sample in the vicinity of our galaxies, the overdensity of the local environment estimated at ~3 Mpc scale from the three-dimensional reconstruction of the cosmic density field of the local Universe, and the membership of our galaxies in the SDSS galaxy groups to segregate central to satellite systems. We find a weak, but significant trend for early-type galaxies with a bar to be more strongly clustered on scales from a few 100 kpc to 1 Mpc, when compared to early-type galaxies without a bar. For late-type galaxies, we find less neighbours within ~50 kpc around the barred late-types when compared to the unbarred late-types. For late-type galaxies we also detect a decrease of the bar fraction for dark matter dominated systems, and finally we find no obvious correlation between the overdensity and the fraction of barred galaxies in our sample.We present results of our investigation of intrinsic brightness temperatures of compact radio jets at radio frequencies. The intrinsic brightness temperatures of about 100 compact radio jets at 2, 5, 8, 15, and 86 GHz are estimated based on large VLBI surveys conducted in 2001-2003 (or in 1996 for the 5 GHz sample). The multi-freqeuncy intrinsic brightness temperatures of the sample of the jets are determined with a statistical method relating the observed brightness temperatures with the maximal apparent jet speed, assuming one representative intrinsic brightness temperature for the sample at each observing frequency. With investigating the observed brightness temperatures at 15 GHz in multiple epochs, we found that the determination of the intrinsc brightness temperature for our sample is affected by variability of individual jets in flux density at the time scales of a few years. This implies an importance of contemporaneity of the multi-frequency VLBI observations for the statistical method. Since our analysis is based on the VLBI observations conducted in 2001-2003, the results are less affected by the flux density variability. We found that the intrinsic brightness temperature$T_0$ increases as$T_0{\propto}{\nu}^{\epsilon}$ with${\epsilon}{\approx}0.7$ below a critical frequency${\nu}_c{\approx}10GHz$ where energy losses begin to dominate the emission, and above the critical frequency,$T_0$ decreases with${\epsilon}{\approx}-1.2$ supporting for the decelerating jet model.Red active galactic nuclei (AGNs) are supposed to be transitional objects becoming normal AGNs in the galaxy evolution scenario. So far, ~200 red AGNs have been found by very red color in optical through NIR wavelength (e.g., r'-K >5 and J-K>1.3; Urrutia et al. 2009). Here, we compare nuclear activities of the red AGNs to those of normal AGNs to verify the evolutionary phase of the red AGNs. In order to study the nuclear activities of the red AGNs, we use broad emission lines of$P{\beta}$ ($1.28{\mu}m$ ) of which flux is less suppressed by a factor of 100 than the$H{\beta}$ line in the case of the red AGNs with a color excess of E(B-V)=2 mag. We use 16 red AGNs discovered in previous red AGN surveys by using SDSS, 2MASS, and FIRST (Glikman et al. 2007; Urrutia et al. 2009) at z ~0.7 for which$P{\beta}$ lines are redshifted to the sky window at${\sim}2.2{\mu}m$ . The mean Eddington ratio of the 16 red AGNs is 0.562, and that of the normal AGNs is 0.320, which indicates the red AGNs include more active black hole (BH) than the normal AGNs. To test how significantly the nuclear activities of the red AGNs and the normal AGNs are different, we perform a two-dimensional Kolmogorov-Smirnov test (K-S test) on their Eddington ratio distributions. The K-S test shows the maximum deviation between the cumulative distributions, D, is 0.48, and the probability of null hypothesis, p, is even less than 0.001. This result is consistent with a picture of that the red AGNs are in intermediate phase between the stage of merger-driven starburst galaxy and the normal AGN.Energetic gas outflows from active galactic nuclei (AGNs) may have a crucial role in galaxy evolution. In this contribution, we present a census of ionized gas outflows using a large sample (~23,000) of local (z < 0.1) type-2 AGNs selected from the Sloan Digital Sky Survey DR 7. By measuring the velocity offset of narrow emission lines, i.e., [O III]${\lambda}5007$ and the Balmer lines, with respect to the systemic velocity measured from the stellar absorption lines, we find ~47% of AGNs showing an [O III] line-of-sight velocity offset${\geq}20km\;s-1$ . The fraction in type-2 AGNs is similar to that in type-1 AGNs after considering the projection effect. AGNs with larger [O III] velocity offsets, in particular with no or weak$H{\alpha}$ velocity offsets, tend to have higher Eddington ratios, implying that the [O III] velocity offset is related to on-going black hole activity. Also, we find the different distributions of the host galaxy inclination between the AGNs with blueshifted [O III] and the AGNs with redshifted [O III], supporting the model of biconical outflow with dust obscuration. Meanwhile, for ~3% of AGNs, [O III] and$H{\alpha}$ exhibit comparable large velocity offsets, suggesting a more complex gas kinematics than decelerating outflows in the narrow-line region.We present the results of the KVN observations of central galaxies in cool-core and non cool-core clusters. The goal is to study how cooling environments affect the AGN activities in the core where their host galaxies are embedded. From the HIghest FLUx Galaxy Cluster Sample (HIFLUGCS), we have selected 19 radio bright AGNs located in the center of clusters with various cooling timescale. In our pilot study, we have obtained 22 and 43 GHz fluxes and morphologies of the sample using the Korean VLBI network. We find that 22/43 GHz fluxes do not strongly depend on the presence of a cool gas flow. However, an intriguing fact is that most AGNs in the cool-core clusters show the hint of a pc-scale jet component while the ones in the non cool-core clusters do not. Based on these results, we discuss the role of cooling flows in the central cluster AGNs and their co-evolution.AGN feedback has been believed as playing an important role in the galaxy-super massive black hole (SMBH) co-evolution. AGN gas outflow can lead to AGN feedback. We investigate gas outflow of low-redshift AGNs by using blue shift/asymmetric index (BAI), and velocity offset of CIV line. By comparing these gas outflow indicators (BAI and velocity offset) to AGN properties (i.e., SMBH mass, bolometric luminosity, and Eddington ratio) and BLR gas metallicity, we find positive correlations among outflow, Eddington ratio, and metallicity. These relations are consistent with those observed at high-redshift. We discuss the possibility of the connection between previous star formation with current AGN accretion and outflow.We study the environmental dependences of various quasar properties using the Sloan Digital Sky Survey (SDSS). For an environmental indicator, we construct the galaxy number density field from the latest data (Data Release 12) of Constant MASS (CMASS) galaxies of SDSS in the redshift range 0.46<=z<=0.59. The galaxy number density field is determined by searching the 20 nearest galaxies from each grid point. For quasars, we use the fifth edition of the SDSS Quasar Catalog made by Schneider et al. (2010) and the catalog of properties for the quasars by Shen et al. (2011). We find environmental dependences of quasar properties as a function of the galaxy number density. This will help us to understand the evolution of quasars with their environment, which will be useful to improve modeling Active Galactic Nuclei feedback in cosmological hydrodynamic simulations.In the center of an Active Galactic Nuclei(AGN) is a supermassive black hole which accretes matter from its surroundings. The radio-loud AGN launch two relativistic jets perpendicular to the accretion disk which terminates into radio lobes located up to megaparsec away. Blazars form a small subset of radio-loud AGNs with one of two relativistic jets pointing toward the observer's line of sight. Many blazars often show flares at different frequencies. And these flares at different frequencies are known that they often correlate with each other. In 2013 December, there was a gamma-ray flare in 3C 279, one of the brightest blazars, Dec 2013. So we want to reveal that whether this flare correlates with radio flare or not, and where the flare originate. With polarization observation at radio frequencies, we can study the physical properties of the magnetic field in the innermost regions of the relativistic jets. Therefore, we have conducted polarization monitoring of this source from Dec. 2013 to Jun. 2014 with KVN(Korea VLBI Network) radio telescopes at 22, 43 and 86GHz. Here we present the initial results of the monitoring of 3C 279. We prospect that we can reveal the origin of this gamma-ray flare by comparing with our radio data.Hierarchical structure of star-forming regions is widespread and may be characteristic of all star formation. We studied the hierarchical structure of star-forming regions in the Local Group galaxies (M31, M33, Phoenix, Pegasus, Sextans A, Sextans B, WLM). The star-forming regions were selected from Galaxy Evolution Explorer (GALEX) far-UV imaging in various detection thresholds for investigating hierarchical structure. We examined the spatial distribution of the hot massive stars within star-forming regions from Hubble Space Telescope (HST) multi-band photometry. Small compact groups arranged within large complexes. The cumulative mass distribution follows a power law. The results allow us to understand the hierarchical structure of star formation and recent evolution of the Local Group galaxies.Kim, Seongjoong;Lee, Bumhyun;Oh, Se-Heon;Chung, Aeree;Rey, Soo-Chang;Jung, Teahyun;Kang, Miju 61.1
IC 10 is one of the most well-known irregular starburst dwarf galaxies in the Local Group. Its low metal and oxygen abundance together with proximity make it an excellent laboratory to test star formation models, especially in low-metallicity systems like galaxies in the early Universe as well as many other local dwarfs. Among a number of active star forming regions, we have detected H2O kilo-maser emission in the south-east region of IC 10(IC 10 SE) using the Korean VLBI Network(KVN). This maser line is likely to be associated with a giant molecular cloud identified in IC 10 SE by former CO studies. Using the HI and CO data from the VLA and SMA archive, we probe the atomic and molecular gas properties of IC 10 SE. We discuss how the cool gas morphology and kinematics are related with maser and star formation activity in IC 10 SE.Kim, Eunbin;Kim, Sungsoo S.;Lee, Gwang-Ho;Lee, Myung Gyoon;de Grijs, Richard;Choi, Yun-Young 61.2
A non-axisymmetric mass distribution of galactic structures including bulge (or bar) causes gas inflow from the disk to the nuclear region, including intense star formation within few hundred parsecs of galactic central. In order to investigate the relation between the ellipticity of the bulge and the presence of a nuclear starburst, we use a volume-limited sample of galaxies with Mr < -19.5 mag at 0.02 < z < 0.05 from the Sloan Digital Sky Survey Data Release 7. Total sample is 3252 spiral galaxies, which include nuclear starburst galaxies. We find that the occurrence of nuclear starbursts has a moderate correlation with bulge ellipticity of intermediate-type spiral galaxies (morphology classes Sab-Sb) in low galaxy number density environments and isolated regions where the distance between the target galaxies and the closest galaxies is relatively far. In high galaxy number density environments and interacting regions, close encounters and mergers between galaxies can cause gas inflow to the nuclear region even without the presence of non-axisymmetric bulges.Metallicity distribution of globular clusters (GCs) provides an important clue for star formation history of their host galaxy. With an assumption that GCs are generally old, GC colors have been used as a proxy of GC metallicities. Bimodal GC color distributions observed in most large galaxies have, for decades, been interpreted as bimodal metallicity distributions, indicating the presence of two populations within a galaxy. However, the conventional view has been challenged by a new theory that non-linear GC color-metallicity relations (CMRs) can cause a bimodal color distribution even from a single-peaked metallicity distribution. Using the photometric and spectroscopic data of NGC 5128 GCs in combination with stellar population simulation models, we examine the effect of non-linearity in GC CMRs on the transformation of GC color distributions into metallicity distributions. Although, in some colors, offsets are present between observations and models in the CMRs, their overall shape agrees well for various colors. After the offsets are corrected, the observed spectroscopic metallicity distribution is well reproduced via modeled CMRs from various color distributions having different morphologies. On the other hand, the linearly converted metallicity distributions from GC colors show a significant discrepancy with the observed spectroscopic metallicity distribution. We discuss the implications of our results.A relativistic jet associated with active galactic nuclei (AGNs) is almost ubiquitous while its formation mechanism is still not well understood. To get a deeper understanding of how an AGN jet forms and evolves, we have obtained Very Large Baseline Array (VLBA) data of a compact and optically violent variable quasar, OVV 1633+382 which is a small line-of-sight angle version of Fanaroff-Reily type 2 galaxy. Before our data were taken, a pronounced flare had been reported at mm wavelengths, making this object an excellent laboratory to study detailed properties of a radio jet powered by an AGN. The target have been observed in 12 epochs between 2002 and 2005 at 22, 43 and 86 GHz in full polarization mode. Among these observations, in this work, we present 43 GHz total intensity maps of our target for three epochs to discuss kinematics and geometry of the jet.The galaxy disk warp is a common phenomenon, yet their properties and formation mechanism(s) are still unclear. Here, we introduce a new automatic measurement method for the warp properties of stellar disks in nearby edge-on galaxies, including warp's angle, shape, and asymmetry. We obtain isophotal maps of edge-on galaxies and express each of isophote contours in polar coordinates (${\Phi}$ , R) centered on the galaxy centers. Two peaks in the${\Phi}$ -R diagram correspond to the outermost tips of each isophote. The locations of peaks, in turn, inform us of the misalignment between their inner and outer galactic planes, i.e., the warp. We apply this method to SDSS Stripe 82 co-added data and discuss its reliability and validity. Based on the measurement of warp properties, we also investigate their correlations with both intrinsic and environmental properties of warped galaxies.We observed a bright type Ia Supernovae SN 2014J located in the nearby starburst galaxy M82 using BOES (Bohyunsan Optical Echelle Spectrograph) for eight nights from day -11 (Jan. 22) to day +102 (May. 15) with respect to maximum brightness in B-band. We found the lines formed in the ejecta such as Si ($6300{\AA}$ ), whose velocity is more than 10,000km/s respect to the host galaxy as well as those formed in the circumstellar material (e.g. Na I D [$5890{\AA}$ ,$5896{\AA}$ ], 100km/s) Also, we found other weak iron ($5780{\AA}$ ,$5797{\AA}$ ,$6376{\AA}$ ,$6613{\AA}$ , and$7543{\AA}$ ), carbon ($8059{\AA}$ ) and other unknown elements. These lines are also thought to have been formed in circumstellar material. We expect that this study will contribute to revelation of the nature of the progenitor stars.We study the dust and star-formation characteristics of a nearby dwarf elliptical galaxy, NGC 855. With various archival data from ultraviolet to far-infrared, we build up the spectral energy distribution (SED) that can give us constraints on stellar populations, dust characteristics, star-formation history, etc. From GALEX and SDSS data, slightly de-centered bluer central core is confirmed, where star formation might take place. This regions is coincident with seemingly dis-integrated cores detected by Spitzer IRAC data and with bright Ha feature observed at ground-based telescope. The PACS and SPIRE data by Herschel Space Observatory show the dominant dust features at the center. Lastly, we propose necessary follow-up observations with ground-based telescopes to investigate spectral properties of NGC 855.Interacting galaxy pairs are important for study of galaxy evolution. We selected 8,542 interacting galaxy pairs out of 593,514 KIAS-VAGC galaxy sample with 0.02 < z < 0.047 and r_mag <17.6. We then classified by their interacting features into 6 types by visual inspection. We focused on two types whose spiral tidal features extend to the center of early type galaxy (ETG) or to the edge of ETG. We compared galactic parameters of these two types with those of entire 8,542 pairs as well as between the two types. Preliminary result shows both types are very close pairs (projected distance ~ 20 kpc). Spiral galaxies in the center type are more massive but less bright than those in edge type. ETGs in the edge type are brighter but not more massive than those in the center type. The center type has a mass ratio 3.4 times greater than the edge type, but the edge type has a higher angular momentum than the center type.We present Palomar/SWIFT integral field spectroscopy of z~0.2 strong$H{\alpha}$ emitters identified in the Sloan Digital Sky Survey. The large Halpha equivalent widths as well as the huge specific star formation rates of these galaxies are comparable with that of z>4 Lyman break galaxies, thus understanding the gas kinematics and the distribution of massive stars in these systems will help to obtain a better understanding of high-redshift star forming environments and the growth of massive galaxies. We measure the velocity dispersion across the entire galaxy, estimate the number density and the spatial distribution of massive stars from the emission line morphologies. The role of minor mergers in powering star formation is investigated as an alternative to cold flow driven star formation.We present a new hydrodynamic simulation code based on the Voronoi tessellation for estimating the density precisely. The code employs both of Lagrangian and Eulerian description by adopting the movable mesh scheme, which is superior to the conventional SPH (smoothed particle hydrodynamics) and AMR (adaptive mesh refinement) schemes. The code first generates unstructured meshes by the Voronoi tessellation at every time step, and then solves the Riemann problem for all surfaces of each Voronoi cell so as to update the hydrodynamic states as well as to move current meshes. Besides, the IEM (incremental expanding method) is devised to compute the Voronoi tessellation to desired degree of speed, thereby the CPU time is turned out to be just proportional to the number of particles, i.e., O(N). We discuss the applications of our code in the context of cosmological simulations as well as numerical experiments for galaxy formation.We study the environment of the most massive galaxies and the most massive black holes. We use SDSS DR7 data, the catalog from Simard et al. (2011), Mendel et al. (2014), and KIAS value-added galaxy catalog (Choi et al. 2011). Currently, we investigate the number density as an environment around each galaxy. Number densities are measured by$5^{th}$ and$10^{th}$ nearest photometric galaxies within 7000km/s from the spectroscopic galaxies. The most massive galaxies (M >$10^{12}M_{\odot}$ ) or black holes ($M{\sim}10^{10}M_{\odot}$ ) tend to reside in very dense regions in comparison with less massive ones. We also present the research plan and future work.The size evolution of galaxies is one of the fascinating issues in these days. It is known that the size of a galaxy is closely related to other galactic properties, such as the central surface brightness, stellar mass, and redshift. However, we need to measure the sizes of galaxies precisely to understand those relations. We determine the sizes of early-type galaxies in the nearby clusters (z<0.2) using the GALAPAGOS. The GALAPAGOS is a tool which provides surface photometry for multiple sources, which make it fast and convenient to deal with huge image data. We run the GALAPAGOS individually to the Subaru/Suprime-Cam and the HST/ACS images for the same targets. We present and discuss the result of our size measurements for further applications.Abell 2537 has been regarded as one of relaxed galaxy clusters because the X-ray emission is regular and symmetric, while there is also evidence to the contrary that the brightest cluster galaxy (BCG) is offset from the velocity center. To investigate the dynamical state of A2537 we obtain the redshift information of cluster galaxy candidates using Hectospec mounted on the MMT 6.5 m and compile those in the literature. The velocity distribution of member galaxies appears bimodal, with the main peak including the BCG and a secondary peak at velocity difference ~2000 km s-1. Based on the three-dimensional analysis and statistical tests we conclude that A2537 has at least two substructures and is not fully relaxed from a merger near the line-of-sight. We discuss more about the dynamical state of A2537 based on the color-magnitude diagram and X-ray scaling relation.The presence of multiple populations is now well-established in most globular clusters in the Milky Way. In light of this progress, here we suggest a new model explaining the origin of the Sandage period-shift and the difference in mean period of type ab RR Lyrae variables between the two Oosterhoff groups. In our models, the instability strip in the metal-poor group II clusters, such as M15, is populated by second generation stars (G2) with enhanced helium and CNO abundances, while the RR Lyraes in the relatively metal-rich group I clusters like M3 are mostly produced by first generation stars (G1) without these enhancements. This population shift within the instability strip with metallicity can create the observed period-shift between the two groups, since both helium and CNO abundances play a role in increasing the period of RR Lyrae variables. The presence of more metal-rich clusters having Oosterhoff-intermediate characteristics, such as NGC 1851, as well as of most metal-rich clusters having RR Lyraes with longest periods (group III) can also be reproduced, as more helium-rich third and later generations of stars (G3) penetrate into the instability strip with further increase in metallicity. Therefore, although there are systems where the suggested population shift cannot be a viable explanation, for the most general cases, our models predict that the RR Lyraes are produced mostly by G1, G2, and G3, respectively, for the Oosterhoff groups I, II, and III.M74 is a nearby face-on spiral galaxy that hosts three core-collapse supernovae (SNe) : SN Ic 2002ap, SN II-P 2003gd, and SN II-P 2013ej. Therefore it is an ideal target to investigate the properties of the core-collapse SNe and to improve the calibration of Type II-P SNe as a standardizable candle. However, its distance is not well known. We present a new distance estimate to M74 based on the tip of the red giant branch (TRGB). From the photometry of archival F555W and F814W images taken with the Hubble Space Telescope, we derive the TRGB to be at$ITRGB=26.13{\pm}0.02$ and the distance modulus to be$30.04{\pm}0.04$ (random)${\pm}0.12$ (systematic) (corresponding to a linear distance,$10.19{\pm}0.14{\pm}0.56Mpc$ ). With this result, we calibrate the standardized candle method of SNe II-P. From the absolute magnitude of SN 2003gd corrected for its expansion velocity and reddening, we derive the value of the Hubble constant,$H0=72{\pm}6{\pm}7km\;s-1\;Mpc-1$ . It is in agreement with the uncertainty with the recent estimates based on the luminosity calibration of Type Ia SNe.High Frequency Peakers (HFPs) are radio-loud Active Galactic Nuclei (AGN), which are regarded as being in the earliest evolutionary phase (102-103 years) of radio galaxies. They are expected to be small in size (< ~1 kpc) compared to their host galaxies (~a few 10s kpc), and have convex spectra, which are peaking at high radio frequency (> 5 GHz). Their size and spectral shape are the most obvious supporting evidence of extremely young ages. HFPs are therefore ideal targets to probe the earliest stage of radio sources. To date however, the young radio source classification has been relying mainly on the spectral shape which usually does not cover high enough frequencies where the true peak flux is located. Hence HFPs are often confused with blazars which may show a similar spectral shape and apparent compactness but are a somewhat evolved form of AGNs. Therefore, we have been challenging to identify HFPs among the sample of 19 candidates using the Korean VLBI Network (KVN) which enables us to extend the radio spectrum baseline up to 22 and 43 GHz. These are higher than the frequencies used in most previous studies of HFPs, allowing us to select genuine HFPs. By long-term monitoring of 18 epochs, we have also inspected the variability of the sample to select out blazars which are highly variable yet with a similar radio spectrum. In this work, we present the light curves and spectral properties of the HFP candidates. We discuss the results of our re-identification of HFPs.We present the spatially resolved kinematics of ionized gas and stars along the major axis of 9 pseudo bulge galaxies. Using the high quality long-slit spectra obtained with the FOCAS at the Subaru telescope, we measured the flux, velocity, and velocity dispersion of the [OIII] and$H{\beta}$ lines to determine the size of the narrow-line region, rotation curve, and the radial profile of velocity dispersions. We compare ionized gas kinematics and stellar kinematics to investigate whether ionized gas shows any signs of outflows and whether stars and ionized gas show the same sigma-dip feature (i.e., decrease of velocity dispersion) at the very center.We present space-based near-IR (NIR) and optical photometry of globular clusters (GCs) of 16 early-type galaxies in the Fornax and Virgo Clusters. The NIR imaging data for the nearby galaxies was acquired with the IR Channel of the Wide Field Camera 3 (WFC3/IR) in the F110W ($J_{110}$ ) and F160W ($H_{160}$ ) bandpasses. We introduce the full sample of our WFC3/IR program, describe data reductions and photometric measurements including GC candidate selection criteria, and then show selected GCs' color-magnitude diagrams. The tilted features in the diagrams related to the morphological types of host galaxies are discussed in the context of galaxy formation and evolution histories. Combining F475W ($g_{475}$ ) and F850LP ($z_{850}$ ) data taken from the Advanced Camera for Surveys Virgo and Fornax Cluster Surveys with our NIR data, we investigate the bimodality in optical-NIR color distribution and the nonlinear feature of the optical-NIR color relation as a function of optical color for these extragalactic GC systems.We analyze a newly discovered galaxy-galaxy scale gravitational lens system, FLS 1718+59 in the Spitzer First Look Survey (FLS) field. A background galaxy (z = 0.245) is severely distorted by a foreground galaxy (z = 0.08), via gravitational lensing. We analyze this system by several methods, including surface brightness fitting (Galfit and Ellipse), gravitational lens modeling (gravlens), and spectral energy distribution fitting (Magphys). From Galfit and Ellipse we measure properties of the lens galaxy, such as the effective radius and the average surface brightness inside it, the ellipticity, and the position angle. gravlens gives us the total mass inside the Einstein radius ($R_{Ein}$ ), and Magphys provides us an estimate of the stellar mass inside$R_{Ein}$ . By comparing these obtained parameters, we confirm that the lens galaxy is an elliptical galaxy on the Fundamental Plane, and calculate the stellar mass function inside$R_{Ein}$ , and discuss the implications of the results regarding the initial mass function.Galaxy clusters, the largest gravitationally bound systems, are an important means to place constraints on cosmological models. Moreover, they are excellent places to test galaxy evolution models in connection to the environments. To this day, massive clusters have been found unexpectedly(Kang & Im 2009, Durret et al. 2011, Tashikawa et al. 2012) and evolution of galaxies in cluster have been still controversial (Elbaz et al. 2007, Cooper et al. 2008, Tran et al. 2009). Finding galaxy cluster candidates in a wide, deep imaging survey data will enable us to solve the such issues of modern extragalactic astronomy. We have used multi-wavelength data from the UKIRT Infrared Deep Sky Survey Deep Extragalactic Survey (UKIDSS DXS/J and K bands), Spitzer Wise-area InfraRed Extragalactic survey (SWIRE/two mid-infrared bands), the Panoramic Survey Telescope and Rapid Response System (PAN-STARRS/ g, r, i, z, y bands) and Infrared Medium-deep Survey(IMS/J band). We report new candidates of galaxy clusters and properties of their member galaxies in one of the wide and deep survey fields ELAIS-N1, European Large Area ISO Survey North1, covering sky area of$8.75deg^2$ .Hwang, Ji-Hye;Woo, Jon-Hak;Jung, Taehyun;Chung, Aeree;Trippe, Sascha;Baek, Junhyun;Lee, Taeseok;Park, Dawoo 71.1
The black hole occupation fraction in dwarf galaxies can provide an important clue for understanding the black hole seed formation. As a pilot feasibility study, we performed a KVN radio monitoring campaign over 8 months for 4 dwarf galaxies. Two galaxies (IC10 and NGC1569) are detected at 22 GHz, respectively with 39 mJy, 83 mJy. The measured flux (rms) variability is 13% and 8%, respectively for IC10 and NGC1569, while the mean flux uncertainty is 25% and 12%. Thus, the detection of the radio flux variability is at best marginal. Detecting flux variability of faint sources (i.e., 22 GHz flux < 200 mJy) seems challenging with the KVN single dishes. Combining with the 1.4 GHz flux measurements from the NVSS, we find that these two galaxies have a steep spectrum, supporting that the radio sources are AGNs. Instead of a monitoring, single-epoch multi-band observations can be effective for identifying radio AGNs by providing the constraint of the radio continuum slope.processes at the origin of the star formation in the galaxies over the last 10 billions years. While it was proposed in the past that merging of galaxies has a dominant role to explain the triggering of the star formation in the distant galaxies having high star formation rates. In the opposite, more recent studies revealed scaling laws linking the star formation rate in the galaxies to their stellar mass or their gas mass. The small dispersion of these laws seems to be in contradiction with the idea of powerful stochastic events due to interactions, but rather in agreement with the new vision of galaxy history where the latter are continuously fed by intergalactic gas. I was especially interested in one of this scaling law, the relation between the star formation (SFR) and the stellar mass (M*) of galaxies, commonly called the main sequence of star forming galaxies. I have studied this main sequence, SFR-M*, in function of the morphology and other physical parameters as the radius, the colour, the clumpiness. The goal was to understand the origin of the sequence's dispersion related to the physical processes underlying this sequence in order to identify the main mode of star formation controlling this sequence. This work needed a multi-wavelength approach as well as the use of galaxies profile simulation to distinguish between the different galaxy morphological types implied in the main sequence.In the Joseon Dynasty, A day divided into 100 gak (刻, approximately a quarter) or 12 Sijin (時辰, double hours) that was composed of half-Sijin as Cho (初, beginnings of double hours) and Jeong (正, mid-points double hours). The timekeeping system was changed from 100 gak to 96 gak with using$sh{\acute{i}}xi{\grave{a}}n$ calendar (時憲曆) in 1654. And then 12 Sijin was changed to the 24-hours system in the same manner as current with the enforcement of the solar calendar (太陽曆) in 1896. We examine the record of the timekeeping system and notation of hours from the astronomical almanacs and official gazettes during 50 years after 1896. The Korean Empire Government first adopted the standard meridian of the Gyeongseong (former name of the Seoul in Korea) in 1908. However the mean solar time was applied to the almanac since 1913. After 1896, the year of enforcement of the solar calendar, the expression of times on a Korean almanac was written with O-jeon (午前, morning) and O-hu (午後, afternoon). The definition of 1day 24-hours system was first stated by the legislation in 1900. The expression of times was used 24 hours without O-jeon and O-hu in 1916. In daily life, the 24-hours system has used in parallel with 12-hours system divided into morning and afternoon even today.빅 히스토리(거대사)는 빅뱅부터 생명과 인류의 등장, 그리고 문명에 이르기까지 인문학과 자연과학을 모두 아우르는 융합 학문분야로, 최근 들어 중등 및 고등 교육기관 교육자들의 관심을 차츰 받고 있는 분야이다. 미국에서는 현재 빌 게이츠의 지원 아래 '빅 히스토리 프로젝트'를 운영하며 중등학교 교사들이 이용할 수 있는 자료를 구축하고 제공하는 등 활발한 교육 및 연구가 이루어지고 있지만, 아직 우리나라에서는 관련 연구가 교육이 활발히 이루어지고 있지는 않다. 이번 연구에서 우리는 1) 빅 히스토리 프로젝트, 2) 새로운 모습으로 올해 소개된 다큐멘터리 '코스모스', 3) 빅 히스토리 관련 서적들의 콘텐츠를 정리하고, 이들을 시대별, 주제별, 그리고 소주제별로 분류하여 얼마나 다양한 방법으로 접근할 수 있는지 보일 것이다. 향후에는 이 콘텐츠를 대학의 교양교육과정에서 어떻게 이용할 수 있는지를 제시하는 것이 목표이다.We investigate the influence of the galactic magnetic field (GMF) on the arrival direction (AD) of ultra-high energy cosmic rays (UHECRs) by searching the correlation with the large-scale structure (LSS) of the universe. The deflection angle of UHECRs from sources by the GMF is reflected in a source model by introducing the Gaussian smearing angle as a free parameter. Assuming the deflections by the GMF are mainly dependent on the galactic latitude, b, we divide the regions of sky by b and analyze the correlation between the AD of UHECRs and the LSS of the universe in each region varying the smearing angle. We find the deflection is strongly dependent on the galactic latitude by the maximum likelihood estimation. Specifically, the best-fit smearing angles are$9^{\circ}$ and$84^{\circ}$ in the high galactic latitude (HGL),$-90^{\circ}$ < b <$-60^{\circ}$ , and in the low galactic latitude (LGL),$-30^{\circ}$ < b <$30^{\circ}$ , respectively. The strength of GMF becomes stronger from the HGL to the LGL. From the results, we can estimate the strength of GMF in each region. In the LGL, for example, if we assume UHECRs are protons, we have the order of$100{\mu}G$ GMF, which is much stronger than the expected value of conventional GMF model. However, if the primaries are heavy nuclei, which is consistent with the observational result of mass composition analysis, the order of GMF strength is a few${\mu}G$ . More data from the future experiments make it possible to study the GMF between the source of UHECRs and Earth more accurately.We investigate the rotation measure (RM) of the nearby low luminosity AGN M87 by using archival polarimetric VLA data at 8, 15, 22 and 43 GHz. For the first time, the RM properties of its jet are resolved at at arc-second scales. The distribution of the RM appears to be a gaussian with a mean value of ~200rad/m2 and the power spectrum follows a power law with index -2.5. A simple Kolmogorov model assuming a random turbulent magnetic fields extrinsic to the jet appears not to be adequate to explain the observed RM power spectra. On the other hand, underlying RM gradients possibly connected with the jet could be a possible interpretation.Hayasaki, Kimitake;Sohn, Bong Won;Okazaki, Atsuo T.;Jung, Taehyun;Zhao, Guangyao;Naito, Tsuguya 74.1
We study a wraping instability of a geometrically thin, non-self-gravitating disk surrounding binary supermassive black holes on a circular orbit. Such a circumbinay disk is subject to not only tidal torques due Line 8 to the binary gravitational potential but also radiative rorques due to radiation emitted from each accretion disk. We find tat a circumbinary disk initially aligned with the binary orbital plane is unstable to radiation-driven warping beyond the marginally stable warping radius, which is sensitive to both the ratio of vertical to horizontal shear viscosities and the mass-to-energy conversion efficiency. As expected, the tidal torques give no contribution to the growth of warping modes but tend to align the circumbinary disk with the orbital plane. Since the tidal torques can suppress the warping modes in the inner part of circumbinary disk, the circumbinaary disk starts to be warped at the radii larger than the marginally stable warping radius. If the warping radius is of the order of 0.1 pc, a resultant semi-major axis is estimated to be of the order of 10-2 pc to 10-4 pc for 107 Msun black hole. We also discuss the posibility that the central objects of observed warped maser disks in active galactic nuclei are binary supermassive black holes with a triple disk: two accretion disks around the individual black holes and one circumbinary disk surrounding them.Magnetohydrodynamics(MHD) dynamo depends on many factors such as viscosity${\gamma}$ , magnetic diffusivity${\eta}$ , magnetic Reynolds number$Re_M$ , external driving source, or magnetic Prandtl number$Pr_M$ .$Pr_M$ , the ratio of${\gamma}$ to${\eta}$ (for example, galaxy${\sim}10^{14}$ ), plays an important role in small scale dynamo. With the high PrM, conductivity effect becomes very important in small scale regime between the viscous scale ($k_{\gamma}{\sim}Re^{3/4}k_fk_f$ :forcing scale) and resistivity scale ($k_{\eta}{\sim}PrM^{1/2}k_{\gamma}$ ). Since${\eta}$ is very small, the balance of local energy transport due to the advection term and nonlocal energy transfer decides the magnetic energy spectra. Beyond the viscous scale, the stretched magnetic field (magnetic tension in Lorentz force) transfers the magnetic energy, which is originally from the kinetic energy, back to the kinetic eddies leading to the extension of the viscous scale. This repeated process eventually decides the energy spectrum of the coupled momentum and magnetic induction equation. However, the evolving profile does not follow Kolmogorov's -3/5 law. The spectra of EV (${\sim}k^{-4}$ ) and EM (${\sim}k^0$ or$k^{-1}$ ) in high$Pr_M$ have been reported, but our recent simulation results show a little different scaling law ($E_V{\sim}k^{-3}-k^{-4}$ ,$EM{\sim}k^{-1/2}-k^{-1}$ ). We show the results and explain the reason.We present the result of a long-slit spectroscopic study of DG Tau, which is known to emanate parsec-scale outflows. To study the kinematics and physical properties of the jet, we obtained the optical emission lines of$H{\alpha}$ , [OI], [NII], and [SII] from HH 158 and HH 702 using the long-slit spectrograph at Bohyunsan Optical Astronomical Observatory. HH 158 shows the peak radial velocity in a range of ~ - 270 to - 30 km s-1. HH 702, located at 11' away from DG Tau shows the velocity of ~ - 80 km s-1. The proper motion velocities of detected knots are estimated through the comparisons with the locations of those knots in the previous studies. We also examine the variations of physical parameters depending on the velocity distribution and the distance from the source using line ratio maps derived from obtained forbidden emission lines.CS molecule as an important tracer for studying inward motions in dense cores is known to be adsorbed onto dusts in cold (T~10K) dense cores, resulting in its significant depletion in the central region of the cores which may hamper a proper study of kinematics stage of star formation. In this study we choose five 'evolved' dense starless cores, L1544, L1552, L1689B, L694-2 and L1197, to investigate how depletion of CS molecule is significant and how the molecule differentiates depending on the evolutional status of the dense cores, by using a rare isotopomer C34S. We performed mapping observations in C34S (J=2-1) and N2H+ (J=1-0) with Nobeyama 45 m telescope, and compared$850{\mu}m$ continuum data as a reference of the density distribution of the dense cores. Our data confirm the claim that CS molecule generally depletes out in the central region in dense starless cores, while N2H+ keeps abundant as they get evolved. All of integrated intensity maps show 'semi-ring-like' depletion holes in CS, and all of abundance radial profiles show decrease toward center. The CS depletion and molecular chemical differentiation seems to depend on the evolutional status in dense cores. The evolved cores shows low abundance at both central and outer regions, implying that in the case of highly evolved cores CS freeze-out occurs over the most area of the cores.We present near-infrared spectroscopic and photometric observations of the nova V2468 Cyg taken from 2008 March 14 till 2008 November 11 following its outburst on 2008 March 7. The JHK spectra of the nova have been taken from the Mount Abu Infrared Observatory using the Near-Infrared Imager/Spectrometer. The early spectra are dominated by strong H I lines from the Brackett and Paschen series, Fe II, O I and C I lines, typical of Fe II type novae but after 46 days from outburst there is significant reduction in the strength of the C I lines and the spectra are dominated by He I lines. The FWHM of the Pa-beta and Br-gamma lines change from 2200-2300 km s-1 to 1700-1800 km s-1 after 12 days from outburst. Three additional small amplitude outbursts are seen near 110, 185 and 240 days in the V band light curve after the discovery. The upper limit for the ejecta mass for V2468 Cyg is estimated to be$5.2{\times}10-6Msun$ .The Arches cluster is one of the compact, young, massive star clusters near the center of our galaxy. Since it is located only ~30 pc away in projection from the galactic center (GC), the cluster is an excellent target for studying the effects of star forming environment on, for example, the initial mass function under the extreme condition of GC. To estimate the initial condition of the Arches cluster, we compare our calculation results from the anisotropic Fokker-Planck method with the most recent observational data sets for the surface density and velocity dispersion profiles and the present-day mass function.Galactic spiral arms are abundant with interesting gaseous substructures. It has been suggested that arm substructures arise from the wiggle instability (WI) of spiral shocks. While the nature of the WI remained elusive, our recent work without considering magnetic fields shows that the WI is physically originated from the accumulation of potential vorticity (PV) generated by deformed shock fronts. To elucidate the characteristics of the WI in more realistic galactic situations, we extend our previous linear stability analysis of spiral shocks by including magnetic fields. We find that magnetic fields reduce the amount of density compression at shocks, making the shock fronts to move toward the upstream direction. Magnetic tension forces from bent field lines stabilize the WI by prevent the generation of PV. When the spiral-arm forcing is F=5% of the centrifugal force of galaxy rotation, the maximum growth rate of the WI is found to be about 1.0, 0.4, and 0.2 times the orbital angular frequency for the plasma parameter${\beta}=100$ , 10, and 5, respectively. Shocks with${\beta}=1$ are stable to the WI for F=5%, while becoming still unstable when F=10%.Questions of how our Milky Way evolves through the interaction with its environment have been constantly raised. One particularly interesting question is how the metallicity would change as our Milky Way goes through collision with HVCs. Because of the possibility of HVCs providing fuel for star formation in the Galactic disk, we simulate the collision between HVCs and the Galactic disk. More specifically, we trace how the Galactic metallicity changes throughout the process of HVCs colliding with our Milky Way based upon a specific scenario that HVCs are primordial gas left-overs from an ancient galaxy formation. Such mixing between metal-rich gas (disk) and metal-poor HVC can be traced by running numerical simulations with the FLASH code due to its capability of tracking down the abundance change of a specific element such as carbon at each time step of the hydrodynamic evolution. As for now, we give how this mixing depends on model parameters that we choose such as collision speed, initial metallicities, temperature and so on.An ionization front (IF) surrounding an H II region is a sharp interface through which a cold neutral gas makes transition to a warm ionized phase by absorbing UV photons from central massive stars. We investigate the structure and instability of a plane-parallel D-type IF threaded by magnetic fields parallel to the front. We find that magnetic fields increase the maximum propagation speed of the IFs, while reducing the expansion factor, defined as the density ratio of neutral to ionized phases. IFs become unstable to distortional perturbations due to gas expansion across the fronts, exactly analogous to the Darrieus-Landau instability of ablation fronts in terrestrial flames. The growth rate of the IF instability is proportional linearly to the perturbation wavenumber as well as the upstream flow speed. The IF instability is stabilized by gas compressibility and becomes completely quenched when the front is D-critical. The instability is also stabilized by magnetic pressure when the perturbations propagate in the direction perpendicular to the fields. When the perturbations propagate in the direction parallel to the fields, on the other hand, it is magnetic tension that reduces the growth rate, completely suppressing the instability when${\beta}$ < 1.5, with${\beta}$ denoting the square of the ratio of the sound speed to the Alfven speed in the pre-IF region. When the front experiences an acceleration, the IF instability cooperates with the Rayleigh-Taylor instability to make the front more unstable. We discuss potential effects of IF instability on the evolution and dynamics of IFs in the interstellar medium.Kim, Il-Joong;Pyo, Jeonghyun;Jeong, Woong-Seob;Han, Wonyong;Park, Won-Kee;Lee, Dukhang;Moon, Bongkon;Park, Sung-Joon;Park, Youngsik;Lee, Dae-Hee;Ko, Kyeongyeon;Seon, Kwang-Il;Kim, Min Gyu;Lee, Hyung Mok;Matsumoto, Toshio 78.2
MIRIS (Multi-purpose Infrared Imaging System) is the primary payload on the Korean science and technology satellite, STSAT-3, which was launched on 2013 November 21. It is designed to observe the near-infrared sky with a$3.67^{\circ}{\times}3.67^{\circ}$ field of view and a$51.6^{{\prime}{\prime}}{\times}51.6^{{\prime}{\prime}}$ pixel resolution. Using two narrow-band filters at$1.88{\mu}m$ (Pa${\alpha}$ line) and$1.84+1.92{\mu}m$ (Pa${\alpha}$ dual continuum), the Paschen${\alpha}$ Galactic plane survey has been carrying out, and the area for the Galactic longitude from$+280^{\circ}$ to$+100^{\circ}$ (with the width of$-3^{\circ}$ < b <$+3^{\circ}$ ) has been covered by 2014 August 31. In this contribution, we present the preliminary results of the MIRIS Paschen${\alpha}$ emission maps and compare them with other wavelength maps such as$H{\alpha}$ and dust maps. Many of the Paschen${\alpha}$ features have been detected along the plane, and some of them are weak or invisible in the$H{\alpha}$ map and coincide well with dense cloud regions.We present the result of near-infrared (near-IR) imaging polarimetry of star-forming regions in the Large Magellanic Cloud (LMC). We compiled near-IR photometric and polarimetric data of N159/160 regions. The photometric and polarimetric data were simultaneously obtained in J, H, and Ks bands using SIRPOL, an imaging polarimeter of the InfraRed Survey Facility (IRSF), in 2007 February. We measured Stokes parameters of point-like sources to derive their degree of polarization and polarization position angles. In this poster, we present polarization properties of these star-forming regions. We also discuss the polarization structure in these regions compared with mid-infrared dust emission structure from the Spitzer SAGE survey.Galactic radio pulsar population is diverse. So far about 2300 radio pulsars are known in the Milky Way, in addition to Large and Small Magellanic Clouds. Radio pulsar observations at a few hundreds MHz up to ~10 GHz have been active and they are proved to be fruitful. Low frequencies are preferred mainly because of the steep ratio spectrum of pulsars. However, developments in pulsar backends (e.g. a wide-band spectrometer) and improved system sensitivities make it possible to observe pulsars at higher frequencies using large, single-dish telescopes up to ~18 GHz. Going forward, mm-wavelength observations is expected to open a new window in pulsar astronomy. In particular, frequencies well above ~15 GHz are pre-requisite to detect pulsars in the Galactic Center where radio pulsed signals are severely scattered by interactions with the interstellar medium. Recent discoveries strongly imply that there are subsets of pulsars with an apparently flat spectrum, such as magnetars. In April 2014, the first pulsar (magnetar) was discovered only 3 arcmin from Sgr A*, PSR J1745-2900. We will present a brief overview on pulsar populations focusing on those observable at high frequencies. We will also discuss prospects of pulsar observations in mm-wavelengths and how we can utilize the Korean VLBI network.We made simultaneous surveys of 22 GHz water and 44 / 95 GHz methanol masers toward 299 high-mass protostellar objects using the Korea VLBI Network (KVN) 21-m telescope. The sources were selected from the catalog of Red MSX Source (RMS) survey. Initial selection of the sample present high-mass protostellar objects in an evolutionary phase prior to ultra-compact HII regions, which have bolometric luminosities >$10^3L_{\odot}$ but are not associated with any radio continuum emission. After the follow-up work of ongoing RMS survey, final samples contains 56 sources classified as HII regions. We performed a simultaneous survey of 22 GHz water and 44 GHz methanol masers in 2011 and then conducted a simultaneous survey of 22 GHz water and 44 / 95 GHz methanol masers in 2012. The primary scientific goals of these surveys are to investigate the relationship among the three masers and to explore the relationship between each maser and the central star or the parental dense core. The detection rates of two epochs are 42% and 38% for water, 25% and 26% for 44 GHz methanol, and 23% (2012 only) for 95 GHz methanol masers. We performed a statistical analysis on subsample associated with a large data found in literature. In this poster, we will the preliminary data analysis results and discuss the implications.Park, Sunkyung;Lee, Jeong-Eun;Kang, Wonseok;Sung, Hyun-Il;Lee, Sang-Gak;Green, Joel D.;Cochran, William D. 80.2
We present the results of high resolution (R>35,000) optical spectroscopic monitoring observations of a new FU Orionis-like young stellar object, HBC 722. We observed HBC 722 with the Bohyunsan Optical Echelle Spectrograph (BOES) and Hobby-Eberly Telescope (HET) since November 26, 2010. HBC 722 is the FU Orionis-like object best characterized for the pre-outburst phase, and it provides the first opportunity to profile the burst phase of accretion across all wavelengths. We detected a number of lines such as$H{\alpha}$ ,$H{\beta}$ , Fe II${\lambda}$ 5018, Mg I${\lambda}$ 5183, Na I D doublets, and metallic photospheric lines. In this work, we focus on the time variations of those spectral lines to understand the accretion process of HBC 722.We utilized a 2-D PDR code developed by Lee et al. (2014) to explore the observed OH line fluxes toward embedded protostars. This 2-D PDR code combines self-consistently the FUV radiative transfer, gas-energetics, chemistry, and line radiative transfer. We modeled two sources, GSS30-IRS1 and Elias29, which show conspicuous line emission in the Herschel/PACS wavelength range. The physical and chemical structure for a given embedded source was derived by fitting the PACS CO line fluxes. After exploring various parameter spaces, we conclude that IR-pumping effect either by the central IR source and dust in-situ is insignificant for OH emission, unlike previous studies. We here present a possible solution for the observed OH fluxes, which require a high OH abundance and temperature at the inner-part of the UV heated cavity wall.We have analyzed the archival data of far ultraviolet (FUV) observations made for the region of GSH 006-15+7, a large shell-like structure discovered by Moss et al. (2012) from the H I velocity maps. FUV emission is seen enhanced in the lower supershell region and is believed to originate from dust scattering of interstellar photons. A corresponding Monte Carlo simulation indicates that the supershell is located at a distance of$1250^{+750}{_{-500}}$ pc, similar to the previous estimation of 1.5{\pm}0.5 kpc based on kinematic considerations. The spectrum obtained for the lower supershell exhibits molecular hydrogen fluorescence lines: a simulation model for this candidate photodissociation region (PDR) yields a rather high total hydrogen density of$n_H{\sim}30cm^{-3}$ with H2 column density of$N(H_2){=}^{1017.5-20.0}cm^{-2}$ . It is argued that the region is in a transition stage from a warm to a cool neutral phase. Strong C IV emission is also seen in the spectrum, but it is not believed to be associated with the supershell as the corresponding spectral map shows a broad region of enhancement both inside and outside the supershell.Kepler-47 is the first multi-body circumbinary planetary system detected by the Kepler space telescope. The two planets were detected by the transit method. In the discovery paper the authors report about the presence of an additional transit-like signal in their dataset which cannot be explained by a four-body (binary + 2 planets) system. Therefore it is likely that the unexplained signal could be due to a third planet. In this talk I will present recent results from a dynamical investigation of the five-body system (binary + 3 planets). We have applied the MEGNO technique to detect regions of quasi- or near quasi-periodic orbits of a hypothetical third planet. Quasi-periodic regions exists for a third planet and the long-term stability has been tested. Although the existence of a third planet is most likely to be confirmed from transit photometry we calculate transit-timing variation (TTV) signals due to the third planet which also can be used to infer its presence.Flare and rotational variabilities induced by stellar activity are important for studying the effect of magnetic fields on the evolution of red dwarf stars. The level and frequency of magnetic activity in these stars have a different aspect at every moment of the observations due to the effect of age-rotation relation. The use of both tracers is thus essential to have a relatively homogeneous set of stellar activity data for statistical studies. The archival light curves and imaging data of the open cluster M37 taken by MMT 6.5m telescope were used for this work. In order to achieve much more accurate photometric precisions and also to make the most efficient use of the data, the entire imaging database were re-analyzed with our new time-series photometry technique and carefully calibration procedures. Based on the new light curves, we study, for the first time, a variety of aspects of those two variabilities in red dwarfs and their relation to magnetic activity. In this talk, we present all observational evidences that support the idea that the strength of magnetic activity is closely connected with the rotation rate of a star and its evolutionary status (age-activity-rotation paradigm). In conclusion, we suggest future directions to improve our understanding of stellar activity in cool stars with photometric time-series data.This research is to study the effects of individual element(C, N, O, Na, Mg, Al, Si, and Fe) on the standard stellar models. Our work is different from previous works in two aspects. Firstly, we have chosen to maintain helium abundance and other metal elements as target elements were changed. This is to see the effects more clearly, without further complication. Secondly, the amount of enhancement or reduction in each element has been based on the recent observation of stars in globular clusters. For comparison study with observation of the globular clusters, the mass and metallicity grids of the standard stellar models have been constructed in range$0.7{\sim}1.0M{\odot}$ and 0.0002~0.007, respectively. The opacity as a function of depth in stellar models at equal evolutionary point, as well as the evolutionary tracks, have been analyzed. The quantified shifts of the evolutionary tracks for the stellar models which have changed abundance of individual element and the astronomical meaning with physical reasons which produce the results, are going to be presented in this talk.We report the discovery of a new Milky Way globular cluster (GC) candidate in the Galactic plane. We found this object during our WISE survey of star clusters in the Milky Way. We derived physical parameters of this object using the 2MASS JHK photometry. The color-magnitude diagram of the resolved stars shows a well-developed red giant branch (RGB). We derived its reddening, distance and metallicity. These results indicate that it is probably an old globular cluster, located behind the Galactic disk.The progenitors of Type Ibc supernovae (SNe Ibc) have been believed to be massive Wolf-Rayet (WR) stars, formed either through stellar wind mass loss or Roche-lobe outflow in a binary system. But observations indicate that ordinary SNe Ibc have relatively low ejecta masses (~2 Msun), which is not compatible with the WR star scenario for SN Ibc progenitors. On the other hand, helium stars in binary systems which can be produced via mass transfer are also suggested as a possible candidate for SN Ibc progenitors. Binary star evolution models predict that SN Ibc progenitors having final masses of 3-7 Msun can be produced, but their observational properties are not well understood. In this study, we present the parameter study on the observational constraints of helium stars of 3-5 Msun in binary systems using evolutionary models and the atmospheric radiative transfer code CMFGEN. We present the predicted magnitudes and spectra of helium stars in optical bands for different wind velocity profiles and mass loss rates. We also present those observables of the progenitor binary system considering O-type companion stars. Based on the results, we discuss the expected observational properties of SN Ibc progenitors in binary systems. In particular, we discuss the constraints on the progenitor of the SN Ib iPTF13bvn of which progenitor candidate has been identified for the first time in pre-explosion images among SNe Ibc.최근 10년 동안의 측광 및 분광관측을 통하여 우리은하 내 구상성단들 중 대부분이 적어도 2개 이상의 항성종족을 갖는다고 밝혀졌다. 현재까지 이루어진 대부분의 구상성단의 항성종족 연구에서는 관측된 색등급도와 항성종족 합성모델 사이에 eye-fitting을 함으로써 항성종족 파라미터, 즉 중원소함량, 나이, 헬륨함량 등을 추정해왔다. 우리는 구상성단의 항성종족을 분석하기 위해${\chi}^2$ -Minimization에 의거하여 구상성단과 항성종족 합성모델의 Hess Diagram을 비교하고, 수치계산 기법을 도입하여 최적의 파라미터를 추정하는 알고리즘을 개발하였다. 이 연구에서는 가상으로 만든 성단에 대하여 Recovery Test를 수행함으로써 이 알고리즘의 Self-Consistency를 검증하였고, 실제 관측결과를 사용하여 이 연구의 적용 가능성을 조사하였다.Two substellar companion candidates with planetary mass, around a T-Tauri star in the${\rho}$ Ophiuchi star-forming region, are discovered by results of Subaru Telescope's near-infrared imaging. Candidates are separated by 1400au and 500au. If these candidates were real companions, they are the widest-orbit and the lowest mass planetary-mass companions(PMCs) candidates. This discovery may suggest that PMCs form via extreme case of cloud core fragmentation for multiple stars. And also stellar disk are imaged by HiCIAO, hight contrast instrument for exoplanets and disks, with Subaru Telescope. This could be the first case, which imaged both of planetary mass companions and disk around same star. Even two companions candidates are not bounded around the star, they still could be one of the lowest mass objects. In this presentation, I will discuss about observations and confirmations of these objects, and the latest results about their properties.We present a new ray-tracing code, "Odyssey", for the Kerr spacetime accelerated by the Graphics Processing Unit (GPU). Taking advantage of the ability of nVidia graphic cards to evaluate trajectories of a large amount of photon simultaneously, the code is two orders of magnitude as fast as the previous CPU-based code corresponding to the speed of few nanoseconds per photon per time step. In the light of the Graphic User Interface (GUI) powered by the GPU-enhanced 2D/3D displaying technique, DirectX, it is feasible for users to manipulate diverse results such as rotating and zooming in/out the trajectories of photon instantly near the black hole. Thus the Odyssey can serve as a tool not only for scientific but also for the educational purpose. We discuss possible applications in detail in light of several results such as the shape of the silhouette of a black hole, the shape of a hot spot orbiting a black hole, and 3D photon trajectories.우리는 늙은 산개성단 NGC 2420의 외곽 헤일로 구조를 연구하였다. Sloan Digital Sky Survey (SDSS)의 DR10 자료에 공개된 g, i의 영상을 이용하여 psf측광을 수행하였다. 이로부터 얻어진 측광 자료로부터 g vs (g-i) 색-등급도, 별들의 공간분포 및 측광학적인 비 구성원별들의 공간분포의 특징을 종합적으로 고려하여 4차원 구성원 확률을 얻었다. 구성원 확률을 고려한 유효 밀도 분포를 조사하여 밝은 별과 어두운 별의 반경에 따른 분포특징을 통해 질량 분리의 증거를 살펴보았으며, 성단 외곽 헤일로의 구조에 대해 고찰한다.Symbiotic stars and quasars exhibit prominent$H{\alpha}$ emission lines often accompanied with broad wings.$H{\alpha}$ emission nebulae in these objects are proposed to be optically thick to resonance scattering. The transfer of$H{\alpha}$ line photons are further complicated by the existence of another scattering channel leading to re-emission of$Ly{\beta}$ . In this work are develop a Monte Carlo code to simulate the transfer of$H{\alpha}$ line photons incorporating the scattering channel into$Ly{\beta}$ . We show various line profiles of$H{\alpha}$ and$Ly{\beta}$ emergent from our model nebulae. It is shown that temperature is a critical parameter which controls the ratio of emergent$Ly{\beta}$ flux to that of$H{\alpha}$ .Helium mass in the envelope is one of the most important properties in progenitors of type Ib/c supernovae (SNe Ib/c), since SN Ib/c progenitors are distinguished by the presence of He I lines. However, previous progenitor models do not reproduce the required He mass limit($M_{He}$ <$0.14M_{\odot}$ ) suggested by a spectroscopic analysis of SN Ib/c. In this work, we investigated the effect of overshooting on the evolution of pure helium stars, focusing on the final He mass in the envelope,$M_{He,f}$ . We used the MESA code to calculate single helium star models with the initial masses of$M_{init}=5{\sim}30M_{\odot}$ , Z=0.02, 0.04 and overshooting parameters of$f_{ov}=0{\sim}0.4$ . The final He mass$M_{He,f}$ decreases as$f_{ov}$ increases, due to larger burning core compared to weak overshooting models. Dependence of the final mass$M_{He,f}$ on overshooting is strongest for models with$M_{init}=7{\sim}10M_{\odot}$ , and this effect originates from accelerated mass loss during transition between WNE and WC/O phase. However,$M_{He,f}$ exceeds$0.27M_{\odot}$ for all models, which still doesn't meet the criteria of$M_{He}$ <$0.14M_{\odot}$ . This implies that mass loss during the post helium burning phase must be enhanced dramatically compared to what the standard models predict.The symbiotic star V1016 Cygni shows the Raman scattered O VI features at$6825{\AA}$ and$7088{\AA}$ . These are formed through inelastic scattering of O VI 1032, 1038 by atomic hydrogen. They exhibit characteristic double peak profiles with a stronger red peak, which is explained by the accretion flow around the white dwarf. In addition, the two Raman features have different profiles in such a way that the blue part of the Raman 7088 feature is relatively more suppressed than the Raman 6825 counterpart. We produced the Doppler maps of the two Raman features in order to trace the origin of the disparate profiles. We conclude that the profile difference is due to various O VI 1032 to O VI 1038 flux ratios in the accretion region. This is consistent with the picture where the slow stellar wind from the giant interacts with the accretion flow around the white dwarf.Jeong, Ueejeong;Chun, Moo-Young;Oh, Jae-Sok;Park, Chan;Yu, Young Sam;Oh, Heeyoung;Yuk, In-Soo;Kim, Kang-Min;Ko, Kyeong Yeon;Pavel, Michael;Jaffe, Daniel T. 91.1
IGRINS (the Immersion GRating INfrared Spectrometer) is a high resolution wide-band infrared spectrograph developed by the Korea Astronomy and Space Science Institute (KASI) and the University of Texas at Austin (UT). This spectrograph has H-band and K-band science cameras, both of which use Teledyne's$2.5{\mu}m$ cutoff$2k{\times}2k$ HgCdTe HAWAII-2RG CMOS science grade detectors. Teledyne's cryogenic SIDECAR ASIC boards and JADE2 USB interface cards were installed to control these detectors. We performed lab experiments and test observations to optimize and evaluate the detector systems of science cameras. In this presentation, we describe a process to optimize bias voltages and way to reduce pattern noise with reference pixel subtraction schemes. We also present measurements of the following properties under optimized settings of bias voltages at cryogenic temperature (70K): read noise, Fowler noise, dark current, and reference-level stability, full well depth, linearity and conversion gain.Oh, Jae Sok;Park, Chan;Kim, Kang-Min;Chun, Moo-Young;Yuk, In-Soo;Yu, Young Sam;Oh, Heeyoung;Jeong, Ueejeong;Lee, Hanshin;Jaffe, Daniel T. 91.2
A near infrared wide-band high resolution spectrograph, immersion grating infrared spectrometer (IGRINS) has been jointly developed by the Korea Astronomy and Space Science Institute and the University of Texas at Austin. The compact white-pupil design of the instrument optics includes five cryogenic flat mirrors including a slit mirror, an input fold mirror, a dichroic mirror, and H&K camera fold mirrors. In this study, we introduce the optomechanical mount designs of the five cryogenic mirrors. In order to meet the structural stability and thermal requirements of the mount models, we conducted the design work with the aid of 3-dimensional computer modeling and the finite element analysis (FEA) method. We also present the actual fabricated parts and assemblies of the mounts and mirrors as well as their CAD models.Lee, Hye-In;Pak, Soojong;Le, Huynh Anh N.;Kang, Wonseok;Mace, Gregory;Pavel, Michael;Jaffe, Daniel T.;Lee, Jae-Joon;Kim, Hwihyun;Jeong, Ueejeong;Chun, Moo-Young;Park, Chan;Yuk, In-Soo;Kim, Kangmin 92.1
In astronomical spectroscopy, stable auto-guiding and accurate target centering capabilities are critical to increase the achievement of high observation efficiency and sensitivity. We developed an instrument control software for the Immersion GRating INfrared Spectrograph (IGRINS), a high spectral resolution near-infrared slit spectrograph with (R=40,000). IGRINS is currently installed on the McDonald 2.7 m telescope in Texas, USA. We had successful commissioning observations in March, May, and July of 2014. The role of the IGRINS slit-viewing camera (SVC) is to move the target onto the slit, and to provide feedback about the tracking offsets for the auto-guiding. For a point source, we guide the telescope with the target on the slit. While for an extended source, we use another a guide star in the field offset from the slit. Since the slit blocks the center of the point spread function, it is challenging to fit the Gaussian function to guide and center the target on slit. We developed several center finding algorithms, e.g., 2D-Gaussian Fitting, 1D-Gaussian Fitting, and Center Balancing methods. In this presentation, we show the results of auto-guiding performances with these algorithms.Pak, Soojong;Lee, Hye-In;Le, Huynh Anh N.;Lee, Sungho;Chung, Aeree;Kaplan, Kyle;Jaffe, Daniel T. 92.2
NGC 6822 is a dwarf irregular galaxy in the Local Group. Unlike clouds in the Large Magellanic Cloud and the Small Magellanic Cloud, molecular clouds in NGC 6822 are not influenced by the Galactic tidal force. Therefore the star forming processes are only dictated by local conditions. Hubble V is the brightest of the several bright H II region complexes in NGC 6822. The core of Hubble V, surrounded by a molecular cloud complex, contains compact clusters of bright blue stars. During the commissioning runs of the new high-resolution near-infrared spectrometer, IGRINS (Immersion GRating near-INfrared Spectrometer), we observed Hubble V and detected many emission lines from the H II regions and from the photodissociation region at the interface between the ionized gas and the molecular cloud. In this presentation, we report preliminary results of the IGRINS observations. We discuss the implications of the observed lines ratios and kinematics for our understanding of the evolution of star forming molecular clouds.Le, Huynh Anh N.;Pak, Soojong;Lee, Hye-In;Lee, Jae-Joon;Nguyen-Luong, Quang;Kaplan, Kyle;Jaffe, Daniel T. 93.1
The reflection nebula NGC 7023 is a typical example of a photodissociation region (PDR), which consists of high density molecular gas that is exposed to an intense UV radiation field. The source of the UV photons in NGC 7023 is the young pre-main-sequence Be star HD 200755. We present our near-infrared high-resolution (R ~ 40,000) spectrum of NGC 7023, covering a region of$1{\times}15$ arcseconds, observed during the commissioning runs of IGRINS (Immersion GRating near-INfrared Spectrometer). The spectrum shows many strong narrow emission lines that arise from the molecular rovibrational transitions of H2. From the intensity ratios between these H2 lines, we investigate physical conditions within the PDR such as the temperature, density, and pressure. The high spectral resolution of IGRINS allows us to resolve the velocity field of the PDR. In addition, we compare the IGRINS spectrum to Cloudy PDR model.Planetary nebulae (PN) are the last stages of evolution of intermediate mass (1-8 Msolar) stars. Their shapes are thought to result from interactions between the present-day, fast (emerging white dwarf) and previously ejected, slow (red giant) stellar winds. The observation of young, bright PN, NGC7027 and BD+30 3639, was made on July 7, 2014 using the 2.7m Harlan J. Smith telescope at the McDonald Observatory. IGRINS with high spatial (0.27") and high spectral ($7.5km\;s^{-1}$ ) resolution will provide more nebular lines and excitation/abundances to constrain the morphology and kinematics of the Nebula and the PDRs. Combined with other archival data (X-ray, 2MASS, WISE, Spitzer, Herschel) for PN, high-resolution IR spectroscopy will yield insight into poorly understood aspects of PN morphologies and the late stages of binary star evolution.We have carried out IGRINS test observations during its May commissioning run. Our targets were composed of three Luminous Blue Variables (LBVs), one supernova remnant (SNR), and an unidentified stellar source emitting [Fe II] 1.644 um line. In the preliminary results, three LBVs MWC 314, P Cygni, and AFGL 2298 show different characteristics: the spectrum of MWC 314 which is known to be in a binary system clearly shows double-peak structures in hydrogen and iron lines, the P Cygni spectrum reveals the Brackett series of hydrogen emission lines with prominent P-Cygni profiles, and AFGL 2298 likely at its visual minimum phase shows rather different spectrum with relatively weak hydrogen lines. The SNR (G11.2-0.3) was to test the sensitivity of IGRINS for diffuse emission. We successfully detected a dozen H2 emission lines with a velocity width of ~13 km/s, which might indicate a C-shock origin. The unidentified stellar source was one of stellar/compact sources of unknown nature detected in the survey of the Galactic plane in [Fe II] 1.644 um emission line (http://gems0.kasi.re.kr/uwife/). Its spectrum is under investigation. We will present the spectra of test observations and will discuss their scientific significance.Lee, Jae-Joon;Hwang, Narae;Park, Byeong-Gon;Yuk, In-Soo;Park, Chan;Le, Huynh Anh N.;Pak, Soojong 94.2
After successful commissioning observations, IGRINS will soon begin its normal scientific operations on the 2.7m Harlan J. Smith telescope at the McDonald Observatory. We will present a working version of the IGRINS operation plan. A fraction of IGRINS guaranteed time will be devoted to a selection of strategic programs with legacy values, whereas the rest of the time will be used for normal programs. We will also describe the current status of the IGRINS data reduction pipeline package and its future development plan.The rotation of asteroids can help reveal not only the fundamental characteristics of asteroids but also the origin and evolution of our Solar System. From the photometric observations for NEA 162173 (1999 JU3) and Maria family asteroids using 0.5 m- to 2 m- class telescopes at 10 observatories in the northern hemisphere, I obtained a total of 260 lightcurves for 97 asteroids and derived synodic rotational periods for 51 objects, including newly obtained periods of 34 asteroids. For the sake of efficiency, I developed an observation scheduler, SMART (Scheduler for Measuring Asteroid RoTation) and a photometric analysis software subsystem, ASAP (Asteroid Spin Analysis Package). Based on the lightcurve analysis of NEA 162173 (1999 JU3) and Maria family asteroids, 1) I present the rotational and observational characteristics of 1999 JU3 and provided the Hayabusa-2 Science team with the information on pole orientations, 2) I investigated correlations among rotational periods, amplitudes of lightcurves, and sizes, and conclude that the rotational properties of old-type family asteroids have been changed considerably by the YORP effect. 3) Finally, I found the Yarkovsky footprints on the Maria asteroid family and estimated that approximately 37 to 75 Maria family asteroids larger than 1 km have entered the near-Earth space every 100 Myr. This study should reveal the collisional history and transport route of the members from the resonance region to the near Earth space, for the first time.Using solar occultation data obtained by Cassini/Visual Infrared Mapping Spectrometer (VIMS), we were able to retrieve the 1 - 5 mm optical-depth spectra of the Titanian haze, for which only selected wavelength and altitudinal ranges were previously analyzed. We found that the gross 1 - 5 mm shapes of the retrieved haze spectra are significantly different from the spectra of tholin samples in the literature. We also derived the vertical variation of the spectral structure of the$3.3-3.4{\mu}m$ absorption feature of the Titan haze from the VIMS data recorded between 250 and 700 km altitude. We found a marked change between 480 and 580 km in the relative amplitudes of the 3.33 and$3.38{\mu}m$ features which are characteristic of aromatic (double C=Cchains or rings) or aliphatic (single C-C chains) structural groups, respectively. Dicussions on this spectral and altitudinal variation will be presented.We clarify the dynamics connecting a solar flare and a coronal mass ejection (CME) based on the results of a magnetohydrodynamic (MHD) simulation starting from a nonlinear force-free field (NLFFF) in Inoue et al. 2014. In previous studies, many authors proposed numerous candidates for triggering processes of a solar flare and the associated CME. Among them, the tether-cutting reconnection or the torus instability has been supported by recent simulations and observations. On the other hand, our MHD simulation in accordance with more realistic situations show that highly twisted field lines are first produced through a tether-cutting reconnection between the twisted field lines in the NLFFF, and then the newly formed, strongly twisted field erupts away from the solar surface because of a loss of equilibrium. This dynamics corresponds to the onset of a solar flare. Furthermore we have found that the strongly twisted erupting field reconnect with the weakly twisted ambient field during the eruption, creating a large flux tube, and then it rises over a critical height of the torus instability to trigger a CME. From these results, we conclude that the coupled process of tether-cutting reconnection and torus instability is important in the flare-CME relationship.In this paper, we study the stability and dynamics of a magnetic field producing the M6.6 class solar flare taking place in NOAA active region (AR) 11158 on 2011 February 13th. Toriumi et. al. (2013) recently suggest that a fine scale magnetic structure on the photosphere gives a major possibility to produce the M6.6 class flare. On the other hand, they don't discuss the torus instability as a plausible mechanism even though Zhao et. al. (2014) and Janvier et. al. (2014) suspect it as the trigger mechanism of X2.2 class flare taking place later in the same AR. We are the first to investigate the stability of a nonlinear force-free field (NLFFF) prior to the M6.6 class flare against the torus instability by using analytical and numerical approaches. Consequently, we found that our NLFFF is quite stable against small perturbation. This result supports that the flare is triggered by the photospheric motion suggested by Toriumi et. al. (2013). We further perform another MHD simulation with an anomalous resistivity using the NLFFF as an initial condition. As a result, we found the eruption of strongly twisted lines. We compare our simulation results with observations and discuss relevant dynamics in detail.Lee, Jung-Kyu;Lee, Hyojeong;Baek, Seul-Min;Kim, Khan-Hyuck;Jin, Ho;Hemingway, Doug;Garrick-Bethell, Ian 99.1
달은 global magnetic fields가 존재하지 않으나, 달 표면에 국지적으로 자기장이 존재하며 이러한 현상의 원인은 계속 연구중이다. 달의 자기이상 현상이 나타나는 지역 중 광학적으로 밝고 어두운 패턴이 관측되는 지역을 Swirl이라한다. Mare Crisium ($17.18^{\circ}N$ ,$59.1^{\circ}E$ )은 표면에 2개의 자기이상 지역과 광학적으로 밝은 지역들이 존재하지만, Swirl로 잘 알려진 Reiner Gamma와 같은 지역의 광학적 밝기와 패턴의 차이가 있다. 이를 위해 본 연구에서는 Lunar Prospector (LP) 위성의 magnetometer (MAG) 자료를 이용하여 자기장 분포에 관한 연구 및 Clementine 위성의 UV/VIS 영상자료를 이용하여 광학적 특성 연구를 진행하였다. LP의 MAG 자료는 Mare Cirisium지역의 22.3 km 고도에서 관측된 744개의 자료를 활용하였으며, Clementine의 영상자료는 750 nm, 950 nm의 반사도에 따른 Optical Maturity (OMAT)를 활용하였다. Mare Crisium의 북쪽지역은 자기이상 현상과 OMAT의 고유특성이 동시에 나타나며 이는 swirl과 유사하다. 특히, Mare Cirisum서쪽에 있는 Proclus crater 잔해 일부가 Mare Crisium의 북쪽지역까지 퍼져있어 이와 관련하여 자기장 존재여부에 따른 광학적 특성의 차이점을 조사하였다. 본 논문에서는 Mare Crisium 지역의 Swirl 진위여부를 추론하며, 본 논문에서 이용한 방법의 유용성에 대하여 검증하고자 한다.We investigate how a solar eruption occurs in an environment where a solar wind exists during a pre-eruptive phase. To understand it, we have performed three-dimensional simulations based on a zero-beta magnetohydrodynamic (MHD) equations in various ways to drive an eruption with a solar wind. A pre-eruptive state is derived by applying a nonlinear force-free reconstruction method to a flux emergence full MHD simulation. We discuss what is the most appropriate way to drive a solar wind-related eruption.Park, Byeong-Gon;Yuk, In-Soo;Lee, Jae-Joon;Yoon, Yang-Noh;Hwang, Narae;Park, Chan;Kim, Jihun 100.1
Korea Astronomy and Space Science Institute (KASI) has been participating in the Giant Magellan Telescope (GMT) project since 2009. In 2014, GMT project has passed its important milestones toward construction of the telescope and observatory facilities. We will report the recent achievements and current status of the project in this contribution.The DOTIFS is a new multi-object Integral Field Spectrograph (IFS) planned to be designed and built by the Inter-University Center for Astronomy and Astrophysics, Pune, India, (IUCAA) for cassegrain side port of the 3.6m Devasthal Optical Telescope (DOT) being constructed by the Aryabhatta Research Institute of Observational Sciences, Nainital. (ARIES) It is a multi-integral field unit (IFU) spectrograph which has 370-740nm wavelength coverage with spectral resolution R~1200-2400. Sixteen IFUs with microlens arrays and fibers can be deployed on 8 arcmin field. Each IFU has$8.7^{{\prime}{\prime}}{\times}7.4^{{\prime}{\prime}}$ field of view with 144 spaxel elements. 2304 fibers coming from IFUs are dispersed by eight identical spectrographs with all refractive and all spherical optics. In this work, we show optical design of the DOTIFS spectrograph. Expected performance and result of tolerance and thermal analysis are also shown. The optics is comprised of f=520mm collimator, broadband filter, dispersion element and f=195mm camera. Pupil size is determined as 130mm from spectral resolution and budget requirements. To maintain good transmission down to 370nm, calcium fluoride elements and high transmission optical glasses have been used. Volume Phase Holographic grating is selected as a dispersion element to maximize the grating efficiency and to minimize the size of the optics. Detailed optics design report had been documented. The design was finalized through optical design review and now ready for order optics.The fluctuation of VLBI visibility phase can be occurred, predominantly caused by the irregular distribution and motion of water vapor in the atmosphere at high frequencies (>1GHz). This radio-seeing effect shows up on filled-aperture telescopes as an anomalous refraction (AR). This can be shown as if the antenna pointing-offset increases, in other words the apparent displacement of radio sources from its nominal position happens. We carried out the single-dish observations on KVN sites in order to check the effect of AR from 2010 to 2014. Orion KL, U Her, and R Leo were observed with 1second sampling time at 22.235GHz and 43.122GHz simultaneously. Each source was observed with the tracking mode for 30 minutes per a source. We analyzed the structure function, power spectrum and Allan variance of the data according to a day and a night, a season and observatories. Finally, we can infer that the AR effect depends on the atmospheric environment, especially tropospheric turbulence.적외선 파장 대역에서 관측되는 우주배경복사의 요동은 초기 우주가 재이온화되는 시기에 존재하였던 우주 최초의 별 또는 은하에서 기원한다고 믿어진다. 적외선우주배경복사 관측을 위해서는 배경의 잡음이 되는 별, 은하, 황도광등을 제거하고 희미한 배경을 검출해야 하므로 광시야, 고감도로 광학에서 근적외선까지 다파장으로 관측하는 기능이 필요하다. CIBER2는 이러한 적외선우주배경복사 관측을 위해 개발되고 있는 NASA 사운딩로켓 탑재용 적외선카메라 시스템이다. 2009년부터 2013년까지 4차례에 걸쳐 성공적으로 발사된 CIBER를 업그레이드한 관측기기로써 한국 KASI, 미국 Caltech, 일본 ISAS가 공동으로 개발하고 있다. CIBER2는 28.5cm의 주경에 광분배기를 사용하여 3대의 카메라가 장착되는 형상을 이루고 있으며 각 카메라에는$2K{\times}2K$ H2RG 검출기 위에 2개의 밴드 필터를 부착하여 0.6 - 2.1 um의 파장 대역을 6개의 구간으로 나누어 관측한다. 각 밴드의 시야각은$1.1{\times}2.2$ 도이다. CIBER2는 현재 최종 설계를 마치고 각 서브시스템 별 제작 단계에 있으며, 조립 및 시험을 거쳐 2015년에 미국 화이트샌드 미사일기지에서 발사될 예정이다.Kang, Yong-Woo;Song, Min-Gyu;Je, Do-Heung;Wi, Seog-Oh;Byun, Do-Young;Jung, Taehyun;Oh, Chungsik;Nam, Wook-Won 104.1
한국우주전파관측망(KVN, Korea VLBI Network)의 우주전파수신시스템(22GHz, 43GHz, 86GHz, 129GHz의 4파수 동시관측 시스템)으로부터 수신된 전파신호를 디지털 신호로 바꾸어 주는 장치인 초고속 샘플러의 국산화와 성능 향상을 위하여, 우리는 1GHz 샘플링을 할 수 있는 전파관측 자료의 샘플링 장치를 설계, 제작하였다. GHz 샘플링 기본 기술 확보와 독자 개발을 위하여 제작된 1GHz 샘플러를 KVN울산전파천문대에 설치하여 관측 시험한 결과, 연구 관측에 적용할 수 있음을 보여 주었다. 한편, 광대역 관측과 e-VLBI 구현을 위하여 샘플러에서 직접 첨단망으로 VDIF(VLBI Data Interchange Format, VLBI 자료전송 규격)의 자료를 보낼 수 있는 차세대 4GHz 샘플러를 개발 중에 있다. 이번 발표에서는 1GHz 샘플러에 대한 개발 내용과 관측 결과 및 향후 계획을 소개한다.The RGB Bayer filter system consists of mosaic R, G, and B filters on the grid of photo sensors with which typical commercial DSLR (Digital Single Lens Reflex) cameras and CCD/CMOS cameras are taken. Many unique astronomical data taken with RGB Bayer filter systems are available, including transient objects, e.g., supernovae, variable stars, and solar system bodies. The utilization of such data in scientific research strongly requires reliable photometry transformation methods. In this work, we develop a series of formulae to derive magnitudes in the Johnson-Cousins BVR filter system from those in the RGB Bayer filter system.The study on linear correlation between auxiliary channels in LIGO data has been performed by using Pearson's correlation coefficient, generating a correlation map.Song, Min-Gyu;Wagner, Jan;Yeom, Jae-Hwan;Jung, Tae-Hyun;Kang, Yong-Woo;Byun, Do-Young;Kim, Jong-Soo;Kim, Hyo-Ryung 105.2
Mark6는 최대 16Gbps의 데이터 입출력을 지원하는 차세대 기록 시스템으로서 올 하반기 내에 KVN의 관측 연구에 활용되기 위해 현재 기록 실험이 진행 중에 있다. VDIF(VLBI Data Interchage Format) 기반의 Mark6가 KVN 각 사이트에서 실제 관측에 활용되기 위해서는 FILA10G, VOA(VSI Optical Adapter) 등의 VSI-VDIF 컨버터가 수반되어야 하며 샘플러, DAS(Data Acquisition System) 등 내부적으로도 많은 시스템 변화가 필요하다. 본 발표에서는 기본 사양, 동작 원리 등 Mark6에 대한 간단한 소개를 시작으로 데이터 기록 실험 결과에 대해 설명하고자 한다. 나아가 이를 기반으로 향후 KVN의 광대역 관측 수행을 위한 Mark6의 활용 방안에 대해 살펴보고자 한다.Oh, Sang Hoon;Kim, Kyungmin;Harry, Ian W.;Hodge, Kari A.;Kim, Young-Min;Lee, Chang-Hwan;Lee, Hyun Kyu;Oh, John J.;Son, Edwin J. 107.1
We apply a machine learning algorithm, artificial neural network, to the search for gravitational-wave signals associated with short gamma-ray bursts. The multi-dimensional samples consisting of data corresponding to the statistical and physical quantities from the coherent search pipeline are fed into the artificial neural network to distinguish simulated gravitational-wave signals from background noise artifacts. Our result shows that the data classification efficiency at a fixed false alarm probability is improved by the artificial neural network in comparison to the conventional detection statistic. Therefore, this algorithm increases the distance at which a gravitational-wave signal could be observed in coincidence with a gamma-ray burst. We also evaluate the gravitational-wave data within a few seconds of the selected short gamma-ray bursts' event times using the trained networks and obtain the false alarm probability. We suggest that artificial neural network can be a complementary method to the conventional detection statistic for identifying gravitational-wave signals related to the short gamma-ray bursts.The study on non-linear correlation between auxiliary channels in LIGO data has been performed by using mutual information coefficient, generating a correlation map.Lee, Dukhang;Moon, Bongkon;Park, Sung-Joon;Jeong, Woong-Seob;Suh, Jeong-Ki;Pyo, Jeonghyun;Park, Youngsik;Lee, Dae-Hee;Kim, Il-Joong;Park, Won-Kee;Ko, Kyeongyeon;Kim, Min-Gyu;Nam, Uk-Won;Park, Chan;Shin, Goo-Whan;Matsumoto, Toshio;Han, Wonyong 108.1
Near-infrared Imaging Spectrometer for Star formation history (NISS), one of the main payloads of NEXTSat-1, is being developed by Korea Astronomy & Space Science Institute (KASI). Since NISS adopts an infrared reflecting optical system, its performance is highly sensitive to changes in system temperature. Therefore, it is important to figure out the temperature through thermal analysis and cooling tests in order to optimize the optical system design. We conducted thermal analysis of NISS for the recently updated model, and obtained steady state temperature of the optical system for two cases of satellite attitude: about 190 K for the Normal case and about 210 K for the Hot case. In this paper, we present thermal design of NISS and the preliminary thermal analysis results.Lee, Hyojeong;Lee, Jung-Kyu;Baek, Seul-Min;Jin, Ho;Kim, Kwan-Hyuk;Song, Young-Joo;Hemingway, Doug;Garrick-Bethell, Ian 108.2
과거 달 탐사 미션으로 달에는 global magnetic fields는 존재하지 않고 표면에 국부적으로 자기장이 존재함이 확인되었다. 그러나 이렇게 측정된 자기장 데이터는 일정 고도 (> 20 km) 이상에서 측정되었기 때문에, 지표에 비해 그 세기가 매우 약해 자기장의 형태와 분포를 연구하는데 한계가 있다. 보다 자세한 연구를 위해서는 표면에서부터 다양한 고도에 이르는 위치에서 측정된 자기장 데이터가 필요하며, 이는 달 표토의 자화나 Swirl 형성 메커니즘을 이해하는데 중요한 정보이다. 따라서 본 연구에서는 큐브위성을 이용하여 저궤도부터 지표까지의 자기장을 측정하는 방안을 소개한다. 큐브위성은 달 궤도 모선에서 사출되어 자기이상 지역 표면에 충돌하는 임무를 가진다. 자력계는 모선과 큐브위성에 각각 탑재되어 자기장을 측정하며, 모선으로 부터 사출된 큐브위성은 충돌 직전까지 자기장을 측정하고 모선에 습득한 데이터를 실시간으로 전송한다. 이렇게 측정된 자기장 데이터는 모선의 궤도부터 표면에 이르기까지 여러 고도에서 측정되었기 때문에 자기이상 지역의 자기장 구조를 파악하는데 중요한 자료로 활용할 수 있다. 이에 본 연구에서는 달의 자기이상 지역과 큐브위성 임무 설계에 대하여 기술하였다.다이아몬드 선삭 기계(DTM)를 이용한 렌즈 및 반사경 가공은 제작시간 단축 및 비용 절감의 장점을 가지고 있다. 그러나 알루미늄과 같은 무른 금속을 가공하여 반사경을 제작하는 경우에는 반사경 표면에 가공오차가 발생한다. 오차는 크기에 따라 고주파 오차(High Frequency Error, HFE), 중주파 오차(Mid Frequency Error, MFE), 저주파 오차(Low Frequency Error, LFE)로 분류 할 수 있다. LFE는 가공한 반사경 표면이 설계된 형상과 얼마나 다른지를 표현하는 값으로 광학 수차와 같이 해상도를 저하시킨다. MFE는 반사경 표면에 수십 마이크로미터 크기로 나타난다. 회전하는 반사경 시료에 다이아몬드 툴의 홈이 동심원으로 생기면서 회절격자와 같이 회절 및 간섭 현상을 만든다. HFE는 표면의 거친 정도를 나타내며 반사율과 관련되고 수 나노미터 크기로 나타난다. 본 연구에서는 광학 레이저를 사용하여 MFE가 광학 성능에 미치는 영향을 분석하였다. 유리 반사경과 MFE를 제거한 반사경, 제거하지 않은 반사경에 대하여 실험을 진행하였다. 본 실험 결과는 반사경 가공 표면을 평가할 수 있는 유용한 자료가 될 것이다.Chung, HyunSoo;Moon, Jun-Cheol;Yu, Dai-Hyuk;Je, Do-Heung;Jo, Jung-Hyun;Roh, Duk-Gyoo;Oh, Se-Jin;Sohn, Bong-Won;Lee, SangSung;Kim, Hyo-Ryung 109.2
세계전파통신회의 (WRC; World Radiocommunication Conference)회의는 국제전기통신연합 (ITU)에서 규정하는 국제 전파법 제개정을 위해, 3-4년 간격으로 개최되는 전파통신 관련 최고회의이다. WRC-15회의는 2015년 11월 2일 - 11월 27일에 걸쳐 스위스 제네바에서 개최될 예정이며, 과학업무 관련 의제들은 다음과 같다. 즉, 7145-7250MHz 대역의 지구탐사위성(지구대우주)업무의 1순위 분배연구, 8,700~10,500MHz 대역의 지구탐사위성업무의 신규 SAR용 대역(연속 1.2GHz) 분배방안 연구, 우주선 근거리통신용 410-420MHz 대역 규제 철폐 관련 검토, 윤초삭제와 관련된 세계협정시(UTC) 개정 또는 대처방안 연구가 있다. 그리고 모바일 광대역 응용 실현을 위한 이동통신업무 추가 분배 및 IMT 추가 지정 연구, 나노 위성 및 피코 위성 규제 관련 연구들이 있다. 따라서 본 발표에서는 WRC-15회의의 과학업무 의제에 관한 사전 연구결과를 소개하고, 국내전파망원경 운용에 영향을 미칠 수 있는 주파수 대역 및 윤초 삭제 등과 관련된 주요 이슈에 대한 향후 대응책 검토를 하고자 한다.The optics of Space telescope is one of the major parts of space mission used for imaging observation of astronomical targets and the Earth. These kinds of space mission have a bulky and complex opto-mechanics with a long optical tube, but there are attempts have been made to observe a target with a small satellite in many ways. In this paper, we describe an optical design of a reflecting telescope for use in a CubeSat mission. For this design, we adopt the off-axis segmented method of astronomical observation techniques based on the Ritchey-Chr$\acute{e}$ tien type telescope. The primary mirror shape is a rectangle with dimensions of$8cm{\times}8cm$ , and a secondary mirror has dimensions of$2.4cm{\times}4.1cm$ . The focal ratio is 3 which can obtain a$0.3{\times}0.2$ degree diagonal angle in a$1280{\times}800$ CMOS color image sensor with a pixel size of$3{\mu}m{\times}3{\mu}m$ . This optical design can capture a${\sim}4km{\times}{\sim}2.3km$ area of the earth's surface at 700 km altitude operation. Based on this conceptual design, we will keep trying to study more for astronomical observation with Attitude control system.Han, Inwoo;Jang, Jeonggyun;Jang, Biho;Kim, Gwangdong;Yim, In Sung;Jeong, Gwanghui;Choi, Dongsoo;Cho, Kyujung;Kim, Kyoung-Rock;Kang, Hyosung 110.2
본 연구는 중소기업청 공고 중소기업기술개발 지원사업 과제로 한국천문연구원(주관기관)과 (주)져스텍(공동개발기관)이 공동으로 수행하였다. 지원사업 과제는 출연연과 중소기업이 기술개발 및 이전을 하여 개발된 망원경을 상용화하는 것이 목표이다. 망원경에서 가대부는 (주)져스텍에서, 경통부는 한국천문연구원에서 각각 담당하여 제작 하였다. 시스템을 설계하고 가대부, 경통부, 디로테이터 등을 조립,정렬하였고, 제작품을 시험한 결과, 초기 개발 목표치에 달성 하였다. 망원경을 제작하면서 한국천문연구원에서 가지고 있던 기계부, 전자부, 프로그램에 대한 기술을 (주)져스텍에 이전하여 독자적으로 제작이 가능하게 하였다. 본 과제를 수행하면서 국립 고흥청소년우주체험센터 망원경을 제작하게 되어 가격경쟁력을 갖는 망원경 제작이 가능하다는 것을 입증 하였다. 향후 광학계가 완성되고 원하는 성과를 내면 중형망원경을 개발하는데 많은 도움이 될 것이다.KVN은 현재 연간 3000시간 이상의 VLBI 관측 시간을 운영하는 안정적인 운영단계에 들어섰다. 또한 일본의 VLBI 관측망인 VERA와 연결한 KaVA (KVN and VERA Array)도 한일상관센터의 운영시작과 더불어 연간 1000 시간의 관측 운영을 하고 있으며 KaVA를 이용한 연구 성과가 나오기 시작하였다. KVN은 다파장 Astrometry를 위해 다파장 P-Cal 시스템을 개발하고 있으며 관측 감도를 높이기 위해 8Gbps 운영을 준비하고 있다. KVN의 운영 및 시스템 개선 계획, 국제 협력 내용 등을 소개한다.We propose simultaneous monitoring observations of 22 GHz$H_2O$ and 43/86/129 GHz SiO masers toward ~15 evolved stars in order to investigate spatial structure and dynamical effect from SiO to$H_2O$ maser regions including mass-loss process and development of asymmetry in circumstellar envelopes. We also aim at investigating mutual association and difference between SiO and$H_2O$ masers for establishing SiO and$H_2O$ maser models coupled to hydrodynamical model of circumstellar envelope. In addition, the correlation and difference of SiO maser properties among J=1-0, J=2-1, and J=3-2 transition masers are traced according to different type of stars for constraining SiO pumping models. These scientific goals and target sources were determined based on KVN single dish and VLBI feasibility test observations at 4 bands. As a total observing time of every 2 month monitoring, about 90 and 360 hours (in average per year) are required for single dish and VLBI observations, respectively. From the 2014B observing season, these monitoring observations will be derived as one of KVN key science programs.Lee, Sang-Sung;Kang, Sincheol;Han, Myoung-Hee;Algaba-Marcos, Juan-Carlos;Byun, Do-Young;Kim, Jeong-Sook;Kim, Soon-Wook;Kino, Motoki;Trippe, Sascha;Wajima, Kiyoaki;Miyazaki, Atsushi 113.1
We propose a three-year Key Science Program (KSP) consisting of VLBI monitoring observations and single dish (SD) rapid response observations (RRO). The VLBI monitoring observations are comprised of ten 24-hr observations per year (every month) of about 30 gamma-ray brigt active galactic nuclei (AGNs) with Korea VLBI Network (KVN) at 22, 43, 86, and 129 GHz. The SD RROs may consist of twelve 7-hr observations per source (every week for 3 months after triggering) of gamma-ray flaring sources with two KVN SD telescopes at 22, 43, and 86 GHz in dual polarization. We expect one or two sources per year for the SD RROs. Gamma-ray flares of AGNs are known to be occured in innermost regions of relativistic jets which radiate in whole ranges of electromagnetic spectra due to synchrotron radiation, syschrotron self absorption, inverse-compton scttering, doppler boosting etc. Possible explanations of the gamma-ray flares in AGNs are a) shocks-in-jets propagating within jet flow and b) bending of the whole jets. For both cases, we should expect changes in polarization, luminosity, particle distribution, and structures of jets at mas-scale. The multifrequency simultaneous VLBI/SD observations with KVN are the best tool for detecting such changes correlated with gamma-ray flares. This KSP proposal aims to answer the fundamental questions about the basic nature of the flares of AGNs.Methanol masers are divided into two classes, I and II. Class II methanol masers trace the disk-outflow systems of massive young stellar objects (YSOs), while class I methanol masers appear to trace the interaction regions of outflows with the ambient molecular gas. Class II masers have been extensively studied by single dishes, connected arrays, and VLBIs. Meanwhile, class I masers have been much less studied. They have not been detected by any VLBI facility. Thus they have been believed to have more extended structures than class II masers. We made fringe surveys of 44GHz class I methanol maser emission towards more than 150 massive YSOs with flux densities >10 Jy using the Korean VLBI Network (KVN), and detected fringes in ~10% of the sources. We performed follow-up imaging observations of the detected maser sources with KVN and KVN+VERA (KaVA). The observations aim to investigate the distribution and kinematics of 44GHz methanol maser features in each source at milli-arcsecond resolutions, and to understand what they trace. In this talk we will present the fringe survey and imaging results and our plans for further studies. Additionally, we will also introduce the preliminary results of single-dish polarization observations of water and class I methanol masers.Korea officially joined the ALMA (Atacama Large Millimeter/submillimeter Array) project on August 17, 2014. Korea was allowed to apply for the Cycle 2 call-for-proposal before joining the project. Korea submitted 17 proposals, and 4 of them were selected as high-priority. The fund of an 11-year Korean ALMA project in the KASI (Korea Astronomy and Space Science Institute) was approved. The project team formulated an ARC (ALMA Regional Center) node at the KASI and already started its supporting activities for the Korean Astronomical Society. The team also set up a future development plan for ASTE (Atacama Submillimeter Telescope Experiment) and ALMA. A couple of engineers are now doing concept design of a multi-beam receiver system for the ASTE, Because of the ALMA participation, Korea could also access open-use time of ASTE and Mopra telescopes organized by Japan. As of this writing, EACOA (East Asia Core Observatories Association) is now under discussion on making an organization called "East Asian Observatory" and the possible operation of JCMT (James Clerk Maxwell Telescope). I will briefly mention the future prospect of these activities.As Korean engineering contribution to ALMA enhancement, development of focal plane arrays(FPAs) for the total power array in ALMA compact array has been projected mainly to increase mapping speed in interferometric multi-pointing observation(mosaicking). To tackle engineering issues expected in order to be compatible with the existing ALMA receivers, we plan to develop a prototype 300-500 GHz heterodyne FPA system including a software spectrometer using GPU clusters for ASTE(Atacama Submillimeter Telescope Experiment) telescope by 2017."Circumstellar disks, exoplanets and the solar system" is the one of ALMA proposal categories, which is closely related to the one of the fundamental questions in astrophysics, " when, where, and how planets form". I will review the Cycle-0/1 observational results of this topic, which had only 16/32 antennas and the maximum angular resolutions of 0.45/0.16 arcsec at 345GHz at that time. Eventually, ALMA equipped with 66 antennas and 0.01 arcsec angular resolution will allow us to study details of the circumstellar disks with the 1AU resolution at the distance of 100pc.Astrochemistry is a tool to understand the physical processes occurring in the interstellar medium in a variety of astrophysical environments. Many ALMA sciences are utilizing our knowledge of astrochemistry, which has grown explosively in recent years thanks to sensitive observations and laboratory work. We will review the ALMA sciences employing astrochemistry and discuss how astrochemistry can serve to answer some unique astrophysical questions.Stars create and expel new chemical elements and dust at the end of the stellar life cycle. Therefore, understanding the evolved stars, their mass loss process, and the conditions of the returning material to be mixed with the surrounding interstellar medium is an important step toward studies on the new generation of stars as well as the evolution of cosmic elements in galactic scale. I will review the first results from the ALMA Early Science on the evolved stars and direct future works.As the most sensitive radio interferometer ever operated in millimeter/submillimeter, the ALMA has opened a new window on extragalactic astronomy. Its superior resolution and sensitivity allow the community to study the gas kinematics of distant galaxies as well as the molecular gas properties of nearby galaxies in GMC scale, already in its early commissioning stage. Also the ALMA provides a great tool to probe the dust contents of extragalactic sources at all redshifts, which is important in understanding of galaxy formation and evolution history over cosmic time. In this presentation, I will review the ALMA capabilities with the emphasis on the extragalactic science. I will also revisit some highlights from the early science and discuss future perspectives.We present the scanned digital images and their preliminary analysis results of objective-prism plates taken with the Michigan Curtis Schmidt telescope at Cerro Tololo Inter-American Observatory. In order to separate an individual spectrum of a star, it should be required to identify each field star in the plate. Using the PPM(Position and Proper Motion) catalog, we are verifying which star corresponds to the spectrum in a plate. In addition to this, we plan to devise the method for wavelength calibration in each spectrum. Finally we will make them for public use, not only for professional astronomers but also for high school and college students for encouraging them to be interested in the astronomy, especially astronomical spectroscopy and stellar astronomy.Many astrophysical phenomena involve processes of magnetohydrodynamics (MHD) and relativistic magnetohydrodynamics (RMHD). A number of numerical schemes have been developed to solve the equations of ideal MHD and RMHD. Recent codes are based on upwind schemes which solve hyperbolic systems of equations following the characteristics of the systems. Upwind schemes stand out by their robustness, clarity of the underlying physical model, and ability of achieving high resolution. We present MHD and RMHD codes based on the total variation diminishing (TVD) and weighted essentially non-oscillatory (WENO) schemes, which are second and higher order accurate extensions of upwind schemes. We demonstrate the ability and limitation of codes based on upwind schemes through a series of tests.Kim, Jihun;Kim, Young-Soo;Song, Je Heon;Cho, Myung;Park, Won Hyun;Yang, Ho-Soon;Lee, Joohyung;Kim, Ho-Sang;Lee, Chanhee;Lee, Won Gi;Kim, Kyung Il;Lee, Kyoung-Don;Park, Byeong-Gon 120.1
Fast-steering Secondary Mirror prototype (FSMP) of the Giant Magellan Telescope (GMT) has been developed by the consortium consisting of institutes in Korea and the US. In 2014 we are finalizing the FSMP project as combining two sub-systems, the mirror fabricated by Korea Research Institute of Standards and Science (KRISS) and the mirror cell with tip-tilt controlling system developed by Institute for Advanced Engineering (IAE), in the KRISS facility. In the assembly process we will identify potential difficulties or problems for the process, such that this process can be reflected to the further development of the FSM for GMT. In the presentation, we present how the assembly process can be carried out in safety.Shin, La El;Yoon, Ji Eon;Ahn, Jae Hyung;Choi, Won Seok;Choi, Joon Young;Kim, Jae Jin;Kim, Chol U;Lee, Sang Hyun 120.2
본 연구에서는 2011년에 설립된 부산과학고등학교 별샘천문대에 있는 32인치 반사망원경을 비롯한 여러 천체망원경들을 간단히 소개하고 관측을 통해 성능을 분석하여 향후 교육과 연구에 활용할 수 있는 기초 자료를 제공하고자 한다. 관측기기들의 기계적인 특성을 분석하기 위해 가대의 추적 특성과 정밀도, 지향특성 등을 조사한다. BVI 표준성 관측을 통한 표준계 변환 결과를 제시하고, 한계등급에 대해 고찰한다. 이를 통해 32인치 주망원경과 기타 보조 망원경 및 교육용 기자재를 활용하여 관측할 수 있는 주제를 모색하고 그 한계를 제시한다.Lee, Gwang-Ho;Kim, Suk;Bae, Hyun-Jin;Kang, Yijung;Kim, Minjin;Kim, Eunbin;Lee, Youngdae;Lee, Yunhee;Chung, Chul;Kim, Minbae;Bang, Taeyang;Sohn, Jubee;Lee, Jaehyun 121.1
2014년 7월 23일부터 25일까지 전라북도 무주에서 제 1회 대학원생 외부은하 워크샵 "We Love Galaxies"를 개최하였습니다. 초청연사 박사 연구원 2명을 포함, 8개 대학 및 기관에서 총 27명이 참석한 이번 워크샵은 외부은하를 연구하는 대학원생들이 서로의 연구를 이해하고, 현대 외부은하 천문학의 문제들을 공유하며, 자유로운 토의를 통해 더 큰 우주를 그릴 수 있는 기회를 마련하는 것을 목적으로 하였습니다. 총 9개의 세션 27개의 구두발표를 통해 은하의 다파장 특성, 형태 분류 및 내부 구조, 주변 환경과 은하 특성과의 관계, 은하 병합 및 진화, 활동성 은하핵 등의 다양한 주제들을 다루었습니다. 본 포스터를 통해 "We Love Galaxies"의 결과 및 성과, 이후 계획에 대해 소개하고자 합니다.Lee, Min-Uk;Kim, Min Ji;Park, Minki;Choi, Jee Won;Jo, Hyungyu;Son, Jeong Woo;Nam, Sung Woo;Park, Jae Han;Lee, Sang Hyun 121.2
2013년 설립된 부산일과학고등학교 천문대는 교육 및 연구목적으로 12인치 굴절망원경, 16인치 반사망원경 및 다수의 소형망원경들이 설치되어 있다. 우리는 본격적인 관측, 연구를 수행하기에 앞서 망원경의 다양한 성능을 검증하여 향후 연구 활동에 기초자료로 사용하고자 한다. 본 연구에서는 망원경에 4K CCD 및 DSLR을 장착하여 얻은 관측 영상으로부터 망원경의 추적 특성, 지향정밀도, 광학적 특성을 고찰하고, Landolt (1992)의 표준성을 이용한 BV측광을 수행하여 표준계변환의 특성을 조사하였다. 또한 산개성단의 BV관측을 통해 한계등급을 측정하였다. 이 연구결과로부터 향후 부산일과학고등학교 천문대에서 수행할 수 있는 적합한 관측 연구의 방향을 제시한다.Lee, Joon Hyeop;Hwang, Narae;Park, Byeong-Gon;Kim, Yee Jin;Lee, Jae-Joon;Lee, Ho-Gyu;Kim, Minjin 122.1
다가오는 거대마젤란망원경 (GMT) 시대를 이끌어갈 신진 연구자들의 연구역량 증진을 위해, 2014년 8월 25일부터 29일까지 4박5일에 걸쳐 경상북도 경주시 대명리조트에서 제4회 거대마젤란망원경 여름학교를 개최하였다. 총 40명이 학생으로서 참가한 이번 여름학교에서는 다음과 같은 두 가지 새로운 프로그램이 시도되었다. (1) 관측천문학의 기초, 우리은하 천문학의 기초, 외부은하 천문학의 기초 등 세 번의 기초강의를 선택적으로 제공하였다. (2) 별과 행성, 항성종족과 화학진화, 은하 형성, 고적색이동 천체와 재이온화, 우주론 등 총 다섯 개 분야에서 심화강의를 제공한 뒤에 각 강의내용과 연관된 열린 질문들을 화두로 해서 학생들 간에 조별 토론을 진행하였다. 이는 정해진 답이 없는 문제를 놓고 토론을 통해 능동적으로 답을 찾아가는 과정을 훈련하기 위해 고안된 것이다. 본 포스터에서는 제4회 거대마젤란망원경 여름학교의 결과를 정리하고 앞으로 나아갈 GMT 계절학교의 방향을 점검해본다.Hyun, Minhee;Kang, Yijung;Park, Jintae;Heo, Jeong-Eun;Yun, Hyeong-Sik;An, Sung-Ho;Choi, Hoseung;Jeon, Yiseul 122.2
한국 젊은 천문학자들의 모임(Korea Young Astronomers Meeting, KYAM)은 지난 8월 18일부터 22일까지 대전광역시 대전 컨벤션 센터에서 개최된 제12회 국제천문연맹 아시아태평양지역 총회(12th Asia-Pacific Regional IAU Meeting, APRIM 2014)에서 부스 전시에 참여하였다. 부스에서는 자체 제작한 전통 부채를 방문자에게 배포하였으며, 천상열차분야지도의 탁본을 직접 찍어 볼 수 있는 체험 활동을 진행하였다. 이 활동을 통해 KYAM 및 천상열차분야지도와 첨성대와 같은 우리나라 고유의 천문학적 유물에 대한 홍보 활동을 수행하였다. 더불어 8월 19일 저녁 모임을 개최하였고, 이를 통하여 한국인 36명 및 외국인 24명을 포함하여 총 60명의 젊은 천문학자들이 모여 친목 도모 및 교류의 시간을 가질 수 있었다. 본 포스터 발표에서는 이와 같은 APRIM 2014 기간 KYAM에서 진행한 활동에 대해 보고할 것이며, 앞으로의 KYAM의 활동 계획에 대해 논의하고자 한다.
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.