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 43 Issue 1
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While astronomers are working hard to detect the earliest galaxies and to follow their evolution to redshift z~0, they remain baffled by the present-day dichotomy between disky, star forming (aka late-type) galaxies and quiescent, spheroidal (aka early-type) galaxies. The key is to find galaxies in transition from one class to the other, whose spectra indicate intense recent star formation that has now ended. We have identified thousands of such "post-starburst galaxies" and discovered that they are often the products of late-type galaxy-galaxy mergers. Their current kinematics, stellar populations, and morphologies are consistent with late- to early-type galaxy evolution. I will discuss recent work that suggests new connections between this violent history and the central supermassive black hole. In particular, the molecular gas reservoir of a post-starburst galaxy declines rapidly after the starburst ends and in a manner consistent with feedback from an active nucleus. Furthermore, a star is ~300x more likely to be tidally disrupted by the nucleus of a post-starburst galaxy than in other galaxies. Like the well-known black hole-bulge mass correlation, these surprising links between the properties of a galaxy on kpc scales and its supermassive black hole on pc scales require explanation.
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The progenitor star properties of supernovae (SNe) are not fully understood though a large number of SNe have been discovered so far. One of the promising ways to understand the properties of progenitor stars is to study SN early light curve where the shock heated emission after explosion is imprinted in. We have performed Intensive Monitoring Survey of Nearby Galaxies (IMSNG) using a global network of telescopes with the aim to snatch the very early moments of SNe explosion. As one of the fruits of our project, we present the result on the type Ic SN, SN 2017ein which was discovered at 2017 May 25 in NGC 3938. We will present the physical properties of the type Ic SN progenitor star that are obtained from the analysis of early epoch data.
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Supernovae (SNe) are well known as good cosmological distance probes owing to their brightness. Specifically, type Ia SNe contribute greatly to our understanding of acceleration of cosmic expansion. However, type IIP supernovae are the most common type of SNe and have been found out to a large redshift, so the application of these SNe as distance indicators is promising. IMSNG is a project for monitoring nearby galaxies (<50Mpc) to catch early light curves of transients and get inspections of their progenitors. The daily monitoring observation allows us to construct a dense light curve of SNe, too. In this talk, we present the light curves of two SNe IIP, SN 2014cx (NGC337) and SN 2017eaw (NGC6946), using our IMSNG data. A newly developed technique, the Photometric Color Method (PCM), employs only photometric data to estimate distances for SNe IIP. We present the distances to our targets measured through PCM and compare this to that of obtained via other methods.
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A Search for Low Surface Brightness Dwarf Satellite Galaxies in Low Density Environments Using IMSNGSearching for low surface brightness (LSB) dwarf galaxies in low density environments (isolated and group) can help us resolve the discrepancy between observation and theory known as the 'missing satellite' problem. They are also important to study the evolution of low mass galaxies in these environments. Although the number of dwarfs in such environments is rapidly increasing in many recent studies, it is still not easy to characterize their general properties. Motivated by this, we present preliminary results of our search for LSB dwarf galaxies around 60 nearby galaxies (D<50Mpc) using deep optical images. Imaging data from Maidanak Astronomical Observatory (MAO) in Uzbekistan as a part of Intensive Monitoring Survey of Nearby Galaxies (IMSNG; Im in prep.) and other archival data are used to find previously unknown LSB dwarf galaxies. Extended LSB sources (central surface brightness
${\mu}_0$ >$23mag/arcsec^2$ ) are first selected in the${\mu}_0$ - magnitude plane (Rines & Geller 2008). The dwarf galaxy candidates are chosen by visual inspection. We discuss whether these candidates are actual satellite galaxies, by measuring the projected number densities in group environments and in the field. Also, their structural and photometric properties are compared with those of previously discovered dwarf galaxies in the literature. -
We present the structural parameters of ~ 910 dwarf elliptical-like galaxies in the local universe (
$z{\lesssim}0.01$ ) derived from the r-band images of the Sloan Digital SKy Survey (SDSS). We examine the dependence of structural parameters on the morphological types (dS0, dE, dEbc, dSph, and dEblue) and the environment. There is not much difference in the structural parameters among the five subtypes but the mean surface brightness within the effective radius (<${\mu}e$ >) of dSph galaxies is clearly different from that of other subtypes. The frequency of disk features such as spiral arm, bar, lens, and rings strongly depends on the morphology of dwarf elliptical-like galaxies with no disk features in dSph galaxies. The absence of disk features and the low surface brightness of dSph galaxies are thought to be closely related to their low mass which leads to different evolution from other subtypes of dwarf elliptical-like galaxies. Density Environments Using IMSNG. -
We report a possible discovery of a relic of a dissolved star cluster in the Sextans dwarf spheroidal galaxy. Using the hk index (
${\equiv}$ (Ca-b)-(b-y)) as a photometric metallicity indicator, we have successfully discriminated the metal-poor and metal-rich stars in the galaxy and found an unexpected number density peak of metal-poor stars near the galaxy center. The analysis of color-magnitude diagrams reveals that they appear to be originated from an old, metal-poor globular cluster which might be slightly farther than the bulk of field stars in the galaxy. This supports the presence of the star cluster remnants in the galaxy which have been suggested by previous studies. If confirmed, dissolution of a star cluster provides a piece of evidence of a cored dark-matter halo profile for the Sextans dwarf galaxy. -
We study the kinematical properties of the Seyfert galaxy, NGC 4051 and Mrk 79. The data used in this study had been observed with OASIS spectrometer at CFHT 3.6m telescope using O300 grism, MR1. The wavelength coverage is
$4760{\AA}$ $-5558{\AA}$ , which includes emission lines,$H{\beta}4861{\AA}$ ,$[OIII ] 4959{\AA}$ , and$[OIII ] 5007{\AA}$ . We observe that forbidden lines have both narrow and broad components. Radial velocity of NGC 4051 is blue-shifted, perhaps due to the z value derived by the earlier studies, 0.002336. We use the revised z, 0.002099, according to the radial velocity of the central spectrum. NGC 4051 is face-on galaxy without rotation observed. Radial velocity of Mrk 79 shows a rotation characteristic in narrow components, relative to$PA=60^{\circ}$ , red-shifted to north-west, and blue-shifted to south-east. In the [OIII] broad components, blue-shifted points are observed at the place at 2 arcsec apart from the center of Mrk 79 to north-west, which are likely to be gas outflow. -
Choi, Hoseung;Yi, Sukyoung K.;Dubois, Yohan;Kimm, Taysun;Devriendt, Julien. E.G.;Pichon, Christophe 33.1
The differential rotational properties of early-type galaxies (ETGs) revealed by integral field spectroscopy surveys is arguably one of the most exciting findings in the galaxy evolution study during the past decade. Numerical studies have shown that galaxy mergers under various configurations can reproduce the observed distribution of ETG spin. However, we suggest an alternative scenario for the spin evolution of a large fraction of ETGs. Using the Horizon-AGN simulation, we follow the spin evolution of 10037 color-selected ETGs more massive than 1010 Msun that are divided into four groups: cluster centrals (3%), cluster satellites (33%), group centrals(5%), and field ETGs (59%). We find a strong mass dependence of the slow rotator fraction, fSR, and the mean spin of massive ETGs. Although the environmental dependence is not clear in the fSR, it is visible in the mean value of the spin parameter. The environmental dependence is driven by the satellite ETGs whose spin gradually decreases as their environment becomes denser. Galaxy mergers appear to be the main cause of total spin changes in 94% of central ETGs of halos with Mvir > 1012.5 Msun, but only 22% of satellite and field ETGs. We find that non-merger induced tidal perturbations better correlate with the galaxy spin-down in satellite ETGs than mergers. Given that the majority of ETGs are not central in dense environments, we conclude that non-merger tidal perturbation effects played a key role in the spin evolution of ETGs observed in the local (z < 1) universe. -
Galaxies associated with massive groups/clusters are normally gas deficient in contrast to field galaxies. HI observations on such galaxies have revealed signs of violent gas stripping, the direct evidence of the environmental effect. At the same time, the notable number of passive galaxies at the cluster outskirts indicates the presence of pre-processing that makes galaxies gas-poor before entering clusters. We investigate the possible channels for the production of the gas deficient galaxies using the state-of-the-art cosmological hydrodynamic zoom-in simulations of 16 clusters (Choi&Yi). We find cluster effect and pre-processing together play an important role in producing the gas-poor galaxies and in both cases gas loss qualitatively agrees with the ram pressure stripping description. Among the currently gas-poor cluster galaxies, 34% are pre-processed before the cluster infall. They are mainly satellites that have undergone ram pressure stripping in group halos. 43% deplete quickly after arriving at cluster during their first approach to the center. Some of them are group halo satellites low in the gas at the infall compared to galaxies directly coming from the field. 24% retain gas even after their first pericentric pass mainly because they are falling into low mass clusters and/or they have a circular orbit that minimizes the ram pressure effect. This study highlights the importance of the past history of galaxies, especially in group halos, before joining the current cluster when understanding the excess of passive galaxies in clusters.
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Using cosmological N-body simulations we investigate statistical properties of flyby encounters between halos in comparison with mergers. We classify halo pairs into two groups based on the total energy (E12); flybys (E12 > 0) and mergers (E12 < 0). By measuring the flyby and merger fractions, we assess their dependencies on redshift (0 < z < 4), halo mass (10.8 < log Mhalo/Msun < 13.0), and large-scale environment (from field to cluster). We find that the flyby and merger fractions similarly increase with redshift until z = 1, and that the flyby fraction at higher redshift (1 < z < 4) slightly decreases in contrast to the continuously increasing merger fraction. While the merger fraction has little or no dependence on the mass and environment, the flyby fraction correlates negatively with mass and positively with environment. The flyby fraction exceeds the merger fraction in filaments and clusters; even 10 times greater in the densest environment. Our results suggest that the flyby makes a substantial contribution to the observed pair fraction, thus heavily influencing galactic evolution across the cosmic time.
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Galaxy transition from star-forming to quiescent, accompanied with morphology transformation, is one of the key unresolved issues in extragalactic astronomy. Although several environmental mechanisms have been proposed, a deeper understanding of the impact of environment on galaxy transition still requires much exploration. My Ph.D. thesis focuses on which environmental mechanisms are primarily responsible for galaxy transition in different environments and looks at what happens during the transition phase using multi-wavelength photometric/spectroscopic data, from UV to mid-infrared (MIR), derived from several large surveys (GALEX, SDSS, and WISE) and our GMOS-North IFU observations. Our multi-wavelength approach provides new insights into the *late* stages of galaxy transition with a definition of the MIR green valley different from the optical green valley. I will present highlights from three areas in my thesis. First, through an in-depth study of environmental dependence of various properties of galaxies in a nearby supercluster A2199 (Lee et al. 2015), we found that the star formation of galaxies is quenched before the galaxies enter the MIR green valley, which is driven mainly by strangulation. Then, the morphological transformation from late- to early-type galaxies occurs in the MIR green valley. The main environmental mechanisms for the morphological transformation are galaxy-galaxy mergers and interactions that are likely to happen in high-density regions such as galaxy groups/clusters. After the transformation, early-type MIR green valley galaxies keep the memory of their last star formation for several Gyr until they move on to the next stage for completely quiescent galaxies. Second, compact groups (CGs) of galaxies are the most favorable environments for galaxy interactions. We studied MIR properties of galaxies in CGs and their environmental dependence (Lee et al. 2017), using a sample of 670 CGs identified using a friends-of-friends algorithms. We found that MIR [3.4]-[12] colors of CG galaxies are, on average, bluer than those of cluster galaxies. As CGs are located in denser regions, they tend to have larger early-type galaxy fractions and bluer MIR color galaxies. These trends can also be seen for neighboring galaxies around CGs. However, CG members always have larger early-type fractions and bluer MIR colors than their neighboring galaxies. These results suggest that galaxy evolution is faster in CGs than in other environments and that CGs are likely to be the best place for pre-processing. Third, post-starburst galaxies (PSBs) are an ideal laboratory to investigate the details of the transition phase. Their spectra reveal a phase of vigorous star formation activity, which is abruptly ended within the last 1 Gyr. Numerical simulations predict that the starburst, and thus the current A-type stellar population, should be localized within the galaxy's center (< kpc). Yet our GMOS IFU observations show otherwise; all five PSBs in our sample have Hdelta absorption line profiles that extend well beyond the central kpc. Most interestingly, we found a negative correlation between the Hdelta gradient slopes and the fractions of the stellar mass produced during the starburst, suggesting that stronger starbursts are more centrally-concentrated. I will discuss the results in relation with the origin of PSBs.
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Shock waves have been observed in the outskirts of galaxy clusters. They are commonly interpreted as being driven by mergers of sub-clumps, so are called "merger shocks". We here report a study of the properties of merger shocks in merging galaxy clusters with cosmological hydrodynamic simulations. As a representative case, we describe the case where sub-clusters with mass ratio ~ 2 go through an almost head-on, binary-like merger. Because of the turbulent nature of hierarchical clustering, shock surfaces are not uniform, but composed of parts with different Mach numbers. As merger shocks expand from the core to the outskirts, the average Mach number, <
$M_s$ >, increases. The shocks propagating along the merger axis could be observed as X-ray shocks and/or radio relics. The kinetic energy through the shocks peaks at ~ 1 Gyr after shock launching, or at ~ 1 - 2 Mpc from the core. The most energetic shocks are found to have the kinetic-energy weighted Mach number, <$M_s$ >$_{\phi}{\simeq}2-3$ , and the CR-energy weighted Mach number, <$M_s$ >$_{CR}{\simeq}3-4$ . We then discuss the observational implications of our results. -
Magnetic fields in clusters of galaxies play a critical role in shaping up the intracluster medium. Their existence has been established through observations of synchrotron emission, especially from radio relics and halos, as well as observations of rotation measure. In the so-called Sausage relic, which is one of Mpc-size giant radio relics detected in the outskirts of merging clusters, for instance, the magnetic fields are believed to have a few
${\mu}G$ strength and a Mpc scale. The observed magnetic fields are conjectured to be produced by the process of small-scale turbulence dynamo. To investigate the dynamo origin, we simulate the development of turbulence and the follow-up amplification of magnetic fields in galaxy clusters using a three-dimensional magnetohydrodynamical(MHD) code. Turbulence is induced in highly stratified backgrounds expected in clusters, and driven sporadically mimicking major mergers. We here present preliminary results, aiming to answer whether the turbulence dynamo scenario can explain observed magnetic fields in clusters of galaxies. -
Incorporating the fully quantum mechanical computation of scattering cross-section and statistical moment analysis of absorption profiles, we investigate the Lyman line asymmetry of extremely high column density systems. Recent high redshift observations detected strong damped Lyman alpha systems (DLAs) whose column density is larger than N_HI ~ [10]^21.3 cm^(-2). Absorption profiles of these DLAs are characterized by the broad and asymmetric damping wing. For accurate description of radiation damping, the second-order time-dependent perturbation theory is adopted. To quantitatively address line asymmetry, we define a distribution function for each Lyman line, and compute statistical moments (mean, standard deviation, skewness and kurtosis) regarding column densities N_HI > [10]^18 cm^(-2). In this work, we present statistical properties of the intrinsic line profiles, and compare them with the Lorentzian cases.
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$Ly{\alpha}$ blobs are mysterious, giant (~100 kpc), glowing gas clouds in the distant universe. They occupy the dark matter halos that will evolve into the richest groups and clusters today. The blob's gas may be the proto-intracluster medium and their embedded galaxies are considered as the progenitors of massive cluster galaxies. Yet we do not know why$Ly{\alpha}$ blobs glow. There are evidences of kinematic measurements to exclude shocks and winds from AGN or starbursts as a power source, suggesting that photoionizing radiation or scattering of$Ly{\alpha}$ photons might be responsible. Polarization mapping can discriminate between these photo-ionization and scattering. Previous results of imaging polarimetry for$Ly{\alpha}$ nebulae are roughly consistent with scattering models. However the polarization morphologies in those of previous results are all different, motivating our polarimetric survey of$Ly{\alpha}$ nebulae for the statisticallymeaningful sample. As initial results of our survey, we present the total polarization map of the LABd05 which has the spatial offset between the peak of$Ly{\alpha}$ surface brightness and an obscured AGN. We detect the significant polarization in this target with the radially increasing polarization gradient, suggesting that scattering plays major role within this nebula. The polarization pattern is more aligned with the$Ly{\alpha}$ peak rather than the AGN (the potential energy source), indicating that the$Ly{\alpha}$ photons are originated from the region near the peak of$Ly{\alpha}$ intensity. -
Kimm, Taysun;Haehnelt, Martin;Blaizot, Jeremy;Katz, Harley;Michel-Dansac, Leo;Garel, Thibault;Rosdahl, Joakim;Teyssier, Romain 36.1
Understanding the origin of strong galactic outflows and the suppression of star formation in dwarf galaxies is a key problem in galaxy formation. Using a set of radiation-hydrodynamic simulations of an isolated dwarf galaxy, we show that the momentum transferred from resonantly scattered Lyman-alpha(LyA) photons can suppress star formation by a factor of two in metal-poor galaxies by regulating the dynamics of star-forming clouds before the onset of supernova explosions (SNe). This is possible because each LyA photon resonantly scatters and imparts ~10-300 times greater momentum than in the single scattering limit. Consequently, the number of star clusters predicted in the simulations is reduced by a factor of ~5, compared to the model without the early feedback. More importantly, we find that galactic outflows become weaker in the presence of strong LyA radiation feedback, as star formation and associated SNe become less bursty. We also examine a model in which radiation field is arbitrarily enhanced by a factor of up to 10, and reach the same conclusion. The typical mass-loading factors in our metal-poor dwarf system are estimated to be ~5-10 near the mid-plane, while it is reduced to ~1 at larger radii. -
Radiative transfer models were developed to understand the optical polarizations in edge-on galaxies, which are observed to occur even outside the geometrically thin dust disk, with a scale height of ~0.2 kpc. In order to reproduce the vertically extended polarization structure, we find it is essential to include a geometrically thick dust layer in the radiative transfer model, in addition to the commonly-known thin dust layer. The models include polarizations due to both dust scattering and dichroic extinction which is responsible for the observed interstellar polarization in the Milky Way. It is found that the magnetic fields in edge-on galaxies are in general vertical (or poloidal) except the central part, where the magnetic fields are mainly toroidal. We also find that the polarization level is enhanced if the clumpiness of the interstellar medium, and the dichroic extinction by vertical magnetic fields in the outer regions of the dust lane are included in the radiative transfer model. The predicted degree of polarization outside the dust lane was found to be consistent with that (ranging from 1% to 4%) observed in NGC 891.
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Oh, Kyuseok;Koss, Michael;Markwardt, Craig B.;Schawinski, Kevin;Baumgartner, Wayne H.;Barthelmy, Scott D.;Cenko, Bradley;Gehrels, Neil;Mushotzky, Richard;Petulante, Abigail;Ricci, Claudio;Lien, Amy;Trakhtenbrot, Benny 36.3
We present a new catalog of hard X-ray sources detected in the first 105 months of observations with the Burst Alert Telescope (BAT) on board the Neil Gehrels Swift observatory. The 105 month Swift-BAT survey is a uniform hard X-ray all-sky survey performed in the 14-195 keV band. The Swift-BAT 105 month catalog provides 1632 (422 new detections) hard X-ray sources in the 14 - 195 keV band above the 4.8 sigma significance level. Adding to the previously known hard X-ray sources, 34% (144/422) of the new detections are identified as Seyfert AGN in nearby galaxies (z < 0.2). The majority of the remaining identified sources are X-ray binaries (7%, 31) and blazars/BL Lac objects (10%, 43). As part of this new edition of the Swift-BAT catalog, we release eight-channel spectra and monthly sampled light curves for each object in the online journal and at the Swift-BAT 105 month Web site. -
A Korean VLBI Network key science program, the Interferometric Monitoring of Gamma-ray Bright AGNs (iMOGABA) program continues to reveal the nature of the gamma-ray flares in active galactic nuclei (AGNs). Here in this presentation, we would like to introduce an interesting story about four gamma-ray bright AGNs - BL Lac, 1633+382, 3C 84, and M87 - based on the recent results of the iMGOABA. The results will include a) a sad story of an 'orphan' gamma-ray flare from BL Lac, b) a position offset of 40 pc for a gamma-ray flaring site from the radio regions in 1633+382, c) a position alignment of a gamma-ray flaring site with a central engine region in 3C 84, and d) a flat millimeter spectrum of a core in M87 revealed by the iMOGABA.
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The Wide-field Infrared Survey Explorer (WISE) mission has been efficient in selecting Active Galactic Nuclei (AGN) with high luminosities and large obscuration. According to the merger driven AGN powering scenarios, luminous and obscured AGN are in a stage where they go through feeding of gas accretion into the central black hole, and feedback to the host galaxy through outflows. We report the rest-frame UV-optical spectra of 11 Hot Dust Obscured Galaxies (Hot DOGs) at z~2, WISE color-selected to be extremely reddened AGN. A fraction of the targets show blueshifted and broadened [OIII] profiles indicative of ionized gas outflows. We present the occurrence and strength of the outflows, and discuss what impact these AGN activity could give on their hosts.
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Theoretical simulation studies suggest that dust-obscured AGNs appear for a certain period when merger-driven star-forming galaxies evolve to unobscured type 1 AGNs. The dust-obscured AGNs would have red colors due to the dust extinction in their host galaxies, and they are expected to have higher accretion rates than unobscured type 1 AGNs. Red AGNs are found by selecting type 1 AGNs with very red colors, and they have been suspected as the intermediate-stage, dusty AGNs. However, it is not yet clear if red AGNs really correspond to the dusty AGNs due to a lack of intrinsic properties of red AGNs. For unveiling intrinsic properties of red AGNs, we study the NIR and MIR spectra of unobscured type 1 AGNs and red AGNs. There are three main themes: (i) derivation of NIR and MIR BH mass estimators can be used for red AGN study; (ii) investigation of red AGN selection methods to test its usefulness to identify dusty red AGNs; and (iii) investigation of the accretion rates of red AGNs to see if they have the properties as predicted in the simulation studies.
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The HULQ project proposes to use gravitational lensing to determine the masses of QSO host galaxies, an otherwise difficult goal. If these host galaxy masses, along with their SMBH masses from single-epoch measurements, are estimated for a substantial number of QSOs at various redshifts, the co-evolution of SMBHs and their host galaxies can be studied for a large portion of the history of the universe. To determine the feasibility of this study, we present how to estimate the number of sources lensed by QSO hosts, i.e. the number of lensing QSO host galaxies (hereafter QSO lenses). SMBH masses in the literature are transformed into the velocity dispersions of their host galaxies using the M_BH -sigma relation, and in turn the Einstein radii for each QSO -source redshift combination is calculated, assuming singular isothermal spherical mass distributions. Using QSOs and galaxies as potential sources, the probability of a QSO host galaxy being a QSO lens is calculated, as a function of limiting magnitude. The expected numbers of QSO lenses are estimated for ongoing and future wide-imaging surveys, and the Hyper Suprime-Cam Wide survey is illustrated as an example.
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With upcoming high-quality data from surveys such as eBOSS or DESI, improving the theoretical modeling and gaining a deeper understanding of the effects of neutrinos and dark radiation on structure formation at small scales are necessary, to obtain robust constraints free from systematic biases. Using a novel suite of hydrodynamical simulations that incorporate dark matter, baryons, massive neutrinos, and dark radiation, we present a detailed study of their impact on Lyman-Alpha forest observables. In particular, we accurately measure the tomographic evolution of the shape and amplitude of the small-scale matter and flux power spectra and search for unique signatures along with preferred scales where a neutrino mass detection may be feasible. We then investigate the thermal state of the intergalactic medium (IGM) through the temperature-density relation. Our results indicate that the IGM at z ~ 3 provides the best sensitivity to active and sterile neutrinos.
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Sloan Digital Sky Survey 12번째 Data release의 CMASS catalog를 이용하여 우주의 균일, 등방성 여부를 조사하였다. Redshift 범위에 따라 얻은 2차원 영역들을 조사한 결과, CMASS 은하들은 통계조사가 가능한 최대 규모인 반지름 300Mpc/h에서도 여전히 Random catalog에 비해 불균일하게 분포하고 있음을 보였다. 결과를 더 명확하게 보여주기 위해 은하의 분포가 불균일함을 나타내는 통계량을 여러 방법으로 시각화하는 연구를 진행하였다. 밀도 분포를 입체적으로 나타낸 그림에서 최대, 최소 밀도의 차이는 300Mpc/h규모에서 약 27%에 달한다. 이는 같은 규모에서 최대 약 4.5%의 차이만이 나타나는 Random catalog의 밀도 분포와는 상이한 결과로, 이 규모에서조차 우주에서 은하는 균일하게 분포하고 있지 않다는 것을 밝혔다.
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The properties of unseen high-redshift sources (and sinks) are encoded in the 3D structure of the cosmic 21-cm signal. Here I introduce a flexible parametrization for high-z galaxies' properties, including their star formation rates, ionizing escape fraction and their evolution with the mass of the host dark matter halos. With this parametrization, I self-consistently calculate the corresponding 21-cm signal during reionization and the cosmic dawn. Using a Monte Carlo Markov Chain sampler of 3D simulations, 21CMMC, I demonstrate how combining high-z luminosity functions with a mock 21-cm signal can break degeneracies, resulting in ~ percent level constraints on early universe astrophysics.
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We analyze the Planck 2015 cosmic microwave background temperature fluctuation data to find any anomaly in the angular power spectra measured for partial regions on the sky. For disks with radius of
$20^{\circ}$ ,$45^{\circ}$ and$90^{\circ}$ , which are densely overlapping on the sky, we estimate the power excess and its statistical significance relative to the LambdaCDM expectation for some chosen ranges of angular scales. We also investigate the dipolar asymmetry using the power excess maps obtained for some chosen angular scales, and confirm the previously announced consistent dipole directions. The average dipole amplitude and the inner products of dipoles have been measured from the power excess maps at different angular scales. We conclude that although dipole directions are consistent the measured amplitudes are not statistically significant compared to the LambdaCDM model prediction. -
Although it is agreed that the gamma-ray bursts (GRBs) invoke highly relativistic jets with bulk Lorentz factors of a few hundreds, the exact physical mechanism producing such powerful gamma-rays still remains debated. Three outstanding and important questions in the field concern (1) the composition of GRB jets (i.e., matter-dominated vs Poynting-flux-dominated), (2) the involved radiative process responsible for the observed gamma-rays (i.e., synchrotron mechanism vs photospheric radiation), and (3) the distance of the emitting region from the central engine where the prompt gamma-rays are released (i.e., ~10^12 cm vs 10^14 cm vs 10^16 cm). I will present recent important breakthroughs that we have made, which answer these three questions.
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GW170817/GRB170817A establishes a double neutron star merger as the progenitor of a short gamma-ray burst, starting 1.7 s post-coalescence. GRB170817A represents prompt or continuous emission from a newly formed hyper-massive neutron star or black hole. We report on a deep search for broadband extended gravitational-wave emission in spectrograms up to 700 Hz of LIGO O2 data covering this event produced by butterfly filtering comprising a bank of templates of 0.5 s. A detailed discussion is given of signal-to-noise ratios in image analysis of spectrograms and confidence levels of candidate features. This new pipeline is realized by heterogeneous computing with modern graphics processor units (GPUs). (Based on van Putten, M.H.PM., 2017, PTEP, 093F01.)
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Lee, Chung-Uk;Kim, Seung-Lee;Lee, Dong-Joo;Cha, Sang-Mok;Lee, Yongseok;Kim, Dong-Jin;Kim, Hyun-Woo;Shin, Min-Su;Park, HongSoo;Lim, Jin-Sun;Park, Byeong-Gon 39.3
외계행성 탐색시스템 운영현황과 계획을 소개한다. 2017년 관측장비 가동율은 97.4% 이며, 시스템이 설치된 3개 천문대에서 천문박명시간을 기준으로 총 10,157 시간이 연구에 할당되었고 총 7,178 시간 관측이 이루어졌다. 관측시스템의 성능개선을 위해 주경 코팅, 돔 레벨조정, 망원경 구동롤러 정렬, 주경 배플 마스크 설치 등 돔과 망원경의 기계부 업그레이드와 카메라 전자부 조정 및 앰프보드 교체 등이 이루어졌다. 관측효율 향상을 위해 1년간 관측된 약 177,000 장의 자료를 분석하여 불량자료 태깅기반을 마련했고, 시상모니터링과 관측 스크립트 코드를 개발하여 현재 관측에 적용하고 있다. 관측 자료는 각 연구 프로그램의 자료공개 정책에 따라 영상형태 또는 측광 파일형태로 이용이 가능하며, 관측로그는 홈페이지를 통해 확인할 수 있다. 2020년 10월부터 시작되는 2단계 관측 프로그램 선정을 위해 2019년 상반기에 관측제안서를 접수받아 하반기에 선정을 마칠 계획이며, 다양한 연구주제 발굴을 위해 파일롯 프로그램을 선별 지원할 계획이다. -
Lee, Yongseok;Cha, Sang-Mok;Lee, Chung-Uk;Kim, Seung-Lee;Lee, Dong-Joo;Jeon, Young-Beom;Park, Hong Soo;Jin, Ho 39.4
KMTNet 광시야 망원경의 성능 개선을 위해 2017년에 이루어진 주요 작업으로 주경 배플(baffle) 설치, 주경 코팅, 돔 플랫(dome flat) 장치 설치에 대해 발표한다. 망원경 주경의 가장자리(turn down edge)는 경면 가공이나 코팅 상태가 균질하지 않을 수 있으며, 이로 인한 난반사는 밝은 별 주위에 넓은 wing profile과 여러 갈래의 방사상 빛줄기를 만든다. 이런 난반사를 제거하기 위해 주경면 바로 앞에 배플을 설치하였다. 주경의 광학 성능과 집광력이 최적이 되도록 배플 내부 직경 값을 1,580 mm로 조정하여 설치한 결과, 관측 영상에서 별의 영상이 크게 개선되었다. 호주 관측소는 상대적으로 습기가 높아서 망원경 주경의 반사율이 빨리 낮아졌으며, 이를 개선하기 위해 기존의 코팅(protected silver)을 제거하고 알루미늄으로 새로 코팅하였다. KMTNet 3개 관측소는 주경의 반사율과 코팅 면의 확대 영상을 정기적으로 모니터링하여 광학 성능의 변화를 추적하고 있다. 밤하늘 플랫(twilight sky flat) 영상을 보완하기 위해, 돔 인클로져에 플랫 스크린과 광원을 설치하여 돔 플랫 영상을 획득하였다. 마지막으로 KMNet 관측시스템을 운영하며 발생한 돔 회전 및 돔 셔터 구동부 문제 등에 대해 소개하고, 문제 발생 원인과 주기, 문제 해결 방안을 발표한다. -
Cha, Sang-Mok;Lee, Chung-Uk;Kim, Seung-Lee;Lee, Yongseok;Atwood, Bruce;Lim, Beomdu;O'Brien, Thomas P.;Jin, Ho 40.1
외계행성 탐색시스템 18k 모자이크 CCD 카메라는 4개의 9k CCD로 구성되며 총 32개 채널의 영상영역과 리드아웃 회로를 가진다. 관측 영상에는 각 영상영역에 대한 오버스캔(overscan) 영역이 포함되는데, 영상 신호에 의한 오버스캔 영역의 바이어스(bias) 교란을 최소화하기 위해 리드아웃 회로의 인버팅 앰프에 대한 Common Mode Rejection Ratio(CMRR)를 미세 조정하였다. 그 결과 세 사이트의 평균 CMRR이 55 dB에서 73 dB로 향상되었고, 기존에는 영상 신호에 따른 오버스캔 바이어스 레벨의 선형적 관계가 약 2/1,000의 기울기를 가졌으나 조정 후에는 약 2/10,000로 바이어스 오차가 줄어들었다. CCD 리드아웃 회로의 미세조정과 클락(clock) 개선을 통해 물결무늬 잡음 제거 및 읽기 잡음 감소가 이루어졌으며, 향후의 추가적인 바이어스 안정화와 크로스톡 개선 방안이 검토되고 있다. 카메라 전자부 조정 과정 및 결과와 더불어, 카메라 듀어와 부대장비 유지보수, Polycold CryoTiger 냉각기 운영 및 개선 관련 노하우도 함께 발표한다. -
외계행성 탐색시스템으로 관측한 영상은 한국천문연구원 본원에 있는 자료처리 시스템으로 실시간 전송된다. 이를 위해 한국과학기술정보연구원이 운영 중인 첨단망과 UDP 전송 프로그램을 활용하고 있으며 연간 약 140TB의 관측 영상을 칠레 55Mbps, 남아공 39Mbps, 호주 410Mbps의 속도로 전송하고 있다. 관측 영상이 전송되면 MEF 포맷으로 구조화 하고 bias, flat, crosstalk 보정과 bad pixel masking 등의 전처리 과정을 거쳐 각 연구과제별로 실시간 배포하고 있다. 중력렌즈 연구를 위한 우리 은하 중심부 관측영상은 차감영상 기법을 사용하여 약 3억 개의 별에 대해 측광하고 있으며,
$18K{\times}18K$ 크기의 대용량 관측 영상을 빠르고 효율적으로 처리하기 위해 256개로 분할하여 분산처리하고 있다. 2014년부터 자료처리를 위한 시스템을 구축하고 증설하였으며 현재 11대의 서버(212Core)와 2.7PB의 NAS 스토리지를 운영하며 연간 700TB이상의 자료를 처리하고 있다. 우리은하 중심부 측광자료에서 검출된 변광 현상을 정리하여 측광데이터베이스를 구축하였다. 본 발표에서는 KMTNet 실시간 자료처리 과정에 대한 상세한 내용과 향후 자료처리 시스템 개선방향에 대해 소개한다. -
We present results from our two experiments of using machine learning algorithms in processing and analyzing the KMTNet imaging data. First, density estimation and clustering methods find meaningful structures in the metric space of imaging quality measurements described by photometric quantities. Second, we also develop a method to separate out light curves of reliable microlensing event candidates from spurious events, estimating reliability scores of the candidates.
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We introduce a coordinate catalog for photometry of the KMTNet Galactic bulge observation program and how to find the microlensing event candidates in the photometry result. Basically, the KMTNet bulge program is monitoring a total of 27 target fields (108 deg2) with four different cadences of 0.5, 1.0, 2.5, and 5.0 hours. In order to measure the stellar flux of each target, we made a 'observation coordinate catalog' by using the 'OGLE-III catalog' and 'DoPhot package'. The catalog contains approximately 0.3 billion stars in the bulge fields. We also search for a microlensing event candidates by means of the 'Event Finder algorithm' which calculates the restricted single-lens fitting (t0, teff, u0; u0 = 0 or 1) model. As a result, we found more than 2,000 microlensing event candidates per each year including about 700 events from the other survey groups such as OGLE and MOA. In this year, we will improve our current pipeline system, e.g. upgrading the catalog and applying real-time photometry.
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Chung, Sun-Ju;Gould, Andrew;Jung, Youn Kil;Hwang, Kyu-Ha;Ryu, Yoon-Hyun;Shin, In-Gu;Yee, Jennifer C.;Zhu, Wei;Han, Cheongho;Cha, Sang-Mok;Kim, Dong-Jin;Kim, Hyun-Woo;Kim, Seung-Lee;Lee, Chung-Uk;Lee, Yongseok 41.1
We introduce a current status and future plans of Korea Microlensing Telescope Network (KMTNet) microlensing experiments, which include an observational strategy, pipeline, event-finder, and collaborations with Spitzer. The KMTNet experiments were initiated in 2015. From 2016, KMTNet observes 27 fields including 6 main fields and 21 subfields. In 2017, we have finished the DIA photometry for all 2016 and 2017 data. Thus, it is possible to do a real-time DIA photometry from 2018. The DIA photometric data is used for finding events from the KMTNet event-finder. The KMTNet event-finder has been improved relative to the previous version, which already found 857 events in 4 main fields of 2015. We have applied the improved version to all 2016 data. As a result, we find that 2597 events are found, and out of them, 265 are found in KMTNet-K2C9 overlapping fields. For increasing the detection efficiency of event-finder, we are working on filtering false events out by machine-learning method. In 2018, we plan to measure event detection efficiency of KMTNet by injecting fake events into the pipeline near the image level. Thanks to high-cadence observations, KMTNet found fruitful interesting events including exoplanets and brown dwarfs, which were not found by other groups. Masses of such exoplanets and brown dwarfs are measured from collaborations with Spitzer and other groups. Especially, KMTNet has been closely cooperating with Spitzer from 2015. Thus, KMTNet observes Spitzer fields. As a result, we could measure the microlens parallaxes for many events. Also, the automated KMTNet PySIS pipeline was developed before the 2017 Spitzer season and it played a very important role in selecting the Spitzer target. For the 2018 Spitzer season, we will improve the PySIS pipeline to obtain better photometric results. -
Kim, Seung-Lee;Lee, Jae Woo;Lee, Chung-Uk;Lee, Yongseok;Lee, Dong-Joo;Hong, Kyeongsoo;Cha, Sang-Mok;Kim, Dong-Jin;Park, Byeong-Gon 41.2
EL CVn-type eclipsing binaries are composed of a massive A-type main-sequence primary star and a hotter B-type secondary one. These are worthy of particular attention because the secondary stars are rare objects to be extremely low-mass white dwarf precursors (ELM proto-WD) with the mass of${\leq}0.2M_{\odot}$ , evolving to higher effective temperatures and higher surface gravities. A few of them were discovered to show multi-periodic pulsations in one or both components. We monitored one of these rare and interesting objects, J0247-25 (=1SWASP J024743.37-251549.2), at two KMTNet sites of SAAO in South Africa and SSO in Australia. The observations were performed with the KMTNet 1.6m telescopes and pre-science 4K CCD cameras during the system test run from July to November 2014. Using the photometric data obtained for a total of 23 nights, we constructed well-defined eclipsing light curves in B/V-bands and derived absolute parameters (mass and radius, etc.) of each binary component. After subtracting model eclipsing curves from the data, we detected seven frequencies with 33~53 cycles per day (c/d) and identified them to be Delta Sct-type pulsations originated from the A-type primary component. Five frequencies were turned out to be excited by rotational splitting of non-radial pressure modes, enabled us to investigate rotational properties. We could not detect any frequency higher than 100 c/d, implying that pulsation amplitudes of the proto-WD secondary decrease greatly. -
Moon, Hong-Kyu;Kim, Myung-Jin;Park, Jintae;JeongAhn, Youngmin;Yang, Hongu;Lee, Hee-Jae;Kim, Dong-Heun;Roh, Dong-Goo;Choi, Young-Jun;Yim, Hong-Suh;Lee, Sang-Min;Kwak, SungWon 42.1
Deep Ecliptic Patrol of the Southern Sky (DEEP-South) observation is being made during the off-season for exoplanet survey, using Korea Microlensing Telescope Network (KMTNet). An optimal combination of its prime focus optics and the 0.3 billion pixel CCD provides a four square degrees field of view with 0.4 arcsec/pixel plate scale which is also best suited for small body studies. Normal operation of KMTNet started in October 2015, and a significant portion of the allocated telescope time for DEEP-South is dedicated to targeted observation, Opposition Census (OC), of near-Earth asteroids for physical and taxonomic characterization. This is effectively achieved through multiband, time series photometry using Johnson-Cousins BVRI filters. Uninterrupted monitoring of the southern sky with KMTNet is optimized for spin characterization of a broad spectrum of asteroids ranging from the near-Earth space to the main-belt, including binaries, asteroids with satellites, slow/fast- and non-principal axis-rotators, and thus is expected to facilitate the debiasing of previously reported lightcurve observations. Our software subsystem consists of an automated observation scheduler, a pipelined data processing system for differential photometry, and an easy-to-use lightcurve analysis toolkit. Lightcurves, spin periods and provisional determination of class of asteroids to which the lightcurve belongs will be presented, using the dataset from first year operation of KMTNet. Our new taxonomic classification scheme for asteroids will also be summarized. -
JeongAhn, Youngmin;Kim, Dong-Heun;Lee, Hee-Jae;Choi, Young-Jun;Moon, Hong-Kyu;Lee, Sang Min 42.2
고전적인 소행성과 혜성의 경계는 무너지고 있다. 처음 발견했을 때는 소행성으로 분류됐던 천체도, 예기치 않은 활동성이 나타나면 혜성의 일원이 된다. 소행성은 충돌이나 회전가속에 의해 갑자기 활동성을 나타내기도 하지만, 강한 태양복사를 견디지 못하고 오랜 시간 간직해온 휘발성 물질을 우주 공간으로 흩뿌리기도 한다. 한국천문연구원 딥사우스 (DEEP-South) 팀은, 이렇게 태양 근방에서 혜성으로 탈바꿈할 것으로 예상되는 소행성으로 2000 XO8을 지목하고, 근일점을 막 지난 2017년 10월 말부터 KMTNet 망원경으로 약 한 달간 지속 관측을 하였다. 이 기간 동안 2000 XO8은 활동성이 급격히 증가하여 선명한 꼬리를 나타냈고, 이내 검출 한계 이하로 활동성이 줄어드는 것까지 확인하였다. 이번에 혜성으로 밝혀진 2000 XO8은 한국인 또는 한국 기관에서 새로 발견 및 동정한 것으로 알려진 혜성 중에 그 주기가 8.8년으로 가장 짧다. 이는 궤도장반경이 목성보다 안쪽에 위치한다는 점에서 이례적인 일이다. 우리는 궤도 실험을 통해 2000 XO8이 현 궤도에 자리 잡은 지 오래 되지 않았으며, 또 다른 주기 혜성 265P/LINEAR에서 쪼개져 나온 조각일 가능성을 제시하고자 한다. -
Transformation of Surface Brightness Profile Types of Dwarf Galaxies : KMTNet Supernova Program DataLee, Youngdae;Park, Hong Soo;Kim, Sang Chul;Moon, Dae-Sik;Lee, Jae-Joon;Kim, Dong-Jin;Cha, Sang-Mok 42.3
We investigate surface brightness profiles (SBPs) of dwarf galaxies in field, group, and cluster environments. Using images from the Korea Microlensing Telescope Network (KMTNet) Supernova Program (KSP) for the NGC 2784 group and SDSS for the Virgo cluster, SBP types are classified into profiles with single exponential (Type I), double exponential (Type II and Type III). Type II and Type III have smaller and larger outer sizes than inner sizes, respectively. SBP types of field dwarfs are compiled from a previous study. The distributions of SBP types are different in three environments. After comparing sizes of dwarfs in different environments, we suggest that since sizes of some dwarfs are changed due to the environmental effects, SBP types are able to be transformed. It makes that the distributions of SBP types in three environments are different. -
Byun, Woowon;Kim, Minjin;Sheen, Yun-Kyeong;Ho, Luis C.;Lee, Joon Hyeop;Jeong, Hyunjin;Kim, Sang Chul;Park, Byeong-Gon;Seon, Kwang-Il 42.4
Most galaxies are believed to evolve through mergers and accretions. In particular, minor mergers and gas accretion appear to play an important role in galaxy evolution in the present-day Universe. Tidally-disrupted debris from such processes remain as diffuse, low-surface brightness structures because the dynamical timescale in the outskirts is significantly longer than that in the central regions. Although these structures will give us useful insight into the mass assembly history of galaxies, it is difficult to detect them due to their faint surface brightness. In order to investigate the structural properties of outskirts in nearby galaxies, we conduct deep and wide-field imaging survey with KMTNet. We present our observing strategy and an optimal data reduction process to recover faint extended features in the images of KMTNet. Using the imaging data of NGC 1291 obtained from KMTNet, we find that a peak-to-peak sky gradient can be reduced less than 0.4-0.6% of the original sky level in the entire image. We also find that we can reach the surface brightness of${\mu}_{(B,1{\sigma})}$ ~ 29.5,${\mu}_{(R,1{\sigma})}$ ~ 28.5 mag$arcsec^{-2}$ in one-dimensional profile, that is mainly limited by the uncertainty in the sky determination. It indicates that deep imaging data of KMTNet is suitable to study the extended faint features of nearby galaxies, such as stellar halos, outer disks, and dwarf companions. -
Star formation in galaxies predominantly takes place in giant molecular clouds (GMCs). While it is widely believed that UV radiation feedback from young massive stars can destroy natal GMCs by exciting HII regions and driving their expansion, our understanding on how this actually occurs remains incomplete. To quantitatively assess the effect of UV radiation feedback on cloud disruption, we conduct a series of theoretical studies on the dynamics of HII regions and its role in controlling the star formation efficiency (SFE) and lifetime of GMCs in a wide range of star-forming environments. We first develop a semi-analytic model for the expansion of spherical dusty HII regions driven by the combination of gas and radiation pressures, finding that GMCs in normal disk galaxies are destroyed by gas-pressure driven expansion with SFE < 10%, while more dense and massive clouds with higher SFE are disrupted primarily by radiation pressure. Next, we turn to radiation hydrodynamic simulations of GMC dispersal to allow for self-consistent star formation as well as inhomogeneous density and velocity structures arising from supersonic turbulence. For this, we develop an efficient parallel algorithm for ray tracing method, which enables us to probe a range of cloud masses and sizes. Our parameter study shows that the net SFE, lifetime (measured in units of free-fall time), and the importance of radiation pressure (relative to photoionization) increase primarily with the initial surface density of the cloud. Unlike in the idealized spherical model, we find that the dominant mass loss mechanism is photoevaporation rather than dynamical ejection and that a significant fraction of radiation escapes through low optical-depth channels. We will discuss the astronomical.
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One of the keys to interpreting the characteristics and evolution of interstellar medium in the Milky Way is to understand the distribution of hot gas (
$10^5-10^6K$ ). Gases in this phase are difficult to observe because they are in low density and lack of easily observable tracers. Hot gases are observed mainly in the emission of the FUV ($912-1800{\AA}$ ), EUV ($80-912{\AA}$ ), and X-rays (T>$10^6K$ ) of which attenuation is very high. Of these, FUV emission lines originated from high-stage ions such as O VI and C IV can be the most effective tracers of hot gases. To determine the spatial distribution of O VI and C IV emissions, we have analyzed the spectra obtained from FIMS (Far-ultraviolet IMaging Spectrograph), which covers about 80 percent of the sky. The hot gas volume filling factor, which varies widely from 0.1 to 0.9 depending on the supernova explosion frequency and the evolution model, has been calculated from the O VI and C IV maps. The hot gas generation models has been verified from the global distribution of O VI and C IV emissions, and a new complementary model has been proposed in this study. -
We present a spectroscopic study of the Galactic supernova remnant (SNR) Cygnus Loop using the fifth Data Release (DR5) of LAMOST. The LAMOST (Large Sky Area Multi-Object Fiber Spectroscopic Telescope) features both a large field-of-view (about 20 deg2) and a large aperture (~4 m in diameter), which allow us to obtain 4000 spectra simultaneously. Its wavelength coverage ranges from
${\sim}3700{\AA}$ to$9000{\AA}$ with a spectral resolution of$R{\approx}1800$ . The Cygnus Loop is a prototype of middle-aged SNRs, which has advantages of being bright, large in angular size (${\sim}3.8^{\circ}{\times}3^{\circ}$ ), and relatively unobscured by dust. Along the line of sight of the Cygnus Loop, 2747 LAMOST DR5 spectra are found in total, which are spatially distributed over the entire remnant. Among them, 778 spectra are selected based on the presence of emission lines (i.e., [O III]${\lambda}5007$ , Ha, and [S II]${\lambda}{\lambda}$ 6717, 6731) for further visual inspection. About half of them (336 spectra) show clear spectral features to confirm their association with the remnant, 370 spectra show stellar features only, and 72 spectra are ambiguous and need further investigation. For those associated with the remnant, we identify emission lines and measure their intensities. Spectral properties considerably vary within the remnant, and we compare them with theoretical models to derive physical properties of the SNR such as electron density and temperature, and shock velocity. While some line ratios are in good agreement with model prediction, others cannot be explained by simple shock models with a range of shock velocities. We discuss these discrepancies between model predictions and the observations and finally highlight the powerfulness of the LAMOST data to investigate spatial variations of physical properties of the Cygnus Loop. -
G33.92+0.11, classified as a core-halo UC HII region at a distance of 7.1 kpc, contains several sub-clumps (~20-200 solar masses) as identified by dust continuum emission. This source shows very complicated features associated with vigorous massive star-forming activities with a nearly face-on projection. The ambient gas is still accreting to the massive molecular clumps dynamically, while the whole cloud is under disruption by newly formed stars. Using the recent high resolution (< 0.2") ALMA observations, we investigate the detailed structure associated with the star-forming activities by comparing different chemical tracers. The sub-clumps having extremely complex morphologies still preserve cold dense gas together with the turbulent and dense warm gas resulted by newly formed stars and interaction with accreting gas. The accretion of the ambient gas may have occurred episodically to this source. Most recent star formation, which probably the third generation of star formation in this region, is taking place in the northern part (A5 clump). The relatively small mass (~ 1/3 of A1 or A2) and the lack of turbulent gas of this star-forming core may suggest that this core was formed already during the overall collapse of the whole cloud for the first star formation. We think that gravitational collapse of these sub-clumps appears as sequential star formation of this region. The later interaction with accreting gas may have not been a direct cause of the star formation activities of this source.
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Kwon, Woojin;Stephens, Ian W.;Tobin, John J.;Looney, Leslie W.;Li, Zhi-Yun;Crutcher, Richard M.;Kim, Jongsoo;van der Tak, Floris F.S. 44.3
Magnetic fields affect star formation in a broad range of scales from parsec to hundreds au. In particular, interferometric observations and ideal magneto-hydrodynamic (MHD) simulations have reported that formation of a rotation-supported disk at the earliest young stellar objects (YSOs) is largely suppressed by magnetic fields aligned to the rotational axis of YSOs: magnetic braking. Our recent ALMA observations toward L1448 IRS 2, which has a rotation detected and its magnetic fields aligned to the rotation axis (poloidal fields) in ~500 au scales, show that the fields switch to toroidal at the center in ~100 au scales. This result suggests that magnetic braking may not be so catastrophic for early disk formation even in YSOs with magnetic fields aligned to the rotational axis. -
Formation of filaments and subsequent dense cores in ISM is one of the essential questions to address in star formation. To investigate this scenario in detail, we recently started a molecular line survey namely 'Filaments, the Universal Nursery of Stars (FUNS)' toward nearby filamentary clouds in Gould Belt using TRAO 14m single dish telescope equipped with a 16 multi-beam array. In the present work, we report the first look results of kinematics of a low mass star forming region L1478 of California molecular cloud. This region is found to be consisting of long filaments with a hub-filament structure. We performed On-The-Fly mapping observations covering ~1.1 square degree area of this region using C18O(1-0) as a low density tracer and 0.13 square degree area using N2H+(1-0) as a high density tracer, respectively. CS (2-1) and SO (32-21) were also used simultaneously to map ~290 square arcminute area of this region. We identified 10 filaments applying Dendrogram technique to C18O data-cube and 13 dense cores using FellWalker and N2H+ data set. Basic physical properties of filaments such as mass, length, width, velocity field, and velocity dispersion are derived. It is found that filaments in L~1478 are velocity coherent and supercritical. Especially the filaments which are highly supercritical are found to have dense cores detected in N2H+. Non-thermal velocity dispersions derived from C18O and N2H+ suggest that most of the dense cores are subsonic or transonic while the surrounding filaments are transonic or supersonic. We concluded that filaments in L~1478 are gravitationally unstable which might collapse to form dense cores and stars. We also suggest that formation mechanism can be different in individual filament depending on its morphology and environment.
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CS molecule is known to be adsorbed onto dust in cold dense cores, causing its significant depletion in the center region of cores. This study is aimed to investigate the depletion of CS molecule with optically thin
$C^{34}S$ molecular line observations, including significance of its differentiation depending on the evolutionary status of the dense cores. We mapped five evolved starless cores, L1544, L1552, L1689B, L694-2 and L1197 using two molecular lines,$C^{34}S$ (J=2-1) and$N_2H^+$ (J=1-0) with NRO 45 m telescope. The$H^2$ column density and temperature structures of each targets were obtained by SED fitting for Herschel continuum images and the internal number density profiles by model fitting. All of the integrated intensity maps of$C^{34}S$ show depletion holes and 'semi-ring-like' distribution, indicating that the depletion of CS is clear and general. The radial profiles of CS abundance also show significant decrease towards the core center, while$N_2H^+$ abundance is almost constant or enhanced. We find that the more evolved cores with higher$H^2$ density tend to have a stronger depletion of CS. Our data strongly support claims that CS molecule generally depletes out in the central regions of starless dense cores and such chemical differentiation is closely related to their evolution. -
Kim, Jaeyeong;Lee, Jeong-Eun;Aikawa, Yuri;Kim, Il-Seok;Lee, Ho-Gyu;Jeong, Woong-Seob;Noble, Jennifer A. 45.3
Although mass accretion from the disk to the central protostar is a key process of low mass star formation, the accretion mechanism is still poorly understood. To investigate "episodic accretion", which has been suggested as an accretion mechanism in low mass star formation, we have carried out near-infrared spectroscopic observations of three very low-luminosity objects (VeLLOs) and one background source, using InfraRed Camera onboard the AKARI space telescope. The ice absorption features of$H_2O$ ,$CO_2$ , and CO were detected around the wavelengths of 3.0, 4.26, and$4.67{\mu}m$ , respectively. In addition, we revealed the XCN ice feature, which is attributed to high energy UV photons produced by the episodic burst accretion. The comparisons of the ice abundances of our targets with those of other YSOs observed previously with AKARI IRC imply that the three VeLLOs had experienced burst accretions although they are now in a very quiescent phase. -
In order to investigate the origin of multiple stellar populations in the halo and bulge of the Milky Way, we have constructed chemical evolution models for the low-mass proto-Galactic subsystems such as globular clusters. Unlike previous studies, we assume that supernova blast waves undergo blowout without expelling the pre-enriched gas, while relatively slow winds of massive stars, together with the winds and ejecta from low and intermediate mass asymptotic-giant-branch stars, are all locally retained in these less massive systems. We find that the observed Na-O anti-correlations in metal-poor GCs can be reproduced when multiple episodes of starbursts are allowed to continue in these subsystems. A specific form of star formation history with decreasing time intervals between the stellar generations, however, is required to obtain this result, which is in good agreement with the parameters obtained from our stellar evolution models for the horizontal-branch. The "mass budget problem" is also much alleviated by our models without ad-hoc assumptions on star formation efficiency and initial mass function. We also applied these models to investigate the origin of super helium-rich red clump stars in the metal-rich bulge as recently suggested by Lee et al. (2015). We find that chemical enrichments by the winds of massive stars can naturally reproduce the required helium enhancement (dY/dZ = 6) for the second-generation stars. Disruption of proto-globular clusters in a hierarchical merging paradigm would have provided helium enhanced stars to the bulge field.
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Using the high-resolution observational data obtained by the Hubble Space Telescope, we found that there is the diversity of the radial trends of blue straggler stars (BSSs) in young massive clusters (YMCs) in the Large Magellanic Cloud unlike BSSs in old globular clusters usually showing the segregated radial distributions. To understand the dynamical processes that lead to the none-segregated or even inversely-segregated radial distribution of BSSs, we performed direct N-body simulations for YMCs. Our numerical simulations show that the presence of black hole subsystems inside the cluster centre can significantly affect the dynamical evolution of BSSs and eventually lead to none- or inversely-segregated radial distribution of BSSs.
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We present a general N-body exasolar system simulator in anticipation of upcoming searches for exoplanets and even exomoons by next generation telescopes such as James Webb Space Telescope. For habitable zones, traditionally defined by temperature, we here address the essential problem of dynamical stability of planetary orbits. Illustrative examples are presented on P-type orbits in stellar binary systems, that should be fairly common as in Kepler 16b. Specific attention is paid to reduced orbital lifetimes of exoplanets in the habitable zone by the stellar binary, that is propoesed by Maurice van Putten (2017). Especially, we focused on a classic work of complex three-body problem that is well known by Dvorak(1986). We charge his elliptic restricted three-body problem to extend unrestricted three-body problem to look into dynamical motions in view of circumbinary planet, furthermore, we suggest that opposite angular orientation of the planet is relative to the stability of orbits. In here, counter-rotation case is relatively more faster than co-rotation case for being stable. As a result, we find that various initial conditions and thresholds to approach dynamical stability and unstability with unexpectable isolated islands over enormous parameter space. Even, superkeplerian effect of binary is important to habitability of the exoplanet and we can verify that superfaster binary doesn't effect on th planet and increases survivality of planet around the binary.
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Jeong, Woong-Seob;Kim, Minjin;Im, Myungshin;Lee, Jeong-Eun;Pyo, Jeonghyun;Song, Yong-Seon;Park, Sung-Joon;Moon, Bongkon;Lee, Dae-Hee;Park, Won-Kee;Jo, Youngsoo;Lee, Duk-Hang;Ko, Kyeongyeon;Kim, Il-Joong;Park, Youngsik;Yang, Yujin;Ko, Jongwan;Lee, Hyung Mok;Shim, Hyunjin;Shin, Goo-Hwan;Chae, Jangsoo;Matsumoto, Toshio 47.1
The NISS (Near-infrared Imaging Spectrometer for Star formation history) onboard NEXTSat-1 have successfully developed by KASI. The capability of both imaging and spectroscopy is a unique function of the NISS. At first, it have realized the low-resolution spectroscopy (R~20) with a wide field of view of$2{\times}2deg$ . in a wide near-infrared range from 0.95 to$2.5{\mu}m$ . The major scientific mission is to study the cosmic star formation history in local and distant universe. It will also demonstrate the space technologies related to the infrared spectro-photometry in space. Now, the NISS is ready to launch in late 2018. After the launch, the NISS will be operated during 2 years. As an extension of the NISS, the SPEHREx (Spectro-Photometer for the History of the Universe Epoch of Reionization, and Ices Explorer) is the NASA MIDEX (Medium-class Explorer) mission proposed together with KASI (PI Institute: Caltech). It will perform the first all-sky infrared spectro-photometric survey to probe the origin of our Universe, to explore the origin and evolution of galaxies, and to explore whether planets around other stars could harbor life. Compared to the NISS, the SPHEREx is designed to have much more wide FoV of$3.5{\times}11.3deg$ . as well as wide spectral range from 0.75 to$5.0{\mu}m$ . After passing the first selection process, the SPHEREx is under the Phase-A study. The final selection will be made in the end of 2018. Here, we report the status of the NISS and SPHEREx missions. -
In this talk, we will review extragalactic science cases with NISS and SPHEREx. With its capability to perform a low resolution spectroscopy over a wide area, NISS and SPHEREx can provide valuable information about the evolution of spectral shapes of galaxies in different environments over cosmic history. This talk will focus on the cases for the studies that are closely related to the galaxy evolution and formation.
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SPHEREx is a proposed MIDEX mission, planned to conduct spectral imaging survey to cover 0.75-5 um with a spectral resolution of R~40-135. We will briefly overview the uniqueness of SPHEREx data, and how Korean community can take advantage of it. We will present extragalactic science cases that can be addressed with SPHEREx dataset. In particular, SPHEREx survey will uniquely provide the variability information of bright QSOs, both in continuum and fluxes of emission lines, which enables us to investigate the central structures of QSOs through the reverberation mapping method. SPHEREx will also allow us to understand how supermassive black holes and host galaxies co-evolve, by discovering new high-z QSOs, and investigating star formation properties in nearby QSOs.
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SPHEREx의 중요 임무 중 하나는
$0.75{\mu}m$ 와$5{\mu}m$ 사이에서$H_2O$ , CO,$CO_2$ , XCN, OCS, 그리고$CH_3OH$ 와 같은 얼음 분자의 전천 탐사 스펙트럼을 제공하는 것이다. 이러한 얼음 분자는 성간분자운의 먼지 티끌 표면에서 생성되어 별 탄생의 필연적 산물이며, 행성이 형성되는 원시행성계원반에서 다양한 변화를 겪게 되고, 복잡한 유기분자를 합성하게 된다. 하지만 충분하지 않은 관측 자료로 인해, 얼음 분자의 진화에 대한 이해가 미약한 상태이다. 현재까지는 근적외선에서 충분히 밝은 100 여개의 배경별이나 원시성에 대해서만 얼음 스펙트럼을 관측할 수 있었다. SPHEREx를 이용한 고감도 전천 탐사 미션은 약 20,000 여개의 배경별과 원시성에 대해 얼음 분자 스펙트럼을 제공할 것이다. 이렇게 100 배 이상 늘어난 샘플 스펙트럼 수로 인해, 얼음 분자의 진화에 대해서 통계적으로 의미있는 연구가 가능해 질 것이다. 본 발표에서는 SPHEREx의 Ice Program을 소개하고, 기대되어지는 결과에 대해서 논의하고자 한다. -
SPHEREx is expected to provide us with the opportunity of unbiased sampling of small Solar System objects along with near-infrared (
$0.75-5.0{\mu}m$ ) spectroscopic (R ~ 41) information. The estimated numbers of detections are tens of thousands for asteroids, thousands for Trojans, hundreds for comets, and several for Kuiper Belt Objects, Centaurs and Scattered Disk Objects. Wide spectral range covering many bands from carbon-bearing molecules and ices will enable us to systematically survey the volatile materials throughout the Solar System. SPHEREx will, for the first time, produce the near-infrared spectral map of the zodiacal light to pin-down the relative contributions of various populations of Solar System objects and interstellar dust to the dust grains in the interplanetary space. The study of the zodiacal light is also important to remove the foreground for the EBL (extragalactic background light) study, one of the main topics of the mission. -
We present the methodology to probe the initial condition of the universe using SPHEREx.
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대한민국 달탐사 시험용 궤도선은 2020년 말에 발사를 예정으로 위성개발이 진행되고 있다. KPLO(Korea Pathfinder Lunar Orbiter) 라고 명명된 달 궤도선에는 6개의 탑재체가 있으며, 경희대학교 우주탐사학과에서는 달 주위 공간 및 달 표면의 이상 자기장 영역을 관측하는 탑재체 (KMAG: Kplo MAGnetometer)를 개발하고 있다. 자기장센서는 3축 플럭스게이트 센서를 사용하며 약 0.2nT 이하의 분해능을 가지고 있다. 측정주기는 10Hz이며 총 무게는 3.5kg 이다. 1.2m 길이의 붐(Boom) 구조물 내부에 3개의 자기장 센서들을 설치하였으며 가능한 위성체로부터 거리를 두고 자기장을 측정하는 구조로 구성하였다. 시험모델 개발을 완료하고, 개발된 탑제체의 환경시험결과와 성능시험결과 요구조건에 부합되는 결과를 얻었다. KAMG는 국내최초의 심우주 탐사용 자기장 측정기로서 향 후, 행성 및 소행성 탐사 등에 활용하기 위한 기반 기술로 활용할 수 있을 것으로 기대한다.
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우주를 관측하기 위한 대부분의 천문학 미션을 위한 인공위성은 광학계를 가지는 망원경 구조물과 관측기기를 포함하고 있다. 망원경 구조물은 작은 렌즈 광학계에서 미터급의 대형 미러 광학계에 이르기까지 다양하며, 관측기기에 포함된 광학계는 그 용도에 따라서 다양한 형태를 보여준다. 이러한 광학계는 광기계 설계를 통한 광학계 지지구조물을 필수적으로 설계하며, 이 광기계 설계는 광학적 성능을 만족시키면서 광학계가 발사체의 진동, 충격 및 열진공의 우주환경을 모두 견뎌낼 수 있도록 설계해야만 한다. 이 발표에서는 최근 한국에서 수행한 천문우주 미션 경험을 바탕으로 실제 적용된 광학계 마운팅 기법을 사례별로 정리하고 그 연구결과를 소개하고자 한다.
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The MATS (Mesosphere Airglow/Aerosol Tomography Spectroscopy) satellite is the next Swedish science microsatellite. We report optical performance test results of the limb telescope, which is the major payload. This telescope is designed with "linear astigmatism-free" (LAF) off-axis optical system in order to have high optical performance across the wide field of view. We measured Modulation Transfer Function (MTF) and Encircled Energy Diameter (EED) of the limb telescope. Full field imaging tests show expected results without linear astigmatism across the full field of view (
$5.67^{\circ}{\times}0.91^{\circ}$ ). Since the amount of stray light is from the earth and the sun, we also simulated and measured the stray light in the field image. -
Flux calibration for narrow band photometric data gives us an opportunity to get a line flux of extended targets. We developed flux calibration processes for narrow band photometry using broad band filters as a continuum indicator. We derived parameters for color correction and zero point correction including color terms. Applying our method, we successfully subtracted continuum emissions and calibrated the emission lines from an FU Ori type object, V960 Mon.
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가시광 CCD나 HxRG 등의 적외선 어레이 디텍터는 천문관측기기를 구성하는 핵심부품으로, 관측기기의 종합 성능 결정에 중요한 영향을 미친다. 따라서 디텍터의 성능을 정확하게 진단하는 것은 관측기기의 성능을 예측하거나 유지 또는 개선하는데 중요한 요소가 된다. 한국천문연구원은 최근에 디텍터 성능을 직접적으로 측정할 수 있는 광전자 시스템을 구축하고 장치를 구동하기 위한 소프트웨어를 자체 개발하였다. 본 시스템을 기반으로 Andor iKon-M 카메라 CCD의 시스템 게인, 최대 포화전자수, 감도, 비선형성, 양자효율, 암전류, 읽기 잡음, 불량 픽셀의 특성을 측정하였으며 특히, 양자효율의 경우 디텍터의 구동 온도에 따라 파장별로 2%에서 30% 이상까지 편차가 발생하는 것을 확인하였다. 본 연구는 디텍터의 성능 평가와 그 중요성에 대하여 논의한다.
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Measurement result of ultra wideband corrugated horn for combined ALMA band 7 and band 8 frequenciesWe present measurement results of the fabricated ultra wideband corrugated horn for the planned ASTE band7+8 receiver. Return loss and vector beam pattern measurements were carried out over 275-500 GHz frequency range. Hardware set-ups for these measurements are described as well as beam measurement data are compared with such design criteria as beam width, phase curvature and cross-polarization. We discuss the impact of these beam measurement results to the aperture efficiency of the proposed 2-mirror receiver optics for the ASTE telescope.
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Korean chronicles have a large amount of observational records over two thousand years. Many historical astronomical records are useful in modern times. In this study, we examined solar eclipses in Goguryeo-bongi(高句麗本紀) by using the modified(newest) nutation value and reviewed the observation area through eclipsing map. There are 11 solar eclipse records in the book. We calculated intersectional visible area with 0.6 eclipsing magnitude using the records of AD116, 124, 149, 158 and 219 and found the observational area of
$N40-43^{\circ}$ and$E123-127^{\circ}$ , which corresponds to the Liaodong(遼東). We also examined historical Chinese solar eclipse records and compared them with Korean eclipses. -
Kang, Wonseok;Kim, Taewoo;Kim, Jeongeun;Shin, Yong Cheol;Yoo, Jihyun;Jeong, Shinu;Choi, Yoonho;Kwon, Sun-gill 50.1
We present the development of tools for Echelle spectrograph of NYSC 1-m telescope. The eShel spectrograph(Shelyak) has operated at Deokheung Optical Astronomy Observatory since 2016. We carried out test observation in 2016 and completed the preprocessing and wavelength calibration of the spectroscopic data using IRAF. Based on the reduction process in IRAF, PySpecW, a set of tools for spectroscopic data was developed in 2017. PySpecW was optimized for NYSC 1m telescope, and written in Python for youth to use easily on any OS. PySpecW consists of preprocessing, aperture tracing, aperture extraction, wavelength calibration, and dispersion correction for extracted spectra. -
Kim, Taewoo;Kim, Jeongeun;Shin, Yong Cheol;Yoo, Jihyun;Jeong, Shinu;Choi, Yoonho;Kang, Wonseok;Kwon, Sun-gill 50.2
국립청소년우주센터 덕흥천문대의 NYSC 1m 망원경은 청소년을 대상으로 관측제안서를 공개모집하고, 청소년의 전문적인 천문관측을 지원하고 있다. 2017년 한 해, 접수된 청소년의 관측제안은 총 10건이었다. 이외에도 덕흥천문대는 양질의 관측자료를 국내 연구팀과의 공동연구를 통해 제공하고 있으며, 공동연구 장기관측과제 3건을 운영 중에 있다. 덕흥천문대 관측팀은 청소년 관측 및 공동연구를 지원하는 것과 더불어 망원경의 상태를 상시 점검하고 있다. 스티커 및$CO_2$ 분사를 이용한 경면 세척을 진행하였고, 2017년 하반기에는 1m 망원경의 성능을 최대로 발휘할 수 있도록 CCD 카메라를 Princeton Instruments의 SOPHIA 2048B로 교체하였다. 그리고 앞으로 덕흥천문대에서 진행할 향후 운영 계획에 대해서도 논하고자 한다. -
Lyo, A Ran;Kang, Wonseok;Kwon, Sun-gill;Kim, Min Gyu;Kim, Yonggi;Kim, Woong-Tae;Kim, Taewoo;Moon, Hong-Kyu;Pak, Soojong;Park, Soon Chang;Park, Changbom;Shin, Yongcheol;Lee, Kang Hwan;Lee, Dukhang;Lee, Myung Gyoon;Lee, Sang Gak;Lee, Sang Hyun;Lee, Jeong Ae;Lee, Hye-In;Yim, Insung;Han, JaEun;Hyun, Minhee;Lee, Kyungyong;Evans, John Ashley 50.3
2018년부터 한국천문학회 특별 사업단으로 교육, 홍보위원회에 해외교육지원단이 만들어졌다. 해외교육지원단은 지난 2년 동안 한국천문학회가 지원해오던 캄보디아 천문교육지원 활동을 확장하고 체계적인 운영을 목표로 만들어졌다. 먼저, 그동안의 활동에 대해 보고하고 좀 더 내실 있는 계획을 세우기 위해 천문학회 회원들의 의견과 조언을 듣고자 한다. 첫 번째 캄보디아 천문학 교육은 2016년 6월 13-24일(2주) 동안 수도 프롬펜에서 북서쪽, 차편으로 4시간 거리에 있는 뿌삿시 끄로압에서 이루어졌다. 초. 중등학생 50여명이 참여하여 망원경 조작 방법을 배우고, 종이 망원경과 카메라 만들기, 태양과 행성 관측, 축구공, 야구공, 풍선과 찰흙을 이용한 태양계 행성들 크기 비교, 별자리판 만들기와 천문학 여러 현상들에 대한 비디오 영상 보기와 같은 다양한 프로그램을 수행하였다. 두 번째 교육은 국립청소년우주센터와 캄보디아의 Xavier Jesuit School이 연계하여 2017년 4월 3-7일(5일) 동안 지역 중등과학교사 18명을 대상으로 천문교육을 진행하였다. 시간과 좌표, 간이 망원경 제작, 결상의 원리, 분광, 망원경의 조립과 분해 및 천체관측 등 천체관측과 관련된 내용을 위주로 교육을 진행하였다. -
Jung, Taehyun;Byun, Do-Young;Lee, Sang-Sung;Mihn, YoungChol;Cho, Se-Hyung;Sohn, Bong Won;Kim, Kee-Tae;Wi, Seog-Oh;Han, Seog-Tae;Kim, Hyun Goo;Kim, Jongsoo 50.4
한국우주전파관측망(KVN: Korean VLBI Network)은 서울, 울산, 제주에 직경 21m 전파망원경 3기로 이루어진 우리나라 최초의 초장기선 전파간섭계(VLBI: Very Long Baseline Interferometry)이다. KVN은 밀리미터 파장의 22, 43, 86, 129 GHz 대역을 동시에 관측할 수 있는 수신시스템을 이용하여 독보적인 다파장 관측연구를 진행해오고 있으며, 뛰어난 위상보정 성능을 바탕으로 기존의 밀리미터 대역에서 검출되지 않았던 많은 천체들을 검출하고 있다. 하지만, KVN 3기 VLBI 관측으로부터 얻어지는 천체의 합성영상(synthesized image)은 초미세구조에서 발생하는 물리 기작을 연구하기에는 한계를 지닌다. 따라서 KVN을 활용한 연구 성과를 극대화하기 위한 최적의 방안을 도출하기 위하여, KVN 확장 기획연구를 진행하였다. 본 발표에서는 KVN 확장에 따른 예상 성능과 이릍 통한 과학연구를 소개한다. -
Wajima, Kiyoaki;Hada, Kazuhiro;Jung, Taehyun;Oh, Se-Jin;Roh, Duk-Gyoo;Jiang, Wu;Cui, Lang;Byun, Do-Young;Kim, Jongsoo;Honma, Mareki;Shen, Zhi-Qiang;Wang, Na 51.1
동아시아 VLBI 관측망(East-Asian VLBI Network; EAVN)은 한 중 일 각국의 전파망원경을 통합해서 구성되는 동아시아 지역의 새로운 VLBI 네트워크이다. EAVN은 2013년부터 공동이용관측을 실시하고 있는 한일 VLBI 관측망(KaVA)을 중심으로 총 20개 전파망원경을 포함한다. 4개 주파수(6.7/8/22/43 GHz)로 관측할 수 있으며, 최대로 0.6 mas (22 GHz)의 해상도로 관측할 수 있는 기능을 가지고 있다. 우리는 2017년 3월부터 5월까지 EAVN을 이용한 총 17번의 AGN 관측 캠페인을 실시하였다. 이것은 ALMA를 이용한 Event Horizon Telescope (EHT) 관측과 같은 시기에 실시되며, 총 15개의 전파망원경이 참가하였다. 이 관측을 통해서 EAVN으로 얻은 영상이 KaVA의 영상에 대해 80% 정도 성능이 개선되는 것을 확인하였다. 또한, 주된 관측천체인 M87과 Sgr A*의 영상은 과거의 결과를 재현해서 AGN 중심 주변의 sub-pc 스케일의 제트 구조를 보다 자세히 볼 수가 있었다. 이 결과에 의거해서 우리는 KaVA의 관측시간의 일부를 이용해서 2018년 하반기부터 EAVN의 공동이용관측을 시작한다. 공개될 범위는 KaVA, 일본 Nobeyama 45 m, 중국 Tianma 65 m의 총 9개 망원경이며, 중국 Nanshan 26 m 망원경도 Large Program 관측에 한해서 참가한다. 관측주파수는 22 GHz (KaVA + Tianma) 및 43 GHz (KaVA + Tianma + Nobeyama) 이며, 오는 관측시즌(2018년 8월부터 2019년 1월까지)에 제공될 총 관측시간은 100 시간이다. 관측제안서 제출 마감날은 6월 1일이며, 많은 관측제안서가 제출될 것을 기대한다. 이 발표에서는 EAVN AGN 캠페인의 결과 및 EAVN 공동이용 관측의 자세한 내용을 보고한다. -
Geem, Jooyeon;Ishiguro, Masateru;Bach, Yoonsoo P.;Kuroda, Daisuke;Naito, Hiroyuki;Kim, Yoonyoung;Kwon, Yuna G.;Imai, Masataka;Kuramoto, Kiyoshi;Watanabe, Makoto;Okazaki, Ryo 51.2
Polarimetry is a powerful technique to investigate the physical properties of surface materials on airless bodies in the solar system. It is known that the degree of linear polarization changes as a function of the phase angle (the angle between Sun-target-Observer). Especially, the dependency of the polarization degree at large phase angle allows us to obtain information related to the particle size and porosity, which is difficult to be determined via other observation techniques (i.e., photometry and spectroscopy). However, despite the advantage, only a few asteroids were observed with polarimetric devices at large phase angles. Here, we present our new polarimetric research of Near-Earth Asteroids (NEAs) observed at the large phase angles. Among the NEAs, we focus on S- and Q-type asteroids, which include: (331471) 1984 QY1, (90075) 2002 VU94, and (66391) 1999 KW4. The observation was conducted using the Pirka 1.6-m Telescope at the Nayoro Observatory of Hokkaido University at the phase angles${\alpha}{\sim}100degree$ , which provides us the maximum polarization degrees of these objects. Considering the observational results together with two objects ((1566) Icarus and (4179) Toutatis) in reference papers [1], [2], we will discuss the implication of the regolith size on their surfaces. -
Since Voyager 1 passed the Heliopause in 2012, it has provided the observations of the charged particles in the local interstellar medium. However, Voyager 1 only provides the information along with its trajectory. In order to understand the global view of the interstellar plasma flow surrounding the Heliopause, we need another tool. When the interstellar plasmas approach the Heliopause, the ions are deflected around the Heliopause due to the draping of the interstellar magnetic field. The draping of the interstellar magnetic field is strongly connected with the shape of the Heliopause. A fraction of the diverted ions exchanges their charges with the undisturbed primary interstellar neutral atoms, and then the ions become neutral atoms called the secondary interstellar neutral atoms. The newly created neutral atoms carry information on the diverted flow of the interstellar ions, and a fraction of them can travel to the Sun. Therefore, the secondary component of the interstellar neutrals is an excellent diagnostic tool to provide important information to constrain the shape of the Heliopause. The secondary interstellar neutrals are observed by Interstellar Boundary Explorer (IBEX) at Earth's orbit. Since 2009, two energetic neutral atom cameras on IBEX have measured neutral atoms and it has provided sky maps of neutral atoms. In this presentation, we will discuss the directional distribution of the secondary interstellar neutrals at Earth's orbit. In the sky maps, the primary interstellar neutral gas is seen between
$200^{\circ}$ and$260^{\circ}$ in ecliptic longitude and the secondary components are seen in the longitude range of$160^{\circ}-200^{\circ}$ . We also present a simplified model of the outer heliosheath to help interpret the observations of interstellar neutrals by the IBEX-Lo instruments. We extract information on the large-scale shape of the Heliopause by comparing the neutral flux measured at IBEX along four different look directions with simple models of deflected plasma flow around hypothetical obstacles of different aspect ratios to the flow. Our comparisons between the model results and the observations indicate that the Heliopause is very blunt in the vicinity of the Heliospheric nose, especially compared to a Rankine half-body or cometary shape. -
We investigate initial Fe/O enhancements for 44 large gradual solar energetic particles events from 2010 to 2014 and examine the associations of the Fe/O enhancements with the structures of the heliospheric current sheet (HCS). For this study, we use STEREO SIT Fe and O data in 0.32-0.45 MeV channel as well as ACE ULEIS Fe and O data in 0.32-0.64 MeV channel. We determine 1) the magnetic polarities of the SEP source regions using the potential field source surface (PFSS) model of the coronal field and 2) the spacecraft magnetic footpoints with Parker spiral approximation of interplanetary magnetic field using the in-situ measurements of STEREO and ACE. We find that 29 out of 44 events have initial Fe/O enhanced more than 5 times of the typical gradual event values. In the 6 events, the enhancements are simultaneously observed by two spacecraft. There is a tendency that the high Fe/O enhancements are observed near SEP source regions. It is also noted that the Fe/O enhancements are associated with the polarity of the magnetic footpoints. The high Fe/O enhancements are usually observed where their footpoints lie in the same polarity regions of SEP sources rather than the opposite polarity regions. Although Fe/O enhancements could be due to a transport effect and/or a flare contribution, our result implies that the structure of HCS is likely to affect particle propagations in the interplanetary space.
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Liu, Hongyu;Chen, Yao;Cho, Kyungsuk;Feng, Shiwei;Vasanth, Veluchamy;Koval, Artem;Du, Guohui;Wu, Zhao;Li, Chuanyang 52.2
A stationary Type IV (IVs) radio burst was observed on September 24, 2011. Observations from the Nançay RadioHeliograph (NRH) show that the brightness temperature (TB ) of this burst is extremely high, over 10^11K at 150 MHz and over 10^8K in general. The degree of circular polarization (q ) is between -60%~-100%, which means that it is highly left-handed circularly polarized. The flux-frequency spectrum follows a power-law distribution, and the spectral index is considered to be roughly -3~-4 throughout the IVs. Radio sources of this event are located in the wake of the coronal mass ejection and are spatially dispersed. They line up to present a formation in which lower-frequency sources are higher. Based on these observations, it is suggested that the IVs was generated through electron cyclotron maser emission. -
During a major solar eruption, the erupting plasma is possibly out of the equilibrium ionization state because of its rapid heating or cooling. The non-equilibrium ionization process is important in a rapidly evolving system where the thermodynamical time scale is shorter than the ionization or recombination time scales. We investigate the effects of non-equilibrium ionization on EUV and X-ray observations by the Atmospheric Imaging Assembly (AIA) on board Solar Dynamic Observatory and X-ray Telescope (XRT) on board Hinode. For the investigation, first, we find the emissivities for all the lines of ions of elements using CHIANTI 8.07, and then we find the temperature responses multiplying the emissivities by the effective area for each AIA and XRT passband. Second, we obtain the ion fractions using a time-dependent ionization model (Shen et al. 2015), which uses an eigenvalue method, for all the lines of ion, as a function of temperature, and a characteristic time scale,
$n_et$ , where$n_e$ and t are density and time, respectively. Lastly, the ion fractions are multiplied to the temperature response for each passband, which results in a 2D grid for each combination of temperature and the characteristic time scale. This is the set of passband responses for plasma that is rapidly ionized in a current sheet or a shock. We investigate an observed event which has a relatively large uncertainty in an analysis using a differential emission measure method assuming equilibrium ionization state. We verify whether the observed coronal plasmas are in non-equilibrium or equilibrium ionization state using the passband responses. -
We perform seismological diagnostics of the physical parameters in umbral photospheres and G-band bright points. The technique is based on the theory of slow magneto-acoustic waves in a non-isothermally stratified photosphere with uniform vertical magnetic fields. For the seismology of sunspot umbrae, we calculate the weighted frequency of three-minute oscillations observed by SDO/HMI continuum and use it to estimate the Alfvn speed and plasma-beta, which range 7.5-10.5 km/s and 0.65-1.15, respectively. We identify and track bright points in the G-band movie by using a 3D region growing method. Then we apply the seismological diagnostics to the bright points in the Hinode/BFI Blue continuum. We will present the Alfvn speed and plasma-beta in the bright points.
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Solar Proton Events (SPEs) are the energetic phenomena related particle acceleration occurred in solar corona. Conventionally, they have been classified into two groups as the impulsive and gradual cases caused by reconnection in the flaring site and by shock generated by CME, respectively. In the previous studies, we classified these into four groups by analyzing the proton acceleration patterns in multi-energy channel observation. This showed that acceleration due to the magnetic reconnection may occur in the corona region relatively higher than the flaring site. In this study, we analyzes 54 SPEs observed in the energy band over 25 MeV from 2009 to 2013, where STEREO observations as well as SOHO can be utilized. From the multi-positional observation, we determine the exact time at which the Sun-Earth magnetic field line meets the CME shock structure by considering 3-dimensional structure of CME. Also, we determine the path length by considering the solar wind velocity for each event, so that the SPE onset time near the sun is obtained more accurately. Based on this study, we can get a more understanding of the correlation between CME progression and proton acceleration in the solar coronal region.
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For space weather forecast, it is important to determine three-dimensional parameters of coronal mass ejections (CMEs). To estimate three-dimensional parameters of CMEs, we have developed a full ice-cream cone model which is a combination of a symmetrical flat cone and a hemisphere. By applying this model to 12 SOHO/LASCO halo CMEs, we find that three-dimensional parameters from our method are similar to those from other stereoscopic methods. For several geoeffective CME events, we determine CME mass by applying the Solarsoft procedure (e.g., cme_mass.pro) to SOHO/LASCO C3 images. CME volumes are estimated from the full ice-cream cone structure. We derive CME mean density as a function of CME height for these CMEs, which are approximately fitted to power-law functions. We find that the ICME mean densities extrapolated from the power law functions, are correlated with their corresponding ICME ones in logarithmic scales.
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It is important to understand very fast CMEs which are the main cause of geomagnetic storms and solar particle events (SPEs). During this solar cycle 24, there are 10 very fast CMEs whose speeds are over 2000 km/s. Among these, there were only two fronside events (2012 January 23 and 2012 March 7) and they are associated with two major flares (M8.7 and X5.4) and the most strong SPEs (6310 pfu and 6530 pfu). They have a similar characteristics: there were successive CMEs within 2 hours in the same active region. We analyze their magnetic properties using SDO HMI magnetograms and kinematic ones from STEREO EUVI/COR1/COR2 observations. We can measure their speeds and initial accelerations without projection effects because their source locations are almost the limb. Additionally, we are investigating magnetic and kinematic characteristics of 8 backside events using AI-generated magnetograms constructed by deep learning methods.
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In this study, we perform a statistical investigation on the kinematic classication of 4264 coronal mass ejections (CMEs) from 1996 to 2015 observed by SOHO/LASCO C3. Using the constant acceleration model, we classify these CMEs into three groups; deceleration, constant velocity, and acceleration motion. For this, we devise four dierent classication methods by acceleration, fractional speed variation, height contribution, and visual inspection. Our major results are as follows. First, the fractions of three groups depend on the method used. Second, about half of the events belong to the groups of acceleration and deceleration. Third, the fractions of three motion groups as a function of CME speed classied by the last three methods are consistent with one another. Fourth, according to the last three methods, the fraction of acceleration motion decreases as CME speed increases, while the fractions of other motions increase with speed. In addition, the acceleration motions are dominant in low speed CMEs whereas the constant velocity motions are dominant in high speed CMEs.
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Propagating speeds of coronal mass ejections (CMEs) have been calculated by several geometrical models based on multi-view observations (STEREO/SECCHI and SOHO/LASCO). But in 2015, we were unable to obtain radial velocity of a CME because the STEREO satellites were located near the backside of the sun. As an alternative to resolve this problem, we propose a method to combine a coronal shock front, which appears on the outermost of the CME, and an EUV-wave that occurs on the solar disk. According to recent studies, EUV-wave occurs as a footprint of the coronal shockwave on the lower solar atmosphere. In this study, the shock, observed as a bubble shape, is assumed as a perfect sphere. This assumption makes it possible to determine the height of a coronal shock, by matching the position of an EUV-wave on the solar disk and a coronal shock front in coronagraph. The radial velocity of Halo-CME is calculated from the rate of coronal shock position shift. For an event happened on 2011 February 15, the calculated speed in this method is a little slower than the real velocity but faster than the apparent one. And these results and the efficiency of this approach are discussed.
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Studies on rotation-powered pulsars with strong surface magnetic field may help us clarify the unclear link between magnetars and canonical radio pulsars because the magnetar-like emission is expected to be observed. PSR J1119-6127 associated with SNR G292.2-0.5 has a high magnetic field of
$4.1{\times}1013$ gauss, and a young characteristic age of ~1700 years can be served as the good candidate to compare with magnetars and rotation-powered pulsars. The glitch accompanied by the radiative changes detected in 2007 is the first case we observed for a rotationally powered radio pulsar. This pulsar experienced magnetar-like outbursts in mid. 2016, similar to the 2006 transition occurred on the other radio-quiet rotation-powered pulsar with strong surface magnetic field, PSR J1846-0258. In this talk, I'll report the investigation with X-ray and gamma-ray data of this magnetar-like pulsar. A sudden decrease in the gamma-ray emission at the GeV band was detected immediately after the X-ray outburst. Accompanying with the disappearance of the radio pulsation, the gamma-ray pulsation cannot be resolved as well after the outburst. We tried to derive the timing behavior and some intriguing features of this pulsar in this work corresponding to the outburst using the Swift data, NuSTAR and XMM observations. -
Neutron stars (NS) are rapidly spinning compact objects. Their rotation energy is released by particles, electromagnetic waves, and even gravitational waves. The source of the energy is of course the rotation, so by studying the rotational properties of neutron stars, we can gain some insights into matter under extreme conditions. In particular, it is known that the braking index n is sensitive to the moment of inertia and/or NS winds. The neutron star PSR B0540-69 exhibits interesting timing behavior; previous measurements of the braking index for this pulsar may suggest a change in time. In order to see if the change is real, We investigate the timing properties of B0540-69 using recent ~1000-days Swift satellite data.
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Magnetars are neutron stars powered by strong magnetic field (B >
$10^{14}G$ ). Their spin period is in the range of 2 - 12s. The magnetic stress in the star may distort the crust (observed as outbursts), so magnetars (especially in outbursts) may emit gravitational waves. There are 29 magnetars known (potential gravitational waves sources), and increasing the number will increase the chance of detecting low-frequency gravitational waves. In addition, magnetars can be used for studying matter under extreme condition. In this study, we searched for more magnetars using extensive Chandra archival data and found 11 candidates. Due to the limited sensitivity of Chandra, form identification cannot be made, and more sensitivity X-ray data are needed. -
Tidal disruption events (TDEs) provide evidence for quiescent supermassive black holes (SMBHs) in the centers of inactive galaxies. TDEs occur when a star on a parabolic orbit approaches close enough to a SMBH to be disrupted by the tidal force of the SMBH. The subsequent super-Eddington accretion of stellar debris falling back to the SMBH produces a characteristic flare lasting several months. The theoretically expected bolometric light curve decays with time as proportional to
$t^{-5/3}$ . However, the light curves observed in most of the optical-UV TDEs deviate from the$t^{-5/3}$ decay rate especially at early time, while the light curves of some soft-X-ray TDEs are overall in good agreement with the$t^{-5/3}$ law. Therefore, it is required to construct the theoretical model for explaining these light curve variations consistently. In this paper, we revisit the mass fallback rates analytically and semi-analytically by taking account of the structure of the star, which is simply modeled by the polytrope. We find the relation between a polytropic index and the power law index of the mass fallback rate. We also discuss whether and how the decay curves, which we derived, fit the observed ones. -
Astrophysical shocks accelerate particles to high velocities, which we observe as cosmic rays. The acceleration process changes the nature of the shock because the particles interact with the local magnetic field, removing energy and potentially triggering instabilities. In order to simulate this process, we need a computational method that can handle large scale structures while, at the same time, following the motion of individual particles. We achieve this by combining the grid magnetohydrodynamics (MHD) method with the particle-in-cell (PIC) approach. MHD can be used to simulate the thermal gas that forms the majority of the gas near the shock, while the PIC method allows us to model the interactions between the magnetic field and those particles that deviate from thermal equilibrium. Using this code, we simulate shocks at various sonic and Alfvenic Mach numbers in order to determine how the behaviour of the shock and the particles depends on local conditions.
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The present study formulates the theory of spontaneously emitted electromagnetic fluctuations in magnetized plasmas containing particles with an anisotropic suparthermal (bi-Kappa) velocity distribution function. The formalism is general applying for an arbitrary wave vector orientation and wave polarization, and for any wave-frequency range. As specific applications, the high-frequency electromagnetic fluctuations emitted in the upper-hybrid and multiple harmonic electron cyclotron frequency range are evaluated. The fluctuations for low-frequency are also applied, which include the kinetic
$Alfv\acute{e}n$ , fast magnetosonic/whistler, kinetic slow mode, ion Bernstein cyclotron modes, and higher-order modes. The model predictions are confirmed by a comparison with particle-in-cell simulations. The study describes how energetic particles described by kappa velocity distribution functions influence the spectrum of high and low frequency fluctuations in magnetized plasmas. The new formalism provides quantitative analysis of naturally occurring electromagnetic fluctuations, and contribute to an understanding of the electromagnetic fluctuations observed in space plasmas, where kappa-distributed particles are ubiquitous. -
Kimm, Taysun;Katz, Harley;Haehnelt, Martin;Rosdahl, Joakim;Devriendt, Julien;Slyz, Adrianne 57.1
Reionisation in the early Universe is likely driven by dwarf galaxies. Using cosmological RHD simulations, we study star formation and the escape of Lyman continuum (LyC) photons from mini-haloes with Mhalo<108Msun. We find that feedback reduces star formation very efficiently in mini-haloes, resulting in the stellar mass consistent with the empirical stellar mass-to-halo mass relation derived in the local Universe. Because star formation is stochastic and dominated by a few gas clumps, the escape fraction in mini-haloes is generally determined by photo-ionization, rather than supernova explosions. We find that the photon number-weighted mean escape fraction in mini-haloes is higher (20-40%) than that in atomic-cooling haloes. Despite their high escape fractions, LyC photons from mini-haloes are of minor importance for reionization due to inefficient star formation. We confirm previous claims that stars in atomic-cooling haloes with masses$10^8M_{sun}$ $10^{11}M_{sun}$ are likely to be the most important source of reionization. -
Poojon, Panomporn;Chung, Aeree;Lee, Bumhyun;Baek, Junhyun;Jung, Taehyun;Sohn, Bong Won;Oh, Se-Heon;Sengupta, Chandreyee 57.2
We present the preliminary result from our KVN single-dish observations of the MALATANG sample. The MALATANG (Mapping the dense molecular gas in the strongest star-forming Galaxies) is one of the JCMT legacy surveys on the nearest 23 IR-brightest galaxies beyond the Local Group. The goal of the MALATANG survey is to map the sample in the dense gas tracers (HCN and HCO+J=4-3), and probe the relationships between the dense molecular gas and star formation activities. As a complementary study, we recently launched a KVN/KaVA program on the same sample, in order to measure their flux densities and parsec-scale jet/outflows in the millimeter regime, which will be greatly useful in understanding the initial conditions of the feedback process. In this work, we present the preliminary result from our pilot KVN single-dish program on a sub-sample, which will be used to select the future VLBI imaging study under plan. We investigate the KVN spectral energy distributions (SED) of the sample as a function of the power source of the luminous IR brightness of each target (starburst? AGN? or hybrid?). We also discuss the technical challenges that we experienced during our KVN observations due to the large size of the sample in the sky. -
We explore the role of various environments in triggering star formation (SF) and narrow-line active galactic nucleus (AGN) in SDSS spiral galaxies and the SF-AGN connection, using a volume-limited sample with
$M_r$ < -19.5 and 0.02 < z < 0.055 selected from the SDSS Release 7. To avoid the dependency of AGN activity on bulge mass, the central velocity dispersion of the sample galaxies is limited to have a narrow range of$130{\leq}{\sigma}{\leq}200km\;s^{-1}$ . We note that in gas sufficient galaxies, AGN feeding lags behind starburst, whereas as the gas exhausts, the SF slows down and AGN seems to even prevent the SF, and thus divide the high-${\sigma}$ sample into two subsamples according to their cold gas content at central region traced by fiber star formation rate,$SFR_{fib}$ . We find that a high density (cluster) environment causes a significant increase in AGN activity as well as gas depletion in host galaxies. However, the finding is only noticeable in the high-${\sigma}$ and low$SFR_{fib}$ sample. It seems that a galaxy interaction with the nearest neighbor directly affects the SF of the central region. However, it is unclear whether it directly affects AGN activity. -
The redshift range
$1.4{\lesssim}z{\lesssim}2.5$ is often called the 'redshift desert' because of the difficulties in measuring spectroscopic redshifts due to the shifting of the major spectroscopic features into near-infrared wavelength (Steidel et al. 2004). One of the most efficient and fast way to select galaxies at this redshift range is the BzK technique designed by Daddi et al. (2004). Combining deep BVRz data from Deep Lens Survey with the wide-field (~4.08 deg2) K-band image, we select 1200 star-forming BzKs (sBzKs) and 120 passive BzKs (pBzKs) at K < 21.25. We discuss about the photometric redshifts, star formation rates, and stellar mass of the selected BzKs. Possible large scale structure at$1.4{\lesssim}z$ < 1.6 based on the spatial distribution of the BzKs is also introduced. -
Fossil groups of galaxies have characteristic features of a dominant central elliptical galaxy (
${\Delta}M_{12}$ > 2 in$0.5R_{vir}$ ) embedded in highly relaxed X-ray halo, which indicates dynamically stable and evolved systems. These are thought as a final stage of the evolution of galaxy groups in the hierarchical structure formation scenario. However, the formation and evolution of fossil clusters are still unclear due to lack of detailed studies. Therefore, we perform a kinematic research of a known fossil cluster Abell 2261 (A2261 hereafter) using spectroscopic data of 589 galaxies in the A2261 field. Even though A2261 is known as a fossil cluster, previous studies found several unusual features such as quite high X-ray entropy for a stable cluster, and an elongated shape, which are not expected in standard fossil clusters. Using the caustic method, we identify cluster member galaxies and discover a second bright galaxy (${\Delta}M_{12}=1.68$ ) at${\sim}1.5R_{vir}$ . The presence of such a bright galaxy can break the current fossil state of cluster in the near future. In addition, with two independent substructure finding methods, we confirm that the previously detected elongated galaxy distribution of the cluster is a real feature. These findings indicate that A2261 is not in a fully stable state, unlike the existing fossil definition diagnostic. We require a more stringent criterion for the fossil definition to represent a genuinely final stage of cluster evolution. -
Moon, Hyeonwoo;Park, Keun-Hong;Yoon, Tae Seog;Sung, Hyun-Il;Kim, Soo Hyun;Han, Ilseung;Park, Sunkyung 58.3
We present the results of high resolution spectral analysis for Type Ia supernova SN 2014J in M82, which was discovered on 21 January 2014 UT. We performed spectroscopic observations for SN 2014J in its early phase at Bohyunsan Optical Astronomy Observatory with the high resolution echelle spectrograph BOES attached to 1.8-m reflector. Spectra of 26 epochs in 6 nights were obtained from 22 January 2014 to 23 February 2014 UT. Spectral feature variations for several significant lines including Si II and Ca II lines will be shown and discussed. -
On 2018 February 5 a gamma ray burst with trigger time 04:25:29.3 UT was detected by Swift BAT and this event was named GRB 180205A. We observed the optical afterglow of GRB 180205A starting from about 1 hour after the burst until February 22 in the optical bands with the 1m telescope of Deokheung Optical Astronomy Observatory (DOAO), the 1m telescope at Mt. Lemmon Optical Astronomy Observatory(LOAO) and the 0.8m and 0.25m telescopes at McDonald Observatory. According to the fireball model, which is a well-accepted and conventional model for the afterglow of the GRB, the mechanism of the afterglow is that the expanding external blast wave of the GRB successively collides with the ambient medium and loses its energy, and as a result emits radiation at wavelengths longer than gamma rays. Here we present optical photometry and light curve of the afterglow in the R band and analyze it to characterize GRB 180205A.
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Recent studies of galaxy clusters have shown that the galaxy clusters in dense environment tend to have lower star formation rate in local universe with z < 1. However, this correlation is not significant in galaxy clusters with z > 1. The study of galaxy clusters around z=1 can yield insight into cosmological galaxy evolution. Nevertheless, the identification of galaxy clusters beyond the scope of immediate local universe requires wide field data in optical and near-infrared bands. By incorporating data from Canada-France-Hawaii Telescope Legacy Survey(CFHTLS) and Infrared Medium-Deep Survey(IMS), the photometric redshifts of galaxies in CFHTLS W2 field were calculated. Using spatial distribution and photometric redshifts, the galaxies in the field were divided into redshift bins. The image of each redshift bin was analyzed by measuring the number density within proper distance of 1Mpc. By comparing high density regions in consecutive redshift bins, we identified the cluster candidates and mapped the large-scale structure within the CFHTLS W2 field.
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With a recent observational study of extended Lyman-alpha halos around individual high-z star-forming galaxies by Leclercq et al. (2017) using MUSE, we perform radiative transfer calculations to see if Lyman-alpha scattering can explain the spatial extents of the halos together with their spectra. We adopt a spherically-symmetric halo model in which Lyman-alpha sources and neutral hydrogen (HI) medium have exponential density distributions. The HI medium is set to have outflowing motion based on a momentum-driven wind scenario in a gravitational potential well. We run our Lyman-alpha radiative transfer code, LaRT, upon this halo model for various sets of parameters regarding the HI medium such as temperature, optical depth, density scale radius, outflow velocities, and dust content. We analyze simulation results to see the impact of each parameter on Lyman-alpha spectra and surface brightness profiles, and degeneracies between the parameters. We also find a parameter set that best reproduces simultaneously the observed spectra and surface brightness profiles of the MUSE Lyman-alpha halos.
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Shin, Suhyun;Im, Myungshin;Kim, Yongjung;Hyun, Minhee;Park, Woojin;Ji, Tae-geun;Jeon, Yiseul;Kim, Minjin;Kim, Dohyeong;Kim, Jae-Woo;Taak, Yoon Chan;Yoon, Yongmin;Choi, Changsu;Hong, Jueun;Jun, Hyunsung David;Karouzos, Marios;Kim, Duho;Kim, Ji Hoon;Lee, Seong-Kook;Pak, Soojong;Park, Won-Kee 59.4
To investigate the impact of the high-redshift quasars on cosmic reionization, the faint end slope of the quasars luminosity function has to be determined precisely. More quasars with low luminosity are needed to constrain the contribution to reionization in the early universe. However, finding these quasars has been regarded as tough process owing to the improper shallow depth of imaging data. In recent days, the release data of Subaru Hyper Suprime-Cam (HSC) Strategic Program survey which provide the deep images reaching ~ 25 mag facilitates searching the faint quasars candidates. To find faint quasar candidates in ELAIS-N1 field, along with the HSC data, two near-infrared (NIR) data sets also be used : The Infrared Medium-deep Survey (IMS) and The UKIRT Infrared Deep Sky Survey (UKIDSS) - Deep Extragalactic Survey (DXS). Quasar candidates selected from the multi-band color cut were observed by the SED camera for QUasars in EArly uNiverse (SQUEAN) instrument. To trace the redshifted Lyman break efficiently, appropriate medium bands comparable to targeted redshift range are chosen. The most reliable quasar candidates are finally determined through SED fitting. Using this less luminous quasars candidates, we can speculate the relation between the quasar growth and the host galaxy unbiasedly and estimate the contribution to the cosmic reionization. -
We investigate the
$SFR-M_{\star}$ relation of the infrared luminous galaxies selected in either$11{\mu}m$ and$15{\mu}m$ from the$5.6deg^2$ of the AKARI NEP-Wide field. From the constructed multi-wavelength catalog spanning$0.3{\mu}m$ to$24{\mu}m$ , we select 3,408 S11 >$50{\mu }Jy$ galaxies and 1,896 L15 >$20{\mu}Jy$ galaxies which corresponds to$L_{IR}{\sim}10^{11}L_{\odot}$ at z ~ 0.5 and 0.7 respectively. Photometric redshifts of the selected galaxies were derived using LePHARE and Coleman Extended templates. ~98% S11 selected galaxies are galaxies with(median redshift) ~ 0.4, and ~96% L15 selected galaxies are galaxies with ~ 0.6. Star formation rates and stellar mass of these galaxies were calculated using MAGPHYS which derives physical parameters with SED fitting. In the SFR- $M_{\star}$ diagram,$11{\mu}m/15{\mu}m$ selected galaxies are located in the main sequence of star-forming galaxies at z ~ 1. -
We present the near infrared JHK photometric properties and the spatial distribution of red supergiants(RSGs) of NGC 3623, NGC 3627 and NGC 3628 in the Leo Triplet system using the data obtained with 3.8m UKIRT(United Kingdom Infra-Red Telescope) at Hawaii. We checked interaction between the three galaxies by making a spatial density map of RSGs. From (J-K,K)0 Color-Magnitude Diagram which include resolved stars in three galaxy and control field with PARSEC isochrone, we figured out the RSG candidates of the Leo triplet are at 0.9<(J-K)0<1.2, mK<17.5 and separated them from background and foreground sources. Using gaussian kernel density estimation, we drew spatial density map of RSGs in the Leo triplet with an assumption that all RSGs are an identical population. The density map shows extended features of NGC 3628 to NGC 3627 along the declination direction. The asymmetries between NGC 3627 and NGC 3628 might be evidence for that the distribution of actual star components(RSGs) follows the neutral hydrogen distribution and also for interaction between two galaxies. And the extended features along the right ascension direction might be a supporting evidence for the existence of a TDG(Tidal Dwarf Galaxy). In case of NGC 3623, we could not see any sign of interaction in density map.
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Abell 115 is a renowned cluster merger at z=0.197. It exhibits an asymmetric X-ray distribution with cometary tails and a megaparsec-sized radio relic stretching in the northeastern direction from the core of the northern cluster. Many observations have concluded that this cluster merger has a large impact parameter, but there has been no numerical analysis on the structure of Abell 115. In this study, we simulate Abell 115 with Gadget2 N-body/SPH code to reproduce the X-ray and weak lensing features of Abell 115. We find a new plausible merger scenario of Abell 115, wherein the northern cluster is currently in an outgoing phase. The predicted X-ray emission has a similar morphology to the observed tail of the northern cluster. However, in order to reproduce the observed line-of-sight velocity and projected distance while maintaining the two systems gravitationally bound, the system should possess a large projection angle, which makes the shock look considerably more diffused than the observed radio relic.
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Outflows are common among local AGNs. Woo et al. (2017) suggested that AGN feedback through outflows is delayed by a dynamical time scale before the suppression of SFR is observationally detected. However, these SFR have large uncertainties because they were estimated by Artificial Neural Network (ANN) method (Ellison et al. 2016). We measured the SFR of 21 far-IR matched sources (z < 0.1) with total IR luminosity from multi-wavelength SED fitting from UV to radio. 15 out of 21 sources were observed with JCMT SCUBA-2 450 and 850um and 4 and 2 sources were matched with archival data of JCMT SCUBA-2 and Herschel SPIRE, respectively. We compared the true SFR by SED fitting with ANN-based one. In addition, we confirmed that sub-mm data are important to determine the SFR with total IR luminosity from SED fitting. Finally, we discuss the significance of true SFR and further the AGN-SF link.
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ZwCL 1447.2+2619 is a merging galaxy cluster at z=0.37 with clear substructures in X-ray emission and galaxy distribution. In addition, the system possesses distinct radio relics. In order to constrain the merger scenario, it is necessary to measure both the distribution and mass of the cluster dark matter. We perform weak lensing analysis of ZwCL 1447.2+2619 using Subaru imaging data. We detect clear lensing signal from the cluster after carefully addressing instrumental systematics. In this poster, we present our preliminary results on our mass reconstruction and discuss the comparison with X-ray and radio results.
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To understand the assembly of the galaxy population in clusters today, it is important to first understand the impact of previous environments prior to cluster infall, namely preprocessing. We use 15 cluster samples from hydrodynamic zoom-in simulation YZiCS to determine the significance of preprocessing focusing primarily on the tidal mass loss of dark matter halos. We find ~48% of the cluster member halos were once satellites of another host. The preprocessed fraction is not a clear function of cluster mass. Instead, we find it is related to each individual cluster's recent mass growth history. We find that the total mass loss is a clear function of time spent in a host. However, two factors can considerably increase the mass loss rate. First, if the satellite mass is approaching the mass of its host. Second, when the halo suffers tidal mass loss at a higher redshift. The preprocessing provides an opportunity for halos to experience tidal mass loss for a more extended period of time than would be possible if they simply fell directly into the cluster, and at earlier epochs when hosts were more destructive to their satellites.
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We use smoothed particle hydrodynamics (SPH) models to study the evolution of galactic spin and the distribution of gas and young stars in the inner region of the galaxies through galaxy encounters. Specifically, we perform numerical simulations of interactions of a late- or an early-type galaxy with either a late- or an early-type galaxy with and without a gas halo at the closest approach distances of 25 and 50 kpc. We find that an early-type galaxy encountering a late-type galaxy have a higher galactic spin and more gas and young stars in the central region of the galaxy after the collision. We are analyzing the role of a gas halo on the changes of galactic spin and central mass distribution during various galaxy-galaxy encounters.
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Galaxies in the cluster environment interact with the intracluster medium (ICM), losing the interstellar medium (ISM) and alternating their evolution. Observational evidences of the extraplanar ISM stripped by the ICM's ram pressure are prevalent in HI imaging studies of cluster galaxies. However, current theoretical understanding of the ram pressure stripping (or ICM-ISM interaction in general) is still limited mainly due to the lack of numerical resolution at ISM scales in large-scale simulations. Especially, self-consistent modeling of the turbulent, multiphase ISM is critical to understand star formation in galaxies interacting with the ICM. To achieve this goal, we utilize the TIGRESS simulation suite, simulating a local patch of galactic disks with high resolution to resolve key physical processes in the ISM, including cooling/heating, self-gravity, MHD, star formation, and supernova feedback. We then expose the ISM disk to ICM flows and investigate the evolution of star formation rate and the properties of the ISM. By exploring ICM parameter space, we discuss an implication of the simple ram pressure stripping condition (so called the Gunn-Gott condition) to the realistic ISM.
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From the gaussian, near scale-invariant density perturbations observed in the CMB to the late time clustering of galaxies, CDM provides a minimal theoretical explanation for a variety of cosmological data. However accepting this explanation, requires that we include within our cosmic ontology a vacuum energy that is ~122 orders of magnitude lower than QM predictions, or alternatively a new scalar field (dark energy) that has negative pressure. Alternatively, modifications to Einstein's General Relativity have been proposed as a model for cosmic acceleration. Recently there have been many works attempting to test for modified gravity using the large scale clustering of galaxies, ISW, cluster abundance, RSD, 21cm observations, and weak lensing. In this work, we compare various modified gravity models using cosmic shear data from the Deep Lens Survey as well as data from CMB, SNe Ia, and BAO. We use the Bayesian Evidence to quantify the comparison robustly, which naturally penalizes complex models with weak data support. In this poster we present our methodology and preliminary constraints on f(R) gravity.
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Trends of Type Ia supernova (SN Ia) luminosities with the properties of host galaxies are important to study the underlying physics for an SN progenitor system and explosion mechanism. In the YONSEI SN catalog, we have a sample of ~600 SN and host data in the wider redshift range, and two independent light-curve models, SALT2 and MLCS2k2. From this catalog, here we present that SNe Ia in low-mass, globally and locally star-forming environments are fainter than those in high-mass, globally and locally passive environments, after light-curve shape and color or extinction corrections. Our results are then compared to previous studies, and show consistent results.
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The modern large-scale surveys and state-of-the-art cosmological simulations produce various kinds of big data composed of millions and billions of galaxies. Inevitably, we need to adopt modern Big Data platforms to properly handle such large-scale data sets. In my talk, I will briefly introduce the de facto standard of modern Big Data platform, Apache Spark, and present some examples to demonstrate how Apache Spark can be utilized for solving data-driven astronomical problems.
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보현산 천문대 1.8m 망원경과 고분산 에셀 분광기 BOES(BOao Echelle Spectrograph)를 이용한 공생별 AG Draconis와 UV Aurigae의 분광학적 특성을 파악한다. 중성수소 Balmer 선과 주요 원소에 의한 방출선들의 특징과 변화를 살펴보며, 두 별의 활동성 및 등급에 따른 Balmer 선의 변화 양상에 대해 알아보고자 한다.
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A comparison study between two low temperature opacity tables has been conducted. The opacity is the one of the major input physics in stellar model construction. Opacity is generally provided in a tabular form and as a function of 3 parameters, ie, density, temperature and chemical composition. Among available opacity tables, it has been common practice to utilize OPAL opacity table (Iglesias & Rogers, 1996) augmented with Ferguson opacity table (Ferguson et al. 2005) for the low temperature domain. For low temperature domain, another table, AESOPUS (Marigo & Aringer, 2009), has been announced in 2007. Reportedly, this opacity covers even lower temperature region, and is compatible with that of Ferguson in the overlapping temperature domain. To test the compatibility, stellar models and isochrones for various ranges in mass, metallicity and chemical composition, have been constructed. It is confirmed that there is no significant difference in the stellar models and isochrones constructed with the two different low temperature opacities. Therefore, in the construction of stellar models and isochrones, Ferguson low temperature opacity can be replaced with the AESOPUS opacity. The wider range in the temperature and chemical mixtures, and the easier accessibility make AESOPUS favorable in practical purpose.
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High resolution spectroscopy of the yellow symbiotic star AG Draconis is performed with the Canada-France-Hawaii Telescope to analyse the line profiles of Raman scattered O VI broad emission features at
$6825{\AA}$ and$7082{\AA}$ with a view to investigating the wind accretion process from the mass losing giant to the white dwarf. These two spectral features are formed through inelastic scattering of O$VI{\lambda}{\lambda}32$ and 1038 with atomic hydrogen. We find that these features exhibit double-component profiles with red parts stronger than blue ones with the velocity separation of ~ 60 km s-1 in the O VI velocity space. Monte Carlo simulations for O VI line radiative transfer are performed by assuming that the O VI emission region constitutes a part of the accretion flow around the white dwarf and that Raman O VI features are formed in the neutral part of the slow stellar wind from the giant companion. The overall Raman O VI profiles are reasonably fit with an azimuthally asymmetric accretion flow and the mass loss rate ~ 4${\times}$ 10^{-7} M_sun yr^{-1}. We also find that additional bipolar neutral regions moving away with a speed ~ 70 km s^{-1} in the directions perpendicular to the orbital plane provide considerably improved fit to the red wing parts of Raman features. -
Im, Myungshin;Choi, Changsu;Lim, Gu;Kim, Sophia;Paek, Seunghak Gregory;Kim, Joonho;Hwang, Sungyong;Shin, Suhyung;Baek, Insu;Lee, Sangyun;O, Sung A;Yoon, Sung Chul;Sung, Hyun-Il;Jeon, Yeong-Beaom;Lee, Sang Gak;Kang, Wonseok;Kim, Tae-Woo;Kwon, Sun-gil;Pak, Soojong;Eghamberdiev, Shuhrat 64.1
SNe light curves have been used to understand the expansion history of the universe, and a lot of efforts have gone into understanding the overall shape of the radioactively powered light curve. However, we still have little direct observational evidence for the theorized SN progenitor systems. Recent studies suggest that the light curve of a supernova shortly after its explosion (< 1 day) contains valuable information about its progenitor system and can be used to set a limit on the progenitor size, R*. In order to catch the early light curve of SNe explosion and understand SNe progenitors, we are performing a ~8hr interval monitoring survey of nearby galaxies (d < 50 Mpc) with 1-m class telescopes around the world. Through this survey, we expect to catch the very early precursor emission as faint as R=21 mag (~0.1 Rsun for the progenitor). In this poster, we outline this project, and present a few scientific highlights, such as the early light curve of SN 2015F in NGC 2442. -
지금으로부터 100년 전, 하버드대학교 천문대에서 에드워드 찰스 피커링과 윌리어미나 플레밍, 애니 점프 캐넌 등의 여성 천문학자들이 분광관측 자료를 가지고 헨리 드레이퍼 목록(HD catalog)을 만들기 시작했다. 이는 항성분류의 근간을 마련하고 현대 천문학의 본격적인 시작을 알리는 일이었다. 현재 국립청소년우주센터는 이를 기념하여, 디지털 이미지로 보유중인 1975년에서 1999년에 걸쳐 발간된 "Michigan catalog of HD stars"의 사진건판을 활용한 연구를 진행 중이다. 본 센터를 방문하는 청소년이 100년 전 그들과 한 것과 같은 고전적 항성 분류과정을 체험하며, 별의 스펙트럼을 이해하고 우주를 이해하는데 필수적인 분광학에 대한 이해를 높이길 기대한다. 이를 위한 선행 작업인 대물프리즘 사진건판 이미지에서 별의 스펙트럼을 추출하는 과정을 소개하고자 한다.
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Yu, Jinhee;Kim, Seunghyun;Byun, Yongik;NamKung, San;Lee, Eunseok;Park, Donggan;Jo, Hyunsik;Lee, Hyunyoung;Hyun, Yojun;Kim, Jungmin;Yu, Jeehye;Lee, Honggyu 64.3
어린이천문대는 2003년부터 15년간 어린이들의 천문지식 함양과 과학탐구 능력의 향상을 도모하기 위해 수준별 3단계 프로그램을 연구 개발해왔다. 우리의 3단계 천문교육 시스템은 저학년을 대상으로 한 체험교실, 고학년을 대상으로 한 탐구교실, 그리고 탐구교실을 수료한 학생들을 위한 심화 단계인 테마교실로 이루어져 있다. 단계별 교재, 교보재, 관측실험 및 시각자료의 개발을 통해 프로그램의 완성도를 높여왔다. 우리의 천문교육 프로그램으로 교육된 누적 인원은 모두 67986명(2018년 3월 31일 기준)에 달한다. 그중 천문학 진출 사례로는 페리지로켓의 신동윤 대표와 다수의 천문학 전공 학생들이 있다. 전문적인 초등학생 천문교육 프로그램의 지속적인 연구개발을 통해 대한민국 천문학 대중화에 이바지할 수 있을 것으로 기대된다. -
Hong, Sukbum A.;Rhee, SeungJun;Yun, Jeongjun;Kim, Minseok;Lee, Seung Ho;Kim, Jaihyun;Son, Gukmyeong 64.4
We present a study of citizen science performed at Korean Minjok Leadership Academy (KMLA). The importance of citizen involvements in scientific studies has been increasing, with remarkable results and performances. For instance, the discovery of an impact scar near Jupiter's south polar region (A. Wesley, 2009) led to an international campaign of professional observations to understand the asteroidal collision responsible for the scar. Citizen science at KMLA has been and will be mainly conducted by members of the astronomical observation club 'Apple-Pie' through amateur telescopes. Members of 'Apple-Pie' are specialized in various fields related to astronomy, from planetary science to cosmology. The spectrum not only includes fields that are directly related to astronomy but also fields such as computer science and astrophotography. The scheduled construction of a new observatory will further enable students to participate in higher level projects such as planetary monitoring over long timescales and the observation and detection of solar system bodies and exoplanets. In addition, a new supervisor with expertise and research experience in galactic astronomy, planetary science, and meteorology has joined the school faculty. He will supplement students with fundamental theoretical backgrounds and essential research techniques to enhance astronomical research at KMLA. KMLA's ultimate goal is to deploy a remote-controlled observatory available to aspiring scientists around the world to create a network of citizen science system. The prime observational conditions of KMLA and the willingness of the students and faculty members will provide a competitive edge for KMLA over other similar institutes in Korea. -
Choi, Doohyun;Kim, Jinhyub;Han, Doori;Chang, Seok-jun;Kang, Jisu;Kim, Donghyun;Kim, Sophia;Park, Mina;Park, So-Myoung 65.1
지난 2017년 4월, 젊은 천문학자 모임 (Young Astronomers Meeting, YAM) 정기총회에서 2017-18년도 임원진으로 회장 최두현 회원(세종대학교), 부회장 김진협 회원(연세대학교), 총무 한두리 회원(충남대학교)를 선출하였다. 임원진은 경북대학교 김동현 회원, 경희대학교 박소명 회원, 과학기술연합대학원 박민아 회원, 서울대학교 김소피아 회원을 학교별 운영위원으로 임명하였다. 현 임원진은 본 모임의 온라인 소식지인 <하늘 사랑>을 2017년 가을에 7호, 2018년 봄에 8호를 발간하였다. 이와 더불어 2017년 일본 이시가키에서 개최된 EAYAM에 권유나 회원 외 6명의 회원이 참여하여 동아시아 젊은 천문학자들과 함께 학술 발표 및 교류를 하였다. 2018년 2월에는 We Love Galaxies - Young Astronomers Meet Universe 워크샵을 개최하고 YAM의 지속적인 학술 모임을 위한 기반을 다졌다. 이번 포스터에서는 2017-18년도 동안의 활동 내용을 보고하고 이후의 계획에 대해 논의하려고 한다. -
Through MIRIS
$Pa{\alpha}$ Galactic plane survey, a lot of$Pa{\alpha}$ blobs were detected along the plane. To reveal their characteristics, we are planning to collect NIR high-resolution spectroscopic data for them by using Immersion GRating INfrared Spectrograph (IGRINS). Here, we present the preliminary results of the IGRINS observations for a Herbig Be star, MWC 1080, which is one of the$Pa{\alpha}$ blobs detected in Cepheus. This Herbig Be star is known to possess a lot of young stellar objects (YSOs) and bright MIR ($10-20{\mu}m$ ) nebulosity in its vicinity. From IPHAS$H{\alpha}$ data, we revealed large extended$H{\alpha}$ features that correlate well with MIR and 13CO morphologies around MWC 1080. A part of the$H{\alpha}$ features shows a bow shock shape to the northeast of the primary star MWC 1080A, which seems to be due to an outflow from MWC 1080A. Through IGRINS observations, we detected faint [Fe II]${\lambda}1.644{\mu}m$ and H2 1-0 S(1)${\lambda}2.122{\mu}m$ emission lines around the bow shock feature. Interestingly, to the east region of MWC 1080A, we also detected strong [Fe II] and H2 emission lines with a couple of velocity components, which suggests the detection of a new outflow from another YSO. Broad$Br{\gamma}$ ${\lambda}2.1662{\mu}m$ line and H2 lines with various velocity components were detected around the bright MIR and$H{\alpha}$ nebulosity as well. -
Park, Sunkyung;Lee, Jeong-Eun;Pyo, Tae-Soo;Sung, Hyun-Il;Lee, Sang-Gak;Kang, Wonseok;Yoon, Tae Seog;Park, Won-Kee 65.3
We present the results of high-resolution optical (R ~ 30,000) and near-infrared (R ~ 45,000) spectroscopic monitoring observations of a new FU Orionis-like young stellar object, 2MASS J06593158-0405277. FU Orionis objects (FUors) are well-studied examples of episodic accretion because of their outburst phenomenon. Recently, 2MASS J06593158-0405277 exhibited an outburst and was identified as a FUor. It provides an important opportunity to investigate the whole FUors phenomenon from its pre-outburst to its post-outburst phase. We monitored 2MASS J06593158-0405277 with the BOES and the IGRINS since Dec 25, 2014 (UT). We detected several wind and disk features and present here our analysis for time variations of those spectral lines. -
Yun, Hyeong-Sik;Lee, Jeong-Eun;Choi, Yunhee;Lee, Seokho;Baek, Giseon;Lee, Yong-Hee;Choi, Minho;Kang, Hyunwoo;Tatematsu, Ken'ichi;Gaches, Brandt A.L.;Heyer, Mark H.;Evans, Neal J. II;Offner, Stella S.R.;Yang, Yao-Lun 66.1
Turbulence is a phenomenon which largely determines the density and velocity fields in molecular clouds. Turbulence can produce density fluctuation which triggers a gravitational collapse, and it can also produce a non-thermal pressure against gravity. Therefore, turbulence controls the mode and tempo of star formation. However, despite many years of study, the properties of turbulence remain poorly understood. As part of the Taeduk Radio Astronomy Observatory (TRAO) Key Science Program (KSP), "apping Turbulent properties In star-forming MolEcular clouds down to the Sonic scale (TIMES; PI: Jeong-Eun Lee)", we have mapped two star-forming clouds, the Orion A and the${\rho}$ Ophiuchus molecular clouds, in 3 sets of lines (13CO 1-0/C18O 1-0, HCN 1-0/HCO+ 1-0, and CS 2-1/N2H+ 1-0) using the TRAO 14-m telescope. We aim to map entire clouds with a high-velocity resolution (~0.05 km/s) to compare turbulent properties between two different star-forming environments. We will present the preliminary results using a statistical method, Principal Component Analysis (PCA), that is a useful tool to represent turbulent power spectrum. -
Lee, Yong-Hee;Lee, Jeong-Eun;Yun, Hyeong-Sik;Kim, Jongsoo;Choi, Yunhee;Mairs, Steve;Johnstone, Doug 66.2
The probability distribution function of column density (N-PDF) has been used for studying the characteristics of molecular clouds. In particular, the properties of N-PDF can reveal the nature of turbulence and gravity inside the molecular cloud. We use the dust continuum emission at$450{\mu}m$ and$850{\mu}m$ observed as part of the JCMT Gould Belt Survey (GBS) (Mairs et al. 2016), the 12CO J=1-0 line observed with the 45 m telescope at Nobeyama Radio Observatory (NRO) (Shimajiri et al. 2011), 13CO, C18O and HCO+ J=1-0 observed with the 13.7 m telescope at Taeduk Radio Astronomy Observatory (TRAO), as part of the TRAO key science project, "mapping Turbulent properties In star-forming MolEcular clouds down to the Sonic scale" (TIMES; PI: Jeong-Eun Lee). We here present the N-PDFs derived from the continuum and the molecular line emission toward the Orion A molecular cloud and compare their behaviors in order to investigate the chemical and optical depth effects on the N-PDF. -
We present distinct chemical and kinematic properties associated with the inner and outer halos of the Milky Way, as identified by metal-poor stars from the Sloan Digital Sky Survey. In particular, using carbon-enhance metal-poor (CEMP) giants, we first map out the fractions of CEMP-no stars (without strongly enhanced neutron-capture elements) and CEMP-s stars (with a large enhancement of s-process elements) in the inner- and outer-halo populations, separated by their spatial distribution of carbonicity ([C/Fe]). The CEMP-no and CEMP-s objects are classified by their different levels of absolute carbon abundances, A(C). We investigate characteristics of rotational velocity and orbital eccentricity for these sub-classes within the halo populations. Distinct kinematic features and fractions between CEMP-no and CEMP-s stars identified in each halo region will provide important clues on the origin of the dichotomy of the Galactic halo.
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Hong, Jihye;An, Deokkeun;Simpson, Janet P.;Sellgren, Kris;Ramirez, Solange V.;Cotera, Angela S. 67.1
We present high-resolution near infrared (IR) spectra of two candidate planetary nebulae (PNe) that were serendipitously found toward the Galactic center (GC). Our spectra obtained using GNIRS on Gemini North reveal strong Br ♑ and He I recombination lines. In one of the targets, we confidently detect Pa ♌ emission. Based on Br ♑ and Pa ♌ lines, we estimate a foreground reddening to be Av=27 mag, which confidently puts this object at the GC distance. Along with the presence of highly excited emission lines such as [S IV], [Ne III], [Ne V], and [O IV] detected in the mid-IR spectra from the Spitzer Space Telescope, and the extended emission in the Pa ♋ narrow-band image from the Hubble Space Telescope, this makes it the first spectroscopically confirmed PN in the GC. -
Magnetic fields play an important role in star-forming processes by regulating gravitational collapse. In filamentary structures of star-forming regions, magnetic fields are likely to be aligned with minor axes of filamentary molecular clouds because matter freely moves along magnetic field lines. Orion A region, one of the well-known high-mass star forming regions, has long filament structure. In order to study magnetic field directions with respect to the filamentary structure in Orion A, we have analyzed
$850{\mu}m$ dust polarization observations obtained with the James Clerk Maxwell Telescope (JCMT). We found tight correlation of dust intensity gradients and magnetic field directions. It was estimated that 81% of magnetic field segments are aligned with density gradients within 40 degree. In conclusion, we confirmed most of magnetic field segments are perpendicular to the major axis of the filament in Orion A. -
We plan to automatize the operation of Kyung Hee Astronomical Observatory (KHAO) 76 cm Telescope by adapting KAOS30 (KHU Automatic Observing Software for McDonald 30 inch Telescope). The software is developed to improve the efficiency of the observation system for monitoring transients and variable sources. It has installed and operated at McDonald 30 inch telescope since 2017 August. KAOS76 (KHU Automatic Observing Software for KHAO 76 cm Telescope) consists of four packages: Telescope Control Package (TCP), Data Acquisition Package (DAP), Auto Focus Package (AFP), and Script Mode Package (SMP). Most of the packages can be configured by minimized modifications of the codes because it includes common libraries for FLI instruments and also ASCOM standard. TCP, DAP, and AFP control astronomical devices. SMP supports automatic observing in a script mode. TCP of KAOS76 can communicate with the TCS via ASCOM. Also, KAOS76 has an extra function to compensate the misalignment of the polar axis. In this poster, we show the current status of the observing system with KAOS76.
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Yeom, Jae-Hwan;Oh, Se-Jin;Roh, Duk-Gyoo;Jung, Dong-Kyu;Oh, Chung-Sik;Kim, Hyo-Ryoung;Shin, Jae-Sik;Hwang, Ju-Yeon;Song, Min-Gyu;Jung, Tae-Hyun 68.1
KaVA(KVN and VERA Array)는 KVN 3기, 일본 VERA 4기로 구성되어 있다. 더 나아가 일본의 JVN, 중국의 CVN으로 확장한다면 동아시아에 더 많은 기선들이 존재한다. 각 전파망원경은 천문학자의 연구수요, 디지털 백엔드(Back-end) 시스템 기술수준에 의해 각기 다른 다양한 자료구조를 이용한다. 이와 함께, 현재 전파천문관측은 디지털 백엔드 시스템의 발달로 2Gbps 관측이 주를 이루고 있으며 32Gbps 시험 관측이 이루어지고 있다. 이에 한일상관센터는 이런 다양한 자료구조와 관측 대역폭을 지원하기 위해 KaVA용 디지털필터를 개발하고 있다. 기존에 개발된 CPU기반의 디지털필터를 연산속도와 자료 입출력 대역폭을 상당히 높인 GPU 기반 디지털필터로 업그레이드하고 있다. 본 발표는 GPU를 활용한 KaVA용 디지털 필터 개발에 관하여 소개하고자 한다. -
Spectroscopic observations commonly use a slit or fiber; however, non-slit spectroscopy enables us to observe a larger number of targets in one frame of image. Hence, it has been adopted as an observational mode for observatories like HST and JWST. Slitless spectroscopy requires wavelength calibration solutions in order to distinguish and measure the absorption / emission lines from the spectra with high accuracy. We installed the Volume Phase Holographic (VPH) grating to SQUEAN camera on the McDonald 2.1m telescope and obtained images with spectral resolutions of ~ 100 and 200. In order to derive the wavelength calibration, we measured the distances between the 0th order images and spectral features of various quasars. The distances are converted to wavelengths using the known wavelengths of the emission lines. We tested several different methods of spectral extraction and peak estimation of emission lines. We will present the results for the wavelength calibration and suggest the reliable methods to find the solution.
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The MATS (Mesosphere Airglow / Aerosol Tomography Spectroscopy) satellite is a Swedish scientific microsatellite which Kyung Hee University participates in developing. The limb telescope of the MATS satellite is designed with linear astigmatism-free off axis optical configuration which allows wide field of view (
$5.67^{\circ}{\times}0.91^{\circ}$ ). Here we present the full-field optical performance test setup that consists of a point source, a collimator, the limb telescope and a CCD (Charged Coupled Device). The incidence angle of the collimator was carefully controlled by the rotary stage under the limb telescope. The imaging tests represent expected results without dominant aberrations. -
Lee, Hye-In;Cook, Erika;Ji, Tae-Geun;Byeon, Seoyeon;Pak, Suehee;Cynthia, Froning;Marshall, Jennifer;Depoy, Darren L.;Pak, Soojong 68.4
GMACS is one of the instruments for the Giant Magellan Telescope (GMT) which will provide wide field, multi-object, moderate resolution spectroscopy of faint targets. KHU (Kyung Hee University) is in charge of control software of GMACS. As a first step, the Slit Mask Exchange Mechanism Prototype (SMEM-P) will be used as a preliminary example to make development process between electronics and high level software. Recently, we have developed a sample program to communicate with low level devices via EtherCAT. It is expected to be a mockup design for software and control system of GMACS. In this poster, we show the development process and test operation results of control software for SMEM-P. -
Astronomy education and research can benefit from a high performance telescope that is easily accessible in campus. Such a facility allows hands-on education of observations, small research projects, test of new instruments, and time-domian study of astronomical phenomena. Recently, SNU reconstructed a 40-year old observatory (also known as 구천문대), and established the new SNU Astronomical Observatory (SAO) on that site. On 2018 March 27, the 1-m optical telescope was successfully installed at SAO. Since then, this telescope has been producing wonderful images. This poster will give an overview of the 1-m telescope, and its performance.
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On 2018 March 27, a 1-m telescope was installed at the SNU Astronomical Observatory (SAO) which is a newly constructed building at the site where the previous Kwanak Observatory (Old observatory; 구천문대) stood. A series of test observations have been performed on this telescope, and we report the first results from the test observations in this poster. In particular, we present seeing values, limiting magnitudes and sample images taken with a
$4k{\times}4k$ CCD camera ($21^{\prime}{\times}21^{\prime}$ ). -
한국우주전파관측망(KVN, Korean VLBI Network)의 86 GHz 대역 수신기는 VLBI에서 주로 관측하는 85-95 GHz 주파수 대역에서 동작하도록 설계, 제작되었다. UMASS(University of Massachusetts) 대학으로부터 도입된 수신기의 대역폭을 84-116 GHz로 확장하기 위해 2017년도부터 수신기 설계, 부품 구입 등을 진행하고 있다.기존 수신기의 대역폭을 확장하기 위해, 협대역 주파수 변환기의 설계를 변경해야 한다. 주파수 변환기는 일반적으로 사용되는 SSB(Single Side Band) Mixer를 사용하지 않았다. 그 대신에 20 dB 이상의 높은 이미지 제거율을 갖도록 HPF(High Pass Filter)와 LPF(Low Pass Filter)를 사용하여 RF 주파수를 84-100 GHz와 100-116 GHz로 나눈 후 주파수 변환토록 하였다. 사용된 Filter의 특성을 이용, 이미지 대역 신호를 수 십 dB 이상 제거할 수 있다. RF 단에서의 신호 분리로 인해 수신기 등가잡음 온도는 수 K 정도 증가한다. 2017년에 제안된 주파수 변환기를 상온에서 구성하여 그 가능성을 검증하였고, 2018년 9월 까지 KVN W-band 수신기 1 대의 업그레이드를 진행할 것이다. 2019년까지 KVN 3 사이트의 W-band 수신기 주파수 확장을 완료할 계획이다.
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Ji, Tae-Geun;Byeon, Seoyeon;Lee, Hye-In;Park, Woojin;Lee, Sang-Yun;Hwang, Sungyong;Choi, Changsu;Gibson, Coyne A.;Kuehne, John W.;Prochaska, Travis;Marshall, Jennifer;Im, Myungshin;Pak, Soojong 69.4
KAOS30 is an automatic observing software for the wide-field 10-inch telescope as a piggyback system on the 30-inch telescope at the McDonald Observatory in Texas, US. The software has four packages in terms of functionality and is divided into communication with Telescope Control System (TCS), controlling of CCD camera and filter wheel, controlling of focuser, and script for automation observing. Each interconnect of those are based on exe-exe communication. The advantage of this distinction is that each package can be independently maintained for further updates. KAOS30 has an integrated control library that combines function library connecting each device and package. This ensures that the software can extensible interface because all packages are access to the control devices independently. Also, the library includes the ASCOM driver platform. ASCOM is a standard general purpose library that supports Application Programming Interface (API) of astronomical devices. We present the software architecture of KAOS30, and structure of interfacing between hardware and package or package and package. -
Shin, Min-Su;Chang, Seo-Won;Byun, Yong-Ik;Yi, Hahn;Kim, Myung-Jin;Moon, Hong-Kyu;Choi, Young-Jun;Cha, Sang-Mok;Lee, Yongseok 70.1
The DEEP-South photometric census of small Solar System bodies is producing massive time-series data of variable, transient or moving objects as a by-product. To fully investigate unexplored variable phenomena, we present an application of multi-aperture photometry and FastBit indexing techniques to a portion of the DEEP-South year-one data. Our new pipeline is designed to do automated point source detection, robust high-precision photometry and calibration of non-crowded fields overlapped with area previously surveyed. We also adopt an efficient data indexing algorithm for faster access to the DEEP-South database. In this paper, we show some application examples of catalog-based variability searches to find new variable stars and to recover targeted asteroids. We discovered 21 new periodic variables including two eclipsing binary systems and one white dwarf/M dwarf pair candidate. We also successfully recovered astrometry and photometry of two near-earth asteroids, 2006 DZ169 and 1996 SK, along with the updated properties of their rotational signals (e.g., period and amplitude). -
KMTNet에서는 프로젝트의 소개와 운영현황 등 파악하기 위해 웹서비스를 운영하고 있다. 홈페이지(http://kmtnet.kasi.re.kr; 국문, 영문)에는 최신 뉴스와 공지사항, 실시간 모니터링 영상 및 기상정보, 관측일정, 관측자료 공개, 활용성과 등을 게시 하였고, 관측 결과와 운영 정보 관리를 위해서 모니터링 홈페이지(kmtnet-monitor)를 제작하였다. KMTNet은 남반구 3개 관측소에 상주하는 현지 관측자에 의해 관측이 이루어지기 때문에, 국내 연구자가 남반구 관측소 현황을 파악할 수 있는 모니터링 시스템이 필수적이다. 웹서비스에 실시간 기상과 관측자료 전송속도를 함께 표시하여 관측 진행 여부를 확인할 수 있으며, 관측일지를 데이터베이스화하여 망원경/카메라/관측돔의 이상 유무, 관측 현황, 기상/시상 통계 등으로 활용하고 있다. 여기서는 지금까지 개발한 웹 서비스를 소개하고 앞으로 관측소 운영에 유용한 정보와 웹 서비스의 발전 방향에 대해 논의하고자 한다.
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Cha, Sang-Mok;Lee, Chung-Uk;Lee, Yongseok;Kim, Dong-Jin;Lee, Dong-Joo;Kim, Seung-Lee;Jin, Ho 70.3
외계행성 탐색시스템의 망원경-카메라 제어 시스템 및 소프트웨어 구성과 관측 유틸리티에 대해 소개한다. 망원경 제어 소프트웨어는 천문 위치보정, 포인팅, 돔 회전 등을 담당하는 PC-TCS 프로그램, 망원경 적경-적위 축 서보 제어를 담당하는 full-closed loop PID 컨트롤 프로그램, 포커서, 필터박스, 돔 셔터, 주경냉각, 온도 모니터 등의 보조 시스템을 제어하는 AUX controls 프로그램으로 구성된다. 카메라 제어 소프트웨어는 모자이크로 구성된 여러 CCD를 각각 독립적으로 제어하는 IC(Instrument Control) 패키지와 이들을 총괄 제어하는 ICS(IC Science) 패키지로 구성되며 망원경과 카메라 소프트웨어의 인터페이스 역할을 하는 TCS Agent 프로그램이 포함된다. 관측 진행을 돕는 유틸리티로서 관측제어 명령어 입력 및 관측 스크립트 구동 기능을 제공하는 OBS Agent 프로그램과 가이드 CCD를 이용한 시상 모니터링 및 자동초점조정 프로그램을 개발하여 활용하고 있다. 각 소프트웨어는 UDP, TCP/IP, RS-232, Redis server 등 다양한 인터페이스를 통하여 서로 통신하며, CCD 영상 자료 전달을 위해 RAM(Random Access Memory) 디스크와 Network File System(NSF)을 이용하고 있다. -
천문학자들에게 분광관측은 천체를 연구하는데 가장 강력한 방법이다. 태양계 바깥쪽에 위치한 목성, 토성, 타이탄 연구도 분광관측은 행성천문학자들에게 매우 유용하여 대형 지상 망원경을 사용한 분광 관측과 더불어 행성탐사선들에 장착된 분광기를 사용하여 새롭고 유용한 과학적 정보를 얻어왔다. 본 발표에서는 20세기 말에 시작된 탐사선을 이용한 외행성계 탐사와 지상관측 결과를 리뷰하고 얼마 전 토성 탐사를 마친 카시니 탐사선, 현재 목성에서 활약하고 있는 주노 탐사선, 이들과 병행하여 수행되었고, 수행되고 있는 지상 분광관측 결과를 소개한다. 목성, 토성, 타이탄 탐사는 미국과 서구유럽에 의해 주도적으로 수행되어 왔는데, 지금까지의 탐사선들과 지상관측으로 축적된 자료들에 대한 정밀 분석과 비판적 검토를 수행하면 우리나라 우주개발 중장기 계획에 포함 되어 있는 행성탐사계획의 최적화된 방향 결정에도 도움이 될 것이다.
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태양계 질량의 대부분은 플라즈마, 기체, 또는 액체 상태로 존재하며, 극히 일부만이 고체 즉 암석과 광물로 존재한다. 하지만, 반응 특히 혼합(mixing)이 일어나는 속도가 매우 느린 고체의 특성상 태양계의 탄생과 진화 과정의 기록은 고체태양계 물질에 더 잘 보관되어 있다. 지구를 제외한 고체 태양계 물질을 확보하기 위해서는 지구로 낙하한 암석인 운석(meteorites)을 발견하거나, 우주로 나가 시료를 가져와야 한다. 아폴로 미션(Apollo mission)에 의한 월석(lunar rocks) 채취(Papike et al., 1998), 하야부사 미션(Hayabusa mission)에 의한 소행성(asteroid) 시료 채취(Nakamura et al., 2011), 스타더스트 미션(Stardust mission)에 의한 혜성 시료 채취(Zolensky et al., 2006) 등이 후자에 속한다. 능동적으로 가져온 시료는 아직까지는 그 종류와 양에서 운석에 비해 매우 부족하므로 현재까지 우리가 알고 있는 고체 태양계에 관한 대부분은 운석 연구를 통해 얻어졌다. 운석은 크게 미분화운석 즉 콘드라이트(chondrites)와 분화운석(differentiated meteorites)으로 구분한다. 분화운석 중 일부는 달운석(lunar meteorites) 또는 화성운석(martian meteorites)이며, 나머지 분화운석과 콘드라이트는 암석-지구화학적 특징과 성인적 연관성에 의해 다양한 그룹으로 세분되는데 각 그룹은 하나의, 또는 둘 이상의 매우 유사한, 소행성에서 유래한 것으로 해석된다(Krot et al., 2014; 최변각 2009). 다양한 종류의 운석과 구성 광물에 포함된 기록으로는 (1) 태양계 이전 존재한 항성의 대기에서 생성된 광물, 즉 선태양계 광물(presolar grains), (2) 태양계 성운 탄생과 각 진화 단계의 정확한 시기, (3) 태양계 성운의 화학조성-동위원소 조성, 온도-압력 조건 등을 포함한 물리-화학적 특징, (4) 가스-먼지로부터 미행성, 소행성, 행성으로의 진화 과정, (5) 행성 진화의 열원, (6) 소행성 핵의 생성 과정 등이 있다. 강연에서는 이들을 간략히 살펴보고자 한다. 운석연구 등을 통해 태양계 생성과 진화과정에 관한 다양한 정보가 축적되었지만, 앞으로 연구할 것들이 더 많다. 또한 태양계 물질 중에는 운석의 형태로 지구로 들어왔거나 앞으로 들어올 수 있는 것도 있지만 그렇지 않은 것도 있다. 가스나 기체의 경우가 그러할 것이며, 고체지만 결합이 약해 일부라도 원형을 유지한 채 대기권을 통과 할 수 없는 것도 있을 것이다. 또 공전궤도나 중력 등 물리적 이유로 지구권 진입이 불가능한 것도 있다. 이러한 태양계 구성원에는 우리가 아직까지 얻지 못한 정보들이 다량 보존되어 있을 것이다. 미래의 태양계탐사가 기대되는 이유 중 하나이다.
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Asteroids represent a significant resource for space exploration and scientific research. Various scientific missions have already performed and planned to investigate and understand the characteristics of asteroids. This talk introduces many space missions to asteroids. Representing missions to asteroids are the NASA's NEAR, Deep Space-1, Dawn, OSIRIS-Rex, SCOUT, DART, and ESA's Rosetta, and JAXA's Hayabusa 1 and 2, and DESTINY+ missions, and others. Although it is a very rare event, the possibility of Earth-crossing asteroids (ECAs) colliding with the Earth can never also be ignored. Numerous mitigation concepts also have been proposed to deflect ECAs in preparing for the disasters which might occur in future days. In the early studies for mitigation schemes, most of analyses were centered on to deflect ECAs with impacting the energy to the object to change its orbit. This talk also introduces many methods to deflect the orbit of ECAs, and shows spacecraft trajectories to asteroids.
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Recently, an analysis of 3-micron spectra of CH4 line emission from our Gemini/GNIRS observations of Jupiter's polar regions yielded an unexpected result: The homopause (~1 microbar pressure level) located directly above the long-lasting 8-micron CH4 north-polar hot spot (Great 8-micron Hot Spot: GHS) is cool compared with the temperatures of nearby auroral regions (Kim et al. 2017). Most of the 8-micron emission of the GHS originates from CH4 at the ~1 mbar level (i.e., deeper in the stratosphere, where cooling time is several years), much longer than at the altitude of the homopause. We propose a mechanism to explain the temperature difference: locally-fixed and transient, but energetic auroral particles, which can penetrate to the 1 mbar level and deposit energy there creating and maintaining the GHS. For Saturn, thus far we have not detected distinctive 8-micron nor 3-micron CH4 hot spots in the polar regions. We will present a possible implication for this difference between Jupiter and Saturn.
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The Opposition Effect (OE) is an enhancement of the brightness of a reflecting light as the phase angle (the Sun-target-observer angle) approaches zero. The mechanisms have been studied both theoretically and experimentally and nowadays recognized that there are two major mechanisms, namely, coherent backscattering OE (CBOE) and shadow hiding OE (SHOE). From data analyses of an S-type asteroid Itokawa taken with the Hayabusa spacecraft onboard camera, it is suggested that the CBOE would be dominant at phase angle smaller than ~ 1.4 deg, while SHOE dominates at larger phase angles (M. Lee & M. Ishiguro, under review). The study on the physical parameters which affect the OE, such as size and composition, will lead us to find a way to disentangle each of them from observation. The experiments in lab, however, faces two major difficulties: (a) the detector blocks the incident light if phase angle is nearly zero and (b) incident and emission angles must be controlled with high angular resolution to prevent blurring of OEs at different phase angles in one measurement. In this presentation, we introduce a new apparatus which has been installed at Seoul National University to investigate the OE in our lab, and summarize the initial results. It will be a valuable starting point to establish infrastructure in Korea, and will shed light on the investigation of OE physics using laboratory simulants.
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Since there are two-different observational constraints for the lunar exosphere data, it is interesting to find the best exospheric model that can account for the observed characteristics of the lunar coma and tail simultaneously (Lee & Kim, 2017).The characteristics of the lunar exosphere can be constrained by comparing simulated models with observational data of the coma and tail. In this work, considering effects of triple sodium sources (two dayside sources: a low- and a high-velocity component; and an Isotropic source component), we present time-dependent simulations showing initial conditions around the lunar coma and the final stage of the lunar tail. Based on an updated 3-D lunar exosphere model (Lee & Kim, 2017), we are presenting the simulated images of the lunar sodium coma and its correlation with lunar tail's physical parameters.
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북극 스발바르의 사면 지형에는 걸리가 발달되어 있다. 이러한 걸리는, 그 성인에는 여러 의견이 있으나, 화성에도 중고위도를 중심으로 다수 분포한다. 화성의 걸리는 2000년대에 들어 비로소 본격적으로 규명되고 있으나, 지형적 특성으로 인한 탐사의 한계로 지구에 분포하는 유사지형을 통한 비교 연구가 일반적이다(Costard, et al. 2007 등). 이 연구에서는 스발바르의 주도 롱이어비엔에서 UAV을 이용하여 획득한 DEM으로 스발바르 걸리를 측량하고, 이를 화성 중위도의 테라 사이메리아, 테라 시레넘, 노아 키스 테라에 분포하는 걸리와 비교하였다. Longyearbreen 빙하 전방에 위치한 사면을 UAV로 촬영하고, 이를 SfM-MVS(Structure from Motion & MultiView Stereo) 기법으로 3차원 점군 모델과 고해상도 DEM을 제작하여 분석하였다. 화성의 경우 MRO궤도 탐사선이 촬영한 HiRise DTM을 이용하여 분석하였다. 두 걸리는 기후와 지질 조건에 차이가 있음에도 불구하고 유사한 패턴을 보였다. 특히 테라 사이메리아에 위치한 걸리와 롱이어비엔 북사면의 걸리는 기준거리, 단면적, 폭, 경사, 제방 두께 등에서 상당한 정량적 유사관계가 있었다. 이는 두 행성의 걸리가 유사한 성인 및 형성 프로세스를 거쳤을 가능성을 시사한다. 측량 기법과 UAV 의 안정성을 개선시키면 지형 모델의 품질 향상 및 극지에서의 UAV 운용이 용이해질 것으로 기대된다. 또한 스발바르의 기후 요소 및 물리량 적용은 향후 화성 지형연구에도 응용할 수 있을 것으로 사료된다.
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We investigated shock history of three achondrite meteorites: NWA 3117, a howardite from asteroid Vesta, NWA 2727, a breccia from the Moon, and NWA 856, a shergottite from Mars. Shock histories were evaluated from deformation of plagioclase feldspars. Feldspar grains were classified based on observations in cross-polarized light as undulatory, mosaic, mosaic-recrystallized or maskelynite. This sequence represents increasing deformation of original feldspar crystals. Undulatory crystals have wavy extinction, mosaic crystals have patchy extinction, and mosaic-recrystallized grains appear as if they were originally coarse-grained and have recrystallized to mosaics of small equant crystals. Maskelynite grains are isotropic, indicating transformation to glass. Based on feldspar deformation, the degrees of impact processing are NWA 856 > NWA 3117 > NWA 2727. The high deformation of NWA 856 is expected because this sample is from Mars, which is a large parent body and requires a powerful impact to accelerate a rock to escape velocity. In contrast, the parent body of NWA 3117 (Vesta) is smaller than that of NWA 2727 (the Moon), yet NWA 3117 appears more highly deformed than NWA 2727. One possible explanation is that NWA 2727 is from a relatively young part of the Moon, which has not been exposed to impacts as long as the surface of Vesta.
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The Hayabusa remote-sensing images of near-Earth asteroid (25143) Itokawa exhibited large diversity in spectral properties. The evidence suggests a various degrees of space weathering on the surface. It is known that the space weathering changes the spectra of S-type asteroids redder and reduces the depths of absorption around
$1{\mu}m$ . It is therefore possible to determine the surface ages through the investigation of the degree of space weathering. It is, however, reported that the scattered light components severely degrade the Asteroid Multiband Imaging Camera (AMICA) images, especially at the wavelengths >$0.86{\mu}m$ . Our team came up with a technique for subtracting the scattered light components (Ishiguro 2014). Here, we upgraded the techniqu e by applying simplex algorism to correct the artifacts for all AMICA bands. This new technique enables to apply for the longest channel (i.e., zs-band at$1.01{\mu}m$ ) images, which was not studied so far. With the AMICA all bands data, we estimated the surface ages at the different location to be 0.6-2 Myr. Based on this data together with the geological information (e.g. gravitational potentials and local). we will discuss about the evolution of surface materials on the asteroid.