• The Bulletin of The Korean Astronomical Society
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• v.36 no.1
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• pp.83.1-83.1
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• 2011

We report multi-epoch, simultaneous 22 GHz water and 44 GHz Class I methanol maser line survey towards 180 intermediate-mass young stellar objects, including 14 Class 0, 19 Class I objects, and 147 Herbig Ae/Be stars. We detected $H_2O$ and $CH_3OH$ maser emission towards 16 (9%) and 10 (6%) sources with one new $H_2O$ and six new $CH_3OH$ maser sources. The detection rates of both masers rapidly decrease as the central (proto)stars evolve, which is contrary to the trends in high-mass star-forming regions. This suggests that the excitations of the two masers are closely related to the evolutionary stage of the central (proto)stars and the circumstellar environments. $H_2O$ maser velocities deviate on average 9 km s-1 from the ambient gas velocities whereas $CH_3OH$ maser velocities well match with. For both maser emissions, large velocity difference (${\mid}v_{H2O}-v_{sys}{\mid}\;>\; 10kms^{-1}\; and\;{\mid}v_{CH3OH}-v_{sys}{\mid}\;>\;1kms^{-1}$) is mostly confined to Class 0 objects. The formation and disappearance of $H_2O$ maser lines are frequent and the integrated intensities of them change up to two orders of magnitude. In contrast, $CH_3OH$ maser lines usually show no significant change in the intensity, shape, and velocity. This consistent with the previous suggestion that $H_2O$ maser emission originates from the base of an outflow while 44 GHz Class I $CH_3OH$ maser emission arises from the interaction region of the outflow with the ambient gas. The isotropic maser luminosities are well correlated with the bolometric luminosities of the central the objects. The fitted relations are $L_{H2O}=1.71{\ast}10^{-9}(L_{bol})^{0.97}$ and $L_{CH3OH}=1.71{\ast}10^{-10}(L_{bol})^{1.22}$.

• Journal of The Korean Astronomical Society
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• v.47 no.5
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• pp.167-178
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• 2014

We search for misclassified type 1 AGNs among type 2 AGNs identified with emission line flux ratios, and investigate the properties of the sample. Using 4 113 local type 2 AGNs at 0.02 < z < 0.05 selected from Sloan Digital Sky Survey Data Release 7, we detected a broad component of the $H{\alpha}$ line with a Full-Width at Half-Maximum (FWHM) ranging from 1 700 to $19090km\;s^{-1}$ for 142 objects, based on the spectral decomposition and visual inspection. The fraction of the misclassified type 1 AGNs among type 2 AGN sample is ~3.5%, implying that a large number of missing type 1 AGN population may exist. The misclassified type 1 AGNs have relatively low luminosity with a mean broad $H{\alpha}$ luminosity, log $L_{H\alpha}=40.50{\pm}0.35\;erg\;s^{-1}$, while black hole mass of the sample is comparable to that of the local black hole population, with a mean black hole mass, log $M_{BH}=6.94{\pm}0.51\;M_{\odot}$. The mean Eddington ratio of the sample is log $L_{bol}/L_{Edd}=-2.00{\pm}0.40$, indicating that black hole activity is relatively weak, hence, AGN continuum is too weak to change the host galaxy color. We find that the O III lines show significant velocity offsets, presumably due to outflows in the narrow-line region, while the velocity offset of the narrow component of the $H{\alpha}$ line is not prominent, consistent with the ionized gas kinematics of general type 1 AGN population.

• Journal of Life Science
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• v.15 no.4 s.71
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• pp.664-667
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• 2005

Hydrosyringomyelia is a dilation of the spinal cord central canal. In human it may be caused by congenital malformations such as Dandy-Walker syndrome and Chiari malformations or may be acquired as a result of infection, trauma or neoplasia. Hydrocephalus is an excessive accumulation of cerebrospinal fluid within the ventricles and occipital dysplasia is the dorsal extension of the foramen magnum. Hydrosyringomyelia and hydrocephalus can be confirmed by computed tomography or magnetic resonance imaging (MRI). A 3-year-old male maltese was presented with a history of long-term seizure. Blood examination was all unremarkable. On rostrodorsal-caudoventral oblique radiograph of the skull showed severe occipital dysplasia. On brain sonography through the persistent fontanelle, severe lateral ventriculomegaly was revealed. MRI examination revealed hydrocephalus and hydrosyringomyelia. Diuretic therapy didn't reduce clinical symptoms and surgical decompression was conducted. The dog responded well with ventriculo-peritoneal shunting. MRI is the most superior modality to diagnose hydrocephalus and hydrosyringomyelia, to plan therapy and to determine the prognosis.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.2
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• pp.95-95
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• 2012

Constellations are formed of bright stars which appear close to each other on the sky, but are really far apart in space. The shapes you see all depend on your point of view. Back before people had televisions and electricity to light their homes at night, they spent a lot more time looking at the stars. People all over the world used their imaginations to draw pictures in the sky, as if it were a giant connect-the-dot game. The patterns they imagined are called constellations. People usually saw patterns that reflected their different cultures. Native Americans in North America imagined many animals and shapes from the natural world. The ancient Greeks found images of gods and goddesses in the stars. Sometimes people from very different parts of the world even imagined the same animal or shape in the same stars. Most of the constellations we recognize today were made up by the ancient Greeks around 6,000 years ago. Different constellations are visible at different times of year, so the first appearance of these patterns told farmers of the changing seasons and reminded them to plant or harvest their crops. The constellations also help us to find our way around the night sky and to remember which stars are which. The star names we use today are mostly from Greek and Arabic, but many are changed a bit from the original, as often happens when words are passed from one language to another. It can be difficult to picture just what those folks long ago were seeing in the stars, so don't be discouraged if you have trouble seeing their patterns. You can even make up your own! In ancient world all the countries or regions had their own way to name things up in the sky, make up stories and draw different shapes for constellations. Today there are 88 official constellations, but you may find that different books show their stars connected in slightly different ways. The official constellations are specific regions of the sky, so the exact patterns are not all that important. However in various cultures there are some famous star patterns that use stars from only apart of a constellation, or even connect stars from different constellations. These patterns of stars that are not official constellations are called asterisms. The Big Dipper is a very famous asterism, found in the constellation Ursa Major, or Great Bear.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.2
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• pp.81-81
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• 2012

Since the ultraviolet (UV) flux of an integrated population is a good tracer of recent star formation activities, UV observations provide an important constraint on star formation history (SFH) in galaxies. We present UV color-magnitude relations (CMRs) of early-type dwarf galaxies in the Virgo cluster, based on Galaxy Evolution Explorer (GALEX) UV data and the Extended Virgo Cluster Catalog (EVCC, Kim, S. in prep.). The EVCC covers an area 5.4 times larger (750 deg2) than the footprint of the classical Virgo cluster catalog by Binggeli and collaborators. We secure 1304 galaxies as members of the Virgo cluster and 526 galaxies of them are new objects not contained in the VCC. Morphological classification of galaxies in the EVCC is based on the optical image ("Primary Classification") and spectral feature ("Secondary Classification") of the SDSS data. We find that dwarf lenticular galaxies (dS0s) show a surprisingly distinct and tight locus separated from that of ordinary dwarf elliptical galaxies (dEs), which is not clearly seen in previous CMRs. The dS0s in UV CMRs follow a steeper sequence than dEs and show bluer UV-optical color at a given magnitude. Most early type dwarf galaxies with blue UV colors (FUV-r < 6 and NUV-r < 4) are identified as those showing spectroscopic hints of recent or ongoing star formation activities. We explore the observed CMRs with population models of a luminosity-dependent delayed exponential star formation history. The observed CMR of dS0s is well matched with models with relatively long delayed star formation. Our results suggest that dS0s are most likely transitional objects at the stage of subsequent transformation of late-type progenitors to ordinary red dEs in the cluster environment. In any case, UV photometry provides a powerful tool to disentangle the diverse subpopulations of early-type dwarf galaxies and uncover their evolutionary histories.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.1
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• pp.42.1-42.1
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• 2011

The main payload of the Science and Technology Satellite 3 (STSAT-3), Multipurpose Infrared Imaging System (MIRIS), will be equipped with the wide-field near-infrared camera. Its wide field-of-view ($3.67^{\circ}{\times}3.67^{\circ}$) is optimal for the observation of the zodiacal light (ZL), the sunlight scattered by the interplanetary dust (IPD). The MIRIS will continuously monitor the seasonal variation of the ZL towards both north and south ecliptic poles, which is caused by the asymmetries of the IPD distribution with respect to the Sun and the ecliptic plane. In addition to the monitoring observations, we are planning pointed observations for compelling structures in the ZL, the asteroidal dust bands and the gegenschein. This presentation proposes the zodiacal light observations with the MIRIS and discusses the expected results.

• Journal of the Institute of Convergence Signal Processing
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• v.18 no.2
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• pp.55-61
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• 2017

In radio astronomy, high-capacity HDDs are being used to save huge amounts of HDDs in order to record the observational data. For VLBI observations, observational speeds increase and huge amounts of observational data must be stored as they expand to broadband. As the HDD is frequently used, the number of failures occurred, and then it takes a lot of time to recover it. In addition, if a failed HDD is continuously used, observational data loss occurs. And it costs a lot of money to buy a new HDD. In this study, we developed the integrity verification system of the Serial ATA HDD using FirmOS. The FirmOS is an OS that has been developed to function exclusively for specific purposes on a system having a general server board and CPU. The developed system performs the process of writing and reading specific patterns of data in a physical area of the SATA HDD based on a FirmOS. In addition, we introduced a method to investigate the integrity of HDD integrity by comparing it with the stored pattern data from the HDD controller. Using the developed system, it was easy to determine whether the disk pack used in VLBI observations has error or not, and it is very useful to improve the observation efficiency. This paper introduces the detail for the design, configuration, testing, etc. of the SATA HDD integrity verification system developed.

• Proceedings of the Korea Technology Innovation Society Conference
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• 1999.11c
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• pp.219-236
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• 1999

This study is to acquire a thorough understanding of the S&T level of Korea to serve as an important basis for the government policy-making, and to make basic information available to effectively promote the National R&D Program by survey of the overall S&T level in Korea S&T level survey is a comparison to the highest levels in the world to the third 3digit of the technology tree table. And, survey of technological gaps by year, during which Korea is able to reach the current level of the advanced countries. The findings of the surveys should be applied to strategic technology Planning for solving or narrowing the technology gap, e the major criteria for resources allocation in National R&D programs. And, the findings of the surveys should be the fundamental information used to establish strategic S&T policy in government.

• Journal of the Korea Academia-Industrial cooperation Society
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• v.21 no.1
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• pp.97-102
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• 2020

With the advancement of technology, there are almost no constraints on expression in virtual reality (VR) art; however, it still has some limitations. VR artists can be largely classified into two groups in terms of style. The first group is artists who create their works as a live performance. In this case, a major limitation is that the artist cannot see how the audience reacts to the work because he/she wears a VR device while performing, and the audience cannot fully experience the work, since they view it only on-screen without any VR devices. This problem can be solved if all members of the audience wear VR devices; however, that requires astronomical costs and brings about another problem related to device management. If the price of VR devices decreases as technology develops, it may help solve this problem. The second group is exhibition artists who regularly display their works online. In this case, the limitation is that their work using VR remains only in the virtual digital space. In this case, a solution may be creating space in exhibition halls, and providing VR devices to audience members in existing art exhibitions.

• Journal of radiological science and technology
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• v.39 no.1
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• pp.43-49
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• 2016

In this study, equivalent dose and LET (Linear Energy Transfer) calibration of CR-39 SSNTD (Solid State Nuclear Track Detector) were performed using 400 MeV/u C heavy ions in HIMAC (Heavy Ion Medical Accelerator in Chiba) for high LET radiation therapy. The irradiated CR-39 SSNDTs were etched according the etching condition of JAXA (Japan Aerospace Exploration Agency). And the etched SSNTDs were analyzed by using Image J. Determined frequency mean dose (${\bar{y_D}}$)and dose-mean lineal energy (${\bar{y_F}}$)of 400 MeV/u C are about 8.5keV/mm and 10.1 keV/mm, respectively by using the CR-39 SSNTD. This value is very similar to the results calculated by GEANT4 Monte Carlo simulation and measured with TEPC (Tissue Equivalent Proportional Counter) active radiation detector. We could determine the equivalent dose and LET calibration factors of CR-39. And we confirmed that the CR-39 SSNTD was useful for high LET radiation dosimetry in hadron radiotherapy.