• 천문학회지
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• 제40권4호
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• pp.157-160
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• 2007

I present a model to explain the mass segregation and shallow mass functions observed in the central parts of starburst stellar clusters. The model assumes that the initial pre-stellar cores mass function resulting from the turbulent fragmentation of the proto-cluster cloud is significantly altered by the cores coalescence before they collapse to form stars. With appropriate, yet realistic parameters, this model based on the competition between cores coalescence and collapse reproduces the mass spectra of the well studied Arches cluster. Namely, the slopes at the intermediate and high mass ends, as well as the peculiar bump observed at $6M_{\bigodot}$. This coalescence-collapse process occurs on a short timescale of the order of the free fall time of the proto-cluster cloud (i.e., a few $10^4$ years), suggesting that mass segregation in Arches and similar clusters is primordial. The best fitting model implies the total mass of the Arches cluster is $1.45{\times}10^5M_{\bigodot}$, which is slightly higher than the often quoted, but completeness affected, observational value of a few $10^4M_{\bigodot}$. The model implies a star formation efficiency of ${\sim}30$ percent which implies that the Arches cluster is likely to a gravitationally bound system.

• 천문학회지
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• 제41권3호
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• pp.49-58
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• 2008

Resonance doublets including O VI 1032, 1038, NV 1239, 1243 and C IV 1548, 1551 constitute prominent emission lines in symbiotic stars and planetary nebulae. Spectroscopic studies of symbiotic stars and planetary nebulae from UV space telescopes show various line ratios of these doublets deviating from the theoretical ratio of 2:1. Using a Monte Carlo technique, we investigate the collisional de-excitation effect in these emission nebulae. We consider an emission nebula around the hot component of a symbiotic star characterized by the collisional de-excitation probability $p_{coll}\;{\sim}\;10^{-3}\;-\;10^{-4}$ per each resonance scattering, and the line center optical depths for major resonance doublets in the range ${\tau}_0\;{\sim}\;10^2\;-\;10^5$. We find that various line ratios are obtained when the product $p_{coll}{\tau}_0$ is of order unity. Our Monte Carlo calculations show that the flux ratio can be approximately fitted by a linear function of ${\log}{\tau}_0$ when ${\tau}_0p_{coll}\;{\sim}\;1$. It is briefly discussed that this corresponds to the range relevant to the emission nebulae of symbiotic stars.

• 천문학논총
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• 제30권2호
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• pp.109-112
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• 2015

We present [$Fe\;{\small{II}}$] ${\lambda}1.257{\mu}m$ spectra toward the interacting binary UY Aur with 0".14 angular resolution, obtained with the Near infrared Integral Field Spectrograph (NIFS) combined with the adaptive optics system Altair of the GEMINI observatory. In the [$Fe\;{\small{II}}$] emission, UY Aur A (primary) is brighter than UY Aur B (secondary). The blueshifted and redshifted emission between the primary and secondary show a complicated structure. The radial velocities of the [$Fe\;{\small{II}}$] emission features are similar for UY Aur A and B: ${\sim}-100km\;s^{-1}$ and ${\sim}+130km\;s^{-1}$ for the blueshifted and redshifted components, respectively. Considering the morphologies of the [$Fe\;{\small{II}}$] emissions and bipolar outflow context, we concluded that UY Aur A drives fast and widely opening outflows with an opening angle of ${\sim}90^{\circ}$ while UY Aur B has micro collimated jets.

• 천문학회보
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• 제44권1호
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• pp.77.1-77.1
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• 2019

It has been proposed by Gunn & Gott (1972) that galaxies may lose their interstellar gas by ram pressure due to the dense intra-cluster medium while falling to the cluster potential. The observational evidence for this process, which is known as ram pressure stripping, is increasing, and it is believed to be one of the key environmental effects that can dramatically change the star formation activity of galaxies and hence their evolution. Intriguingly however, some cases with clear signs of ram pressure stripping are found in the environment which betrays our expectations (e.g. large clustercentric distances), and our understandings to the detailed working principle behind ram pressure stripping seem to be still lacking. As one of the ways to gain more theoretical insights into the conditions for ram pressure stripping process, we have been comparing the gas truncation radius which is predicted based on the simple Gunn & Gott's prescription with what is actually observed in a sample of carefully selected Virgo galaxies. In this work, we present the results of our comparisons between the theoretically predicted truncation radius and the observationally measured truncation radius for individual galaxies in the sample and discuss which additional conditions are needed in order to fully understand the observations.

• 천문학회보
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• 제44권2호
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• pp.49.2-49.2
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• 2019

We present results from our long-term observing campaign, using the NASA IRTF at Maunakea, to obtain 2 - 4 ㎛ spectra of 118 red point sources in the line of sight to the Galactic Center (GC). Our sample is largely composed of point sources selected from near- and mid-infrared photometry, but also includes a number of massive young stellar objects. Many of these sources show high foreground extinction as shown by deep 3.4 ㎛ aliphatic hydrocarbon absorption feature, which is a characteristic of the diffuse ISM and comes from the long line of sight through the diffuse medium toward the Central Molecular Zone (CMZ), the central 300 pc region of the GC. The deep 3.1 ㎛ H₂O ice absorption band coming from the local, dense material in the GC CMZ suggests that most sources are likely located in the GC CMZ. A few of these sources show weak CCH₃OH ice absorption at 3.535 ㎛, which can provide a strong constraint on the CCH₃OH ice formation in the unique environment of the CMZ. From the best-fitting models, the optical depths of these features are determined and used to generate a well-rounded view of the ice composition across the GC CMZ and the spectral characteristics of massive YSOs in the GC.

• 천문학논총
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• 제32권1호
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• pp.141-145
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• 2017

We study $CO_2/H_2O$ ice abundance ratios in nearby galaxies using AKARI near-infrared slit spectroscopy. Past studies of the ices intensively examined $CO_2/H_2O$ ratios mainly in our Galaxy, and found that there were considerable variations in the $CO_2/H_2O$ ratios from object to object. The cause of the variations is, however, still under debate. As a result of the analysis of our sample that includes 1031 regions in 158 galaxies, the $CO_2/H_2O$ ratios are in a range of 0.05-0.30. In the dataset, we find that the $CO_2/H_2O$ ratios positively correlate with the $Br{\alpha}/PAH$ $3.3{\mu}m$ ratios which reflect the massive star formation activity. Furthermore, we find that the $CO_2/H_2O$ ratios positively correlate with the specific star formation rates of the galaxies where the ices are detected, that reflect the evolutionary stage of a galaxy. These results suggest that the $CO_2/H_2O$ ratios are enhanced in active star-forming regions and young galaxies.

• 천문학회보
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• 제46권1호
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• pp.50.2-51
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• 2021

Stars form exclusively in cold and dense molecular clouds. To fully understand star formation processes, it is hence a key to investigate how molecular clouds form out of the surrounding diffuse atomic gas. With an aim of shedding light in the process of the atomic-to-molecular transition in the interstellar medium, we analyze Arecibo HI emission and absorption spectral pairs along with TRAO/PMO 12CO(1-0) emission spectra toward 58 lines of sight probing in and around molecular clouds in the solar neighborhood, i.e., Perseus, Taurus, and California. 12CO(1-0) is detected from 19 out of 58 lines of sight, and we report the physical properties of HI (e.g., central velocity, spin temperature, and column density) in the vicinity of CO. Our preliminary results show that the velocity difference between the cold HI (Cold Neutral Medium or CNM) and CO (median ~ 0.7 km/s) is on average more than a factor of two smaller than the velocity difference between the warm HI (Warm Neutral Medium or WNM) and CO (median ~ 1.7 km/s). In addition, we find that the CNM tends to become colder (median spin temperature ~ 43 K) and abundant (median CNM fraction ~ 0.55) as it gets closer to CO. These results hints at the evolution of the CNM in the vicinity of CO, implying a close association between the CNM and molecular gas. Finally, in order to examine the role of HI in the formation of molecular gas, we compare the observed CNM properties to the theoretical model by Bialy & Sternberg (2016), where the HI column density for the HI-to-H2 transition point is predicted as a function of density, metallicity, and UV radiation field. Our comparison shows that while the model reproduces the observations reasonably well on average, the observed CNM components with high column densities are much denser than the model prediction. Several sources of this discrepancy, e.g., missing physical and chemical ingredients in the model such as the multi-phase ISM, non-equilibrium chemistry, and turbulence, will be discussed.

• 천문학논총
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• 제27권4호
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• pp.117-122
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• 2012

The interstellar dust grains are formed and supplied to interstellar space from asymptotic giant branch (AGB) stars or supernova remnants, and become constituents of the star- and planet-formation processes that lead to the next generation of stars. Both a qualitative, and a compositional study of this cycle are essential to understanding the origin of the pre-solar grains, the missing sources of the interstellar material, and the chemical evolution of our Galaxy. The AKARI/MIR all-sky survey was performed with two mid-infrared photometric bands centered at 9 and $18{\mu}m$. These data have advantages in detecting carbonaceous and silicate circumstellar dust of AGB stars, and the interstellar polycyclic aromatic hydrocarbons separately from large grains of amorphous silicate. By using the AKARI/MIR All-Sky point source catalogue, we surveyed C-rich and O-rich AGB stars in our Galaxy, which are the dominant suppliers of carbonaceous and silicate grains, respectively. The C-rich stars are uniformly distributed across the Galactic disk, whereas O-rich stars are concentrated toward the Galactic center, following the metallicity gradient of the interstellar medium, and are presumably affected by the environment of their birth place. We will compare the distributions of the dust suppliers with the distributions of the interstellar grains themselves by using the AKARI/MIR All-Sky diffuse maps. To enable discussions on the faint diffuse interstellar radiation, we are developing an accurate AKARI/MIR All-Sky diffuse map by correcting artifacts such as the ionising radiation effects, scattered light from the moon, and stray light from bright sources.

• 천문학논총
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• 제27권4호
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• pp.201-207
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• 2012

Following the first Public Release of the AKARI Point Source catalogues, we have worked on the production of a new far-infrared All-Sky Diffuse mapping product. In this paper we report first results from the All Sky diffuse maps that will shortly be released to the community, based on analysis of data from the Far Infrared Surveyor ($65{\mu}m-160{\mu}m$) instrument. These data are likely to have a strong impact on studies of extended structures, and the diffuse ISM.

• 미술이론과 현장
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• 제1호
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• pp.109-144
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• 2003

Orientalness is a concept that expresses the collective identity of the Orient in relation to the West. The concept itself is mutable and defined by the relationship between the two regions at different points in time. Changes in the concept depend on a number of factors, such as cultural influence, the political balance of power between the two regions, and on the interpretative scheme that defines the relationship. In addition, the geographical notion of the concept evolves culturally, socially and politically. During this process, Oriental-ness becomes Oriental-ism at times. I will attempt to survey and measure the progression of Orientalness from its emergence in early 17th century to its subsequent transformation in modern Korea as reflected in art theory and art works. The recognition of the comparative characteristics of Oriental art began when the Orient was exposed to the art of the West in the late Ming dynasty during the early 17th century. The changes in the artistic climate in China affected the late Chosun. I will start with a brief introduction of this time and the birth of Orientalness. The concept gradually changed during the period of Enlightenment(開化期) towards the end of the 19th century, and during the colonial period( 1910-1945) it took on a new form. Establishment of the concept of "Orient"as a single, unifying concept spanning across cultures and national boundaries has been attributed to late Meiji period Japan, whose intention at that time is believed to have been to build a pan-Asia(亞細亞) empire with Japan at its commanding center. It has been stressed that the real motive behind the formation of one single cultural unit, where the shared common written language was Chinese and Confucianism and Taoism were the common metaphysical traditions, was to build one political unit. When the notion of a geographical unit of Asia was replaced by the concept of Asia as a cultural and political unit, a massive growth of interest and discourse were provoked around the concept of Orientalism. When Orientalism was being formulated, Korea automatically became member of "one Asia" when the country became colonized. For Koreans, the identity of the Orient had to be defined in cultural terms, as the political notion of a nation was non-existent at that time. The definition of identity was pursued at two levels, pan-Asian and local. If Orientalism was an elite discourse centered in pan-Asian philosophical and religious tradition, localized Orientalism was a popular discourse emphasizing locality as the byproduct of natural geographic condition. After the liberation in 1945 from colonial rule, a thrust of movement arose towards political nationalism. Two types of discourses on Orientalism, elite and popular, continued as central themes in art. Despite the effort to redefine the national identity by eradicating the cultural language of the colonial past, the past was enduring well into the present time. As discussed above, even when the painting themes were selected from Korean history, the tradition of using history painting as a manifestation of political policy to glorify the local identity had its founding during the Meiji period. The elevation of folk art to the level of high art also goes back to the colonial promotion of local color and local sentiment. Again, the succession of the past (colonial) ideal was defended as the tradition assumed a distinct modern shape that was abstract in style. The concept of the "Orient" is of relative and changing nature. It was formulated in relation to Western culture or civilization. Whatever the real motive of the adoption of them had been, the superiority of the Orient was emphasized at all times. The essence of the Orient was always perceived as the metaphysical tradition as a way to downgrade Western culture as materialistic. This view still prevails and the principle of Orient was always sought in Confucianism, Taoism, and Buddhism. Even when Orientalism was employed by imperialist Japan in an effort to establish her position as the center of the Orient, the spiritual source was still in Chinese philosophy and religion. In art also, the Chinese literati tradition became the major platform for elite discourse. Orientalism was also defined locally, and the so-called local color was pursued in terms of theme and style. Thus trend continued despite the effort to eradicate the remnants of colonial culture long after liberation. These efforts are now being supported politically and also institutionalized to become the aesthetic ideal of the modern Korean art.