• 천문학회보
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• 제43권1호
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• pp.62.3-63
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• 2018

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.

• 한국대기환경학회지
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• 제12권4호
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• pp.407-419
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• 1996

Characteristics of visual air quality in Seoul have been investigated between June 13 and 21, 1994. Optical properties (extinction coefficient and particle scattering coefficient), meteorological parameters (relative humidity, temperature, wind speed, wind direction, and cloud cover), particle characteristics (mass size distribution, components) were measured and analyzed. During measurement periods, northwest wind with less than 2m/sec of wind speed deteriorates visibility. Effects of relative humidity are though to be not a direct factor which influence to visibility through the size change due to hygroscopic species in aerosol. During the smoggy period both the aerosol mass concentration and fine particle fraction of the size distribution are increased compared to the clear period. Sulfate, organic carbon, and elemental carbon in aerosol are the major species in determining the occurrence and severity of a smog in Seoul.

• 대한원격탐사학회지
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• 제37권6_2호
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• pp.1793-1801
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• 2021

2015년 1월부터 2020년 6월까지 라이다를 이용하여 측정된 532와 1064 nm의 후방산란계수와 532 nm의 편광소멸도를 이용하여 532 nm의 후방산란계수를 PM₁₀, PM_2.5-10, PM_2.5에 해당하는 세 유형으로 구분하고 지상에서 측정된 질량 농도를 이용하여 각각의 질량소산효율을 산출하였다. 산출된 질량소산효율의 전체 평균값은 PM₁₀, PM_2.5-10, PM_2.5에서 각각 5.1±2.5, 1.7±3.7, 9.3±6.3 m²/g으로 PM_2.5가 가장 높은 값을 보였다. PM₁₀과 PM_2.5의 질량 농도가 낮을 때 평균 이상의 높은 질량소산효율이 산출되었으며 질량 농도가 높아질수록 질량소산효율이 감소되는 경향을 확인하였다. 황사의 혼합 정도에 따른 유형별로 질량소산효율을 산출하였을 때, PM_2.5-10는 황사의 영향으로 오염입자(pollution aerosol, PA)가 2.1±2.8 m²/g으로 오염입자가 주요한 혼합입자(pollution-dominated mixture, PDM), 황사가 주요한 혼합입자 (dust-dominated mixture, DDM), 순수황사 (pure dust, PD)의 1.1±1.8, 1.4±3.3, 1.1±1.5 m²/g보다 두 배 정도 높은 값을 보였다. 하지만, PM_2.5는 9.4±6.5, 9.0±5.8, 10.3±7.5, 9.1±9.0 m²/g으로 유형 구분 없이 비슷한 값을 보였다. PM₁₀의 질량소산효율은 PA, PDM, DDM, PD 에서 각각 5.6±2.9, 4.4±2.0, 3.6±2.9, 2.8±2.4 m²/g으로 황사의 비율이 감소할수록 증가하는 경향을 보였다. 동일한 질량 농도 또는 황사 혼합에 따른 동일한 유형을 보이더라도 PM_2.5/PM₁₀ 값이 낮아질수록 PM_2.5-10의 질량소산효율은 감소하고, PM_2.5의 질량소산효율은 증가하는 경향을 보였다.

• 천문학논총
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• 제32권1호
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• pp.313-315
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• 2017

We present physical properties of $24{\mu}m$ galaxies detected by AKARI and Spitzer and their evolution between redshifts 0.4 < z < 2. Using multi-wavelength data from X-ray to radio observations in NEP Deep Field (for AKARI) and Subaru/XMM-Newton Deep Field (for Spitzer), we derive photometric redshift, stellar mass, star-formation rate (SFR), dust extinction magnitude and rest-frame luminosities/colors of the $24{\mu}m$ galaxies from photometric SED fitting. We infer the SFRs from rest-frame ultraviolet luminosity and total infrared luminosity calibrated against Herschel photometric data. For both survey fields, we obtain complete samples with stellar mass of > $10^{10}M_{\odot}$ and SFR of > $30M_{\odot}/yr$ up to z = 2. We find that specific SFRs evolves with redshift at all stellar masses in NON-power-law galaxies (non-PLGs) as star-formation dominant luminous infrared galaxies (LIRGs). The correlations between specific SFR and stellar mass in the Spitzer and AKARI galaxy samples are well consistent with trends of the main sequence galaxies. We also discuss nature of PLGs and their evolution.

• 천문학회보
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• 제41권2호
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• pp.57.2-57.2
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• 2016

Polarimetry is an important tool for studying the physical processes in the interstellar medium, including star-forming regions. Polarimetry of young stellar objects and their circumstellar structures provides invaluable information about distributions of matter and configurations of magnetic fields in their environments. However, only a few near-infrared circular polarization (CP) observations were reported so far (before our survey). A systematic near-infrared CP survey has been firstly conducted in various star-forming regions, covering high-mass, intermediate-mass, and low-mass young stellar objects. All the observations were made using the SIRPOL imaging polarimeter on the Infrared Survey Facility (IRSF) 1.4 m telescope at the South African Astronomical Observatory (SAAO). In this presentation, we present the first CP survey results. The polarization patterns, extents, and maximum degrees of circular and linear polarizations are used to determine the prevalence and origin of CP in the star-forming regions. Our results are explained with a combination of circumstellar scattering and dichroic extinction mechanism generating the high degrees of CP in star-forming regions. The universality of the large and extended CPs in star-formaing regions can also be linked with the origin of homochirality of life.

• 천문학회지
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• 제49권3호
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• pp.93-107
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• 2016

Augmenting the Wide Field Infrared Survey Telescope (WFIRST) microlensing campaigns with intensive observations from a ground-based network of wide-field survey telescopes would have several major advantages. First, it would enable full two-dimensional (2-D) vector microlens parallax measurements for a substantial fraction of low-mass lenses as well as planetary and binary events that show caustic crossing features. For a significant fraction of the free-floating planet (FFP) events and all caustic-crossing planetary/binary events, these 2-D parallax measurements directly lead to complete solutions (mass, distance, transverse velocity) of the lens object (or lens system). For even more events, the complementary ground-based observations will yield 1-D parallax measurements. Together with the 1-D parallaxes from WFIRST alone, they can probe the entire mass range M ≳ M_⊕. For luminous lenses, such 1-D parallax measurements can be promoted to complete solutions (mass, distance, transverse velocity) by high-resolution imaging. This would provide crucial information not only about the hosts of planets and other lenses, but also enable a much more precise Galactic model. Other benefits of such a survey include improved understanding of binaries (particularly with low mass primaries), and sensitivity to distant ice-giant and gas-giant companions of WFIRST lenses that cannot be detected by WFIRST itself due to its restricted observing windows. Existing ground-based microlensing surveys can be employed if WFIRST is pointed at lower-extinction fields than is currently envisaged. This would come at some cost to the event rate. Therefore the benefits of improved characterization of lenses must be weighed against these costs.

• 한국가시화정보학회지
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• 제1권1호
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• pp.98-106
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• 2003

A PLLIF (Planar Liquid Laser Induced Fluorescence) technique has been known to be a useful tool for the measurement of the spray patterns for various spray injectors because it can obtain two-dimensional images with high spatial resolutions without any intrusion on the spray field. In case of dense spray, however, the secondary emission as well as the extinction of an incident laser beam or a fluorescence signal can cause errors in quantifying a mass distribution. Unfortunately, a like-doublet injector which has a dense spray zone at the center may not be a good example or the application of the PLLIF technique. Therefore, we took PLLIF data for the like-doublet injector with a 12 bit color CCD camera by varying laser power, and then assessed their accuracy by comparing with the data obtained with a mechanical patternator and a PDPA (Phase Doppler Particle Analyzer). The experimental results showed that the gray level of fluorescence signal increases nonlinearly due to a secondary emission at the dense spray zone but this nonlinearity can be avoided by reducing the incident laser beam power. In addition, the mass flux distribution of the spray could be obtained by using the mass concentration data from PLLIF technique and the velocity profiles of liquid drops, and this distribution showed good agreement with that of mechanical pattemator. Therefore, it is possible that the PLLIF technique can be successfully applied to finding the mass distributions of like-doublet injectors.

• 천문학회지
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• 제48권6호
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• pp.343-355
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• 2015

There is much observational evidence that active star formation is taking place in the Hii regions Sh 2-255 – 257. We present a photometric study of this star forming region (SFR) using imaging data obtained in passbands from the optical to the mid-infrared, in order to study the star formation process. A total of 218 members were identified using various selection criteria based on their observational properties. The SFR is reddened by at least E(B −V ) = 0.8 mag, and the reddening law toward the region is normal (R_V = 3.1). From the zero-age main sequence fitting method it is confirmed that the SFR is 2.1 ± 0.3 kpc from the Sun. The median age of the identified members is estimated to be about 1.3 Myr from a comparison of the Hertzsprung-Russell diagram (HRD) with stellar evolutionary models. The initial mass function (IMF) is derived from the HRD and the near-infrared (J, J −H) color-magnitude diagram. The slope of the IMF is about Γ = −1.6 ± 0.1, which is slightly steeper than that of the Salpeter/Kroupa IMF. It implies that low-mass star formation is dominant in the SFR. The sum of the masses of all the identified members provides the lower limit of the cluster mass (169M_⊙). We also analyzed the spectral energy distribution (SED) of pre-main sequence stars using the SED fitting tool of Robitaille et al., and confirm that there is a significant discrepancy between stellar mass and age obtained from two different methods based on the SED fitting tool and the HRD.

• 천문학회보
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• 제40권1호
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• pp.71.3-71.3
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• 2015

Deep UBVI and $H{\alpha}$ photometry of the ${\eta}$ Carina nebula, one of the brightest nebulae on the sky, was obtained with the CTIO 4m telescope and MOSAIC II CCD Camera to determine the initial mass function down to low-mass (~1 M¤) stars. We modified the spatial variation coefficients in transformation relations of the MOSAIC II CCD. From the cross-identification of optical sources with previous surveys in X-ray, near-infrared, and mid-infrared, a clear PMS sequence is revealed in the optical color-magnitude diagrams down to V=23 mag. Our previous SSO 1m UBVI data for Trumpler 14 (Tr 14) and Trumpler 16 (Tr 16) region, and additional SSO 1m UBVI data for Trumpler 15 (Tr 15) region were combined with the CTIO 4m data to re-examine the reddening law and distance of the young open clusters in the ${\eta}$ Carina nebula. From the new photometric data for Tr 15 region, we report that RV[=AV/E(B-V)], the total-to-selective extinction ratio, decreases from southern part of the nebula (Tr 14 and Tr 16) to northern part (Tr 15) in our field of view.

• 천문학논총
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• 제32권1호
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• pp.151-153
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• 2017

Early-type galaxies (ETGs) are generally dominated by old low-mass stars, which are not very productive of dust, and hot interstellar plasmas, which are very destructive of dust. Thus ETGs provide harsh environments for survival of dust. It has been found that some ETGs contain a large amount of dust, and yet its supply mechanism is not understood well. We present the result of a systematic study of dust in ETGs with the AKARI mid- and far-infrared all-sky surveys. From the AKARI result and the Ks band data obtained by ground-based telescopes, we find that there is a global correlation between the dust mass and stellar luminosity. We also compare the AKARI all-sky survey result with the CO data to discuss origins of dust in ETGs.