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C. S. Kim,J. H. Kim,H. K. Kwon,H. S. Lee,J. S. Park,이기주,K. J. Yee 한국물리학회 2010 THE JOURNAL OF THE KOREAN PHYSICAL SOCIETY Vol.57 No.4
We demonstrate that photocurrent spectroscopy can be used to study optical absorption in the active layer of InGaN-based light-emitting diodes. The temperature dependence of the photocurrent spectrum was compared with that of the photoluminescence, clearly showing the effect of carrier localizations at low temperatures below 70 K. The photocurrent spectrum investigated by applying reverse biases revealed that type-II optical transitions between the InGaN quantum well and the GaN barrier were considerable at high reverse voltages.
OGLE-2016-BLG-1190Lb: The First<i>Spitzer</i>Bulge Planet Lies Near the Planet/Brown-dwarf Boundary
Ryu, Y.-H.,Yee, J. C.,Udalski, A.,Bond, I. A.,Shvartzvald, Y.,Zang, W.,Jaimes, R. Figuera,Jørgensen, U. G.,Zhu, W.,Huang, C. X.,Jung, Y. K.,Albrow, M. D.,Chung, S.-J.,Gould, A.,Han, C.,Hwang, K.-H.,Sh American Astronomical Society 2018 The Astronomical journal Vol.155 No.1
<P>We report the discovery of OGLE-2016-BLG-1190Lb, which is likely to be the first Spitzer microlensing planet in the Galactic bulge/ bar, an assignation that can be confirmed by two epochs of high-resolution imaging of the combined source-lens baseline object. The planet's mass, M-p = 13.4 +/- 0.9 M-J, places it right at the deuteriumburning limit, i. e., the conventional boundary between 'planets' and 'brown dwarfs.' Its existence raises the question of whether such objects are really ' planets' (formed within the disks of their hosts) or 'failed stars' (lowmass objects formed by gas fragmentation). This question may ultimately be addressed by comparing disk and bulge/bar planets, which is a goal of the Spitzer microlens program. The host is a G dwarf, M-host = 0.89. +/- 0.07 M-circle dot, and the planet has a semimajor axis a similar to 2.0 au. We use Kepler K2 Campaign 9 microlensing data to break the lens-mass degeneracy that generically impacts parallax solutions from Earth-Spitzer observations alone, which is the first successful application of this approach. The microlensing data, derived primarily from near-continuous, ultradense survey observations from OGLE, MOA, and three KMTNet telescopes, contain more orbital information than for any previous microlensing planet, but not quite enough to accurately specify the full orbit. However, these data do permit the first rigorous test of microlensing orbital-motion measurements, which are typically derived from data taken over < 1% of an orbital period.</P>
OGLE-2016-BLG-0693LB: Probing the Brown Dwarf Desert with Microlensing
Ryu, Y.-H.,Udalski, A.,Yee, J. C.,Albrow, M. D.,Chung, S.-J.,Gould, A.,Han, C.,Hwang, K.-H.,Jung, Y. K.,Shin, I.-G.,Zhu, W.,Cha, S.-M.,Kim, D.-J.,Kim, H.-W.,Kim, S.-L.,Lee, C.-U.,Lee, Y.,Park, B.-G.,P American Astronomical Society 2017 The Astronomical journal Vol.154 No.6
<P>We present an analysis of microlensing event OGLE-2016-BLG-0693, based on the survey-only microlensing observations by the OGLE and KMTNet groups. In order to analyze the light curve, we consider the effects of parallax, orbital motion, and baseline slope, and also refine the result using a Galactic model prior. From the microlensing analysis, we find that the event is a binary composed of a low-mass brown dwarf (49(-18)(+20) Mj) companion and a K- or G-dwarf host, which lies at a distance of 5.0 +/- 0.6 kpc toward the Galactic bulge. The projected separation between the brown dwarf and its host star is less than similar to 5 au, thus it is likely that the brown dwarf companion is located in the brown dwarf desert.</P>
Magneto-Photoluminescence and Spin Dynamics of Self-Assembled CdSe Quantum Dots in Zn1-xMnxSe
EunsoonOh,S.M.Soh,이중욱,K.J.Yee,J.C.Woo,H.S.Jeon,김대식,S.Lee,J.K.Furdyna,H.C.Ri,H.S.Chany,S.H.Park 한국물리학회 2003 THE JOURNAL OF THE KOREAN PHYSICAL SOCIETY Vol.42 No.6
We have studied photoluminescence spectra of CdSe self-assembled quantum dots (QD's) embedded in Zn$_{1-x}$Mn$_x$Se ($x$ = 0.05 and 0.15) with and without an external magnetic field. Under a magnetic field, the photoluminescence from CdSe QD's was circularly polarized under light excitation above the bandgap energy of ZnMnSe, indicating carrier spin polarization in CdSe QD's. The time-resolved photoluminescence study showed that spin-flip occured very rapidly as photocarriers transfered from the ZnMnSe to the CdSe QD's to reach statistical equilibrium of the spin states in the CdSe QD's. The Zeeman splitting in the CdSe QD's was several meV, still larger than the thermal energy at 5 K. These results suggest that the spin-polarization in CdSe QD's is mainly due to the Zeeman splitting of carriers in the CdSe quantum dots.
외기조건변화에 따른 전열교환 환기시스템의 성능평가 및 운전방안에 관한 연구
이정재,김 광 현,박 미 지 東亞大學校 附設 環境問題硏究所 2007 硏究報告 Vol.29 No.1
Recently, it has been revising regulation of ventilator installation and detail regulation the secures comfortable & safety indoor air quality(IAQ) and obligated establishment of heat recovery ventilator in new apartment building. In this study, we offers operation and a plan of heat recovery ventilator to energy saving by measure efficiency the come out from outdoor conditions and comparing & analysis the energy saving effect. As a result of in this study was as follows : In case, we think that if it do not show that the upper than average of 30 percents absolute humidity in spring and autumn, it should profitably operation "by-pass mode". (2) Energy saving effect appears the heat recovery ventilator show widely rate ratio compared to constant air volume system.
A SUB-SATURN MASS PLANET, MOA-2009-BLG-319Lb
Miyake, N.,Sumi, T.,Dong, Subo,Street, R.,Mancini, L.,Gould, A.,Bennett, D. P.,Tsapras, Y.,Yee, J. C.,Albrow, M. D.,Bond, I. A.,Fouqué,, P.,Browne, P.,Han, C.,Snodgrass, C.,Finet, F.,Furusawa, K IOP Publishing 2011 The Astrophysical journal Vol.728 No.2
<P>We report the gravitational microlensing discovery of a sub-Saturn mass planet, MOA-2009-BLG-319Lb, orbiting a K-or M-dwarf star in the inner Galactic disk or Galactic bulge. The high-cadence observations of the MOA-II survey discovered this microlensing event and enabled its identification as a high-magnification event approximately 24 hr prior to peak magnification. As a result, the planetary signal at the peak of this light curve was observed by 20 different telescopes, which is the largest number of telescopes to contribute to a planetary discovery to date. The microlensing model for this event indicates a planet-star mass ratio of q = (3.95 +/- 0.02) x 10(-4) and a separation of d = 0.97537 +/- 0.00007 in units of the Einstein radius. A Bayesian analysis based on the measured Einstein radius crossing time, t(E), and angular Einstein radius,theta(E), along with a standard Galactic model indicates a host star mass of M-L = 0.38(-0.18)(+0.34) M-circle dot and a planet mass of M-p = 50(-24)(+44)M(circle plus), which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4(-0.6)(+1.2) AU and a distance to the planetary system of D-L = 6.1(-1.2)(+1.1) kpc. This separation is similar to 2 times the distance of the snow line, a separation similar to most of the other planets discovered by microlensing.</P>
KMT-2016-BLG-0212: First KMTNet-Only Discovery of a Substellar Companion
K.-H. Hwang,H.-W. Kim,D.-J. Kim,A. Gould,M. D. Albrow,S.-J. Chung,C. Han,Y. K. Jung,Y.-H. Ryu,I.-G. Shin,Y. Shvartzvald,J. C. Yee,W. Zang,W. Zhu,S.-M. Cha,S.-L. Kim,C.-U. Lee,D.-J. Lee,Y. Lee,B.-G. Pa 한국천문학회 2018 Journal of The Korean Astronomical Society Vol.51 No.6
We present the analysis of KMT-2016-BLG-0212, a low flux-variation $(I_{\rm flux-var}\sim 20$ mag) microlensing event, which is in a high-cadence ($\Gamma = 4 {\rm hr}^{-1}$) field of the three-telescope Korea Microlensing Telescope Network (KMTNet) survey. The event shows a short anomaly that is incompletely covered due to the brief visibility intervals that characterize the early microlensing season when the anomaly occurred. We show that the data are consistent with two classes of solutions, characterized respectively by low-mass brown-dwarf $(q=0.037)$ and sub-Neptune $(q<10^{-4})$ companions. Future high-resolution imaging should easily distinguish between these solutions.
MOA-2011-BLG-293Lb: A TEST OF PURE SURVEY MICROLENSING PLANET DETECTIONS
Yee, J. C.,Shvartzvald, Y.,Gal-Yam, A.,Bond, I. A.,Udalski, A.,Kozłowski, S.,Han, C.,Gould, A.,Skowron, J.,Suzuki, D.,Abe, F.,Bennett, D. P.,Botzler, C. S.,Chote, P.,Freeman, M.,Fukui, A.,Furusawa, K. IOP Publishing 2012 The Astrophysical journal Vol.755 No.2
<P>Because of the development of large-format, wide-field cameras, microlensing surveys are now able to monitor millions of stars with sufficient cadence to detect planets. These new discoveries will span the full range of significance levels including planetary signals too small to be distinguished from the noise. At present, we do not understand where the threshold is for detecting planets. MOA-2011-BLG-293Lb is the first planet to be published from the new surveys, and it also has substantial follow-up observations. This planet is robustly detected in survey+follow-up data (Delta chi(2) similar to 5400). The planet/host mass ratio is q = (5.3 similar to 0.2) x 10(-3). The best-fit projected separation is s = 0.548 +/- 0.005 Einstein radii. However, due to the s <-> s(-1) degeneracy, projected separations of s-1 are only marginally disfavored at Delta chi(2) = 3. A Bayesian estimate of the host mass gives M-L = 0.43(-0.17)(+0.27) M-circle dot, with a sharp upper limit of M-L < 1.2 M-circle dot from upper limits on the lens flux. Hence, the planet mass is m(p) = 2.4(-0.9)(+1.5) M-Jup, and the physical projected separation is either r(perpendicular to) similar or equal to 1.0 AU or r(perpendicular to) similar or equal to 3.4 AU. We show that survey data alone predict this solution and are able to characterize the planet, but the Delta chi(2) is much smaller (Delta chi(2) similar to 500) than with the follow-up data. The Delta chi(2) for the survey data alone is smaller than for any other securely detected planet. This event suggests a means to probe the detection threshold, by analyzing a large sample of events like MOA-2011-BLG-293, which have both follow-up data and high-cadence survey data, to provide a guide for the interpretation of pure survey microlensing data.</P>
Yee, J. C.,Udalski, A.,Sumi, T.,Dong, Subo,Kozłowski, S.,Bird, J. C.,Cole, A.,Higgins, D.,McCormick, J.,Monard, L. A. G.,Polishook, D.,Shporer, A.,Spector, O.,Szymań,ski, M. K.,Kubiak, M.,Pietrzy IOP Publishing 2009 The Astrophysical journal Vol.703 No.2
<P>We analyze the extreme high-magnification microlensing event OGLE-2008-BLG-279, which peaked at a maximum magnification of A similar to 1600 on 2008 May 30. The peak of this event exhibits both finite-source effects and terrestrial parallax, from which we determine the mass of the lens, M-l = 0.64 +/- 0.10 M-circle dot, and its distance, D-l = 4.0 +/- 0.6 kpc. We rule out Jupiter-mass planetary companions to the lens star for projected separations in the range 0.5-20 AU. More generally, we find that this event was sensitive to planets with masses as small as 0.2 M-circle dot similar or equal to 2 (MMars) with projected separations near the Einstein ring (similar to 3 AU).</P>