Metabolizable Energy Values of Some Poultry Feeds Determined by Various Methods and Their Estimation Using Metabolizability of the Dry Matter

Han, I. K.,Hochstetler, H.W.,Scott, M.L. The Korean Society of Poultry Science 1976 韓國家禽學會誌 Vol.3 No.1

Metabolizable energy (M.E.) values of 12 U.S. feedstuffs and 10 Korean feed ingredients for poultry were determined both by the total collection method and by the chromic oxide indicator method. It was found that M.E. values of most poultry feedstuffs can be measured accurately by either method. Limitation of feed intake to almost maintenance level(approximately 60% of ad libitum) did not increase or decrease the M.E. value of the feeds. An attempt was made to establish a prediction equation to estimate the M.E. values based on the apparent metabolizability of dry matter (D.M.) in the feedstuffs. The results indicated that linear relationships do exist between D. M. metabolizability and M.E. values of carbohydrate-rich feedstuffs (grains and their by-products) or protein-rich feed ingredients (oil seed meals and animal protein feeds) or lipid-rich feeds (fats and oils) as follows: The prediction equation for carbohydrate-rich feedstuffs was Y = 0.0947x - 3.498 ($r^2\;=\;0.99$, Sy.x = 0.015); for protein-rich feed ingredients. it was Y = 0.1234x - 4.898 ($r^2\;=\;0.99$, Sy.x = 0.027); and for lipid-rich feedstuffs it was Y = 0.0844x + 0.774 ($r^2\;=\;0.99$, Sy.x = 0.032). where x = metabolizability of dry matter of feeds in %, and Y=metabolizable energy values in kcal./g. The errors attached to these estimations were relatively small. Thus these prediction equations may be very useful for estimation of the M.E. values from D.M. apparent metaboiizability of feeds, especially in areas of the world where calorimetry is not possible.

OGLE-2011-BLG-0265Lb: A JOVIAN MICROLENSING PLANET ORBITING AN M DWARF

Skowron, J.,Shin, I.-G.,Udalski, A.,Han, C.,Sumi, T.,Shvartzvald, Y.,Gould, A.,Dominis Prester, D.,Street, R. A.,Jørgensen, U. G.,Bennett, D. P.,Bozza, V.,Szymań,ski, M. K.,Kubiak, M.,Pietrzy
IOP Publishing 2015 The Astrophysical journal Vol.804 No.1

<P>We report the discovery of a Jupiter-mass planet orbiting an M-dwarf star that gave rise to the microlensing event OGLE-2011-BLG-0265. Such a system is very rare among known planetary systems and thus the discovery is important for theoretical studies of planetary formation and evolution. High-cadence temporal coverage of the planetary signal, combined with extended observations throughout the event, allows us to accurately model the observed light curve. However, the final microlensing solution remains degenerate, yielding two possible configurations of the planet and the host star. In the case of the preferred solution, the mass of the planet is M-p = 0.9 +/- 0.3 M-J, and the planet is orbiting a star with a mass M = 0.22 +/- 0.06 M-circle dot. The second possible configuration (2 sigma away) consists of a planet with M-p = 0.6 +/- 0.3M(J) and host star with M = 0.14 +/- 0.06M(circle dot). The system is located in the Galactic disk 3-4 kpc toward the Galactic bulge. In both cases, with an orbit size of 1.5-2.0 AU, the planet is a 'cold Jupiter'-located well beyond the 'snow line' of the host star. Currently available data make the secure selection of the correct solution difficult, but there are prospects for lifting the degeneracy with additional follow-up observations in the future, when the lens and source star separate.</P>

General trends of atmospheric mercury concentrations in urban and rural areas in Korea and characteristics of high-concentration events

Han, Y.J.,Kim, J.E.,Kim, P.R.,Kim, W.J.,Yi, S.M.,Seo, Y.S.,Kim, S.H. Pergamon Press ; Elsevier [distribution] 2014 Atmospheric environment Vol.94 No.-

Long-term measurement of speciated Hg concentrations is the first step toward identifying the seasonal and spatial characteristics of Hg concentrations; however, atmospheric Hg research is scarce in Korea. In this study, total gaseous mercury (TGM), gaseous oxidized mercury (GOM) and particle-bound mercury (PBM) were measured in urban (Seoul) and rural (Chuncheon) areas over a more than 3 year period in order to improve the understanding of speciated Hg transport. The mean concentrations of TGM, GOM and PBM were 3.72 +/- 2.96 (0.19-149.84) ng m<SUP>-3</SUP>, 11.3 +/- 9.5 (0.9-57.3) pg m<SUP>-3</SUP>, and 13.4 +/- 12.0 (2.1-64.3) pg m<SUP>-3</SUP> at the Seoul site and 2.12 +/- 1.47 (0.26-10.75) ng m<SUP>-3</SUP>, 2.7 +/- 2.7 (0.1-16.9) pg m<SUP>-3</SUP>, and 3.7 +/- 5.7 (0.1-30.0) pg m<SUP>-3</SUP> in Chuncheon. Both long-range transport and local sources caused high TGM concentration events, while local coal combustion was a main cause of enhancing the GOM and PBM concentrations in Seoul. However, there was no correlation between the pollutants emitted from coal combustion and the speciated Hg concentration in Chuncheon, indicating that other mechanisms were involved in the Hg increase. We found a positive correlation between the GOM and the O<SUB>3</SUB> concentrations and a negative correlation between the GEM and the GOM concentrations, especially on foggy days, suggesting that the oxidation of GEM was an important source for GOM in Chuncheon. In addition, the ratio of PBM/GOM was inversely proportional to the atmospheric temperature and directly proportional to the relative humidity, which suggests that the in-situ formation of PBM through gas-particle partitioning of GOM was important in rural areas.

OGLE-2015-BLG-0196: GROUND-BASED GRAVITATIONAL MICROLENS PARALLAX CONFIRMED BY SPACE-BASED OBSERVATION

Han, C.,Udalski, A.,Gould, A.,Zhu, Wei,Szymań,ski, M. K.,Soszyń,ski, I.,Skowron, J.,Mró,z, P.,Poleski, R.,Pietrukowicz, P.,Kozłowski, S.,Ulaczyk, K.,Pawlak, M.,Yee, J. C.,Beichman, C. American Astronomical Society 2017 The Astrophysical journal Vol.834 No.1

<P>In this paper, we present an analysis of the binary gravitational microlensing event OGLE-2015-BLG-0196. The event lasted for almost a year, and the light curve exhibited significant deviations from the lensing model based on the rectilinear lens-source relative motion, enabling us to measure the microlens parallax. The ground-based microlens parallax is confirmed by the data obtained from space-based microlens observations using the Spitzer telescope. By additionally measuring the angular Einstein radius from the analysis of the resolved caustic crossing, the physical parameters of the lens are determined up to the twofold degeneracy, u(0) < 0 and u(0) > 0, solutions caused by the well-known 'ecliptic' degeneracy. It is found that the binary lens is composed of two M dwarf stars with similar masses, M-1 = 0.38 +/- 0.04M(circle plus) (0.50 +/- 0.05M(circle plus)) and M-2 = 0.38 +/- 0.04M(circle plus) (0.55 +/- 0.06M(circle plus)), and the distance to the lens is D-L = 2.77. +/- 0.23 kpc (3.30 +/- 0.29 kpc). Here the physical parameters outside and inside the parentheses are for the u(0) < 0 and u(0) > 0 solutions, respectively.</P>

OGLE-2016-BLG-1469L: Microlensing Binary Composed of Brown Dwarfs

Han, C.,Udalski, A.,Sumi, T.,Gould, A.,Albrow, M. D.,Chung, S.-J.,Jung, Y. K.,Ryu, Y.-H.,Shin, I.-G.,Yee, J. C.,Zhu, W.,Cha, S.-M.,Kim, S.-L.,Kim, D.-J.,Lee, C.-U.,Lee, Y.,Park, B.-G.,Soszyń,ski, American Astronomical Society 2017 The Astrophysical journal Vol.843 No.1

<P>We report the discovery of a binary composed of two brown dwarfs, based on the analysis of the microlensing event OGLE-2016-BLG-1469. Thanks to the detection of both finite-source and microlens-parallax effects, we are able to measure both the masses M-1 similar to 0.05M(circle dot) and. M-2 similar to 0.01M(circle dot), and the. distance D-L similar to 4.5 kpc, as well as the projected separation a(perpendicular to) similar to 0.33 au. This is the third brown-dwarf binary detected using the microlensing method, demonstrating the usefulness of microlensing in detecting field brown-dwarf binaries with separations of less than 1 au.</P>

Robust PEGylated hyaluronic acid nanoparticles as the carrier of doxorubicin: Mineralization and its effect on tumor targetability in vivo

Han, H.S.,Lee, J.,Kim, H.R.,Chae, S.Y.,Kim, M.,Saravanakumar, G.,Yoon, H.Y.,You, D.G.,Ko, H.,Kim, K.,Kwon, I.C.,Park, J.C.,Park, J.H. Elsevier Science Publishers 2013 Journal of controlled release Vol.168 No.2

The in vivo stability and tumor targetability of self-assembled polymeric nanoparticles are crucial for effective drug delivery. In this study, to develop biostable nanoparticles with high tumor targetability, poly(ethylene glycol)-conjugated hyaluronic acid nanoparticles (PEG-HANPs) were mineralized through controlled deposition of inorganic calcium and phosphate ions on the nanoparticular shell via a sequential addition method. The resulting nanoparticles (M-PEG-HANPs) had a smaller size (153.7+/-4.5nm) than bare PEG-HANPs (265.1+/-9.5nm), implying that mineralization allows the formation of compact nanoparticles. Interestingly, when the mineralized nanoparticles were exposed to acidic buffer conditions (<pH6.5), their sizes increased rapidly due to dissolution of the inorganic minerals. Doxorubicin (DOX), chosen as the model anticancer drug, was effectively encapsulated into the bare and mineralized nanoparticles. For bare PEG-HANPs, DOX was released in a sustained manner and its release rate was not dependent on the pH of the solution. On the other hand, DOX release from M-PEG-HANPs was pH-dependent: i.e. DOX was slowly released from nanoparticles under physiological condition (pH7.4), whereas its release rates were much higher at mildly acidic environments (<pH6.5). From in vivo biodistribution study, it was found that M-PEG-HANPs could reach the tumor site more effectively than bare PEG-HANPs. The antitumor efficacy of DOX-loaded nanoparticles was evaluated after systemic administration into the tumor-bearing mice. Of the samples tested, the most effective antitumor efficacy was observed for DOX-loaded M-PEG-HANPs. Overall, these results suggest that M-PEG-HANPs could be a promising carrier for an anticancer drug.

Phase II study and biomarker analysis of cetuximab combined with modified FOLFOX6 in advanced gastric cancer

Han, S-W,Oh, D-Y,Im, S-A,Park, S R,Lee, K-W,Song, H S,Lee, N-S,Lee, K H,Choi, I S,Lee, M H,Kim, M A,Kim, W H,Bang, Y-J,Kim, T-Y Nature Publishing Group 2009 The British journal of cancer Vol.100 No.2

<P>This prospective study was conducted with the Korean Cancer Study Group to evaluate the efficacy and safety of cetuximab combined with modified FOLFOX6 (mFOLFOX6) as first-line treatment in recurrent or metastatic gastric cancer and to identify potential predictive biomarkers. Patients received cetuximab 400 mg m<SUP>−2</SUP> at week 1 and 250 mg m<SUP>−2</SUP> weekly thereafter until disease progression. Oxaliplatin (100 mg m<SUP>−2</SUP>) and leucovorin (100 mg m<SUP>−2</SUP>) were administered as a 2-h infusion followed by a 46-h continuous infusion of 5-fluorouracil (2400 mg m<SUP>−2</SUP>) every 2 weeks for a maximum of 12 cycles. Biomarkers potentially associated with efficacy were analysed. Among 38 evaluable patients, confirmed response rate (RR) was 50.0% (95% CI 34.1–65.9). Median time-to-progression (TTP) was 5.5 months (95% CI 4.5–6.5) and overall survival (OS) 9.9 months. Eleven patients having tumour EGFR expression by immunohistochemistry with low serum EGF and TGF-<I>α</I> levels showed a 100% RR compared to 37.0% in the remaining 27 patients (<I>P</I><0.001). Moreover, ligand level increased when disease progressed in seven out of eight patients with EGFR expression and low baseline ligand level. No patient exhibited EGFR amplification or K-ras mutations. Gastric cancer patients with EGFR expression and low ligand levels had better outcomes with cetuximab/mFOLFOX6 treatment.</P>

OGLE-2014-BLG-0257L: A MICROLENSING BROWN DWARF ORBITING A LOW-MASS M DWARF

Han, C.,Jung, Y. K.,Udalski, A.,Gould, A.,Bozza, V.,Szymań,ski, M. K.,Soszyń,ski, I.,Poleski, R.,Kozłowski, S.,Pietrukowicz, P.,Skowron, J.,Ulaczyk, K.,Wyrzykowski, Ł. American Astronomical Society 2016 The Astrophysical Journal Vol.822 No.2

<P>In this paper, we report the discovery of a binary composed of a brown dwarf (BD) and a low-mass M dwarf from observation of the microlensing event OGLE-2014-BLG-0257. The resolution of the very brief caustic crossing combined with the detection of subtle continuous deviation in the lensing light curve induced by the Earth's orbital motion enable us to precisely measure both the Einstein radius theta(E) and the lens parallax pi(E), which are the two quantities needed to unambiguously determine the mass and distance to the lens. It is found that the companion is a substellar BD with a mass of 0.036 +/- 0.005 M-circle dot (37.7 +/- 5.2 M-J) and it is orbiting an M dwarf with a mass of 0.19 +/- 0.02 M-circle dot. The binary is located at a distance of 1.25 +/- 0.13 kpc toward the Galactic bulge and the projected separation between the binary components is 0.61 +/- 0.07 au. The separation scaled by the mass of the host is 3.2 au/M-circle dot. Based on the assumption that separations scale with masses, the discovered BD is located in the BD desert. With the growing sample of BDs in various environments, microlensing will provide a powerful probe of BDs in the Galaxy.</P>

Fabrication of highly permeable thin-film nanocomposite forward osmosis membranes <i>via</i> the design of novel freestanding robust nanofiber substrates

Obaid, M.,Kang, Yesol,Wang, Sungrok,Yoon, Myung-Han,Kim, Chang-Min,Song, Jun-ho,Kim, In S. The Royal Society of Chemistry 2018 Journal of Materials Chemistry A Vol.6 No.25

<P>Although forward osmosis (FO) technology is considered to be a sustainable solution for the water and energy shortage, it has not been commercialized yet due to a few factors. Internal concentration polarization (ICP) is one of the most important barriers preventing the commercialization of the technology. To overcome the ICP obstacle, novel high-performance thin-film nanocomposite (TFN) membranes were successfully fabricated <I>via</I> interfacial polymerization on robust freestanding graphene oxide (GO) incorporated polyvinylidene fluoride (PVDF) nanofiber substrates. Compared to the pristine PVDF nanofiber substrate, the incorporation of GO (ranging from 0.1-15 wt%) significantly alters the chemical structure, porosity, wettability, morphology, and mechanical properties of the substrate, leading to an enhancement in the TFN membrane performance. The results showed that TFN5 (containing 5% GO) membrane possesses the lowest structural parameter of 85.5 μm (one of the best values in the literature), indicating a low internal concentration polarization (ICP) effect, resulting in a remarkably heightened water permeability (<I>A</I>; 2.96 L m<SUP>−2</SUP> h<SUP>−1</SUP> bar<SUP>−1</SUP>, enhanced by 167% compared to TFC). As a result, the membrane achieved the highest FO water flux at all draw solution concentrations (0.5-2 M NaCl), and the maximum FO water flux was 80.9 L m<SUP>−2</SUP> h<SUP>−1</SUP> (LMH) with a comparable specific salt flux (<I>J</I>s/<I>J</I>v) of 0.41 g L<SUP>−1</SUP> in the active layer facing the deionized feed water (AL-FS) when 2 M NaCl was applied as a draw solution. Interestingly, TFN5 was found to be the strongest material, with outstanding flexibility and strength over that of the TFC membrane. Furthermore, it showed high stability and durability during long-term FO operation. More importantly, the interaction mechanism between PVDF and GO was proposed schematically. Overall, the obtained results show highly efficient and promising TFN membranes that may overcome the drawbacks of the aforementioned FO membranes.</P>

MOA-2010-BLG-073L: AN M-DWARF WITH A SUBSTELLAR COMPANION AT THE PLANET/BROWN DWARF BOUNDARY

Street, R. A.,Choi, J.-Y.,Tsapras, Y.,Han, C.,Furusawa, K.,Hundertmark, M.,Gould, A.,Sumi, T.,Bond, I. A.,Wouters, D.,Zellem, R.,Udalski, A.,Snodgrass, C.,Horne, K.,Dominik, M.,Browne, P.,Kains, N.,Br IOP Publishing 2013 The Astrophysical journal Vol.763 No.1

<P>We present an analysis of the anomalous microlensing event, MOA-2010-BLG-073, announced by the Microlensing Observations in Astrophysics survey on 2010 March 18. This event was remarkable because the source was previously known to be photometrically variable. Analyzing the pre-event source light curve, we demonstrate that it is an irregular variable over timescales >200 days. Its dereddened color, (V - I)(S),(0), is 1.221 +/- 0.051 mag, and from our lens model we derive a source radius of 14.7 +/- 1.3 R-circle dot, suggesting that it is a red giant star. We initially explored a number of purely microlensing models for the event but found a residual gradient in the data taken prior to and after the event. This is likely to be due to the variability of the source rather than part of the lensing event, so we incorporated a slope parameter in our model in order to derive the true parameters of the lensing system. We find that the lensing system has a mass ratio of q = 0.0654 +/- 0.0006. The Einstein crossing time of the event, t(E) = 44.3 +/- 0.1 days, was sufficiently long that the light curve exhibited parallax effects. In addition, the source trajectory relative to the large caustic structure allowed the orbital motion of the lens system to be detected. Combining the parallax with the Einstein radius, we were able to derive the distance to the lens, D-L = 2.8 +/- 0.4 kpc, and the masses of the lensing objects. The primary of the lens is an M-dwarf with M-L,M-1 = 0.16 +/- 0.03 M-circle dot, while the companion has M-L,M-2 = 11.0 +/- 2.0 M-J, putting it in the boundary zone between planets and brown dwarfs.</P>