Author: "Koo, J.-R." - Searchworks@Jio Institute Digital Library Search Results

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124 results on '"Koo, J.-R."'

1. Apsidal motions of 90 eccentric binary systems in the Small Magellanic Cloud

Author: Hong, K., Lee, J. W., Kim, S. -L., Koo, J. -R., and Lee, C. -U.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We examined light curves of 1138 stars brighter than 18.0 mag in the $I$ band and less than a mean magnitude error of 0.1 mag in the $V$ band from the OGLE-III eclipsing binary catalogue, and found 90 new binary systems exhibiting apsidal motion. In this study, the samples of apsidal motion stars in the SMC were increased by a factor of about 3 than previously known. In order to determine the period of the apsidal motion for the binaries, we analysed in detail both the light curves and eclipse timings using the MACHO and OGLE photometric database. For the eclipse timing diagrams of the systems, new times of minimum light were derived from the full light curve combined at intervals of one year from the survey data. The new 90 binaries have apsidal motion periods in the range of 12$-$897 years. An additional short-term oscillation was detected in four systems (OGLE-SMC-ECL-1634, 1947, 3035, and 4946), which most likely arises from the existence of a third body orbiting each eclipsing binary. Since the systems presented here are based on homogeneous data and have been analysed in the same way, they are suitable for further statistical analysis., Comment: 20 pages, 7 figures, 5 tables. Submitted to MNRAS
Published: 2016
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2. A Sub-Earth-Mass Moon Orbiting a Gas Giant Primary or a High Velocity Planetary System in the Galactic Bulge

Author: Bennett, D. P., Batista, V., Bond, I. A., Bennett, C. S., Suzuki, D., Beaulieu, J. -P., Udalski, A., Donatowicz, J., Abe, F., Botzler, C. S., Freeman, M., Fukunaga, D., Fukui, A., Itow, Y., Koshimoto, N., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Sumi, T., Sweatman, W. L., Tristram, P. J., Tsurumi, N., Wada, K., Yock, P. C. M., Albrow, M. D., Bachelet, E., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Prester, D. Dominis, Fouque, P., Greenhill, J., Horne, K., Koo, J. -R., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J. W., Sahu, K. C., Wambsganss, J., Williams, A., Choi, M. Zub J. Y., DePoy, D. L., Dong, Subo, Gaudi, B. S., Gould, A., Han, C., Henderson, C. B., McGregor, D., Lee, C. -U., Pogge, R. W., Shin, I. -G., Yee, J. C., Szymaski, M. K., Skowron, J., Poleski, R., Kozowski, S., Wyrzykowski, L., Kubiak, M., Pietrukowicz, P., Pietrzyski, G., Soszyski, I., Ulaczyk, K., Tsapras, Y., Street, R. A., Dominik, M., Bramich, D. M., Browne, P., Hundertmark, M., Kains, N., Snodgrass, C., Steele, I. A., Dekany, I., Gonzalez, O. A., Heyrovsky, D., Kandori, R., Kerins, E., Lucas, P. W., Minniti, D., Nagayama, T., Rejkuba, M., Robin, A. C., and Saito, R.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the first microlensing candidate for a free-floating exoplanet-exomoon system, MOA-2011-BLG-262, with a primary lens mass of M_host ~ 4 Jupiter masses hosting a sub-Earth mass moon. The data are well fit by this exomoon model, but an alternate star+planet model fits the data almost as well. Nevertheless, these results indicate the potential of microlensing to detect exomoons, albeit ones that are different from the giant planet moons in our solar system. The argument for an exomoon hinges on the system being relatively close to the Sun. The data constrain the product M pi_rel, where M is the lens system mass and pi_rel is the lens-source relative parallax. If the lens system is nearby (large pi_rel), then M is small (a few Jupiter masses) and the companion is a sub-Earth-mass exomoon. The best-fit solution has a large lens-source relative proper motion, mu_rel = 19.6 +- 1.6 mas/yr, which would rule out a distant lens system unless the source star has an unusually high proper motion. However, data from the OGLE collaboration nearly rule out a high source proper motion, so the exoplanet+exomoon model is the favored interpretation for the best fit model. However, the alternate solution has a lower proper motion, which is compatible with a distant (so stellar) host. A Bayesian analysis does not favor the exoplanet+exomoon interpretation, so Occam's razor favors a lens system in the bulge with host and companion masses of M_host = 0.12 (+0.19 -0.06) M_solar and m_comp = 18 (+28 -100 M_earth, at a projected separation of a_perp ~ 0.84 AU. The existence of this degeneracy is an unlucky accident, so current microlensing experiments are in principle sensitive to exomoons. In some circumstances, it will be possible to definitively establish the low mass of such lens systems through the microlensing parallax effect. Future experiments will be sensitive to less extreme exomoons., Comment: 32 pages with 9 included figures
Published: 2013
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3. A Super-Jupiter orbiting a late-type star: A refined analysis of microlensing event OGLE-2012-BLG-0406

Author: Tsapras, Y., Choi, J. -Y., Street, R. A., Han, C., Bozza, V., Gould, A., Dominik, M., Beaulieu, J. -P., Udalski, A., Jørgensen, U. G., Sumi, T., Bramich, D. M., Browne, P., Horne, K., Hundertmark, M., Ipatov, S., Kains, N., Snodgrass, C., Steele, I. A., Alsubai, K. A., Andersen, J. M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Elyiv, A., Giannini, E., Hardis, S., Harpsøe, K., Hinse, T. C., Juncher, D., Kerins, E., Korhonen, H., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wambsganss, J., Skowron, J., Poleski, R., Kozłowski, S., Wyrzykowski, Łukasz, Szymański, M. K., Kubiak, M., Pietrukowicz, P., Pietrzyński, G., Soszyński, I., Ulaczyk, K., Albrow, M. D., Bachelet, E., Barry, R., Batista, V., Bhattacharya, A., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Menzies, J., P`ere, C., Pollard, K. R., Wouters, D., Christie, G., DePoy, D. L., Dong, S., Drummond, J., Gaudi, B. S., Henderson, C. B., Hwang, K. H., Jung, Y. K., Kavka, A., Koo, J. -R., Lee, C. -U., Maoz, D., Monard, L. A. G., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Porritt, I., Shin, I. -G., Shvartzvald, Y., Tan, T. G., Yee, J. C., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Fukunaga, D., Itow, Y., Koshimoto, N., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Sweatman, W. L., Suzuki, D., Tristram, P. J., Tsurumi, N., Wada, K., Yamai, N., and Yonehara, P. C. M. Yock A.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present a detailed analysis of survey and follow-up observations of microlensing event OGLE-2012-BLG-0406 based on data obtained from 10 different observatories. Intensive coverage of the lightcurve, especially the perturbation part, allowed us to accurately measure the parallax effect and lens orbital motion. Combining our measurement of the lens parallax with the angular Einstein radius determined from finite-source effects, we estimate the physical parameters of the lens system. We find that the event was caused by a $2.73\pm 0.43\ M_{\rm J}$ planet orbiting a $0.44\pm 0.07\ M_{\odot}$ early M-type star. The distance to the lens is $4.97\pm 0.29$\ kpc and the projected separation between the host star and its planet at the time of the event is $3.45\pm 0.26$ AU. We find that the additional coverage provided by follow-up observations, especially during the planetary perturbation, leads to a more accurate determination of the physical parameters of the lens., Comment: 9 pages, 4 figures, accepted by ApJ
Published: 2013
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4. A Giant Planet beyond the Snow Line in Microlensing Event OGLE-2011-BLG-0251

Author: Kains, N., Street, R., Choi, J. -Y., Han, C., Udalski, A., Almeida, L. A., Jablonski, F., Tristram, P., Jorgensen, U. G., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Grundahl, F., Gu, C. -H., Hardis, S., Harpsoe, K., Hessman, F. V., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Sahu, K. C., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Bajek, D., Bramich, D. M., Horne, K., Ipatov, S., Steele, I. A., Tsapras, Y., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D. J., Sumi, T., Suzuki, D., Suzuki, K., Sweatman, W. L., Takino, S., Wada, K., Yock, P. C. M., Allen, W., Batista, V., Chung, S. -J., Christie, G., DePoy, D. L., Drummond, J., Gaudi, B. S., Gould, A., Henderson, C., Jung, Y. -K., Koo, J. -R., Lee, C. -U., McCormick, J., McGregor, D., Munoz, J. A., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Shin, I. -G., Yee, J., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouque, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Williams, A., Wouters, D., and Zub, M.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the analysis of the gravitational microlensing event OGLE-2011-BLG-0251. This anomalous event was observed by several survey and follow-up collaborations conducting microlensing observations towards the Galactic Bulge. Based on detailed modelling of the observed light curve, we find that the lens is composed of two masses with a mass ratio q=1.9 x 10^-3. Thanks to our detection of higher-order effects on the light curve due to the Earth's orbital motion and the finite size of source, we are able to measure the mass and distance to the lens unambiguously. We find that the lens is made up of a planet of mass 0.53 +- 0.21,M_Jup orbiting an M dwarf host star with a mass of 0.26 +- 0.11 M_Sun. The planetary system is located at a distance of 2.57 +- 0.61 kpc towards the Galactic Centre. The projected separation of the planet from its host star is d=1.408 +- 0.019, in units of the Einstein radius, which corresponds to 2.72 +- 0.75 AU in physical units. We also identified a competitive model with similar planet and host star masses, but with a smaller orbital radius of 1.50 +- 0.50 AU. The planet is therefore located beyond the snow line of its host star, which we estimate to be around 1-1.5 AU., Comment: 12 pages, 7 figures, 3 tables; A&A in press
Published: 2013
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5. MOA-2010-BLG-073L: An M-Dwarf with a Substellar Companion at the Planet/Brown Dwarf Boundary

Author: 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., Bramich, D. M., Bajek, D., Steele, I. A., Ipatov, S., Abe, F., Bennett, D. P., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Harris, P., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Nagayama, T., Nishimaya, S., Ohnishi, K., Rattenbury, N., Saito, To., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Ulaczyk, K., Wyrzykowski, L., Yee, J., Dong, S., Shin, I. -G., Lee, C. -U., Skowron, J., De Almeida, L. Andrade, DePoy, D. L., Gaudi, B. S., Hung, L. -W., Jablonski, F., Kaspi, S., Klein, N., Hwang, K. -H., Koo, J. -R., Maoz, D., Munoz, J. A., Pogge, R. W., Polishhook, D., Shporer, A., McCormick, J., Christie, G., Natusch, T., Allen, B., Drummond, J., Moorhouse, D., Thornley, G., Knowler, M., Bos, M., Bolt, G., Beaulieu, J. -P., Albrow, M. D., Batista, V., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouque, P., Bachelet, E., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., Zub, M., Alsubai, K. A., Bozza, V., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dreizler, S., Finet, F., Gerner, T., Hardis, S., Harpsoe, K., Hessman, F., Hinse, T. C., Jorgensen, U. G., Kerins, E., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schafer, S., Schonebeck, F., Southworth, J., and Surdej, J.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present an analysis of the anomalous microlensing event, MOA-2010-BLG-073, announced by the Microlensing Observations in Astrophysics survey on 2010-03-18. This event was remarkable because the source was previously known to be photometrically variable. Analyzing the pre-event source lightcurve, we demonstrate that it is an irregular variable over time scales >200d. Its dereddened color, $(V-I)_{S,0}$, is 1.221$\pm$0.051mag and from our lens model we derive a source radius of 14.7$\pm$1.3 $R_{\odot}$, 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$\pm$0.0006. The Einstein crossing time of the event, $T_{\rm{E}}=44.3$\pm$0.1d, was sufficiently long that the lightcurve 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$\pm$0.4kpc, and the masses of the lensing objects. The primary of the lens is an M-dwarf with $M_{L,p}$=0.16$\pm0.03M_{\odot}$ while the companion has $M_{L,s}$=11.0$\pm2.0M_{\rm{J}}$ putting it in the boundary zone between planets and brown dwarfs., Comment: 24 pages, 8 figures, best viewed in colour, accepted by ApJ
Published: 2012
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6. The second multiple-planet system discovered by microlensing: OGLE-2012-BLG-0026Lb, c, a pair of jovian planets beyond the snow line

Author: Han, C., Udalski, A., Choi, J. -Y., Yee, J. C., Gould, A., Christie, G., Tan, T. -G., Szymański, M. K., Kubiak, M., Soszyński, I., Pietrzyński, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., Almeida, L. A., Batista, V., Depoy, D. L., Dong, Subo, Drummond, J., Gaudi, B. S., Hwang, K. -H., Jablonski, F., Jung, Y. -K., Lee, C. -U., Koo, J. -R., McCormick, J., Monard, L. A. G., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Porritt, Ian, and Shin, I. -G.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of a planetary system from observation of the high-magnification microlensing event OGLE-2012-BLG-0026. The lensing light curve exhibits a complex central perturbation with multiple features. We find that the perturbation was produced by two planets located near the Einstein ring of the planet host star. We identify 4 possible solutions resulting from the well-known close/wide degeneracy. By measuring both the lens parallax and the Einstein radius, we estimate the physical parameters of the planetary system. According to the best-fit model, the two planet masses are ~0.11 M_Jupiter and 0.68 M_Jupiter and they are orbiting a G-type main sequence star with a mass ~0.82 M_Sun. The projected separations of the individual planets are beyond the snow line in all four solutions, being ~3.8 AU and 4.6 AU in the best-fit solution. The deprojected separations are both individually larger and possibly reversed in order. This is the second multi-planet system with both planets beyond the snow line discovered by microlensing. This is the only such a system (other than the Solar System) with measured planet masses without sin(i) degeneracy. The planetary system is located at a distance 4.1 kpc from the Earth toward the Galactic center. It is very likely that extra light from stars other than the lensed star comes from the lens itself. If this is correct, it will be possible to obtain detailed information about the planet-host star from follow-up observation., Comment: 6 pages, 3 figures, 2 tables
Published: 2012
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7. Microlensig Binaries with Candidate Brown Dwarf Companions

Author: Shin, I. -G., Han, C., Gould, A., Udalski, A., Sumi, T., Dominik, M., Beaulieu, J. -P., Tsapras, Y., Bozza, V., Szymański, M. K., Kubiak, M., Soszyński, I., Pietrzyński, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Furusawa, K., Hayashi, F., Hearnshaw, J. B., Hosaka, S., Itow, Y., Kamiya, K., Kilmartin, P. M., Kobara, S., Korpela, A., Lin, W., Ling, C. H., Makita, S., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Nagaya, M., Nishimoto, K., Ohnishi, K., Okumura, T., Omori, K., Perrott, Y. C., Rattenbury, N., Saito, To., Skuljan, L., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Christie, G. W., Depoy, D. L., Dong, S., Gal-Yam, A., Gaudi, B. S., Hung, L. -W., Janczak, J., Kaspi, S., Maoz, D., McCormick, J., McGregor, D., Moorhouse, D., Muñoz, J. A., Natusch, T., Nelson, C., Pogge, R. W., Tan, T. -G., Polishook, D., Shvartzvald, Y., Shporer, A., Thornley, G., Malamud, U., Yee, J. C., Choi, J. -Y., Jung, Y. -K., Park, H., Lee, C. -U., Park, B. -G., Koo, J. -R., Bajek, D., Bramich, D. M., Browne, P., Horne, K., Ipatov, S., Snodgrass, C., Steele, I., Street, R., Alsubai, K. A., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dreizler, S., Fang, X. -S., Grundahl, F., Gu, C. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Hornstrup, A., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., Zimmer, F., Albrow, M. D., Batista, V., Brillant, S., Caldwell, J. A. R., Calitz, J. J., Cassan, A., Cole, A., Cook, K. H., Corrales, E., Coutures, Ch., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Greenhill, J., Hill, K., Hoffman, M., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., Vinter, C., and Zub, M.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Brown dwarfs are important objects because they may provide a missing link between stars and planets, two populations that have dramatically different formation history. In this paper, we present the candidate binaries with brown dwarf companions that are found by analyzing binary microlensing events discovered during 2004 - 2011 observation seasons. Based on the low mass ratio criterion of q < 0.2, we found 7 candidate events, including OGLE-2004-BLG-035, OGLE-2004-BLG-039, OGLE-2007-BLG-006, OGLE-2007-BLG-399/MOA-2007-BLG-334, MOA-2011-BLG-104/OGLE-2011-BLG-0172, MOA-2011-BLG-149, and MOA-201-BLG-278/OGLE-2011-BLG-012N. Among them, we are able to confirm that the companions of the lenses of MOA-2011-BLG-104/OGLE-2011-BLG-0172 and MOA-2011-BLG-149 are brown dwarfs by determining the mass of the lens based on the simultaneous measurement of the Einstein radius and the lens parallax. The measured mass of the brown dwarf companions are (0.02 +/- 0.01) M_Sun and (0.019 +/- 0.002) M_Sun for MOA-2011-BLG-104/OGLE-2011-BLG-0172 and MOA-2011-BLG-149, respectively, and both companions are orbiting low mass M dwarf host stars. More microlensing brown dwarfs are expected to be detected as the number of lensing events with well covered light curves increases with new generation searches., Comment: 10 pages, 9 figures, 4 tables
Published: 2012
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8. MOA-2010-BLG-477Lb: constraining the mass of a microlensing planet from microlensing parallax, orbital motion and detection of blended light

Author: Bachelet, E., Shin, I. -G., Han, C., Fouqué, P., Gould, A., Menzies, J. W., Beaulieu, J. -P., Bennett, D. P., Bond, I. A., Dong, Subo, Heyrovský, D., Marquette, J. B., Marshall, J., Skowron, J., Street, R. A., Sumi, T., Udalski, A., Abe, L., Agabi, K., Albrow, M. D., Allen, W., Bertin, E., Bos, M., Bramich, D. M., Chavez, J., Christie, G. W., Cole, A. A., Crouzet, N., Dieters, S., Dominik, M., Drummond, J., Greenhill, J., Guillot, T., Henderson, C. B., Hessman, F. V., Horne, K., Hundertmark, M., Johnson, J. A., Jørgensen, U. G., Kandori, R., Liebig, C., Mékarnia, D., McCormick, J., Moorhouse, D., Nagayama, T., Nataf, D., Natusch, T., Nishiyama, S., Rivet, J. -P., Sahu, K. C., Shvartzvald, Y., Thornley, G., Tomczak, A. R., Tsapras, Y., Yee, J. C., Batista, V., Bennett, C. S., Brillant, S., Caldwell, J. A. R., Cassan, A., Corrales, E., Coutures, C., Prester, D. Dominis, Donatowicz, J., Kubas, D., Martin, R., Williams, A., Zub, M., de Almeida, L. Andrade, DePoy, D. L., Gaudi, B. S., Hung, L. -W., Jablonski, F., Kaspi, S., Klein, N., Lee, C. -U., Lee, Y., Koo, J. -R., Maoz, D., Muñoz, J. A., Pogge, R. W., Polishook, D., Shporer, A., Abe, F., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Harris, P., Itow, Y., Kobara, S., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Ohmori, K., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Szymański, M. K., Soszyński, I., Kubiak, M., Poleski, R., Ulaczyk, K., Pietrzyński, G., Wyrzykowski, Ł., Kains, N., Snodgrass, C., Steele, I. A., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dreizler, S., Finet, F., Gerner, T., Hardis, S., Harpsøe, K., Hinse, T. C., Kerins, E., Mancini, L., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schäfer, S., Schönebeck, F., Southworth, J., Surdej, J., and Wambsganss, J.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA-2010-BLG-477. The measured planet-star mass ratio is $q=(2.181\pm0.004)\times 10^{-3}$ and the projected separation is $s=1.1228\pm0.0006$ in units of the Einstein radius. The angular Einstein radius is unusually large $\theta_{\rm E}=1.38\pm 0.11$ mas. Combining this measurement with constraints on the "microlens parallax" and the lens flux, we can only limit the host mass to the range $0.13
Published: 2012
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9. Multi-site, multi-year monitoring of the oscillating Algol-type eclipsing binary CT Her

Author: Lampens, P., Strigachev, A., Kim, S. -L., Rodriguez, E., Lopez-Gonzalez, M. J., Vidal-Sainz, J., Mkrtichian, D., Koo, J. -R., Kang, Y. B., Van Cauteren, P., Wils, P., Kraicheva, Z., Dimitrov, D., Southworth, J., Melendo, E. Garcia, and Forellad, J. M. Gomez
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present the results of a multi-site photometric campaign carried out in 2004-2008 for the Algol-type eclipsing binary system CT Her, the primary component of which shows Delta Scuti-type oscillations. Our data consist of differential light curves collected in the filters B and V which have been analysed using the method of Wilson-Devinney (PHOEBE). After identification of an adequate binary model and removal of the best-matching light curve solution, we performed a Fourier analysis of the residual B and V light curves to investigate the pulsational behaviour. We confirm the presence of rapid pulsations with a main period of 27.2 min. Up to eight significant frequencies with semi-amplitudes in the range 3 to 1 mmag were detected, all of which surprisingly lie in the frequency range 43.5-53.5 c\d. This result is independent from the choice of the primary's effective temperature (8200 or 8700 K) since the light curve models for the binary are very similar in both cases. This is yet another case of a complex frequency spectrum observed for an accreting Delta Scuti-type star (after Y Cam). In addition, we demonstrate that the amplitudes of several of these pulsation frequencies show evidence of variability on time scales as short as 1-2 years, perhaps even less. Moreover, our analysis takes into account some recently acquired spectra, from which we obtained the corresponding radial velocities for the years 2007-2009. Investigation of the O-C diagram shows that further monitoring of the epochs of eclipse minima of CT Her will cast a new light on the evolution of its orbital period., Comment: 13 pages, 13 encapsulated Postscript figures. Tables~3, 4, 9 and 12 will be available in electronic form only. Astronomy and Astrophysics, in process (2011). Replaced the abstract with its final version
Published: 2011
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10. A sub-Saturn Mass Planet, MOA-2009-BLG-319Lb

Author: 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., Fouque, P., Browne, P., Han, C., Snodgrass, C., Finet, F., Furusawa, K., Harpsoe, K., Allen, W., Hundertmark, M., Freeman, M., Suzuki, D., Abe, F., Botzler, C. S., Douchin, D., Fukui, A., Hayashi, F., Hearnshaw, J. B., Hosaka, S., Itow, Y., Kamiya, K., Kilmartin, P. M., Korpela, A., Lin, W., Ling, C. H., Makita, S., Masuda, K., Matsubara, Y., Muraki, Y., Nagayama, T., Nishimoto, K., Ohnishi, K., Perrott, Y. C., Rattenbury, N., Saito, To., Skuljan, L., Sullivan, D. J., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Collaboration, The MOA, Bolt, G., Bos, M., Christie, G. W., DePoy, D. L., Drummond, J., Gal-Yam, A., Gaudi, B. S., Gorbikov, E., Higgins, D., Janczak, K. -H. Hwang J., Kaspi, S., Lee, C. -U., Koo, J. -R., lowski, S. Koz, Lee, Y., Mallia, F., Maury, A., Maoz, D., McCormick, J., Monard, L. A. G., Moorhouse, D., Mu~noz, J. A., Natusch, T., Ofek, E. O., Pogge, R. W., Polishook, D., Santallo, R., Shporer, A., Spector, O., Thornley, G., Collaboration, The Micro FUN, Allan, A., Bramich, D. M., Horne, K., Kains, N., Steele, I., Collaboration, The RoboNet, Bozza, V., Burgdorf, M. J., Novati, S. Calchi, Dominik, M., Dreizler, S., Glitrup, M., Hessman, F. V., Hinse, T. C., Jorgensen, U. G., Liebig, C., Maier, G., Mathiasen, M., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Wambsganss, J., Zimmer, F., Consortium, The MiNDSTEp, Batista, V., Beaulieu, J. P., Brillant, S., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Greenhill, J., Kubas, D., Menzies, J., and Collaboration, The PLANET
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: 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 hours 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^{+0.34}_{-0.18} M_{Sun} and a planet mass of M_p = 50^{+44}_{-24} M_{Earth}, which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4^{+1.2}_{-0.6} AU and a distance to the planetary system of D_L = 6.1^{+1.1}_{-1.2} kpc. This separation is ~ 2 times the distance of the snow line, a separation similar to most of the other planets discovered by microlensing., Comment: accepted to ApJ, 28 pages, 6 figures, 3 tables
Published: 2010
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11. RACE-OC Project: Rotation and variability in the open cluster M11 (NGC6705)

Author: Messina, S., Parihar, P., Koo, J. -R., Kim, S. -L., Rey, S. -C., and Lee, C. -U.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Rotation and magnetic activity are intimately linked in main-sequence stars of G or later spectral types. The presence and level of magnetic activity depend on stellar rotation, and rotation itself is strongly influenced by strength and topology of the magnetic fields. Open clusters represent especially useful targets to investigate the rotation/activity/age connection. The open cluster M11 has been studied as a part of the RACE-OC project (Rotation and ACtivity Evolution in Open Clusters), which is aimed at exploring the evolution of rotation and magnetic activity in the late-type members of open clusters with different ages. Photometric observations of the open cluster M11 were carried out in June 2004 using LOAO 1m telescope. The rotation periods of the cluster members are determined by Fourier analysis of photometric data time series. We further investigated the relations between the surface activity, characterized by the light curve amplitude, and rotation. We have discovered a total of 75 periodic variables in the M11 FoV, of which 38 are candidate cluster members. Specifically, among cluster members we discovered 6 early-type, 2 eclipsing binaries and 30 bona-fide single periodic late-type variables. Considering the rotation periods of 16 G-type members of the almost coeval 200-Myr M34 cluster, we could determine the rotation period distribution from a more numerous sample of 46 single G stars at an age of about 200-230 Myr and determine a median rotation period P=4.8d. A comparison with the younger M35 cluster (~150 Myr) and with the older M37 cluster (~550 Myr) shows that G stars rotate slower than younger M35 stars and faster than older M37 stars. The measured variation of the median rotation period is consistent with the scenario of rotational braking of main-sequence spotted stars as they age., Comment: Accepted by Astronomy and Astrophysics on Dec 15, 2009
Published: 2009
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12. Variable stars in the Open Cluster M11 (NGC 6705)

Author: Koo, J. -R., Kim, S. -L., Rey, S. -C., Lee, C. -U., Kim, Y. H., Kang, Y. B., and Jeon, Y. -B.
Subjects: Astrophysics
Abstract: V-band time-series CCD photometric observations of the intermediate-age open cluster M11 were performed to search for variable stars. Using these time-series data, we carefully examined light variations of all stars in the observing field. A total of 82 variable stars were discovered, of which 39 stars had been detected recently by Hargis et al. (2005). On the basis of observational properties such as variable period, light curve shape, and position on a color-magnitude diagram, we classified their variable types as 11 delta Scuti-type pulsating stars, 2 gamma Doradus-type pulsating stars, 40 W UMa-type contact eclipsing binaries, 13 Algol-type detached eclipsing binaries, and 16 eclipsing binaries with long period. Cluster membership for each variable star was deduced from the previous proper motion results (McNamara et al. 1977) and position on the color-magnitude diagram. Many pulsating stars and eclipsing binaries in the region of M11 are probable members of the cluster., Comment: 23 pages, 9 figures, 3 tables, and accepted for publication in PASP
Published: 2007
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13. Multisite campaign on the open cluster M67. III. Delta Scuti pulsations in the blue stragglers

Author: Bruntt, H., Stello, D., Suarez, J. C., Arentoft, T., Bedding, T. R., Bouzid, M. Y., Csubry, Z., Dall, T. H., Dind, Z. E., Frandsen, S., Gilliland, R. L., Jacob, A. P., Jensen, H. R., Kang, Y. B., Kim, S. -L., Kiss, L. L., Kjeldsen, H., Koo, J. -R., Lee, J. -A., Lee, C. -U., Nuspl, J., Sterken, C., and Szabo, R.
Subjects: Astrophysics
Abstract: We have made an asteroseismic analysis of the variable blue stragglers in the open cluster M67. The data set consists of photometric time series from eight sites using nine 0.6-2.1 meter telescopes with a time baseline of 43 days. In two stars, EW Cnc and EX Cnc, we detect the highest number of frequencies (41 and 26) detected in delta Scuti stars belonging to a stellar cluster, and EW Cnc has the second highest number of frequencies detected in any delta Scuti star. We have computed a grid of pulsation models that take the effects of rotation into account. The distribution of observed and theoretical frequencies show that in a wide frequency range a significant fraction of the radial and non-radial low-degree modes are excited to detectable amplitudes. Despite the large number of observed frequencies we cannot constrain the fundamental parameters of the stars. To make progress we need to identify the degrees of some of the modes either from multi-colour photometry or spectroscopy., Comment: 15 pages, 14 figs, one appendix. Part three in a series of papers describing results from an extensive multi-site campaign on the open cluster M67
Published: 2007
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14. Variable Stars in the Open Cluster NGC 2099 (M37)

Author: Kang, Y. B., Kim, S. -L., Rey, S. -C., Lee, C. -U., Kim, Y. H., Koo, J. -R., and Jeon, Y. -B.
Subjects: Astrophysics
Abstract: Time-series CCD photometric observations of the intermediate-age open cluster NGC 2099 were performed to search for variable stars. We also carried out BV photometry to study physical properties of variables in the cluster. Using V-band time-series data, we carefully examined light variations of about 12,000 stars in the range of 10 < V < 22 mag. A total of 24 variable stars have been identified; seven stars are previously known variables and 17 stars are newly identified. On the basis of observational properties such as light curve shape, period, and amplitude, we classified the new variable stars as nine delta Scuti-type pulsating stars, seven eclipsing binaries, and one peculiar variable star. Judging from the position of delta Scuti-type stars in the color-magnitude diagram, only two stars are likely to have the cluster membership. One new variable KV10 shows peculiar light variations with a delta Scuti-type short period of about 0.044 day as well as a long period of 0.417 day., Comment: 26 pages, 9 figures, 4 tables, accepted for publication in PASP
Published: 2007
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15. Solar-like oscillations in open cluster stars

Author: Stello, D., Bruntt, H., Arentoft, T., Gilliland, R. L., Nuspl, J., Kim, S. -L., Kang, Y. B., Koo, J. -R., Lee, J. -A., Lee, C. -U., Sterken, C., Jacob, A. P., Frandsen, S., Dind, Z. E., Jensen, H. R., Szabo, R., Csubry, Z., Kiss, L. L., Bouzid, M. Y., Dall, T. H., Bedding, T. R., and Kjeldsen, H.
Subjects: Astrophysics
Abstract: Asteroseismology of stellar clusters is potentially a powerful tool. The assumption of a common age, distance, and chemical composition provides constraints on each cluster member, which significantly improves the asteroseismic output. Driven by this great potential, we carried out multi-site observations aimed at detecting solar-like oscillations in the red giant stars in the open cluster M67 (NGC 2682) (Stello et al. 2006). Here we present the first analysis of our data, which show evidence of excess power in the Fourier spectra, shifting to lower frequencies for more luminous stars, consistent with expectations from oscillations. If the observed power excesses were due to stellar oscillations, this result would show great prospects for asteroseismology in stellar clusters., Comment: 2 pages, 2 figures. Accepted for publication in CoAst
Published: 2007
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16. Multisite campaign on the open cluster M67. II. Evidence for solar-like oscillations in red giant stars

Author: Stello, D., Bruntt, H., Kjeldsen, H., Bedding, T. R., Arentoft, T., Gilliland, R. L., Nuspl, J., Kim, S. -L., Kang, Y. B., Koo, J. -R., Lee, J. -A., Sterken, C., Lee, C. -U., Jensen, H. R., Jacob, A. P., Szabo, R., Frandsen, S., Csubry, Z., Dind, Z. E., Bouzid, M. Y., Dall, T. H., and Kiss, L. L.
Subjects: Astrophysics
Abstract: Measuring solar-like oscillations in an ensemble of stars in a cluster, holds promise for testing stellar structure and evolution more stringently than just fitting parameters to single field stars. The most ambitious attempt to pursue these prospects was by Gilliland et al. (1993) who targeted 11 turn-off stars in the open cluster M67 (NGC 2682), but the oscillation amplitudes were too small (<20micromag) to obtain unambiguous detections. Like Gilliland et al. (1993) we also aim at detecting solar-like oscillations in M67, but we target red giant stars with expected amplitudes in the range 50-500micromag and periods of 1 to 8 hours. We analyse our recently published photometry measurements, obtained during a six-week multisite campaign using nine telescopes around the world. The observations are compared with simulations and with estimated properties of the stellar oscillations. Noise levels in the Fourier spectra as low as 27micromag are obtained for single sites, while the combined data reach 19micromag, making this the best photometric time series of an ensemble of red giant stars. These data enable us to make the first test of the scaling relations (used to estimate frequency and amplitude) with an homogeneous ensemble of stars. The detected excess power is consistent with the expected signal from stellar oscillations, both in terms of its frequency range and amplitude. However, our results are limited by apparent high levels of non-white noise, which cannot be clearly separated from the stellar signal., Comment: 12 pages, 10 figures. Accepted for publication in MNRAS
Published: 2007
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17. Multi-site campaign on the open cluster M67. I. Observations and photometric reductions

Author: Stello, D., Arentoft, T., Bedding, T. R., Bouzid, M. Y., Bruntt, H., Csubry, Z., Dind, Z. E., Frandsen, S., Gilliland, R. L., Jacob, A. P., Jensen, H. R., Kang, Y. B., Kim, S. -L., Kiss, L. L., Kjeldsen, H., Koo, J. -R., Lee, J. -A., Lee, C. -U., Nuspl, J., Sterken, C., and Szabo, R.
Subjects: Astrophysics
Abstract: We report on an ambitious multi-site campaign aimed at detecting stellar variability, particularly solar-like oscillations, in the red giant stars in the open cluster M67 (NGC 2682). During the six-week observing run, which comprised 164 telescope nights, we used nine 0.6-m to 2.1-m class telescopes located around the world to obtain uninterrupted time-series photometry. We outline here the data acquisition and reduction, with emphasis on the optimisation of the signal-to-noise of the low amplitude (50-500 micromag) solar-like oscillations. This includes a new and efficient method for obtaining the linearity profile of the CCD response at ultra high precision (~10 parts per million). The noise in the final time series is 0.50 mmag per minute integration for the best site, while the noise in the Fourier spectrum of all sites combined is 20 micromag. In addition to the red giant stars, this data set proves to be very valuable for studying high-amplitude variable stars such as eclipsing binaries, W UMa systems and delta Scuti stars., Comment: 12 pages, 13 figures, accepted by MNRAS
Published: 2006
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18. “Variable Stars in the Open Cluster NGC 2099 (M37)” ( PASP, 119, 239, [2007] )

Author: Kang, Y. B., Kim, S. -L., Rey, S. -C., Lee, C. U., Kim, Y. H., Koo, J. -R., and Jeon, Y. -B.
Published: 2008
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19. A Super-Jupiter Orbiting A Late-Type Star: A Refined Analysis of Microlensing Event OGLE-2012-BLG-0406

Author: Tsapras, Y, Choi, J.-Y, Street, R. A, Han, C, Bozza, V, Gould, A, Dominik, M, Beaulieu, J.-P, Udalski, A, Jørgensen, U. G, Sumi, T, Bramich, D. M, Browne, P, Horne, K, Hundertmark, M, Kains, N, Snodgrass, C, Steele, I. A, Andersen, J. M, Novati, S. Calchi, Diehl, C, Giannini, E, Hardis, S, Harpsøe, K, Hinse, T. C, Juncher, D, Kerins, E, Korhonen, H, Liebig, C, Mancini, L, Mathiasen, M, Penny, M. T, Rabus, M, Rahvar, S, Scarpetta, G, Skottfelt, J, Southworth, J, Tregloan-Reed, J, Vilela, C, Wambsganss, J, Skowron, J, Poleski, R, Kozłowski, S, Wyrzykowski, Ł, Szymański, M. K, Kubiak, M, Pietrukowicz, P, Pietrzyński, G, Soszyński, I, Ulaczyk, K, Albrow, M. D, Bachelet, E, Barry, R, Batista, V, Bhattacharya, A, Brillant, S, Caldwell, J. A. R, Cassan, A, Cole, A, Corrales, E, Coutures, Ch, Dieters, S, Prester, D. Dominis, Donatowicz, J, Fouqu, P, Greenhill, J, Kane, S. R, Kubas, D, Marquette, J. B, Menzies, J, Père, C, Pollard, K. R, Zub, M, Christie, G, DePoy, D. L, Dong, S, Gaudi, B. S, Henderson, C. B, Hwang, K. H, Jung, Y. K, Kavka, A, Koo, J.-R, Lee, C.-U, Maoz, D, Natusch, T, Ngan, H, Park, H, Pogge, R. W, Shin, I. G, Shvartzvald, Y, Yee, J. C, Abe, F, Bennett, D. P, Bond, I. A, Botzler, C. S, Freeman, M, Fukui, A, Fukunaga, D, Itow, Y, Koshimoto, N, Ling, C. H, Masuda, K, Matsubara, Y, Muraki, Y, Namba, S, Ohnishi, K, Rattenbury, N. J, Saito, To, Sullivan, D. J, Sweatman, W. L, Suzuki, D, Tristram, P. J, Tsurumi, N, Wada, K, Yamai, N, Yock, P. C. M, and Yonehara, A
Subjects: Astronomy, Astrophysics
Abstract: We present a detailed analysis of survey and follow-up observations of microlensing event OGLE-2012-BLG-0406 based on data obtained from 10 different observatories. Intensive coverage of the light curve, especially the perturbation part, allowed us to accurately measure the parallax effect and lens orbital motion. Combining our measurement of the lens parallax with the angular Einstein radius determined from finite-source effects, we estimate the physical parameters of the lens system. We find that the event was caused by a 2.73 plus or minus 0.43 M (sub J) planet orbiting a 0.44 plus or minus 0.07 solar mass early M-type star. The distance to the lens is 4.97 plus or minus 0.29 kpc and the projected separation between the host star and its planet at the time of the event is 3.45 plus or minus 0.26 AU. We find that the additional coverage provided by follow-up observations, especially during the planetary perturbation, leads to a more accurate determination of the physical parameters of the lens.
Published: 2014
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20. Prevalence and prognosis of hypoglycaemia in patients receiving maintenance dialysis

Author: Cho, A., primary, Noh, J.-W., additional, Kim, J. K., additional, Yoon, J.-W., additional, Koo, J.-R., additional, Lee, H. R., additional, Hong, E.-G., additional, and Lee, Y. K., additional
Published: 2016
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21. MOA-2011-BLG-262Lb: A Sub-Earth-Mass Moon Orbiting a Gas Giant Primary or a High Velocity Planetary System in the Galactic Bulge

Author: Bennett, D.P., Batista, V., Bond, I.A., Bennett, C.S., Suzuki, D., Beaulieu, J.-P., Udalski, A., Donatowicz, J., Bozza, V., Abe, F., Botzler, C.S., Freeman, M., Fukunaga, D., Fukui, A., Itow, Y., Koshimoto, N., Ling, C.H., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Rattenbury, N.J., Saito, T., Sullivan, D.J., Sumi, T., Sweatman, W.L., Tristram, P.J., Tsurumi, N., Wada, K., Yock, P.C.M., Albrow, M.D., Bachelet, E., Brillant, S., Caldwell, J.A.R., Cassan, A., Cole, A.A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Fouqué, P., Greenhill, J., Horne, K., Koo, J.-R., Kubas, D., Marquette, J.-B., Martin, R., Menzies, J.W., Sahu, K.C., Wambsganss, J., Williams, A., Zub, M., Choi, J.Y., Depoy, D.L., Dong, S., Gaudi, B.S., Gould, A., Han, C., Henderson, C.B., McGregor, D., Lee, C.-U., Pogge, R.W., Shin, I.-G., Yee, J.C., Szymański, M.K., Skowron, J., Poleski, R., Kozłowski, S., Wyrzykowski, Ł., Kubiak, M., Pietrukowicz, P., Pietrzyński, G., Soszyński, I., Ulaczyk, K., Tsapras, Y., Street, R.A., Dominik, M., Bramich, D.M., Browne, P., Hundertmark, M., Kains, N., Snodgrass, C., Steele, I.A., Dekany, I., Gonzalez, O.A., Heyrovský, D., Kandori, R., Kerins, E., Lucas, P.W., Minniti, D., Nagayama, T., Rejkuba, M., Robin, A.C., Saito, A.R., The Royal Society, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, Ohio State University [Columbus] (OSU), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astronomical Observatory [Warsaw], Faculty of Physics [Warsaw] (FUW), University of Warsaw (UW)-University of Warsaw (UW), Okayama Astrophysical Observatory, National Astronomical Observatory of Japan (NAOJ), Nagoya University, Osaka University [Osaka], Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Proper motion, 010504 meteorology & atmospheric sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, 7. Clean energy, 01 natural sciences, micro [Gravitational lensing], Jupiter, Planet, 0103 physical sciences, QB Astronomy, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, QC, Astrophysics::Galaxy Astrophysics, QB, 0105 earth and related environmental sciences, Physics, Exomoon, Giant planet, Astronomy, Astronomy and Astrophysics, Planetary system, Exoplanet, Planetary systems, QC Physics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], BDC
Abstract: D.P.B. was supported by grants NASA-NNX12AF54G, JPL-RSA 1453175 and NSF AST-1211875. This MOA project is supported by the grants JSPS18253002 and JSPS20340052. T.S. acknowledges the financial support from the JSPS, JSPS23340044, JSPS24253004. This work was partially supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. B.S.G. and A.G. were supported by NSF grant AST 110347. B.S.G., A.G., R.P.G. were supported by NASA grant NNX12AB99G. S.D. was partly supported through a Ralph E. and Doris M. Hansmann Membership at the IAS and by NSF grant AST-0807444. Work by J.C.Y. was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 246678 to A.U. D.H. was supported by Czech Science Foundation grant GACR P209/10/1318. D.M.B., M.D., K.H., C.S., R.A.S., M.H. and Y.T. are supported by NPRP grant NPRP-09-476-1-78 from the Qatar National Research Fund (a member of the Qatar Foundation). We present the first microlensing candidate for a free-floating exoplanet-exomoon system, MOA-2011-BLG-262, with a primary lens mass of M host ~ 4 Jupiter masses hosting a sub-Earth mass moon. The argument for an exomoon hinges on the system being relatively close to the Sun. The data constrain the product MLπrel where ML is the lens system mass and πrel is the lens-source relative parallax. If the lens system is nearby (large πrel), then ML is small (a few Jupiter masses) and the companion is a sub-Earth-mass exomoon. The best-fit solution has a large lens-source relative proper motion, μrel = 19.6 ± 1.6 mas yr–1, which would rule out a distant lens system unless the source star has an unusually high proper motion. However, data from the OGLE collaboration nearly rule out a high source proper motion, so the exoplanet+exomoon model is the favored interpretation for the best fit model. However, there is an alternate solution that has a lower proper motion and fits the data almost as well. This solution is compatible with a distant (so stellar) host. A Bayesian analysis does not favor the exoplanet+exomoon interpretation, so Occam's razor favors a lens system in the bulge with host and companion masses of M host = 0.12 +0.19-0.06 MΘ and mcomp = 18+28-10M⊕, at a projected separation of a⊥ = 0.84+0.25−0.14 AU. The existence of this degeneracy is an unlucky accident, so current microlensing experiments are in principle sensitive to exomoons. In some circumstances, it will be possible to definitively establish the mass of such lens systems through the microlensing parallax effect. Future experiments will be sensitive to less extreme exomoons. Publisher PDF
Published: 2014

22. The Second Multiple-planet System Discovered by Microlensing: OGLE-2012-BLG-0026Lb, c\u2014A Pair of Jovian Planets beyond the Snow Line

Author: Han, C, Udalski, A, Choi, J.-Y, Yee, J. C, Gould, A, Christie, G, Tan, T.-G, Szymański, M. K, Kubiak, M, Soszyński, I, Pietrzyński, G, Poleski, R, Ulaczyk, K, Pietrukowicz, P, Kozłowski, S, Skowron, J, Wyrzykowski, Ł, The OGLE Collaboration, Almeida, L. A, Batista, V, Depoy, D. L, Dong, Subo, Drummond, J, Gaudi, B. S, Hwang, K.-H, Jablonski, F, Jung, Y.-K, Lee, C.-U, Koo, J.-R, McCormick, J, Monard, L. A. G, Natusch, T, Ngan, H, Park, H, Pogge, R. W, and Porritt, Ian, Shin, I.
Published: 2013

23. Microlensing Binaries with Candidate Brown Dwarf Companions

Author: Shin, I.-G., Han, C., Gould, A., Udalski, A., Sumi, T., Dominik, M., Beaulieu, J.-P., Tsapras, Y., Bozza, V., Szymański, M. K., Kubiak, M., Soszyński, I., Pietrzyński, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., The OGLE Collaboration, Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Furusawa, K., Hayashi, F., Hearnshaw, J. B., Hosaka, S., Itow, Y., Kamiya, K., Kilmartin, P. M., Kobara, S., Korpela, A., Lin, W., Ling, C. H., Makita, S., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Nagaya, M., Nishimoto, K., Ohnishi, K., Okumura, T., Omori, K., Perrott, Y. C., Rattenbury, N., Saito, To., Skuljan, L., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., The MOA Collaboration, Christie, G. W., Depoy, D. L., Dong, S., Gal-Yam, A., Gaudi, B. S., Hung, L.-W., Janczak, J., Kaspi, S., Maoz, D., McCormick, J., McGregor, D., Moorhouse, D., Muñoz, J. A., Natusch, T., Nelson, C., Pogge, R. W., Tan, T.-G., Polishook, D., Shvartzvald, Y., Shporer, A., Thornley, G., Malamud, U., Yee, J. C., Choi, J.-Y., Jung, Y.-K., Park, H., Lee, C.-U., Park, B.-G., Koo, J.-R., The μFUN Collaboration, Bajek, D., Bramich, D. M., Browne, P., Horne, K., Ipatov, S., Snodgrass, C., Steele, I., Street, R., Alsubai, K. A., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dreizler, S., Fang, X.-S., Grundahl, F., Gu, C.-H., Hardis, S., Harpsøe, Kennet Bomann West, Hinse, T. C., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, Mikkel Nørup, Lundkvist, M., Mancini, L., Mathiasen, M., Hornstrup, A., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, Jesper Fælling, Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., Zimmer, F., Albrow, M. D., Batista, V., Brillant, S., Caldwell, J. A. R., Calitz, J. J., Cassan, A., Cole, A., Cook, K. H., Corrales, E., Coutures, Ch., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouqué, P., Greenhill, J., Hill, K., Hoffman, M., Kane, S. R., Kubas, D., Marquette, J.-B., Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., Vinter, Christian, and Zub, M.
Subjects: Physics, 010308 nuclear & particles physics, Brown dwarf, FOS: Physical sciences, Astronomy and Astrophysics, gravitational lensing: micro, Astrophysics, Light curve, Gravitational microlensing, 01 natural sciences, Einstein radius, Stars, binaries: general, Settore FIS/05 - Astronomia e Astrofisica, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, brown dwarfs, Parallax, Low Mass, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Brown dwarfs are important objects because they may provide a missing link between stars and planets, two populations that have dramatically different formation history. In this paper, we present the candidate binaries with brown dwarf companions that are found by analyzing binary microlensing events discovered during 2004 - 2011 observation seasons. Based on the low mass ratio criterion of q < 0.2, we found 7 candidate events, including OGLE-2004-BLG-035, OGLE-2004-BLG-039, OGLE-2007-BLG-006, OGLE-2007-BLG-399/MOA-2007-BLG-334, MOA-2011-BLG-104/OGLE-2011-BLG-0172, MOA-2011-BLG-149, and MOA-201-BLG-278/OGLE-2011-BLG-012N. Among them, we are able to confirm that the companions of the lenses of MOA-2011-BLG-104/OGLE-2011-BLG-0172 and MOA-2011-BLG-149 are brown dwarfs by determining the mass of the lens based on the simultaneous measurement of the Einstein radius and the lens parallax. The measured mass of the brown dwarf companions are (0.02 +/- 0.01) M_Sun and (0.019 +/- 0.002) M_Sun for MOA-2011-BLG-104/OGLE-2011-BLG-0172 and MOA-2011-BLG-149, respectively, and both companions are orbiting low mass M dwarf host stars. More microlensing brown dwarfs are expected to be detected as the number of lensing events with well covered light curves increases with new generation searches., 10 pages, 9 figures, 4 tables
Published: 2012

24. A sub-Saturn mass planet, MOA-2009-BLG-319Lb

Author: 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., Fouque, P., Browne, P., Han, C., Snodgrass, C., Finet, F., Furusawa, K., Harpsoe, K., Allen, W., Hundertmark, M., Freeman, M., Suzuki, D., Abe, F., Botzler, C. S., Douchin, D., Fukui, A., Hayashi, F., Hearnshaw, J. B., Hosaka, S., Itow, Y., Kamiya, K., Kilmartin, P. M., Korpela, A., Lin, W., Ling, C. H., Makita, S., Masuda, K., Matsubara, Y., Muraki, Y., Nagayama, T., Nishimoto, K., Ohnishi, K., Perrott, Y. C., Rattenbury, N., Saito, To., Skuljan, L., Sullivan, D. J., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Collaboration, The MOA, Bolt, G., Bos, M., Christie, G. W., DePoy, D. L., Drummond, J., Gal-Yam, A., Gaudi, B. S., Gorbikov, E., Higgins, D., Janczak, K. -H. Hwang J., Kaspi, S., Lee, C. -U., Koo, J. -R., lowski, S. Koz, Lee, Y., Mallia, F., Maury, A., Maoz, D., McCormick, J., Monard, L. A. G., Moorhouse, D., Mu~noz, J. A., Natusch, T., Ofek, E. O., Pogge, R. W., Polishook, D., Santallo, R., Shporer, A., Spector, O., Thornley, G., Collaboration, The Micro FUN, Allan, A., Bramich, D. M., Horne, K., Kains, N., Steele, I., Collaboration, The RoboNet, Bozza, V., Burgdorf, M. J., Novati, S. Calchi, Dominik, M., Dreizler, S., Glitrup, M., Hessman, F. V., Hinse, T. C., Jorgensen, U. G., Liebig, C., Maier, G., Mathiasen, M., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Wambsganss, J., Zimmer, F., Consortium, The MiNDSTEp, Batista, V., Beaulieu, J. P., Brillant, S., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Greenhill, J., Kubas, D., Menzies, J., and Collaboration, The PLANET
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Planetary system, Mass ratio, Gravitational microlensing, Light curve, 01 natural sciences, Einstein radius, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, Planet, Saturn, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Planetary mass, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: 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 hours 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^{+0.34}_{-0.18} M_{Sun} and a planet mass of M_p = 50^{+44}_{-24} M_{Earth}, which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4^{+1.2}_{-0.6} AU and a distance to the planetary system of D_L = 6.1^{+1.1}_{-1.2} kpc. This separation is ~ 2 times the distance of the snow line, a separation similar to most of the other planets discovered by microlensing., Comment: accepted to ApJ, 28 pages, 6 figures, 3 tables
Published: 2011

25. A SUPER-JUPITER ORBITING A LATE-TYPE STAR:A REFINED ANALYSIS OF MICROLENSING EVENT OGLE-2012-BLG-0406

Author: Tsapras, Y., Choi, J. -Y., Street, R. A., Han, C., Bozza, V., Gould, A., Dominik, M., Beaulieu, J. -P., Udalski, A., Jorgensen, U. G., Sumi, T., Bramich, D. M., Browne, P., Horne, K., Hundertmark, Markus Peter Gerhard, Ipatov, S., Kains, N., Snodgrass, C., Steele, I. A., Alsubai, K. A., Andersen, J. M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Elyiv, A., Giannini, E., Hardis, S., Harpsøe, Kennet Bomann West, Hinse, T. C., Juncher, D., Kerins, E., Korhonen, H., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wambsganss, J., Skowron, J., Poleski, R., Kozllowski, S., Wyrzykowski, E., Szymanski, M. K., Kubiak, M., Pietrukowicz, P., Pietrzynski, G., Soszynski, I., Ulaczyk, K., Albrow, M. D., Bachelet, E., Barry, R., Batista, V., Bhattacharya, A., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouque, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Menzies, J., Ere, C. P., Pollard, K. R., Zub, M., Christie, G., Depoy, D. L., Dong, S., Drummond, J., Gaudi, B. S., Henderson, C. B., Hwang, K. H., Jung, Y. K., Kavka, A., Koo, J. -R., Lee, C. -U., Maoz, D., Monard, L. A. G., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Porritt, I., Shin, I. -G., Shvartzvald, Y., Tan, T. G., Yee, J. C., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Fukunaga, D., Itow, Y., Koshimoto, N., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Sweatman, W. L., Suzuki, D., Tristram, P. J., Tsurumi, N., Wada, K., Yamai, N., Yock, P. C. M., Yonehara, A., Tsapras, Y., Choi, J. -Y., Street, R. A., Han, C., Bozza, V., Gould, A., Dominik, M., Beaulieu, J. -P., Udalski, A., Jorgensen, U. G., Sumi, T., Bramich, D. M., Browne, P., Horne, K., Hundertmark, Markus Peter Gerhard, Ipatov, S., Kains, N., Snodgrass, C., Steele, I. A., Alsubai, K. A., Andersen, J. M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Elyiv, A., Giannini, E., Hardis, S., Harpsøe, Kennet Bomann West, Hinse, T. C., Juncher, D., Kerins, E., Korhonen, H., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wambsganss, J., Skowron, J., Poleski, R., Kozllowski, S., Wyrzykowski, E., Szymanski, M. K., Kubiak, M., Pietrukowicz, P., Pietrzynski, G., Soszynski, I., Ulaczyk, K., Albrow, M. D., Bachelet, E., Barry, R., Batista, V., Bhattacharya, A., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouque, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Menzies, J., Ere, C. P., Pollard, K. R., Zub, M., Christie, G., Depoy, D. L., Dong, S., Drummond, J., Gaudi, B. S., Henderson, C. B., Hwang, K. H., Jung, Y. K., Kavka, A., Koo, J. -R., Lee, C. -U., Maoz, D., Monard, L. A. G., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Porritt, I., Shin, I. -G., Shvartzvald, Y., Tan, T. G., Yee, J. C., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Fukunaga, D., Itow, Y., Koshimoto, N., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Sweatman, W. L., Suzuki, D., Tristram, P. J., Tsurumi, N., Wada, K., Yamai, N., Yock, P. C. M., and Yonehara, A.
Published: 2014

26. Solar-like oscillations in open cluster stars

Author: Stello, Dennis, Bruntt, Hans, Arentoft, Torben, Gilliland, R.L., Nuspl, J., Kim, S.-L., Kang, Y.B., Koo, J.-R., Lee, J.-A., Lee, C.-U., Sterken, C., Jacob, A.P., Frandsen, Søren, Dind, Z.E., Jensen, H.R., Szabó, R., Csubry, Z., Kiss, L.L., Bouzid, M.Y., Dall, T.H., Bedding, T.R., Kjeldsen, Hans, Handler, 6., and Houdek, G.
Published: 2007

27. Multisite campaign on the open cluster M67: III. δ Scuti pulsations in the blue stragglers

Author: Bruntt, Hans, Stello, Dennis, Surez, J.C., Arentoft, Torben, Bedding, T.R., Bouzid, M.Y., Csubry, Z., Dall, T.H., Dind, Z.E., Frandsen, Søren, Gilliland, R.L., Jacob, A.P., Jensen, H.R., Kang, Y.B., Kim, S.-L., Kiss, L.L., Kjeldsen, Hans, Koo, J.-R., Lee, J.-A., Lee, C.-U., Nuspl, J., Sterken, C., and Szabo, R.
Published: 2007

28. Effect of an Organic Buffer Layer on the Stability of Zinc Oxide Thin-Film Transistors

Author: Lee, H. W., primary, Hyung, G. W., additional, Koo, J. R., additional, Cho, E. S., additional, Kwon, S. J., additional, Park, J. H., additional, and Kim, Y. K., additional
Published: 2014
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29. DIALYSIS CARDIOVASCULAR COMPLICATIONS 1

Author: Wheeler, D. C., primary, Abdalla, S., additional, Chertow, G., additional, Parfrey, P., additional, Herzog, C., additional, Mikolasevic, I., additional, Racki, S., additional, Lukenda, V., additional, Milic, S., additional, Devcic, B., additional, Orlic, L., additional, Suttorp, M. M., additional, Hoekstra, T., additional, Ocak, G., additional, Van Diepen, A. T. N., additional, Ott, I., additional, Mittelman, M., additional, Rabelink, T. J., additional, Krediet, R. T., additional, Dekker, F. W., additional, Simone, S., additional, Dell'Oglio, M. P. S., additional, Ciccone, M., additional, Corciulo, R., additional, Castellano, G., additional, Balestra, C., additional, Grandaliano, G., additional, Gesualdo, L., additional, Pertosa, G., additional, Nishida, M., additional, Ando, M., additional, Karasawa, K., additional, Iwamoto, Y., additional, Tsuchiya, K., additional, Nitta, K., additional, Krzanowski, M., additional, Janda, K., additional, Gajda, M., additional, Dumnicka, P., additional, Fedak, D., additional, Lis, G., additional, Ja kowski, P., additional, Litwin, J. A., additional, Su owicz, W., additional, Freitas, G. R., additional, Silva, V. B., additional, Abensur, H., additional, Luders, C., additional, Pereira, B. J., additional, Castro, M. C., additional, Oliverira, R. B., additional, Moyses, R. M., additional, Elias, R. M., additional, Silva, B. C., additional, Tekce, H., additional, Ozturk, S., additional, Aktas, G., additional, Kin Tekce, B., additional, Erdem, A., additional, Ozyasar, M., additional, Taslamacioglu Duman, T., additional, Yazici, M., additional, Kirkpantur, A., additional, Balci, M. M., additional, Turkvatan, A., additional, Afsar, B., additional, Alkis, M., additional, Mandiroglu, F., additional, Voroneanu, L., additional, Siriopol, D., additional, Nistor, I., additional, Apetrii, M., additional, Hogas, S., additional, Onofriescu, M., additional, Covic, A., additional, An, W. S., additional, Kim, S. E., additional, Son, Y. K., additional, Oh, Y. J., additional, Gelev, S., additional, Toshev, S., additional, Trajceska, L., additional, Selim, G., additional, Dzekova, P., additional, Shikole, A., additional, Park, J., additional, Lee, J. S., additional, Shin, E.-S., additional, Ann, S. H., additional, Kim, S.-J., additional, Chung, H. C., additional, Sulowicz, W., additional, Elewa, U., additional, Bichari, W., additional, Abo-Seif, K., additional, Seferi, S., additional, Rroji, M., additional, Likaj, E., additional, Spahia, N., additional, Barbullushi, M., additional, Thereska, N., additional, Kopecky, C. M., additional, Genser, B., additional, Maerz, W., additional, Wanner, C., additional, Saemann, M. D., additional, Weichhart, T., additional, Sezer, S., additional, Gurlek Demirci, B., additional, Tutal, E., additional, Bal, Z., additional, Erkmen Uyar, M., additional, Ozdemir Acar, F. N., additional, Macunluoglu, B., additional, Atakan, A., additional, Ari Bakir, E., additional, Georgianos, P., additional, Sarafidis, P. A., additional, Stamatiadis, D. N., additional, Liakopoulos, V., additional, Zebekakis, P. E., additional, Papagianni, A., additional, Lasaridis, A. N., additional, Eftimovska - Otovic, N., additional, Babalj-Banskolieva, E., additional, Kostadinska-Bogdanoska, S., additional, Grozdanovski, R., additional, Aono, M., additional, Sato, Y., additional, El Amrani, M., additional, Asserraji, M., additional, Benyahia, M., additional, Lee, Y.-K., additional, Choi, S. R., additional, Cho, A., additional, Kim, J.-K., additional, Choi, M.-J., additional, Kim, S. J., additional, Yoon, J.-W., additional, Koo, J.-R., additional, Kim, H. J., additional, Noh, J.-W., additional, Inagaki, H., additional, Yokota, N., additional, Chiyotanda, S., additional, Fukami, K., additional, Fujimoto, S., additional, Kendi Celebi, Z., additional, Kutlay, S., additional, Sengul, S., additional, Nergizoglu, G., additional, Erturk, S., additional, Ates, K., additional, Vishnevskii, K. A., additional, Rumyantsev, A. S., additional, Zemchenkov, A. Y., additional, Smirnov, A. V., additional, Reinhardt, B., additional, Knaup, R., additional, Esteve Simo, V., additional, Carneiro Oliveira, J., additional, Moreno Guzman, F., additional, Fulquet Nicolas, M., additional, Pou Potau, M., additional, Saurina Sole, A., additional, Duarte Gallego, V., additional, Ramirez De Arellano Serna, M., additional, Turkmen, K., additional, Demirtas, L., additional, Akbas, E. M., additional, Bakirci, E. M., additional, Buyuklu, M., additional, Timuroglu, A., additional, Georgianos, P. I., additional, Karpetas, A., additional, Taira, T., additional, Nohtomi, K., additional, Takemura, T., additional, Chiba, T., additional, Hirano, T., additional, Chang, C.-T., additional, Huang, C.-C., additional, Chen, C.-J., additional, Mohamed, A., additional, Kanai, H., additional, Tamura, Y., additional, Kaizu, Y., additional, Kali, A., additional, Yayar, O., additional, Erdogan, B., additional, Eser, B., additional, Ercan, Z., additional, Buyukbakkal, M., additional, Merhametsiz, O., additional, Haspulat, A., additional, Yildirim, T., additional, Bozkurt, B., additional, Ayli, M. D., additional, Gokustun, D., additional, Markaki, A., additional, Grammatikopoulou, M., additional, Fragkiadakis, G., additional, Stylianou, K., additional, Venyhaki, M., additional, Chatzi, V., additional, Stojceva-Taneva, O., additional, Tozija, L., additional, Dzekova-Vidimliski, P., additional, Petronievic, Z., additional, Sikole, A., additional, Moyseyenko, V., additional, Nykula, T., additional, Fernandes, R. T., additional, Barreto, D. V., additional, Rodrigues, G. G. C., additional, Misael, A., additional, Branco-Martins, C. T., additional, and Barreto, F. C., additional
Published: 2014
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30. CELL PHYSIOLOGY AND ELECTROLYTES

Author: Yang, A., primary, Low, J. J., additional, Leon, A., additional, Rasmussen, H. S., additional, Therwani, S. A., additional, Bruschi, M., additional, Santucci, L., additional, Bonsano, M., additional, Candiano, G., additional, Ghiggeri, G. M., additional, Verrina, E., additional, Nagaraju, S. P., additional, Kirpalani, D. A., additional, Daga, G., additional, Shah, H., additional, Bhabhe, A. S., additional, Kirpalani, A. L., additional, Sarlak, H., additional, Bulucu, F., additional, Akhan, M., additional, Demirbas, S., additional, Cakar, M., additional, Yamanel, L., additional, Lee, Y.-K., additional, Lee, S. M., additional, Cho, A., additional, Kim, J.-K., additional, Choi, M.-J., additional, Shin, D.-H., additional, Yoon, J.-W., additional, Koo, J.-R., additional, Kim, H. J., additional, Noh, J.-W., additional, Lee, Y. G., additional, Onuigbo, M., additional, Agbasi, N., additional, Minako, K., additional, Saeko, K., additional, Ryosuke, U., additional, Shinzo, K., additional, Sirou, O., additional, Jensen, J., additional, Mose, F. H., additional, Kulik, A.-E. O., additional, Bech, J. N., additional, and Pedersen, E. B., additional
Published: 2014
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31. Microlensing Binaries with Candidate Brown Dwarf Companions

Author: Shin, I.-G, Han, C., Gould, A., Udalski, A., Sumi, T., Dominik, M., Beaulieu, J.-P, Tsapras, Y., Bozza, V., Szyman´ski, M. K., Kubiak, M., Soszyn´ski, I., Pietrzyn´ski, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Furusawa, K., Hayashi, F., Hearnshaw, J. B., Hosaka, S., Itow, Y., Kamiya, K., Kilmartin, P. M., Kobara, S., Korpela, A., Lin, W., Ling, C. H., Makita, S., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Nagaya, M., Nishimoto, K., Ohnishi, K., Okumura, T., Omori, K., Perrott, Y. C., Rattenbury, N., Saito, To, Skuljan, L., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Christie, G. W., Depoy, D. L., Dong, S., Gal-Yam, A., Gaudi, B. S., Hung, L.-W, Janczak, J., Kaspi, S., Maoz, D., McCormick, J., McGregor, D., Moorhouse, D., Muñoz, J. A., Natusch, T., Nelson, C., Pogge, R. W., Tan, T.-G, Polishook, D., Shvartzvald, Y., Shporer, A., Thornley, G., Malamud, U., Yee, J. C., Choi, J.-Y, Jung, Y.-K, Park, H., Lee, C.-U, Park, B.-G, Koo, J.-R, Bajek, D., Bramich, D. M., Browne, P., Horne, K., Ipatov, S., Snodgrass, C., Steele, I., Street, R., Alsubai, K. A., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dreizler, S., Fang, X.-S, Grundahl, F., Gu, C.-H, Hardis, S., Harpsøe, K., Hinse, T. C., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Hornstrup, Allan, Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., Zimmer, F., Albrow, M. D., Batista, V., Brillant, S., Caldwell, J. A. R., Calitz, J. J., Cassan, A., Cole, A., Cook, K. H., Corrales, E., Coutures, Ch, Dieters, S., Dominis Prester, D., Donatowicz, J., Fouque´, P., Greenhill, J., Hill, K., Hoffman, M., Kane, S. R., Kubas, D., Marquette, J.-B, Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., Vinter, C., Zub, M., Shin, I.-G, Han, C., Gould, A., Udalski, A., Sumi, T., Dominik, M., Beaulieu, J.-P, Tsapras, Y., Bozza, V., Szyman´ski, M. K., Kubiak, M., Soszyn´ski, I., Pietrzyn´ski, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Furusawa, K., Hayashi, F., Hearnshaw, J. B., Hosaka, S., Itow, Y., Kamiya, K., Kilmartin, P. M., Kobara, S., Korpela, A., Lin, W., Ling, C. H., Makita, S., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Nagaya, M., Nishimoto, K., Ohnishi, K., Okumura, T., Omori, K., Perrott, Y. C., Rattenbury, N., Saito, To, Skuljan, L., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Christie, G. W., Depoy, D. L., Dong, S., Gal-Yam, A., Gaudi, B. S., Hung, L.-W, Janczak, J., Kaspi, S., Maoz, D., McCormick, J., McGregor, D., Moorhouse, D., Muñoz, J. A., Natusch, T., Nelson, C., Pogge, R. W., Tan, T.-G, Polishook, D., Shvartzvald, Y., Shporer, A., Thornley, G., Malamud, U., Yee, J. C., Choi, J.-Y, Jung, Y.-K, Park, H., Lee, C.-U, Park, B.-G, Koo, J.-R, Bajek, D., Bramich, D. M., Browne, P., Horne, K., Ipatov, S., Snodgrass, C., Steele, I., Street, R., Alsubai, K. A., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dreizler, S., Fang, X.-S, Grundahl, F., Gu, C.-H, Hardis, S., Harpsøe, K., Hinse, T. C., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Hornstrup, Allan, Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., Zimmer, F., Albrow, M. D., Batista, V., Brillant, S., Caldwell, J. A. R., Calitz, J. J., Cassan, A., Cole, A., Cook, K. H., Corrales, E., Coutures, Ch, Dieters, S., Dominis Prester, D., Donatowicz, J., Fouque´, P., Greenhill, J., Hill, K., Hoffman, M., Kane, S. R., Kubas, D., Marquette, J.-B, Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., Vinter, C., and Zub, M.
Abstract: Brown dwarfs are important objects because they may provide a missing link between stars and planets, two populations that have dramatically different formation histories. In this paper, we present the candidate binaries with brown dwarf companions that are found by analyzing binary microlensing events discovered during the 2004-2011 observation seasons. Based on the low mass ratio criterion of q <0.2, we found seven candidate events: OGLE-2004-BLG-035, OGLE-2004-BLG-039, OGLE-2007-BLG-006, OGLE-2007-BLG-399/MOA-2007-BLG-334, MOA-2011-BLG-104/OGLE-2011-BLG-0172, MOA-2011-BLG-149, and MOA-201-BLG-278/OGLE-2011-BLG-012N. Among them, we are able to confirm that the companions of the lenses of MOA-2011-BLG-104/OGLE-2011-BLG-0172 and MOA-2011-BLG-149 are brown dwarfs by determining the mass of the lens based on the simultaneous measurement of the Einstein radius and the lens parallax. The measured masses of the brown dwarf companions are 0.02 ± 0.01 M⊙ and 0.019 ± 0.002 M⊙ for MOA-2011-BLG-104/OGLE-2011-BLG-0172 and MOA-2011-BLG-149, respectively, and both companions are orbiting low-mass M dwarf host stars. More microlensing brown dwarfs are expected to be detected as the number of lensing events with well-covered light curves increases with new-generation searches.
Published: 2012

32. A giant planet beyond the snow line in microlensing event OGLE-2011-BLG-0251

Author: Kains, N., primary, Street, R. A., additional, Choi, J.-Y., additional, Han, C., additional, Udalski, A., additional, Almeida, L. A., additional, Jablonski, F., additional, Tristram, P. J., additional, Jørgensen, U. G., additional, Szymański, M. K., additional, Kubiak, M., additional, Pietrzyński, G., additional, Soszyński, I., additional, Poleski, R., additional, Kozłowski, S., additional, Pietrukowicz, P., additional, Ulaczyk, K., additional, Wyrzykowski, Ł., additional, Skowron, J., additional, Alsubai, K. A., additional, Bozza, V., additional, Browne, P., additional, Burgdorf, M. J., additional, Calchi Novati, S., additional, Dodds, P., additional, Dominik, M., additional, Dreizler, S., additional, Fang, X.-S., additional, Grundahl, F., additional, Gu, C.-H., additional, Hardis, S., additional, Harpsøe, K., additional, Hessman, F. V., additional, Hinse, T. C., additional, Hornstrup, A., additional, Hundertmark, M., additional, Jessen-Hansen, J., additional, Kerins, E., additional, Liebig, C., additional, Lund, M., additional, Lundkvist, M., additional, Mancini, L., additional, Mathiasen, M., additional, Penny, M. T., additional, Rahvar, S., additional, Ricci, D., additional, Sahu, K. C., additional, Scarpetta, G., additional, Skottfelt, J., additional, Snodgrass, C., additional, Southworth, J., additional, Surdej, J., additional, Tregloan-Reed, J., additional, Wambsganss, J., additional, Wertz, O., additional, Bajek, D., additional, Bramich, D. M., additional, Horne, K., additional, Ipatov, S., additional, Steele, I. A., additional, Tsapras, Y., additional, Abe, F., additional, Bennett, D. P., additional, Bond, I. A., additional, Botzler, C. S., additional, Chote, P., additional, Freeman, M., additional, Fukui, A., additional, Furusawa, K., additional, Itow, Y., additional, Ling, C. H., additional, Masuda, K., additional, Matsubara, Y., additional, Miyake, N., additional, Muraki, Y., additional, Ohnishi, K., additional, Rattenbury, N., additional, Saito, T., additional, Sullivan, D. J., additional, Sumi, T., additional, Suzuki, D., additional, Suzuki, K., additional, Sweatman, W. L., additional, Takino, S., additional, Wada, K., additional, Yock, P. C. M., additional, Allen, W., additional, Batista, V., additional, Chung, S.-J., additional, Christie, G., additional, DePoy, D. L., additional, Drummond, J., additional, Gaudi, B. S., additional, Gould, A., additional, Henderson, C., additional, Jung, Y.-K., additional, Koo, J.-R., additional, Lee, C.-U., additional, McCormick, J., additional, McGregor, D., additional, Muñoz, J. A., additional, Natusch, T., additional, Ngan, H., additional, Park, H., additional, Pogge, R. W., additional, Shin, I.-G., additional, Yee, J., additional, Albrow, M. D., additional, Bachelet, E., additional, Beaulieu, J.-P., additional, Brillant, S., additional, Caldwell, J. A. R., additional, Cassan, A., additional, Cole, A., additional, Corrales, E., additional, Coutures, Ch., additional, Dieters, S., additional, Dominis Prester, D., additional, Donatowicz, J., additional, Fouqué, P., additional, Greenhill, J., additional, Kane, S. R., additional, Kubas, D., additional, Marquette, J.-B., additional, Martin, R., additional, Meintjes, P., additional, Menzies, J., additional, Pollard, K. R., additional, Williams, A., additional, Wouters, D., additional, and Zub, M., additional
Published: 2013
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33. Peritoneal dialysis

Author: Liu, J., primary, Liu, J., additional, Liu, Y., additional, Xu, Y., additional, Zhao, X., additional, Qian, J., additional, Sun, B., additional, Xing, C., additional, Kanda, R., additional, Hamada, C., additional, Nakano, T., additional, Wakabayashi, K., additional, Io, H., additional, Horikoshi, S., additional, Tomino, Y., additional, Ishimatsu, N., additional, Miyamoto, T., additional, Morimoto, H., additional, Nakamata, J., additional, Baba, R., additional, Kanegae, K., additional, Serino, R., additional, Kabashima, N., additional, Otsuji, Y., additional, Doi, Y., additional, Tamura, M., additional, Kusumoto, T., additional, Fukami, K., additional, Yamagishi, S.-I., additional, Ueda, S., additional, Kaida, Y., additional, Hazama, T., additional, Nakayama, Y., additional, Ando, R., additional, Obara, N., additional, Okuda, S., additional, Matsumoto, M., additional, Furuno, Y., additional, Bang-Gee, H., additional, Mazzotta, L., additional, Rosati, A., additional, Carlini, A., additional, Henriques, V. T., additional, Zangiacomi Martinez, E., additional, Divino-Filho, J. C., additional, Pecoits-Filho, R., additional, Cardeal Da Costa, J. A., additional, Gama Axelsson, T., additional, Lindholm, B., additional, Carrero, J. J., additional, Heimburger, O., additional, Stenvinkel, P., additional, Qureshi, A. R., additional, Akazawa, M., additional, Uno, T., additional, Kanda, E., additional, Maeda, Y., additional, Aktsiali, M., additional, Antonopoulou, S., additional, Tsiolaki, K., additional, Bakirtzi, N., additional, Patrinou, A., additional, Georgopoulou, M., additional, Liaveri, P., additional, Afentakis, N., additional, Tsirpanlis, G., additional, Hasegawa, T., additional, Nishiwaki, H., additional, Hirose, M., additional, Komukai, D., additional, Tayama, H., additional, Koiwa, F., additional, Yoshimura, A., additional, Lui, S. L., additional, Lui, S., additional, Yung, S., additional, Tang, C., additional, Ng, F., additional, Lo, W. K., additional, Chan, T. M., additional, Koo, H. M., additional, Doh, F. M., additional, Yoo, D. E., additional, Oh, H. J., additional, Yoo, T.-H., additional, Choi, K. H., additional, Kang, S.-W., additional, Han, D. S., additional, Han, S. H., additional, Fernandes, N., additional, Bastos, M. G., additional, Gianotti Franco, M. R., additional, Chaoubah, A., additional, Gloria Lima, M. D., additional, Kang, S., additional, Do, J., additional, Cho, K., additional, Park, J., additional, Yoon, K., additional, Chen, J.-B., additional, Cheng, B.-C., additional, Chen, T.-C., additional, Su, Y.-J., additional, Wu, C.-H., additional, Park, Y., additional, Jeon, J., additional, Tsikeloudi, M., additional, Pateinakis, P., additional, Patsatsi, K., additional, Manou, E., additional, Sotiriadis, D., additional, Tsakiris, D., additional, Teixeira, L., additional, Rodrigues, A., additional, Carvalho, M. J., additional, Cabrita, A., additional, Mendonca, D., additional, Bruschi, M., additional, Candiano, G., additional, Santucci, L., additional, Luzio, S., additional, Cannavo, R., additional, Ghiggeri, G. M., additional, Verrina, E., additional, Varadarajan, Y., additional, Raju, B., additional, Cho, K.-H., additional, Park, J.-W., additional, Yoon, K.-W., additional, Kim, T.-W., additional, Kimmel, M., additional, Braun, N., additional, Latus, J., additional, Alscher, M. D., additional, Struijk, D., additional, Van Esch, S., additional, Krediet, R. T., additional, Van den Beukel, T., additional, Hoekstra, T., additional, Tirapani, L., additional, De Andrade Bastos, K., additional, Bastos, M., additional, Dekker, F., additional, Yasuhisa, T., additional, Kanai, H., additional, Harada, K., additional, Kawai, Y., additional, Sugiyama, H., additional, Ito, Y., additional, Tsuruya, K., additional, Yoshida, H., additional, Maruyama, H., additional, Goto, S., additional, Nakayama, M., additional, Nakamoto, H., additional, Morinaga, H., additional, Matsuo, S., additional, Makino, H., additional, DI Gioia, M. C., additional, Gallar, P., additional, Laso, N., additional, Rodriguez, I., additional, Cobo, G., additional, Oliet, A., additional, Hynostroza, J., additional, Herrero, J. C., additional, Mon, C., additional, Ortiz, M., additional, Vigil, A., additional, Tomo, T., additional, Portoles, J., additional, Uta, S., additional, Tato, A. M., additional, Lopez-Sanchez, P., additional, Rivera, M., additional, Rodriguez-Pena, R., additional, Del Peso, G., additional, Ortega, M., additional, Felipe, C., additional, Tsampikaki, E., additional, Aperis, G., additional, Kaikis, A., additional, Paliouras, C., additional, Karvouniaris, N., additional, Maragaki, M., additional, Alivanis, P., additional, Kortus-Gotze, B., additional, Hoferhusch, T., additional, Hoyer, J., additional, Martino, F., additional, Kaushik, M., additional, Rodighiero, M. P., additional, Creapldi, C., additional, Ronco, C., additional, Lacquaniti, A., additional, Donato, V., additional, Fazio, M. R., additional, Lucisano, S., additional, Cernaro, V., additional, Lupica, R., additional, Buemi, M., additional, Aloisi, C., additional, Bavbek Ruzgaresen, N., additional, Secilmis, S., additional, Yilmaz, H., additional, Akcay, A., additional, Duranay, M., additional, Akalin, N., additional, Altiparmak, M. R., additional, Trabulus, S., additional, Yalin, A. S., additional, Ataman, R., additional, Serdengecti, K., additional, Schneider, K., additional, Bator, B., additional, Niko, B., additional, Peter, F., additional, Ulmer, C., additional, Joerg, L., additional, Martin, K., additional, Dagmar, B., additional, German, O., additional, Fabian, R., additional, Juergen, D., additional, Stephan, S., additional, Dominik, A., additional, Fritz, P., additional, Rettenmaier, B., additional, Hirschburger, S., additional, Segerer, S., additional, Biegger, D., additional, Lang, T., additional, Ott, G., additional, Habib, M., additional, Korte, M., additional, Hagen, M., additional, Dor, F., additional, Betjes, M., additional, Zietse, R., additional, Scharpf, C., additional, Chang, T. I., additional, Shin, D. H., additional, Han, D.-S., additional, Choi, H. Y., additional, Lee, Y. K., additional, Kim, B. S., additional, Yoo, T. H., additional, Park, H. C., additional, Lee, H. Y., additional, Horimoto, N., additional, Tuji, K., additional, Kitamura, S., additional, Isshiki, R., additional, Iwagami, M., additional, Tsutsumi, D., additional, Mochida, Y., additional, Ishioka, K., additional, Oka, M., additional, Maesato, K., additional, Moriya, H., additional, Ohtake, T., additional, Hidaka, S., additional, Kobayashi, S., additional, Higuchi, C., additional, Tanihata, Y., additional, Ishii, M., additional, Sugimoto, H., additional, Sato, N., additional, Kyono, A., additional, Ogawa, T., additional, Nishimura, H., additional, Otsuka, K., additional, Do, J.-Y., additional, Du Halgouet, C., additional, Latifa, A., additional, Anne Sophie, V., additional, Emmanuel, D., additional, Christine, R., additional, Francois, V., additional, Grzelak, T., additional, Czyzewska-Majchrzak, L., additional, Kramkowska, M., additional, Witmanowski, H., additional, Czyzewska, K., additional, Janda, K., additional, Krzanowski, M., additional, Dumnicka, P., additional, Sulowicz, W., additional, Rroji, M., additional, Seferi, S., additional, Barbullushi, M., additional, Likaj, E., additional, Petrela, E., additional, Thereska, N., additional, Cabiddu, G., additional, Dessi, E., additional, Arceri, A., additional, Laura, P., additional, Manca, E., additional, Conti, M., additional, Cao, R., additional, Pani, A., additional, Liao, C.-T., additional, Vega Vega, O., additional, Mendoza de la Garza, A., additional, Correa-Rotter, R., additional, Ueda, A., additional, Nagai, K., additional, Morimoto, M., additional, Hirayama, A., additional, Owada, S., additional, Tonozuka, Y., additional, Saito, C., additional, Yamagata, K., additional, Matsuda, A., additional, Tayama, Y., additional, Iwanaga, M., additional, Noiri, C., additional, Hatano, M., additional, Kiba, T., additional, Kanozawa, K., additional, Katou, H., additional, Hasegawa, H., additional, Mitarai, T., additional, Ros-Ruiz, S., additional, Fuentes-Sanchez, L., additional, Jironda-Gallegos, C., additional, Gutierrez-Vilches, E., additional, Garcia-Frias, P., additional, Hernandez-Marrero, D., additional, Lee, S., additional, Lai, X., additional, Chen, W., additional, Guo, Z., additional, Braide, M., additional, Cristina, V., additional, Popa, S. G., additional, Maria, M., additional, Eugen, M., additional, DI Loreto, P., additional, Spahia, N., additional, Sanchez Macias, L. O., additional, Lares Castellanos, K. I., additional, Hernandez Pacheco, J. A., additional, Correa Rotter, R., additional, Pedro Ventura, A., additional, Olivia, S., additional, Joana, V., additional, Francisco, F., additional, Maria Joao, C., additional, Antonio, C., additional, Rodrigues, A. S., additional, Atas, N., additional, Erten, Y., additional, Onec, K., additional, Inal, S., additional, Topal, S., additional, Akyel, A., additional, Celik, B., additional, Okyay, G. U., additional, Tavil, Y., additional, Zeiler, M., additional, Monteburini, T., additional, Agostinelli, R. M., additional, Marinelli, R., additional, Santarelli, S., additional, Yaylaci, C., additional, Sahin, G., additional, Guz, G., additional, Sindel, S., additional, Pinho, A., additional, Malho Guedes, A., additional, Fragoso, A., additional, Carreira, H., additional, Pinto, I., additional, Bernardo, I., additional, Leao, P., additional, Kusnierz-Cabala, B., additional, Krasniak, A., additional, Chowaniec, E., additional, Tabor-Ciepiela, B., additional, Turkmen, K., additional, Ozbek, O., additional, Kayrak, M., additional, Samur, C., additional, Guler, I., additional, Tonbul, H. Z., additional, Rusai, K., additional, Herzog, R., additional, Kratochwill, K., additional, Kuster, L., additional, Aufricht, C., additional, Meier, C.-M., additional, Fliser, D., additional, Schilling, M. K., additional, Klingele, M., additional, Fukasawa, M., additional, Takeda, M., additional, Kamiyama, M., additional, Song, Y. R., additional, Kim, H. J., additional, Kim, S. G., additional, Kim, J.-K., additional, Noh, J. W., additional, Yoon, J. W., additional, and Koo, J.-R., additional
Published: 2012
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34. Multi-site, multi-year monitoring of the oscillating Algol-type eclipsing binary CT Herculis

Author: Lampens, P., primary, Strigachev, A., additional, Kim, S.-L., additional, Rodríguez, E., additional, López-González, M. J., additional, Vidal-Saínz, J., additional, Mkrtichian, D., additional, Koo, J.-R., additional, Kang, Y. B., additional, Van Cauteren, P., additional, Wils, P., additional, Kraicheva, Z., additional, Dimitrov, D., additional, Southworth, J., additional, García Melendo, E., additional, and Gómez Forellad, J. M., additional
Published: 2011
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35. RACE-OC project: rotation and variability in the open cluster M 11 (NGC 6705)

Author: Messina, S., primary, Parihar, P., additional, Koo, J.-R., additional, Kim, S.-L., additional, Rey, S.-C., additional, and Lee, C.-U., additional
Published: 2010
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36. The RACE-OC project: Rotation and Activity Evolution in Open Clusters

Author: Messina, S., primary, Distefano, E., additional, Parihar, Padmakar, additional, Busà, I., additional, Cutispoto, G., additional, Lanza, A. F., additional, Lanzafame, A., additional, Pagano, I., additional, Biazzo, K., additional, Leto, G., additional, Hatzidimitriou, D., additional, Kim, S.-L., additional, Koo, J.-R., additional, Kang, Y. B., additional, and Stempels, Eric, additional
Published: 2009
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37. A comparison between once-weekly and twice- or thrice-weekly subcutaneous injection of epoetin alfa: results from a randomized controlled multicentre study

Author: Lee, Y. K., primary, Kim, S. G., additional, Seo, J. W., additional, Oh, J. E., additional, Yoon, J.-W., additional, Koo, J.-R., additional, Kim, H. J., additional, and Noh, J. W., additional
Published: 2008
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38. Variable Stars in the Open Cluster M11 (NGC 6705)

Author: Koo, J.‐R., primary, Kim, S.‐L., additional, Rey, S.‐C., additional, Lee, C.‐U., additional, Kim, Y. H., additional, Kang, Y. B., additional, and Jeon, Y.‐B., additional
Published: 2007
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39. Multisite campaign on the open cluster M67 - III. Scuti pulsations in the blue stragglers

Author: Bruntt, H., primary, Stello, D., additional, Suarez, J. C., additional, Arentoft, T., additional, Bedding, T. R., additional, Bouzid, M. Y., additional, Csubry, Z., additional, Dall, T. H., additional, Dind, Z. E., additional, Frandsen, S., additional, Gilliland, R. L., additional, Jacob, A. P., additional, Jensen, H. R., additional, Kang, Y. B., additional, Kim, S.- L., additional, Kiss, L. L., additional, Kjeldsen, H., additional, Koo, J.- R., additional, Lee, J.- A., additional, Lee, C.- U., additional, Nuspl, J., additional, Sterken, C., additional, and Szabo, R., additional
Published: 2007
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40. Multisite campaign on the open cluster M67 - II. Evidence for solar-like oscillations in red giant stars

Author: Stello, D., primary, Bruntt, H., additional, Kjeldsen, H., additional, Bedding, T. R., additional, Arentoft, T., additional, Gilliland, R. L., additional, Nuspl, J., additional, Kim, S.-L., additional, Kang, Y. B., additional, Koo, J.-R., additional, Lee, J.-A., additional, Sterken, C., additional, Lee, C.-U., additional, Jensen, H. R., additional, Jacob, A. P., additional, Szabó, R., additional, Frandsen, S., additional, Csubry, Z., additional, Dind, Z. E., additional, Bouzid, M. Y., additional, Dall, T. H., additional, and Kiss, L. L., additional
Published: 2007
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41. Variable Stars in the Open Cluster NGC 2099 (M37)

Author: Kang, Y. B., primary, Kim, S.‐L., additional, Rey, S.‐C., additional, Lee, C.‐U., additional, Kim, Y. H., additional, Koo, J.‐R., additional, and Jeon, Y.‐B., additional
Published: 2007
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42. Multisite campaign on the open cluster M67 – I. Observations and photometric reductions

Author: Stello, D., primary, Arentoft, T., additional, Bedding, T. R., additional, Bouzid, M. Y., additional, Bruntt, H., additional, Csubry, Z., additional, Dall, T. H., additional, Dind, Z. E., additional, Frandsen, S., additional, Gilliland, R. L., additional, Jacob, A. P., additional, Jensen, H. R., additional, Kang, Y. B., additional, Kim, S.-L., additional, Kiss, L. L., additional, Kjeldsen, H., additional, Koo, J.-R., additional, Lee, J.-A., additional, Lee, C.-U., additional, Nuspl, J., additional, Sterken, C., additional, and Szabó, R., additional
Published: 2006
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43. Organic Thin-Film Transistors Based on Vapor-Deposition Polymerized Gate Insulators

Author: Pyo, S. W., primary, Lee, D. H., additional, Koo, J. R., additional, Kim, J. H., additional, Shim, J. H., additional, and Kim, Y. K., additional
Published: 2005
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44. PHOTOMETRIC PROPERTIES OF FOUR NEW VARIABLE STARS IN THE VICINITY OF BR CAM

Author: KIM, S.-L., primary, LEE, C.-D., additional, LEE, J. W., additional, LEE, J. A., additional, KANG, Y.B., additional, KOO, J.-R., additional, and VAUCLAIR, G., additional
Published: 2004
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45. P.1.005 The serum cytokines and nutritional status after antidepressant treatment in hemodialysis patients

Author: Lee, S.-K., primary, Koo, J.-R., additional, Kim, D.-H., additional, and Son, B.-K., additional
Published: 2003
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46. Multisite campaign on the open cluster M67 – III. δ Scuti pulsations in the blue stragglers.

Author: Bruntt, H., Stello, D., Suárez, J. C., Arentoft, T., Bedding, T. R., Bouzid, M. Y., Csubry, Z., Dall, T. H., Dind, Z. E., Frandsen, S., Gilliland, R. L., Jacob, A. P., Jensen, H. R., Kang, Y. B., Kim, S.-L., Kiss, L. L., Kjeldsen, H., Koo, J.-R., Lee, J.-A., and Lee, C.-U.
Subjects: BLUE stragglers (Stars), OPEN clusters of stars, ASTRONOMICAL photometry, ASTRONOMICAL spectroscopy, STELLAR oscillations
Abstract: We have made an asteroseismic analysis of the variable blue stragglers in the open cluster M67. The data set consists of photometric time-series from eight sites using nine 0.6–2.1 m telescopes with a time-baseline of 43 d. In two stars, EW Cnc and EX Cnc, we detect the highest number of frequencies (41 and 26) detected in δ Scuti stars belonging to a stellar cluster, and EW Cnc has the second highest number of frequencies detected in any δ Scuti star. We have computed a grid of pulsation models that take the effects of rotation into account. The distribution of observed and theoretical frequencies shows that in a wide frequency range a significant fraction of the radial and non-radial low-degree modes are excited to detectable amplitudes. Despite the large number of observed frequencies we cannot constrain the fundamental parameters of the stars. To make progress we need to identify the degrees of some of the modes from either multicolour photometry or spectroscopy. [ABSTRACT FROM AUTHOR]
Published: 2007
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47. Th1/Th2 predominance and proinflammatory cytokines determine the clinicopathological severity of IgA nephropathy.

Author: Lim, C S, Zheng, S, Kim, Y S, Ahn, C, Han, J S, Kim, S, Lee, J S, Chae, D W, Koo, J R, Chun, R W, and Noh, J W
Abstract: IgA nephropathy is one of the most common forms of primary glomerulonephritis in adults. Its pathogenesis is complex. The nature of infiltrating and proliferating cells and of cellular mediators could contribute to the progression of IgA nephropathy towards end-stage renal failure.
Published: 2001
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48. Case report. Acute renal cortical necrosis caused by an antifibrinolytic drug (tranexamic acid).

Author: Koo, J-R, Lee, Y-K, Kim, Y-S, Cho, W-Y, Kim, H-K, and Won, N-H
Abstract: Keywords:acute renal cortical necrosis; antifibrinolytic drug; tranexamic acid [ABSTRACT FROM PUBLISHER]
Published: 1999
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49. Multi-site time series photometry of the open cluster M67

Author: Stello, D., Arentoft, T., Bedding, T. R., Bouzid, M. Y., Bruntt, H., Csubry, Z., Dall, T. H., Dind, Z. E., Frandsen, S., Gilliland, R. L., Jacob, A. P., Jensen, H. R., Kang, Y. B., Kim, S. -L, Kiss, L. L., Kjeldsen, H., Koo, J. -R, Lee, J. -A, Lee, C. -U, Nuspl, J., Qiu, Y., Sterken, C., Robert Szabo, and Xiao, P.

50. Acute renal cortical necrosis caused by an antifibrinolytic drug (tranexamic acid).

Author: Koo, J R, Lee, Y K, Kim, Y S, Cho, W Y, Kim, H K, and Won, N H
Published: 1999
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