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1. Association between Fiber Intake and Risk of Incident Chronic Kidney Disease: The UK Biobank Study

Author: Heo, G. Y., Kim, H. J., Kalantar, D., Jung, C. Y., Kim, H. W., Park, J. T., Chang, T. I., Yoo, T. H., Kang, S. W., Rhee, C. M., Kalantar-Zadeh, K., and Han, Seung Hyeok
Published: 2023
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2. OGLE-2018-BLG-1185b : A Low-Mass Microlensing Planet Orbiting a Low-Mass Dwarf

Author: Kondo, Iona, Yee, Jennifer C., Bennett, David P., Sumi, Takahiro, Koshimoto, Naoki, Bond, Ian A., Gould, Andrew, Udalski, Andrzej, Shvartzvald, Yossi, Jung, Youn Kil, Zang, Weicheng, Bozza, Valerio, Bachelet, Etienne, Hundertmark, Markus P. G., Rattenbury, Nicholas J., Abe, F., Barry, R., Bhattacharya, A., Donachie, M., Fukui, A., Fujii, H., Hirao, Y., Silva, S. Ishitani, Itow, Y., Kirikawa, R., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Olmschenk, G., Ranc, C., Satoh, Y., Shoji, H., Suzuki, D., Tanaka, Y., Tristram, P. J., Yamawaki, T., Yonehara, A., Mróz, P., Poleski, R., Skowron, J., Szymański, M. K., Soszyński, I., Kozłowski, S., Ulaczyk, P. Pietrukowicz K., Rybicki, K. A., Iwanek, P., Wrona, M., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Kim, H. -W., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Ryu, Y. -H., Beichman, C. A., Bryden, G., Novati, S. Calchi, Carey, S., Gaudi, B. S., Henderson, C. B., Zhu, W., Maoz, D., Penny, M. T., Dominik, M., Jørgensen, U. G., n}}a, P. Longa-Pe{\~{, Peixinho, N., Sajadian, S., Skottfelt, J., Snodgrass, C., Tregloan-Reed, J., Burgdorf, M. J., Campbell-White, J., Dib, S., Fujii, Y. I., Hinse, T. C., Khalouei, E., Rahvar, S., Rabus, M., Southworth, J., Tsapras, Y., Street, R. A., Bramich, D. M., Cassan, A., Horne, K., Wambsganss, J., Mao, S., and Saha, A.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the analysis of planetary microlensing event OGLE-2018-BLG-1185, which was observed by a large number of ground-based telescopes and by the $Spitzer$ Space Telescope. The ground-based light curve indicates a low planet-host star mass ratio of $q = (6.9 \pm 0.2) \times 10^{-5}$, which is near the peak of the wide-orbit exoplanet mass-ratio distribution. We estimate the host star and planet masses with a Bayesian analysis using the measured angular Einstein radius under the assumption that stars of all masses have an equal probability to host this planet. The flux variation observed by $Spitzer$ was marginal, but still places a constraint on the microlens parallax. Imposing a conservative constraint that this flux variation should be $\Delta f_{\rm Spz} < 4$ instrumental flux units indicates a host mass of $M_{\rm host} = 0.37^{+0.35}_{-0.21}\ M_\odot$ and a planet mass of $m_{\rm p} = 8.4^{+7.9}_{-4.7}\ M_\oplus$. A Bayesian analysis including the full parallax constraint from $Spitzer$ suggests smaller host star and planet masses of $M_{\rm host} = 0.091^{+0.064}_{-0.018}\ M_\odot$ and $m_{\rm p} = 2.1^{+1.5}_{-0.4}\ M_\oplus$, respectively. Future high-resolution imaging observations with $HST$ or ELTs could distinguish between these two scenarios and help to reveal the planetary system properties in more detail., Comment: 30 pages, 11 figures, 5 tables, Accepted for publication in Astronomical Journal (AJ)
Published: 2021
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3. A terrestrial-mass rogue planet candidate detected in the shortest-timescale microlensing event

Author: Mroz, P., Poleski, R., Gould, A., Udalski, A., Sumi, T., Szymanski, M. K., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Skowron, J., Ulaczyk, K., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Kim, H. -W., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zang, W., Cha, S. -M., Kim, D. -J., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Some low-mass planets are expected to be ejected from their parent planetary systems during early stages of planetary system formation. According to planet-formation theories, such as the core accretion theory, typical masses of ejected planets should be between 0.3 and 1.0 $M_{\oplus}$. Although in practice such objects do not emit any light, they may be detected using gravitational microlensing via their light-bending gravity. Microlensing events due to terrestrial-mass rogue planets are expected to have extremely small angular Einstein radii (< 1 uas) and extremely short timescales (< 0.1 day). Here, we present the discovery of the shortest-timescale microlensing event, OGLE-2016-BLG-1928, identified to date ($t_{\rm E} \approx 0.0288\ \mathrm{day} = 41.5 \mathrm{min}$). Thanks to the detection of finite-source effects in the light curve of the event, we were able to measure the angular Einstein radius of the lens $\theta_{\rm E} = 0.842 \pm 0.064$ uas, making the event the most extreme short-timescale microlens discovered to date. Depending on its unknown distance, the lens may be a Mars- to Earth-mass object, with the former possibility favored by the Gaia proper motion measurement of the source. The planet may be orbiting a star but we rule out the presence of stellar companions up to the projected distance of 8.0 au from the planet. Our discovery demonstrates that terrestrial-mass free-floating planets can be detected and characterized using microlensing., Comment: accepted for publication in ApJ Letters, minor changes
Published: 2020
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4. Ogle-2018-blg-0677lb: A super earth near the galactic bulge

Author: Herrera-Martín, Antonio, Albrow, M. D., Udalski, A., Gould, A., Ryu, Y. -H., Yee, J. C., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Lee, C. -U., Shin, I. -G., Shvartzvald, Y., Zang, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Szymański, M. K., Mróz, P., Skowron, J., Poleski, R., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Rybicki, K., Iwanek, P., and Wrona, M.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: We report the analysis of the microlensing event OGLE-2018-BLG-0677. A small feature in the light curve of the event leads to the discovery that the lens is a star-planet system. Although there are two degenerate solutions that could not be distinguished for this event, both lead to a similar planet-host mass ratio. We perform a Bayesian analysis based on a Galactic model to obtain the properties of the system and find that the planet corresponds to a super-Earth/sub-Neptune with a mass $M_{\mathrm{planet}} = {3.96}^{+5.88}_{-2.66}\mathrm{M_\oplus}$. The host star has a mass $ M_{\mathrm{host}} = {0.12}^{+0.14}_{-0.08}\mathrm{M_\odot}$. The projected separation for the inner and outer solutions are ${0.63}^{+0.20}_{-0.17}$~AU and ${0.72}^{+0.23}_{-0.19}$~AU respectively. At $\Delta\chi^2=\chi^2({\rm 1L1S})-\chi^2({\rm 2L1S})=46$, this is by far the lowest $\Delta\chi^2$ for any securely-detected microlensing planet to date, a feature that is closely connected to the fact that it is detected primarily via a "dip" rather than a "bump"., Comment: 15 page, 12 figures, Published in AJ
Published: 2020
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5. The 2L1S/1L2S Degeneracy for Two Microlensing Planet Candidates Discovered by the KMTNet Survey in 2017

Author: Shin, I. -G., Yee, J. C., Gould, A., Penny, M. T., Bond, I. A., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shvartzvald, Y., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Fujii, H., Fukui, A., Hirao, Y., Itow, Y., Kamei, Y., Kondo, Iona, Koshimoto, N., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, Harmon, Sullivan, D. J., Sumi, T., Suzuki, Daisuke, Tristram, P. J., Yamakawa, T., Yonehara, A., Fouqué, P., and Zang, W.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report two microlensing planet candidates discovered by the KMTNet survey in $2017$. However, both events have the 2L1S/1L2S degeneracy, which is an obstacle to claiming the discovery of the planets with certainty unless the degeneracy can be resolved. For KMT-2017-BLG-0962, the degeneracy cannot be resolved. If the 2L1S solution is correct, KMT-2017-BLG-0962 might be produced by a super Jupiter-mass planet orbiting a mid-M dwarf host star. For KMT-2017-BLG-1119, the light curve modeling favors the 2L1S solution but higher-resolution observations of the baseline object tend to support the 1L2S interpretation rather than the planetary interpretation. This degeneracy might be resolved by a future measurement of the lens-source relative proper motion. This study shows the problem of resolving 2L1S/1L2S degeneracy exists over a much wider range of conditions than those considered by the theoretical study of Gaudi (1998)., Comment: 15 pages, 12 figures, 4 tables, accepted in AJ
Published: 2019
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6. Two Jupiter-Mass Planets Discovered by the KMTNet Survey in 2017

Author: Shin, I. -G., Ryu, Y. -H., Yee, J. C., Gould, A., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Shvartzvald, Y., Zang, W., Lee, C. -U., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, Y., Lee, D. -J., Park, B. -G., and Pogge, R. W.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report two microlensing events, KMT-2017-BLG-1038 and KMT-2017-BLG-1146 that are caused by planetary systems. These events were discovered by KMTNet survey observations from the $2017$ bulge season. The discovered systems consist of a planet and host star with mass ratios, $5.3_{-0.4}^{+0.2} \times 10^{-3}$ and $2.0_{-0.1}^{+0.6} \times 10^{-3}$, respectively. Based on a Bayesian analysis assuming a Galactic model without stellar remnant hosts, we find that the planet, KMT-2017-BLG-1038Lb, is a super Jupiter-mass planet ($M_{\rm p}= 2.04_{-1.15}^{+2.02}\,M_{\rm J}$) orbiting a mid-M dwarf host ($M_{\rm h}= 0.37_{-0.20}^{+0.36}\, M_{\odot}$) that is located at $6.01_{-1.72}^{+1.27}$ kpc toward the Galactic bulge. The other planet, KMT-2017-BLG-1146Lb, is a sub Jupiter-mass planet ($M_{\rm p}= 0.71_{-0.42}^{+0.80}\,M_{\rm J}$) orbiting a mid-M dwarf host ($M_{\rm h}= 0.33_{-0.20}^{+0.36}\,M_{\odot}$) at a distance toward the Galactic bulge of $6.50_{-2.00}^{+1.38}$ kpc. Both are potentially gaseous planets that are beyond their hosts' snow lines. These typical microlensing planets will be routinely discovered by second-generation microlensing surveys, rapidly increasing the number of detections., Comment: 8 pages, 10 figures, 2 tables, accepted for publication in AJ
Published: 2018
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7. Two new free-floating or wide-orbit planets from microlensing

Author: Mroz, P., Udalski, A., Bennett, D. P., Ryu, Y. -H., Sumi, T., Shvartzvald, Y., Skowron, J., Poleski, R., Pietrukowicz, P., Kozlowski, S., Szymanski, M. K., Wyrzykowski, L., Soszynski, I., Ulaczyk, K., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Hwang, K. -H., Jung, Y. K., Shin, I. -G., Yee, J. C., Zang, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Abe, F., Barry, R., Bhattacharya, A., Bond, I. A., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Kondo, I., Koshimoto, N., Li, M. C. A., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, H., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Maoz, D., Kaspi, S., and Friedmann, M.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Planet formation theories predict the existence of free-floating planets that have been ejected from their parent systems. Although they emit little or no light, they can be detected during gravitational microlensing events. Microlensing events caused by rogue planets are characterized by very short timescales $t_{\rm E}$ (typically below two days) and small angular Einstein radii $\theta_{\rm E}$ (up to several uas). Here we present the discovery and characterization of two ultra-short microlensing events identified in data from the Optical Gravitational Lensing Experiment (OGLE) survey, which may have been caused by free-floating or wide-orbit planets. OGLE-2012-BLG-1323 is one of the shortest events discovered thus far ($t_{\rm E}$=0.155 +/- 0.005 d, $\theta_{\rm E}$=2.37 +/- 0.10 uas) and was caused by an Earth-mass object in the Galactic disk or a Neptune-mass planet in the Galactic bulge. OGLE-2017-BLG-0560 ($t_{\rm E}$=0.905 +/- 0.005 d, $\theta_{\rm E}$=38.7 +/- 1.6 uas) was caused by a Jupiter-mass planet in the Galactic disk or a brown dwarf in the bulge. We rule out stellar companions up to a distance of 6.0 and 3.9 au, respectively. We suggest that the lensing objects, whether located on very wide orbits or free-floating, may originate from the same physical mechanism. Although the sample of ultrashort microlensing events is small, these detections are consistent with low-mass wide-orbit or unbound planets being more common than stars in the Milky Way., Comment: accepted for publication in A&A, minor changes
Published: 2018
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8. OGLE-2017-BLG-0039: Microlensing Event with Light from the Lens Identified from Mass Measurement

Author: Han, C., Jung, Y. K., Udalski, A., Bond, I., Bozza, V., Albrow, M. D., Chung, S. -J., Gould, A., Hwang, K. -H., Kim, D., Lee, C. -U., Kim, H. -W., Ryu, Y. -H., Shin, I. -G., Yee, J. C., Shvartzvald, Y., Cha, S. -M., Kim, S. -L., Kim, D. -J., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Szymański, M. K., Mróz, P., Skowron, J., Poleski, R., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., and Yonehara, A.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present the analysis of the caustic-crossing binary microlensing event OGLE-2017-BLG-0039. Thanks to the very long duration of the event, with an event time scale $t_{\rm E}\sim 130$ days, the microlens parallax is precisely measured despite its small value of $\pie\sim 0.06$. The analysis of the well-resolved caustic crossings during both the source star's entrance and exit of the caustic yields the angular Einstein radius $\thetae\sim 0.6$~mas. The measured $\pie$ and $\thetae$ indicate that the lens is a binary composed of two stars with masses $\sim 1.0~M_\odot$ and $\sim 0.15~M_\odot$, and it is located at a distance of $\sim 6$ kpc. From the color and brightness of the lens estimated from the determined lens mass and distance, it is expected that $\sim 2/3$ of the $I$-band blended flux comes from the lens. Therefore, the event is a rare case of a bright lens event for which high-resolution follow-up observations can confirm the nature of the lens., Comment: 8 pages, 6 figures, 5 tables
Published: 2018
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9. OGLE-2017-BLG-0537: Microlensing Event with a Resolvable Lens in $\lesssim 5$ years from High-resolution Follow-up Observations

Author: Jung, Y. K., Han, C., Udalski, A., Gould, A., Albrow, M. D., Chung, S. -J., Hwang, K. -H., Lee, C. -U., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zang, W., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Kim, W. -T., Mróz, P., Poleski, R., Skowron, J., Szymański, M. K., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., and Pawlak, M.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present the analysis of the binary-lens microlensing event OGLE-2017-BLG-0537. The light curve of the event exhibits two strong caustic-crossing spikes among which the second caustic crossing was resolved by high-cadence surveys. It is found that the lens components with a mass ratio $\sim 0.5$ are separated in projection by $\sim 1.3\thetae$, where $\thetae$ is the angular Einstein radius. Analysis of the caustic-crossing part yields $\thetae=1.77\pm 0.16$~mas and a lens-source relative proper motion of $\mu =12.4\pm 1.1~{\rm mas}~{\rm yr}^{-1}$. The measured $\mu$ is the third highest value among the events with measured proper motions and $\sim 3$ times higher than the value of typical Galactic bulge events, making the event a strong candidate for follow-up observations to directly image the lens by separating it from the source. From the angular Einstein radius combined with the microlens parallax, it is estimated that the lens is composed of two main-sequence stars with masses $M_1\sim 0.4~M_\odot$ and $M_2\sim 0.2~M_\odot$ located at a distance of $D_{\rm L}\sim 1.2$~kpc. However, the physical lens parameters are not very secure due to the weak microlens-parallax signal, and thus we cross check the parameters by conducting a Bayesian analysis based on the measured Einstein radius and event timescale combined with the blending constraint. From this, we find that the physical parameters estimated from the Bayesian analysis are consistent with those based on the measured microlens parallax. Resolving the lens from the source can be done in about 5 years from high-resolution follow-up observations and this will provide a rare opportunity to test and refine the microlensing model., Comment: 9 pages, 6 figure, 2 tables
Published: 2018
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10. The KMTNet 2016 Data Release

Author: Kim, H. -W., Hwang, K. -H., Kim, D. -J., Albrow, M. D., Cha, S. -M., Chung, S. -J., Gould, A., Han, C., Jung, Y. K., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zang, W., and Zhu, W.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present Korea Microlensing Telescope Network (KMTNet) light curves for microlensing-event candidates for the 2016 season, which covers an area of 97 sq.deg observed at cadences ranging from Gamma=0.2/hr to Gamma=8/hr from three southern sites in Chile, South Africa, and Australia. These 2163 light curves are comprised of 1856 "clear microlensing" and 307 "possible microlensing" events (including 265 previously released from the K2 C9 field). The data policy is very similar to the one governing the 2015 release. The changes relative to 2015 in the algorithms to find and vet microlensing events are comprehensively described., Comment: 14 pages, 2 Figures, submitted to AAS Journals
Published: 2018

11. MOA-2015-BLG-337: A Planetary System with a Low-mass Brown Dwarf/Planetary Boundary Host, or a Brown Dwarf Binary

Author: Miyazaki, S., Sumi, T., Bennett, D. P., Gould, A., Udalski, A., Bond, I. A., Koshimoto, N., Nagakane, M., Rattenbury, N., Abe, F., Bhattacharya, A., Barry, R., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Li, M. C., Ling, C. H., Matsubara, Y., Matsuo, T., Muraki, Y., Ohnishi, K., Ranc, C., Saito, T., Sharan, A., Shibai, H., Suematsu, H., Suzuki, D., Sullivan, D. J., Tristram, P. J., Yamada, T., Yonehara, A., owski, S., Mr'oz, P., Pawlak, M., Poleski, R., Pietrukowicz, P., Skowron, J., Soszy'nski, I., Szyma'nski, M. K., Ulaczyk, K., Albrow, M. D., Chung, S. -J., Han, C., Jung, Y. K., Hwang, K. -H., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zang, W., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery and the analysis of the short timescale binary-lens microlensing event, MOA-2015-BLG-337. The lens system could be a planetary system with a very low mass host, around the brown dwarf/planetary mass boundary, or a brown dwarf binary. We found two competing models that explain the observed light curves with companion/host mass ratios of q~0.01 and ~0.17, respectively. From the measurement of finite source effects in the best-fit planetary model, we find a relatively small angular Einstein radius of theta_E ~ 0.03 mas which favors a low mass lens. We conduct a Bayesian analysis to obtain the probability distribution of the lens properties. The results for the planetary models strongly depend on the minimum mass, M_min, in the assumed mass function. In summary, there are two solutions of the lens system: (1) a brown dwarf/planetary mass boundary object orbited by a super-Neptune (the planetary model with M_min=0.001 M_sun) and (2) a brown dwarf binary (the binary model). If the planetary models is correct, this system can be one of a new class of planetary system, having a low host mass and also a planetary mass ratio (q <0.03) between the host and its companion. The discovery of the event is important for the study of planetary formation in very low mass objects. In addition, it is important to consider all viable solutions in these kinds of ambiguous events in order for the future comprehensive statistical analyses of planetary/binary microlensing events., Comment: 17 pages, 7 figures, Accepted for publication in AJ
Published: 2018
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12. OGLE-2017-BLG-0482Lb: A Microlensing Super-Earth Orbiting a Low-mass Host Star

Author: Han, C., Hirao, Y., Udalski, A., Lee, C. -U., Bozza, V., Gould, A., Abe, F., Barry, R., Bond, I. A., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Mróz, P., Poleski, R., Kozłowski, S., Soszyński, I., Pietrukowicz, P., Skowron, J., Szymańsk, M. K., Ulaczyk, K., Pawlak, M., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S. -J., Hwang, K. -H., Jung, Y. K., Kim, D., Kim, W. -T., Kim, H. -W., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zhu, W., Cha, S. -M., Kim, S. -L., Kim, D. -J., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of a planetary system in which a super-earth orbits a late M-dwarf host. The planetary system was found from the analysis of the microlensing event OGLE-2017-BLG-0482, wherein the planet signal appears as a short-term anomaly to the smooth lensing light curve produced by the host. Despite its weak signal and short duration, the planetary signal was firmly detected from the dense and continuous coverage by three microlensing surveys. We find a planet/host mass ratio of $q\sim 1.4\times 10^{-4}$. We measure the microlens parallax $\pi_{\rm E}$ from the long-term deviation in the observed lensing light curve, but the angular Einstein radius $\theta_{\rm E}$ cannot be measured because the source trajectory did not cross the planet-induced caustic. Using the measured event timescale and the microlens parallax, we find that the masses of the planet and the host are $M_{\rm p}=9.0_{-4.5}^{+9.0}\ M_\oplus$ and $M_{\rm host}=0.20_{-0.10}^{+0.20}\ M_\odot$, respectively, and the projected separation between them is $a_\perp=1.8_{-0.7}^{+0.6}$ au. The estimated distance to the lens is $D_{\rm L}=5.8_{-2.1}^{+1.8}$ kpc. The discovery of the planetary system demonstrates that microlensing provides an important method to detect low-mass planets orbiting low-mass stars., Comment: 10 pages, 10 figures, 2 tables
Published: 2018
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13. OGLE-2017-BLG-1522: A giant planet around a brown dwarf located in the Galactic bulge

Author: Jung, Y. K., Udalski, A., Gould, A., Ryu, Y. -H., Yee, J. C., Han, C., Albrow, M. D., Lee, C. -U., Kim, S. -L., Hwang, K. -H., Chung, S. -J., Shin, I. -G., Zhu, W., Cha, S. -M., Kim, D. -J., Lee, Y., Park, B. -G., Lee, D. -J., Kim, H. -W., Pogge, R. W., Szymański, M. K., Mróz, P., Poleski, R., Skowron, J., Pietrukowicz, P., Soszyński, I., Kozłowski, S., Ulaczyk, K., Pawlak, M., and Rybicki, K.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We report the discovery of a giant planet in the OGLE-2017-BLG-1522 microlensing event. The planetary perturbations were clearly identified by high-cadence survey experiments despite the relatively short event timescale of $t_{\rm E} \sim 7.5$ days. The Einstein radius is unusually small, $\theta_{\rm E} = 0.065\,$mas, implying that the lens system either has very low mass or lies much closer to the microlensed source than the Sun, or both. A Bayesian analysis yields component masses $(M_{\rm host}, M_{\rm planet})=(46_{-25}^{+79}, 0.75_{-0.40}^{+1.26})~M_{\rm J}$ and source-lens distance $D_{\rm LS} = 0.99_{-0.54}^{+0.91}~{\rm kpc}$, implying that this is a brown-dwarf/Jupiter system that probably lies in the Galactic bulge, a location that is also consistent with the relatively low lens-source relative proper motion $\mu = 3.2 \pm 0.5~{\rm mas}~{\rm yr^{-1}}$. The projected companion-host separation is $0.59_{-0.11}^{+0.12}~{\rm AU}$, indicating that the planet is placed beyond the snow line of the host, i.e., $a_{sl} \sim 0.12~{\rm AU}$. Planet formation scenarios combined with the small companion-host mass ratio $q \sim 0.016$ and separation suggest that the companion could be the first discovery of a giant planet that formed in a protoplanetary disk around a brown dwarf host., Comment: 20 pages, 6 figures
Published: 2018
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14. Spitzer Opens New Path to Break Classic Degeneracy for Jupiter-Mass Microlensing Planet OGLE-2017-BLG-1140Lb

Author: Novati, S. Calchi, Skowron, J., Jung, Y. K., Beichman, C., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Shvartzvald, Y., Yee, J. C., Zhu, W., Udalski, A., Szymański, M. K., Mróz, P., Poleski, R., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Hwang, K. -H., Ryu, Y. -H., Shin, I. -G., Zang, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We analyze the combined Spitzer and ground-based data for OGLE-2017-BLG-1140 and show that the event was generated by a Jupiter-class $(m_p\simeq 1.6\,M_{\rm jup})$ planet orbiting a mid-late M dwarf $(M\simeq 0.2\,M_\odot)$ that lies $D_{LS}\simeq 1.0\,\mathrm{kpc}$ in the foreground of the microlensed, Galactic-bar, source star. The planet-host projected separation is $a_\perp \simeq 1.0\,\mathrm{au}$, i.e., well-beyond the snow line. By measuring the source proper motion ${\mathbf{\mu}}_s$ from ongoing, long-term OGLE imaging, and combining this with the lens-source relative proper motion ${\mathbf{\mu}}_\mathrm{rel}$ derived from the microlensing solution, we show that the lens proper motion ${\mathbf{\mu}}_l={\mathbf{\mu}}_\mathrm{rel} + {\mathbf{\mu}}_s$ is consistent with the lens lying in the Galactic disk, although a bulge lens is not ruled out. We show that while the Spitzer and ground-based data are comparably well fitted by planetary (i.e., binary-lens, 2L1S) models and by binary-source (1L2S) models, the combination of Spitzer and ground-based data decisively favor the planetary model. This is a new channel to resolve the 2L1S/1L2S degeneracy, which can be difficult to break in some cases., Comment: Revised version accepted for publication in The Astronomical Journal
Published: 2018
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15. KMT-2016-BLG-0212: First KMTNet-Only Discovery of a Substellar Companion

Author: Hwang, K. -H., Kim, H. -W., Kim, D. -J., Gould, A., Albrow, M. D., Chung, S. -J., Han, C., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zang, W., Zhu, W., Cha, S. -M., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the analysis of KMT-2016-BLG-0212, a low flux-variation $(I_{\rm flux-var}\sim 20$) microlensing event, which is well-covered by high-cadence data from the three Korea Microlensing Telescope Network (KMTNet) telescopes. The event shows a short anomaly that is incompletely covered due to the brief visibility intervals that characterize the early microlensing season when the anomaly occurred. We show that the data are consistent with two classes of solutions, characterized respectively by low-mass brown-dwarf $(q=0.037)$ and sub-Neptune $(q<10^{-4})$ companions, respectively. Future high-resolution imaging should easily distinguish between these solutions., Comment: 9 pages, 8 figures
Published: 2018
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16. OGLE-2017-BLG-0373Lb: A Jovian Mass-Ratio Planet Exposes A New Accidental Microlensing Degeneracy

Author: Skowron, J., Ryu, Y. -H., Hwang, K. -H., Udalski, A., Mróz, P., Kozłowski, S., Soszyński, I., Pietrukowicz, P., Szymański, M. K., Poleski, R., Ulaczyk, K., Pawlak, M., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Jung, Y. K., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zang, W., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of microlensing planet OGLE-2017-BLG-0373Lb. We show that while the planet-host system has an unambiguous microlens topology, there are two geometries within this topology that fit the data equally well, which leads to a factor 2.5 difference in planet-host mass ratio, i.e., $q=1.5\times 10^{-3}$ vs. $q=0.6\times 10^{-3}$. We show that this is an "accidental degeneracy" in the sense that it is due to a gap in the data. We dub it "the caustic-chirality degeneracy". We trace the mathematical origins of this degeneracy, which should enable similar degenerate solutions to be easily located in the future. A Bayesian estimate, based on a Galactic model, yields a host mass $M=0.25^{+0.30}_{-0.15} M_\odot$ at a distance $D_L=5.9^{+1.3}_{-1.95}$ kpc. The lens-source relative proper motion is relatively fast, $\mu=9$ mas/yr, which implies that the host mass and distance can be determined by high-resolution imaging after about 10 years. The same observations could in principle resolve the discrete degeneracy in $q$, but this will be more challenging., Comment: 24 pages, 7 figures, 3 tables. Accepted for publication in Acta Astronomica. Light curves and callibration data are available on arXiv as Ancillary files and http://www.astrouw.edu.pl/~jskowron/ogle/ob170373/
Published: 2018
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17. OGLE-2017-BLG-0329L: A Microlensing Binary Characterized with Dramatically Enhanced Precision Using Data from Space-based Observations

Author: Han, C., Novati, S. Calchi, Udalski, A., Lee, C. -U., Gould, A., Bozza, V., Mróz, P., Pietrukowicz, P., Skowron, J., Szymański, M. K., Poleski, R., Soszyński, I., Kozłowski, S., Ulaczyk, K., Pawlak, M., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S. -J., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zang, W., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Kim, W. -T., Beichman, C., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Dominik, M., Helling, C., Hundertmark, M., Jørgensen, U. G., Longa-Peña, P., Lowry, S., Sajadian, S., Burgdorf, M. J., Campbell-White, J., Ciceri, S., Evans, D. F., Haikala, L. K., Hinse, T. C., Rahvar, S., Rabus, M., and Snodgrass, C.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Mass measurements of gravitational microlenses require one to determine the microlens parallax $\pie$, but precise $\pie$ measurement, in many cases, is hampered due to the subtlety of the microlens-parallax signal combined with the difficulty of distinguishing the signal from those induced by other higher-order effects. In this work, we present the analysis of the binary-lens event OGLE-2017-BLG-0329, for which $\pie$ is measured with a dramatically improved precision using additional data from space-based $Spitzer$ observations. We find that while the parallax model based on the ground-based data cannot be distinguished from a zero-$\pie$ model at 2$\sigma$ level, the addition of the $Spitzer$ data enables us to identify 2 classes of solutions, each composed of a pair of solutions according to the well-known ecliptic degeneracy. It is found that the space-based data reduce the measurement uncertainties of the north and east components of the microlens-parallax vector $\pivec_{\rm E}$ by factors $\sim 18$ and $\sim 4$, respectively. With the measured microlens parallax combined with the angular Einstein radius measured from the resolved caustic crossings, we find that the lens is composed of a binary with components masses of either $(M_1,M_2)\sim (1.1,0.8)\ M_\odot$ or $\sim (0.4,0.3)\ M_\odot$ according to the two solution classes. The first solution is significantly favored but the second cannot be securely ruled out based on the microlensing data alone. However, the degeneracy can be resolved from adaptive optics observations taken $\sim 10$ years after the event., Comment: 9 pages, 4 tables, 6 figures
Published: 2018
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18. OGLE-2016-BLG-1266: A Probable Brown-Dwarf/Planet Binary at the Deuterium Fusion Limit

Author: Albrow, M. D., Yee, J. C., Udalski, A., Novati, S. Calchi, Carey, S., Henderson, C. B., Beichman, C., Bryden, G., Gaudi, B. S., Shvartzvald, Y., Szymanśki, M. K., Mroź, P., Skowron, J., Poleski, R., Soszynśki, I., Kozlowski, S., Pietrukowicz, ., Ulaczyk, K., Pawlak, M., Chung, S. -J., Gould, A., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery, via the microlensing method, of a new very-low-mass binary system. By combining measurements from Earth and from the Spitzer telescope in Earth-trailing orbit, we are able to measure the microlensing parallax of the event, and find that the lens likely consists of an $(12.0 \pm 0.6) M_{\rm J}$ + $(15.7 \pm 1.5) M_{\rm J}$ super-Jupiter / brown-dwarf pair. The binary is located at a distance of $(3.08 \pm 0.18)$ kpc in the Galactic Plane, and the components have a projected separation of $(0.43 \pm 0.03)$ AU. Two alternative solutions with much lower likelihoods are also discussed, an 8- and 6-$M_{\rm J}$ model and a 90- and 70-$M_{\rm J}$ model. Although disfavored at the 3-$\sigma$ and 5-$\sigma$ levels, these alternatives cannot be rejected entirely. We show how the more-massive of these models could be tested with future direct imaging., Comment: 23 pages, 7 figures, submitted to AAS Journals
Published: 2018
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19. OGLE-2017-BLG-1130: The First Binary Gravitational Microlens Detected From Spitzer Only

Author: Wang, Tianshu, Novati, S. Calchi, Udalski, A., Gould, A., Mao, Shude, Zang, W., Beichman, C., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Shvartzvald, Y., Yee, J. C., Mroz, P., Poleski, R., Skowron, J., Szymanski, M. K., Soszynski, I., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We analyze the binary gravitational microlensing event OGLE-2017-BLG-1130 (mass ratio q~0.45), the first published case in which the binary anomaly was only detected by the Spitzer Space Telescope. This event provides strong evidence that some binary signals can be missed by observations from the ground alone but detected by Spitzer. We therefore invert the normal procedure, first finding the lens parameters by fitting the space-based data and then measuring the microlensing parallax using ground-based observations. We also show that the normal four-fold space-based degeneracy in the single-lens case can become a weak eight-fold degeneracy in binary-lens events. Although this degeneracy is resolved in event OGLE-2017-BLG-1130, it might persist in other events., Comment: 14 pages, 5 figures
Published: 2018
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20. OGLE-2017-BLG-1434Lb: Eighth q < 1 * 10^-4 Mass-Ratio Microlens Planet Confirms Turnover in Planet Mass-Ratio Function

Author: Udalski, A., Ryu, Y. -H., Sajadian, S., Gould, A., Mróz, P., Poleski, R., Szymański, M. K., Skowron, J., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zang, W., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Bozza, V., Dominik, M., Helling, C., Hundertmark, M., Jørgensen, U. G., Longa-Peña, P., Lowry, S., Burgdorf, M., Campbell-White, J., Ciceri, S., Evans, D., Jaimes, R. Figuera, Fujii, Y. I., Haikala, L. K., Henning, T., Hinse, T. C., Mancini, L., Peixinho, N., Rahvar, S., Rabus, M., Skottfelt, J., Snodgrass, C., Southworth, J., and von Essen, C.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of a cold Super-Earth planet (m_p=4.4 +/- 0.5 M_Earth) orbiting a low-mass (M=0.23 +/- 0.03 M_Sun) M dwarf at projected separation a_perp = 1.18 +/- 0.10 AU, i.e., about 1.9 times the snow line. The system is quite nearby for a microlensing planet, D_Lens = 0.86 +/- 0.09 kpc. Indeed, it was the large lens-source relative parallax pi_rel=1.0 mas (combined with the low mass M) that gave rise to the large, and thus well-measured, "microlens parallax" that enabled these precise measurements. OGLE-2017-BLG-1434Lb is the eighth microlensing planet with planet-host mass ratio q < 1 * 10^-4. We apply a new planet-detection sensitivity method, which is a variant of "V/V_max", to seven of these eight planets to derive the mass-ratio function in this regime. We find dN/d(ln q) ~ q^p, with p = 1.05 (+0.78,-0.68), which confirms the "turnover" in the mass function found by Suzuki et al. relative to the power law of opposite sign n = -0.93 +/- 0.13 at higher mass ratios q >~ 2 * 10^-4. We combine our result with that of Suzuki et al. to obtain p = 0.73 (+0.42,-0.34)., Comment: 53 pages, 16 figures
Published: 2018
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21. The KMTNet/K2-C9 (Kepler) Data Release

Author: Kim, H. -W., Hwang, K. -H., Kim, D. -J., Albrow, M. D., Cha, S. -M., Chung, S. -J., Gould, A., Han, C., Jung, Y. K., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zang, W., and Zhu, W.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present Korea Microlensing Telescope Network (KMTNet) light curves for microlensing-event candidates in the Kepler K2 C9 field having peaks within 3 effective timescales of the Kepler observations. These include 181 "clear microlensing" and 84 "possible microlensing" events found by the KMTNet event finder, plus 56 other events found by OGLE and/or MOA that were not found by KMTNet. All data for the first two classes are immediately available for public use without restriction., Comment: Submitted AAS Journals, 10 pages, 1 Figure. Lightcurves are available at http://kmtnet.kasi.re.kr/ulens/
Published: 2018
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22. Spitzer Microlensing Parallax for OGLE-2016-BLG-1067: a sub-Jupiter Orbiting an M-dwarf in the Disk

Author: Novati, S. Calchi, Suzuki, D., Udalski, A., Gould, A., Shvartzvald, Y., Bozza, V., Bennett, D. P., Beichman, C., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Yee, J. C., Zhu, W., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Bond, I. A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Tristram, P. J., Yamada, T., Yonehara, A., Mróz, P., Poleski, R., Skowron, J., Szymański, M. K., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Zang, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of a sub-Jupiter mass planet orbiting beyond the snow line of an M-dwarf most likely in the Galactic disk as part of the joint Spitzer and ground-based monitoring of microlensing planetary anomalies toward the Galactic bulge. The microlensing parameters are strongly constrained by the light curve modeling and in particular by the Spitzer-based measurement of the microlens parallax, $\pi_\mathrm{E}$. However, in contrast to many planetary microlensing events, there are no caustic crossings, so the angular Einstein radius, $\theta_\mathrm{E}$ has only an upper limit based on the light curve modeling alone. Additionally, the analysis leads us to identify 8 degenerate configurations: the four-fold microlensing parallax degeneracy being doubled by a degeneracy in the caustic structure present at the level of the ground-based solutions. To pinpoint the physical parameters, and at the same time to break the parallax degeneracy, we make use of a series of arguments: the $\chi^2$ hierarchy, the Rich argument, and a prior Galactic model. The preferred configuration is for a host at $D_L=3.73_{-0.67}^{+0.66}~\mathrm{kpc}$ with mass $M_\mathrm{L}=0.30_{-0.12}^{+0.15}~\mathrm{M_\odot}$, orbited by a Saturn-like planet with $M_\mathrm{planet}=0.43_{-0.17}^{+0.21}~\mathrm{M_\mathrm{Jup}}$ at projected separation $a_\perp = 1.70_{-0.39}^{+0.38}~\mathrm{au}$, about 2.1 times beyond the system snow line. Therefore, it adds to the growing population of sub-Jupiter planets orbiting near or beyond the snow line of M-dwarfs discovered by microlensing. Based on the rules of the real-time protocol for the selection of events to be followed up with Spitzer, this planet will not enter the sample for measuring the Galactic distribution of planets., Comment: Submitted to AAS Journals
Published: 2018
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23. Recent advances in drug delivery systems for glaucoma treatment

Author: Patel, K.D., Barrios Silva, L., Park, Y., Shakouri, T., Keskin-Erdogan, Z., Sawadkar, P., Cho, K.J., Knowles, J.C., Chau, D.Y.S., and Kim, H.-W.
Published: 2022
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24. OGLE-2016-BLG-1045: A Test of Cheap Space-Based Microlens Parallaxes

Author: Shin, I. -G., Udalski, A., Yee, J. C., Novati, S. Calchi, Christie, G., Poleski, R., Mróz, P., Skowron, J., Szymański, M. K., Soszyński, I., Pietrukowicz, P., Kozłowski, S., Ulaczyk, K., Pawlak, M., Natusch, T., Pogge, R. W., Gould, A., Han, C., Albrow, M. D., Chung, S. -J., Hwang, K. -H., Ryu, Y. -H., Jung, Y. K., Zhu, W., Lee, C. -U., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, Y., Lee, D. -J., Park, B. -G., Beichman, C., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., and Shvartzvald, Y.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Microlensing is a powerful and unique technique to probe isolated objects in the Galaxy. To study the characteristics of these interesting objects based on the microlensing method, measurement of the microlens parallax is required to determine the properties of the lens. Of the various methods to measure microlens parallax, the most robust way is to make simultaneous ground- and space-based observations, i.e., by measuring the space-based microlens parallax. However, space-based campaigns usually require "expensive" resources. Gould & Yee (2012) proposed an idea called the "cheap space-based microlens parallax" that can measure the lens-parallax using only $2$ or $3$ space-based observations of high-magnification events. This cost-effective observation strategy to measure microlens parallaxes could be used by space-borne telescopes to build a complete sample for studying isolated objects. This would enable a direct measurement of the mass function including both extremely low-mass objects and high-mass stellar remnants. However, to adopt this idea requires a test to check how it would work in actual situations. Thus, we present the first practical test of the idea using the high-magnification microlensing event OGLE-2016-BLG-1045, for which a subset of Spitzer observations fortuitously duplicate the prescription of Gould & Yee (2012). From the test, we confirm that the measurement of the lens-parallax adopting this idea has sufficient accuracy to determine the physical properties of the isolated lens., Comment: 7 Figures and 2 Tables, Accepted for publication in the ApJ
Published: 2017
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25. A Neptune-mass Free-floating Planet Candidate Discovered by Microlensing Surveys

Author: Mroz, Przemek, Ryu, Y. -H., Skowron, J., Udalski, A., Gould, A., Szymanski, M. K., Soszynski, I., Poleski, R., Pietrukowicz, P., Kozlowski, S., Pawlak, M., Ulaczyk, K., Albrow, M. D., Chung, S. -J., Jung, Y. K., Han, C., Hwang, K. -H., Shin, I. -G., Yee, J. C., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Current microlensing surveys are sensitive to free-floating planets down to Earth-mass objects. All published microlensing events attributed to unbound planets were identified based on their short timescale (below two days), but lacked an angular Einstein radius measurement (and hence lacked a significant constraint on the lens mass). Here, we present the discovery of a Neptune-mass free-floating planet candidate in the ultrashort ($t_{\rm E}=0.320\pm0.003$ days) microlensing event OGLE-2016-BLG-1540. The event exhibited strong finite-source effects, which allowed us to measure its angular Einstein radius of $\theta_{\rm E}=9.2\pm0.5\,\mu$as. There remains, however, a degeneracy between the lens mass and distance. The combination of the source proper motion and source-lens relative proper motion measurements favors a Neptune-mass lens located in the Galactic disk. However, we cannot rule out that the lens is a Saturn-mass object belonging to the bulge population. We exclude stellar companions up to 15 au., Comment: accepted to AJ
Published: 2017
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26. OGLE-2015-BLG-1459L: The Challenges of Exo-Moon Microlensing

Author: Hwang, K. -H., Udalski, A., Bond, I. A., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Yee, J. C., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Pawlak, M., Poleski, R., Szymański, M. K., Skowron, J., Soszyński, I., Mróz, P., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., and Yonehara, A.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We show that dense OGLE and KMTNet $I$-band survey data require four bodies (sources plus lenses) to explain the microlensing light curve of OGLE-2015-BLG-1459. However, these can equally well consist of three lenses and one source (3L1S), two lenses and two sources (2L2S) or one lens and three sources (1L3S). In the 3L1S and 2L2S interpretations, the host is a brown dwarf and the dominant companion is a Neptune-class planet, with the third body (in the 3L1S case) being a Mars-class object that could have been a moon of the planet. In the 1L3S solution, the light curve anomalies are explained by a tight (five stellar radii) low-luminosity binary source that is offset from the principal source of the event by $\sim 0.17\,\au$. These degeneracies are resolved in favor of the 1L3S solution by color effects derived from comparison to MOA data, which are taken in a slightly different ($R/I$) passband. To enable current and future ($WFIRST$) surveys to routinely characterize exomoons and distinguish among such exotic systems requires an observing strategy that includes both a cadence faster than 9 min$^{-1}$ and observations in a second band on a similar timescale., Comment: 29 pages, 8 figures, accepted for publication in AJ
Published: 2017
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27. OGLE-2016-BLG-1190Lb: First Spitzer Bulge Planet Lies Near the Planet/Brown-Dwarf Boundary

Author: Ryu, Y. -H., Yee, J. C., Udalski, A., Bond, I. A., Shvartzvald, Y., Zang, W., Jaimes, R. Figuera, Jorgensen, U. G., Zhu, W., Huang, C. X., Jung, Y. K., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Hwang, K. -H., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Novati, S. Calchi, Carey, S., Henderson, C. B., Beichman, C., Gaudi, B. S., Mróz, P., Poleski, R., Skowron, J., Szymanski, M. K., Soszynski, I., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Bryden, G., Howell, S. B., Jacklin, S., Penny, M. T., Mao, S., Fouque, Pascal, Wang, T., Street, R. A., Tsapras, Y., Hundertmark, M., Bachelet, E., Dominik, M., Li, Z., Cross, S., Cassan, A., Horne, K., Schmidt, R., Wambsganss, J., Ment, S. K., Maoz, D., Snodgrass, C., Steele, I. A., Bozza, V., Burgdorf, M. J., Ciceri, S., D'Ago, G., Evans, D. F., Hinse, T. C., Kerins, E., Kokotanekova, R., Longa, P., MacKenzie, J., Popovas, A., Rabus, M., Rahvar, S., Sejadian, S., Skottfelt, J., Southworth, J., and von Essen, C.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of OGLE-2016-BLG-1190Lb, which is likely to be the first Spitzer microlensing planet in the Galactic bulge/bar, an assignation that can be confirmed by two epochs of high-resolution imaging of the combined source-lens baseline object. The planet's mass M_p= 13.4+-0.9 M_J places it right at the deuterium burning limit, i.e., the conventional boundary between "planets" and "brown dwarfs". Its existence raises the question of whether such objects are really "planets" (formed within the disks of their hosts) or "failed stars" (low mass objects formed by gas fragmentation). This question may ultimately be addressed by comparing disk and bulge/bar planets, which is a goal of the Spitzer microlens program. The host is a G dwarf M_host = 0.89+-0.07 M_sun and the planet has a semi-major axis a~2.0 AU. We use Kepler K2 Campaign 9 microlensing data to break the lens-mass degeneracy that generically impacts parallax solutions from Earth-Spitzer observations alone, which is the first successful application of this approach. The microlensing data, derived primarily from near-continuous, ultra-dense survey observations from OGLE, MOA, and three KMTNet telescopes, contain more orbital information than for any previous microlensing planet, but not quite enough to accurately specify the full orbit. However, these data do permit the first rigorous test of microlensing orbital-motion measurements, which are typically derived from data taken over <1% of an orbital period., Comment: 63 pages, 13 figures, 7 tables, AJ, in press
Published: 2017
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28. OGLE-2016-BLG-0613LABb: A Microlensing Planet in a Binary System

Author: Han, C., Udalski, A., Gould, A., Lee, C. -U., Shvartzvald, Y., Zang, W. C., Mao, S., Kozłowski, S., Albrow, M. D., Chung, S. -J., Hwang, K. -H., Jung, Y. K., Kim, D., Kim, H. -W., Ryu, Y. -H., Shin, I. -G., Yee, J. C., Zhu, W., Cha, S. -M., Kim, S. -L., Kim, D. -J., Lee, Y., Park, B. -G., Skowron, J., Mróz, P., Pietrukowicz, P., Poleski, R., Szymański, M. K., Soszyński, I., Ulaczyk, K., Beichman, M. Pawlak C., Bryden, G., Novati, S. Calchi, Gaudi, B. S., Henderson, C. B., Howell, S. B., Jacklin, S., Penny, M. T., Fouqué, P., and Wang, T. S.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the analysis of OGLE-2016-BLG-0613, for which the lensing light curve appears to be that of a typical binary-lens event with two caustic spikes but with a discontinuous feature on the trough between the spikes. We find that the discontinuous feature was produced by a planetary companion to the binary lens. We find 4 degenerate triple-lens solution classes, each composed of a pair of solutions according to the well-known wide/close planetary degeneracy. One of these solution classes is excluded due to its relatively poor fit. For the remaining three pairs of solutions, the most-likely primary mass is about $M_1\sim 0.7\,M_\odot$ while the planet is a super-Jupiter. In all cases the system lies in the Galactic disk, about half-way toward the Galactic bulge. However, in one of these three solution classes, the secondary of the binary system is a low-mass brown dwarf, with relative mass ratios (1 : 0.03 : 0.003), while in the two others the masses of the binary components are comparable. These two possibilities can be distinguished in about 2024 when the measured lens-source relative proper motion will permit separate resolution of the lens and source., Comment: 14 pages, 9 figures
Published: 2017
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29. OGLE-2017-BLG-0173Lb: Low Mass-Ratio Planet in a 'Hollywood' Microlensing Event

Author: Hwang, K. -H., Udalski, A., Shvartzvald, Y., Ryu, Y. -H., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Jung, Y. K., Shin, I. -G., Yee, J. C., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Skowron, J., Mroz, P., Poleski, R., Kozlowski, S., Soszynski, I., Pietrukowicz, P., Szymanski, M. K., Ulaczyk, K., Pawlak, M., Bryden, G., Beichman, C., Novati, S. Calchi, Gaudi, B. S., Henderson, C. B., Jacklin, S., and Penny, M. T.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present microlensing planet OGLE-2017-BLG-0173Lb, with planet-host mass ratio either $q\simeq 2.5\times 10^{-5}$ or $q\simeq 6.5\times 10^{-5}$, the lowest or among the lowest ever detected. The planetary perturbation is strongly detected, $\Delta\chi^2\sim 10,000$, because it arises from a bright (therefore, large) source passing over and enveloping the planetary caustic: a so-called "Hollywood" event. The factor $\sim 2.5$ offset in $q$ arises because of a previously unrecognized discrete degeneracy between Hollywood events in which the caustic is fully enveloped and those in which only one flank is enveloped, which we dub "Cannae" and "von Schlieffen", respectively. This degeneracy is "accidental" in that it arises from gaps in the data. Nevertheless, the fact that it appears in a $\Delta\chi^2=10,000$ planetary anomaly is striking. We present a simple formalism to estimate the sensitivity of other Hollywood events to planets and show that they can lead to detections close to, but perhaps not quite reaching, the Earth/Sun mass ratio of $3\times 10^{-6}$. This formalism also enables an analytic understanding of the factor $\sim 2.5$ offset in $q$ between the Cannae and von Schlieffen solutions. The Bayesian estimates for the host-mass, system distance, and planet-host projected separation are $M=0.39^{+0.40}_{-0.24}\,M_\odot$, $D_L=4.8^{+1.5}_{-1.8}\,\kpc$, and $a_\perp=3.8\pm 1.6\,\au$. The two estimates of the planet mass are $m_p=3.3^{+3.8}_{-2.1}\,M_\oplus$ and $m_p=8^{+11}_{-6}\,M_\oplus$. The measured lens-source relative proper motion $\mu=6\,\masyr$ will permit imaging of the lens in about 15 years or at first light on adaptive-optics imagers on next-generation telescopes. These will allow to measure the host mass but probably cannot resolve the planet-host mass-ratio degeneracy., Comment: 30 pages, 9 figures, AJ in press
Published: 2017
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30. Ground-based parallax confirmed by Spitzer: binary microlensing event MOA-2015-BLG-020

Author: Wang, Tianshu, Zhu, Wei, Mao, Shude, Bond, I. A., Gould, A., Udalski, A., Sumi, T., Bozza, V., Ranc, C., Cassan, A., Yee, J. C., Han, C., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Rattenbury, N., Saito, To., Sharan, A., Shibai, H., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Pawlak, M., Pietrukowicz, P., Poleski, R., Skowron, J., Soszynski, I., KozLowski, S., Mroz, P., Ulaczyk, K., Szymanski, M. K., Beichman, C., Bryden, G., Novati, S. Calchi, Carey, S., Fausnaugh, M., Gaudi, B. S., Henderson, C. B., Shvartzvald, Y., Wibking, B., Albrow, M. D., Chung, S. -J., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Yee, Y., Park, B. -G., Pogge, R. W., Street, R. A., Tsapras, Y., Hundertmark, M., Bachelet, E., Dominik, M., Horne, K., Jaimes, R. Figuera, Wambsganss, J., Bramich, D. M., Schmidt, R., Snodgrass, C., Steele, I. A., and Menzies, J.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present the analysis of the binary gravitational microlensing event MOA-2015-BLG-020. The event has a fairly long timescale (about 63 days) and thus the light curve deviates significantly from the lensing model that is based on the rectilinear lens-source relative motion. This enables us to measure the microlensing parallax through the annual parallax effect. The microlensing parallax parameters constrained by the ground-based data are confirmed by the Spitzer observations through the satellite parallax method. By additionally measuring the angular Einstein radius from the analysis of the resolved caustic crossing, the physical parameters of the lens are determined. It is found that the binary lens is composed of two dwarf stars with masses $M_1 = 0.606 \pm 0.028M_\odot$ and $M_2 = 0.125 \pm 0.006M_\odot$ in the Galactic disk. Assuming the source star is at the same distance as the bulge red clump stars, we find the lens is at a distance $D_L = 2.44 \pm 0.10 kpc$. In the end, we provide a summary and short discussion of all published microlensing events in which the annual parallax effect is confirmed by other independent observations., Comment: 16 pages, 5 figures
Published: 2017
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31. OGLE-2016-BLG-0693LB: Probing the Brown Dwarf Desert with Microlensing

Author: Ryu, Y. -H., Udalski, A., Yee, J. C., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Hwang, K. -H., Jung, Y. K., Shin, I. -G., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, Y., Park, B. -G., Pogge, R. W., Pietrukowicz, P., Kozlowski, S., Poleski, R., Skowron, J., Mroz, P., Szymanski, M. K., Soszynski, I., Pawlak, M., and Ulaczyk, K.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present an analysis of microlensing event OGLE-2016-BLG-0693, based on the survey-only microlensing observations by the OGLE and KMTNet groups. In order to analyze the light curve, we consider the effects of parallax, orbital motion, and baseline slope, and also refine the result using a Galactic model prior. From the microlensing analysis, we find that the event is a binary composed of a low-mass brown dwarf 49+-20 M_J companion and a K- or G-dwarf host, which lies at a distance 5.0+-0.6 kpc toward the Galactic bulge. The projected separation between the brown dwarf and its host star is less than 5 AU, and thus it is likely that the brown dwarf companion is located in the brown dwarf desert., Comment: 27 pages, 7 figures, 4 tables, Accepted for publication in AJ
Published: 2017
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32. OGLE-2016-BLG-0168 Binary Microlensing Event: Prediction and Confirmation of the Micorlens Parallax Effect from Space-based Observation

Author: Shin, I. -G., Udalski, A., Yee, J. C., Novati, S. Calchi, Han, C., Skowron, J., Mróz, P., Soszyński, I., Poleski, R., Szymański, M. K., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Albrow, M. D., Gould, A., Chung, S. -J., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, Y., Park, B. -G., Pogge, R. W., Beichman, C., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., and Shvartzvald, Y.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: The microlens parallax is a crucial observable for conclusively identifying the nature of lens systems in microlensing events containing or composed of faint (even dark) astronomical objects such as planets, neutron stars, brown dwarfs, and black holes. With the commencement of a new era of microlensing in collaboration with space-based observations, the microlens parallax can be routinely measured. In addition, space-based observations can provide opportunities to verify the microlens parallax measured from ground-only observations and to find a unique solution of the lensing lightcurve analysis. However, since most space-based observations cannot cover the full lightcurves of lensing events, it is also necessary to verify the reliability of the information extracted from fragmentary space-based lightcurves. We conduct a test based on the microlensing event OGLE-2016-BLG-0168 created by a binary lens system consisting of almost equal mass M-dwarf stars to demonstrate that it is possible to verify the microlens parallax and to resolve degeneracies by using the space-based lightcurve even though the observations are fragmentary. Since space-based observatories will frequently produce fragmentary lightcurves due to their short observing windows, the methodology of this test will be useful for next-generation microlensing experiments that combine space-based and ground-based collaboration., Comment: 9 pages, 5 figures, 3 tables, submitted in ApJ
Published: 2017
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33. An Earth-mass Planet in a 1-AU Orbit around an Ultracool Dwarf

Author: Shvartzvald, Y., Yee, J. C., Novati, S. Calchi, Gould, A., Lee, C. -U., Beichman, C., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Zhu, W., Albrow, M. D., Cha, S. -M., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, Y., Park, B. -G., Pogge, R. W., Ryu, Y. -H., and Shin, I. -G.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We combine $Spitzer$ and ground-based KMTNet microlensing observations to identify and precisely measure an Earth-mass ($1.43^{+0.45}_{-0.32} M_\oplus$) planet OGLE-2016-BLG-1195Lb at $1.16^{+0.16}_{-0.13}$ AU orbiting a $0.078^{+0.016}_{-0.012} M_\odot$ ultracool dwarf. This is the lowest-mass microlensing planet to date. At $3.91^{+0.42}_{-0.46}$ kpc, it is the third consecutive case among the $Spitzer$ "Galactic distribution" planets toward the Galactic bulge that lies in the Galactic disk as opposed to the bulge itself, hinting at a skewed distribution of planets. Together with previous microlensing discoveries, the seven Earth-size planets orbiting the ultracool dwarf TRAPPIST-1, and the detection of disks around young brown dwarfs, OGLE-2016-BLG-1195Lb suggests that such planets might be common around ultracool dwarfs. It therefore sheds light on the formation of both ultracool dwarfs and planetary systems at the limit of low-mass protoplanetary disks., Comment: 19 pages, 4 figures, 2 tables. Main difference from previous version is new CMD, since previous patch was too small to locate clump properly. Accepted for publication in ApJL
Published: 2017
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34. Korea Microlensing Telescope Network Microlensing Events from 2015: Event-Finding Algorithm, Vetting, and Photometry

Author: Kim, D. -J., Kim, H. -W., Hwang, K. -H., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Yee, J. C., Zhu, W., Cha, S. -M., Kim, S. -L., Lee, C. -U., Lee, Y., Park, B. -G., and Pogge, R. W.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present microlensing events in the 2015 Korea Microlensing Telescope Network (KMTNet) data and our procedure for identifying these events. In particular, candidates were detected with a novel "completed event" microlensing event-finder algorithm. The algorithm works by making linear fits to a (t0,teff,u0) grid of point-lens microlensing models. This approach is rendered computationally efficient by restricting u0 to just two values (0 and 1), which we show is quite adequate. The implementation presented here is specifically tailored to the commission-year character of the 2015 data, but the algorithm is quite general and has already been applied to a completely different (non-KMTNet) data set. We outline expected improvements for 2016 and future KMTNet data. The light curves of the 660 "clear microlensing" and 182 "possible microlensing" events that were found in 2015 are presented along with our policy for their public release., Comment: AJ, in press, 39 pages, 12 figures. Lightcurves at http://kmtnet.kasi.re.kr/~ulens/event/2015/ . See Section 5 for data policy
Published: 2017
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35. OGLE-2015-BLG-1482L: the first isolated low-mass microlens in the Galactic bulge

Author: Chung, S. -J., Zhu, W., Udalski, A., Lee, C. -U., Ryu, Y. -H., Jung, Y. K., Shin, I. -G., Yee, J. C., Hwang, K. -H., Gould, A., Albrow, M., Cha, S. -M., Han, C., Kim, D. -J., Kim, H. -W., Kim, S. -L., Kim, Y. -H., Lee, Y., Park, B. -G., Pogge, R. W., Poleski, R., Mróz, P., Pietrukowicz, P., Skowron, J., Szymański, M. K., Soszyński, I., Kozłowski, S., Ulaczyk, K., Pawlak, M., Beichman, C., Bryden, G., Novati, S. Calchi, Carey, S., Fausnaugh, M., Gaudi, B. S., Henderson, Calen B., Shvartzvald, Y., and Wibking, B.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We analyze the single microlensing event OGLE-2015-BLG-1482 simultaneously observed from two ground-based surveys and from \textit{Spitzer}. The \textit{Spitzer} data exhibit finite-source effects due to the passage of the lens close to or directly over the surface of the source star as seen from \textit{Spitzer}. Such finite-source effects generally yield measurements of the angular Einstein radius, which when combined with the microlens parallax derived from a comparison between the ground-based and the \textit{Spitzer} light curves, yields the lens mass and lens-source relative parallax. From this analysis, we find that the lens of OGLE-2015-BLG-1482 is a very low-mass star with the mass $0.10 \pm 0.02 \ M_\odot$ or a brown dwarf with the mass $55\pm 9 \ M_{J}$, which are respectively located at $D_{\rm LS} = 0.80 \pm 0.19\ \textrm{kpc}$ and $ D_{\rm LS} = 0.54 \pm 0.08\ \textrm{kpc}$, and thus it is the first isolated low-mass microlens that has been decisively located in the Galactic bulge. The fundamental reason for the degeneracy is that the finite-source effect is seen only in a single data point from \textit{Spitzer} and this single data point gives rise to two solutions for $\rho$. Because the $\rho$ degeneracy can be resolved only by relatively high cadence observations around the peak, while the \textit{Spitzer} cadence is typically $\sim 1\,{\rm day}^{-1}$, we expect that events for which the finite-source effect is seen only in the \textit{Spitzer} data may frequently exhibit this $\rho$ degeneracy. For OGLE-2015-BLG-1482, the relative proper motion of the lens and source for the low-mass star is $\mu_{\rm rel} = 9.0 \pm 1.9\ \textrm{mas yr$^{-1}$}$, while for the brown dwarf it is $5.5 \pm 0.5\ \textrm{mas yr$^{-1}$}$. Hence, the degeneracy can be resolved within $\sim 10\ \rm yrs$ from direct lens imaging by using next-generation instruments with high spatial resolution., Comment: 18 pages, 4 figures, accepted for publication in ApJ
Published: 2017
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36. Toward a Galactic Distribution of Planets. I. Methodology & Planet Sensitivities of the 2015 High-Cadence Spitzer Microlens Sample

Author: Zhu, Wei, Udalski, A., Novati, S. Calchi, Chung, S. -J., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Gould, A., Lee, C. -U., Albrow, M. D., Yee, J. C., Han, C., Hwang, K. -H., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Kim, Y. -H., Lee, Y., Park, B. -G., Pogge, R., Poleski, R., Skowron, J., Mroz, P., Szymanski, M. K., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Pawlak, M., Beichman, C., Bryden, G., Carey, S., Fausnaugh, M., Gaudi, B. S., Henderson, C., Shvartzvald, Y., and Wibking, B.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We analyze an ensemble of microlensing events from the 2015 Spitzer microlensing campaign, all of which were densely monitored by ground-based high-cadence survey teams. The simultaneous observations from Spitzer and the ground yield measurements of the microlensing parallax vector $\pi_{\rm E}$, from which compact constraints on the microlens properties are derived, including $\lesssim$25\% uncertainties on the lens mass and distance. With the current sample, we demonstrate that the majority of microlenses are indeed in the mass range of M dwarfs. The planet sensitivities of all 41 events in the sample are calculated, from which we provide constraints on the planet distribution function. In particular, assuming a planet distribution function that is uniform in $\log{q}$, where $q$ is the planet-to-star mass ratio, we find a $95\%$ upper limit on the fraction of stars that host typical microlensing planets of 49\%, which is consistent with previous studies. Based on this planet-free sample, we develop the methodology to statistically study the Galactic distribution of planets using microlensing parallax measurements. Under the assumption that the planet distributions are the same in the bulge as in the disk, we predict that $\sim$1/3 of all planet detections from the microlensing campaigns with Spitzer should be in the bulge. This prediction will be tested with a much larger sample, and deviations from it can be used to constrain the abundance of planets in the bulge relative to the disk., Comment: published on Astronomical Journal
Published: 2017
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37. A Vibration-Based Strategy for Structural Health Monitoring with Cosine Similarity

Author: Min, C. H., Cho, S. G., Oh, J. W., Kim, H. W., Kim, B. M., Oberst, Sebastian, editor, Halkon, Benjamin, editor, Ji, Jinchen, editor, and Brown, Terry, editor
Published: 2021
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38. AB0665 FACTORS INFLUENCING ATTAINMENT OF LOW DISEASE ACTIVITY IN RHEUMATOID ARTHRITIS PATIENTS DEVIATING FROM TREAT-TO-TARGET STRATEGY

Author: Song, Y. J., primary, Cho, S. K., additional, Han, J. Y., additional, Lee, S. B., additional, Park, H. R., additional, Kim, H. W., additional, Nam, E., additional, Lee, S. W., additional, and Sung, Y. K., additional
Published: 2024
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39. Chapter 7. Hygienic issues associated with waste to food

Author: Cho, S.J., primary, Kim, H.-W., additional, Kim, H.S., additional, Ham, Y.-K., additional, Shin, J., additional, and Shin, S.G., additional
Published: 2022
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40. P761 Clinical efficacy and durability of subcutaneous infliximab in patients with moderate-to-severe inflammatory bowel disease : a real-world data from a Korean multicentre prospective cohort study

Author: Kim, K, primary, Hong, S N H, additional, Kang, S B K, additional, Lee, K M, additional, Koo, J S K, additional, Jung, Y, additional, Lee, B J L, additional, Yoon, H Y, additional, Kim, H W, additional, Lim, Y J, additional, Lee, H S, additional, Lee, Y J, additional, Lee, J, additional, Lee, C K, additional, Moon, J M, additional, Shin, S Y, additional, Seo, J, additional, and Choi, C H, additional
Published: 2024
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41. P513 Clinical efficacy and durability of subcutaneous infliximab in patients with inflammatory bowel disease after switching from intravenous in a Korean multicenter prospective cohort study

Author: Kim, K, primary, Hong, S N, additional, Kang, S B, additional, Lee, K M, additional, Koo, J S, additional, Jung, Y, additional, Lee, B J, additional, Yoon, H, additional, Kim, H W, additional, Lim, Y J, additional, Lee, H S, additional, Lee, Y J, additional, Lee, J, additional, Lee, C K, additional, Shin, S Y, additional, Moon, J M, additional, Seo, J, additional, and Choi, C H, additional
Published: 2024
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42. P1022 One-year safety and effectiveness of ustekinumab in patients with Crohn’s disease: The K-STAR study

Author: Lee, C K, primary, Moon, W, additional, Chun, J, additional, Kim, E S, additional, Kim, H W, additional, Yoon, H, additional, Kim, H S, additional, Lee, Y J, additional, Choi, C H, additional, Jung, Y, additional, Park, S C, additional, Song, G A, additional, Lee, J H, additional, Jung, E S, additional, Kim, Y, additional, Jung, S Y, additional, Choi, J M, additional, and Ye, B D, additional
Published: 2024
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43. The Physics of the B Factories

Author: Bevan, A. J., Golob, B., Mannel, Th., Prell, S., Yabsley, B. D., Abe, K., Aihara, H., Anulli, F., Arnaud, N., Aushev, T., Beneke, M., Beringer, J., Bianchi, F., Bigi, I. I., Bona, M., Brambilla, N., rodzicka, J. B, Chang, P., Charles, M. J., Cheng, C. H., Cheng, H. -Y., Chistov, R., Colangelo, P., Coleman, J. P., Drutskoy, A., Druzhinin, V. P., Eidelman, S., Eigen, G., Eisner, A. M., Faccini, R., Flood, K. T ., Gambino, P., Gaz, A., Gradl, W., Hayashii, H., Higuchi, T., Hulsbergen, W. D., Hurth, T., Iijima, T., Itoh, R., Jackson, P. D., Kass, R., Kolomensky, Yu. G., Kou, E., Križan, P., Kronfeld, A., Kumano, S., Kwon, Y. J., Latham, T. E., Leith, D. W. G. S., Lüth, V., Martinez-Vidal, F., Meadows, B. T., Mussa, R., Nakao, M., Nishida, S., Ocariz, J., Olsen, S. L., Pakhlov, P., Pakhlova, G., Palano, A., Pich, A., Playfer, S., Poluektov, A., Porter, F. C., Robertson, S. H., Roney, J. M., Roodman, A., Sakai, Y., Schwanda, C., Schwartz, A. J., Seidl, R., Sekula, S. J., Steinhauser, M., Sumisawa, K., Swanson, E. S., Tackmann, F., Trabelsi, K., Uehara, S., Uno, S., van der Water, R., Vasseur, G., Verkerke, W., Waldi, R., Wang, M. Z., Wilson, F. F., Zupan, J., Zupanc, A., Adachi, I., Albert, J., Banerjee, Sw., Bellis, M., Ben-Haim, E., Biassoni, P., Cahn, R. N., Cartaro, C., Chauveau, J., Chen, C., Chiang, C. C., Cowan, R., Dalseno, J., Davier, M., Davies, C., Dingfelder, J. C., nard, B. Eche, Epifanov, D., Fulsom, B. G., Gabareen, A. M., Gary, J. W., Godang, R., Graham, M. T., Hafner, A., Hamilton, B., Hartmann, T., Hayasaka, K., Hearty, C., Iwasaki, Y., Khodjamirian, A., Kusaka, A., Kuzmin, A., Lafferty, G. D., Lazzaro, A., Li, J., Lindemann, D., Long, O., Lusiani, A., Marchiori, G., Martinelli, M., Miyabayashi, K., Mizuk, R., Mohanty, G. B., Muller, D. R., Nakazawa, H., Ongmongkolkul, P., Pacetti, S., Palombo, F., Pedlar, T. K., Piilonen, L. E., Pilloni, A., Poireau, V., Prothmann, K., Pulliam, T., Rama, M., Ratcliff, B. N., Roudeau, P., Schrenk, S., Schroeder, T., Schubert, K. R., Shen, C. P., Shwartz, B., Soffer, A., Solodov, E. P., Somov, A., Starič, M., Stracka, S., Telnov, A. V., Todyshev, K. Yu., Tsuboyama, T., Uglov, T., Vinokurova, A., Walsh, J. J., Watanabe, Y., Won, E., Wormser, G., Wright, D. H., Ye, S., Zhang, C. C., Abachi, S., Abashian, A., Abe, N., Abe, R., Abe, T., Abrams, G. S., Adam, I., Adamczyk, K., Adametz, A., Adye, T., Agarwal, A., Ahmed, H., Ahmed, M., Ahmed, S., Ahn, B. S., Ahn, H. S., Aitchison, I. J. R., Akai, K., Akar, S., Akatsu, M., Akemoto, M., Akhmetshin, R., Akre, R., Alam, M. S., Albert, J. N., Aleksan, R., Alexander, J. P., Alimonti, G., Allen, M. T., Allison, J., Allmendinger, T., Alsmiller, J. R. G., Altenburg, D., Alwyn, K. E., An, Q., Anderson, J., Andreassen, R., Andreotti, D., Andreotti, M., Andress, J. C., Angelini, C., Anipko, D., Anjomshoaa, A., Anthony, P. L., Antillon, E. A., Antonioli, E., Aoki, K., Arguin, J. F., Arinstein, K., Arisaka, K., Asai, K., Asai, M., Asano, Y., Asgeirsson, D. J., Asner, D. M., Aso, T., Aspinwall, M. L., Aston, D., Atmacan, H., Aubert, B., Aulchenko, V., Ayad, R., Azemoon, T., Aziz, T., Azzolini, V., Azzopardi, D. E., Baak, M. A., Back, J. J., Bagnasco, S., Bahinipati, S., Bailey, D. S., Bailey, S., Bailly, P., van Bakel, N., Bakich, A. M., Bala, A., Balagura, V., Baldini-Ferroli, R., Ban, Y., Banas, E., Band, H. R., Banerjee, S., Baracchini, E., Barate, R., Barberio, E., Barbero, M., Bard, D. J., Barillari, T., Barlow, N. R., Barlow, R. J., Barrett, M., Bartel, W., Bartelt, J., Bartoldus, R., Batignani, G., Battaglia, M., Bauer, J. M., Bay, A., Beaulieu, M., Bechtle, P., Beck, T. W., Becker, J., Becla, J., Bedny, I., Behari, S., Behera, P. K., Behn, E., Behr, L., Beigbeder, C., Beiline, D., Bell, R., Bellini, F., Bellodi, G., Belous, K., Benayoun, M., Benelli, G., Benitez, J. F., Benkebil, M., Berger, N., Bernabeu, J., Bernard, D., Bernet, R., Bernlochner, F. U., Berryhill, J. W., Bertsche, K., Besson, P., Best, D. S., Bettarini, S., Bettoni, D., Bhardwaj, V., Bhimji, W., Bhuyan, B., Biagini, M. E., Biasini, M., van Bibber, K., Biesiada, J., Bingham, I., Bionta, R. M., Bischofberger, M., Bitenc, U., Bizjak, I., Blanc, F., Blaylock, G., Blinov, V. E., Bloom, E., Bloom, P. C., Blount, N. L., Blouw, J., Bly, M., Blyth, S., Boeheim, C. T., Bomben, M., Bondar, A., Bondioli, M., Bonneaud, G. R., Bonvicini, G., Booke, M., Booth, J., Borean, C., Borgland, A. W., Borsato, E., Bosi, F., Bosisio, L., Botov, A. A., Bougher, J., Bouldin, K., Bourgeois, P., Boutigny, D., Bowerman, D. A., Boyarski, A. M., Boyce, R. F., Boyd, J. T., Bozek, A., Bozzi, C., Bračko, M., Brandenburg, G., Brandt, T., Brau, B., Brau, J., Breon, A. B., Breton, D., Brew, C., Briand, H., Bright-Thomas, P. G., Brigljević, V., Britton, D. I., Brochard, F., Broomer, B., Brose, J., Browder, T. E., Brown, C. L., Brown, C. M., Brown, D. N., Browne, M., Bruinsma, M., Brunet, S., Bucci, F., Buchanan, C., Buchmueller, O. L., Bünger, C., Bugg, W., Bukin, A. D., Bula, R., Bulten, H., Burchat, P. R., Burgess, W., Burke, J. P., Button-Shafer, J., Buzykaev, A. R., Buzzo, A., Cai, Y., Calabrese, R., Calcaterra, A., Calderini, G., Camanzi, B., Campagna, E., Campagnari, C., Capra, R., Carassiti, V., Carpinelli, M., Carroll, M., Casarosa, G., Casey, B. C. K., Cason, N. M., Castelli, G., Cavallo, N., Cavoto, G., Cecchi, A., Cenci, R., Cerizza, G., Cervelli, A., Ceseracciu, A., Chai, X., Chaisanguanthum, K. S., Chang, M. C., Chang, Y. H., Chang, Y. W., Chao, D. S., Chao, M., Chao, Y., Charles, E., Chavez, C. A., Cheaib, R., Chekelian, V., Chen, A., Chen, E., Chen, G. P., Chen, H. F., Chen, J. -H., Chen, J. C., Chen, K. F., Chen, P., Chen, S., Chen, W. T., Chen, X., Chen, X. R., Chen, Y. Q., Cheng, B., Cheon, B. G., Chevalier, N., Chia, Y. M., Chidzik, S., Chilikin, K., Chistiakova, M. V., Cizeron, R., Cho, I. S., Cho, K., Chobanova, V., Choi, H. H. F., Choi, K. S., Choi, S. K., Choi, Y., Choi, Y. K., Christ, S., Chu, P. H., Chun, S., Chuvikov, A., Cibinetto, G., Cinabro, D., Clark, A. R., Clark, P. J., Clarke, C. K., Claus, R., Claxton, B., Clifton, Z. C., Cochran, J., Cohen-Tanugi, J., Cohn, H., Colberg, T., Cole, S., Colecchia, F., Condurache, C., Contri, R., Convert, P., Convery, M. R., Cooke, P., Copty, N., Cormack, C. M., Corso, F. Dal, Corwin, L. A., Cossutti, F., Cote, D., Ramusino, A. Cotta, Cottingham, W. N., Couderc, F., Coupal, D. P., Covarelli, R., Cowan, G., Craddock, W. W., Crane, G., Crawley, H. B., Cremaldi, L., Crescente, A., Cristinziani, M., Crnkovic, J., Crosetti, G., Cuhadar-Donszelmann, T., Cunha, A., Curry, S., D'Orazio, A., Dû, S., Dahlinger, G., Dahmes, B., Dallapiccola, C., Danielson, N., Danilov, M., Das, A., Dash, M., Dasu, S., Datta, M., Daudo, F., Dauncey, P. D., David, P., Davis, C. L., Day, C. T., De Mori, F., De Domenico, G., De Groot, N., De la Vaissière, C., de la Vaissière, Ch., de Lesquen, A., De Nardo, G., de Sangro, R., De Silva, A., DeBarger, S., Decker, F. J., Sanchez, P. del Amo, Del Buono, L., Del Gamba, V., del Re, D., Della Ricca, G., Denig, A. G., Derkach, D., Derrington, I. M., DeStaebler, H., Destree, J., Devmal, S., Dey, B., Di Girolamo, B., Di Marco, E., Dickopp, M., Dima, M. O., Dittrich, S., Dittongo, S., Dixon, P., Dneprovsky, L., Dohou, F., Doi, Y., Doležal, Z., Doll, D. A., Donald, M., Dong, L., Dong, L. Y., Dorfan, J., Dorigo, A., Dorsten, M. P., Dowd, R., Dowdell, J., Drásal, Z., Dragic, J., Drummond, B. W., Dubitzky, R. S., Dubois-Felsmann, G. P., Dubrovin, M. S., Duh, Y. C., Duh, Y. T., Dujmic, D., Dungel, W., Dunwoodie, W., Dutta, D., Dvoretskii, A., Dyce, N., Ebert, M., Eckhart, E. A., Ecklund, S., Eckmann, R., Eckstein, P., Edgar, C. L., Edwards, A. J., Egede, U., Eichenbaum, A. M., Elmer, P., Emery, S., Enari, Y., Enomoto, R., Erdos, E., Erickson, R., Ernst, J. A., Erwin, R. J., Escalier, M., Eschenburg, V., Eschrich, I., Esen, S., Esteve, L., Evangelisti, F., Everton, C. W., Eyges, V., Fabby, C., Fabozzi, F., Fahey, S., Falbo, M., Fan, S., Fang, F., Fanin, C., Farbin, A., Farhat, H., Fast, J. E., Feindt, M., Fella, A., Feltresi, E., Ferber, T., Fernholz, R. E., Ferrag, S., Ferrarotto, F., Ferroni, F., Field, R. C., Filippi, A., Finocchiaro, G., Fioravanti, E., da Costa, J. Firmino, Fischer, P. -A., Fisher, A., Fisher, P. H., Flacco, C. J., Flack, R. L., Flaecher, H. U., Flanagan, J., Flanigan, J. M., Ford, K. E., Ford, W. T., Forster, I. J., Forti, A. C., Forti, F., Fortin, D., Foster, B., Foulkes, S. D., Fouque, G., Fox, J., Franchini, P., Sevilla, M. Franco, Franek, B., Frank, E. D., Fransham, K. B., Fratina, S., Fratini, K., Frey, A., Frey, R., Friedl, M., Fritsch, M., Fry, J. R., Fujii, H., Fujikawa, M., Fujita, Y., Fujiyama, Y., Fukunaga, C., Fukushima, M., Fullwood, J., Funahashi, Y., Funakoshi, Y., Furano, F., Furman, M., Furukawa, K., Futterschneider, H., Gabathuler, E., Gabriel, T. A., Gabyshev, N., Gaede, F., Gagliardi, N., Gaidot, A., Gaillard, J. -M., Gaillard, J. R., Galagedera, S., Galeazzi, F., Gallo, F., Gamba, D., Gamet, R., Gan, K. K., Gandini, P., Ganguly, S., Ganzhur, S. F., Gao, Y. Y., Gaponenko, I., Garmash, A., Tico, J. Garra, Garzia, I., Gaspero, M., Gastaldi, F., Gatto, C., Gaur, V., Geddes, N. I., Geld, T. L., Genat, J. -F., George, K. A., George, M., George, S., Georgette, Z., Gershon, T. J., Gill, M. S., Gillard, R., Gilman, J. D., Giordano, F., Giorgi, M. A., Giraud, P. -F., Gladney, L., Glanzman, T., Glattauer, R., Go, A., Goetzen, K., Goh, Y. M., Gokhroo, G., Goldenzweig, P., Golubev, V. B., Gopal, G. P., Gordon, A., Gorišek, A., Goriletsky, V. I., Gorodeisky, R., Gosset, L., Gotow, K., Gowdy, S. J., Graffin, P., Grancagnolo, S., Grauges, E., Graziani, G., Green, M. G., Greene, M. G., Grenier, G. J., Grenier, P., Griessinger, K., Grillo, A. A., Grinyov, B. V., Gritsan, A. V., Grosdidier, G., Perdekamp, M. Grosse, Grosso, P., Grothe, M., Groysman, Y., Grünberg, O., Guido, E., Guler, H., Gunawardane, N. J. W., Guo, Q. H., Guo, R. S., Guo, Z. J., Guttman, N., Ha, H., Ha, H. C., Haas, T., Haba, J., Hachtel, J., Hadavand, H. K., Hadig, T., Hagner, C., Haire, M., Haitani, F., Haji, T., Haller, G., Halyo, V., Hamano, K., Hamasaki, H., de Monchenault, G. Hamel, Hamilton, J., Hamilton, R., Hamon, O., Han, B. Y., Han, Y. L., Hanada, H., Hanagaki, K., Handa, F., Hanson, J. E., Hanushevsky, A., Hara, K., Hara, T., Harada, Y., Harrison, P. F., Harrison, T. J., Harrop, B., Hart, A. J., Hart, P. A., Hartfiel, B. L., Harton, J. L., Haruyama, T., Hasan, A., Hasegawa, Y., Hast, C., Hastings, N. C., Hasuko, K., Hauke, A., Hawkes, C. M., Hayashi, K., Hazumi, M., Hee, C., Heenan, E. M., Heffernan, D., Held, T., Henderson, R., Henderson, S. W., Hertzbach, S. S., Hervé, S., Heß, M., Heusch, C. A., Hicheur, A., Higashi, Y., Higasino, Y., Higuchi, I., Hikita, S., Hill, E. J., Himel, T., Hinz, L., Hirai, T., Hirano, H., Hirschauer, J. F., Hitlin, D. G., Hitomi, N., Hodgkinson, M. C., Höcker, A., Hoi, C. T., Hojo, T., Hokuue, T., Hollar, J. J., Hong, T. M., Honscheid, K., Hooberman, B., Hopkins, D. A., Horii, Y., Hoshi, Y., Hoshina, K., Hou, S., Hou, W. S., Hryn'ova, T., Hsiung, Y. B., Hsu, C. L., Hsu, S. C., Hu, H., Hu, T., Huang, H. C., Huang, T. J., Huang, Y. C., Huard, Z., Huffer, M. E., Hufnagel, D., Hung, T., Hutchcroft, D. E., Hyun, H. J., Ichizawa, S., Igaki, T., Igarashi, A., Igarashi, S., Igarashi, Y., Igonkina, O., Ikado, K., Ikeda, H., Ikeda, K., Ilic, J., Inami, K., Innes, W. R., Inoue, Y., Ishikawa, A., Ishino, H., Itagaki, K., Itami, S., Itoh, K., Ivanchenko, V. N., Iverson, R., Iwabuchi, M., Iwai, G., Iwai, M., Iwaida, S., Iwamoto, M., Iwasaki, H., Iwasaki, M., Iwashita, T., Izen, J. M., Jackson, D. J., Jackson, F., Jackson, G., Jackson, P. S., Jacobsen, R. G., Jacoby, C., Jaegle, I., Jain, V., Jalocha, P., Jang, H. K., Jasper, H., Jawahery, A., Jayatilleke, S., Jen, C. M., Jensen, F., Jessop, C. P., Ji, X. B., John, M. J. J., Johnson, D. R., Johnson, J. R., Jolly, S., Jones, M., Joo, K. K., Joshi, N., Joshi, N. J., Judd, D., Julius, T., Kadel, R. W., Kadyk, J. A., Kagan, H., Kagan, R., Kah, D. H., Kaiser, S., Kaji, H., Kajiwara, S., Kakuno, H., Kameshima, T., Kaminski, J., Kamitani, T., Kaneko, J., Kang, J. H., Kang, J. S., Kani, T., Kapusta, P., Karbach, T. M., Karolak, M., Karyotakis, Y., Kasami, K., Katano, G., Kataoka, S. U., Katayama, N., Kato, E., Kato, Y., Kawai, H., Kawai, M., Kawamura, N., Kawasaki, T., Kay, J., Kay, M., Kelly, M. P., Kelsey, M. H., Kent, N., Kerth, L. T., Khan, A., Khan, H. R., Kharakh, D., Kibayashi, A., Kichimi, H., Kiesling, C., Kikuchi, M., Kikutani, E., Kim, B. H., Kim, C. H., Kim, D. W., Kim, H., Kim, H. J., Kim, H. O., Kim, H. W., Kim, J. B., Kim, J. H., Kim, K. T., Kim, M. J., Kim, P., Kim, S. K., Kim, S. M., Kim, T. H., Kim, Y. I., Kim, Y. J., King, G. J., Kinoshita, K., Kirk, A., Kirkby, D., Kitayama, I., Klemetti, M., Klose, V., Klucar, J., Knecht, N. S., Knoepfel, K. J., Knowles, D. J., Ko, B. R., Kobayashi, N., Kobayashi, S., Kobayashi, T., Kobel, M. J., Koblitz, S., Koch, H., Kocian, M. L., Kodyš, P., Koeneke, K., Kofler, R., Koike, S., Koishi, S., Koiso, H., Kolb, J. A., Kolya, S. D., Kondo, Y., Konishi, H., Koppenburg, P., Koptchev, V. B., Kordich, T. M. B., Korol, A. A., Korotushenko, K., Korpar, S., Kouzes, R. T., Kovalskyi, D., Kowalewski, R., Kozakai, Y., Kozanecki, W., Kral, J. F., Krasnykh, A., Krause, R., Kravchenko, E. A., Krebs, J., Kreisel, A., Kreps, M., Krishnamurthy, M., Kroeger, R., Kroeger, W., Krokovny, P., Kronenbitter, B., Kroseberg, J., Kubo, T., Kuhr, T., Kukartsev, G., Kulasiri, R., Kulikov, A., Kumar, R., Kumar, S., Kumita, T., Kuniya, T., Kunze, M., Kuo, C. C., Kuo, T. -L., Kurashiro, H., Kurihara, E., Kurita, N., Kuroki, Y., Kurup, A., Kutter, P. E., Kuznetsova, N., Kvasnička, P., Kyberd, P., Kyeong, S. H., Lacker, H. M., Lae, C. K., Lamanna, E., Lamsa, J., Lanceri, L., Landi, L., Lang, M. I., Lange, D. J., Lange, J. S., Langenegger, U., Langer, M., Lankford, A. J., Lanni, F., Laplace, S., Latour, E., Lau, Y. P., Lavin, D. R., Layter, J., Lebbolo, H., LeClerc, C., Leddig, T., Leder, G., Diberder, F. Le, Lee, C. L., Lee, J., Lee, J. S., Lee, M. C., Lee, M. H., Lee, M. J., Lee, S. -J., Lee, S. E., Lee, S. H., Lee, Y. J., Lees, J. P., Legendre, M., Leitgab, M., Leitner, R., Leonardi, E., Leonidopoulos, C., Lepeltier, V., Leruste, Ph., Lesiak, T., Levi, M. E., Levy, S. L., Lewandowski, B., Lewczuk, M. J., Lewis, P., Li, H., Li, H. B., Li, S., Li, X., Li, Y., Gioi, L. Li, Libby, J., Lidbury, J., Lillard, V., Lim, C. L., Limosani, A., Lin, C. S., Lin, J. Y., Lin, S. W., Lin, Y. S., Lindquist, B., Lindsay, C., Lista, L., Liu, C., Liu, F., Liu, H., Liu, H. M., Liu, J., Liu, R., Liu, T., Liu, Y., Liu, Z. Q., Liventsev, D., Vetere, M. Lo, Locke, C. B., Lockman, W. S., Di Lodovico, F., Lombardo, V., London, G. W., Pegna, D. Lopes, Lopez, L., Lopez-March, N., Lory, J., LoSecco, J. M., Lou, X. C., Louvot, R., Lu, A., Lu, C., Lu, M., Lu, R. S., Lueck, T., Luitz, S., Lukin, P., Lund, P., Luppi, E., Lutz, A. M., Lutz, O., Lynch, G., Lynch, H. L., Lyon, A. J., Lyubinsky, V. R., MacFarlane, D. B., Mackay, C., MacNaughton, J., Macri, M. M., Madani, S., Mader, W. F., Majewski, S. A., Majumder, G., Makida, Y., Malaescu, B., Malaguti, R., Malclès, J., Mallik, U., Maly, E., Mamada, H., Manabe, A., Mancinelli, G., Mandelkern, M., Mandl, F., Manfredi, P. F., Mangeol, D. 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S., Miyata, H., Miyazaki, Y., Moffitt, L. C., Mohapatra, A., Mohapatra, A. K., Mohapatra, D., Moll, A., Moloney, G. R., Mols, J. P., Mommsen, R. K., Monge, M. R., Monorchio, D., Moore, T. B., Moorhead, G. F., de Freitas, P. Mora, Morandin, M., Morgan, N., Morgan, S. E., Morganti, M., Morganti, S., Mori, S., Mori, T., Morii, M., Morris, J. P., Morsani, F., Morton, G. W., Moss, L. J., Mouly, J. P., Mount, R., Mueller, J., Müller-Pfefferkorn, R., Mugge, M., Muheim, F., Muir, A., Mullin, E., Munerato, M., Murakami, A., Murakami, T., Muramatsu, N., Musico, P., Nagai, I., Nagamine, T., Nagasaka, Y., Nagashima, Y., Nagayama, S., Nagel, M., Naisbit, M. T., Nakadaira, T., Nakahama, Y., Nakajima, M., Nakajima, T., Nakamura, I., Nakamura, T., Nakamura, T. T., Nakano, E., Nakayama, H., Nam, J. W., Narita, S., Narsky, I., Nash, J . A., Natkaniec, Z., Nauenberg, U., Nayak, M., Neal, H., Nedelkovska, E., Negrini, M., Neichi, K., Nelson, D., Nelson, S., Neri, N., Nesom, G., Neubauer, S., Newman-Coburn, D., Ng, C., Nguyen, X., Nicholson, H., Niebuhr, C., Nief, J. Y., Niiyama, M., Nikolich, M. B., Nisar, N. K., Nishimura, K., Nishio, Y., Nitoh, O., Nogowski, R., Noguchi, S., Nomura, T., Nordby, M., Nosochkov, Y., Novokhatski, A., Nozaki, S., Nozaki, T., Nugent, I. M., O'Grady, C. P., O'Neale, S. W., O'Neill, F. G., Oberhof, B., Oddone, P. J., Ofte, I., Ogawa, A., Ogawa, K., Ogawa, S., Ogawa, Y., Ohkubo, R., Ohmi, K., Ohnishi, Y., Ohno, F., Ohshima, T., Ohshima, Y., Ohuchi, N., Oide, K., Oishi, N., Okabe, T., Okazaki, N., Okazaki, T., Okuno, S., Olaiya, E. O., Olivas, A., Olley, P., Olsen, J., Ono, S., Onorato, G., Onuchin, A. P., Onuki, Y., Ooba, T., Orimoto, T. J., Oshima, T., Osipenkov, I. L., Ostrowicz, W., Oswald, C., Otto, S., Oyang, J., Oyanguren, A., Ozaki, H., Ozcan, V. E., Paar, H. P., Padoan, C., Paick, K., Palka, H., Pan, B., Pan, Y., Vazquez, W. Panduro, Panetta, J., Panova, A. I., Panvini, R. S., Panzenböck, E., Paoloni, E., Paolucci, P., Pappagallo, M., Paramesvaran, S., Park, C. S., Park, C. W., Park, H., Park, H. K., Park, K. S., Park, W., Parry, R. J., Parslow, N., Passaggio, S., Pastore, F. C., Patel, P. M., Patrignani, C., Patteri, P., Pavel, T., Pavlovich, J., Payne, D. J., Peak, L. S., Peimer, D. R., Pelizaeus, M., Pellegrini, R., Pelliccioni, M., Peng, C. C., Peng, J. C., Peng, K. C., Peng, T., Penichot, Y., Pennazzi, S., Pennington, M. R., Penny, R. C., Penzkofer, A., Perazzo, A., Perez, A., Perl, M., Pernicka, M., Perroud, J. -P., Peruzzi, I. M., Pestotnik, R., Peters, K., Peters, M., Petersen, B. A., Petersen, T. C., Petigura, E., Petrak, S., Petrella, A., Petrič, M., Petzold, A., Pia, M. G., Piatenko, T., Piccolo, D., Piccolo, M., Piemontese, L., Piemontese, M., Pierini, M., Pierson, S., Pioppi, M., Piredda, G., Pivk, M., Plaszczynski, S., Polci, F., Pompili, A., Poropat, P., Posocco, M., Potter, C. T., Potter, R. J. L., Prasad, V., Prebys, E., Prencipe, E., Prendki, J., Prepost, R., Prest, M., Prim, M., Pripstein, M., Prudent, X., Pruvot, S., Puccio, E. M. T., Purohit, M. V., Qi, N. D., Quinn, H., Raaf, J., Rabberman, R., Raffaelli, F., Ragghianti, G., Rahatlou, S., Rahimi, A. M., Rahmat, R., Rakitin, A. Y., Randle-Conde, A., Rankin, P., Rashevskaya, I., Ratkovsky, S., Raven, G., Re, V., Reep, M., Regensburger, J. J., Reidy, J., Reif, R., Reisert, B., Renard, C., Renga, F., Ricciardi, S., Richman, J. D., Ritchie, J. L., Ritter, M., Rivetta, C., Rizzo, G., Roat, C., Robbe, P., Roberts, D. A., Robertson, A. I., Robutti, E., Rodier, S., Rodriguez, D. M., Rodriguez, J. L., Rodriguez, R., Roe, N. A., Röhrken, M., Roethel, W., Rolquin, J., Romanov, L., Romosan, A., Ronan, M. T., Rong, G., Ronga, F. J., Roos, L., Root, N., Rosen, M., Rosenberg, E. I., Rossi, A., Rostomyan, A., Rotondo, M., Roussot, E., Roy, J., Rozanska, M., Rozen, Y., Rubin, A. E., Ruddick, W. O., Ruland, A. M., Rybicki, K., Ryd, A., Ryu, S., Ryuko, J., Sabik, S., Sacco, R., Saeed, M. A., Tehrani, F. Safai, Sagawa, H., Sahoo, H., Sahu, S., Saigo, M., Saito, T., Saitoh, S., Sakai, K., Sakamoto, H., Sakaue, H., Saleem, M., Salnikov, A. A., Salvati, E., Salvatore, F., Samuel, A., Sanders, D. A., Sanders, P., Sandilya, S., Sandrelli, F., Sands, W., Sands, W. R., Sanpei, M., Santel, D., Santelj, L., Santoro, V., Santroni, A., Sanuki, T., Sarangi, T. R., Saremi, S., Sarti, A., Sasaki, T., Sasao, N., Satapathy, M., Sato, Nobuhiko, Sato, Noriaki, Sato, Y., Satoyama, N., Satpathy, A., Savinov, V., Savvas, N., Saxton, O. H., Sayeed, K., Schaffner, S. F., Schalk, T., Schenk, S., Schieck, J. R., Schietinger, T., Schilling, C. J., Schindler, R. H., Schmid, S., Schmitz, R. E., Schmuecker, H., Schneider, O., Schnell, G., Schönmeier, P., Schofield, K. C., Schott, G., Schröder, H., Schram, M., Schubert, J., Schümann, J., Schultz, J., Schumm, B. A., Schune, M. H., Schwanke, U., Schwarz, H., Schwiening, J., Schwierz, R., Schwitters, R. F., Sciacca, C., Sciolla, G., Scott, I. J., Seeman, J., Seiden, A., Seitz, R., Seki, T., Sekiya, A. I., Semenov, S., Semmler, D., Sen, S., Senyo, K., Seon, O., Serbo, V. V., Serednyakov, S. I., Serfass, B., Serra, M., Serrano, J., Settai, Y., Seuster, R., Sevior, M. E., Shakhova, K. V., Shang, L., Shapkin, M., Sharma, V., Shebalin, V., Shelkov, V. G., Shen, B. C., Shen, D. Z., Shen, Y. T., Sherwood, D. J., Shibata, T., Shibata, T. A., Shibuya, H., Shidara, T., Shimada, K., Shimoyama, M., Shinomiya, S., Shiu, J. G., Shorthouse, H. W., Shpilinskaya, L. I., Sibidanov, A., Sicard, E., Sidorov, A., Sidorov, V., Siegle, V., Sigamani, M., Simani, M. C., Simard, M., Simi, G., Simon, F., Simonetto, F., Sinev, N. B., Singh, H., Singh, J. B., Sinha, R., Sitt, S., Skovpen, Yu. I., Sloane, R. J., Smerkol, P., Smith, A. J. S., Smith, D., Smith, D. S., Smith, J. G., Smol, A., Snoek, H. L., Snyder, A., So, R. Y., Sobie, R. J., Soderstrom, E., Soha, A., Sohn, Y. S., Sokoloff, M. D., Sokolov, A., Solagna, P., Solovieva, E., Soni, N., Sonnek, P., Sordini, V., Spaan, B., Spanier, S. M., Spencer, E., Speziali, V., Spitznagel, M., Spradlin, P., Staengle, H., Stamen, R., Stanek, M., Stanič, S., Stark, J., Steder, M., Steininger, H., Steinke, M., Stelzer, J., Stevanato, E., Stocchi, A., Stock, R., Stoeck, H., Stoker, D. P., Stroili, R., Strom, D., Strother, P., Strube, J., Stugu, B., Stypula, J., Su, D., Suda, R., Sugahara, R., Sugi, A., Sugimura, T., Sugiyama, A., Suitoh, S., Sullivan, M. K., Sumihama, M., Sumiyoshi, T., Summers, D. J., Sun, L., Sun, S., Sundermann, J. E., Sung, H. F., Susaki, Y., Sutcliffe, P., Suzuki, A., Suzuki, J., Suzuki, J. I., Suzuki, K., Suzuki, S., Suzuki, S. Y., Swain, J. E., Swain, S. K., T'Jampens, S., Tabata, M., Tackmann, K., Tajima, H., Tajima, O., Takahashi, K., Takahashi, S., Takahashi, T., Takasaki, F., Takayama, T., Takita, M., Tamai, K., Tamponi, U., Tamura, N., Tan, N., Tan, P., Tanabe, K., Tanabe, T., Tanaka, H. A., Tanaka, J., Tanaka, M., Tanaka, S., Tanaka, Y., Tanida, K., Taniguchi, N., Taras, P., Tasneem, N., Tatishvili, G., Tatomi, T., Tawada, M., Taylor, F., Taylor, G. N., Taylor, G. P., Telnov, V. I., Teodorescu, L., Ter-Antonyan, R., Teramoto, Y., Teytelman, D., Thérin, G., Thiebaux, Ch., Thiessen, D., Thomas, E. W., Thompson, J. M., Thorne, F., Tian, X. C., Tibbetts, M., Tikhomirov, I., Tinslay, J. S., Tiozzo, G., Tisserand, V., Tocut, V., Toki, W. H., Tomassini, E. W., Tomoto, M., Tomura, T., Torassa, E., Torrence, E., Tosi, S., Touramanis, C., Toussaint, J. C., Tovey, S. N., Trapani, P. P., Treadwell, E., Triggiani, G., Trincaz-Duvoid, S., Trischuk, W., Troost, D., Trunov, A., Tsai, K. L., Tsai, Y. T., Tsujita, Y., Tsukada, K., Tsukamoto, T., Tuggle, J. M., Tumanov, A., Tung, Y. W., Turnbull, L., Turner, J., Turri, M., Uchida, K., Uchida, M., Uchida, Y., Ueki, M., Ueno, K., Ujiie, N., Ulmer, K. A., Unno, Y., Urquijo, P., Ushiroda, Y., Usov, Y., Usseglio, M., Usuki, Y., Uwer, U., Va'vra, J., Vahsen, S. E., Vaitsas, G., Valassi, A., Vallazza, E., Vallereau, A., Vanhoefer, P., van Hoek, W. C., Van Hulse, C., van Winkle, D., Varner, G., Varnes, E. W., Varvell, K. E., Vasileiadis, G., Velikzhanin, Y. S., Verderi, M., Versillé, S., Vervink, K., Viaud, B., Vidal, P. B., Villa, S., Villanueva-Perez, P., Vinograd, E. L., Vitale, L., Vitug, G. M., Voß, C., Voci, C., Voena, C., Volk, A., von Wimmersperg-Toeller, J. H., Vorobyev, V., Vossen, A., Vuagnin, G., Vuosalo, C. O., Wacker, K., Wagner, A. P., Wagner, D. L., Wagner, G., Wagner, M. N., Wagner, S. R., Wagoner, D. E., Walker, D., Walkowiak, W., Wallom, D., Wang, C. C., Wang, C. H., Wang, J., Wang, J. G., Wang, K., Wang, L., Wang, L. L., Wang, P., Wang, T. J., Wang, W. F., Wang, X. L., Wang, Y. F., Wappler, F. R., Watanabe, M., Watson, A. T., Watson, J. E., Watson, N. K., Watt, M., Weatherall, J. H., Weaver, M., Weber, T., Wedd, R., Wei, J. T., Weidemann, A. W., Weinstein, A. J. R., Wenzel, W. A., West, C. A., West, C. G., West, T. J., White, E., White, R. M., Wicht, J., Widhalm, L., Wiechczynski, J., Wienands, U., Wilden, L., Wilder, M., Williams, D. C., Williams, G., Williams, J. C., Williams, K. M., Williams, M. I., Willocq, S. Y., Wilson, J. R., Wilson, M. G., Wilson, R. J., Winklmeier, F., Winstrom, L. O., Winter, M. A., Wisniewski, W. J., Wittgen, M., Wittlin, J., Wittmer, W., Wixted, R., Woch, A., Wogsland, B. J., Wong, Q. K., Wray, B. C., Wren, A. C., Wright, D. M., Wu, C. H., Wu, J., Wu, S. L., Wulsin, H. W., Xella, S. M., Xie, Q. L., Xie, Y., Xu, Z. Z., Yèche, Ch., Yamada, Y., Yamaga, M., Yamaguchi, A., Yamaguchi, H., Yamaki, T., Yamamoto, H., Yamamoto, N., Yamamoto, R. K., Yamamoto, S., Yamanaka, T., Yamaoka, H., Yamaoka, J., Yamaoka, Y., Yamashita, Y., Yamauchi, M., Yan, D. S., Yan, Y., Yanai, H., Yanaka, S., Yang, H., Yang, R., Yang, S., Yarritu, A. K., Yashchenko, S., Yashima, J., Yasin, Z., Yasu, Y., Ye, S. W., Yeh, P., Yi, J. I., Yi, K., Yi, M., Yin, Z. W., Ying, J., Yocky, G., Yokoyama, K., Yokoyama, M., Yokoyama, T., Yoshida, K., Yoshida, M., Yoshimura, Y., Young, C. C., Yu, C. X., Yu, Z., Yuan, C. Z., Yuan, Y., Yumiceva, F. X., Yusa, Y., Yushkov, A. N., Yuta, H., Zacek, V., Zain, S. B., Zallo, A., Zambito, S., Zander, D., Zang, S. L., Zanin, D., Zaslavsky, B. G., Zeng, Q. L., Zghiche, A., Zhang, B., Zhang, J., Zhang, L., Zhang, L. M., Zhang, S. Q., Zhang, Z. P., Zhao, H. W., Zhao, M., Zhao, Z. G., Zheng, Y., Zheng, Y. H., Zheng, Z. P., Zhilich, V., Zhou, P., Zhu, R. Y., Zhu, Y. S., Zhu, Z. M., Zhulanov, V., Ziegler, T., Ziegler, V., Zioulas, G., Zisman, M., Zito, M., Zürcher, D., Zwahlen, N., Zyukova, O., Živko, T., and Žontar, D.
Subjects: High Energy Physics - Experiment, High Energy Physics - Phenomenology
Abstract: This work is on the Physics of the B Factories. Part A of this book contains a brief description of the SLAC and KEK B Factories as well as their detectors, BaBar and Belle, and data taking related issues. Part B discusses tools and methods used by the experiments in order to obtain results. The results themselves can be found in Part C. Please note that version 3 on the archive is the auxiliary version of the Physics of the B Factories book. This uses the notation alpha, beta, gamma for the angles of the Unitarity Triangle. The nominal version uses the notation phi_1, phi_2 and phi_3. Please cite this work as Eur. Phys. J. C74 (2014) 3026., Comment: 928 pages, version 3 (arXiv:1406.6311v3) corresponds to the alpha, beta, gamma version of the book, the other versions use the phi1, phi2, phi3 notation
Published: 2014
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44. Measurement of the Mass Difference Between Top and Anti-top Quarks at CDF

Author: Aaltonen, T., Gonzalez, B. Alvarez, Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Apresyan, A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bauer, G., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Binkley, M., Bisello, D., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Brisuda, A., Bromberg, C., Brucken, E., Bucciantonio, M., Budagov, J., Budd, H. S., Budd, S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chou, J. P., Chung, W. H., Chung, Y. S., Ciobanu, C. I., Ciocci, M. A., Clark, A., Clarke, C., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Almenar, C. Cuenca, Cuevas, J., Culbertson, R., Dagenhart, D., d'Ascenzo, N., Datta, M., de Barbaro, P., De Cecco, S., De Lorenzo, G., Dell'Orso, M., Deluca, C., Demortier, L., Deng, J., Deninno, M., Devoto, F., d'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dong, P., Dorigo, M., Dorigo, T., Ebina, K., Elagin, A., Eppig, A., Erbacher, R., Errede, D., Errede, S., Ershaidat, N., Eusebi, R., Fang, H. C., Farrington, S., Feindt, M., Fernandez, J. P., Ferrazza, C., Field, R., Flanagan, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Funakoshi, Y., Furic, I., Gallinaro, M., Galyardt, J., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giunta, M., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Grinstein, S., Grosso-Pilcher, C., Group, R. C., da Costa, J. Guimaraes, Gunay-Unalan, Z., Haber, C., Hahn, S. R., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Hewamanage, S., Hidas, D., Hocker, A., Hopkins, W., Horn, D., Hou, S., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jha, M. K., Jindariani, S., Johnson, W., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, H. W., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kimura, N., Kirby, M., Klimenko, S., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Krumnack, N., Kruse, M., Krutelyov, V., Kuhr, T., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lin, C. -J., Linacre, J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maeshima, K., Makhoul, K., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, C., Martinez, M., Martinez-Ballarin, R., Mastrandrea, P., Mattson, M. E., Mazzanti, P., McFarland, K. S., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Menzione, A., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Neubauer, M. S., Nielsen, J., Nodulman, L., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Griso, S. Pagan, Pagliarone, C., Palencia, E., Papadimitriou, V., Paramonov, A. A., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Poukhov, O., Prokoshin, F., Pronko, A., Ptohos, F., Pueschel, E., Punzi, G., Pursley, J., Rahaman, A., Ramakrishnan, V., Ranjan, N., Ray, J., Redondo, I., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Rossi, M., Rubbo, F., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sakumoto, W. K., Sakurai, Y., Santi, L., Sartori, L., Sato, K., Saveliev, V., Savoy-Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schmidt, M. P., Schmitt, M., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Sedov, A., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Sfyrla, A., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shiraishi, S., Shochet, M., Shreyber, I., Simonenko, A., Sinervo, P., Sissakian, A., Sliwa, K., Smith, J. R., Snider, F. D., Soha, A., Somalwar, S., Sorin, V., Squillacioti, P., Stancari, M., Stanitzki, M., Denis, R. St., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Ttito-Guzman, P., Tkaczyk, S., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tu, Y., Ukegawa, F., Uozumi, S., Varganov, A., Vasquez, J., Vazquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vizan, J., Vogel, M., Volpi, G., Wagner, P., Wagner, R. L., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Weinberger, M., Wester III, W. C., Whitehouse, B., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Wick, F., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamaoka, J., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., Yu, G. B., Yu, I., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: We present a measurement of the mass difference between top ($t$) and anti-top ($\bar{t}$) quarks using $t\bar{t}$ candidate events reconstructed in the final state with one lepton and multiple jets. We use the full data set of Tevatron $\sqrt{s} = 1.96$ TeV proton-antiproton collisions recorded by the CDF II detector, corresponding to an integrated luminosity of 8.7 fb$^{-1}$. We estimate event-by-event the mass difference to construct templates for top-quark signal events and background events. The resulting mass difference distribution of data compared to signal and background templates using a likelihood fit yields $\Delta M_{top} = {M}_{t} - {M}_{\bar{t}} = -1.95 $pm$ 1.11 (stat) $pm$ 0.59 (syst)$ and is in agreement with the standard model prediction of no mass difference., Comment: Accepted in Phys. Rev. D
Published: 2012
Full Text: View/download PDF

45. Search for the Higgs boson in the all-hadronic final state using the full CDF data set

Author: CDF Collaboration, Aaltonen, T., Gonzalez, B. Alvarez, Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Apresyan, A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bauer, G., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Binkley, M., Bisello, D., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Brisuda, A., Bromberg, C., Brucken, E., Bucciantonio, M., Budagov, J., Budd, H. S., Budd, S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chou, J. P., Chung, W. H., Chung, Y. S., Ciobanu, C. I., Ciocci, M. A., Clark, A., Clarke, C., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Almenar, C. Cuenca, Cuevas, J., Culbertson, R., Dagenhart, D., d'Ascenzo, N., Datta, M., de Barbaro, P., De Cecco, S., De Lorenzo, G., Dell'Orso, M., Deluca, C., Demortier, L., Deng, J., Deninno, M., Devoto, F., d'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dong, P., Dorigo, M., Dorigo, T., Ebina, K., Elagin, A., Eppig, A., Erbacher, R., Errede, D., Errede, S., Ershaidat, N., Eusebi, R., Fang, H. C., Farrington, S., Feindt, M., Fernandez, J. P., Ferrazza, C., Field, R., Flanagan, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Funakoshi, Y., Furic, I., Gallinaro, M., Galyardt, J., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giunta, M., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Grinstein, S., Grosso-Pilcher, C., Group, R. C., da Costa, J. Guimaraes, Gunay-Unalan, Z., Haber, C., Hahn, S. R., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Hewamanage, S., Hidas, D., Hocker, A., Hopkins, W., Horn, D., Hou, S., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jha, M. K., Jindariani, S., Johnson, W., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, H. W., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kimura, N., Kirby, M., Klimenko, S., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Krumnack, N., Kruse, M., Krutelyov, V., Kuhr, T., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lin, C. -J., Linacre, J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maeshima, K., Makhoul, K., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, C., Martinez, M., Martinez-Ballarin, R., Mastrandrea, P., Mattson, M. E., Mazzanti, P., McFarland, K. S., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Menzione, A., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Neubauer, M. S., Nielsen, J., Nodulman, L., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Griso, S. Pagan, Pagliarone, C., Palencia, E., Papadimitriou, V., Paramonov, A. A., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Poukhov, O., Prokoshin, F., Pronko, A., Ptohos, F., Pueschel, E., Punzi, G., Pursley, J., Rahaman, A., Ramakrishnan, V., Ranjan, N., Ray, J., Redondo, I., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Rossi, M., Rubbo, F., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sakumoto, W. K., Sakurai, Y., Santi, L., Sartori, L., Sato, K., Saveliev, V., Savoy-Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schmidt, M. P., Schmitt, M., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Sedov, A., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Sfyrla, A., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shiraishi, S., Shochet, M., Shreyber, I., Simonenko, A., Sinervo, P., Sissakian, A., Sliwa, K., Smith, J. R., Snider, F. D., Soha, A., Somalwar, S., Sorin, V., Squillacioti, P., Stancari, M., Stanitzki, M., Denis, R. St., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Ttito-Guzman, P., Tkaczyk, S., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tu, Y., Ukegawa, F., Uozumi, S., Varganov, A., Vasquez, J., Vazquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vizan, J., Vogel, M., Volpi, G., Wagner, P., Wagner, R. L., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Weinberger, M., Wester III, W. C., Whitehouse, B., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Wick, F., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamaoka, J., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., Yu, G. B., Yu, I., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: This paper reports the result of a search for the standard model Higgs boson in events containing four reconstructed jets associated with quarks. For masses below 135GeV/c2, Higgs boson decays to bottom-antibottom quark pairs are dominant and result primarily in two hadronic jets. An additional two jets can be produced in the hadronic decay of a W or Z boson produced in association with the Higgs boson, or from the incoming quarks that produced the Higgs boson through the vector-boson fusion process. The search is performed using a sample of \sqrt{s} = 1.96 TeV proton-antiproton collisions corresponding to an integrated luminosity of 9.45 fb-1 recorded by the CDF II detector. The data are in agreement with the background model and 95% credibility level upper limits on Higgs boson production are set as a function of the Higgs boson mass. The median expected (observed) limit for a 125GeV/c2 Higgs boson is 11.0 (9.0) times the predicted standard model rate., Comment: Submitted to Journal of High Energy Physics
Published: 2012
Full Text: View/download PDF

46. Precision Top-Quark Mass Measurements at CDF

Author: Aaltonen, T., Gonzalez, B. Alvarez, Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Apresyan, A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bauer, G., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Binkley, M., Bisello, D., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Brisuda, A., Bromberg, C., Brucken, E., Bucciantonio, M., Budagov, J., Budd, H. S., Budd, S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chou, J. P., Chung, W. H., Chung, Y. S., Ciobanu, C. I., Ciocci, M. A., Clark, A., Clarke, C., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Almenar, C. Cuenca, Cuevas, J., Culbertson, R., Dagenhart, D., d'Ascenzo, N., Datta, M., de Barbaro, P., De Cecco, S., De Lorenzo, G., Dell'Orso, M., Deluca, C., Demortier, L., Deng, J., Deninno, M., Devoto, F., d'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dong, P., Dorigo, M., Dorigo, T., Ebina, K., Elagin, A., Eppig, A., Erbacher, R., Errede, D., Errede, S., Ershaidat, N., Eusebi, R., Fang, H. C., Farrington, S., Feindt, M., Fernandez, J. P., Ferrazza, C., Field, R., Flanagan, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Funakoshi, Y., Furic, I., Gallinaro, M., Galyardt, J., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giunta, M., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Grinstein, S., Grosso-Pilcher, C., Group, R. C., da Costa, J. Guimaraes, Gunay-Unalan, Z., Haber, C., Hahn, S. R., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Hewamanage, S., Hidas, D., Hocker, A., Hopkins, W., Horn, D., Hou, S., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jha, M. K., Jindariani, S., Johnson, W., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, H. W., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kimura, N., Kirby, M., Klimenko, S., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Krumnack, N., Kruse, M., Krutelyov, V., Kuhr, T., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lin, C. -J., Linacre, J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maeshima, K., Makhoul, K., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, C., Martinez, M., Martinez-Ballarin, R., Mastrandrea, P., Mattson, M. E., Mazzanti, P., McFarland, K. S., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Menzione, A., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Neubauer, M. S., Nielsen, J., Nodulman, L., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Griso, S. Pagan, Pagliarone, C., Palencia, E., Papadimitriou, V., Paramonov, A. A., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Poukhov, O., Prokoshin, F., Pronko, A., Ptohos, F., Pueschel, E., Punzi, G., Pursley, J., Rahaman, A., Ramakrishnan, V., Ranjan, N., Ray, J., Redondo, I., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Rossi, M., Rubbo, F., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sakumoto, W. K., Sakurai, Y., Santi, L., Sartori, L., Sato, K., Saveliev, V., Savoy-Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schmidt, M. P., Schmitt, M., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Sedov, A., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Sfyrla, A., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shiraishi, S., Shochet, M., Shreyber, I., Simonenko, A., Sinervo, P., Sissakian, A., Sliwa, K., Smith, J. R., Snider, F. D., Soha, A., Somalwar, S., Sorin, V., Squillacioti, P., Stancari, M., Stanitzki, M., Denis, R. St., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Ttito-Guzman, P., Tkaczyk, S., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tu, Y., Ukegawa, F., Uozumi, S., Varganov, A., Vasquez, J., Vazquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vizan, J., Vogel, M., Volpi, G., Wagner, P., Wagner, R. L., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Weinberger, M., Wester III, W. C., Whitehouse, B., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Wick, F., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamaoka, J., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., Yu, G. B., Yu, I., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: We present a precision measurement of the top-quark mass using the full sample of Tevatron $\sqrt{s}=1.96$ TeV proton-antiproton collisions collected by the CDF II detector, corresponding to an integrated luminosity of 8.7 $fb^{-1}$. Using a sample of $t\bar{t}$ candidate events decaying into the lepton+jets channel, we obtain distributions of the top-quark masses and the invariant mass of two jets from the $W$ boson decays from data. We then compare these distributions to templates derived from signal and background samples to extract the top-quark mass and the energy scale of the calorimeter jets with {\it in situ} calibration. The likelihood fit of the templates from signal and background events to the data yields the single most-precise measurement of the top-quark mass, $\mtop = 172.85 $\pm$ 0.71 (stat) $\pm$ 0.85 (syst) GeV/c^{2}.$, Comment: submitted to Phys. Rev. Lett
Published: 2012
Full Text: View/download PDF

47. An inclusive search for the Higgs boson in the four-lepton final state at CDF

Author: Aaltonen, T., Gonzalez, B. Alvarez, Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Apresyan, A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bauer, G., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Binkley, M., Bisello, D., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Brisuda, A., Bromberg, C., Brucken, E., Bucciantonio, M., Budagov, J., Budd, H. S., Budd, S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chou, J. P., Chung, W. H., Chung, Y. S., Ciobanu, C. I., Ciocci, M. A., Clark, A., Clarke, C., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Almenar, C. Cuenca, Cuevas, J., Culbertson, R., Dagenhart, D., d'Ascenzo, N., Datta, M., de Barbaro, P., De Cecco, S., De Lorenzo, G., Dell'Orso, M., Deluca, C., Demortier, L., Deng, J., Deninno, M., Devoto, F., d'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dong, P., Dorigo, M., Dorigo, T., Ebina, K., Elagin, A., Eppig, A., Erbacher, R., Errede, D., Errede, S., Ershaidat, N., Eusebi, R., Fang, H. C., Farrington, S., Feindt, M., Fernandez, J. P., Ferrazza, C., Field, R., Flanagan, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Funakoshi, Y., Furic, I., Gallinaro, M., Galyardt, J., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giunta, M., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Grinstein, S., Grosso-Pilcher, C., Group, R. C., da Costa, J. Guimaraes, Gunay-Unalan, Z., Haber, C., Hahn, S. R., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Hewamanage, S., Hidas, D., Hocker, A., Hopkins, W., Horn, D., Hou, S., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jha, M. K., Jindariani, S., Johnson, W., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, H. W., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kimura, N., Kirby, M., Klimenko, S., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Krumnack, N., Kruse, M., Krutelyov, V., Kuhr, T., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lin, C. -J., Linacre, J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maeshima, K., Makhoul, K., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, C., Martinez, M., Martinez-Ballarin, R., Mastrandrea, P., Mattson, M. E., Mazzanti, P., McFarland, K. S., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Menzione, A., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Neubauer, M. S., Nielsen, J., Nodulman, L., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Griso, S. Pagan, Pagliarone, C., Palencia, E., Papadimitriou, V., Paramonov, A. A., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Poukhov, O., Prokoshin, F., Pronko, A., Ptohos, F., Pueschel, E., Punzi, G., Pursley, J., Rahaman, A., Ramakrishnan, V., Ranjan, N., Ray, J., Redondo, I., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Rossi, M., Rubbo, F., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sakumoto, W. K., Sakurai, Y., Santi, L., Sartori, L., Sato, K., Saveliev, V., Savoy-Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schmidt, M. P., Schmitt, M., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Sedov, A., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Sfyrla, A., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shiraishi, S., Shochet, M., Shreyber, I., Simonenko, A., Sinervo, P., Sissakian, A., Sliwa, K., Smith, J. R., Snider, F. D., Soha, A., Somalwar, S., Sorin, V., Squillacioti, P., Stancari, M., Stanitzki, M., Denis, R. St., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Ttito-Guzman, P., Tkaczyk, S., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tu, Y., Ukegawa, F., Uozumi, S., Varganov, A., Vasquez, J., Vazquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vizan, J., Vogel, M., Volpi, G., Wagner, P., Wagner, R. L., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Weinberger, M., Wester III, W. C., Whitehouse, B., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Wick, F., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamaoka, J., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., Yu, G. B., Yu, I., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: An inclusive search for the standard model Higgs boson using the four-lepton final state in proton-antiproton collisions produced by the Tevatron at sqrt(s) = 1.96 TeV is conducted. The data are recorded by the CDF II detector and correspond to an integrated luminosity of 9.7 /fb. Three distinct Higgs decay modes, namely ZZ, WW, and tau-tau, are simultaneously probed. Nine potential signal events are selected and found to be consistent with the background expectation. We set a 95% credibility limit on the production cross section times the branching ratio and subsequent decay to the four lepton final state for hypothetical Higgs boson masses between 120 GeV/c^2 and 300 GeV/c^2., Comment: 8 pages, 3 figures
Published: 2012
Full Text: View/download PDF

48. Search for a low mass Standard Model Higgs boson in the tau-tau decay channel in $p\bar{p}$ collisions at $\sqrt{s}$ = 1.96 TeV

Author: CDF Collaboration, Aaltonen, T., Gonzalez, B. Alvarez, Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Apresyan, A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bauer, G., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Binkley, M., Bisello, D., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Brisuda, A., Bromberg, C., Brucken, E., Bucciantonio, M., Budagov, J., Budd, H. S., Budd, S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Canepa, A., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chou, J. P., Chung, W. H., Chung, Y. S., Ciobanu, C. I., Ciocci, M. A., Clark, A., Clarke, C., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Almenar, C. Cuenca, Cuevas, J., Culbertson, R., Dagenhart, D., d'Ascenzo, N., Datta, M., de Barbaro, P., De Cecco, S., De Lorenzo, G., Dell'Orso, M., Deluca, C., Demortier, L., Deng, J., Deninno, M., Devoto, F., d'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dong, P., Dorigo, M., Dorigo, T., Ebina, K., Elagin, A., Eppig, A., Erbacher, R., Errede, D., Errede, S., Ershaidat, N., Eusebi, R., Fang, H. C., Farrington, S., Feindt, M., Fernandez, J. P., Ferrazza, C., Field, R., Flanagan, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Funakoshi, Y., Furic, I., Gallinaro, M., Galyardt, J., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giunta, M., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Grinstein, S., Grosso-Pilcher, C., Group, R. C., da Costa, J. Guimaraes, Gunay-Unalan, Z., Haber, C., Hahn, S. R., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Hewamanage, S., Hidas, D., Hocker, A., Hopkins, W., Horn, D., Hou, S., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jha, M. K., Jindariani, S., Johnson, W., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, H. W., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kimura, N., Kirby, M., Klimenko, S., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Krumnack, N., Kruse, M., Krutelyov, V., Kuhr, T., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lin, C. -J., Linacre, J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maeshima, K., Makhoul, K., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, C., Martinez, M., Martinez-Ballarin, R., Mastrandrea, P., Mattson, M. E., Mazzanti, P., McFarland, K. S., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Menzione, A., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Neubauer, M. S., Nielsen, J., Nodulman, L., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Griso, S. Pagan, Pagliarone, C., Palencia, E., Papadimitriou, V., Paramonov, A. A., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Poukhov, O., Prokoshin, F., Pronko, A., Ptohos, F., Pueschel, E., Punzi, G., Pursley, J., Rahaman, A., Ramakrishnan, V., Ranjan, N., Ray, J., Redondo, I., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Rossi, M., Rubbo, F., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sakumoto, W. K., Sakurai, Y., Santi, L., Sartori, L., Sato, K., Saveliev, V., Savoy-Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schmidt, M. P., Schmitt, M., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Sedov, A., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Sfyrla, A., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shiraishi, S., Shochet, M., Shreyber, I., Simonenko, A., Sinervo, P., Sissakian, A., Sliwa, K., Smith, J. R., Snider, F. D., Soha, A., Somalwar, S., Sorin, V., Squillacioti, P., Stancari, M., Stanitzki, M., Denis, R. St., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Ttito-Guzman, P., Tkaczyk, S., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tu, Y., Ukegawa, F., Uozumi, S., Varganov, A., Vazquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vizan, J., Vogel, M., Volpi, G., Wagner, P., Wagner, R. L., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Weinberger, M., Wester III, W. C., Whitehouse, B., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Wick, F., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamaoka, J., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., Yu, G. B., Yu, I., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: We report on a search for the standard model Higgs boson decaying into pairs of tau leptons in $p\bar{p}$ collisions produced by the Tevatron at $\sqrt{s}$ = 1.96 TeV. The analyzed data sample was recorded by the CDFII detector and corresponds to an integrated luminosity of 6.0 fb$^{-1}$. The search is performed in the final state with one tau decaying leptonically and the second one identified through its semi-hadronic decay.Since no significant excess is observed, a 95% credibility level upper limit on the production cross section times branching ratio to the tau-tau final state is set for hypothetical Higgs boson masses between 100 and 150 GeV/$c^2$. For a Higgs boson of 120 GeV/$c^2$ the observed (expected) limit is 14.6 (15.3) the predicted value., Comment: 8 pages, 3 figures, submitted to Phys. Rev. Lett
Published: 2012
Full Text: View/download PDF

49. Search for Standard Model Higgs Boson Production in Association with a W Boson Using a Matrix Element Technique at CDF in p-bar{p} Collisions at sqrt{s} = 1.96 TeV

Author: CDF Collaboration, Aaltonen, T., Gonzalez, B. Alvarez, Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Apresyan, A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bauer, G., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Binkley, M., Bisello, D., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Brisuda, A., Bromberg, C., Brucken, E., Bucciantonio, M., Budagov, J., Budd, H. S., Budd, S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chou, J. P., Chung, W. H., Chung, Y. S., Ciobanu, C. I., Ciocci, M. A., Clark, A., Clarke, C., Coibanu, C., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Almenar, C. Cuenca, Cuevas, J., Culbertson, R., Dagenhart, D., d'Ascenzo, N., Datta, M., de Barbaro, P., De Cecco, S., De Lorenzo, G., Dell'Orso, M., Deluca, C., Demortier, L., Deng, J., Deninno, M., Devoto, F., d'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dong, P., Dorigo, M., Dorigo, T., Ebina, K., Elagin, A., Eppig, A., Erbacher, R., Errede, D., Errede, S., Ershaidat, N., Eusebi, R., Fang, H. C., Farrington, S., Feindt, M., Fernandez, J. P., Ferrazza, C., Field, R., Flanagan, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Funakoshi, Y., Furic, I., Gallinaro, M., Galyardt, J., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giunta, M., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Grinstein, S., Grosso-Pilcher, C., Group, R. C., da Costa, J. Guimaraes, Gunay-Unalan, Z., Haber, C., Hahn, S. R., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Hewamanage, S., Hidas, D., Hocker, A., Hopkins, W., Horn, D., Hou, S., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jha, M. K., Jindariani, S., Johnson, W., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, H. W., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kimura, N., Kirby, M., Klimenko, S., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Krumnack, N., Kruse, M., Krutelyov, V., Kuhr, T., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lin, C. -J., Linacre, J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maeshima, K., Makhoul, K., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, C., Martinez, M., Martinez-Ballarin, R., Mastrandrea, P., Mattson, M. E., Mazzanti, P., McFarland, K. S., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Menzione, A., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Neubauer, M. S., Nielsen, J., Nodulman, L., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Griso, S. Pagan, Pagliarone, C., Palencia, E., Papadimitriou, V., Paramonov, A. A., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Poukhov, O., Prokoshin, F., Pronko, A., Ptohos, F., Pueschel, E., Punzi, G., Pursley, J., Rahaman, A., Ramakrishnan, V., Ranjan, N., Redondo, I., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Rossi, M., Rubbo, F., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sakumoto, W. K., Sakurai, Y., Santi, L., Sartori, L., Sato, K., Saveliev, V., Savoy-Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schmidt, M. P., Schmitt, M., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Sedov, A., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Sfyrla, A., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shiraishi, S., Shochet, M., Shreyber, I., Simonenko, A., Sinervo, P., Sissakian, A., Sliwa, K., Smith, J. R., Snider, F. D., Soha, A., Somalwar, S., Sorin, V., Squillacioti, P., Stancari, M., Stanitzki, M., Denis, R. St., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Ttito-Guzman, P., Tkaczyk, S., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tu, Y., Ukegawa, F., Uozumi, S., Varganov, A., Vazquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vizan, J., Vogel, M., Volpi, G., Wagner, P., Wagner, R. L., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Weinberger, M., Wester III, W. C., Whitehouse, B., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Wick, F., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamaoka, J., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., Yu, G. B., Yu, I., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: This paper presents a search for standard model Higgs boson production in association with a $W$ boson using events recorded by the CDF experiment in a dataset corresponding to an integrated luminosity of 5.6 fb-1. The search is performed using a matrix element technique in which the signal and background hypotheses are used to create a powerful discriminator. The discriminant output distributions for signal and background are fit to the observed events using a binned likelihood approach to search for the Higgs boson signal. We find no evidence for a Higgs boson, and 95% confidence level (C.L.) upper limits are set on the Higgs boson production rate. The observed limits range from 3.5 to 37.6 relative to the standard model expectation for Higgs boson masses between 100 and 150 GeV. The 95% C.L. expected limit is estimated from the median of an ensemble of simulated experiments and varies between 2.9 and 32.7 relative to the production rate predicted by the standard model over the Higgs boson mass range studied.
Published: 2011
Full Text: View/download PDF

50. Measurement of ZZ production in leptonic final states at {\surd}s of 1.96 TeV at CDF

Author: Aaltonen, T., Gonzalez, B. Alvarez, Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Apresyan, A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bauer, G., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Binkley, M., Bisello, D., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Brisuda, A., Bromberg, C., Brucken, E., Bucciantonio, M., Budagov, J., Budd, H. S., Budd, S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chou, J. P., Chung, W. H., Chung, Y. S., Ciobanu, C. I., Ciocci, M. A., Clark, A., Clarke, C., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Almenar, C. Cuenca, Cuevas, J., Culbertson, R., Dagenhart, D., d'Ascenzo, N., Datta, M., de Barbaro, P., De Cecco, S., De Lorenzo, G., Dell'Orso, M., Deluca, C., Demortier, L., Deng, J., Deninno, M., Devoto, F., d'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dong, P., Dorigo, M., Dorigo, T., Ebina, K., Elagin, A., Eppig, A., Erbacher, R., Errede, D., Errede, S., Ershaidat, N., Eusebi, R., Fang, H. C., Farrington, S., Feindt, M., Fernandez, J. P., Ferrazza, C., Field, R., Flanagan, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Funakoshi, Y., Furic, I., Gallinaro, M., Galyardt, J., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giunta, M., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Grinstein, S., Grosso-Pilcher, C., Group, R. C., da Costa, J. Guimaraes, Gunay-Unalan, Z., Haber, C., Hahn, S. R., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Hewamanage, S., Hidas, D., Hocker, A., Hopkins, W., Horn, D., Hou, S., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jha, M. K., Jindariani, S., Johnson, W., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, H. W., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kimura, N., Kirby, M., Klimenko, S., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Krumnack, N., Kruse, M., Krutelyov, V., Kuhr, T., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lin, C. -J., Linacre, J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maeshima, K., Makhoul, K., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, C., Martinez, M., Martinez-Ballarin, R., Mastrandrea, P., Mattson, M. E., Mazzanti, P., McFarland, K. S., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Menzione, A., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Neubauer, M. S., Nielsen, J., Nodulman, L., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Griso, S. Pagan, Pagliarone, C., Palencia, E., Papadimitriou, V., Paramonov, A. A., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Poukhov, O., Prokoshin, F., Pronko, A., Ptohos, F., Pueschel, E., Punzi, G., Pursley, J., Rahaman, A., Ramakrishnan, V., Ranjan, N., Ray, J., Redondo, I., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Rossi, M., Rubbo, F., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sakumoto, W. K., Sakurai, Y., Santi, L., Sartori, L., Sato, K., Saveliev, V., Savoy-Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schmidt, M. P., Schmitt, M., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Sedov, A., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Sfyrla, A., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shiraishi, S., Shochet, M., Shreyber, I., Simonenko, A., Sinervo, P., Sissakian, A., Sliwa, K., Smith, J. R., Snider, F. D., Soha, A., Somalwar, S., Sorin, V., Squillacioti, P., Stancari, M., Stanitzki, M., Denis, R. St., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Ttito-Guzman, P., Tkaczyk, S., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tu, Y., Ukegawa, F., Uozumi, S., Varganov, A., Vasquez, J., Vazquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vizan, J., Vogel, M., Volpi, G., Wagner, P., Wagner, R. L., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Weinberger, M., Wester III, W. C., Whitehouse, B., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Wick, F., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamaoka, J., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., Yu, G. B., Yu, I., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: In this paper we present a precise measurement of the total ZZ production cross section in pp collisions at {\surd}s= 1.96 TeV, using data collected with the CDF II detector corresponding to an integrated luminosity of approximately 6 fb-1. The result is obtained by combining separate measurements in the four-charged (lll'l'), and two-charged-lepton and two-neutral-lepton (llvv) decay modes of the Z. The combined measured cross section for pp {\to} ZZ is 1.64^(+0.44)_(-0.38) pb. This is the most precise measurement of the ZZ production cross section in 1.96 TeV pp collisions to date., Comment: submitted to Phys. Rev. Lett
Published: 2011
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