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First upper limits on the radar cross section of cosmic-ray induced extensive air showers
Abbasi, R.U.,Abe, M.,Abou Bakr Othman, M.,Abu-Zayyad, T.,Allen, M.,Anderson, R.,Azuma, R.,Barcikowski, E.,Belz, J.W.,Bergman, D.R.,Besson, D.,Blake, S.A.,Byrne, M.,Cady, R.,Chae, M.J.,Cheon, B.G.,Chib North-Holland 2017 Astroparticle physics Vol.87 No.-
<P>TARA (Telescope Array Radar) is a cosmic ray radar detection experiment colocated with Telescope Array, the conventional surface scintillation detector (SD) and fluorescence telescope detector (FD) near Delta, Utah, U.S.A. The TARA detector combines a 40 kW, 54.1 MHz VHF transmitter and high-gain transmitting antenna which broadcasts the radar carrier over the SD array and within the FD field of view, towards a 250 MS/s DAQ receiver. TARA has been collecting data since 2013 with the primary goal of observing the radar signatures of extensive air showers (EAS). Simulations indicate that echoes are expected to be short in duration (similar to 10 mu s) and exhibit rapidly changing frequency, with rates on the order 1 MHz/mu s. The EAS radar cross-section (RCS) is currently unknown although it is the subject of over 70 years of speculation. A novel signal search technique is described in which the expected radar echo of a particular air shower is used as a matched filter template and compared to waveforms obtained by triggering the radar DAQ using the Telescope Array fluorescence detector. No evidence for the scattering of radio frequency radiation by EAS is obtained to date. We report the first quantitative RCS upper limits using EAS that triggered the Telescope Array Fluorescence Detector. (C) 2016 Elsevier B.V. All rights reserved.</P>
MOA-2011-BLG-293Lb: A TEST OF PURE SURVEY MICROLENSING PLANET DETECTIONS
Yee, J. C.,Shvartzvald, Y.,Gal-Yam, A.,Bond, I. A.,Udalski, A.,Kozłowski, S.,Han, C.,Gould, A.,Skowron, J.,Suzuki, D.,Abe, F.,Bennett, D. P.,Botzler, C. S.,Chote, P.,Freeman, M.,Fukui, A.,Furusawa, K. IOP Publishing 2012 The Astrophysical journal Vol.755 No.2
<P>Because of the development of large-format, wide-field cameras, microlensing surveys are now able to monitor millions of stars with sufficient cadence to detect planets. These new discoveries will span the full range of significance levels including planetary signals too small to be distinguished from the noise. At present, we do not understand where the threshold is for detecting planets. MOA-2011-BLG-293Lb is the first planet to be published from the new surveys, and it also has substantial follow-up observations. This planet is robustly detected in survey+follow-up data (Delta chi(2) similar to 5400). The planet/host mass ratio is q = (5.3 similar to 0.2) x 10(-3). The best-fit projected separation is s = 0.548 +/- 0.005 Einstein radii. However, due to the s <-> s(-1) degeneracy, projected separations of s-1 are only marginally disfavored at Delta chi(2) = 3. A Bayesian estimate of the host mass gives M-L = 0.43(-0.17)(+0.27) M-circle dot, with a sharp upper limit of M-L < 1.2 M-circle dot from upper limits on the lens flux. Hence, the planet mass is m(p) = 2.4(-0.9)(+1.5) M-Jup, and the physical projected separation is either r(perpendicular to) similar or equal to 1.0 AU or r(perpendicular to) similar or equal to 3.4 AU. We show that survey data alone predict this solution and are able to characterize the planet, but the Delta chi(2) is much smaller (Delta chi(2) similar to 500) than with the follow-up data. The Delta chi(2) for the survey data alone is smaller than for any other securely detected planet. This event suggests a means to probe the detection threshold, by analyzing a large sample of events like MOA-2011-BLG-293, which have both follow-up data and high-cadence survey data, to provide a guide for the interpretation of pure survey microlensing data.</P>
Adachi, N.,Suzuki, K.,Kasai, K.,Hiroki, M.,Kume, S.,Nonaka, I.,Abe, A. Asian Australasian Association of Animal Productio 2000 Animal Bioscience Vol.13 No.3
Data of 15 multiparous Holstein cows kept at Ibaraki Prefectural Animal Experiment Station were collected from 10 weeks prepartum to 20 weeks postpartum. Cows were assigned randomly to a soybean meal (S8M) diet or a fish meal (FM) diet from 4 weeks before expected calving date to 20 weeks postpartum. Each diet was formulated to contain similar amounts of CP, ADF, and NDF. In the FM diet, 2.5 and 5% of fish meal were supplemented as total mixed rations in prepartum and postpartum periods, respectively. Compared to the SBM diet, undegraded intake protein (UIP) and Met were higher in the FM diet, but Lys was low. Body weight and dry matter intake were not affected by supplemental FM, and dry matter intake increased by 6 weeks postpartum and maintained constant after 7 weeks postpartum. Cows in the FM diet remained high milk production during the experimental period, but milk yield in the SBM diet decreased gradually after 6 weeks postpartum. Supplemental FM increased milk yield and protein yield from 10 to 20 weeks postpartum when FM intake was 1.19 kg/d, although milk protein was not improved. There were no significance differences in fat content and fat yield between FM and SBM diets. Supplemental FM had no effect on plasma glucose and urea-N at parturition and 7 weeks postpartum. Thus, the increased milk and protein yield may be due to the combination of carryover effect of supplemental UIP or Met in FM from 4 weeks prepartum to 10 weeks postpartum and direct effect of supplemental FM.
Belle Collaboration,Chen, W.T.,Abe, K.,Abe, K.,Adachi, I.,Aihara, H.,Anipko, D.,Aulchenko, V.,Bakich, A.M.,Barberio, E.,Bay, A.,Bedny, I.,Bitenc, U.,Bizjak, I.,Blyth, S.,Bondar, A.,Bozek, A.,Bracko, M North-Holland Pub. Co 2007 Physics letters: B Vol.651 No.1
K<SUB>S</SUB><SUP>0</SUP>K<SUB>S</SUB><SUP>0</SUP> production in two-photon collisions has been studied using a 397.6 fb<SUP>-1</SUP> data sample collected with the Belle detector at the KEKB e<SUP>+</SUP>e<SUP>-</SUP> collider. For the first time the cross sections are measured in the two-photon center-of-mass energy range between 2.4 GeV and 4.0 GeV and angular range |cosθ<SUP>*</SUP>|<0.6. Combining the results with measurements of γγ->K<SUP>+</SUP>K<SUP>-</SUP> from Belle, we observe that the cross section ratio σ(K<SUB>S</SUB><SUP>0</SUP>K<SUB>S</SUB><SUP>0</SUP>)/σ(K<SUP>+</SUP>K<SUP>-</SUP>) decreases from ∼0.13 to ∼0.01 with increasing energy. Signals for the χ<SUB>c0</SUB> and χ<SUB>c2</SUB> charmonium states are also observed.
IWASA, M.A.,OHDACHI, S.,HAN, S.-H.,OH, H.-S.,ABE, H.,SUZUKI, H. 濟州大學校 基礎科學硏究所 2003 基礎科學硏究 Vol.16 No.2
We revised the taxonomic status of a white-toothed shrew (Insectivora, Mammalia) on Cheju Island, South Korea, which has been regarded as japanese white-toothed shrew, Crodidura dsinezumi, by analyzing karyotype and restriction fragment length polymorphism (RFLP) for the nuclear ribosoma RNA gene(rDNA) spacer regions. Karyotype of a specimen of Crocidura from Cheju Island was the same as in lesser white-toothed shrew, C. suaveolens, from Tsushima Island and the Eurasian Continent, carrying 2n=40 and FN (fundamental arm number of diploid autosomal set) = 46, whereas C. dsinezumi from the Japanese Islands shows 2n=40 and FN=52. The rDNA-RFLP was examined in two specimens of Crocidura from Cheju Island, two C. dsinezumi from Japan (Honshu and Kyusuh), and one C. suaveolens from the Korean Peninsula, using six restriction sites with the 28S mouse rDNA probe. The shrews from Cheju Islnad possessed four restriction sites common to C. suaveolens from the Koeran Peninsula but only one site common to C. dsinezumi, indicating the shrews from Cheju Island are genetically more close but distinct from the Korean Penisula populations of C. suaveolens. From the results of karyotype and rDNA-RFLP, the specimens from Cheju Island can be regarded as C. suaveolens as a taxonomic unit. Nous avons re´vise´ le statut taxonomique d'une musaraigne a` dents blanched (Mammalia, Insectivora) de l'ile cheju, Core´e du Sud, qui a e´te´ conside´re´e comme la musaraigne japonaise a` dents blanches Crocidura dsinezumi d'apre's I'analyse de son caryotype et de restructuration du polymorphisme d'un fragment de longueur(RFLF) pour les re´gions plus espace´es du ge`ne ribosomal nucle´aire RNA (rDNA). Le caryotype d'un spe´cimen de Crocidura de l'ile Cheju e´tait le me^me qui celui de la petite Crocldura, C. suaveolens, de l'ile Tsushima et du continent eurasien qui a 2n=40 et NF=46, tandis que C. dsinezumi des i^les japonaises a 2n=40 te NF=52. Le rDNA-RFLP a e´te´ examine´ dans deux spe´cimens de Crocidura de l'ile Cheju, deux C. dsinezumi du Japon (Honshu et Kyushu), et un C. suavelens de la pe´ninsule de Core´e, utilisant six sites de restriction avec la sonde rDNA 285 de la souris. Les musaraignes de l'ile Cheju pre´sentent quatre sites de restriction en commun avec C. suaveolens de la pe´ninsule de Core´e, mais seulement un site en commun avec C. dsinezumi, ce qui indique que les musaraignes de l'ile de Cheju sont ge´ne´tiquement plus proches mais distinctes des population de C. suaveolens de la pe´ninsule de core´e. D'apre`s re´sultats du caryotype de RFLP et de rDNA, les spe´cimens de l'ile de Cheju peuvent e^tre regarde´s comme des C. suaveolens.
Abe, K.,Bronner, C.,Pronost, G.,Hayato, Y.,Ikeda, M.,Iyogi, K.,Kameda, J.,Kato, Y.,Kishimoto, Y.,Marti, Ll.,Miura, M.,Moriyama, S.,Nakahata, M.,Nakano, Y.,Nakayama, S.,Okajima, Y.,Orii, A.,Sekiya, H. American Astronomical Society 2017 The Astrophysical journal Vol.850 No.2
<P>We present the results of a search in the Super-Kamiokande (SK) detector for excesses of neutrinos with energies above a few GeV that are in the direction of the track events reported in IceCube. Data from all SK phases (SK-I through SK-IV) were used, spanning a period from 1996 April to 2016 April and corresponding to an exposure of 225 kiloton-years. We considered the 14 IceCube track events from a data set with 1347 livetime days taken from 2010 to 2014. We use Poisson counting to determine if there is an excess of neutrinos detected in SK in a 10 degrees search cone (5 degrees for the highest energy data set) around the reconstructed direction of the IceCube event. No significant excess was found in any of the search directions we examined. We also looked for coincidences with a recently reported IceCube multiplet event. No events were detected within a +/- 500 s time window around the first detected event, and no significant excess was seen from that direction over the lifetime of SK.</P>
Solar neutrino measurements in Super-Kamiokande-IV
Abe, K.,Haga, Y.,Hayato, Y.,Ikeda, M.,Iyogi, K.,Kameda, J.,Kishimoto, Y.,Marti, Ll.,Miura, M.,Moriyama, S.,Nakahata, M.,Nakajima, T.,Nakayama, S.,Orii, A.,Sekiya, H.,Shiozawa, M.,Sonoda, Y.,Takeda, A. American Physical Society 2016 Physical Review D Vol.94 No.5
<P>Upgraded electronics, improved water system dynamics, better calibration and analysis techniques allowed Super-Kamiokande-IV to clearly observe very low-energy B-8 solar neutrino interactions, with recoil electron kinetic energies as low as similar to 3.5 MeV. Super-Kamiokande-IV data-taking began in September of 2008; this paper includes data until February 2014, a total livetime of 1664 days. The measured solar neutrino flux is (2.308 +/- 0.020)(stat)(-0.040)(+0.039) (syst)) x 10(6)/(cm(2) sec) assuming no oscillations. The observed recoil electron energy spectrum is consistent with no distortions due to neutrino oscillations. An extended maximum likelihood fit to the amplitude of the expected solar zenith angle variation of the neutrino-electron elastic scattering rate in SK-IV results in a day/night asymmetry of (-3.6 +/- 1.6(stat) +/- 0.6(syst)%. The SK-IV solar neutrino data determine the solar mixing angle as sin(2)theta(12) = 0.327(-0.031)(+0.026), all SK solar data (SK-I, SK-II, SK III and SK-IV) measures this angle to be sin(2)theta(12) = 0.334(-0.023)(+0.027), the determined mass-squared splitting is Delta m(21)(2) = 4.8(-0.8)(+1.5) x 10(-5) eV(2).</P>
Abe, K.,Hieda, K.,Hiraide, K.,Hirano, S.,Kishimoto, Y.,Kobayashi, K.,Moriyama, S.,Nakagawa, K.,Nakahata, M.,Ogawa, H.,Oka, N.,Sekiya, H.,Shinozaki, A.,Suzuki, Y.,Takeda, A.,Takachio, O.,Ueshima, K.,Um North-Holland Pub. Co 2013 Physics letters: B Vol.719 No.1
A search for light dark matter using low-threshold data from the single phase liquid xenon scintillation detector XMASS, has been conducted. Using the entire 835 kg inner volume as target, the analysis threshold can be lowered to 0.3 keVee (electron-equivalent) to search for light dark matter. With low-threshold data corresponding to a 5591.4 kg@?day exposure of the detector and without discriminating between nuclear-recoil and electronic events, XMASS excludes part of the parameter space favored by other experiments.
Search for dark matter in the form of hidden photons and axion-like particles in the XMASS detector
Abe, K.,Hiraide, K.,Ichimura, K.,Kishimoto, Y.,Kobayashi, K.,Kobayashi, M.,Moriyama, S.,Nakahata, M.,Ogawa, H.,Sato, K.,Sekiya, H.,Suzuki, T.,Takachio, O.,Takeda, A.,Tasaka, S.,Yamashita, M.,Yang, B.S Elsevier 2018 Physics letters: B Vol.787 No.-
<P><B>Abstract</B></P> <P>Hidden photons and axion-like particles are candidates for cold dark matter if they were produced non-thermally in the early universe. We conducted a search for both of these bosons using 800 live-days of data from the XMASS detector with 327 kg of liquid xenon in the fiducial volume. No significant signal was observed, and thus we set constraints on the <SUP> α ′ </SUP> / α parameter related to kinetic mixing of hidden photons and the coupling constant <SUB> g A e </SUB> of axion-like particles in the mass range from 40 to 120 keV/ <SUP> c 2 </SUP> , resulting in <SUP> α ′ </SUP> / α < 6 × <SUP> 10 − 26 </SUP> and <SUB> g A e </SUB> < 4 × <SUP> 10 − 13 </SUP> . These limits are the most stringent over this mass range derived from both direct and indirect searches to date.</P>