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Sample records for gijutsu kiso koza

  1. Kiso Supernova Survey (KISS): Survey strategy

    NASA Astrophysics Data System (ADS)

    Morokuma, Tomoki; Tominaga, Nozomu; Tanaka, Masaomi; Mori, Kensho; Matsumoto, Emiko; Kikuchi, Yuki; Shibata, Takumi; Sako, Shigeyuki; Aoki, Tsutomu; Doi, Mamoru; Kobayashi, Naoto; Maehara, Hiroyuki; Matsunaga, Noriyuki; Mito, Hiroyuki; Miyata, Takashi; Nakada, Yoshikazu; Soyano, Takao; Tarusawa, Ken'ichi; Miyazaki, Satoshi; Nakata, Fumiaki; Okada, Norio; Sarugaku, Yuki; Richmond, Michael W.; Akitaya, Hiroshi; Aldering, Greg; Arimatsu, Ko; Contreras, Carlos; Horiuchi, Takashi; Hsiao, Eric Y.; Itoh, Ryosuke; Iwata, Ikuru; Kawabata, Koji S.; Kawai, Nobuyuki; Kitagawa, Yutaro; Kokubo, Mitsuru; Kuroda, Daisuke; Mazzali, Paolo; Misawa, Toru; Moritani, Yuki; Morrell, Nidia; Okamoto, Rina; Pavlyuk, Nikolay; Phillips, Mark M.; Pian, Elena; Sahu, Devendra; Saito, Yoshihiko; Sano, Kei; Stritzinger, Maximilian D.; Tachibana, Yutaro; Taddia, Francesco; Takaki, Katsutoshi; Tateuchi, Ken; Tomita, Akihiko; Tsvetkov, Dmitry; Ui, Takahiro; Ukita, Nobuharu; Urata, Yuji; Walker, Emma S.; Yoshii, Taketoshi

    2014-12-01

    The Kiso Supernova Survey (KISS) is a high-cadence optical wide-field supernova (SN) survey. The primary goal of the survey is to catch the very early light of a SN, during the shock breakout phase. Detection of SN shock breakouts combined with multi-band photometry obtained with other facilities would provide detailed physical information on the progenitor stars of SNe. The survey is performed using a 2.2° × 2.2° field-of-view instrument on the 1.05-m Kiso Schmidt telescope, the Kiso Wide Field Camera (KWFC). We take a 3-min exposure in g-band once every hour in our survey, reaching magnitude g ˜ 20-21. About 100 nights of telescope time per year have been spent on the survey since 2012 April. The number of the shock breakout detections is estimated to be of the order of 1 during our three-year project. This paper summarizes the KISS project including the KWFC observing setup, the survey strategy, the data reduction system, and CBET-reported SNe discovered so far by KISS.

  2. Star formation in Kiso measle galaxies

    NASA Astrophysics Data System (ADS)

    Elmegreen, Debra M.; Elmegreen, B. G.

    2012-05-01

    The Kiso sample of several thousand local ultraviolet-bright galaxies includes galaxies classified as irregular disk galaxies with large star-forming complexes (I,g). We selected a sample of all I,g galaxies with both Sloan Digital Sky Survey images and spectra. They contain up to several dozen giant clumps each, so we refer to them as measle galaxies. We determined ages and masses of the clumps based on a comparison of photometry with population synthesis models of cluster evolution. The spectra were used to determine global star formation rates. Several hundred clumps were measured in the sample, with masses ranging from 10^5 to several x10^8 solar masses, scaling with galaxy absolute g magnitude of -14 to -21 mag. The galaxies are starbursting, sitting above the Groth strip “main sequence” of star formation rate versus galaxy mass by an order of magnitude. These Kiso measle galaxies have 10x the star formation rates of the Kiso tadpole galaxies. We compare their clump luminosity distribution functions with normal disk galaxies.

  3. Hematological and biochemical reference values for the endangered kiso horse.

    PubMed

    Takasu, Masaki; Nagatani, Nana; Tozaki, Teruaki; Kakoi, Hironaga; Maeda, Masami; Murase, Tetsuma; Mukoyama, Harutaka

    2013-01-01

    To establish blood and biochemical references for the endangered Kiso horse, blood samples were collected from 111 adult Kiso horses, 74.5% of the existing breed. The samples were analyzed for 23 hematological and biochemical parameters to determine their means and standard deviations (SD). We compared the mean ± 2SD with the reference values cited in one of the most commonly used veterinary textbooks in Japan. The hematology of Kiso horses is characterized by lower erythrocyte count and hematocrit and hemoglobin levels. In addition, their serum biochemistry showed lower levels of aspartate transaminase, alkaline phosphatase, and γ-glutamyl transferase. Whether these propensities are attributed to breed-specific factors or are acquired factors remains unclear. Nevertheless, this study provides useful diagnostic indices for the endangered Kiso horse.

  4. Genetic characterization of the endangered Kiso horse using 31 microsatellite DNAs.

    PubMed

    Takasu, Masaki; Hiramatsu, Nana; Tozaki, Teruaki; Kakoi, Hironaga; Nakagawa, Takeru; Hasegawa, Telhisa; Huricha; Maeda, Masami; Murase, Tetsuma; Mukoyama, Harutaka

    2012-02-01

    In order to contribute to conservation of the endangered Kiso horse, we clarified their genetic information using 31 microsatellite DNAs, and genotyped 125 horses, 83% of the existing breed. First, we clarified the current status of the horses. The horses were confirmed to have experienced rapid loss of population causing a bottleneck, and their effective population size was much smaller than their census size. Moreover, the number of alleles (6.3), observed heterozygosity (0.674), and expected heterozygosity (0.662) were in the same range as other endangered horses all over the world. Therefore, although their inbreeding level was not so severe (F(is): -0.017), the Kiso horse is surely one of the endangered. Second, we obtained genetic information of individuals. This information allowed us to understand the genetic distance of individuals, and might help in development of a reproductive strategy concerning the genetic distance between the mating pairs. Moreover, there appeared to be 4 subpopulations of Kiso horse, and this result was in good agreement with their historical background. Third, we confirmed that the parentage test for identification using the 31 microsatellite DNAs was highly reliable (probability of exclusion: 0.999999993). This identification increases the reliability of stud certification, and is also helpful for effective management. Understanding the genetic diversity within the population and the relationships among individuals is important to ensuring effective management for maintenance of genetic variation, and this study may help in conservation of the endangered Kiso horse.

  5. Application of KISOS for the Monitoring Environmental Risks Assessment in Deep-water Gas Hydrate Test Production in the Ulleung Basin, East Sea of Korea

    NASA Astrophysics Data System (ADS)

    Lee, S. R.; Chun, J. H.

    2015-12-01

    Korea Institute of Geoscience and Mineral Resources (KIGAM) has developed the KIGAM Seafloor Observation System (KISOS) for the baseline studies in the monitoring gas hydrate test production in the deep-water (>2,000m) Ulleung Basin of the East Sea of Korea. The KISOS consists of an acoustic positioning system (USBL), altimeter, still camera, video camera, water sampler, measuring devices (dissolved methane, dissolved oxygen, turbidity, chlorophyll, and currents) mounted on the unmanned ROV, and a seafloor sediment collecting device. The ultimate goals of the seafloor monitoring are to assess environmental risks (gas leakage and production water/drilling discharge, and so on) which may occur during and after the gas hydrate test production drilling. The KISOS was applied to solely conduct baseline studies during the last three years. We will conduct the KIGAM seafloor monitoring system (KIMOS) of the Korean gas hydrate program in the future. The large scale of environmental monitoring program includes the environmental impact assessments such as seafloor disturbance and subsidence, detection of methane gas leakage around well and cold seep, methane bubbles and dissolved methane, change of marine environments, chemical factor variation of water column and seabed, diffusion of drilling mud and production water, and biological factors of biodiversity and marine habitats before and after production drilling test well and nearby areas. Topics that will cover include:1) configuration of KISOS and general layout/operational design of KIMOS, 2) numerical simulation of gas and materials transport using SIMAP/CHEMMAP + MUDMAP softwares, 3) sensitivity analysis such as gas leakage modeling, operational produced water discharge, and 4) modeling of drilling discharge with cuttings and mud. Key words: gas hydrate, environmental monitoring, KISOS, KIMOS, Ulleung Basin

  6. Faint meteor observation by large-format CMOS sensor with 1.05-m Kiso schmidt telescope

    NASA Astrophysics Data System (ADS)

    Watanabe, J.; Kasuga, T.; Terai, T.; Miyazaki, S.; Ohta, K.; Murooka, F.; Ohnishi, T.; Yamasaki, T.; Mito, H.; Aoki, T.; Soyano, T.; Tarusawa, K.; Matsunaga, N.; Sako, S.; Kobayashi, N.; Doi, M.; Enomoto, T.

    2014-07-01

    We tried to use a new high-sensitivity CMOS sensor of the world's largest size as a one-chip 20cmx 20cm square attached to the prime focus of the 1.05 m (F3.1) Schmidt telescope at the Kiso Observatory, University of Tokyo, for faint meteor observation. The resulting field of view was 3.3 by 3.3 degrees, with a limiting magnitude of about 12 in our preliminary analysis. Assuming the height of faint meteors at 100 km, the derived flux of sporadic meteors is about 5x10^{-4} km^{-2}s^{-1}. Although the analysis is still on going, it is clear that this CMOS sensor is useful and effective for observing faint meteors.

  7. KIGAM Seafloor Observation System (KISOS) for the baseline study in monitoring of gas hydrate test production in the Ulleung Basin, Korea

    NASA Astrophysics Data System (ADS)

    Lee, Sung-rock; Chun, Jong-hwa

    2013-04-01

    For the baseline study in the monitoring gas hydrate test production in the Ulleung Basin, Korea Institute of Geoscience and Mineral Resources (KIGAM) has developed the KIGAM Seafloor Observation System (KISOS) for seafloor exploration using unmanned remotely operated vehicle connected with a ship by a cable. The KISOS consists of a transponder of an acoustic positioning system (USBL), a bottom finding pinger, still camera, video camera, water sampler, and measuring devices (methane, oxygen, CTD, and turbidity sensors) mounted on the unmanned ROV, and a sediment collecting device collecting sediment on the seafloor. It is very important to monitoring the environmental risks (gas leakage and production water/drilling mud discharge) which may be occurred during the gas hydrate test production drilling. The KISOS will be applied to solely conduct baseline study with the KIGAM seafloor monitoring system (KIMOS) of the Korean gas hydrate program in the future. The large scale of environmental monitoring program includes the environmental impact assessment such as seafloor disturbance and subsidence, detection of methane gas leakage around well and cold seep, methane bubbles and dissolved methane, change of marine environments, chemical factor variation of water column and seabed, diffusion of drilling mud and production water, and biological factors of biodiversity and marine habitats before and after drilling test well and nearby areas. The design of the baseline survey will be determined based on the result of SIMAP simulation in 2013. The baseline survey will be performed to provide the gas leakage and production water/drilling mud discharge before and after gas hydrate test production. The field data of the baseline study will be evaluated by the simulation and verification of SIMAP simulator in 2014. In the presentation, the authors would like introduce the configuration of KISOS and applicability to the seafloor observation for the gas hydrate test production in

  8. Ultraviolet Spectra of Subluminous Objects Found in the Kiso Schmidt Survey and Systematic Reanalysis of the Archived Ultraviolet Spectra of White Dwarfs Observed with the IUE Satellite Under the Astrophysics Data Program (ADP)

    NASA Technical Reports Server (NTRS)

    Wegner, Gary A.

    1988-01-01

    Recent research under NASA grant NAG5-971 consisted of the performance of two projects in conjunction with the International Ultraviolet Explorer (IUE) satellites. These are: (1) to look at the ultraviolet spectra of subluminous stars identified from visual wavelength spectroscopy that had been originally discovered from the Kiso Schmidt survey for ultraviolet excess stars and (2) to carry out a systematic reanalysis of the archived IUE spectra of white dwarfs. This report presents information on the progress of the re-reduction of over 600 IUE white dwarf spectra and their subsequent analysis employing model atmospheres and the observation of the Kiso ultraviolet excess stars.

  9. A new substance (Yoshixol) with an interesting antibiotic mechanism from wood oil of Japanese traditional tree (Kiso-Hinoki), Chamaecyparis obtusa.

    PubMed

    Koyama, S; Yamaguchi, Y; Tanaka, S; Motoyoshiya, J

    1997-05-01

    1. A neutral wood oil was extracted from Chamaecyparis obtusa (Kiso-Hinoki), which has been trusted nationally and preserved historically in the central part of Japan (Kiso, Nagano). 2. Hinokitiol, or thujaplicin (C10H12O2), which has been believed to exist in Cupressaceae, was not found in this neutral wood oil. Some differences between the extracting processes of the natural products are discussed. 3. A new chemical substance (Yoshixol, 4,4-dimethyl-6-methylene-2-cyclohexen-1-one) was simulated by several criteria (details in the text) as a major candidate of the neutral wood oil from Chamaecyparis obtusa. Thus, Yoshixol was newly synthesized. 4. The antibiotic effects of hinokitiol, the neutral wood oil and Yoshixol on methicillin-resistant Staphylococcus aureus (MRSA) were examined bacteriologically and morphologically. 5. All of the aforementioned three test materials showed complete antibiotic effects on MRSA by the bacteriological examination. However, the morphological findings showed entirely different aspects of cell death. 6. Hinokitiol caused an aggregative, degenerative and/or necrotic aspect, but the neutral wood oil and Yoshixol produced characteristic aspects: separation of contacted cells, blebbing, bugging-like eruption, formation of granules and an extensive reduction of individual cell size of MRSA. 7. Yoshixol was able to enhance those antibiotic effects on MRSA distinctly more than the neutral wood oil. 8. Yoshixol also showed a strong antibiotic effect on Escherichia coli, Mycobacterium chelonei, Pseudomonas aureginosa and Candida albicans. Morphological observations of those bacilli after Yoshixol revealed characteristic aspects of separation of contacted cells, bugging-like swelling, granulation, ballooning and reduction of cell size. 9. A possible mechanism of Yoshixol is discussed in regard to a molecular orbital theory on the basis of its electron orbits and to a thermodynamic interaction with the prokaryotic cell membrane. On the basis

  10. Apoptosis-like (possible quantum thermodynamic) cell death induced by Yoshixol and wood oil of Chamaecyparis obtusa (Kiso-Hinoki) on HeLa cell.

    PubMed

    Koyama, S; Tanaka, S; Yamaguchi, Y; Motoyoshya, J

    1997-05-01

    1. We report on the cytotoxic effects of neutral wood oil extracted from Chamaecyparis obtusa (Kiso-Hinoki) and of the newly synthetized substance Yoshixol (4,4-dimethyl-6-methylene-2-cyclohexen-1-one) on cultured HeLa cells. 2. The neutral wood oil produced cell death, led to the formation of granules, which were connected with fibrous networks, and reduced cell size. 3. Yoshixol caused a separation of cells, granulation, formation of high-density materials (probably apoptotic body), and reduction of cell size. 4. DNA fragmentation on the electrophoresis was observed with Yoshixol. A low-molecular-weight smear band appeared in the supernatant after treatment with the neutral wood oil. Neither treatment showed higher lactate dehydrogenase (LDH) activity in the culture medium than seen with ethanol as a control. 5. These findings suggest that both the neutral wood oil and Yoshixol have a similar cytotoxic mechanism, reducing cell size and producing a granulation (fragmentation) of eukaryotic cells. 6. Yoshixol may be a potent antitumor agent that induces apoptotic-like cell death. This possible mechanism is discussed.

  11. Ultraviolet Spectra of Two Magnetic White Dwarfs and Ultraviolet Spectra of Subluminous Objects Found in the Kiso Schmidt Survey and Ultraviolet Absorptions in the Spectra of DA White Dwarfds

    NASA Technical Reports Server (NTRS)

    Wegner, Gary A.

    1988-01-01

    Research under NASA Grant NAG5-287 has carried out a number of projects in conjunction with the International Ultraviolet Explorer (IUE) satellite. These include: (1) studies of the UV spectra of DA white dwarfs which show quasi-molecular bands of H2 and H2(+); (2) the peculiar star HR6560; (3) the UV spectra of two magnetic white dwarfs that also show the quasi-molecular features; (4) investigations of the UV spectra of subluminous stars, primarily identified from visual wavelength spectroscopy in the Kiso survey of UV excess stars, some of which show interesting metal lines in their UV spectra; and (5) completion of studies of UV spectra of DB stars. The main result of this research has been to further knowledge of the structure and compositions of subluminous stars which helps cast light on their formation and evolution.

  12. Occupational and Employment Characteristics of Post-War Japanese Immigrants in Metropolitan Vancouver.

    ERIC Educational Resources Information Center

    Ujimoto, K. Victor

    The universe of Japanese immigrants selected for this study consisted of a diverse group such as the kika nisei (returned second generation), the yobiyose (sponsored immigrant), and the gijutsu imin (technical immigrant). Each group possessed different characteristics. This present paper is limited in scope to the yobiyose and gijutsu imin because…

  13. JPRS Report, Science & Technology, Japan.

    DTIC Science & Technology

    2007-11-02

    Telecommunications Terminal System Discussed [Takahiro Kawazoe; JIDOSHA GIJUTSU, Feb 88] 81 Development of Hand -Free Mobile Phone Reported [Nobuyuki Ishihara...34 concept announced by President Reagan a month after that made the eyes of the space transport scientific technicians of the world turn again to the...Aerospace Laboratory, the National Space Science Laboratory, and NASDA. The "Space Plane Coordinating Committee" was created by these three

  14. A Response to Elizabeth Gould, "Nomadic Turns: Epistemology, Experience, and Women University Band Directors"

    ERIC Educational Resources Information Center

    Koza, Julia, Eklund

    2005-01-01

    In this response to Gould, the author has two goals: first, to forward another, not necessarily competing, postmodern understanding of feminism and power; and second, to expand Gould's project of examining professional climate. Koza defines feminism as a constellation of dynamic political positions that address and attempt to change the unequal…

  15. Listening for Whiteness: Hearing Racial Politics in Undergraduate School Music

    ERIC Educational Resources Information Center

    Koza, Julia Eklund

    2008-01-01

    This article describes how admissions auditions at schools of music may demonstrate and participate in what critical race theorist, Gloria Ladson-Billings, calls the full social funding of race. Julia Eklund Koza argues that the construction of musical difference, which is an effect of power and is accomplished by the materialization of styles of…

  16. My Body Had a Mind of Its Own: On Teaching, the Illusion of Control, and the Terrifying Limits of Governmentality (Part 2)

    ERIC Educational Resources Information Center

    Koza, Julia Eklund

    2010-01-01

    In the final installment of her two-part essay, Julia Eklund Koza analyzes prevalent control and management discourse in education, specifically, music education. Arguing that dominant understandings are hierarchical, gendered, illusory, and integrally related to projects and practices largely unrelated to schooling, she invites teachers and…

  17. MASSIVE CLUMPS IN LOCAL GALAXIES: COMPARISONS WITH HIGH-REDSHIFT CLUMPS

    SciTech Connect

    Elmegreen, Bruce G.; Elmegreen, Debra Meloy; Dewberry, J.; Putko, J.; Teich, Y.; Popinchalk, M.; Sanchez Almeida, J.; Munoz-Tunon, C.

    2013-09-01

    Local UV-bright galaxies in the Kiso survey include clumpy systems with kiloparsec-size star complexes that resemble clumpy young galaxies in surveys at high redshift. We compare clump masses and underlying disks in several dozen galaxies from each of these surveys to the star complexes and disks of normal spirals. Photometry and spectroscopy for the Kiso and spiral sample come from the Sloan Digital Sky Survey. We find that the largest Kiso clumpy galaxies resemble Ultra Deep Field (UDF) clumpies in terms of the star formation rates, clump masses, and clump surface densities. Clump masses and surface densities in normal spirals are smaller. If the clump masses are proportional to the turbulent Jeans mass in the interstellar medium, then for the most luminous galaxies in the sequence of normal:Kiso:UDF, the turbulent speeds and surface densities increase in the proportions 1.0:4.7:5.0 and 1.0:4.0:5.1, respectively, for fixed restframe B-band absolute magnitude. For the least luminous galaxies in the overlapping magnitude range, the turbulent speed and surface density trends are 1.0:2.7:7.4 and 1.0:1.4:3.0, respectively. We also find that while all three types have radially decreasing disk intensities when measured with ellipse-fit azimuthal averages, the average profiles are more irregular for UDF clumpies (which are viewed in their restframe UV) than for Kiso galaxies (viewed at g-band), and major axis intensity scans are even more irregular for the UDF than Kiso galaxies. Local clumpy galaxies in the Kiso survey appear to be intermediate between UDF clumpies and normal spirals.

  18. Effects of Cardiopulmonary Bypass on Hemostasis

    DTIC Science & Technology

    2007-11-02

    agents as possible alternatives to heparin anticoagulation during CPB. Some of the agents mat have been found to be promising in these studies...67-76. 22Q. Terrell MR, Walenga JM, Koza MJ, et al. Efficacy of aprotinin with various anticoagulant agents in cardiopulmonary bypass. AnnThorac Surg...procedures, systemic anticoagulation with 3mg/kg of heparin prior to the institution of CPB elicits a modest but significant prolongation of the

  19. System and Method for Tracking Vehicles Using Random Search Algorithms.

    DTIC Science & Technology

    1997-01-31

    patent application is available for licensing. Requests for information should be addressed to: OFFICE OF NAVAL RESEARCH DEPARTMENT OF THE NAVY...relates to a system and a method for 22 tracking vehicles using random search algorithm methodolgies . 23 (2) Description of the Prior Art 24 Contact...algorithm methodologies for finding peaks in non-linear 14 functions. U.S. Patent No. 5,148,513 to Koza et al., for 15 example, relates to a non-linear

  20. Multimedia-Based Integration of Cross-Layer Techniques

    DTIC Science & Technology

    2014-06-01

    spectrum access/ cognitive radio wireless networks: A survey ,” Computer Networks, vol. 50, pp. 2127-2159, 2006. 16. “XG Communications Program ...Nonlinear Integer Programming . International Series in Operations Research and Management Science, Springer, USA, 2006. 43. F. Li and G. Liu...Natural and Artificial Systems. MIT press Cambridge, MA, 1992. 89. J. R. Koza, “ Survey of Genetic Algorithms and Genetic Programming ,” WESCON

  1. Pre-discovery observations of MASTER OT J004514.13+420007.2

    NASA Astrophysics Data System (ADS)

    Maehara, Hiroyuki

    2016-01-01

    I report pre-discovery observations of the possible nova in M31 MASTER OT J004514.13+420007.2 (ATel # 8603). The observations were performed with the 1.05-m Schmidt telescope and KWFC (Sako et al. 2012, SPIE, 8446, 84466L) at Kiso Observatory.

  2. Discovery of a Possible Nova in M31

    NASA Astrophysics Data System (ADS)

    Maehara, Hiroyuki

    2016-11-01

    We report the discovery of a possible nova in M31 on V-band CCD images taken on 2016-11-12.372 UT with the 1.05-m Schmidt telescope and KWFC (Sako et al. 2012, SPIE, 8446, 84466L) at Kiso Observatory, the University of Tokyo.

  3. [A short biography of Ashihara Kengyo].

    PubMed

    Oura, Hiromasa

    2005-03-01

    Ashihara Kengyo was one of the most famous acupuncturists of the latter part of the Edo period. He wrote the book Shindo Happi on acupuncture theory. He was blind, but he was unrivaled when it came to acupuncture. As a result, he became the medical doctor for the feudal government and treated the shogun Tokugawa Ienari and many daimyos.He was a descendant of Kiso Yoshinaka, who was a famous samurai of the Kamakura era. Thus he re-established the Kiso family name, and always held a service for his ancestors.I investigated the history of Ashihara Kengyo, on the basis of the data I found on "Kisoshi Karoku". As a result, I discovered a wooden statute of him and many related historical spots.

  4. A search for ultraviolet-excess objects (Kondo, Noguchi, and Maehara 1984): Documentation for the machine-readable version

    NASA Technical Reports Server (NTRS)

    Warren, Wayne H., Jr.

    1990-01-01

    A list of 1186 ultraviolet-excess objects (designated KUV) was compiled as a result of a search conducted with the 105-cm Schmidt telescope of the Kiso station of the Tokyo Astronomical Observatory. This document describes the machine readable version of the KUV survey list and presents a sample listing showing the logical records as they are recorded in the machine readable catalog. The KUV data include equatorial coordinates, magnitudes, color indices, and identifications for previously cataloged objects.

  5. [Development of analysis software package for the two kinds of Japanese fluoro-d-glucose-positron emission tomography guideline].

    PubMed

    Matsumoto, Keiichi; Endo, Keigo

    2013-06-01

    Two kinds of Japanese guidelines for the data acquisition protocol of oncology fluoro-D-glucose-positron emission tomography (FDG-PET)/computed tomography (CT) scans were created by the joint task force of the Japanese Society of Nuclear Medicine Technology (JSNMT) and the Japanese Society of Nuclear Medicine (JSNM), and published in Kakuigaku-Gijutsu 27(5): 425-456, 2007 and 29(2): 195-235, 2009. These guidelines aim to standardize PET image quality among facilities and different PET/CT scanner models. The objective of this study was to develop a personal computer-based performance measurement and image quality processor for the two kinds of Japanese guidelines for oncology (18)F-FDG PET/CT scans. We call this software package the "PET quality control tool" (PETquact). Microsoft Corporation's Windows(™) is used as the operating system for PETquact, which requires 1070×720 image resolution and includes 12 different applications. The accuracy was examined for numerous applications of PETquact. For example, in the sensitivity application, the system sensitivity measurement results were equivalent when comparing two PET sinograms obtained from the PETquact and the report. PETquact is suited for analysis of the two kinds of Japanese guideline, and it shows excellent spec to performance measurements and image quality analysis. PETquact can be used at any facility if the software package is installed on a laptop computer.

  6. Development of public science archive system of Subaro Telescope. 2

    NASA Astrophysics Data System (ADS)

    Yamamoto, Naotaka; Noda, Sachiyo; Taga, Masatoshi; Ozawa, Tomohiko; Horaguchi, Toshihiro; Okumura, Shin-Ichiro; Furusho, Reiko; Baba, Hajime; Yagi, Masafumi; Yasuda, Naoki; Takata, Tadafumi; Ichikawa, Shin-Ichi

    2003-09-01

    We report various improvements in a public science archive system, SMOKA (Subaru-Mitaka-Okayama-Kiso Archive system). We have developed a new interface to search observational data of minor bodies in the solar system. In addition, the other improvements (1) to search frames by specifying wavelength directly, (2) to find out calibration data set automatically, (3) to browse data on weather, humidity, and temperature, which provide information of image quality, (4) to provide quick-look images of OHS/CISCO and IRCS, and (5) to include the data from OAO HIDES (HIgh Dispersion Echelle Spectrograph), are also summarized.

  7. Mean-field approaches for Ξ- hypernuclei and current experimental data

    NASA Astrophysics Data System (ADS)

    Sun, T. T.; Hiyama, E.; Sagawa, H.; Schulze, H.-J.; Meng, J.

    2016-12-01

    Motivated by the recently observed hypernucleus (Kiso event) C15Ξ (14N+Ξ- ), we identify the state of this system theoretically within the framework of the relativistic-mean-field and Skyrme-Hartree-Fock models. The Ξ N interactions are constructed to reproduce the two possibly observed Ξ- removal energies, 4.38 ±0.25 MeV or 1.11 ±0.25 MeV. The present result is preferable to be 14N(g .s .) +Ξ-(1 p ) , corresponding to the latter value.

  8. Observations of minor planets.

    NASA Astrophysics Data System (ADS)

    Observations made at the following stations are published: Bucharest, Catania, Caussols, Cent. Astron. Yebes, Cerro Tololo Interam. Obs., Chirorin, Crimean Astrophys. Obs. (52nd Report), Eur. South. Obs., Falkensee, Geisei, Goethe Link Obs., Göttingen, Haute Provence, Hemingford Abbots, JCPM Oi Stn., Kambah (near Canberra), Kitt Peak, Klet', Le Creusot, Lick Obs., Lincoln Lab., Lowell Obs., Lowell Obs. Anderson Mesa Stn., Madonnna di Dossobuono, Mt. John Obs., Mt. Palomar, Oak Ridge Obs., Purple Mountain Obs., Quonochontaug Stn. (Rhode Island), Reintal, S. Vittore (Bologna), Seewalchen, Siding Spring, Skalnaté Pleso, Spec. Astrophys. Obs., Steward Obs., Sydney, Tautenburg, Telford, Tokyo Obs. Kiso Stn., Turku, Zimmerwald.

  9. High dissolved methane concentrations in the deep-water Ulleung Basin, East Sea of Korea

    NASA Astrophysics Data System (ADS)

    Ryu, Byong-Jae; Chun, Jong-Hwa

    2014-05-01

    As a part of the Korean National Gas Hydrate Program, a production test in the Ulleung Basin is planned to be performed in 2015. The targets are the gas hydrate-bearing sand reservoirs, which were found during the Second Ulleung Basin Gas Hydrate Drilling Expedition (UBGH2) in 2010. To ensure a safe production test, an environmental program has been conducted by the Korea Institute of Geoscience and Mineral Resources (KIGAM) since 2012. This program includes a baseline survey using a KIGAM Seafloor Observation System (KISOS) and R/V TAMHAE II of KIGAM, development of a KIGAM Seafloor Monitoring System (KIMOS), and seafloor monitoring on various potential hazards associated with the dissociated gas from gas hydrates using the KIMOS during the production test. A survey for measuring the dissolved methane concentrations in the area at and nearby the gas hydrate production testing site was performed using R/V TAMHAE II and the KISOS. The water samples were also collected and analyzed to measure the dissolved methane concentrations by the SBE carousel water sampler installed in the KISOS and gas chromatography (GC) at KIGAM. The dissolved methane concentrations were also measured using a Frantech METS methane sensor installed in the KISOS. No dissolved methane anomaly was detected at the site where any evidence of gas hydrate presence has not been observed. On the other hand, the water analysis showed high dissolved methane concentrations at the water depth above and within the gas hydrate stability zone (GHSZ) at the site where gas hydrates were identified by drilling. However, these dissolved methane anomalies within the GHSZ were not detected by methane sensor. To examine these uncertain dissolved methane anomalies within the GHSZ, the water samples will be collected and analyzed once again, and the analytical result will be also carefully compared with the data collected using the methane sensor and deep ocean mass spectrometer (DOMS) developed by the University of

  10. Mixed Anion Heterostructure Materials

    DTIC Science & Technology

    2004-10-01

    data presented Sb(g) Sb(ads) Sb(s) Kads D (1) (2)Very low + GaAs no reaction ( 3 ) kexch 33 for As2 which indicates that the...Kads D (1) (2) ( 3 ) Anion Exchange kexch (4) Isoelectronic AsSb formation Favoured by As4 +As GaAsySb1-y + Sby(s) GaSb1-y + AsSby(s) +As kiso (5...experiment implemented for this investigation provided a basis for modeling the P(g) P(ads) P(s) + GaAs Kads D (1) (2) ( 3 ) kexch (4) +P GaPyAs1-y

  11. Mosaic CCD method: A new technique for observing dynamics of cometary magnetospheres

    NASA Technical Reports Server (NTRS)

    Saito, T.; Takeuchi, H.; Kozuba, Y.; Okamura, S.; Konno, I.; Hamabe, M.; Aoki, T.; Minami, S.; Isobe, S.

    1992-01-01

    On April 29, 1990, the plasma tail of Comet Austin was observed with a CCD camera on the 105-cm Schmidt telescope at the Kiso Observatory of the University of Tokyo. The area of the CCD used in this observation is only about 1 sq cm. When this CCD is used on the 105-cm Schmidt telescope at the Kiso Observatory, the area corresponds to a narrow square view of 12 ft x 12 ft. By comparison with the photograph of Comet Austin taken by Numazawa (personal communication) on the same night, we see that only a small part of the plasma tail can be photographed at one time with the CCD. However, by shifting the view on the CCD after each exposure, we succeeded in imaging the entire length of the cometary magnetosphere of 1.6 x 10(exp 6) km. This new technique is called 'the mosaic CCD method'. In order to study the dynamics of cometary plasma tails, seven frames of the comet from the head to the tail region were twice imaged with the mosaic CCD method and two sets of images were obtained. Six microstructures, including arcade structures, were identified in both the images. Sketches of the plasma tail including microstructures are included.

  12. Isostatic gravity map of the Monterey 30 x 60 minute quadrangle and adjacent areas, California

    USGS Publications Warehouse

    Langenheim, V.E.; Stiles, S.R.; Jachens, R.C.

    2002-01-01

    The digital dataset consists of one file (monterey_100k.iso) containing 2,385 gravity stations. The file, monterey_100k.iso, contains the principal facts of the gravity stations, with one point coded per line. The format of the data is described below. Each gravity station has a station name, location (latitude and longitude, NAD27 projection), elevation, and an observed gravity reading. The data are on the IGSN71 datum and the reference ellipsoid is the Geodetic Reference System 1967 (GRS67). The free-air gravity anomalies were calculated using standard formulas (Telford and others, 1976). The Bouguer, curvature, and terrain corrections were applied to the free-air anomaly at each station to determine the complete Bouguer gravity anomalies at a reduction density of 2.67 g/cc. An isostatic correction was then applied to remove the long-wavelength effect of deep crustal and/or upper mantle masses that isostatically support regional topography.

  13. J-GEM follow-up observations to search for an optical counterpart of the first gravitational wave source GW150914

    NASA Astrophysics Data System (ADS)

    Morokuma, Tomoki; Tanaka, Masaomi; Asakura, Yuichiro; Abe, Fumio; Tristram, Paul J.; Utsumi, Yousuke; Doi, Mamoru; Fujisawa, Kenta; Itoh, Ryosuke; Itoh, Yoichi; Kawabata, Koji S.; Kawai, Nobuyuki; Kuroda, Daisuke; Matsubayashi, Kazuya; Motohara, Kentaro; Murata, Katsuhiro L.; Nagayama, Takahiro; Ohta, Kouji; Saito, Yoshihiko; Tamura, Yoichi; Tominaga, Nozomu; Uemura, Makoto; Yanagisawa, Kenshi; Yatsu, Yoichi; Yoshida, Michitoshi

    2016-08-01

    We present our optical follow-up observations to search for an electromagnetic counterpart of the first gravitational wave source GW150914 in the framework of the Japanese collaboration for Gravitational wave ElectroMagnetic follow-up (J-GEM), which is an observing group utilizing optical and radio telescopes in Japan, as well as in New Zealand, China, South Africa, Chile, and Hawaii. We carried out a wide-field imaging survey with the Kiso Wide Field Camera (KWFC) on the 1.05 m Kiso Schmidt telescope in Japan and a galaxy-targeted survey with Tripole5 on the B&C 61 cm telescope in New Zealand. Approximately 24 deg2 regions in total were surveyed in i-band with KWFC and 18 nearby galaxies were observed with Tripole5 in g-, r-, and i-bands 4-12 days after the gravitational wave detection. Median 5 σ depths are i ˜ 18.9 mag for the KWFC data and g ˜ 18.9 mag, r ˜ 18.7 mag, and i ˜ 18.3 mag for the Tripole5 data. The probability for a counterpart to be in the observed area is 1.2% in the initial skymap and 0.1% in the final skymap. We do not find any transient source associated to an external galaxy with spatial offset from its center, which is consistent with the local supernova rate.

  14. Emergent system identification using particle swarm optimization

    NASA Astrophysics Data System (ADS)

    Voss, Mark S.; Feng, Xin

    2001-10-01

    Complex Adaptive Structures can be viewed as a combination of Complex Adaptive Systems and fully integrated autonomous Smart Structures. Traditionally when designing a structure, one combines rules of thumb with theoretical results to develop an acceptable solution. This methodology will have to be extended for Complex Adaptive Structures, since they, by definition, will participate in their own design. In this paper we introduce a new methodology for Emergent System Identification that is concerned with combining the methodologies of self-organizing functional networks (GMDH - Alexy G. Ivakhnenko), Particle Swarm Optimization (PSO - James Kennedy and Russell C. Eberhart) and Genetic Programming (GP - John Koza). This paper will concentrate on the utilization of Particle Swarm Optimization in this effort and discuss how Particle Swarm Optimization relates to our ultimate goal of emergent self-organizing functional networks that can be used to identify overlapping internal structural models. The ability for Complex Adaptive Structures to identify emerging internal models will be a key component for their success.

  15. The solar wind structure that caused a large-scale disturbance of the plasma tail of comet Austin

    NASA Technical Reports Server (NTRS)

    Kozuka, Yukio; Konno, Ichishiro; Saito, Takao; Numazawa, Shigemi

    1992-01-01

    The plasma tail of Comet Austin (1989c1) showed remarkable disturbances because of the solar maximum periods and its orbit. Figure 1 shows photographs of Comet Austin taken in Shibata, Japan, on 29 Apr. 1990 UT, during about 20 minutes with the exposure times of 90 to 120 s. There are two main features in the disturbance; one is many bowed structures, which seem to move tailwards; and the other is a large-scale wavy structure. The bowed structures can be interpreted as arcade structures brushing the surface of both sides of the cometary plasma surrounding the nucleus. We identified thirteen structures of the arcades from each of the five photographs and calculated the relation between the distance of each structure from the cometary nucleus, chi, and the velocity, upsilon. The result is shown. This indicates that the velocity of the structures increases with distance. This is consistent with the result obtained from the observation at the Kiso Observatory.

  16. Role of environmental factors in autoantibody production - importance of a detailed analysis in a small cohort

    PubMed Central

    2012-01-01

    In the previous issue of Arthritis Research & Therapy, Muro and colleagues reported a detailed epidemiologic analysis in central Japan on one of the new myositis-specific autoantibodies to MDA-5 (melanoma differentiation-associated gene 5), which is associated with clinically amyopathic dermatomyositis accompanying interstitial lung disease. The increasing prevalence of anti-MDA-5, higher prevalence in small rural towns, and geographical clustering in two areas along the Kiso River suggest a role of environmental factors associated with rural communities or the river/water system or both. A detailed analysis of a small cohort may offer clues, which is ignored in multi-center studies, to the pathogenesis of systemic rheumatic diseases and autoantibody production. PMID:22380573

  17. Emission-line stars in the Canis Major star-formation region

    NASA Astrophysics Data System (ADS)

    Wiramihardja, S. D.; Kogure, T.; Nakano, M.; Yoshida, S.

    Using the Schmidt telescope of the Kiso Observatory, H-alpha-emission stars have been surveyed in the Canis Major star-formation region and its adjacent reference area. In the area of about 58 square degrees a total of 179 H-alpha-emission stars have been found in the magnitude range between V = 6 and 15 with a majority in the V = 11-14 range. Based on the color properties and on the location relative to the CMa R1 association, the stars are provisionally classified into two main groups of early-type H-alpha-emission stars and of T Tauri candidates. It is found that the early-type H-alpha-emission stars are distributed rather uniformly over the survey area in contrast to the group of T Tauri candidates which show good coincidence with the CMa R1 association in the surface distribution.

  18. The time-dependence of the defective nature of ice Ic (cubic ice) and its implications for atmospheric science

    NASA Astrophysics Data System (ADS)

    Sippel, Christian; Koza, Michael M.; Hansen, Thomas C.; Kuhs, Werner F.

    2010-05-01

    flat low-indexed crystal faces. [1] T Kobayashi & T Kuroda (1987) Snow Crystals. In: Morphology of Crystals (ed. I Sunagawa), Terra Scientific Publishing, Tokyo, pp.649-743. [2] RS Gao & 19 other authors (2004) Evidence that nitric acid increases relative humidity in low-temperature cirrus clouds. Science 303, 516-520. [3] T Peter, C Marcolli, P Spichtinger, T Corti, MC Baker & T Koop (2006) When dry air is too humid. Science 314, 1399-1402. [4] JE Shilling, MA Tolbert, OB Toon, EJ Jensen, BJ Murray & AK Bertram (2006) Measurements of the vapor pressure of cubic ice and their implications for atmospheric ice clouds. Geophys.Res.Lett. 33, 026671. [5] TC Hansen, MM Koza & WF Kuhs (2008) Formation and annealing of cubic ice: I Modelling of stacking faults. J.Phys.Cond.Matt. 20, 285104. [6] TC Hansen, MM Koza, P Lindner & WF Kuhs (2008) Formation and annealing of cubic ice: II. Kinetic study. J.Phys.Cond.Matt. 20, 285105. [7] WF Kuhs, G Genov, DK Staykova & AN Salamatin, T Hansen (2004) Ice perfection and the onset of anomalous preservation of gas hydrates. Phys.Chem.Chem.Phys. 6, 4917-4920. [8] BJ Murray, DA Knopf & AK Bertram (2005) The formation of cubic ice under conditions relevant to Earth's atmosphere. Nature 434, 292-205.

  19. The defective nature of ice Ic and its implications for atmospheric science

    NASA Astrophysics Data System (ADS)

    Kuhs, W. F.; Hansen, T. C.

    2009-04-01

    ) Evidence that nitric acid increases relative humidity in low-temperature cirrus clouds. Science 303, 516-520. [4] T Peter, C Marcolli, P Spaichinger, T Corti, MC Baker & T Koop (2006) When dry air is too humid. Science 314, 1399-1402. [5] JE Shilling, MA Tolbert, OB Toon, EJ Jensen, BJ Murray & AK Bertram (2006) Measurements of the vapor pressure of cubic ice and their implications for atmospheric ice clouds. Geophys.Res.Lett. 33, 026671. [6] TC Hansen, MM Koza & WF Kuhs (2008) Formation and annealing of cubic ice: I Modelling of stacking faults. J.Phys.Cond.Matt. 20, 285104. [7] TC Hansen, MM Koza, P Lindner & WF Kuhs (2008) Formation and annealing of cubic ice: II. Kinetic study. J.Phys.Cond.Matt. 20, 285105. [8] WF Kuhs, G Genov, DK Staykova & AN Salamatin (2004) Ice perfection and the onset of anomalous preservation of gas hydrates. Phys.Chem.Chem.Phys. 6, 4917-4920. [9] BJ Murray, DA Knopf & AK Bertram (2005) The formation of cubic ice under conditions relevant to Earth's atmosphere. Nature 434, 292-205.

  20. Silicon and oxygen isotopic trends in Mesozoic radiolarites

    NASA Astrophysics Data System (ADS)

    Bôle, Maximlien; Baumgartner Peter, O.; Lukas, Baumgartner; Anne-Sophie, Bouvier; Rie, Hori; Masayuki, Ikeda

    2016-04-01

    Silicon and oxygen isotopes (δ30Si and δ18O) of siliceous tests (diatoms, sponges and radiolarians) preserve environmental signatures in unconsolidated sediments, but few studies show such signatures for ancient biosilicieous rocks. In Precambrian cherts from greenstone belts, small scaled isotopic variations were interpreted as a primary diagenetic feature. They were used, coupled to mean δ18O, to reconstruct seawater temperature at which cherts precipitated. Here, we examine stable isotopes in Mesozoic biogenic cherts that may also preserve an environmental signature. We measured δ30Si and δ18O in situ by SIMS, in the chalcedony of individual radiolarian tests preserved in Mesozoic radiolarites. Microanalysis of chalcedony, rather than the bulk rock isotopic composition, is likely to reveal a palaeoenvironmental signal, since it is derived from biogenic opal, the most mobile silica phase during earliest diagenesis. Our data reveal clear trends through several Mesozoic radiolarite sections from Panthalassa (Kiso River, Japan) and Western Tethys (Sogno, Italy). δ18O records measured in radiolarites show a relatively good correlation to δ18O-variations of Mesozoic low magnesium calcite shells, which are commonly used as a palaeotemperature proxy. Once these variations, attributed to seawater temperature, are removed, the residual δ18O trends are opposite to the δ30Si trends. δ30Si increases from Middle Triassic to Early Jurassic in the Kiso River sections and decrease during the Middle Jurassic in the Sogno section. The observed d30Si-trends are likely to represent a palaeoenvironmental signal, because they are not compatible with simple models of progressive diagenesis along P/T-paths (or depth below sea bottom in drill holes). Among the palaeoenvironmental factors that may have influenced these trends are the oceanic silica cycle changing though time, oceanic circulation and/or the palaeogeographic location of each studied site. Siliceous organisms are

  1. Data Compression for the Tomo-e Gozen Using Low-rank Matrix Approximation

    NASA Astrophysics Data System (ADS)

    Morii, Mikio; Ikeda, Shiro; Sako, Shigeyuki; Ohsawa, Ryou

    2017-01-01

    Optical wide-field surveys with a high cadence are expected to create a new field of astronomy, so-called “movie astronomy,” in the near future. The amount of data from the observations will be huge, and hence efficient data compression will be indispensable. Here we propose a low-rank matrix approximation with sparse matrix decomposition as a promising solution to reduce the data size effectively while preserving sufficient scientific information. We apply one of the methods to the movie data obtained with the prototype model of the Tomo-e Gozen mounted on the 1.0 m Schmidt telescope of Kiso Observatory. Once full-scale observation with the Tomo-e Gozen commences, it will generate ∼30 TB of data per night. We demonstrate that the data are compressed by a factor of about 10 in size without losing transient events like optical short transient point sources and meteors. The intensity of point sources can be recovered from the compressed data. The processing runs sufficiently fast, compared with the expected data-acquisition rate in the actual observing runs.

  2. Optical variability properties of mini-BAL and NAL quasars

    NASA Astrophysics Data System (ADS)

    Horiuchi, Takashi; Misawa, Toru; Morokuma, Tomoki; Koyamada, Suzuka; Takahashi, Kazuma; Wada, Hisashi

    2016-08-01

    While narrow absorption lines (NALs) are relatively stable, broad absorption lines (BALs) and mini-BAL systems usually show violent time variability within a few years via a mechanism that is not yet understood. In this study, we examine the variable ionization state (VIS) scenario as a plausible mechanism, as previously suspected. Over three years, we performed photometric monitoring observations of four mini-BAL and five NAL quasars at zem ˜ 2.0-3.1 using the 105 cm Kiso Schmidt Telescope in u, g, and i bands. We also performed spectroscopic monitoring observation of one of our mini-BAL quasars (HS 1603+3820) using the 188 cm Okayama Telescope over the same period as the photometric observations. Our main results are as follows: (1) Structure function (SF) analysis revealed that the quasar UV flux variability over three years was not large enough to support the VIS scenario, unless the ionization condition of outflow gas is very low. (2) There was no crucial difference between the SFs of mini-BAL and NAL quasars. (3) The variability of the mini-BAL and quasar light curves was weakly synchronized with a small time delay for HS 1603+3820. These results suggest that the VIS scenario may need additional mechanisms such as variable shielding by X-ray warm absorbers.

  3. Discovery of Dramatic Optical Variability in SDSS J1100+4421: A Peculiar Radio-loud Narrow-line Seyfert 1 Galaxy?

    NASA Astrophysics Data System (ADS)

    Tanaka, Masaomi; Morokuma, Tomoki; Itoh, Ryosuke; Akitaya, Hiroshi; Tominaga, Nozomu; Saito, Yoshihiko; Stawarz, Łukasz; Tanaka, Yasuyuki T.; Gandhi, Poshak; Ali, Gamal; Aoki, Tsutomu; Contreras, Carlos; Doi, Mamoru; Essam, Ahmad; Hamed, Gamal; Hsiao, Eric Y.; Iwata, Ikuru; Kawabata, Koji S.; Kawai, Nobuyuki; Kikuchi, Yuki; Kobayashi, Naoto; Kuroda, Daisuke; Maehara, Hiroyuki; Matsumoto, Emiko; Mazzali, Paolo A.; Minezaki, Takeo; Mito, Hiroyuki; Miyata, Takashi; Miyazaki, Satoshi; Mori, Kensho; Moritani, Yuki; Morokuma-Matsui, Kana; Morrell, Nidia; Nagao, Tohru; Nakada, Yoshikazu; Nakata, Fumiaki; Noma, Chinami; Ohsuga, Ken; Okada, Norio; Phillips, Mark M.; Pian, Elena; Richmond, Michael W.; Sahu, Devendra; Sako, Shigeyuki; Sarugaku, Yuki; Shibata, Takumi; Soyano, Takao; Stritzinger, Maximilian D.; Tachibana, Yutaro; Taddia, Francesco; Takaki, Katsutoshi; Takey, Ali; Tarusawa, Ken'ichi; Ui, Takahiro; Ukita, Nobuharu; Urata, Yuji; Walker, Emma S.; Yoshii, Taketoshi

    2014-10-01

    We present our discovery of dramatic variability in SDSS J1100+4421 by the high-cadence transient survey Kiso Supernova Survey. The source brightened in the optical by at least a factor of three within about half a day. Spectroscopic observations suggest that this object is likely a narrow-line Seyfert 1 galaxy (NLS1) at z = 0.840, however, with unusually strong narrow emission lines. The estimated black hole mass of ~107 M ⊙ implies bolometric nuclear luminosity close to the Eddington limit. SDSS J1100+4421 is also extremely radio-loud, with a radio loudness parameter of R ~= 4 × 102-3 × 103, which implies the presence of relativistic jets. Rapid and large-amplitude optical variability of the target, reminiscent of that found in a few radio- and γ-ray-loud NLS1s, is therefore produced most likely in a blazar-like core. The 1.4 GHz radio image of the source shows an extended structure with a linear size of about 100 kpc. If SDSS J1100+4421 is a genuine NLS1, as suggested here, this radio structure would then be the largest ever discovered in this type of active galaxies.

  4. Development of a real-time data processing system for a prototype of the Tomo-e Gozen wide field CMOS camera

    NASA Astrophysics Data System (ADS)

    Ohsawa, Ryou; Sako, Shigeyuki; Takahashi, Hidenori; Kikuchi, Yuki; Doi, Mamoru; Kobayashi, Naoto; Aoki, Tsutomu; Arimatsu, Ko; Ichiki, Makoto; Ikeda, Shiro; Ita, Yoshifusa; Kasuga, Toshihiro; Kawakita, Hideo; Kokubo, Mitsuru; Maehara, Hiroyuki; Matsunaga, Noriyuki; Mito, Hiroyuki; Mitsuda, Kazuma; Miyata, Takashi; Mori, Kiyoshi; Mori, Yuki; Morii, Mikio; Morokuma, Tomoki; Motohara, Kentaro; Nakada, Yoshikazu; Okumura, Shin-ichiro; Onozato, Hiroki; Osawa, Kentaro; Sarugaku, Yuki; Sato, Mikiya; Shigeyama, Toshikazu; Soyano, Takao; Tanaka, Masaomi; Taniguchi, Yuki; Tanikawa, Ataru; Tarusawa, Ken'ichi; Tominaga, Nozomu; Totani, Tomonori; Urakawa, Seitaro; Usui, Fumihiko; Watanabe, Junichi; Yamaguchi, Jumpei; Yoshikawa, Makoto

    2016-08-01

    The Tomo-e Gozen camera is a next-generation, extremely wide field optical camera, equipped with 84 CMOS sensors. The camera records about a 20 square degree area at 2 Hz, providing "astronomical movie data". We have developed a prototype of the Tomo-e Gozen camera (hereafter, Tomo-e PM), to evaluate the basic design of the Tomo-e Gozen camera. Tomo-e PM, equipped with 8 CMOS sensors, can capture a 2 square degree area at up to 2 Hz. Each CMOS sensor has about 2.6 M pixels. The data rate of Tomo-e PM is about 80 MB/s, corresponding to about 280 GB/hour. We have developed an operating system and reduction softwares to handle such a large amount of data. Tomo-e PM was mounted on 1.0-m Schmidt Telescope in Kiso Observatory at the University of Tokyo. Experimental observations were carried out in the winter of 2015 and the spring of 2016. The observations and software implementation were successfully completed. The data reduction is now in execution.

  5. Development of a prototype of the Tomo-e Gozen wide-field CMOS camera

    NASA Astrophysics Data System (ADS)

    Sako, Shigeyuki; Osawa, Ryou; Takahashi, Hidenori; Kikuchi, Yuki; Doi, Mamoru; Kobayashi, Naoto; Aoki, Tsutomu; Arimatsu, Ko; Ichiki, Makoto; Ikeda, Shiro; Ita, Yoshifusa; Kasuga, Toshihiro; Kawakita, Hideyo; Kokubo, Mitsuru; Maehara, Hiroyuki; Matsunaga, Noriyuki; Mito, Hiroyuki; Mitsuda, Kazuma; Miyata, Takashi; Mori, Kiyoshi; Mori, Yuki; Morii, Mikio; Morokuma, Tomoki; Motohara, Kentaro; Nakada, Yoshikazu; Osawa, Kentaro; Okumura, Shin-ichiro; Onozato, Hiroki; Sarugaku, Yuki; Sato, Mikiya; Shigeyama, Toshikazu; Soyano, Takao; Tanaka, Masaomi; Taniguchi, Yuki; Tanikawa, Ataru; Tarusawa, Ken'ichi; Tominaga, Nozomu; Totani, Tomonori; Urakawa, Seitaro; Usui, Fumihiko; Watanabe, Junichi; Yamaguchi, Jumpei; Yoshikawa, Makoto

    2016-08-01

    The Tomo-e Gozen is an extremely wide-field optical camera for the Kiso 1.0-m Schmidt telescope. It is capable of taking consecutive frames with a field-of-view of 20 deg2 and a sub-second time-resolution, which are achieved by 84 chips of 2k×1k CMOS sensor. This camera adopts unconventional designs including a lightweight structure, a nonvacuumed and naturally-air cooled system, front-side-illuminated CMOS sensors with microlens arrays, a sensor alignment along a spherical focal plane of the telescope, and massive readout electronics. To develop technical components necessary for the Tomo-e Gozen and confirm a feasibility of its basic design, we have developed a prototype-model (PM) of the Tomo-e Gozen prior to the final-model (FM). The Tomo-e PM is equipped with eight chips of the CMOS sensor arranged in a line along the RA direction, covering a sky area of 2.0 deg2. The maximum frame rate is 2 fps. The total data production rate is 80 MByte sec-1 at 2 fps, corresponding to approximately 3 TByte night-1. After laboratory testing, we have successfully obtained consecutive movie data at 2 fps with the Tomo-e PM in the first commissioning run conducted in the end of 2015.

  6. DISCOVERY OF DRAMATIC OPTICAL VARIABILITY IN SDSS J1100+4421: A PECULIAR RADIO-LOUD NARROW-LINE SEYFERT 1 GALAXY?

    SciTech Connect

    Tanaka, Masaomi; Morokuma, Tomoki; Doi, Mamoru; Kikuchi, Yuki; Itoh, Ryosuke; Akitaya, Hiroshi; Tanaka, Yasuyuki T.; Kawabata, Koji S.; Tominaga, Nozomu; Saito, Yoshihiko; Kawai, Nobuyuki; Stawarz, Łukasz; Gandhi, Poshak; Ali, Gamal; Essam, Ahmad; Hamed, Gamal; Aoki, Tsutomu; Contreras, Carlos; Hsiao, Eric Y.; Iwata, Ikuru; and others

    2014-10-01

    We present our discovery of dramatic variability in SDSS J1100+4421 by the high-cadence transient survey Kiso Supernova Survey. The source brightened in the optical by at least a factor of three within about half a day. Spectroscopic observations suggest that this object is likely a narrow-line Seyfert 1 galaxy (NLS1) at z = 0.840, however, with unusually strong narrow emission lines. The estimated black hole mass of ∼10{sup 7} M {sub ☉} implies bolometric nuclear luminosity close to the Eddington limit. SDSS J1100+4421 is also extremely radio-loud, with a radio loudness parameter of R ≅ 4 × 10{sup 2}-3 × 10{sup 3}, which implies the presence of relativistic jets. Rapid and large-amplitude optical variability of the target, reminiscent of that found in a few radio- and γ-ray-loud NLS1s, is therefore produced most likely in a blazar-like core. The 1.4 GHz radio image of the source shows an extended structure with a linear size of about 100 kpc. If SDSS J1100+4421 is a genuine NLS1, as suggested here, this radio structure would then be the largest ever discovered in this type of active galaxies.

  7. Probabilistic modelling of rainfall induced landslide hazard assessment

    NASA Astrophysics Data System (ADS)

    Kawagoe, S.; Kazama, S.; Sarukkalige, P. R.

    2010-06-01

    To evaluate the frequency and distribution of landslides hazards over Japan, this study uses a probabilistic model based on multiple logistic regression analysis. Study particular concerns several important physical parameters such as hydraulic parameters, geographical parameters and the geological parameters which are considered to be influential in the occurrence of landslides. Sensitivity analysis confirmed that hydrological parameter (hydraulic gradient) is the most influential factor in the occurrence of landslides. Therefore, the hydraulic gradient is used as the main hydraulic parameter; dynamic factor which includes the effect of heavy rainfall and their return period. Using the constructed spatial data-sets, a multiple logistic regression model is applied and landslide hazard probability maps are produced showing the spatial-temporal distribution of landslide hazard probability over Japan. To represent the landslide hazard in different temporal scales, extreme precipitation in 5 years, 30 years, and 100 years return periods are used for the evaluation. The results show that the highest landslide hazard probability exists in the mountain ranges on the western side of Japan (Japan Sea side), including the Hida and Kiso, Iide and the Asahi mountainous range, the south side of Chugoku mountainous range, the south side of Kyusu mountainous and the Dewa mountainous range and the Hokuriku region. The developed landslide hazard probability maps in this study will assist authorities, policy makers and decision makers, who are responsible for infrastructural planning and development, as they can identify landslide-susceptible areas and thus decrease landslide damage through proper preparation.

  8. Probabilistic modelling of rainfall induced landslide hazard assessment

    NASA Astrophysics Data System (ADS)

    Kawagoe, S.; Kazama, S.; Sarukkalige, P. R.

    2010-01-01

    To evaluate the frequency and distribution of landslides hazards over Japan, this study uses a probabilistic model based on multiple logistic regression analysis. Study particular concerns several important physical parameters such as hydraulic parameters, geographical parameters and the geological parameters which are considered to be influential in the occurrence of landslides. Sensitivity analysis confirmed that hydrological parameter (hydraulic gradient) is the most influential factor in the occurrence of landslides. Therefore, the hydraulic gradient is used as the main hydraulic parameter; dynamic factor which includes the effect of heavy rainfall and their return period. Using the constructed spatial data-sets, a multiple logistic regression model is applied and landslide susceptibility maps are produced showing the spatial-temporal distribution of landslide hazard susceptibility over Japan. To represent the susceptibility in different temporal scales, extreme precipitation in 5 years, 30 years, and 100 years return periods are used for the evaluation. The results show that the highest landslide hazard susceptibility exists in the mountain ranges on the western side of Japan (Japan Sea side), including the Hida and Kiso, Iide and the Asahi mountainous range, the south side of Chugoku mountainous range, the south side of Kyusu mountainous and the Dewa mountainous range and the Hokuriku region. The developed landslide hazard susceptibility maps in this study will assist authorities, policy makers and decision makers, who are responsible for infrastructural planning and development, as they can identify landslide-susceptible areas and thus decrease landslide damage through proper preparation.

  9. Characterization of the Surface Properties of MUSES-C/Hayabusa Spacecraft Target Asteroid 25143 Itokawa (1998 SF36)

    NASA Technical Reports Server (NTRS)

    Lederer, S. M.; Domingue, D. L.; Vilas, F.; Abe, M.; Farnham, T. L.; Jarvis, K. S.; Lowry, S. C.; Ohba, Y.; Weissman, P. R.; French, L. M.

    2004-01-01

    Several spacecraft missions have recently targeted asteroids to study their morphologies and physical properties (e.g. Galileo, NEAR Shoemaker), and more are planned. MUSES-C is a Japanese mission designed to rendezvous with a near-Earth asteroid (NEA). The MUSES-C spacecraft, Hayabusa, was launched successfully in May 2003. It will rendezvous with its target asteroid in 2005, and return samples to the Earth in 2007. Its target, 25143 Itokawa (1998 SF36), made a close approach to the Earth in 2001. We collected an extensive ground-based database of broadband photometry obtained during this time, which maximized the phase angle coverage, to characterize this target in preparation for the mission. Our project was designed to capitalize on the broadband UBVRI photometric observations taken with a series of telescopes, instrumentation, and observers. Photometry and spectrophotometry of Itokawa were acquired at Lowell, McDonald, Steward, Palomar, Table Mountain and Kiso Observatories. The photometric data sets were combined to calculate Hapke model parameters of the surface material of Itokawa, and examine the solar-corrected broadband color characteristics of the asteroid. Broadband photometry of an object can be used to: (1) determine its colors and thereby contribute to the understanding of its surface composition and taxonomic class, and (2) infer global physical surface properties of the target body. We present both colors from UBVRI observations of the MUSES-C target Itokawa, and physical properties derived by applying a Hapke model to the broadband BVRI photometry.

  10. VizieR Online Data Catalog: Optical monitoring of the Seyfert I NGC 3516 (Noda+, 2016)

    NASA Astrophysics Data System (ADS)

    Noda, H.; Minezaki, T.; Watanabe, M.; Kokubo, M.; Kawaguchi, K.; Itoh, R.; Morihana, K.; Saito, Y.; Nakao, H.; Imai, M.; Moritani, Y.; Takaki, K.; Kawabata, M.; Nakaoka, T.; Uemura, M.; Kawabata, K.; Yoshida, M.; Arai, A.; Takagi, Y.; Morokuma, T.; Doi, M.; Itoh, Y.; Yamada, S.; Nakazawa, K.; Fukazawa, Y.; Makishima, K.

    2016-11-01

    The X-ray monitoring observations of NGC 3516 were performed in the Suzaku AO-8 cycle during 2013-2014. Specifically, NGC 3516 was observed with Suzaku five times from 2013 April 10 to May 29, with intervals of ~1-2 weeks. Another pointing was carried out on November 7, and the last one on 2014 April 4, making a total of seven observations, with various intervals from days to months. The optical photometric monitoring observations of NGC 3516 were performed by using the charge-coupled device (CCD) cameras installed at the Pirka, MITSuME, Kiso Schmidt, Nayuta, and Kanata telescopes. Simultaneous monitoring observations were performed at the same seven epochs as the X-ray observations by Suzaku. In addition, from 2013 January to 2014 April, these telescopes densely monitored the source even without simultaneous X-ray coverage, with a typical intervals of ~1 day. In the present paper, we present the B-band and g'-band photometric data, because the optical continuum emission of AGNs is generally bluer than that of the host galaxy, thus ensuring better sensitivity to the AGN signals. (1 data file).

  11. Asymmetric Dust Jets and Extended Structure of 22P/Kopff Observed During 2009 Appearance

    NASA Astrophysics Data System (ADS)

    Hanayama, Hidekazu; Ishiguro, Masateru; Watanabe, Jun-Ichi; Sarugaku, Yuki; Fukushima, Hideo; Miyaji, Takeshi; Yanagisawa, Kenshi; Kuroda, Daisuke; Yoshida, Michitoshi; Ohta, Kouji; Nobuyuki, Kawai

    2012-12-01

    22P/Kopff images were taken with Multicolor Imaging Telescopes for Survey and Monstrous Explosions (MITSuME) 3ch simultaneous CCD cameras on the Ishigakijima astronomical observatory 105-cm telescope and a 2kCCD camera on the Kiso 105-cm Schmidt telescope from 2009 August to December after the passage of its perihelion on 2009 May 25. We confirmed that the near-nuclear fan-shaped jet structure extended toward the south. Whereas we detected a dust trail structure on the project orbit of the parent nucleus, we could not confirm the obvious neck-line structure. We deduced a pole orientation of (αp1, δp1) = (302°±30°, 62°±10°) or (αp1, δp1) = (122°±30°, -62°±10°) in the case of prograde or retrograde rotation, based on the fan-shaped jet. In addition, we conducted a model simulation of the dust orbital evolution, and found that the observed dust morphology of the fan-shaped jet and dust trail can well explain the dust emission near the south polar region. Finally, we conclude that the surface of 22P/Kopff is becoming largely dormant, but the polar region is still active, as we saw in the Deep Space 1 image of 19P/Borrelly.

  12. GIS-based numerical simulations of the July 2014 Nagiso debris flow in Nagano Prefecture, Japan

    NASA Astrophysics Data System (ADS)

    Wang, Chunxiang; Fukuoka, Hiroshi

    2015-04-01

    A debris flow disaster took place in Nagiso, Nagano Prefecture of Japan in the later afternoon of 9 July 2014 triggered by 76 mm torrential rain associated with the typhoon Neoguri. This debris flow killed one resident and completely destroyed several houses. Although the source of the debris flows, especially the origin of their large boulders exceeding 5 m, are not clear, it seems that those debris flows initiated in the two upstream torrents and they joined Nashisawa torrent. Finally the debris flow ran and deposited in the Kiso River. The downstream residents are much aware of the many historical cases on similar debris flow disasters in the torrents in Nagiso and surrounding communities. Most of the residents could evacuate immediately after they felt the ground tremors induced by the running debris flow. Authors used LAHARZ (Schilling 1998) to simulate the Nagiso debris flow using 5-meter resolution Digital Elevation Model and several debris-flow volumes for the calibration. We also performed a numerical simulation to predicting the runout distance and to get insight into the behavior of the debris flow movement. A GIS-based depth-averaged 2D numerical model using a coupled viscous and Coulomb type law is used to simulate a debris flow from initiation to deposition. We compared the two simulation results and suggested the more appropriate coefficients of equations in LAHARZ for calculating the cross sectional area and planimetric area for application to the July 2014 Nagiso debris flows.

  13. Polyamorphism in Water: Amorphous Ices and their Glassy States

    NASA Astrophysics Data System (ADS)

    Amann-Winkel, K.; Boehmer, R.; Fujara, F.; Gainaru, C.; Geil, B.; Loerting, T.

    2015-12-01

    . Phys. 125, 2006 [3] P.G. Debenedetti, J. Phys.: Condens. Matter 15, R1669, 2003 [4] H. Schober, M.M. Koza et al., PRL 85, 4100, 2000 [5] G.P. Johari, A. Hallbrucker and E. Mayer Nature 330, 552, 1987 [6] K. Amann-Winkel, C. Gainaru, et al., PNAS 110, 17720, 2013 [7] Andersson, O., PNAS 108, 11013, 2011

  14. Local electromagnetic properties of magnetic pnictides: a comparative study probed by NMR measurements.

    PubMed

    Majumder, M; Ghoshray, K; Ghoshray, A; Pal, A; Awana, V P S

    2013-05-15

    (75)As and (31)P NMR studies are performed in PrCoAsO and NdCoPO respectively. The Knight shift data in PrCoAsO indicate the presence of an antiferromagnetic interaction between the 4f moments along the c axis in the ferromagnetic state of Co 3d moments. We propose a possible spin structure in this system. The (75)As quadrupolar coupling constant, νQ, increases continuously with decrease of temperature and is found to vary linearly with the intrinsic spin susceptibility, K(iso). This indicates the possibility of the presence of a coupling between charge density and spin density fluctuations. Further, the (31)P NMR Knight shift and spin-lattice relaxation rate (1/T1) in the paramagnetic state of NdCoPO indicate that the differences of LaCoPO and NdCoPO from SmCoPO are due to the decrement of the interlayer separation and not due to the moments of the 4f electrons. The nuclear spin-lattice relaxation time (T1) in NdCoPO shows weak anisotropy at 300 K. Using the self-consistent renormalization (SCR) theory of itinerant ferromagnets, it is shown that in the ab plane, the spin fluctuations are three-dimensional ferromagnetic in nature. From SCR theory the important spin-fluctuation parameters (T0, TA, F¯1) are evaluated. The similarities and dissimilarities of the NMR results in As and P based systems with different rare earths are also discussed.

  15. Development of a new readout system for the near-infrared detector of HONIR

    NASA Astrophysics Data System (ADS)

    Ui, Takahiro; Sako, Shigeyuki; Yamashita, Takuya; Akitaya, Hiroshi; Kawabata, Koji S.; Nakaya, Hidehiko; Moritani, Yuki; Itoh, Ryosuke; Takaki, Katsutoshi; Urano, Takeshi; Ueno, Issei; Ohsugi, Takashi; Yoshida, Michitoshi; Nakao, Hikaru; Hashiba, Yasuhito

    2014-08-01

    We developed a new readout system for the near-infrared detector VIRGO-2K (2kx2k HgCdTe array) installed in the optical-infrared simultaneous camera, HONIR, for the 1.5 m Kanata telescope at Higashi-Hiroshima observatory. The main goal of this development is to read out one frame within ~ 1 second through 16 output readout mode of the detector, in order to reduce the overhead time per exposure. The system is based on a CCD controller, Kiso Array Controller (KAC). We redesigned the analog part of KAC to fit VIRGO-2K. We employed a fully differential input circuit and a third order Bessel low-pass filter for noise reduction and a constant current system to improve the linearity of the detector. We set the cutoff frequency of the Bessel low-pass filter at the readout clock rate (120 kHz). We also set the constant current at 200 μA according to the data sheet of VIRGO-2K. We tested the new readout system at room temperature and confirmed that the low-pass filter works well as designed. The fluctuation of the current level of the constant current system is less than 2% for the typical output voltage range of VIRGO-2K (3.2-4.4 V). We measured the readout noise caused by the new readout system (connected to cooled multiplexer) and found that it is 30-40 μV rms, being comparable to or slightly higher than the typical readout noise of VIRGO-2K, ˜ 37 μV rms.

  16. J-GEM follow-up observations of the gravitational wave source GW151226*

    NASA Astrophysics Data System (ADS)

    Yoshida, Michitoshi; Utsumi, Yousuke; Tominaga, Nozomu; Morokuma, Tomoki; Tanaka, Masaomi; Asakura, Yuichiro; Matsubayashi, Kazuya; Ohta, Kouji; Abe, Fumio; Chimasu, Sho; Furusawa, Hisanori; Itoh, Ryosuke; Itoh, Yoichi; Kanda, Yuka; Kawabata, Koji S.; Kawabata, Miho; Koshida, Shintaro; Koshimoto, Naoki; Kuroda, Daisuke; Moritani, Yuki; Motohara, Kentaro; Murata, Katsuhiro L.; Nagayama, Takahiro; Nakaoka, Tatsuya; Nakata, Fumiaki; Nishioka, Tsubasa; Saito, Yoshihiko; Terai, Tsuyoshi; Tristram, Paul J.; Yanagisawa, Kenshi; Yasuda, Naoki; Doi, Mamoru; Fujisawa, Kenta; Kawachi, Akiko; Kawai, Nobuyuki; Tamura, Yoichi; Uemura, Makoto; Yatsu, Yoichi

    2017-02-01

    We report the results of optical-infrared follow-up observations of the gravitational wave (GW) event GW151226 detected by the Advanced LIGO in the framework of J-GEM (Japanese collaboration for Gravitational wave ElectroMagnetic follow-up). We performed wide-field optical imaging surveys with the Kiso Wide Field Camera (KWFC), Hyper Suprime-Cam (HSC), and MOA-cam3. The KWFC survey started at 2.26 d after the GW event and covered 778 deg2 centered at the high Galactic region of the skymap of GW151226. We started the HSC follow-up observations from ˜12 d after the event and covered an area of 63.5 deg2 of the highest probability region of the northern sky with limiting magnitudes of 24.6 and 23.8 for the i and z bands, respectively. MOA-cam3 covered 145 deg2 of the skymap with the MOA-red filter ˜2.5 mon after the GW alert. The total area covered by the wide-field surveys was 986.5 deg2. The integrated detection probability for the observed area was ˜29%. We also performed galaxy-targeted observations with six optical and near-infrared telescopes from 1.61 d after the event. A total of 238 nearby (≤100 Mpc) galaxies were observed with a typical I band limiting magnitude of ˜19.5. We detected 13 supernova candidates with the KWFC survey, and 60 extragalactic transients with the HSC survey. Two thirds of the HSC transients were likely supernovae and the remaining one third were possible active galactic nuclei. With our observational campaign, we found no transients that are likely to be associated with GW151226.

  17. Spatial distribution of allochthonous fine-grained sediments from drilling activities in the deepwater Ulleung Basin, Korea

    NASA Astrophysics Data System (ADS)

    Chun, Jong-Hwa; Um, In-Kwon; Bahk, Jang-Jun; Kim, Yuri; Ryu, Byong-Jae

    2015-04-01

    The marine sediments in deepwater basins can be used as sedimentologic, stratigraphic, paleoceanographic, and paleoclimatologic tools to interpret the various scientific topics in the world. As a result, many drilling and coring activities were performed by international ocean drilling programs in deepwater basins during the last 50 years. In the deepwater Ulleung Basin, the Second Ulleung Basin Gas Hydrate Drilling Expedition (UBGH2) was conducted to perform the gas hydrate R&D in 2010. During the UBGH2, drilling and coring activities were successfully accomplished in 13 sites ranging from 898 m to 2,156 m water depth. The three major sediment facies in the Ulleung Basin are composed of light-colored bioturbated hemipelagic muds under a highly oxygenated bottom-water conditions, dark-colored crudely laminated muds under a poorly oxygenated bottom-water conditions, and laminated/massive sand with turbidites. The present seafloor sediments commonly consist of 1-2 thick light-colored bioturbated hemipelagic muds in the deepwater Ulleung Basin. We observed the UBGH2 drilling holes using by Ultra-short Baseline (USBL)-guided KIGAM Seafloor Observation System (KISOS) in 2013. The UBGH2 drilling holes were found on the seafloor with partially collapse of the margin. We also found the multi-colored sediment patches on the seafloor due to allochthonous sediment input. We analyzed the elements using a non-destructive Itrax X-ray fluorescence (XRF) core scanner for split core. The sediment patches have relatively low concentrations of Fe, Ba, Mn and Pb compared to the element concentrations of the present seafloor sediments. The concentrations of K, Ca, and Ti are higher than the present seafloor sediments. The patch sediments are observed no more than 50 m away from the UBGH2 drilling holes. The allochthonous sediments occur at depth of about 6 cm below seafloor in the observed drilling holes. The origin of allochthonous sediments on the seafloor is interpreted as drilling

  18. Faint-meteor survey with a large-format CMOS sensor

    NASA Astrophysics Data System (ADS)

    Watanabe, J.; Enomoto, T.; Terai, T.; Kasuga, T.; Miyazaki, S.; Oota, K.; Muraoka, F.; Onishi, T.; Yamasaki, T.; Mito, H.; Aoki, T.; Soyano, T.; Tarusawa, K.; Matsunaga, N.; Sako, S.; Kobayashi, N.; Doi, M.

    2014-07-01

    For observing faint meteors, we need a large telescope or similar optics, which always give a restriction of the field of view. It is a kind of trade-off between the high sensitivity by using larger telescope and narrower field of view. Reconciling this contradiction, we need a large-format imaging detector together with fast readout for meteor observations. A high-sensitivity CMOS sensor of the large format was developed by Canon Inc. in 2010[1]. Its size is 202 mm×205 mm which makes it the largest one-chip CMOS sensor in the world, and approximately 40 times the size of Canon's largest commercial CMOS sensor as shown in the figure. The number of pixel is 1280×1248. Because the increased size of the new CMOS sensor allows more light to be gathered, it enables shooting in low-light environments. The sensor makes image capture possible in one-hundredth the amount of light required by a 35 mm full-frame CMOS sensor, facilitating the shooting of 60 frame-per-second video with a mere 0.3 lux of illumination. We tried to use this large-format CMOS sensor attached to the prime focus of the 1.05-m (F3.1) Schmidt telescope at the Kiso Observatory, University of Tokyo, for surveying faint meteors. The field of view is 3.3 by 3.3 degrees. Test observations including operation check of the system were carried out in January 2011, September 2011,and December 2012. Images were obtained at a time resolution of 60 frames per second. In this system, the limiting magnitude is estimated to be about 11-12. Because of the limitation of the data storage, full-power observations (14-bit data per 1/60 second) were performed for about one or two hours each night. During the first period, we can count a sporadic meteor every 5 seconds. This is about one order higher detection rate of the faint meteors compared with the previous work[2]. Assuming the height of faint meteors at 100 km, the derived flux of the sporadic meteors is about 5 × 10^{-4} km^{-2} sec^{-1}. The last run was

  19. Gas hydrate environmental monitoring program in the Ulleung Basin, East Sea of Korea

    NASA Astrophysics Data System (ADS)

    Ryu, Byong-Jae; Chun, Jong-Hwa; McLean, Scott

    2013-04-01

    As a part of the Korean National Gas Hydrate Program, the Korea Institute of Geoscience and Mineral Resources (KIGAM) has been planned and conducted the environmental monitoring program for the gas hydrate production test in the Ulleung Basin, East Sea of Korea in 2014. This program includes a baseline survey using a KIGAM Seafloor Observation System (KISOS) and R/V TAMHAE II of KIGAM, development of a KIGAM Seafloor Monitoring System (KIMOS), and seafloor monitoring on various potential hazards associated with the dissociated gas from gas hydrates during the production test. The KIGAM also plans to conduct the geophysical survey for determining the change of gas hydrate reservoirs and production-efficiency around the production well before and after the production test. During production test, release of gas dissociated from the gas hydrate to the water column, seafloor deformation, changes in chemical characteristics of bottom water, changes in seafloor turbidity, etc. will be monitored by using the various monitoring instruments. The KIMOS consists of a near-field observation array and a far-field array. The near-field array is constructed with four remote sensor platforms each, and cabled to the primary node. The far-field sensor array will consists of four autonomous instrument pods. A scientific Remotely Operated Vehicle (ROV) will be used to deploy the sensor arrays, and to connect the cables to each field instrument package and a primary node. A ROV will also be tasked to collect the water and/or gas samples, and to identify any gas (bubble) plumes from the seafloor using a high-frequency sector scanning sonar. Power to the near-field instrument packages will be supplied by battery units located on the seafloor near the primary node. Data obtained from the instruments on the near-field array will be logged and downloaded in-situ at the primary node, and transmitted real-time to the support vessel using a ROV. These data will also be transmitted real-time to

  20. DETECTION OF REMNANT DUST CLOUD ASSOCIATED WITH THE 2007 OUTBURST OF 17P/HOLMES

    SciTech Connect

    Ishiguro, Masateru; Kim, Yoonyoung; Kwon, Yuna G.; Sarugaku, Yuki; Kuroda, Daisuke; Maehara, Hiroyuki; Hanayama, Hidekazu; Takahashi, Jun; Terai, Tsuyoshi; Usui, Fumihiko; Vaubaillon, Jeremie J.; Morokuma, Tomoki; Kobayashi, Naoto; Watanabe, Jun-ichi

    2016-01-20

    This article reports a new optical observation of 17P/Holmes one orbital period after the historical outburst event in 2007. We detected not only a common dust tail near the nucleus but also a long narrow structure that extended along the position angle 274.°6 ± 0.°1 beyond the field of view (FOV) of the Kiso Wide Field Camera, i.e., >0.°2 eastward and >2.°0 westward from the nuclear position. The width of the structure decreased westward with increasing distance from the nucleus. We obtained the total cross section of the long extended structure in the FOV, C{sub FOV} = (2.3 ± 0.5) × 10{sup 10} m{sup 2}. From the position angle, morphology, and mass, we concluded that the long narrow structure consists of materials ejected during the 2007 outburst. On the basis of the dynamical behavior of dust grains in the solar radiation field, we estimated that the long narrow structure would be composed of 1 mm–1 cm grains having an ejection velocity of >50 m s{sup −1}. The velocity was more than one order of magnitude faster than that of millimeter–centimeter grains from typical comets around a heliocentric distance r{sub h} of 2.5 AU. We considered that sudden sublimation of a large amount of water-ice (≈10{sup 30} mol s{sup −1}) would be responsible for the high ejection velocity. We finally estimated a total mass of M{sub TOT} = (4–8) × 10{sup 11} kg and a total kinetic energy of E{sub TOT} = (1–6) × 10{sup 15} J for the 2007 outburst ejecta, which are consistent with those of previous studies that were conducted soon after the outburst.

  1. Compensation effects and relation between the activation energy of spin transition and the hysteresis loop width for an iron(ii) complex.

    PubMed

    Bushuev, Mark B; Pishchur, Denis P; Nikolaenkova, Elena B; Krivopalov, Viktor P

    2016-06-22

    The enthalpy-entropy compensation was observed for the cooperative → spin transition (the phase is a mononuclear complex [FeL2](BF4)2, L is 4-(3,5-dimethyl-1H-pyrazol-1-yl)-2-(pyridin-2-yl)-6-methylpyrimidine). The physical origin of this effect is the fact that the → spin transition is the first order phase transition accompanied by noticeable variations in the Tonset↑, ΔH and ΔS values. Higher ΔH and ΔS values are correlated with higher Tonset↑ values. The higher the enthalpy and entropy of the spin transition, the wider the hysteresis loop. The kinetic compensation effect, i.e. a linear relationship between ln A and Ea, was observed for the → spin transition. Moreover, an isokinetic relationship was detected in this system: the Arrhenius lines (ln k vs. 1/T) obtained from magnetochemical data for different samples of the phase undergoing the → transition show a common point of intersection (Tiso = 490 ± 2 K, ln kiso = -6.0 ± 0.2). The validity of this conclusion was confirmed by the Exner-Linert statistical method. This means that the isokinetic relationship and the kinetic compensation effect (ln A vs. Ea) in this system are true ones. The existence of a true kinetic compensation effect is supported independently by the fact that the hysteresis loop width for the cooperative spin transition ↔ increases with increasing activation barrier height. Estimating the energy of excitations for the phase with Tiso ∼ 490 K yields wavenumbers of ca. 340 cm(-1) corresponding to the frequencies of the stretching vibrations of the Fe(LS)-N bonds, i.e. the bonds directly involved in the mechanism of the spin transition. This is the first observation of the kinetic compensation effect (ln A vs. Ea) and the isokinetic relationship for a cooperative spin crossover system showing thermal hysteresis. Our results provide the first experimental evidence that the higher the activation barrier for the spin transition, the wider the hysteresis loop for a

  2. Crystal structure of δ-isobutoxypentabromo-cyclododecanes, kinetics and selectivity of their isomerization during thermal treatment of flame-proofed polystyrenes.

    PubMed

    Heeb, Norbert V; Graf, Heidi; Schweizer, W Bernd; Heeb, Meret; Lienemann, P

    2011-06-01

    Hexabromocyclododecanes (HBCDs) are persistent organic pollutants now ubiquitous in the environment. Technical HBCD mixtures and with it flame-proofed polystyrenes (FP-PS) also contain isobutoxypentabromocyclododecanes (iBPBCDs) as minor constituents, which are possibly released together with HBCDs. So far, eight diastereomeric pairs of enantiomers named as α-, β-, γ-, δ-, ϵ-, ξ-, η-, and θ-iBPBCDs with proportions of 10%, 5%, 2%, 21%, 11%, 11%, 12% and 28% were found in technical HBCD. Herein the crystal structure of racemic δ-iBPBCD, the second most prominent diastereomer, is presented and assigned to (1S)-1-isobutoxy-(2R,5R,6S,9S,10S)-2,5,6,9,10-pentabromocyclododecane and its enantiomer. During thermal treatment of FP-PS, e.g. the production of extruded polystyrenes (XPS), proportions of δ-iBPBCDs decrease and those of other stereoisomers increase. Evidence was found that δ-iBPBCDs isomerize stereo- and regioselectively to β-iBPBCDs. Based on structural and kinetic data, a transformation mechanism was proposed. Apparent first-order rate constants (k(iso)) of 0.0019, 0.0050, and 0.012min(-1) are found for the δ- to β-iBPBCD isomerization at 120, 130, and 140°C, respectively, corresponding to half-lives of 360, 140, and 56min. These transformations also occur during the production of XPS, which predominantly contain β-iBPBCDs, whereas δ-iBPBCDs dominate in materials experiencing lower thermal stress, e.g. expanded polystyrenes (EPS). The relative configurations of δ- and θ-iBPBCDs are TtCtCt, like the one of γ-HBCDs. γ-HBCDs are the kinetically and α-HBCDs with a TcCtCc configuration the thermodynamically favored products. In analogy, β-iBPBCDs are assumed to have a TcCtCc configuration like α-HBCDs because they are formed from δ-iBPBCDs under thermodynamic control. In conclusion, HBCD- and iBPBCD-patterns in flame-proofed polystyrenes vary substantially, reflecting the thermal stress these materials have experienced. When released to the

  3. THE AFTERGLOW AND ENVIRONMENT OF THE SHORT GRB 111117A

    SciTech Connect

    Margutti, R.; Berger, E.; Fong, W.; Zauderer, B. A.; Soderberg, A. M.; Milisavljevic, D.; Sanders, N.; Cenko, S. B.; Greiner, J.; Cucchiara, A.

    2012-09-01

    We present multi-wavelength observations of the afterglow of the short GRB 111117A, and follow-up observations of its host galaxy. From rapid optical and radio observations, we place limits of r {approx}> 25.5 mag at {delta}t Almost-Equal-To 0.55 days and F{sub {nu}}(5.8 GHz) {approx}< 18 {mu}Jy at {delta}t Almost-Equal-To 0.50 days, respectively. However, using a Chandra observation at {delta}t Almost-Equal-To 3.0 days we locate the absolute position of the X-ray afterglow to an accuracy of 0.''22 (1{sigma}), a factor of about six times better than the Swift/XRT position. This allows us to robustly identify the host galaxy and to locate the burst at a projected offset of 1.''25 {+-} 0.''20 from the host centroid. Using optical and near-IR observations of the host galaxy we determine a photometric redshift of z = 1.3{sup +0.3}{sub -0.2}, one of the highest for any short gamma-ray burst (GRB), leading to a projected physical offset for the burst of 10.5 {+-} 1.7 kpc, typical of previous short GRBs. At this redshift, the isotropic {gamma}-ray energy is E{sub {gamma},iso} Almost-Equal-To 3.0 Multiplication-Sign 10{sup 51} erg (rest-frame 23-2300 keV) with a peak energy of E{sub pk} Almost-Equal-To 850-2300 keV (rest-frame). In conjunction with the isotropic X-ray energy, GRB 111117A appears to follow our recently reported E{sub x,iso}-E{sub {gamma},iso}-E{sub pk} universal scaling. Using the X-ray data along with the optical and radio non-detections, we find that for a blastwave kinetic energy of E{sub K,iso} Almost-Equal-To E{sub {gamma},iso} erg, the circumburst density is n{sub 0} Almost-Equal-To 3 Multiplication-Sign 10{sup -4} - 1 cm{sup -3} (for a range of {epsilon}{sub B} = 0.001-0.1). Similarly, from the non-detection of a break in the X-ray light curve at {delta}t {approx}< 3 days, we infer a minimum opening angle for the outflow of {theta}{sub j} {approx}> 3-10 Degree-Sign (depending on the circumburst density). We conclude that Chandra observations of short