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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. Development of the Subaru-Mitaka-Okayama-Kiso Archive System

    NASA Astrophysics Data System (ADS)

    Baba, Hajime; Yasuda, Naoki; Ichikawa, Shin-Ichi; Yagi, Masafumi; Iwamoto, Nobuyuki; Takata, Tadafumi; Horaguchi, Toshihiro; Taga, Masatoshi; Watanabe, Masaru; Ozawa, Tomohiko; Hamabe, Masaru

    We have developed the Subaru-Mitaka-Okayama-Kiso-Archive (SMOKA) public science archive system which provides access to the data of the Subaru Telescope, the 188 cm telescope at Okayama Astrophysical Observatory, and the 105 cm Schmidt telescope at Kiso Observatory/University of Tokyo. SMOKA is the successor of the MOKA3 system. The user can browse the Quick-Look Images, Header Information (HDI) and the ASCII Table Extension (ATE) of each frame from the search result table. A request for data can be submitted in a simple manner. The system is developed with Java Servlet for the back-end, and Java Server Pages (JSP) for content display. The advantage of JSP's is the separation of the front-end presentation from the middle- and back-end tiers which led to an efficient development of the system. The SMOKA homepage is available at SMOKA

  3. A SPECTROSCOPIC ANALYSIS OF WHITE DWARFS IN THE KISO SURVEY

    SciTech Connect

    Limoges, M.-M.; Bergeron, P. E-mail: bergeron@astro.umontreal.c

    2010-05-10

    We present a spectroscopic analysis of white dwarfs found in the Kiso survey. Spectroscopic observations at high signal-to-noise ratio have been obtained for all DA and DB stars in the Kiso Schmidt ultraviolet excess survey (KUV stars). These observations led to the reclassification of several KUV objects, including the discovery of three unresolved DA+DB double-degenerate binaries. The atmospheric parameters (T{sub eff} and log g) are obtained from detailed model atmosphere fits to optical spectroscopic data. The mass distribution of our sample is characterized by a mean value of 0.606 M{sub sun} and a dispersion of 0.135 M{sub sun} for DA stars, and 0.758 M{sub sun} and a dispersion of 0.192 M{sub sun} for DB stars. Absolute visual magnitudes obtained from our spectroscopic fits allow us to derive an improved luminosity function for the DA and DB stars identified in the Kiso survey. Our luminosity function is found to be significantly different from earlier estimates based on empirical photometric calibrations of M{sub V} for the same sample. The results for the DA stars now appear entirely consistent with those obtained for the PG survey using the same spectroscopic approach. The space density for DA stars with M{sub V} {<=} 12.75 is 2.80 x 10{sup -4} pc{sup -3} in the Kiso survey, which is 9.6% smaller than the value found in the PG survey. The completeness of both surveys is briefly discussed.

  4. GRB 151205C: Optical follow-up observations at Kiso

    NASA Astrophysics Data System (ADS)

    Kikuchi, Yuki; Tanaka, Masaomi; Ohsawa, Ryou; Ichiki, Makoto; Sako, Shigeyuki; Morokuma, Tomoki; Doi, Mamoru; Tominaga, Nozomu; Serino, Motoko; Suzuki, Akihiro; Maeda, Keiichi; Sakamoto, Takanori

    2015-12-01

    We performed optical non-filter imaging observations for the MAXI-detected burst GRB 151205C (Nakajima et al. GCN Circ. 18666) with a prototype model camera of Tomo-e Gozen (Tomo-e PM). Tomo-e Gozen is a wide-field optical imaging camera with 84 1kx2k CMOS sensors on the focal plane of the 1.05-m Kiso Schmidt telescope (Sako et al. in preparation, http://www.ioa.s.u-tokyo.ac.jp/tomoe/).

  5. KWFC: four square degrees camera for the Kiso Schmidt Telescope

    NASA Astrophysics Data System (ADS)

    Sako, Shigeyuki; Aoki, Tsutomu; Doi, Mamoru; Ienaka, Nobuyuki; Kobayashi, Naoto; Matsunaga, Noriyuki; Mito, Hiroyuki; Miyata, Takashi; Morokuma, Tomoki; Nakada, Yoshikazu; Soyano, Takao; Tarusawa, Ken'ichi; Miyazaki, Satoshi; Nakata, Fumiaki; Okada, Norio; Sarugaku, Yuki; Richmond, Michael W.

    2012-09-01

    The Kiso Wide Field Camera (KWFC) is a facility instrument for the 105-cm Schmidt telescope being operated by the Kiso Observatory of the University of Tokyo. This camera has been designed for wide-field observations by taking advantage of a large focal-plane area of the Schmidt telescope. Eight CCD chips with a total of 8k x 8k pixels cover a field-of-view of 2.2 degrees x 2.2 degrees on the sky. The dewar window works as a field flattener lens minimizing an image distortion across the field of view. Two shutter plates moving in parallel achieve uniform exposures on all the CCD pixels. The KWFC is equipped with a filter exchanger composed of an industrial robotic arm, a filter magazine capable of storing 12 filters, and a filter holder at the focal plane. Both the arm and the magazine are installed inside the tube framework of the telescope but without vignetting the beam. Wide-field survey programs searching for supernovae and late-type variable stars have begun in April 2012. The survey observations are performed with a management software system for facility instruments including the telescope and the KWFC. This system automatically carries out observations based on target lists registered in advance and makes appropriate decisions for implementation of observations by referring to weather conditions and status of the instruments. Image data obtained in the surveys are processed with pipeline software in real time to search for candidates of time-variable sources.

  6. 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. PMID:21963881

  7. Genetic Diversity of Maternal Lineage in the Endangered Kiso Horse Based on Polymorphism of the Mitochondrial DNA D-Loop Region

    PubMed Central

    TAKASU, Masaki; ISHIHARA, Namiko; TOZAKI, Teruaki; KAKOI, Hironaga; MAEDA, Masami; MUKOYAMA, Harutaka

    2014-01-01

    ABSTRACT To determine genetic characteristics of the maternal lineage of the Kiso horse based on polymorphisms of the mitochondrial DNA D-loop region, we collected blood samples from 136 Kiso horses, 91% of the entire population, and sequenced 411 bp from 15,437 to 15,847 in the region. First of all, we estimated the demographic history; by searching homology between the obtained and known sequences using Basic Local Alignment Search Tool, by mismatch analysis to evaluate the mutation processes using Arlequin, and by building a phylogenetic tree showing the relationship of the mtDNA haplotypes for 24 horse breeds around the world using Molecular Evolutionary Genetics Analysis softwear. The results suggested that various horses that came to Japan stayed at Kiso region and became ancestors of Kiso horse and also genetically supported the theory that the Kiso horse was historically improved by other Japanese native horse breeds. Next, we analyzed the diversity of current maternal lineage by classifying the resulting sequences, and by calculating the haplotype diversity and nucleotide diversity using Arlequin. Then, we visualized the relationship among haplotypes by a median-joining network using NETWORK 4.6.0.0. The results suggested the diversity of maternal lineage in the Kiso horse was reasonably maintained. Lastly, we predicted future change of the diversity of maternal lineage in Kiso horse by assessing the regional distribution of the acquired haplotypes. The distribution suggested that diversity of maternal lineage would possibly be reducing. PMID:25056676

  8. Genetic diversity of maternal lineage in the endangered Kiso horse based on polymorphism of the mitochondrial DNA D-loop region.

    PubMed

    Takasu, Masaki; Ishihara, Namiko; Tozaki, Teruaki; Kakoi, Hironaga; Maeda, Masami; Mukoyama, Harutaka

    2014-11-01

    To determine genetic characteristics of the maternal lineage of the Kiso horse based on polymorphisms of the mitochondrial DNA D-loop region, we collected blood samples from 136 Kiso horses, 91% of the entire population, and sequenced 411 bp from 15,437 to 15,847 in the region. First of all, we estimated the demographic history; by searching homology between the obtained and known sequences using Basic Local Alignment Search Tool, by mismatch analysis to evaluate the mutation processes using Arlequin, and by building a phylogenetic tree showing the relationship of the mtDNA haplotypes for 24 horse breeds around the world using Molecular Evolutionary Genetics Analysis softwear. The results suggested that various horses that came to Japan stayed at Kiso region and became ancestors of Kiso horse and also genetically supported the theory that the Kiso horse was historically improved by other Japanese native horse breeds. Next, we analyzed the diversity of current maternal lineage by classifying the resulting sequences, and by calculating the haplotype diversity and nucleotide diversity using Arlequin. Then, we visualized the relationship among haplotypes by a median-joining network using NETWORK 4.6.0.0. The results suggested the diversity of maternal lineage in the Kiso horse was reasonably maintained. Lastly, we predicted future change of the diversity of maternal lineage in Kiso horse by assessing the regional distribution of the acquired haplotypes. The distribution suggested that diversity of maternal lineage would possibly be reducing. PMID:25056676

  9. Spectral types for objects in the Kiso survey. IV - Data for 81 stars

    NASA Technical Reports Server (NTRS)

    Wegner, Gary; Mcmahan, Robert K.

    1988-01-01

    Spectroscopy and spectral types for 81 ultraviolet-excess objects found in the Kiso Schmidt-camera survey are reported. The data were secured with the McGraw-Hill 1.3 m telescope at 8-A resolution covering the wavelength interval 4000 -7200 A using the Mark II spectrograph. Descriptions of the spectra of some of the more peculiar objects found in this sample are given and include 14 sub-dwarfs, 23 definite DA white dwarfs, including a magnetic one, and one DQ whie dwarf, eight quasars and emission-line objects, and a new composite DA + dM system. More spectroscopy of the new cataclysmic variable KUV 01584-0939 and a possibly related object is also described.

  10. 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

  11. Hubble Space Telescope Observations of Accretion-Induced Star Formation in the Tadpole Galaxy Kiso 5639

    NASA Astrophysics Data System (ADS)

    Elmegreen, Debra Meloy; Elmegreen, Bruce G.; Sánchez Almeida, Jorge; Muñoz-Tuñón, Casiana; Mendez-Abreu, Jairo; Gallagher, John S.; Rafelski, Marc; Filho, Mercedes; Ceverino, Daniel

    2016-07-01

    The tadpole galaxy Kiso 5639 has a slowly rotating disk with a drop in metallicity at its star-forming head, suggesting that star formation was triggered by the accretion of metal-poor gas. We present multi-wavelength Hubble Space Telescope Wide Field Camera 3 images of UV through I band plus Hα to search for peripheral emission and determine the properties of various regions. The head has a mass in young stars of ∼ {10}6 {M}ȯ and an ionization rate of 6.4× {10}51 s‑1, equivalent to ∼2100 O9-type stars. There are four older star-forming regions in the tail, and an underlying disk with a photometric age of ∼1 Gyr. The mass distribution function of 61 star clusters is a power law with a slope of ‑1.73 ± 0.51. Fourteen young clusters in the head are more massive than {10}4 {M}ȯ , suggesting a clustering fraction of 30%–45%. Wispy filaments of Hα emission and young stars extend away from the galaxy. Shells and holes in the head H ii region could be from winds and supernovae. Gravity from the disk should limit the expansion of the H ii region, although hot gas might escape through the holes. The star formation surface density determined from Hα in the head is compared to that expected from likely pre-existing and accreted gas. Unless the surface density of the accreted gas is a factor of ∼3 or more larger than what was in the galaxy before, the star formation rate has to exceed the usual Kennicutt–Schmidt rate by a factor of ≥slant 5.

  12. Hubble Space Telescope Observations of Accretion-Induced Star Formation in the Tadpole Galaxy Kiso 5639

    NASA Astrophysics Data System (ADS)

    Elmegreen, Debra Meloy; Elmegreen, Bruce G.; Sánchez Almeida, Jorge; Muñoz-Tuñón, Casiana; Mendez-Abreu, Jairo; Gallagher, John S.; Rafelski, Marc; Filho, Mercedes; Ceverino, Daniel

    2016-07-01

    The tadpole galaxy Kiso 5639 has a slowly rotating disk with a drop in metallicity at its star-forming head, suggesting that star formation was triggered by the accretion of metal-poor gas. We present multi-wavelength Hubble Space Telescope Wide Field Camera 3 images of UV through I band plus Hα to search for peripheral emission and determine the properties of various regions. The head has a mass in young stars of ˜ {10}6 {M}ȯ and an ionization rate of 6.4× {10}51 s‑1, equivalent to ˜2100 O9-type stars. There are four older star-forming regions in the tail, and an underlying disk with a photometric age of ˜1 Gyr. The mass distribution function of 61 star clusters is a power law with a slope of ‑1.73 ± 0.51. Fourteen young clusters in the head are more massive than {10}4 {M}ȯ , suggesting a clustering fraction of 30%–45%. Wispy filaments of Hα emission and young stars extend away from the galaxy. Shells and holes in the head H ii region could be from winds and supernovae. Gravity from the disk should limit the expansion of the H ii region, although hot gas might escape through the holes. The star formation surface density determined from Hα in the head is compared to that expected from likely pre-existing and accreted gas. Unless the surface density of the accreted gas is a factor of ˜3 or more larger than what was in the galaxy before, the star formation rate has to exceed the usual Kennicutt–Schmidt rate by a factor of ≥slant 5.

  13. Cosmology from the KISO Ultraviolet Excess Survey: a Complete Sample of White Dwarfs and Quasars.

    NASA Astrophysics Data System (ADS)

    Darling, Gerald William

    1994-01-01

    Spectral types for 356 of the 1,186 objects comprising the Kiso Ultraviolet Excess (KUV) Survey are reported. Observations of 277 KUV objects were made at the Michigan-Dartmouth -MIT Observatory on Kitt Peak, using both the 2.4 meter Hiltner and 1.3 meter McGraw-Hill telescopes. Interesting objects reported include: 70 subdwarfs, 33 DA, 6 DQ and 3 DB white dwarfs, and 95 QSO and emission line objects. A search through the literature has revealed the spectral identification of an additional 79 KUV objects. This brings the total identified to 1,115 (94%), including samples of 234 white dwarfs and 170 quasars. The V/Vmax technique (Schmidt 1968) was applied to the complete samples of white dwarfs and quasars to estimate the limiting magnitude of the KUV Survey and construct luminosity functions of these populations. The limiting magnitude was estimated to be 17.35 from the KUV white dwarfs and 17.81 from the KUV quasars. Theoretical white dwarf luminosity functions (WDLF) are used with the observational WDLF determined in this work to estimate the age of the Galactic disc at our galactocentric radius to be between 8.0 Gyr and 110 Gyr, with 9.0 Gyr being the best estimate. If 1.0 Gyr is chosen as the interval between the creation event and star formation in the Galactic disc (Winget et al. 1987), the age of the universe is then estimated to be 10.0 Gyr. The deeper KUV Survey has be used to analyze the completeness of the Palomar-Green (PG) Survey. If completeness is defined by the number of KUV objects located in the overlapping area of the surveys, and brighter than their PG field's limiting magnitude, compared to the number of these KUV objects actually detected by the PG, then an estimate of completeness based on spectral type for the PG is: 57% for quasars, 58% for white dwarfs and 53% for all objects. Limits on the selection function of the PG are calculated, and the PG is determined to be approximately 75% complete out to between 15.15 and 16.15 magnitude where

  14. Ultraviolet Spectra of Two Magnetic White Dwarfs and Ultraviolet Spectra of Subluminous Objects Found in the Kiso Schmidt Survey

    NASA Technical Reports Server (NTRS)

    Wegner, Gary A.

    1987-01-01

    Low resolution International Ultraviolet Explorer (IUE) spectroscopic observations of two magnetic white dwarfs BPM25114 and K813-14 were obtained using both the SWP and LWP cameras. The first object has an observed magnetic field of 4 x 10(7) Gauss and the second has one of 3 x 10(7) Gauss. Both objects have overall spectral energy distributions appropriate for cool DA white dwarfs with T(eff) near 10,000 K and accordingly show strong lambda lambda 1400 and 1600 absorption in their spectra. Compared to non-magnetic DA white dwarfs of comparable effective temperature, there are some differences in the profiles, presumably produced by the magnetic fields in these objects. In addition, the ultraviolet spectra of a number of hot subluminous stars in the Kiso Schmidt survey were observed.

  15. 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.

  16. 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

  17. 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.

  18. Hydrogen and carbon isotope studies on the graphite-bearing metapelites in the northern Kiso district of central Japan

    NASA Astrophysics Data System (ADS)

    Morikiyo, Toshiro

    1986-06-01

    Measurements were made of the hydrogen isotope ratios of hydrous silicates (mica and amphibole) and whole rocks, and the carbon isotope ratios of graphite and carbonaceous matter in the metamorphic rocks from the northern Kiso district in central Japan. δD values of hydrous silicates in the graphite-bearing metapelites are always higher than those in graphite-free schists, even though the sample localities of the two rock-types are very close. Hydrogen isotopic equilibrium has been attained between the coexisting minerals. D/H ratios of water in the metamorphic fluids seem to depend strongly on the presence or absence of graphite and seem to be not constant throughout the district. The district is divided into three areas of low (metamorphic zones I, II), medium (zones IIIa V) and high δ 13Cgr value (zones VIa VII) areas. In the high δ 13Cgr values area, the carbon contents of the graphite-bearing rocks decrease slightly from zones VIa to VII, whereas the δ 13Cgr values increase sharply from the upper part of zone VIa to VIb. The δD values of biotite in these graphite-bearing rocks are higher than those in the medium δ 13Cgr area. This suggests that methane enriched in H and12C is produced and liberated by the devolatilization reactions between muscovite, graphite and water. The fluid produced is composed of water, methane and a subordinate amount of carbon dioxide, and its log fO2 value is deduced to be about 1.2 lower than that defined by the FMQ buffer. In the medium δ 13Cgr area, the δ 13C values of graphite are nearly constant (-20.8‰), while the Fe2O3/(Fe2O3 + FeO) ratio of the graphite-bearing rocks apparently decreases with increasing metamorphic grade. δD differences in hydrous silicates between graphite-bearing and graphite-free rocks are observed. These facts are interpreted to mean that methane was produced in addition to water and carbon dioxide, and that its generation (X_{{text{CH}}_{text{4}} } /X_{{text{CO}}_{text{2}} } ratio of the fluid

  19. 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.

  20. 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…

  1. 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…

  2. 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…

  3. Massive Clumps in Local Galaxies: Comparisons with High-redshift Clumps

    NASA Astrophysics Data System (ADS)

    Elmegreen, Bruce G.; Elmegreen, Debra Meloy; Sánchez Almeida, J.; Muñoz-Tuñón, C.; Dewberry, J.; Putko, J.; Teich, Y.; Popinchalk, M.

    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.

  4. 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.

  5. KISS: Discovery and Spectroscopic Classification of a Type Ia Supernova KISS15q

    NASA Astrophysics Data System (ADS)

    Morokuma, Tomoki; Tominaga, Nozomu; Tanaka, Masaomi; Jiang, Ji-an; Shibata, Takumi; Kokubo, Mitsuru; Hashiba, Yasuhito; Mitsuda, Kazuma; Doi, Mamoru; Sako, Shigeyuki; Kikuchi, Yuki; Takahashi, Hidenori; Tateuchi, Ken; Kuncarayakti, Hanindyo; Watanabe, Makoto; Nakao, Hikaru; Itoh, Yoichi; Morihana, Kumiko; Honda, Satoshi; Takagi, Yuhei; Takahashi, Jun; Takeishi, Masanori

    2015-05-01

    We report the discovery and spectroscopic identification of a Type Ia supernova, KISS15q. In Kiso Supernova Survey (KISS; Morokuma et al. 2014, PASJ, 66, 118), we found a transient object KISS15q of g=20.6 on May 19.60, 2015 UT in the g-band image.

  6. 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.

  7. Optical and CO Radio Observations of Poor Cluster Zwicky 1615.8+3505

    NASA Astrophysics Data System (ADS)

    Tomita, Akihiko; Maehara, Hideo; Takeuchi, Tsutomu T.; Nakanishi, Kouichiro; Honma, Mareki; Tutui, Yoshinori; Sofue, Yoshiaki

    1999-06-01

    The cluster Zwicky 1615.8+3505 is considered to be a dynamically young poor cluster. To investigate the morphology and star-formation activity of galaxies under the environment of a dynamically young poor cluster, we have performed V, R, and I surface photometry, optical low-resolution spectroscopy, and 12CO (J=1-0) line observations for member galaxies. Our data show that more than 90% of the observed galaxies show regular morphologies and no star-formation activities, indicating that the environment does not affect these galaxy properties. Among sixteen galaxies observed, only NGC 6104 shows a significant star-formation activity, and shows a distorted morphology, indicating a tidal interaction. This galaxy contains double knots, and only one knot possesses Seyfert activity, though the sizes and luminosities are similar to each other; we also discuss this feature. Based on observations made at Okayama Astrophysical Observatory (OAO), Kiso Observatory (KISO), and Nobeyama Radio Observatory (NRO). KISO is operated by Institute of Astronomy, School of Science, The University of Tokyo. OAO and NRO are branches of the National Astronomical Observatory, an inter-university research institute operated by the Ministry of Education, Science, Sports and Culture.

  8. Development of public science archive system of Subaru Telescope

    NASA Astrophysics Data System (ADS)

    Baba, Hajime; Yasuda, Naoki; Ichikawa, Shin-Ichi; Yagi, Masafumi; Iwamoto, Nobuyuki; Takata, Tadafumi; Horaguchi, Toshihiro; Taga, Masatochi; Watanabe, Masaru; Okumura, Shin-Ichiro; Ozawa, Tomohiko; Yamamoto, Naotaka; Hamabe, Masaru

    2002-09-01

    We have developed a public science archive system, Subaru-Mitaka-Okayama-Kiso Archive system (SMOKA), as a successor of Mitaka-Okayama-Kiso Archive (MOKA) system. SMOKA provides an access to the public data of Subaru Telescope, the 188 cm telescope at Okayama Astrophysical Observatory, and the 105 cm Schmidt telescope at Kiso Observatory of the University of Tokyo. Since 1997, we have tried to compile the dictionary of FITS header keywords. The accomplishment of the dictionary enabled us to construct an unified public archive of the data obtained with various instruments at the telescopes. SMOKA has two kinds of user interfaces; Simple Search and Advanced Search. Novices can search data by simply selecting the name of the target with the Simple Search interface. Experts would prefer to set detailed constraints on the query, using the Advanced Search interface. In order to improve the efficiency of searching, several new features are implemented, such as archive status plots, calibration data search, an annotation system, and an improved Quick Look Image browsing system. We can efficiently develop and operate SMOKA by adopting a three-tier model for the system. Java servlets and Java Server Pages (JSP) are useful to separate the front-end presentation from the middle and back-end tiers.

  9. An NMR and relativistic DFT investigation of one-bond nuclear spin-spin coupling in solid triphenyl group-14 chlorides.

    PubMed

    Willans, Mathew J; Demko, Bryan A; Wasylishen, Roderick E

    2006-06-21

    A solid-state nuclear magnetic resonance and zeroth-order regular approximation density functional theory, ZORA-DFT, study of one-bond nuclear spin-spin coupling between group-14 nuclei and quadrupolar 35/37Cl nuclei in triphenyl group-14 chlorides, Ph3XCl (X = C, Si, Ge, Sn and Pb), is presented. This represents the first combined experimental and theoretical systematic study of spin-spin coupling involving spin-pairs containing quadrupolar nuclei. Solid-state NMR spectra have been acquired for all compounds in which X has a spin-1/2 isotope--13C, 29Si, [117/119]Sn and 207Pb-at applied magnetic fields of 4.70, 7.05 and 11.75 T. From simulations of these spectra, values describing the indirect spin-spin coupling tensor-the isotropic indirect spin-spin coupling constant, 1J(X, 35/37Cl)iso and the anisotropy of the J tensor, Delta1J(X, 35/37Cl)--have been determined for all but the lead-chlorine spin-pair. To better compare the indirect spin-spin coupling parameters between spin-pairs, 1J(iso) and Delta1J values were converted to their reduced coupling constants, 1K(iso) and Delta1K. From experiment, the sign of 1K(iso) was found to be negative while the sign of Delta1K is positive for all spin-pairs investigated. The magnitude of both 1K(iso) and Delta1K was found to increase as one moves down group-14. Theoretical values of the magnitude and sign of 1K(iso) and Delta1K were obtained from ZORA-DFT calculations and are in agreement with the available experimental data. From the calculations, the Fermi-contact mechanism was determined to provide the largest contribution to 1K(iso) for all spin-pairs while spin-dipolar and paramagnetic spin-orbit mechanisms make significant contributions to the anisotropy of K. The inclusion of relativistic effects was found to influence K(Sn,Cl) and K(Pb,Cl). PMID:16763706

  10. Periodic trends in indirect nuclear spin-spin coupling tensors: relativistic density functional calculations for interhalogen diatomics.

    PubMed

    Bryce, David L; Wasylishen, Roderick E; Autschbach, Jochen; Ziegler, Tom

    2002-05-01

    There have been significant advances in the calculation and interpretation of indirect nuclear spin-spin coupling (J) tensors during the past few years; however, much work remains to be done, especially for molecules containing heavy atoms where relativistic effects may play an important role. Many J tensors cannot be explained based solely on a nonrelativistic Fermi-contact mechanism. In the present work, the relativistic zeroth-order regular approximation density-functional (ZORA-DFT) implementation for the calculation of J has been applied to the complete series of homonuclear and heteronuclear diatomic halogen molecules: F(2), Cl(2), Br(2), I(2), At(2), ClF, BrF, IF, ClBr, ClI, and BrI. For all of these compounds, the reduced isotropic coupling constant (K(iso)) is positive and the reduced anisotropic coupling constant (DeltaK) is negative. With the exception of molecular fluorine, the magnitudes of K(iso) and DeltaK are shown to increase linearly with the product of the atomic numbers of the coupled nuclei. ZORA-DFT calculations of J for F(2) and ClF are in excellent agreement with the results obtained from multiconfigurational self-consistent-field calculations. The relative importance of the various coupling mechanisms is approximately constant for all of the compounds, with the paramagnetic spin-orbit term being the dominant contributor to K(iso), at approximately 70-80%. Available experimental stimulated resonant Raman spectroscopy data are exploited to extract the complete J((127)I,(127)I) tensor for iodine in two rotational states. The dependence of K(iso) and DeltaK on bond length and rovibrational state is investigated by using calculated results in combination with available experimental data. In addition to providing new insights into periodic trends for J coupling tensors, this work further demonstrates the utility of the ZORA-DFT method and emphasizes the necessity of spin-orbit relativistic corrections for J calculations involving heavy nuclei

  11. 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.

  12. 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.

  13. 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.

  14. 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.

  15. 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

    2016-06-01

    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.

  16. Last 900 ka river longprofile changes controlled by Yoro fault activity and glacial sea-level changes, Nobi plain, central Japan

    NASA Astrophysics Data System (ADS)

    Sugai, T.; Sato, T.

    2015-12-01

    This paper compared grain size, thickness, and lithological character of ten fluvial gravel layers formed during the glacial sea-level lowstands intervening inner bay mud layers deposited during the interglacial marine transgressional periods since the last 900 ka by integrated analyses of sediment cores including 600 m deep onein the Nobi plain, central Japan. Linkages between river long profile changes and sea-level and climate changes will be discussed. The Nobi basin is one of the representative delta type alluvial lowlands in Japan dominated by longitudinal drainage system named Kiso river system flowing southward from central Japan Alps with abundant water and sediment discharges. The basin bounded by the Yoro fault on the west has been tilted westward by the repetitive faulting activity. The basin stratigraphy and its stacking patterns suggest uniform and rapid subsidence and tilting rates of the basin with the maximum value of 1 mm yr-1 and 10-4 kyr-1 respectively produced by the Yoro fault activity under the W-E compressional regional stress field during the middle and late Quaternary periods. Tephrochronological, paleomagnetic, geochemical, and diatom analyses enabled to identify ten times repeated marine transgression-regression sequences correlated with full glacial-interglacial sea-level changes during the last 900 ka. All of the ten sequence boundaries were characterized by fluvial gravel layers were formed by the Kiso river system. The mean maximum gravel size is proportional to the magnitude of sea level lowering inferred from MIS curve, i.e. gravels deposited in MIS 12 and 16 are the largest, and those in MIS 14 and 8 are the smallest since MIS 16. This suggests that the longitudinal profile of the Kiso river system has been adjusting to the sea level changes and that the steeper longitudinal profile formed in the lower sea level periods can transport larger gravels to the drilling sites. In fact the present river bed gravel size is in proportion

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

    NASA Astrophysics Data System (ADS)

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

    1992-12-01

    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.

  18. D*Ξ N bound state in strange three-body systems

    NASA Astrophysics Data System (ADS)

    Garcilazo, H.; Valcarce, A.

    2016-06-01

    The recent update of the strangeness -2 ESC08c Nijmegen potential incorporating the NAGARA and KISO events predicts a Ξ N bound state, D*, in the S31(I =1 ) channel. We study if the existence of this two-body bound state could give rise to stable three-body systems. For this purpose we solve the bound state problem of three-body systems where the Ξ N state is merged with N 's , Λ 's , Σ 's , or Ξ 's , making use of the most recent updates of the two-body ESC08c Nijmegen potentials. We found that there appear stable states in the Ξ N N and Ξ Ξ N systems, the Ξ Λ N and Ξ Σ N systems being unbound.

  19. Development of Extremely Wide-Field CMOS Camera Tomo-e:Contribution to Small Solar System Objects

    NASA Astrophysics Data System (ADS)

    Watanabe, Juniichi; Yoshikawa, Makoto; Urakawa, Seitaro; Usui, Fumihiko; Ohsawa, Ryou; Sako, Shigeyuki; Arimatsu, Ko

    2016-07-01

    We are developing an ultra wide-field fast camera, Tomo-e Gozen, which will be set up on the 105cm (F3.1) Schmidt telescope in Kiso Observatory at the University of Tokyo. Tomo-e equipped with 84 CMOS image sensors, which work in a room temperature, has a 20 square degree field of view and a fast readout speed of ~2 Hz. The purpose of this camera is the observation of the transient objects such as the counterpart of the gravitational wave events, the ultra wide-field capability with a high survey efficiency is also useful for small solar system bodies; NEOs, occultation events of the TNOs, and meteors. In the presentation, the specifications of Tomo-e are shown together with some preliminary results of the experimental observation run.

  20. 103Rh-NMR studies in the superconductor Rh17S15

    NASA Astrophysics Data System (ADS)

    Koyama, T.; Kanda, K.; Ueda, K.; Mito, T.; Kohara, T.; Nakamura, H.

    2010-01-01

    103Rh nuclear magnetic resonance (NMR) measurements have been performed in the superconductor Rh17S15 with the transition temperature TC=5.4 K. The observed 103Rh-NMR spectrum shows an asymmetric shape with several peaks, reflecting the local symmetry around each Rh site. We have identified the observed NMR lines corresponding to four different Rh sites and obtained the temperature (T) dependence of the Knight shift of 24m site. The isotropic part of the Knight shift Kiso decreases with decreasing T, indicating the existence of the electron correlation in Rh17S15. In the superconducting state, the resonance lines shift to higher frequencies owing to a decrease of the spin part of the Knight shift with negative hyperfine coupling.

  1. Studies of 27Al NMR in EuAl4

    NASA Astrophysics Data System (ADS)

    Niki, H.; Nakamura, S.; Higa, N.; Kuroshima, H.; Toji, T.; Yogi, M.; Nakamura, A.; Hedo, M.; Nakama, T.; Ōnuki, Y.; Harima, H.

    2015-03-01

    EuAl4 orders antiferromagnetically at TN ≈ 16 K with an effective magnetic moment of 8.02 μB. In the paramagnetic phase, the magnetic susceptibility of EuAl4 follows the Curie-Weiss law with a positive Curie-Weiss temperature θP = +14 K. The antiferromagnetic state is changed into the field induced ferromagnetic state at a critical field Hc of approximately 2 T. In order to microscopically investigate the magnetic and electronic properties in EuAl4, the NMR measurements of EuAl4 have been carried out at temperatures between 2 and 300 K, applying an external magnetic field of approximately 6.5 T. The 27Al NMR spectra corresponding to Al(I) and Al(II) sites are obtained. From the 27Al NMR spectra, the isotropic part Kiso and anisotropic part Kaniso of Knight shift, and nuclear quadrupole frequncy νQ are obtained. The Kiso and Kaniso shift to negative side with decreasing temperature due to the RKKY interaction. These temperature dependences follow the Curie-Weiss law with θP = +14 K, which is consistent with that of the magnetic susceptibility. From the K - χ plot, the values of the hyperfine fields Hhf_iso and Hhf_aniso are -3.231 and -0.162 kOe/μB for Al(I) site, and -1.823 and -0.264 kOe/μB for Al(II) site, respectively. The values of νQ of 27Al nucleus for Al(I) and Al(II) sites are approximately 0.865 and 0.409 MHz, respectively. The nuclear relaxation time T1 of 27Al NMR for both sites is almost constant in the paramagnetic phase, while the value of 1/T1 is abruptly decreased in the ordered ferromagnetic state.

  2. Strategy and results of East Asian GRB FOllow-up Network (EAFON) follow-up observations

    NASA Astrophysics Data System (ADS)

    Urata, Y.; Eafon Team

    We have established Japan-Taiwan-China collaboration on GRBs study in the East-Asian region since 2004 This serves as valuable additions to the world-wide optical and infrared follow-up network because the East-Asia region is otherwise blank for the network We have been carrying out imaging and spectroscopic follow-up observations by Lulin Taiwan Kiso Japan WIDGET Japan and Xinglong China Using Xinglong and Kiso we can locate candidates and obtain early time spectra of afterglows While WIDGET provides early time observations before the burst the high-time resolution for multi-band light curves will be obtained by Lulin With the data from these sites we will obtain detailed information of light curve and redshift of GRBs which are important to understand the mechanism of afterglows Utilizing East Asian GRB Follow-up Observation Network EAFON we have observed 56 GRB optical afterglows and detected 15 early optical afterglow behavior including two short GRBs in multi-bands Based on these observations we have obtained 3 major results 1 first long term monitoring of short GRB afterglow from sim 0 1 days after the burst 2 two components in early optical afterglow 3 catch about 30 high redshift GRB candidates In this meeting we will present mainly report early a common feature of long GRB early afterglow We have found a common feature in long GRB early afterglow light curves These early light curves show re-brightening and or plateau phase around 0 1 days 2 4hours after bursts Combined with other prompt

  3. Mind as Space

    NASA Astrophysics Data System (ADS)

    McKinstry, Chris

    The present article describes a possible method for the automatic discovery of a universal human semantic-affective hyperspatial approximation of the human subcognitive substrate - the associative network which French (1990) asserts is the ultimate foundation of the human ability to pass the Turing Test - that does not require a machine to have direct human experience or a physical human body. This method involves automatic programming - such as Koza's genetic programming (1992) - guided in the discovery of the proposed universal hypergeometry by feedback from a Minimum Intelligent Signal Test or MIST (McKinstry, 1997) constructed from a very large number of human validated probabilistic propositions collected from a large population of Internet users. It will be argued that though a lifetime of human experience is required to pass a rigorous Turing Test, a probabilistic propositional approximation of this experience can be constructed via public participation on the Internet, and then used as a fitness function to direct the artificial evolution of a universal hypergeometry capable of classifying arbitrary propositions. A model of this hypergeometry will be presented; it predicts Miller's "Magical Number Seven" (1956) as the size of human short-term memory from fundamental hypergeometric properties. A system that can lead to the generation of novel propositions or "artificial thoughts" will also be described.

  4. The Kosice meteorite

    NASA Astrophysics Data System (ADS)

    Toth, J.; Svoren, J.

    2012-01-01

    Sciences (under the leadership of the second author), Comenius University in Bratislava (under the leadership of the first author), and the Czech Academy of Sciences (under the leadership of Pavel Spurny) started to sweep meadows and forests at the calculated area. The first meteorite was discovered by Juraj Toth on March 20th. By October 6th, 77 meteorite fragments were found. The heaviest fragment weighs 2.17 kg and was found by Tereza Krejcova; the smallest pieces were only about 0.5 g (finder Julius Koza). The total mass recovered is 4.3 kg. There were 28 finders: Juraj Toth, Diana Buzova, Marek Husarik, Tereza Krejcova, Jan Svoren, Julius Koza, David Capek, Pavel Spurny, Stanislav Kaniansky, Eva Schunova, Marcel Skreka, Dusan Tomko, Pavol Zigo, Miroslav Seben, Jiri Silha, Leonard Kornos, Marcela Bodnarova, Peter Veres, Jozef Nedoroscik, Zuzana Mimovicova, Zuzana Krisandova, Jaromir Petrzala, Stefan Gajdos, Tomas Dobrovodsky, Peter Delincak, Zdenko Bartos, Ales Kucera, and Jozef Vilagi. Preliminary as well as complex mineralogic analysis implies that the recovered meteorite is classified as an ordinary H5 chondrite (Dr. J. Haloda, Czech Geological Survey, D. Ozdin, and P. Uher, Comenius University in Bratislava). The authors are grateful to all collaborators mentioned above. More details about the meteorite will be published in the near future.

  5. The Anisotropic Aphid: Three-Dimensional Induction Modeling of Electrical Texture with Mixed Potentials

    NASA Astrophysics Data System (ADS)

    Weiss, C. J.

    2014-12-01

    At the macroscopic scale, where the e-folding distance of low-frequency electromagnetic fields in conductive geomaterials is much larger than the size of organized heterogeneities such as fracture sets or laminations that constitute the geologic texture therein, electrical properties can be conveniently approximated by a generalized 3x3 tensor σ. Less convenient, however, are the algorithmic consequences of this approximation in electromagnetic modeling of 3D induction methods for geophysical exploration. Previous efforts at modelling generalized anisotropy with finite differences on a staggered Cartesian grid (e.g. Weiss and Newman, 2002; Wang and Fang, 2001) are posed in terms of the electric field with its governing "curl-curl" equation and well-documented null-space issues at low induction numbers. In contrast, Weiss (2013) proposed an alternate full-physics formulation in terms of Lorenz-gauged magentic vector A and electric scalar Φ potentials (Project APhiD) that eliminates the troublesome curl-curl operator, with ultrabroadband examples drawn from geologies with scalar, isotropic conductivity over the frequency range 10-2-1010 Hz. Here, the anisotropic theory presented in Weiss (2013) is implemented with finite differences on a Cartesian grid. Briefly stated, in this theoretical approach the conductivity tensor σ is split in terms of a rotationally-invariant isotropic conductivity σ* = ⅓ Tr(σ) and the residual σ - σ*I. This splitting decomposes the resulting finite difference coefficient matrix K into the sum Kiso + Kaniso, where the Kiso term is the coefficient matrix for the isotropic medium σ*, thus enabling reuse of the various routines previously developed for computing matrix coefficients in the isotropic case. Treatment of anisotropy is algorithmically therefore restricted to computing the coefficients in the sparse matrix Kaniso consisting of simple inner products of (σ - σ*I) · (A-∇Φ) and their divergence. In keeping with the

  6. 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

  7. Constraining the Age and Distance of the Galactic Supernova Remnant G156.2+5.7 by Hα Expansion Measurements

    NASA Astrophysics Data System (ADS)

    Katsuda, Satoru; Tanaka, Masaomi; Morokuma, Tomoki; Fesen, Robert; Milisavljevic, Dan

    2016-08-01

    We present deep Hα images of portions of the X-ray bright, but optically faint, Galactic supernova remnant G156.2+5.7, revealing numerous and delicately thin non-radiative filaments, which mark the location of the remnant’s forward shock. These new images show that these filaments have a complex structure not visible on previous lower resolution optical images. By comparing Hα images taken in 2004 at the McDonald Observatory and in 2015–2016 at the Kiso Observatory, we set a stringent 1σ upper limit of expansion to be 0\\buildrel{\\prime\\prime}\\over{.} 06 yr‑1. This proper motion, combined with a shock speed of 500 km s‑1, inferred from X-ray spectral analyses, gives a distance of ≳1.7 kpc. In addition, a simple comparison of expansion indices of several supernova remnants allows us to infer the age of the remnant to be a few tens of thousands years old. These estimates are more straightforward and reliable than any other previous studies, and clearly rule out the possibility that G156.2+5.7 is physically associated with part of the Taurus–Auriga cloud and dust complex at a distance of 200–300 pc.

  8. 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.

  9. ISO continuum observations of quasars at z=1-4. I. Spectral energy distributions of quasars from the UV to far-infrared

    NASA Astrophysics Data System (ADS)

    Oyabu, S.; Kawara, K.; Tsuzuki, Y.; Sofue, Y.; Sato, Y.; Okuda, H.; Taniguchi, Y.; Shibai, H.; Gabriel, C.; Hasegawa, T.; Nishihara, E.

    2001-01-01

    Eight luminous quasars with -30 < MB < -27 at z = 1.4-3.7 have been observed in the mid- and far-infrared using ISO. All the quasars have been detected in the mid-infrared bands of ISOCAM, while no far-infrared detections have been made with ISOPHOT. SEDs (Spectral Energy Distributions) from the UV to far-infrared have been obtained while supplementing ISO observations with photometry in the optical and near-infrared made from the ground within 17 months. The SEDs are compared with the MED (Mean spectral Energy Distributions) of low-redshift quasars with -27 < MB < -22. It is shown that our far-infrared observations were limited by confusion noise due to crowded sources. The observations reported here were made with ISO, an ESA project with instruments funded by ESA member states (especially the PI countries: France, Germany, The Netherlands, and the UK) and with the participation of ISAS and NASA, and with the facilities at the Cerro Tololo Inter-american Observatory (CTIO), NOAO, which is operated by AURA, Inc., under contract with NSF, at the Kiso Observatory, which is operated by Institute of Astronomy, the University of Tokyo, and at the Okayama Astrophysical Observatory, the National Astronomical Observatory of Japan.

  10. STAR FORMATION STUDIES WITH THE SLOAN DIGITAL SKY SURVEY

    SciTech Connect

    P. MCGEHEE

    2001-03-01

    The determination of timescales associated with planetary formation and circumstellar disk evolution requires large samples of stars having diverse environments and ages. Such a sample can be obtained using the Sloan Digital Sky Survey (York et al. 2000) as it is systematically mapping one-quarter of the entire sky providing photometric data on over 100 million objects in five passbands (Gunn et al. 1998, Fukugita et al. 1996). Pre main sequence stars have distinct colors in the SDSS u'g'r'i'z' photometric system as a consequence of their late-type photospheres and strong UV excess driven by the magnetospheric accretion shock. SDSS observations of known Orion population emission line stars cataloged by the Kiso objective prism survey reveal a color-based signature that correlates well with the H{alpha} emission line strength. As the excess emission is a direct consequence of the presence of a circumstellar disk we can constraint the duration of the planetary formation process by determining the age of the young star. Follow-on observations of SDSS T Tauri candidates have begun at the Astrophysical Research Consortium's 3.5 meter telescope using medium resolution (R = 5000) spectroscopy. The aim is to place these objects on theoretical evolutionary tracks using spectral indicators for effective temperature and surface gravity and to create a catalog for future studies including a circumstellar disk census.

  11. 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

    2016-05-01

    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.

  12. Optical Synchrotron Precursors of Radio Hypernovae

    NASA Astrophysics Data System (ADS)

    Nakauchi, Daisuke; Kashiyama, Kazumi; Nagakura, Hiroki; Suwa, Yudai; Nakamura, Takashi

    2015-06-01

    We examine the bright radio synchrotron counterparts of low-luminosity gamma-ray bursts and relativistic supernovae (SNe) and find that they can be powered by spherical hypernova (HN) explosions. Our results imply that radio-bright HNe are driven by relativistic jets that are choked deep inside the progenitor stars or quasi-spherical magnetized winds from fast-rotating magnetars. We also consider the optical synchrotron counterparts of radio-bright HNe and show that they can be observed as precursors several days before the SN peak with an r-band absolute magnitude of {{M}r}∼ -14 mag. While previous studies suggested that additional trans-relativistic components are required to power the bright radio emission, we find that they overestimated the energy budget of the trans-relativistic component by overlooking some factors related to the minimum energy of non-thermal electrons. If an additional trans-relativistic component exists, then a much brighter optical precursor with {{M}r}∼ -20 mag can be expected. Thus, the scenarios of radio-bright HNe can be distinguished by using optical precursors, which can be detectable from ≲ 100 Mpc by current SN surveys like the Kiso SN Survey, Palomar Transient Factory, and Panoramic Survey Telescope & Rapid Response System.

  13. 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.

  14. 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.

  15. 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.

  16. Study of Double-strangeness Nuclear Systems with Nuclear Emulsion

    NASA Astrophysics Data System (ADS)

    Nakazawa, Kazuma; Endo, Yoko; Hoshino, Kaoru; Ito, Hiroki; Kinbara, Shinji; Kobayashi, Hidetaka; Mishina, Akihiro; Soe, Myint Kyaw; Theint, Aye Moh Moh; Xu, Rong; Tint, Khin Than; Yoshida, Jun'ya; Zhang, Dong Hai

    Double strangeness nuclei such as double-Λ and Ξ hypernuclei have been studied with nuclear emulsion due to its fine position resolution. Recently, we have started an experiment to study Λ-Λ interaction more accurately than that information given by the NAGARA event with ∼102 double-Λ hypernuclei which may provide us understanding free from nuclear medium effect. It is necessary to develop treatment method for huge amount, 2.1 tons of the emulsion gel, even if very pure K- beams are available at J-PARC. We have developed the base film to support the emulsion, emulsion surface coating method with a special layer of 0.5 μm thick, method for making large-size plate (35.0 x 34.5 cm2) and scanning method, called "overall scanning". The first evidence of a deeply bound state of Ξ--14N system, named KISO, was successfully detected in the test operation of the overall scanning.

  17. 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.

  18. 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. PMID:23604391

  19. Detection of Remnant Dust Cloud Associated with the 2007 Outburst of 17P/Holmes

    NASA Astrophysics Data System (ADS)

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

    2016-01-01

    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, CFOV = (2.3 ± 0.5) × 1010 m2. 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-1. The velocity was more than one order of magnitude faster than that of millimeter-centimeter grains from typical comets around a heliocentric distance rh of 2.5 AU. We considered that sudden sublimation of a large amount of water-ice (≈1030 mol s-1) would be responsible for the high ejection velocity. We finally estimated a total mass of MTOT = (4-8) × 1011 kg and a total kinetic energy of ETOT = (1-6) × 1015 J for the 2007 outburst ejecta, which are consistent with those of previous studies that were conducted soon after the outburst.

  20. LOCAL TADPOLE GALAXIES

    SciTech Connect

    Elmegreen, Debra Meloy; Putko, Joseph; Dewberry, Janosz; Elmegreen, Bruce G.; Sanchez Almeida, Jorge; Munoz-Tunon, Casiana

    2012-05-10

    Tadpole galaxies have a giant star-forming region at the end of an elongated intensity distribution. Here we use Sloan Digital Sky Survey data to determine the ages, masses, and surface densities of the heads and tails in 14 local tadpoles selected from the Kiso and Michigan surveys of UV-bright galaxies, and we compare them to tadpoles previously studied in the Hubble Ultra Deep Field. The young stellar mass in the head scales linearly with rest-frame galaxy luminosity, ranging from {approx}10{sup 5} M{sub Sun} at galaxy absolute magnitude U = -13 mag to 10{sup 9} M{sub Sun} at U = -20 mag. The corresponding head surface density increases from several M {sub Sun} pc{sup -2} locally to 10-100 M{sub Sun} pc{sup -2} at high redshift, and the star formation rate (SFR) per unit area in the head increases from {approx}0.01 M{sub Sun} yr{sup -1} kpc{sup -2} locally to {approx}1 M{sub Sun} yr{sup -1} kpc{sup -2} at high z. These local values are normal for star-forming regions, and the increases with redshift are consistent with other cosmological SFRs, most likely reflecting an increase in gas abundance. The tails in the local sample look like bulge-free galaxy disks. Their photometric ages decrease from several Gyr to several hundred Myr with increasing z, and their surface densities are more constant than the surface densities of the heads. The far-outer intensity profiles in the local sample are symmetric and exponential. We suggest that most local tadpoles are bulge-free galaxy disks with lopsided star formation, perhaps from environmental effects such as ram pressure or disk impacts, or from a Jeans length comparable to half the disk size.

  1. 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.

  2. VizieR Online Data Catalog: Spectroscopically Identified Hot Subdwarf Stars (Kilkenny+ 1988)

    NASA Astrophysics Data System (ADS)

    Kilkenny, D.; Heber, U.; Drilling, J. S.

    1996-05-01

    Prior to 1986 there were around 200 spectroscopically classified hot subdwarf stars. The Palomar-Green survey (Green et al., 1986ApJS...61..305G) detected over 900 hot subdwarfs, mostly in the North Galactic Cap and mostly previously unknown objects; the Kitt-Peak_Downes survey found another 60 near the Galactic Plane (Downes, 1986ApJS...61..569D). These form the basis of the present catalog but new subdwarfs are continually being found by spectroscopic surveys of photographically discovered faint blue star samples; examples are the work of Wegner and his co-workers on the Kiso survey (Wegner et al., 1985AJ.....90.1511W, 1986AJ.....91..139W, 1987AJ.....94.1271W) and of Kilkenny and Muller (1987) on southern discoveries by Luyten and collaborators (e.g. Haro and Luyten, 1962, Cat. III/74; Luyten and Anderson, 1958, 1959, 1967, "A Search for Faint Blue Stars"). Only stars for which a spectroscopic classification exists have been included. There is a significant probability that stars with only photometric classifications can be normal high-latitude B stars, white dwarfs or cataclysmic variable, for example. Hot subdwarfs in binary systems have been included but not planetary nebulae nuclei classified 'sd' since the latter have been catalogued elsewhere. Although there is not a universally accepted classification scheme for hot subdwarfs, it is fairly clear that the main criterion is a surface gravity higher than that of hot main sequence stars but less than that of hot white dwarfs. Also, hot subdwarf stars typically show helium abundance anomalies. (2 data files).

  3. 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

  4. 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

  5. X-Ray and Optical Correlation of Type I Seyfert NGC 3516 Studied with Suzaku and Japanese Ground-based Telescopes

    NASA Astrophysics Data System (ADS)

    Noda, Hirofumi; Minezaki, Takeo; Watanabe, Makoto; Kokubo, Mitsuru; Kawaguchi, Kenji; Itoh, Ryosuke; Morihana, Kumiko; Saito, Yoshihiko; Nakao, Hikaru; Imai, Masataka; Moritani, Yuki; Takaki, Katsutoshi; Kawabata, Miho; Nakaoka, Tatsuya; Uemura, Makoto; Kawabata, Koji; Yoshida, Michitoshi; Arai, Akira; Takagi, Yuhei; Morokuma, Tomoki; Doi, Mamoru; Itoh, Yoichi; Yamada, Shin’ya; Nakazawa, Kazuhiro; Fukazawa, Yasushi; Makishima, Kazuo

    2016-09-01

    From 2013 April to 2014 April, we performed X-ray and optical simultaneous monitoring of the type 1.5 Seyfert galaxy NGC 3516. We employed Suzaku and five Japanese ground-based telescopes—the Pirka, Kiso Schmidt, Nayuta, MITSuME, and the Kanata telescopes. The Suzaku observations were conducted seven times with various intervals ranging from days or weeks to months, with an exposure of ∼50 ks each. The optical B-band observations not only covered those of Suzaku almost simultaneously, but also followed the source as frequently as possible. As a result, NGC 3516 was found in its faint phase with a 2–10 keV flux of 0.21–2.70 × 10‑11 erg s‑1 cm‑2. The 2–45 keV X-ray spectra were composed of a dominant variable hard power-law (PL) continuum with a photon index of ∼1.7 and a non-relativistic reflection component with a prominent Fe–Kα emission line. Producing the B-band light curve by differential image photometry, we found that the B-band flux changed by ∼2.7 × 10‑11 erg s‑1 cm‑2, which is comparable to the X-ray variation, and we detected a significant flux correlation between the hard PL component in X-rays and the B-band radiation, for the first time in NGC 3516. By examining their correlation, we found that the X-ray flux preceded that in the B band by {2.0}-0.6+0.7 days (1σ error). Although this result supports the X-ray reprocessing model, the derived lag is too large to be explained by the standard view, which assumes a “lamppost”-type X-ray illuminator located near a standard accretion disk. Our results are better explained by assuming a hot accretion flow and a truncated disk.

  6. 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