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1. Status of the East Asia ALMA development program: Towards the implementation of the ALMA development roadmap

Author

Alvaro Gonzalez, Daisuke Iono, Hitoshi Kiuchi, G. Kosugi, Wenlei Shan, Takafumi Kojima, and Yoshinori Uzawa

Subjects
Telescope, Engineering, business.industry, law, Software development, East Asia, business, Telecommunications, law.invention
Abstract

The ALMA telescope has been producing ground-breaking science since 2011, but it is mostly based on technology from the 2000s. In order to keep ALMA competitive in the coming decade, timely updates are necessary in order to further improve the science output of the telescope in the coming decades. In this contribution, we will present the status of the different projects and studies which constitute the contribution of East Asia to the ALMA Development Program, such as the production of band 1 receivers, the development of band 2 receivers optics, and of the ACA spectrometer. We will also update on the different hardware and software studies towards the implementation of the ALMA Development Roadmap and additional opportunities.

Published
2020
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2. Development of flexible and useful archive system storing observation data of various telescopes

Author

Shigeru Takahashi, Kyoko Ashitagawa, G. Kosugi, Makoto Shizugami, Akira Yoshino, Koji Nakamura, Jun Maekawa, Takeshi Kamazaki, Kazufumi Torii, and Emi Ikeda

Subjects
Database, business.industry, Computer science, Access control, JavaScript, computer.software_genre, JSON, law.invention, Object storage, Metadata, Telescope, Observatory, law, Ticket, business, computer, computer.programming_language
Abstract

We present an archive system named "Adria", which have been developed and maintained by ALMA project team of National Astronomical Observatory of Japan (NAOJ). Adria aims to store and open to the public various science data. Adria is composed of an object storage to store the observation data, the access control by "ticket", JSON format metadata, JavaScript APIs and html documents. The combination has the advantages of flexibility and solidity, which are important to store various telescope data in the same platform and to be maintained with small cost for a long time. Firstly, we have applied Adria to the observation data (since July 2013) of Nobeyama Radio Observatory (NRO) 45m, and then we have added the data (since June 2019) of Atacama Submillimeter Telescope Experiment (ASTE) to the same platform.

Published
2020
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3. Observations of the [CI] ($^3P_1$-$^3P_0$) emission toward the massive star-forming region RCW38: further evidence for highly-clumped density distribution of the molecular gas

Author

Akira Yoshino, Yasuo Fukui, T. Kamazaki, Andrea Silva, Kengo Tachihara, Jun Maekawa, Hiroyuki Kaneko, Shinji Fujita, Takeshi Nakazato, Kanako Sugimoto, Shigeru Takahashi, Shin'ichiro Asayama, Daisuke Iono, Munetake Momose, Natsuko Izumi, G. Kosugi, and Kazufumi Torii

Subjects
Physics, Density distribution, 010308 nuclear & particles physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Star (graph theory), 010303 astronomy & astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies
Abstract

We present observations of the $^3P_1$-$^3P_0$ fine-structure line of atomic carbon using the ASTE 10 m sub-mm telescope towards RCW38, the youngest super star cluster in the Milky Way. The detected [CI] emission is compared with the CO $J$ = 1-0 image cube presented in Fukui et al. (2016) which has an angular resolution of 40$^{\prime \prime}$ ($\sim$ 0.33 pc). The overall distribution of the [CI] emission in this cluster is similar to that of the $^{13}$CO emission. The optical depth of the [CI] emission was found to be $\tau$ = 0.1-0.6, suggesting mostly optically thin emission. An empirical conversion factor from the [CI] integrated intensity to the H$_2$ column density was estimated as $X_{\rm [CI]}$ = 6.3 $\times$ 10$^{20}$ cm$^{-2}$ K$^{-1}$ km$^{-1}$ s (for visual extinction: $A_V$ $\le$ 10 mag) and 1.4 $\times$ 10$^{21}$ cm$^{-2}$ K$^{-1}$ km$^{-1}$ s (for $A_V$ of 10-100 mag). The column density ratio of the [CI] to CO ($N_{\rm [CI]}/N_{\rm CO}$) was derived as $\sim$ 0.1 for $A_V$ of 10-100 mag, which is consistent with that of the Orion cloud presented in Ikeda et al. (2002). However, our results cover an $A_V$ regime of up to 100 mag, which is wider than the coverage found in Orion, which reach up to $\sim$ 60 mag. Such a high [CI]/CO ratio in a high $A_V$ region is difficult to be explained by the plane-parallel photodissociation region (PDR) model, which predicts that this ratio is close to 0 due to the heavy shielding of the ultraviolet (UV) radiation. Our results suggest that the molecular gas in this cluster is highly clumpy, allowing deep penetration of UV radiation even at averaged $A_V$ values of 100 mag. Recent theoretical works have presented models consistent with such clumped gas distribution with a sub-pc clump size (e.g., Tachihara et al. 2018)., Comment: 33 pages, 21 figures, PASJ accepted for publication

Published
2020

4. The Kyoto Tridimensional Spectrograph II on Subaru and the University of Hawaii 88 in Telescopes

Author

Kazuya Matsubayashi, T. Ishigaki, G. Kosugi, T. Hayashi, Yoshiko Okita, Hiroshi Ohtani, Shinobu Ozaki, Hajime Sugai, Minoru Sasaki, Takashi Hattori, Norihide Takeyama, M. Ishii, Atsushi Shimono, and Atsushi Kawai

Subjects
Physics, business.industry, Optical instrument, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Field of view, Astrophysics::Cosmology and Extragalactic Astrophysics, law.invention, Lens (optics), Telescope, Optics, Integral field spectrograph, Space and Planetary Science, law, Chromatic aberration, Astrophysics::Earth and Planetary Astrophysics, Subaru Telescope, business, Spectrograph, Astrophysics::Galaxy Astrophysics
Abstract

In order to investigate physical conditions of ionized gas in galaxies, as well as its kinematics, we have developed the Kyoto tridimensional spectrograph II. It is a multimode optical instrument, including integral field spectrograph (IFS) and Fabry-Perot imager modes. We have designed it compact so that we can mount it on 2 m class telescopes as well as on the 8.2 m Subaru telescope. Special care was taken to obtain high-quality calibrations in the IFS mode. In order to remove the chromatic aberration of micropupil images produced by a lenslet array, we have introduced a corrector lens system behind the lenslet array. The internal calibration system simulates the telescope optics so that the system provides micropupil images identical to those produced by the telescope. The rigidness of the instrument provides the positional stability of micropupil images. We have succeeded in test observations of all the modes on Subaru and the University of Hawaii 88 in (UH88) telescopes and have verified the performance of the instrument. This includes the instrument efficiencies as well as the effective sky background subtraction and the minimization of crosstalk effects in the IFS mode. In the IFS mode a spatial resolution of 0.4'' was obtained in good seeing conditions. Each of 37 × 37 lenslets subtends 0.1'' in Subaru's case. This samples the image size well. A wider field of view is emphasized in the case of UH88.

Published
2010
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5. A logNHI = 22.6 Damped Lyα Absorber in a Dark Gamma-Ray Burst: The Environment of GRB 050401

Author

James Reeves, J. Gorosabel, P. M. Vreeswijk, B. L. Jensen, D. Bersier, K. Torstensson, A. J. Levan, P. Hirst, T. Shahbaz, Kentaro Aoki, Nial Tanvir, Josefa Masegosa, C. Ledoux, D. Diaz-Fraile, Anja C. Andersen, R. L. C. Starling, N. Kawai, Dan M. Watson, K. Wiersema, D. Sharapov, J. P. U. Fynbo, Jesper Sollerman, A. P. Beardmore, Jyri Näränen, K. L. Page, P. Laursen, Vasilij Rumyantsev, G. Kosugi, Alain Smette, Jens Hjorth, K. Pedersen, P. Jakobsson, T. Augusteijn, P. D'Avanzo, J. M. Castro Cerón, and A. Pozanenko

Subjects
Physics, Metallicity, ISM: Dust, Galaxies: Quasars: Absorption Lines, Astronomy and Astrophysics, Astrophysics, Extinction, Galaxies: High-Redshift, Spectral line, Afterglow, Gamma Rays: Bursts, Galaxies: ISM, Space and Planetary Science, Extinction (optical mineralogy), X-Rays: General, Spectral energy distribution, Sublimation (phase transition), Gamma-ray burst, Visible spectrum
Abstract

The optical afterglow spectrum of GRB 050401 (at z=2.8992+/-0.0004) shows the presence of a damped Lyα absorber (DLA), with logNHI=22.6+/-0.3. This is the highest column density ever observed in a DLA and is about 5 times larger than the strongest DLA detected so far in any QSO spectrum. From the optical spectrum, we also find a very large Zn column density, implying an abundance of [Zn/H]=-1.0+/-0.4. These large columns are supported by the early X-ray spectrum from Swift XRT, which shows a column density (in excess of Galactic) of logNH=22.21+0.06-0.08 assuming solar abundances (at z=2.9). The comparison of this X-ray column density, which is dominated by absorption due to α-chain elements, and the H I column density derived from the Lyα absorption line allows us to derive a metallicity for the absorbing matter of [α/H]=-0.4+/-0.3. The optical spectrum is reddened and can be well reproduced with a power law with SMC extinction, where AV=0.62+/-0.06. But the total optical extinction can also be constrained independent of the shape of the extinction curve: from the optical to X-ray spectral energy distribution, we find 0.5VV=9.1+1.4-1.5. This discrepancy might be explained by a small dust content with high metallicity (low dust-to-metals ratio). ``Gray'' extinction cannot explain the discrepancy, since we are comparing the metallicity to a measurement of the total extinction (without reference to the reddening). Little dust with high metallicity may be produced by sublimation of dust grains or may naturally exist in systems younger than a few hundred megayears. Based in part on observations made at the European Southern Observatory, Paranal, Chile under program 075.D-0270, with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, with the Wide Field Camera (WFCAM) on the United Kingdom Infrared Telescope, which is operated by the Joint Astronomy Centre on behalf of the UK Particle Physics and Astronomy Research Council, and on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.

Published
2006

6. The afterglow of GRB 050709 and the nature of the short-hard γ-ray bursts

Author

Alicia M. Soderberg, Kathy Roth, Andrew MacFadyen, D.-S. Moon, Ehud Nakar, Mark M. Phillips, Bruce A. Peterson, Michael Rauch, Miguel Roth, Patrick J. McCarthy, Darach Watson, Mansi M. Kasliwal, Tomonori Totani, Kazuhiro Aoki, Fiona A. Harrison, Brian L. Lee, Nobuyuki Kawai, P. A. Price, Roger A. Chevalier, Stephen Bradley Cenko, Avishay Gal-Yam, Dale A. Frail, Tsvi Piran, Edo Berger, G. Kosugi, Joshua Rich, Bryan E. Penprase, P. B. Cameron, H-S Park, Stephen A. Shectman, Kevin Hurley, Shrinivas R. Kulkarni, Pawan Kumar, D. B. Fox, Brian P. Schmidt, and L. L. Cowie

Subjects
Physics, Multidisciplinary, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, GRB 050709, Light curve, Magnetar, Galaxy, Afterglow, Supernova, Neutron star, Gamma-ray burst
Abstract

The final chapter in the long-standing mystery of the gamma-ray bursts (GRBs) centres on the origin of the short-hard class, suspected on theoretical grounds to result from the coalescence of neutron star or black hole binary systems. Numerous searches for the afterglows of short-hard bursts have been made, galvanized by the revolution in our understanding of long-duration GRBs that followed the discovery in 1997 of their broadband (X-ray, optical, and radio) afterglow emission. Here we present the discovery of the X-ray afterglow of a short-hard burst whose accurate position allows us to unambiguously associate it with a star-forming galaxy at redshift z=0.160, and whose optical lightcurve definitively excludes a supernova association. Together with results from three other recent short-hard bursts, this suggests that short-hard bursts release much less energy than the long-duration GRBs. Models requiring young stellar populations, such as magnetars and collapsars, are ruled out, while coalescing degenerate binaries remain the most promising progenitor candidates., Comment: Nature in press (Oct 6 issue). 23 pages, 4 figures

Published
2005
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7. The 2014 ALMA Long Baseline Campaign: An Overview

Author

ALMA Partnership, E. B. Fomalont, C. Vlahakis, S. Corder, A. Remijan, D. Barkats, R. Lucas, T. R. Hunter, C. L. Brogan, Y. Asaki, S. Matsushita, W. R. F. Dent, R. E. Hills, N. Phillips, A. M. S. Richards, P. Cox, R. Amestica, D. Broguiere, W. Cotton, A. S. Hales, R. Hiriart, A. Hirota, J. A. Hodge, C. M. V. Impellizzeri, J. Kern, R. Kneissl, E. Liuzzo, N. Marcelino, R. Marson, A. Mignano, K. Nakanishi, B. Nikolic, J. E. Perez, L. M. Pérez, I. Toledo, R. Aladro, B. Butler, J. Cortes, P. Cortes, V. Dhawan, J. Di Francesco, D. Espada, F. Galarza, D. Garcia-Appadoo, L. Guzman-Ramirez, E. M. Humphreys, T. Jung, S. Kameno, R. A. Laing, S. Leon, J. Mangum, G. Marconi, H. Nagai, L.-A. Nyman, M. Radiszcz, J. A. Rodón, T. Sawada, S. Takahashi, R. P. J. Tilanus, T. van Kempen, B. Vila Vilaro, L. C. Watson, T. Wiklind, F. Gueth, K. Tatematsu, A. Wootten, A. Castro-Carrizo, E. Chapillon, G. Dumas, I. de Gregorio-Monsalvo, H. Francke, J. Gallardo, J. Garcia, S. Gonzalez, J. E. Hibbard, T. Hill, T. Kaminski, A. Karim, M. Krips, Y. Kurono, C. Lopez, S. Martin, L. Maud, F. Morales, V. Pietu, K. Plarre, G. Schieven, L. Testi, L. Videla, E. Villard, N. Whyborn, M. A. Zwaan, F. Alves, P. Andreani, A. Avison, M. Barta, F. Bedosti, G. J. Bendo, F. Bertoldi, M. Bethermin, A. Biggs, J. Boissier, J. Brand, S. Burkutean, V. Casasola, J. Conway, L. Cortese, B. Dabrowski, T. A. Davis, M. Diaz Trigo, F. Fontani, R. Franco-Hernandez, G. Fuller, R. Galvan Madrid, A. Giannetti, A. Ginsburg, S. F. Graves, E. Hatziminaoglou, M. Hogerheijde, P. Jachym, I. Jimenez Serra, M. Karlicky, P. Klaasen, M. Kraus, D. Kunneriath, C. Lagos, S. Longmore, S. Leurini, M. Maercker, B. Magnelli, I. Marti Vidal, M. Massardi, A. Maury, S. Muehle, S. Muller, T. Muxlow, E. O’Gorman, R. Paladino, D. Petry, J. Pineda, S. Randall, J. S. Richer, A. Rossetti, A. Rushton, K. Rygl, A. Sanchez Monge, R. Schaaf, P. Schilke, T. Stanke, M. Schmalzl, F. Stoehr, S. Urban, E. van Kampen, W. Vlemmings, K. Wang, W. Wild, Y. Yang, S. Iguchi, T. Hasegawa, M. Saito, J. Inatani, N. Mizuno, S. Asayama, G. Kosugi, K.-I. Morita, K. Chiba, S. Kawashima, S. K. Okumura, N. Ohashi, R. Ogasawara, S. Sakamoto, T. Noguchi, Y.-D. Huang, S.-Y. Liu, F. Kemper, P. M. Koch, M.-T. Chen, Y. Chikada, M. Hiramatsu, D. Iono, M. Shimojo, S. Komugi, J. Kim, A.-R. Lyo, E. Muller, C. Herrera, R. E. Miura, J. Ueda, J. Chibueze, Y.-N. Su, A. Trejo-Cruz, K.-S. Wang, H. Kiuchi, N. Ukita, M. Sugimoto, R. Kawabe, M. Hayashi, S. Miyama, P. T. P. Ho, N. Kaifu, M. Ishiguro, A. J. Beasley, S. Bhatnagar, J. A. Braatz III, D. G. Brisbin, N. Brunetti, C. Carilli, J. H. Crossley, L. D’Addario, J. L. Donovan Meyer, D. T. Emerson, A. S. Evans, P. Fisher, K. Golap, D. M. Griffith, A. E. Hale, D. Halstead, E. J. Hardy, M. C. Hatz, M. Holdaway, R. Indebetouw, P. R. Jewell, A. A. Kepley, D.-C. Kim, M. D. Lacy, A. K. Leroy, H. S. Liszt, C. J. Lonsdale, B. Matthews, M. McKinnon, B. S. Mason, G. Moellenbrock, A. Moullet, S. T. Myers, J. Ott, A. B. Peck, J. Pisano, S. J. E. Radford, W. T. Randolph, U. Rao Venkata, M. G. Rawlings, R. Rosen, S. L. Schnee, K. S. Scott, N. K. Sharp, K. Sheth, R. S. Simon, T. Tsutsumi, S. J. Wood, National Radio Astronomy Observatory (NRAO), Joint ALMA Observatory (JAO), European Southern Observatory (ESO)-National Radio Astronomy Observatory (NRAO), Institute for Ethnomedicine, University of Wyoming (UW), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Chimie des métaux de transition et catalyse (CMTC), Centre National de la Recherche Scientifique (CNRS)-Université Louis Pasteur - Strasbourg I, Istituto di Radioastronomia [Bologna] (IRA), Istituto Nazionale di Astrofisica (INAF), Institut Jacques Monod (IJM (UMR_7592)), Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), ESO, European Southern Observatory (ESO), Department of Organic and Polymeric Materials, Tokyo Institute of Technology [Tokyo] (TITECH), Biogeochemistry Research Centre, School of Chemistry, Onsala Space Observatory, Chalmers University of Technology [Göteborg], Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), AMOR 2015, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Departamento de Analisis Matematico, Universidad de Málaga [Málaga] = University of Málaga [Málaga], Unité de recherche Zoologie Forestière (URZF), Institut National de la Recherche Agronomique (INRA), IFP Energies nouvelles (IFPEN), Fastopt GmbH, D-20357 Hamburg, Germany, Mathématiques Appliquées Paris 5 (MAP5 - UMR 8145), Université Paris Descartes - Paris 5 (UPD5)-Institut National des Sciences Mathématiques et de leurs Interactions (INSMI)-Centre National de la Recherche Scientifique (CNRS), Departament de Ecologia, Universitat d'Alacant, Centro de Estudios Ambientales del Mediterraneo, INAF - Osservatorio Astrofisico di Arcetri (OAA), Faculty of Medicine, Universidad de Chile = University of Chile [Santiago] (UCHILE), Université Pierre et Marie Curie - Paris 6 (UPMC), Unité de Recherche sur les Maladies Cardiovasculaires, du Métabolisme et de la Nutrition = Institute of cardiometabolism and nutrition (ICAN), Université Pierre et Marie Curie - Paris 6 (UPMC)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Institut National de la Santé et de la Recherche Médicale (INSERM)-CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Sorbonne Université (SU), Laboratoire de génie électrique de Paris (LGEP), Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Ecole Supérieure d'Electricité - SUPELEC (FRANCE)-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Max-Planck-Institut für Radioastronomie (MPIFR), Northern Illinois University (NORTHERN ILLINOIS UNIVERSITY), Northern Illinois University, Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], foreign laboratories (FL), CERN [Genève], Departements of Medicine and Microbiology, University of Alabama [Tuscaloosa] (UA), Swinburne University of Technology (Hawthorn campus), San Pedro de Atacama Celestial Explorations (SPACE), San Pedro de Atacama Celestial Explorations, General Electric Medical Systems [Buc] (GE Healthcare), General Electric Medical Systems, Laboratoire de Radiopathologie (LRP), Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de la Santé et de la Recherche Médicale (INSERM), Università degli Studi di Milano [Milano] (UNIMI), Altération génétique des cancers, chimioprévention et réponse thérapeutique, Physikalisches Institut [Köln], Universität zu Köln, Ministère de la santé, National Astronomical Observatory of Japan (NAOJ), National Institute for Materials Science (NIMS), Espaces acoustiques et cognitifs (EAC), Sciences et Technologies de la Musique et du Son (STMS), Institut de Recherche et Coordination Acoustique/Musique (IRCAM)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche et Coordination Acoustique/Musique (IRCAM)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Département de Mathématiques et Applications - ENS Paris (DMA), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Department of Chemistry and Biochemistry [Bern], University of Bern, Academia Sinica, Department of Marine Organic Biogeochemistry, Royal Netherlands Institute for Sea Research (NIOZ), Faculty of Geosciences, Utrecht University, Faculty of Geosciences, Brain Mind Institute (BMI - EPFL), Ecole Polytechnique Fédérale de Lausanne (EPFL), Departamento de Ingenieria Eléctrica (DIE), Universidad de Concepción [Chile], Laboratório de Bioinformática, Embrapa Recursos Genéticos e Biotecnologia, Graduate School of Engineering [The Univ of Tokyo] (UTokyo), The University of Tokyo (UTokyo), Kyushu University [Fukuoka], Mitsubishi Research Institute, Inc., Department of Computer Science and Automation [Bangalore] (CSA), Indian Institute of Science [Bangalore] (IISc Bangalore), National Radio Astronomy Observatory [Socorro] (NRAO), Occupational Physiology Laboratory (Vandœuvre-Les -Nancy, France), Computational Science and Engineering Department [Daresbury] (STFC), Science & Technologie Facilities Council, University College of London [London] (UCL), Centre for Atmospheric Chemistry [Wollongong] (CAC), University of Wollongong [Australia], Safety science group, Delft University of Technology (TU Delft), Centre d'Investigation Clinique - Innovation Technologique - INSERM - CHU de Grenoble (CIC-IT Grenoble (CIT803)), CHU Grenoble-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Grenoble Alpes (UGA), Northern Research Station, Forest Research [Great Britain], Department of Helsinki Institute for Information Technology Communications and Networking, Aalto University, University of Washington [Seattle], Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de la Santé et de la Recherche Médicale (INSERM), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Astronomy, Unité de Recherche sur les Maladies Cardiovasculaires, du Métabolisme et de la Nutrition = Research Unit on Cardiovascular and Metabolic Diseases (ICAN), Università degli Studi di Milano = University of Milan (UNIMI), Universität zu Köln = University of Cologne, Universidad de Concepción - University of Concepcion [Chile], Kyushu University, Istituto di Radioastronomia (IRA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Universidad de Málaga [Málaga], Unité de recherche Zoologie Forestière (UZF), Science et Technologie du Lait et de l'Oeuf (STLO), Institut National de la Recherche Agronomique (INRA)-AGROCAMPUS OUEST, Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Mathématiques et de leurs Interactions (INSMI)-Université Paris Descartes - Paris 5 (UPD5), University of Chile [Santiago], Université Pierre et Marie Curie - Paris 6 (UPMC)-Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-Institut National de la Santé et de la Recherche Médicale (INSERM)-CHU Pitié-Salpêtrière [APHP], Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-SUPELEC-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute of the Czech Academy of Sciences, Czech Academy of Sciences [Prague] (ASCR), Jodrell Bank Centre for Astrophysics, School of Physics, Università degli studi di Milano [Milano], National Institute of Materials Science, Equipe Espaces acoustiques et cognitifs, Université Pierre et Marie Curie - Paris 6 (UPMC)-IRCAM-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-IRCAM-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS), Department of Chemistry and Biochemistry, Graduate School of Engineering [Tokyo], The University of Tokyo, Center for Atmospheric Chemistry [Wollongong] (CAC), University of Wollongong, CHU Grenoble-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Joseph Fourier - Grenoble 1 (UJF), Forest Research, Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), École normale supérieure - Paris (ENS Paris), Université Grenoble Alpes (UGA)-Institut National de la Santé et de la Recherche Médicale (INSERM)-CHU Grenoble, Joint ALMA Office (JAO), ALMA, Institut Jacques Monod (IJM), Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Mathématiques et de leurs Interactions-Université Paris Descartes - Paris 5 (UPD5), ALMA Observatory, Laboratoire d'analyse et d'architecture des systèmes [Toulouse] (LAAS), Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UPS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Institut National Polytechnique [Toulouse] (INP), Center for Brain Simulation, Ecole Polytechnique Fédérale de Lausanne, Université Joseph Fourier - Grenoble 1 (UJF)-CHU Grenoble-Institut National de la Santé et de la Recherche Médicale (INSERM), National Radio Astronomy Observatory ( NRAO ), Joint ALMA Office ( JAO ), University of Wyoming ( UW ), Max-Planck-Institut für Astronomie ( MPIA ), Chimie des métaux de transition et catalyse ( CMTC ), Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique ( CNRS ), Istituto di Radioastronomia ( IRA ), Istituto Nazionale di Astrofisica ( INAF ), Institut Jacques Monod ( IJM ), Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), European Southern Observatory ( ESO ), Tokyo Institute of Technology [Tokyo] ( TITECH ), Institut de RadioAstronomie Millimétrique ( IRAM ), Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Unité de recherche Zoologie Forestière ( UZF ), Institut National de la Recherche Agronomique ( INRA ), IFP Energies nouvelles ( IFPEN ), Science et Technologie du Lait et de l'Oeuf ( STLO ), Institut National de la Recherche Agronomique ( INRA ) -AGROCAMPUS OUEST, Mathématiques Appliquées à Paris 5 ( MAP5 - UMR 8145 ), Université Paris Descartes - Paris 5 ( UPD5 ) -Institut National des Sciences Mathématiques et de leurs Interactions-Centre National de la Recherche Scientifique ( CNRS ), INAF - Osservatorio Astrofisico di Arcetri ( OAA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ), Unité de Recherche sur les Maladies Cardiovasculaires, du Métabolisme et de la Nutrition = Institute of cardiometabolism and nutrition ( ICAN ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Assistance publique - Hôpitaux de Paris (AP-HP)-Institut National de la Santé et de la Recherche Médicale ( INSERM ) -CHU Pitié-Salpêtrière [APHP], Laboratoire de génie électrique de Paris ( LGEP ), Université Paris-Sud - Paris 11 ( UP11 ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -SUPELEC-Centre National de la Recherche Scientifique ( CNRS ), Czech Academy of Sciences [Prague] ( ASCR ), Max-Planck-Institut für Radioastronomie ( MPIFR ), Northern Illinois University ( NORTHERN ILLINOIS UNIVERSITY ), Canadian Space Agency, foreign laboratories ( FL ), University of Alabama [Tuscaloosa] ( UA ), San Pedro de Atacama Celestial Explorations ( SPACE ), General Electric Medical Systems [Buc] ( GE Healthcare ), Laboratoire de Radiopathologie ( LRP ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ), Max Planck Institute for Biochemistry, Max-Planck-Institut, Department of Virology, Global COE Program, Nagasaki University-Institute of Tropical Medicine, Sciences et Technologies de la Musique et du Son ( STMS ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -IRCAM-Centre National de la Recherche Scientifique ( CNRS ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -IRCAM-Centre National de la Recherche Scientifique ( CNRS ), Département de Mathématiques et Applications - ENS Paris ( DMA ), École normale supérieure - Paris ( ENS Paris ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'analyse et d'architecture des systèmes [Toulouse] ( LAAS ), Centre National de la Recherche Scientifique ( CNRS ) -Université Toulouse III - Paul Sabatier ( UPS ), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse ( INSA Toulouse ), Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Institut National Polytechnique [Toulouse] ( INP ), Royal Netherlands Institute for Sea Research ( NIOZ ), Departamento de Ingenieria Eléctrica ( DIE ), AUTRES, Department of Computer Science and Automation [Bangalore] ( CSA ), Indian Institute of Science [Bangalore] ( IISc Bangalore ), National Radio Astronomy Observatory [Socorro] ( NRAO ), Computational Science and Engineering Department [Daresbury] ( STFC ), University College of London [London] ( UCL ), Center for Atmospheric Chemistry [Wollongong] ( CAC ), Delft University of Technology ( TU Delft ), Service Hématologie, Hôpital Morvan [Brest]-Centre Hospitalier Régional Universitaire de Brest ( CHRU Brest ), Centre d'Investigation Clinique - Innovation Technologique - INSERM - CHU de Grenoble ( CIC-IT Grenoble (CIT803) ), and Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Centre Hospitalier Universitaire de Grenoble

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], techniques: high angular resolution, Astronomy and Astrophysics, submillimeter: general, telescopes, Submillimeter Array, [ SDU.ASTR.CO ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, techniques: interferometric, Environmental science, Millimeter, Baseline (configuration management), instrumentation: interferometers, QB, Remote sensing
Abstract

著者人数: 248名, Accepted: 2015-04-10, 資料番号: SA1150145000

Published
2015
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8. Optical Spectropolarimetry of SN 2002[CLC]ap[/CLC]: A High-Velocity Asymmetric Explosion

Author

K. S. Kawabata, D. J. Jeffery, M. Iye, Y. Ohyama, G. Kosugi, N. Kashikawa, N. Ebizuka, T. Sasaki, K. Sekiguchi, K. Nomoto, P. Mazzali, J. Deng, K. Maeda, H. Umeda, K. Aoki, Y. Saito, T. Takata, M. Yoshida, R. Asai, M. Inata, K. Okita, K. Ota, T. Ozawa, Y. Shimizu, H. Taguchi, Y. Yadoumaru, T. Misawa, F. Nakata, T. Yamada, I. Tanaka, and T. Kodama

Subjects
Physics, Linear polarization, Axial ratio, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), Astronomy and Astrophysics, Astrophysics, Polarization (waves), Supernova, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Ejecta, Multiplet, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

We present spectropolarimetry of the Type Ic supernova SN 2002ap and give a preliminary analysis: the data were taken at two epochs, close to and one month later than the visual maximum (2002 February 8). In addition we present June 9 spectropolarimetry without analysis. The data show the development of linear polarization. Distinct polarization profiles were seen only in the O I \lambda 7773 multiplet/Ca II IR triplet absorption trough at maximum light and in the Ca II IR triplet absorption trough a month later, with the latter showing a peak polarization as high as ~2 %. The intrinsic polarization shows three clear position angles: 80 degs for the February continuum, 120 degs for the February line feature, and 150 degs for the March data. We conclude that there are multiple asymmetric components in the ejecta. We suggest that the supernova has a bulk asymmetry with an axial ratio projected on the sky that is different from 1 by of order 10 %. Furthermore, we suggest very speculatively that a high velocity ejecta component moving faster than ~0.115c (e.g., a jet) contributes to polarization in the February epoch.

Published
2002
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9. Subaru Deep Near-Infrared Imaging of the Field of a Possible Proto-Cluster Near the Radio Galaxy 53W002 at $z=2.4$

Author

Miwa Goto, Masanori Iye, Fumihide Iwamuro, Tadayuki Kodama, Ryuji Hata, Ichi Tanaka, Masaru Kajisawa, Toshinori Maihara, Kentaro Motohara, Tomoyuki Taguchi, G. Kosugi, Chris Simpson, Hiroshi Terada, Toshiyuki Sasaki, K. Sekiguchi, Tadafumi Takata, Toru Yamada, Tomonori Usuda, and Hirohisa Tanabe

Subjects
Luminous infrared galaxy, Physics, Radio galaxy, Hubble Deep Field, Astrophysics::High Energy Astrophysical Phenomena, Hubble Deep Field South, Astronomy, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Space and Planetary Science, Brightest cluster galaxy, Lenticular galaxy, Astrophysics::Galaxy Astrophysics
Abstract

We present the results of deep K � -a ndJ-band imaging of the field of a proto-cluster region near the radio galaxy 53W002 at z =2 .390 with the Subaru Telescope. The data were analyzed together with deep optical and nearinfrared (NIR) images taken with the Hubble Space Telescope to investigate the properties of ten optically compact emission-line galaxies and candidates. Excluding the three objects which may contain active galactic nuclei, many are faint or undetected at K � (λrest ≈6000 u A), and are therefore revealed to be intrinsically small starbursting objects. On the other hand, we detect few objects with colors and magnitudes expected for quiescent massive galaxies at z =2 . 4i n the f ield.

Published
2001
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10. Hyper-Fine Features of the Dust Distribution in the Central Region of the Seyfert Galaxy NGC 4151

Author

Masanori lye, S. Miyazaki, G. Kosugi, Hiroshi Ohtani, Yutaka Komiyama, Subaru Narrow-Band Team, Takashi Hattori, and Toshiyuki Sasaki

Subjects
Physics, Luminous infrared galaxy, Distribution (number theory), Astronomy, Type-cD galaxy, Astrophysics, Central region, Galaxy
Abstract

Fine features of the dust distribution in the central region of NGC 4151 have been studied from high resolution images obtained by the Subaru Telescope. The two dust lanes lying along a circum-nuclear ellipse of 40“ ×20” have been recognized to consist of a number of fine filaments and knots. In the inner region, there has been found dust distributed in a bipolar cone region extending to 5” from the nucleus. This cone is exactly complementary to the well-known bipolar ionized gaseous region. A dense knot is seen at 2” SE from the nucleus, but no torus-like feature is recognized. The masses of neutral gas in the outer lanes and in the inner region are estimated as 106M⊙ and 105M⊙ respectively. These observational results are compared with results of numerical simulations of gas dynamics.

Published
2001
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11. The First Light of the Subaru Telescope: A New Infrared Image of the Orion Nebula

Author

Naruhisa Takato, Takuya Yamashita, Ryuji Hata, Hirohisa Tanabe, Saeko S. Hayashi, Naoto Kobayashi, Hiroshi Terada, Tomio Kanzawa, Ian Shelton, Yoichi Itoh, Tetsuo Aoki, Takeo Fukuda, Mamoru Doi, Toshinori Maihara, Maki Sekiguchi, Tetsuo Hasegawa, Tetsuo Nishimura, Takashi Ichikawa, Yoshihiko Mizumoto, Tomonori Usuda, Hiroshi Karoji, Masanori Iye, Jun-ichi Watanabe, Yukiyasu Kobayashi, Masami Yutani, Eiji Nishihara, Tomoyuki Taguchi, G. Kosugi, Norio Kaifu, Keiichi Kodaira, Daigo Tomono, Katsumi Imi, Masaru Watanabe, Yasuo Torii, Shigeomi Yoshida, Hirokazu Kataza, Koji Omata, Toshiyuki Sasaki, Hideki Takami, Kyoji Nariai, Yoshihiro Chikada, Shiro Nishimura, Yasumasa Yamashita, Kazuhiro Sekiguchi, Yukiko Kamata, Yoshitaka Mikami, Hiroyasu Ando, Kyoko Tanaka, Masatoshi Imanishi, Tomio Kurakami, Tadafumi Takata, Akihiko Miyashita, Michitoshi Yoshida, Shuzo Isobe, Wataru Tanaka, Nobunari Kashikawa, Chris Simpson, Kentaro Motohara, Koich Nakajima, Kyoko Nakamura, Masashi Otsubo, Takeshi Noguchi, Fumihide Iwamuro, Kiichi Okita, Jun Nishikawa, Miwa Goto, Junichi Noumaru, Motoko Inata, Masafumi Yagi, Koichi Waseda, Norio Oshima, Ryusuke Ogasawara, Goro Sasaki, Hiroshi Suto, Norio Okada, Tetsuo Nishino, Yasushi Nakajima, Masayuki Akiyama, Satoshi Miyazaki, Naoki Yasuda, Jun'ich Iwai, Shin-Ichi Ichikawa, Noboru Ebizuka, Motohide Tamura, Toshihiro Horaguchi, Taichi Kato, Shoken M. Miyama, Takashi Miyata, Masahiko Hayashi, Masaru Hamabe, Kunio Noguchi, Shu-ichiro Inutsuka, and Masao Nakagiri

Subjects
Physics, Infrared image, Emission nebula, Space and Planetary Science, Orion Nebula, Astronomy, Astronomy and Astrophysics, Astrophysics, First light, Subaru Telescope
Published
2000
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12. An optical spectrum of the afterglow of a γ-ray burst at a redshift of z = 6.295

Author

T. Tamagawa, Kouji Ohta, N. Kawai, Ken'ichi Nomoto, Kentaro Aoki, Yoichi Yatsu, Tomonori Totani, Hiroshi Terada, Yuji Shirasaki, Yoshihiko Mizumoto, Masaya Suzuki, Hisanori Furusawa, Naoki Kobayashi, Ryusuke Ogasawara, Toru Yamada, Koji S. Kawabata, Kevin Hurley, Wako Aoki, R. Sato, Takashi Hattori, Yutaka Komiyama, Jun-ichi Watanabe, A. Yoshida, G. Kosugi, Junichi Noumaru, Tadafumi Takata, Kazuhiro Sekiguchi, and Masanori Iye

Subjects
Physics, Multidisciplinary, Star formation, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Billion years, Redshift, Afterglow, GRB 090423, Gamma-ray burst, Reionization, Stellar evolution
Abstract

The γ-ray burst GRB 050904, detected by the Swift satellite on 4 September last year, is one of the most distant objects ever observed. Its redshift of z = 6.3 equates to an explosion taking place 12.8 billion years ago, when the Universe was a mere 890 million years old. Three groups this week present detailed observations of the γ-ray, X-ray, near-infrared and optical spectra of the afterglow of GRB 050904. The results begin to paint a picture of the conditions prevailing when the parent body exploded and suggest that the γ-ray bursts that we see in the future can be used by cosmologists to probe the early Universe for evidence of star and galaxy formation, nucleosynthesis and reionization. The prompt γ-ray emission from γ-ray bursts (GRBs) should be detectable out to distances of z > 10 (ref. 1), and should therefore provide an excellent probe of the evolution of cosmic star formation, reionization of the intergalactic medium, and the metal enrichment history of the Universe1,2,3,4. Hitherto, the highest measured redshift for a GRB has been z = 4.50 (ref. 5). Here we report the optical spectrum of the afterglow of GRB 050904 obtained 3.4 days after the burst; the spectrum shows a clear continuum at the long-wavelength end of the spectrum with a sharp cut-off at around 9,000 A due to Lyman α absorption at z ≈ 6.3 (with a damping wing). A system of absorption lines of heavy elements at z = 6.295 ± 0.002 was also detected, yielding the precise measurement of the redshift. The Si ii fine-structure lines suggest a dense, metal-enriched environment around the progenitor of the GRB.

Published
2006

13. Distribution of extended-spectrum cephalosporin resistance determinants in Salmonella enterica and Escherichia coli isolated from broilers in southern Japan

Author

Taketoshi Iwata, G. Kosugi, Takehisa Chuma, Francis Shahada, Masahiro Kusumoto, and Masato Akiba

Subjects
Serotype, Antiinfective agent, biology, Cephalosporin Resistance, Salmonella enterica, General Medicine, Gene Expression Regulation, Bacterial, biology.organism_classification, medicine.disease_cause, Microbiology, Plasmid, Restriction map, Japan, medicine, Escherichia coli, Multilocus sequence typing, Animals, Animal Science and Zoology, Chickens, Escherichia coli Infections, Phylogeny, Poultry Diseases
Abstract

This study was conducted to investigate the distribution and diversity of extended-spectrum cephalosporin (ESC) resistance determinants in Salmonella enterica and Escherichia coli obtained from the same cecal samples and to provide evidence of transmission of the resistance determinants among these bacteria in broiler farms in southern Japan. Salmonella enterica and E. coli were characterized by serotyping and multilocus sequence typing, respectively. An antimicrobial susceptibility test, plasmid analysis, and identification and localization of resistance genes were performed to determine the relatedness of ESC resistance determinants among the isolates. Of 48 flocks examined, 14 had S. enterica. In total, 57 S. enterica isolates were obtained, 45 of which showed ESC resistance. Extended-spectrum cephalosporin-resistant E. coli were also obtained from all of these ESC-resistant Salmonella-positive samples. β-Lactamase genes, blaTEM-52 (38 isolates), blaCTX-M-14 (1 isolate), and blaCMY-2 (6 isolates), were carried by conjugative untypable or IncP plasmids detected in the S. enterica serovars Infantis and Manhattan. The β-lactamase genes blaCTX-M-14 (3 isolates), blaCTX-M-15 (3 isolates), blaSHV-2 (1 isolate), blaSHV-12 (2 isolates), and blaCMY-2 (32 isolates) associated with IncI1-Iγ, IncFIB, IncFIC, IncK, IncB/O, and IncY plasmids were detected in E. coli co-isolates. Restriction mapping revealed similar plasmids in Salmonella Infantis and Salmonella Manhattan and in different sequence types of E. coli. Intraspecies transmission of plasmids was suggested within S. enterica and E. coli populations, whereas interspecies transmission was not observed. This study highlights the importance of plasmids as carriers of ESC resistance determinants.

Published
2013

14. Implications for Galaxy Evolution from the Cosmic Evolution of Supernova Rate Density

Author

Naoki Yasuda, Takeshi Oda, Tomonori Totani, G. Kosugi, Tomoki Morokuma, Takahiro Sumi, and Masao Doi

Subjects
Physics, Star formation, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Redshift, Luminosity, Supernova, Space and Planetary Science, Galaxy formation and evolution, Intergalactic travel, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Dwarf galaxy
Abstract

We report a comprehensive statistical analysis of the observational data of the cosmic evolution of supernova (SN) rate density, to derive constraints on cosmic star formation history and the nature of type Ia supernova (SN Ia) progenitor. We use all available information of magnitude, SN type, and redshift information of both type Ia and core-collapse (CC) SNe in GOODS and SDF, as well as SN Ia rate densities reported in the literature. Furthermore, we also add 157 SN candidates in the past Subaru/Suprime-Cam data that are newly reported here, to increase the statistics. We find that the current data set of SN rate density evolution already gives a meaningful constraint on the evolution of the cosmic star formation rate (SFR) at z, Comment: 15 pages, 8 figures, accepted to PASJ

Published
2008
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15. On the Spectrum and Spectropolarimetry of Type Ic Hypernova SN 2003dh/GRB 030329

Author

Y. Urata, J. Deng, Nozomu Tominaga, Tadafumi Takata, Naoto Kobayashi, T. Sakamoto, Tomonori Totani, H. Umeda, John C Wheeler, Toru Yamada, Yoshihiko Mizumoto, G. Kosugi, David J. Jeffery, Ken'ichi Nomoto, Kentaro Aoki, Youichi Ohyama, Atsumasa Yoshida, Ken'ichi Torii, Wako Aoki, Koji S. Kawabata, Keiichi Maeda, Paolo A. Mazzali, Jun-ichi Watanabe, Y. Shirasaki, Toshiyuki Sasaki, Yutaka Komiyama, Nobuyuki Kawai, K. Sekiguchi, Nobunari Kashikawa, Ryusuke Ogasawara, Junichi Noumaru, Peter Hoeflich, Masanori Iye, Lifan Wang, and T. Tamagawa

Subjects
Physics, GRB 980425, Stars: Supernovae: Individual: Alphanumeric: SN 2003dh, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Galaxy, Spectral line, Afterglow, Interstellar medium, Gamma Rays: Bursts, Stars: Supernovae: General, Space and Planetary Science, Polarization, GRB 030329, Nuclear Reactions, Abundances, Hypernova, Gamma-ray burst, Nucleosynthesis
Abstract

Spectroscopic and spectropolarimetric observations of SN 2003dh/GRB 030329 obtained in 2003 May using the Subaru 8.2 m telescope are presented. The properties of the SN are investigated through a comparison with spectra of the Type Ic hypernovae SNe 1997ef and 1998bw. (Hypernovae being a tentatively defined class of SNe with very broad absorption features: these features suggest a large velocity of the ejected material and possibly a large explosion kinetic energy.) Comparison with spectra of other hypernovae shows that the spectrum of SN 2003dh obtained on 2003 May 8 and 9, i.e., 34-35 rest-frame days after the GRB (for z=0.1685), are similar to those of SN 1997ef obtained ~34-42 days after the fiducial time of explosion of that SN. The match with SN 1998bw spectra is not as good (at rest 7300-8000 A, but again spectra obtained ~33-43 days after GRB 980425 are preferred. This indicates that the SN may have intermediate properties between SNe 1997ef and 1998bw. Based on the analogy with the other hypernovae, the time of explosion of SN 2003dh is then constrained to be between -8 and +2 days of the GRB. The Si and O P-Cygni lines of SN 2003dh seem comparable to those of SN 1997ef, which suggests that the ejected mass in SN 2003dh may match that in SN 1997ef. Polarization was marginally detected at optical wavelengths. This is consistent with measurements of the late afterglow, implying that it mostly originated in the interstellar medium of the host galaxy., Comment: 7 pages, 4 figures, uses emulateapj5.sty, accepted for puclication in ApJL

Published
2003

16. Observation scheduling and data acquisition with the Subaru control system

Author

Jun Kawai, G. Kosugi, Akihiko Kidou, Tsutomu Aoki, Junichi Noumaru, and Toshiyuki Sasaki

Subjects
Workstation, Computer science, business.industry, Local area network, computer.software_genre, law.invention, Scheduling (computing), Control flow, Software, Data acquisition, law, Control system, Embedded system, Operating system, business, Subaru Telescope, computer
Abstract

The control system for the Subaru telescope is designed to consist of distributed workstations, local processors, and data acquisition computers, which are interconnected by control LANs and data LANs. The control software achieves its functionality with message-based communication. Two key processes, a scheduler and a status logger cooperating with any other processes, are designed to perform efficiency and security in observation. Control flow of observation scheduling and functionality of sub-processes which constitutes the scheduler and the status logger are described. For data acquisition from instruments, Subaru control system provides a variety of data highway which enable instruments to transfer data by up to 20 Mbytes/second. Functionality and characteristics of other subsystems which compose the Subaru control system are described.

Published
1995
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17. 3.13. Outflow in the Seyfert galaxy NGC 7319

Author

M. Yoshida, A. S. Wilson, K. Aoki, H. Ohtani, and G. Kosugi

Subjects
Physics, symbols.namesake, symbols, Type-cD galaxy, Outflow, Astrophysics, Interacting galaxy, Galaxy, Dwarf galaxy, Hubble sequence
Abstract

Aoki et al. (1996) found outflowing gas in the Seyfert galaxy NGC 7319. The velocity of the outflow comes up to 500 km s−1 and its extent is 4 kpc. This outflow is one of the largest outflowing phenomenon that have ever been found in Seyfert galaxies. The radio emission found by van der Hulst & Rots (1981) aligns the outflowing gas. It suggests the radio emission has relation to the outflow. We have made higher resolution radio imaging of NGC 7319 with VLA to study in detail relation of radio emission to outflowing gas. These radio images have been compared to Hubble Space Telescope (HST) archival broad-band WFPC2 image. The systemic velocity 6740 km s−1 (Aoki et al. 1996) gives a distance of 90 Mpc for NGC 7319 assuming a Hubble constant H0=75 km s−1 Mpc−1. Thus 1″ corresponds to 450 pc.

Published
1998
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18. Implications for the cosmic re-ionization from the optical afterglow spectrum of GRB050904 at z = 6.3

Author

Tomonori Totani, Masanori Iye, G. Kosugi, Kouji Ohta, Toru Yamada, Kentaro Aoki, Nobuyuki Kawai, and Takashi Hattori

Subjects
Physics, COSMIC cancer database, Space and Planetary Science, Ionization, Cosmic microwave background, Spectrum (functional analysis), Astronomy, Astronomy and Astrophysics, Non-standard cosmology, Astrophysics, Afterglow
Abstract

We discuss the implications for the cosmic re-ionization from the optical afterglow spectrum of GRB050904 at z = 6.3

Published
2006
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19. Tri-dimensional Spectroscopy of the Seyfert Galaxy NGC 1275: Kinematics and Excitation of the Cooling-Flow Gas

Author

M. Yoshida, G. Kosugi, and K. Aoki

Subjects
Luminous infrared galaxy, Physics, Astronomy, Kinematics, Cooling flow, Spectroscopy, Excitation, Galaxy
Abstract

NGC 1275, the Perseus cluster cD galaxy, is a well-known Seyfert 1 galaxy and also one of the strongest extragalactic radio sources (3C84). Although many studies have been done on the extended optical emission-line region of NGC 1275, which is thought to be associated with the X-ray cooling-flow phenomenon (e.g., Heckman et al. 1989, Ferruit and Pecontal 1994), the excitation mechanism of the emission-line gas and two-dimensional gas kinematics are still unclear. We made tri-dimensional spectroscopy of NGC 1275 in order to reveal two-dimensional kinematics and- the relation between the gas motion and the excitation of the emission lines.

Published
1997
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20. Tridimensional Observations of Nearby Active Galaxies Using OAO Spectronebulagraph

Author

Hiroshi Ohtani, Minoru Sasaki, Y. Shimizu, H. Koyano, G. Kosugi, T. Sasaki, Kentaro Aoki, and M. Yoshida

Subjects
Physics, Active galactic nucleus, Astrophysics
Abstract

We developed a slit-scanning type 3D-spectroscopic system named as Spectronebulagraph (hereafter SNG; Kosugi et al. 1994) at Okayama Astrophysical Observatory. A detailed description about SNG is presented by Ohtani et al. elsewhere in this colloquium. We present here the results of the 3D-spectroscopy of four nearby active galaxies by using SNG.This nearby (at distance of 5.4 Mpc) Magellanic irregular galaxy has many H II regions in its main body suggesting violent star-formation activity. We performed tridimensional observations of NGC 4449 using SNG in order to obtain detailed kinematic structure and then to investigate the star-formation mechanism of NGC 4449. Hα intensity map, Hα velocity field are shown in figure 1. As is obvious in lower panel of figure 1, no global rotational motion was detected. Most impressive feature of the velocity field is kpc-scale mosaic structure of low velocity and high velocity components. Also, many filamentary components were newly found in 3D-datacube of the SNG observation.

Published
1995
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21. Tridimensional spectroscopy of Seyfert Galaxy 3C 120

Author

Kentaro Aoki, M. Yoshida, G. Kosugi, and H. Ohtani

Subjects
Data cube, Luminous infrared galaxy, Physics, Diagram, Astronomy, Type-cD galaxy, Spectroscopy, Intensity ratio, Galaxy, Line (formation)
Abstract

Tridimensional spectroscopy of the Seyfert 1 galaxy 3C 120 was carried out with Spectronebulagraph (SNG). We constructed a data cube which is free from atmospheric variations during the scans. We then separated the blended lines by deconvolving the line profiles, to obtain pure narrow-line images and narrow-line intensity ratio diagram.

Published
1995
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22. Distribution of extended-spectrum cephalosporin resistance determinants in Salmonella enterica and Escherichia coli isolated from broilers in southern Japan.

Author

Shahada F, Chuma T, Kosugi G, Kusumoto M, Iwata T, and Akiba M

Subjects
Animals, Escherichia coli genetics, Escherichia coli Infections epidemiology, Gene Expression Regulation, Bacterial, Japan epidemiology, Phylogeny, Poultry Diseases epidemiology, Salmonella enterica genetics, Cephalosporin Resistance genetics, Chickens, Escherichia coli drug effects, Escherichia coli Infections microbiology, Poultry Diseases microbiology, Salmonella enterica drug effects
Abstract

This study was conducted to investigate the distribution and diversity of extended-spectrum cephalosporin (ESC) resistance determinants in Salmonella enterica and Escherichia coli obtained from the same cecal samples and to provide evidence of transmission of the resistance determinants among these bacteria in broiler farms in southern Japan. Salmonella enterica and E. coli were characterized by serotyping and multilocus sequence typing, respectively. An antimicrobial susceptibility test, plasmid analysis, and identification and localization of resistance genes were performed to determine the relatedness of ESC resistance determinants among the isolates. Of 48 flocks examined, 14 had S. enterica. In total, 57 S. enterica isolates were obtained, 45 of which showed ESC resistance. Extended-spectrum cephalosporin-resistant E. coli were also obtained from all of these ESC-resistant Salmonella-positive samples. β-Lactamase genes, blaTEM-52 (38 isolates), blaCTX-M-14 (1 isolate), and blaCMY-2 (6 isolates), were carried by conjugative untypable or IncP plasmids detected in the S. enterica serovars Infantis and Manhattan. The β-lactamase genes blaCTX-M-14 (3 isolates), blaCTX-M-15 (3 isolates), blaSHV-2 (1 isolate), blaSHV-12 (2 isolates), and blaCMY-2 (32 isolates) associated with IncI1-Iγ, IncFIB, IncFIC, IncK, IncB/O, and IncY plasmids were detected in E. coli co-isolates. Restriction mapping revealed similar plasmids in Salmonella Infantis and Salmonella Manhattan and in different sequence types of E. coli. Intraspecies transmission of plasmids was suggested within S. enterica and E. coli populations, whereas interspecies transmission was not observed. This study highlights the importance of plasmids as carriers of ESC resistance determinants.

Published
2013
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23. Asphericity in supernova explosions from late-time spectroscopy.

Author

Maeda K, Kawabata K, Mazzali PA, Tanaka M, Valenti S, Nomoto K, Hattori T, Deng J, Pian E, Taubenberger S, Iye M, Matheson T, Filippenko AV, Aoki K, Kosugi G, Ohyama Y, Sasaki T, and Takata T

Abstract

Core-collapse supernovae (CC-SNe) are the explosions that announce the death of massive stars. Some CC-SNe are linked to long-duration gamma-ray bursts (GRBs) and are highly aspherical. One important question is to what extent asphericity is common to all CC-SNe. Here we present late-time spectra for a number of CC-SNe from stripped-envelope stars and use them to explore any asphericity generated in the inner part of the exploding star, near the site of collapse. A range of oxygen emission-line profiles is observed, including a high incidence of double-peaked profiles, a distinct signature of an aspherical explosion. Our results suggest that all CC-SNe from stripped-envelope stars are aspherical explosions and that SNe accompanied by GRBs exhibit the highest degree of asphericity.

Published
2008
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24. An optical spectrum of the afterglow of a gamma-ray burst at a redshift of z = 6.295.

Author

Kawai N, Kosugi G, Aoki K, Yamada T, Totani T, Ohta K, Iye M, Hattori T, Aoki W, Furusawa H, Hurley K, Kawabata KS, Kobayashi N, Komiyama Y, Mizumoto Y, Nomoto K, Noumaru J, Ogasawara R, Sato R, Sekiguchi K, Shirasaki Y, Suzuki M, Takata T, Tamagawa T, Terada H, Watanabe J, Yatsu Y, and Yoshida A

Abstract

The prompt gamma-ray emission from gamma-ray bursts (GRBs) should be detectable out to distances of z > 10 (ref. 1), and should therefore provide an excellent probe of the evolution of cosmic star formation, reionization of the intergalactic medium, and the metal enrichment history of the Universe. Hitherto, the highest measured redshift for a GRB has been z = 4.50 (ref. 5). Here we report the optical spectrum of the afterglow of GRB 050904 obtained 3.4 days after the burst; the spectrum shows a clear continuum at the long-wavelength end of the spectrum with a sharp cut-off at around 9,000 A due to Lyman alpha absorption at z approximately 6.3 (with a damping wing). A system of absorption lines of heavy elements at z = 6.295 +/- 0.002 was also detected, yielding the precise measurement of the redshift. The Si ii fine-structure lines suggest a dense, metal-enriched environment around the progenitor of the GRB.

Published
2006
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