Annual Report of the National Astronomical Observatory of Japan Fiscal 2009
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Whole Earth Telescope Observations of AM Canum Venaticorum – Discoseismology at Last
Astron. Astrophys. 332, 939–957 (1998) ASTRONOMY AND ASTROPHYSICS Whole Earth Telescope observations of AM Canum Venaticorum – discoseismology at last J.-E. Solheim1;14, J.L. Provencal2;15, P.A. Bradley2;16, G. Vauclair3, M.A. Barstow4, S.O. Kepler5, G. Fontaine6, A.D. Grauer7, D.E. Winget2, T.M.K. Marar8, E.M. Leibowitz9, P.-I. Emanuelsen1, M. Chevreton10, N. Dolez3, A. Kanaan5, P. Bergeron6, C.F. Claver2;17, J.C. Clemens2;18, S.J. Kleinman2, B.P. Hine12, S. Seetha8, B.N. Ashoka8, T. Mazeh9, A.E. Sansom4;19, R.W. Tweedy4, E.G. Meistasˇ 11;13, A. Bruvold1, and C.M. Massacand1 1 Nordlysobservatoriet, Institutt for Fysikk, Universitetet i Tromsø, N-9037 Tromsø, Norway 2 McDonald Observatory and Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, USA 3 Observatoire Midi–Pyrenees, 14 Avenue E. Belin, F-31400 Toulouse, France 4 Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH, UK 5 Instituto de Fisica, Universidade Federal do Rio Grande do Sul, 91500-970 Porto Alegre - RS, Brazil 6 Department de Physique, Universite´ de Montreal,´ C.P. 6128, Succ A., Montreal,´ PQ H3C 3J7, Canada 7 Department of Physics and Astronomy, University of Arkansas, 2801 S. University Ave, Little Rock, AR 72204, USA 8 Technical Physics Division, ISRO Satelite Centre, Airport Rd, Bangalore, 560 017 India 9 University of Tel Aviv, Department of Physics and Astronomy, Ramat Aviv, Tel Aviv 69978, Israel 10 Observatoire de Paris-Meudon, F-92195 Meudon Principal Cedex, France 11 Institute of Material Research and Applied Sciences, Vilnius University, Ciurlionio 29, Vilnius 2009, Lithuania 12 NASA Ames Research Center, M.S. -
Hubbl E Space T El Escope Wfpc2 Imaging of Fs Tauri and Haro 6-5B1 John E.Krist,2 Karl R.Stapelfeldt,3 Christopher J.Burrows,2,4 Gilda E.Ballester,5 John T
THE ASTROPHYSICAL JOURNAL, 501:841È852, 1998 July 10 ( 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A. HUBBL E SPACE T EL ESCOPE WFPC2 IMAGING OF FS TAURI AND HARO 6-5B1 JOHN E.KRIST,2 KARL R.STAPELFELDT,3 CHRISTOPHER J.BURROWS,2,4 GILDA E.BALLESTER,5 JOHN T. CLARKE,5 DAVID CRISP,3 ROBIN W.EVANS,3 JOHN S.GALLAGHER III,6 RICHARD E.GRIFFITHS,7 J. JEFF HESTER,8 JOHN G.HOESSEL,6 JON A.HOLTZMAN,9 JEREMY R.MOULD,10 PAUL A. SCOWEN,8 JOHN T.TRAUGER,3 ALAN M. WATSON,11 AND JAMES A. WESTPHAL12 Received 1997 December 18; accepted 1998 February 16 ABSTRACT We have observed the Ðeld of FS Tauri (Haro 6-5) with the Wide Field Planetary Camera 2 on the Hubble Space Telescope. Centered on Haro 6-5B and adjacent to the nebulous binary system of FS Tauri A there is an extended complex of reÑection nebulosity that includes a di†use, hourglass-shaped structure. H6-5B, the source of a bipolar jet, is not directly visible but appears to illuminate a compact, bipolar nebula which we assume to be a protostellar disk similar to HH 30. The bipolar jet appears twisted, which explains the unusually broad width measured in ground-based images. We present the Ðrst resolved photometry of the FS Tau A components at visual wavelengths. The Ñuxes of the fainter, eastern component are well matched by a 3360 K blackbody with an extinction ofAV \ 8. For the western star, however, any reasonable, reddened blackbody energy distribution underestimates the K-band photometry by over 2 mag. -
1000 Cataclysmic Variables from the Catalina Real-Time Transient Survey
MNRAS 443, 3174–3207 (2014) doi:10.1093/mnras/stu1377 1000 cataclysmic variables from the Catalina Real-time Transient Survey E. Breedt,1‹ B. T. Gansicke,¨ 1 A. J. Drake,2 P. Rodr´ıguez-Gil,3,4 S. G. Parsons,5 T. R. Marsh,1 P. Szkody,6 M. R. Schreiber5 and S. G. Djorgovski2 1Department of Physics, University of Warwick, Coventry, CV4 7AL, UK 2California Institute of Technology, 1200 E. California Blvd, CA 91225, USA 3Instituto de Astrof´ısica de Canarias, V´ıa Lactea´ s/n, La Laguna, E-38205, Santa Cruz de Tenerife, Spain 4Departamento de Astrof´ısica, Universidad de La Laguna, La Laguna, E-38206, Santa Cruz de Tenerife, Spain 5Instituto de F´ısica y Astronom´ıa, Universidad de Valpara´ıso, Avenida Gran Bretana 1111, 2360102 Valpara´ıso, Chile 6Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580, USA Downloaded from Accepted 2014 July 6. Received 2014 July 5; in original form 2014 May 13 ABSTRACT Over six years of operation, the Catalina Real-time Transient Survey (CRTS) has identified http://mnras.oxfordjournals.org/ 1043 cataclysmic variable (CV) candidates – the largest sample of CVs from a single survey to date. Here, we provide spectroscopic identification of 85 systems fainter than g ≥ 19, including three AM Canum Venaticorum binaries, one helium-enriched CV, one polar and one new eclipsing CV. We analyse the outburst properties of the full sample and show that it contains a large fraction of low-accretion-rate CVs with long outburst recurrence times. We argue that most of the high-accretion-rate dwarf novae in the survey footprint have already been found and that future CRTS discoveries will be mostly low-accretion-rate systems. -
The Interstellar and Circumnuclear Medium of Active Nuclei Traced by H I 21 Cm Absorption
The Astronomy and Astrophysics Review (2018) 26:4 https://doi.org/10.1007/s00159-018-0109-x REVIEW ARTICLE The interstellar and circumnuclear medium of active nuclei traced by H i 21 cm absorption Raffaella Morganti1,2 · Tom Oosterloo1,2 Received: 23 April 2018 © The Author(s) 2018 Abstract This review summarises what we have learnt in the last two decades based on H i 21 cm absorption observations about the cold interstellar medium (ISM) in the central regions of active galaxies and about the interplay between this gas and the active nucleus (AGN). Hi absorption is a powerful tracer on all scales, from the parsec-scales close to the central black hole to structures of many tens of kpc tracing interactions and mergers of galaxies. Given the strong radio continuum emission often associated with the central activity, H i absorption observations can be used to study the Hi near an active nucleus out to much higher redshifts than is possible using H i emission. In this way, Hi absorption has been used to characterise in detail the general ISM in active galaxies, to trace the fuelling of radio-loud AGN, to study the feedback occurring between the energy released by the active nucleus and the ISM, and the impact of such interactions on the evolution of galaxies and of their AGN. In the last two decades, significant progress has been made in all these areas. It is now well established that many radio loud AGN are surrounded by small, regularly rotating gas disks that contain a significant fraction of H i. -
The Birth of Stars and Planets
Unit 6: The Birth of Stars and Planets This material was developed by the Friends of the Dominion Astrophysical Observatory with the assistance of a Natural Science and Engineering Research Council PromoScience grant and the NRC. It is a part of a larger project to present grade-appropriate material that matches 2020 curriculum requirements to help students understand planets, with a focus on exoplanets. This material is aimed at BC Grade 6 students. French versions are available. Instructions for teachers ● For questions and to give feedback contact: Calvin Schmidt [email protected], ● All units build towards the Big Idea in the curriculum showing our solar system in the context of the Milky Way and the Universe, and provide background for understanding exoplanets. ● Look for Ideas for extending this section, Resources, and Review and discussion questions at the end of each topic in this Unit. These should give more background on each subject and spark further classroom ideas. We would be happy to help you expand on each topic and develop your own ideas for your students. Contact us at the [email protected]. Instructions for students ● If there are parts of this unit that you find confusing, please contact us at [email protected] for help. ● We recommend you do a few sections at a time. We have provided links to learn more about each topic. ● You don’t have to do the sections in order, but we recommend that. Do sections you find interesting first and come back and do more at another time. ● It is helpful to try the activities rather than just read them. -
Presentation71.Pdf
The KiboCUBE Programme December 14, 2017 United Nations / South Africa Symposium on Basic Space Technology “Small satellite missions for scientific and technological advancement” Masanobu TSUJI Japan Aerospace Exploration Agency (JAXA) 1 Credit : JAXA/NASA ISS: Japan’s Capabilities and Contributions ISS Kibo (International Space Station) (Japanese Experiment Module) HTV (H-II Transfer Vehicle) ▪ ISS is a huge manned construction located about 400km above the Earth. ▪ 15 countries participate in the ISS program ▪ Japan strives to make concrete international contributions through extensive utilization of Kibo and HTV. H-IIB Credit : JAXA/NASA 2 ISS: Japan’s Capabilities and Contributions Kibo: Japanese Experiment Module Kibo has a unique Exposed Facility (EF) with an Airlock (AL) and a Remote Manipulator System (JEMRMS), and has a high capacity to exchange experimental equipment. Robotic Arm (JEM-Remote Manipulator System) Airlock Credit : JAXA/NASA 3 “Kibo” is Unique! – Exposed Facility Small Satellite Deployment platform using J-SSOD AtIn present,recent years, satellite a growing deployers numberother ofthan universities J-SSOD andthat companiesuse Kibo include around the world have beenthe NanoRacks developing CubeSat the DeployerMicro/Nano (NRCSD)-satellite and (under 100kg, mainlyCyclops CubeSat). (Space Station Integrated Kinetic Launcher for Orbital Payload Systems). Credit : JAXA/NASA J-SSOD#2 NRCSD#1 Cyclops#1 J-SSOD Microsat#1 J-SSOD#1 J-SSOD Upgrade#1 4 Ref: Prof. 2017 Nano/Microsatellite Market Forecast (SpaceWorks Enterprises -
Highlights in Space 2010
International Astronautical Federation Committee on Space Research International Institute of Space Law 94 bis, Avenue de Suffren c/o CNES 94 bis, Avenue de Suffren UNITED NATIONS 75015 Paris, France 2 place Maurice Quentin 75015 Paris, France Tel: +33 1 45 67 42 60 Fax: +33 1 42 73 21 20 Tel. + 33 1 44 76 75 10 E-mail: : [email protected] E-mail: [email protected] Fax. + 33 1 44 76 74 37 URL: www.iislweb.com OFFICE FOR OUTER SPACE AFFAIRS URL: www.iafastro.com E-mail: [email protected] URL : http://cosparhq.cnes.fr Highlights in Space 2010 Prepared in cooperation with the International Astronautical Federation, the Committee on Space Research and the International Institute of Space Law The United Nations Office for Outer Space Affairs is responsible for promoting international cooperation in the peaceful uses of outer space and assisting developing countries in using space science and technology. United Nations Office for Outer Space Affairs P. O. Box 500, 1400 Vienna, Austria Tel: (+43-1) 26060-4950 Fax: (+43-1) 26060-5830 E-mail: [email protected] URL: www.unoosa.org United Nations publication Printed in Austria USD 15 Sales No. E.11.I.3 ISBN 978-92-1-101236-1 ST/SPACE/57 *1180239* V.11-80239—January 2011—775 UNITED NATIONS OFFICE FOR OUTER SPACE AFFAIRS UNITED NATIONS OFFICE AT VIENNA Highlights in Space 2010 Prepared in cooperation with the International Astronautical Federation, the Committee on Space Research and the International Institute of Space Law Progress in space science, technology and applications, international cooperation and space law UNITED NATIONS New York, 2011 UniTEd NationS PUblication Sales no. -
Superwasp Observations of Long Timescale Photometric Variations in Cataclysmic Variables
A&A 514, A30 (2010) Astronomy DOI: 10.1051/0004-6361/200912650 & c ESO 2010 Astrophysics SuperWASP observations of long timescale photometric variations in cataclysmic variables N. L. Thomas1,A.J.Norton1, D. Pollacco2,R.G.West3,P.J.Wheatley4, B. Enoch5, and W. I. Clarkson6 1 Department of Physics and Astronomy, The Open University, Milton Keynes MK7 6AA, UK e-mail: [email protected] 2 Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University, University Road, Belfast BT7 1NN, UK 3 Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UK 4 Department of Physics, University of Warwick, Coventry CV4 7AL, UK 5 SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, St. Andrews, Fife KY16 9SS, UK 6 STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA Received 7 June 2009 / Accepted 26 January 2010 ABSTRACT Aims. We investigated whether the predictions and results of Stanishev et al. (2002, A&A, 394, 625) concerning a possible relation- ship between eclipse depths in PX And and its retrograde disc precession phase, could be confirmed in long term observations made by SuperWASP. In addition, two further CVs (DQ Her and V795 Her) in the same SuperWASP data set were investigated to see whether evidence of superhump periods and disc precession periods were present and what other, if any, long term periods could be detected. Methods. Long term photometry of PX And, V795 Her and DQ Her was carried out and Lomb-Scargle periodogram analysis under- taken on the resulting light curves. For the two eclipsing CVs, PX And and DQ Her, we analysed the potential variations in the depth of the eclipse with cycle number. -
Arxiv:1810.09864V2 [Astro-Ph.SR] 6 Nov 2018
Manuscript for Revista Mexicana de Astronomía y Astrofísica (2007) EXTENSIVE PHOTOMETRY OF V1838 AQL DURING THE 2013 SUPEROUTBURST J. Echevarría1, E. de Miguel2, J. V. Hernández Santisteban3, R. Michel4, R. Costero1, L. J. Sánchez1, A. Ruelas-Mayorga1, J. Olivares5, D. González-Buitrago6, J.L. Jones7, A. Oskanen8, W. Goff9, J. Ulowetz10, G. Bolt11, R. Sabo12, F.-J Hambsch13, D. Slauson14, and W. Stein15 Draft version: September 6, 2021 RESUMEN Presentamos un estudio fotométrico detallado de la super-erupción de V1838 Aql, una variable cataclísmica recientemente descubierta, desde el máx- imo en 2013 hasta su regreso al mínimo. Examinamos en detalle la evolución de los superhumps. Determinamos el período orbital Porb = 0:05698(9) d a partir de la periodicidad de los superhumps tempranos. Comparando los períodos de superhumps en las etapas A y B con el valor del período orbital, derivamos un valor del cambio en el período orbital de = 0:024(2) y un cociente de masa para el sistema de q = 0:10(1). Sugerimos que V1838 Aql se está acercando al mínimo período orbital, por lo que la secundaria sería una estrella de baja masa y no un objeto sub-estelar. ABSTRACT We present an in-depth photometric study of the 2013 superoutburst of the recently discovered cataclysmic variable V1838 Aql and subsequent pho- tometry near its quiescent state. A careful examination of the development of the superhumps is presented. Our best determination of the orbital period is Porb = 0:05698(9) days, based on the periodicity of early superhumps. Com- paring the superhump periods at stages A and B with the early superhump 1Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, Ciudad Universitaria, México D.F., C.P. -
Kibo HANDBOOK
Kibo HANDBOOK September 2007 Japan Aerospace Exploration Agency (JAXA) Human Space Systems and Utilization Program Group Kibo HANDBOOK Contents 1. Background on Development of Kibo ............................................1-1 1.1 Summary ........................................................................................................................... 1-2 1.2 International Space Station (ISS) Program ........................................................................ 1-2 1.2.1 Outline.........................................................................................................................1-2 1.3 Background of Kibo Development...................................................................................... 1-4 2. Kibo Elements...................................................................................2-1 2.1 Kibo Elements.................................................................................................................... 2-2 2.1.1 Pressurized Module (PM)............................................................................................ 2-3 2.1.2 Experiment Logistics Module - Pressurized Section (ELM-PS)................................... 2-4 2.1.3 Exposed Facility (EF) .................................................................................................. 2-5 2.1.4 Experiment Logistics Module - Exposed Section (ELM-ES)........................................ 2-6 2.1.5 JEM Remote Manipulator System (JEMRMS)............................................................ -
Lemmings. I. the Emerlin Legacy Survey of Nearby Galaxies. 1.5-Ghz Parsec-Scale Radio Structures and Cores
MNRAS 000,1{44 (2018) Preprint 8 February 2018 Compiled using MNRAS LATEX style file v3.0 LeMMINGs. I. The eMERLIN legacy survey of nearby galaxies. 1.5-GHz parsec-scale radio structures and cores R. D. Baldi1?, D. R. A. Williams1, I. M. McHardy1, R. J. Beswick2, M. K. Argo2;3, B. T. Dullo4, J. H. Knapen5;6, E. Brinks7, T. W. B. Muxlow2, S. Aalto8, A. Alberdi9, G. J. Bendo2;10, S. Corbel11;12, R. Evans13, D. M. Fenech14, D. A. Green15, H.-R. Kl¨ockner16, E. K¨ording17, P. Kharb18, T. J. Maccarone19, I. Mart´ı-Vidal8, C. G. Mundell20, F. Panessa21, A. B. Peck22, M. A. P´erez-Torres9, D. J. Saikia18, P. Saikia17;23, F. Shankar1, R. E. Spencer2, I. R. Stevens24, P. Uttley25 and J. Westcott7 1 School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK 2 Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK 3 Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK 4 Departamento de Astrofisica y Ciencias de la Atmosfera, Universidad Complutense de Madrid, E-28040 Madrid, Spain 5 Instituto de Astrofisica de Canarias, Via Lactea S/N, E-38205, La Laguna, Tenerife, Spain 6 Departamento de Astrofisica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain 7 Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, AL10 9AB, UK 8 Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, 43992 Onsala, Sweden 9 Instituto de Astrofisica de Andaluc´ıa(IAA, CSIC); Glorieta de la Astronom´ıa s/n, 18008-Granada, Spain 10 ALMA Regional Centre Node, UK 11 Laboratoire AIM (CEA/IRFU - CNRS/INSU - Universit´eParis Diderot), CEA DSM/IRFU/SAp, F-91191 Gif-sur-Yvette, France 12 Station de Radioastronomie de Nan¸cay, Observatoire de Paris, PSL Research University, CNRS, Univ. -
A Massive Core for a Cluster of Galaxies at a Redshift of 4.3 Arxiv
A massive core for a cluster of galaxies at a redshift of 4.3 T. B. Miller1;2, S. C. Chapman1;3;4, M. Aravena5, M. L. N. Ashby6, C. C. Hayward6;7, J. D. Vieira8, A. Weiß9, A. Babul10, M. Bethermin´ 11, C. M. Bradford12;13, M. Brodwin14, J. E. Carlstrom15;16;17;18, Chian-Chou Chen19, D. J. M. Cunningham1;20, C. De Breuck 19, A. H. Gonzalez21, T. R. Greve22,J. Harnett23, Y. Hezaveh24, K. Lacaille1;25, K. C. Litke26, J. Ma21, M. Malkan27, D. P. Marrone26, W. Morningstar24, E. J. Murphy28, D. Narayanan21, E. Pass1;29, R. Perry1, K. A. Phadke8, D. Rennehan10, K. M. Rotermund1, J. Simpson30;31, J. S. Spilker26, J. Sreevani8, A. A. Stark6, M. L. Strandet9;32 & A. L. Strom33 1Department of Physics and Atmospheric Science, Dalhousie University, Halifax, Canada 2Department of Astronomy, Yale University, 52 Hillhouse Avenue, New Haven, CT, 06511, USA 3Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK 4National Research Council, Herzberg Astronomy & Astrophysics, 5071 West Saanich Road, Victoria, BC, V9E 2E7, Canada 5Nucleo´ de Astronom´ıa, Facultad de Ingenier´ıa y Ciencias, Universidad Diego Portales, Av. Ejercito 441, Santiago, Chile 6Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 7Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USA 8Department of Astronomy, University of Illinois, 1002 West Green Street, Urbana, IL 61801, USA 9Max-Planck-Institut fur Radioastronomie, Auf dem Hugel¨ 69 D-53121 Bonn, Germany 10Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 1A1, Canada 11Aix-Marseille Universite,´ CNRS, LAM, Laboratoire d’Astrophysique de Marseille, Marseille, France 12California Institute of Technology, 1200 E.