DOCSLIB.ORG

Programme of Work for 2020 and 2021, and Related Procurement Plan

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Programme of Work for 2020 and 2021, and Related Procurement Plan EUROPEAN SPACE AGENCY INDUSTRIAL POLICY COMMITTEE Science Programme Technology Development Plan: Programme of Work for 2020 and 2021, and Related Procurement Plan SUMMARY This document presents the activities in the Science Core Technology Programme (CTP) and in the Technology Development Element (TDE, replacing the TRP) of the Discovery, Preparation & Technology Development Basic Activities supporting the implementation of ESA’s Science Programme. The national initiatives activities of relevance to the Science programme are provided for information. Activities funded through the Industrial Policy Task Forces (IPTFs) and of relevance to the Science Programme are also provided for information. June 2020 ESA UNCLASSIFIED – Releasable to the Public Page intentionally left blank ESA UNCLASSIFIED – Releasable to the Public 1 Background and Scope This document provides an update to the Science Programme Technology Development Plan (TDP). The plan contains the description of the technology development activities (TDAs) required for the technological preparation of all mission candidates in the Agency’s Science Programme. Critical mission-enabling developments that are generically applicable to several possible future space science missions are also addressed. This plan was first issued in 2008 as ESA/IPC(2008)33,add.1, and the last significant update was presented in ESA/IPC(2019)81.rev.1, approved by the IPC in November 2019. As regularly done for past versions of the plan, activities to be initiated by ESA in the year following the work plan approval are presented for a decision, while activities identified for potential implementation at a later stage are presented for information. When identified, national activities in support of payload developments are recommended for implementation under national funding. 2 Science Programme Missions The European Space Science Programme addresses a number of high-level science questions, originally described in the document “Cosmic Vision Space Science for Europe 2015-2025”. New missions are proposed by the science community and follow a thorough competitive process before being proposed for selection to the Science Programme Committee (SPC). This bottom-up selection process aims at scientific and technical excellence by identifying the best mission to implement at a given time and for specified budget and schedule boundaries. The current implementation status of the Science Programme is briefly recalled below. The first Call for Missions in the context of the Cosmic Vision plan was issued in March 2007 targeting one M-Class and one L-Class mission. This Call has ultimately led to the implementation of the M1, M2 and L1 missions: Solar Orbiter was selected as M1 and was launched in February 2020; Euclid was selected as M2 and is planned for launch in 2022; JUICE was selected as L1 and is also planned for launch in 2022. The second Call for Missions in the same framework was issued in July 2010 for the third M-Class mission (M3), and led to the implementation of PLATO, which is planned for launch in 2026. The Call for the fourth M mission (M4) has led to the selection of the ARIEL mission in March 2018. ARIEL is currently within Phase B1. The mission adoption is planned late 2020 and launch is targeted in 2028, together with Comet Interceptor. The Call for the fifth medium-sized mission opportunity (M5) was issued in April 2016 and resulted in selection of three candidate missions: EnVision (mission devoted to investigate the surface and subsurface of Venus, in collaboration with NASA); SPICA (mid- and far-infrared observatory using a 2.5 m cryogenic telescope following Herschel, in collaboration with JAXA); and THESEUS (mission devoted to Gamma Ray Burst measurements). Parallel Phase A studies for each of the candidate ESA UNCLASSIFIED – Releasable to the Public missions were initiated early 2019 and the selection of the M5 mission is planned mid- 2021. Additionally, a Call for a small mission took place in 2012. Following the Call, CHEOPS was adopted by the SPC as the S1 mission in February 2014 and the industrial implementation contract was kicked-off mid-2014. CHEOPS was launched on a Soyuz rocket from Kourou as a passenger to a main spacecraft in December 2019. The Call for “Fast” mission was issued in July 2018 for a modest-sized mission to be launched as a passenger to ARIEL in 2028 on an Ariane 6.2 launcher. Following the scientific peer review of the proposals carried out in mid-2019, the Comet Interceptor mission was selected and is currently in Phase A/B, aiming at the mission adoption by 2022. In March 2013 ESA issued a Call to define the scientific themes of the Large missions L2 and L3, with envisaged launches before 2035, resulting in the selection of “the hot and energetic Universe” theme (to be addressed by an X-ray observatory) for L2, and “the gravitational Universe” theme (to be addressed by a gravitational wave observatory) for L3. The Call for mission proposals for the L2 launch opportunity was issued early 2014 and resulted in the selection in June 2014 of the Athena mission concept. Athena is an X- ray telescope with two focal plane instruments, a Wide Field Imager (WFI) and a Cryogenic X-ray Spectrometer (XIFU). The Athena Phase A study was completed in 2019, and is currently in the Phase B1, aiming at the mission adoption by mid-2022 and launch in 2032/2033 timeframe. The L3 Call for mission proposals was issued late 2016 and resulted in the selection of the LISA mission concept in June 2017, using laser interferometry for gravitational wave measurement, building on the successful demonstration achieved in orbit by LISA Pathfinder in 2016. The Phase A started in 2018, in parallel with the mission technology preparation, and is expected to be completed in 2021. The mission adoption date is planned in 2024. The overall implementation scheme for LISA and Athena will be discussed with the SPC at its July 2020 meeting. In January 2015 a joint ESA/Chinese Academy of Sciences (CAS) call for a small joint mission led to the selection of the SMILE mission. SMILE will provide for the first time global imaging of the interaction between the solar wind and the magnetosphere of the Earth using innovative X-ray and UV instrumentation. Following the successful completion of Phase A/B, undertaken jointly by ESA and CAS, the mission was adopted in March 2019, with a planned launch in 2024. The Figure 1 summarises the Science Programme plan as of March 2020. An update to the plan will be discussed with the SPC at its July 2020 meeting. ESA UNCLASSIFIED – Releasable to the Public Figure 1: ESA Science Programme Mission Plan Timeline Summary 3 Science Programme Technology Development Plan 3.1 Present Technology Development Plan Update This technology plan was defined, as for previous versions, using the ESA End-to-End technology management process as described in ESA/IPC(2005)39, involving a Technology Network (TECNET) of technical and mission experts from ESA. The proposed technological activities are based on: Critical technologies that were identified based on internal ESA studies. ESA UNCLASSIFIED – Releasable to the Public Technology development activities identified by industry in the course of the mission candidates assessment studies. Technology development activities identified by the science community, through studies done by institutes or consortia in parallel to the industrial studies. An assessment of the technological needs and maturity with respect to on-going running activities, urgency and funding availability. The new activities are addressing the L missions Athena (L2) and LISA (L3), Ariel, Comet Interceptor and technologies applicable to several missions. 3.2 Implementation Principles and Payload-Related Activities A guiding principle of the Science Programme is that critical basic technology developments of the spacecraft and science instruments must be completed before entering the Definition Phase. As a general rule, Technology Readiness Level 5-6 (in ISO scale) is expected for both the space segment and the payload at the start of the Implementation Phase. A summary of the current assumptions on the payload procurement scheme is provided in Table 1 for the M and L missions. Category A = ESA-provided payload; Category B = payload provided by Member States; Category C = payload shared between ESA and Member States. Mission Payload Member State Provision ESA Payload Provision Category Athena C Focal plane instrumentation: X-ray telescope (L2 mission) Wide Field Imager (Silicon Pore Optics) X-ray Spectrometer Cryogenic cooling chain for X- (with JAXA and NASA ray spectrometer contributions) (with possible contributions from partners) LISA C Optical bench, Gravitational Telescope, Laser system (L3 Mission) Reference Sensor, (with possible contributions Phasemeter from NASA) ARIEL B Complete payload V-grooves, AIRS detectors (M4 mission) complement, including cryogenic PLM and warm payload units. SMILE C Soft X-ray Imager (SXI), PLM overall responsibility (ESA-CAS UV Imager (UVI led by mission) Canada), MAG and LIA instruments are provided by CAS Comet B Complete payload Interceptor (F mission) Table 1: Assumptions for the payload provision of the selected missions in the preparation phase. Category A = ESA-provided payload; Category B = payload provided by the Member States; Category C = payload shared between ESA and Member States It is assumed that the Member States will be in charge of the technology developments of the instruments they plan to provide, while ESA will implement the technology developments related to the rest of the spacecraft and payload elements remaining under ESA responsibility. A good coordination between the technology developments under ESA UNCLASSIFIED – Releasable to the Public Member States and ESA responsibility is imperative, thereby avoiding duplication of effort, enabling identification of missing activities and providing ESA with visibility of the payload development. 3.3 Budgets and Implementation Aspects The ESA technology development activities in the Science Programme mainly rely on the CTP and TDE technology budgets and are submitted to the Industrial Policy Committee (IPC) for approval and implementation.
Load more

Recommended publications
  • IVS NICT-TDC News No.39
    ISSN 1882-3432 CONTENTS Proceedings of the 18th NICT TDC Symposium (Kashima, October 1, 2020) KNIFE, Kashima Nobeyama InterFErometer . 3 Makoto Miyoshi Space-Time Measurements Research Inspired by Kashima VLBI Group . 8 Mizuhiko Hosokawa ALMA High Frequency Long Baseline Phase Correction Using Band-to-band ..... 11 (B2B) Phase Referencing Yoshiharu Asaki and Luke T. Maud Development of a 6.5-22.5 GHz Very Wide Band Feed Antenna Using a New ..... 15 Quadruple-Ridged Antenna for the Traditional Radio Telescopes Yutaka Hasegawa*, Yasumasa Yamasaki, Hideo Ogawa, Taiki Kawakami, Yoshi- nori Yonekura, Kimihiro Kimura, Takuya Akahori, Masayuki Ishino, Yuki Kawa- hara Development of Wideband Antenna . 18 Hideki Ujihara Performance Survey of Superconductor Filter Introduced in Wideband Re- ..... 20 ceiver for VGOS of the Ishioka VLBI Station Tomokazu Nakakuki, Haruka Ueshiba, Saho Matsumoto, Yu Takagi, Kyonosuke Hayashi, Toru Yutsudo, Katsuhiro Mori, Tomokazu Kobayashi, and Mamoru Sekido New Calibration Method for a Radiometer Without Using Liquid Nitrogen ..... 23 Cooled Absorber Noriyuki Kawaguchi, Yuichi Chikahiro, Kenichi Harada, and Kensuke Ozeki Comparison of Atmospheric Delay Models (NMF, VMF1, and VMF3) in ..... 27 VLBI analysis Mamoru Sekido and Monia Negusini HINOTORI Status Report . 31 Hiroshi Imai On-the-Fly Interferometer Experiment with the Yamaguchi Interferometer . 34 Kenta Fujisawa, Kotaro Niinuma, Masanori Akimoto, and Hideyuki Kobayashi Superconducting Wide-band BRF for Geodetic VLBI Observation with ..... 36 VGOS Radio Telescope
    [Show full text]
  • Comet Interceptor: a Proposed ESA Mission to a Dynamically New Comet
    EPSC Abstracts Vol. 13, EPSC-DPS2019-1679-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Comet Interceptor: A proposed ESA Mission to a Dynamically New Comet Geraint H. Jones(1,2), Colin Snodgrass(3), and The Comet Interceptor Consortium (see www.cometinterceptor.space ) (1) UCL Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, RH5 6NT, UK ([email protected]) (2) The Centre for Planetary Sciences at UCL/Birkbeck, London, UK (3) University of Edinburgh, United Kingdom ([email protected]) Abstract allow valuable multi-point measurements of the solar wind over different lengtH-scales as tHese craft In response to the recent European Space Agency’s separate. call for proposals for a Fast (F) Mission, a multi- spacecraft project has been submitted to ESA to For the comet encounter, the primary spacecraft, encounter a dynamically new comet or interstellar planned to also act as the primary communication object. SucH an encounter with a comet approacHing point for the whole constellation, would be targetted the Sun for the first time would provide valuable data to pass outside the hazardous inner coma, on the to complement that from all previous comet missions, sunward side of tHe comet. At least one sub-spacecraft whicH Have by necessity studied sHort-period comets would be targetted for tHe nucleus/inner coma region. that Have evolved from their original condition during The various component spacecraft will carry a range their time orbiting near the Sun. of miniaturised instruments for remote and in situ studies of tHe object’s composition, nucleus, coma, The mission’s primary science goal is to cHaracterise, and plasma environment.
    [Show full text]
  • HVAC Controls (DDC/EMS/BAS) Evaluation Protocol
    Chapter 19: HVAC Controls (DDC/EMS/BAS) Evaluation Protocol The Uniform Methods Project: Methods for Determining Energy Efficiency Savings for Specific Measures Created as part of subcontract with period of performance September 2011 – December 2014 Jeff Romberger SBW Consulting, Inc. Bellevue, Washington NREL Technical Monitor: Charles Kurnik NREL is a national laboratory of the U.S. Department of Energy Office of Energy Efficiency & Renewable Energy Operated by the Alliance for Sustainable Energy, LLC This report is available at no cost from the National Renewable Energy Laboratory (NREL) at www.nrel.gov/publications. Subcontract Report NREL/SR-7A40-63167 November 2014 Contract No. DE-AC36-08GO28308 Chapter 19: HVAC Controls (DDC/EMS/BAS) Evaluation Protocol The Uniform Methods Project: Methods for Determining Energy Efficiency Savings for Specific Measures Created as part of subcontract with period of performance September 2011 – December 2014 Jeff Romberger SBW Consulting, Inc. Bellevue, Washington NREL Technical Monitor: Charles Kurnik Prepared under Subcontract No. LGJ-1-11965-01 NREL is a national laboratory of the U.S. Department of Energy Office of Energy Efficiency & Renewable Energy Operated by the Alliance for Sustainable Energy, LLC This report is available at no cost from the National Renewable Energy Laboratory (NREL) at www.nrel.gov/publications. National Renewable Energy Laboratory Subcontract Report 15013 Denver West Parkway NREL/SR-7A40-63167 Golden, CO 80401 November 2014 303-275-3000 • www.nrel.gov Contract No. DE-AC36-08GO28308 NOTICE This report was prepared as an account of work sponsored by an agency of the United States government. Neither the United States government nor any agency thereof, nor any of their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights.
    [Show full text]
  • HD 97658 and Its Super-Earth Spitzer & MOST Transit Analysis and Seismic Modeling of the Host Star
    The space photometry revolution CoRoT3-KASC7 joint meeting HD 97658 and its super-Earth Spitzer & MOST transit analysis and seismic modeling of the host star Valerie Van Grootel (University of Liege, Belgium) M. Gillon (U. Liege), D. Valencia (U. Toronto), N. Madhusudhan (U. Cambridge), D. Dragomir (UC Santa Barbara), and the Spitzer team 1. Introducing HD 97658 and its super-Earth The second brightest star harboring a transiting super-Earth HD 97658 (V=7.7, K=5.7) HD 97658 b, a transiting super-Earth • • Teff = 5170 ± 50 K (Howard et al. 2011) Discovery by Howard et al. (2011) from Keck- Hires RVs: • [Fe/H] = -0.23 ± 0.03 ~ Z - M sin i = 8.2 ± 1.2 M • d = 21.11 ± 0.33 pc ; from Hipparcos P earth - P = 9.494 ± 0.005 d (Van Leeuwen 2007) orb • Transits discovered by Dragomir et al. (2013) with MOST: RP = 2.34 ± 0.18 Rearth From Howard et al. (2011) From Dragomir et al. (2013) Valerie Van Grootel – CoRoT/Kepler July 2014, Toulouse 2 2. Modeling the host star HD 97658 Rp α R* 2/3 Mp α M* Radial velocities Transits + the age of the star is the best proxy for the age of its planets (Sun: 4.57 Gyr, Earth: 4.54 Gyr) • With Asteroseismology: T. Campante, V. Van Eylen’s talks • Without Asteroseismology: stellar evolution modeling Valerie Van Grootel – CoRoT/Kepler July 2014, Toulouse 3 2. Modeling the host star HD 97658 • d = 21.11 ± 0.33 pc, V = 7.7 L* = 0.355 ± 0.018 Lsun • +Teff from spectroscopy: R* = 0.74 ± 0.03 Rsun • Stellar evolution code CLES (Scuflaire et al.
    [Show full text]
  • X-Ray Telescope
    Early results of the Hitomi satellite Hiro Matsumoto Ux group & KMI Nagoya Univ.1 Outline •Hitomi instruments •Early scientific results –DM in Perseus –Turbulence in Perseus –others 2 Japanese history of X-ray satellites Launch, Feb. 17, 2016 Weight Suzaku Ginga ASCA Hitomi Tenma Hakucho Rocket 3 International collaboration More than 160 scientists from Japan/USA/Europe 4 Attitude anomaly Loss of communication (Mar. 26, 2016) spinning Gave up recovery (Apr. 28, 2016)5 Hitomi Obs. List Target Date Perseus Cluster of galaxies Feb. 25—27, 2016 Mar. 4—8, 2016 N132D Supernova remnants Mar. 8—11, 2016 IGR J16318-4848 Pulsar wind nebula Mar. 11—15, 2016 RXJ 1856-3754 Neutron star Mar. 17—19, 2016 Mar. 23—25, 2016 G21.5-0.9 Pulsar wind nebula Mar. 19—23, 2016 Crab Pulsar wind nebula Mar. 25, 2016 6 Scienfitic Instruments 7 4 systems Name X-Ray Telescope SXS Soft Micro-calorimeter (E<10keV) SXI Soft CCD (E<10keV) HXI Hard Si/CdTe (E<80keV) SGD --- Si/CdTe (Compton) 8 Wide energy range (0.3—600keV) HXT 1keV∼ 107K SXT SGD SXI HXI SXS 9 SXT + SXS (0.3—12keV) Soft X-ray Telescope Soft X-ray Spectrometer (X-ray micro-calorimeter) f=5.6m 10 Soft X-ray Spectrometer (SXS) FOV: 3′ × 3′ Δ푇 ∝ ℎ휈 6 × 6 pix 11 Energy Resolution Hitomi SXS Suzaku CCD Δ퐸 = 5 푒푉@ 6푘푒푉 (cf. CCD Δ퐸 = 130 푒푉)12 Before Hitomi: gratings Point source Extended Not good for extended objects 13 X-ray microcalorimeter Extended Non-dispersive type. Spatial extension doesn’t matter.
    [Show full text]
  • Asteroseismology with Corot, Kepler, K2 and TESS: Impact on Galactic Archaeology Talk Miglio’S
    Asteroseismology with CoRoT, Kepler, K2 and TESS: impact on Galactic Archaeology talk Miglio’s CRISTINA CHIAPPINI Leibniz-Institut fuer Astrophysik Potsdam PLATO PIC, Padova 09/2019 AsteroseismologyPlato as it is : a Legacy with CoRoT Mission, Kepler for Galactic, K2 and TESS: impactArchaeology on Galactic Archaeology talk Miglio’s CRISTINA CHIAPPINI Leibniz-Institut fuer Astrophysik Potsdam PLATO PIC, Padova 09/2019 Galactic Archaeology strives to reconstruct the past history of the Milky Way from the present day kinematical and chemical information. Why is it Challenging ? • Complex mix of populations with large overlaps in parameter space (such as Velocities, Metallicities, and Ages) & small volume sampled by current data • Stars move away from their birth places (migrate radially, or even vertically via mergers/interactions of the MW with other Galaxies). • Many are the sources of migration! • Most of information was confined to a small volume Miglio, Chiappini et al. 2017 Key: VOLUME COVERAGE & AGES Chiappini et al. 2018 IAU 334 Quantifying the impact of radial migration The Rbirth mix ! Stars that today (R_now) are in the green bins, came from different R0=birth Radial Migration Sources = bar/spirals + mergers + Inside-out formation (gas accretion) GalacJc Center Z Sun R Outer Disk R = distance from GC Minchev, Chiappini, MarJg 2013, 2014 - MCM I + II A&A A&A 558 id A09, A&A 572, id A92 Two ways to expand volume for GA • Gaia + complementary photometric information (but no ages for far away stars) – also useful for PIC! • Asteroseismology of RGs (with ages!) - also useful for core science PLATO (miglio’s talk) The properties at different places in the disk: AMR CoRoT, Gaia+, K2 + APOGEE Kepler, TESS, K2, Gaia CoRoT, Gaia+, K2 + APOGEE PLATO + 4MOST? Predicon: AMR Scatter increases towards outer regions Age scatter increasestowars outer regions ExtracGng the best froM GaiaDR2 - Anders et al.
    [Show full text]
  • Smart Buildings: Using Smart Technology to Save Energy in Existing Buildings
    Smart Buildings: Using Smart Technology to Save Energy in Existing Buildings Jennifer King and Christopher Perry February 2017 Report A1701 © American Council for an Energy-Efficient Economy 529 14th Street NW, Suite 600, Washington, DC 20045 Phone: (202) 507-4000 • Twitter: @ACEEEDC Facebook.com/myACEEE • aceee.org SMART BUILDINGS © ACEEE Contents About the Authors ..............................................................................................................................iii Acknowledgments ..............................................................................................................................iii Executive Summary ........................................................................................................................... iv Introduction .......................................................................................................................................... 1 Methodology and Scope of This Study ............................................................................................ 1 Smart Building Technologies ............................................................................................................. 3 HVAC Systems ......................................................................................................................... 4 Plug Loads ................................................................................................................................. 9 Lighting ..................................................................................................................................
    [Show full text]
  • Gaianir Combining Optical and Near-Infra-Red (NIR) Capabilities with Time-Delay-Integration (TDI) Sensors for a Future Gaia-Like Mission
    Proposal title: GaiaNIR Combining optical and Near-Infra-Red (NIR) capabilities with Time-Delay-Integration (TDI) sensors for a future Gaia-like mission. PI: Dr. David Hobbs, Lund Observatory, Box 43, SE-221 00 Lund, Sweden. Email: [email protected]. Tel.: +46-46-22 21573 Core team members: The following minimum team is needed to initiate the project. D. Hobbs Lund Observatory, Sweden. A. Brown Leiden Observatory, Holland. A. Mora Aurora Technology B.V., Spain. C. Crowley HE Space Operations B.V., Spain. N. Hambly University of Edinburgh, UK. J. Portell Institut de Ciències del Cosmos, ICCUB-IEEC, Spain. C. Fabricius Institut de Ciències del Cosmos, ICCUB-IEEC, Spain. M. Davidson University of Edinburgh, UK. Proposal writers: See Appendix A. Other supporting scientists: See Appendix B and Appendix C. Senior science advisors: E. Høg Copenhagen University (Retired), Denmark. L. Lindegren Lund Observatory, Sweden. C. Jordi Institut de Ciències del Cosmos, ICCUB-IEEC, Spain. S. Klioner Lohrmann Observatory, Germany. F. Mignard Observatoire de la Côte d’Azur, France. arXiv:1609.07325v2 [astro-ph.IM] 22 May 2020 Fig. 1: Left is an IR image from the Two Micron All-Sky Survey (image G. Kopan, R. Hurt) while on the right an artist’s concept of the Gaia mission superimposed on an optical image, (Image ESA). Images not to scale. 1 1. Executive summary ESA recently called for new “Science Ideas” to be investigated in terms of feasibility and technological developments – for tech- nologies not yet sufficiently mature. These ideas may in the future become candidates for M or L class missions within the ESA Science Program.
    [Show full text]
  • Progress with Litebird
    LiteBIRD Lite (Light) Satellite for the Studies of B-mode Polarization and Inflation from Cosmic Background Radiation Detection Progress with LiteBIRD Masashi Hazumi (KEK/Kavli IPMU/SOKENDAI/ISAS JAXA) for the LiteBIRD working group 1 LiteBIRD JAXA Osaka U. Kavli IPMU Kansei U. Tsukuba APC Paris T. Dotani S. Kuromiya K. Hattori Gakuin U. M. Nagai R. Stompor H. Fuke M. Nakajima N. Katayama S. Matsuura H. Imada S. Takakura Y. Sakurai TIT Cardiff U. I. Kawano K. Takano H. Sugai Kitazato U. S. Matsuoka G. Pisano UC Berkeley / H. Matsuhara T. Kawasaki R. Chendra LBNL T. Matsumura Osaka Pref. U. KEK Paris ILP D. Barron K. Mitsuda M. Inoue M. Hazumi Konan U. U. Tokyo J. Errard J. Borrill T. Nishibori K. Kimura (PI) I. Ohta S. Sekiguchi Y. Chinone K. Nishijo H. Ogawa M. Hasegawa T. Shimizu CU Boulder A. Cukierman A. Noda N. Okada N. Kimura NAOJ S. Shu N. Halverson T. de Haan A. Okamoto K. Kohri A. Dominjon N. Tomita N. Goeckner-wald S. Sakai Okayama U. M. Maki T. Hasebe McGill U. P. Harvey Y. Sato T. Funaki Y. Minami J. Inatani Tohoku U. M. Dobbs C. Hill K. Shinozaki N. Hidehira T. Nagasaki K. Karatsu M. Hattori W. Holzapfel H. Sugita H. Ishino R. Nagata S. Kashima MPA Y. Hori Y. Takei A. Kibayashi H. Nishino T. Noguchi Nagoya U. E. Komatsu O. Jeong S. Utsunomiya Y. Kida S. Oguri Y. Sekimoto K. Ichiki NIST R. Keskitalo T. Wada K. Komatsu T. Okamura M. Sekine T. Kisner G. Hilton R. Yamamoto S. Uozumi N.
    [Show full text]
  • EUCLID Mission Assessment Study
    EUCLID Mission Assessment Study Executive Summary ESA Contract. No. 5856/08/F/VS September 2009 EUCLID– Mapping the Dark Universe EUCLID is a mission to study geometry and nature of the dark universe. It is a medium-class mission candidate within ESA's Cosmic Vision 2015– 2025 Plan for launch around 2017. EUCLID has been derived by ESA from DUNE and SPACE, two complementary Cosmic Vision proposals addressing questions on the origin and the constitution of the Universe. 70% Dark Energy The observational methods applied by EUCLID are shape and redshift measure- ments of galaxies and clusters of galaxies. To 4% Baryonic Matter this end EUCLID is equipped with 3 scientific instruments: 26% Dark Matter • Visible Imager (VIS) • Near-Infrared Photometer (NIP) • Near-Infrared Spectrograph (NIS) The EUCLID Mission Assessment Study is the industrial part of the EUCLID assessment phase. The study has been performed by Astrium from September 2008 to September 2009 and is intended for space segment definition and programmatic evaluation. The prime responsibility is with Astrium GmbH (Friedrichshafen, Germany) with support from Astrium SAS (Toulouse, France) and Astrium Ltd (Stevenage, UK). EUCLID Mission EUCLID shall observe 20.000 deg2 of the extragalactic sky at galactic latitudes |b|>30 deg. The sky is sampled in step & b>30° stare mode with instantaneous fields of about 0.5 deg2 . Nominally a strip of about 20 deg in latitude is scanned per day (corresponding to about 1 deg in longitude). galactic plane step 1 b<30° step 2 step 3 The sky is nominally observed along great circles in planes perpendicular to the Sun- spacecraft axis (SAA=0).
    [Show full text]
  • Arxiv:2005.12932V1 [Astro-Ph.EP] 26 May 2020 with Eccentricity, E = 1.2, ‘Oumuamua Encountered the Solar System with V∞ = 26 Km S
    Draft version May 28, 2020 Typeset using LATEX default style in AASTeX63 Evidence that 1I/2017 U1 (`Oumuamua) was composed of molecular hydrogen ice. Darryl Seligman1 and Gregory Laughlin2 1 Dept. of the Geophysical Sciences, University of Chicago, Chicago, IL 60637 2Dept. of Astronomy, Yale University, New Haven, CT 06517 (Received April 14, 2020; Revised May 22, 2020; Accepted May 28, 2020) Submitted to ApJL ABSTRACT `Oumuamua (I1 2017) was the first macroscopic (l ∼ 100 m) body observed to traverse the inner solar system on an unbound hyperbolic orbit. Its light curve displayed strong periodic variation, and it showed no hint of a coma or emission from molecular outgassing. Astrometric measurements indicate that 'Oumuamua experienced non-gravitational acceleration on its outbound trajectory, but energy balance arguments indicate this acceleration is inconsistent with a water ice sublimation-driven jet of the type exhibited by solar system comets. We show that all of `Oumaumua's observed properties can be explained if it contained a significant fraction of molecular hydrogen (H2) ice. H2 sublimation at a rate proportional to the incident solar flux generates a surface-covering jet that reproduces the observed acceleration. Mass wasting from sublimation leads to monotonic increase in the body axis ratio, explaining `Oumuamua's shape. Back-tracing `Oumuamua's trajectory through the Solar System permits calculation of its mass and aspect ratio prior to encountering the Sun. We show that H2-rich bodies plausibly form in the coldest dense cores of Giant Molecular Clouds, where number densities are of order n ∼ 105, and temperatures approach the T = 3 K background.
    [Show full text]
  • 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.
    [Show full text]