DOCSLIB.ORG

Report of the Astroparticle Physics International Forum (Apif)

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Report of the Astroparticle Physics International Forum (Apif) For Official Use DSTI/STP/GSF(2016)11/FINAL Organisation de Coopération et de Développement Économiques Organisation for Economic Co-operation and Development ___________________________________________________________________________________________ English - Or. English DIRECTORATE FOR SCIENCE, TECHNOLOGY AND INNOVATION COMMITTEE FOR SCIENTIFIC AND TECHNOLOGICAL POLICY For Official Use Official For DSTI/STP/GSF(2016)11/FINAL OECD Global Science Forum REPORT OF THE ASTROPARTICLE PHYSICS INTERNATIONAL FORUM (APIF) Authors of this report are Members of the Astroparticle Physics International Forum (annex 1). Contacts: Carthage Smith ([email protected]) and Qian Dai ([email protected]). English Complete document available on OLIS in its original format - Or. English This document and any map included herein are without prejudice to the status of or sovereignty over any territory, to the delimitation of international frontiers and boundaries and to the name of any territory, city or area. REPORT OF THE ASTROPARTICLE PHYSICS INTERNATIONAL FORUM (APIF) DISCLAIMER This paper should not be reported as representing the official views of the OECD or of its member countries. The opinions expressed and arguments employed are those of the authors. It describes preliminary results or research in progress by the author(s) and is published to stimulate discussion on a broad range of issues on which the OECD works. Comments on this paper are welcomed, and may be sent to Directorate for Science, Technology and Innovation, OECD, 2 rue André-Pascal, 75775 Paris Cedex 16, France. Note to Delegations: This document is also available on OLIS under the reference code: DSTI/STP/GSF(2016)11/FINAL This document, as well as any data and map included herein, are without prejudice to the status of or sovereignty over any territory, to the delimitation of international frontiers and boundaries and to the name of any territory, city or area. The statistical data for Israel are supplied by and under the responsibility of the relevant Israeli authorities. The use of such data by the OECD is without prejudice to the status of the Golan Heights, East Jerusalem and Israeli settlements in the West Bank under the terms of international law. Latvia was not an OECD member country at the time of preparation of this publication. Accordingly, Latvia does not appear in the list of OECD member countries and is not included in the zone aggregates. © OECD 2017 You can copy, download or print OECD content for your own use, and you can include excerpts from OECD publications, databases and multimedia products in your own documents, presentations, blogs, websites and teaching materials, provided that suitable acknowledgment of OECD as source and copyright owner is given. All requests for commercial use and translation rights should be submitted to [email protected]. 2 REPORT OF THE ASTROPARTICLE PHYSICS INTERNATIONAL FORUM (APIF) TABLE OF CONTENTS LIST OF ACRONYMS ................................................................................................................................... 4 About this report .......................................................................................................................................... 7 Preface ......................................................................................................................................................... 8 1. APIF ACTIVITIES, 2011-2016, AND BEYOND ...................................................................................... 9 1.1 Background and Overview .................................................................................................................... 9 1.2 APIF Activities .................................................................................................................................... 11 1.2.1 Exchange of information ............................................................................................................... 11 1.2.2 Exploration of the prospects for joint actions ................................................................................ 12 1.2.3 Consultation on science policy issues ........................................................................................... 12 1.2.4 Discussion on the future development of APIF ............................................................................ 13 1.3 Future APIF structure and hosting arrangements ................................................................................ 14 2. PROGRESS IN KEY SCIENTIFIC DOMAINS IN ASTROPARTICLE PHYSICS ............................... 15 2.1 What is the Universe made of? ............................................................................................................ 15 2.1.1 Dark Matter ................................................................................................................................... 15 2.1.2 Dark Energy .................................................................................................................................. 17 2.1.3 Cosmic Microwave Background ................................................................................................... 19 2.2 What is the role of high-energy phenomena in the Universe? ............................................................. 20 2.2.1 High-Energy Messengers .............................................................................................................. 21 2.2.2 Gravitational Waves ...................................................................................................................... 23 2.3 What is the nature of matter and interactions at the highest energy scale? .......................................... 23 2.3.1 Neutrino Mixing and Proton Decay .............................................................................................. 24 2.3.2 Neutrino Mass ............................................................................................................................... 25 Concluding comments ............................................................................................................................... 26 3. BENEFITS OF ASTROPARTICLE PHYSICS TO OTHER SCIENCES AND SOCIETY .................... 27 3.1 Examples of impact on technology transfer ......................................................................................... 27 3.2 Examples of impact on other scientific disciplines .............................................................................. 28 3.3 Examples of impact on society beyond science and technology ......................................................... 29 Concluding comments ............................................................................................................................... 30 APPENDIX 1. TERMS OF REFERENCE FOR APIF, 2011-2016 ............................................................. 31 APPENDIX 2. THE ASTROPARTICLE PHYSICS INTERNATIONAL FORUM AGREEMENT, 2017 ONWARDS ................................................................................................................................................... 32 APPENDIX 3. A LIST OF APIF MEETINGS AND VENUES, 2011-2016 ............................................... 36 NOTES AND REFERENCES ...................................................................................................................... 37 3 REPORT OF THE ASTROPARTICLE PHYSICS INTERNATIONAL FORUM (APIF) LIST OF ACRONYMS ACT Atacama Cosmology Telescope AGN Active Galactic Nuclei AMS Alpha Magnetic Spectrometer ANTARES Astronomy with a Neutrino Telescope and Abyss environmental RESearch APIF Astroparticle Physics International Forum ApPEC Astroparticle Physics European Consortium of Funding Agencies ApPIC Astroparticle Physics International Committee ARA Askaryan Radio Array ArDM Argon Dark Matter ARIANNA Antarctic Ross Ice-Shelf ANtenna Neutrino Array ASPERA Astro Particle European Research Area network for funding agencies ATLAS A Toroidal LHC ApparatuS BAO Baryon Acoustic Oscillations BICEP Background Imaging of Cosmic Extragalactic Polarization BOREXINO Italian Diminutive of BOREX (Boron Solar Neutrino Experiment) BOSS Baryon acoustic Oscillation Spectroscopic Survey CCD Charge-coupled Device CDM Cold Dark Matter CEA French Alternative Energies and Atomic Energy Commission CERN European Organization for Nuclear Research CHIME Canadian HI Mapping Experiment CLASS Cosmology Large Angular Scale Surveyor CMB Cosmic Microwave Background CMS Compact Muon Solenoid CNES French Space Agency CO2 Carbon Dioxide COBE Cosmic Background Explorer COrE+ Cosmic Origins Explorer + CP Charge-parity CTA Cherenkov Telescope Array CTIO Cerro Tololo Inter-american Observatory CUORE Cryogenic Underground Observatory for Rare Events DECam Dark Energy camera DES Dark Energy Survey DESI Dark Energy Spectroscopic Instrument DM Dark Matter 4 REPORT OF THE ASTROPARTICLE PHYSICS INTERNATIONAL FORUM (APIF) DOE Department of Energy DUNE Deep Underground Neutrino Experiment EBEX E and B Experiment eBOSS Extended Baryon acoustic Oscillation Spectroscopic Survey EC European Commission EGO European Gravitational Observatory ESA European Space Agency ESSENCE Equation of State: SupErNovae trace Cosmic Expansion ETHZ Swiss Federal Institute of Technology in Zurich EUSO Extreme Universe Space Observatory EXO Enriched Xenon Observatory Fermi-LAT Fermi Large Area Telescope GSF Global Science Forum GUT Grand Unified Theories GWIC Gravitational Wave International Committee H.E.S.S.
Load more

Recommended publications
  • XIII Publications, Presentations
    XIII Publications, Presentations 1. Refereed Publications E., Kawamura, A., Nguyen Luong, Q., Sanhueza, P., Kurono, Y.: 2015, The 2014 ALMA Long Baseline Campaign: First Results from Aasi, J., et al. including Fujimoto, M.-K., Hayama, K., Kawamura, High Angular Resolution Observations toward the HL Tau Region, S., Mori, T., Nishida, E., Nishizawa, A.: 2015, Characterization of ApJ, 808, L3. the LIGO detectors during their sixth science run, Classical Quantum ALMA Partnership, et al. including Asaki, Y., Hirota, A., Nakanishi, Gravity, 32, 115012. K., Espada, D., Kameno, S., Sawada, T., Takahashi, S., Ao, Y., Abbott, B. P., et al. including Flaminio, R., LIGO Scientific Hatsukade, B., Matsuda, Y., Iono, D., Kurono, Y.: 2015, The 2014 Collaboration, Virgo Collaboration: 2016, Astrophysical Implications ALMA Long Baseline Campaign: Observations of the Strongly of the Binary Black Hole Merger GW150914, ApJ, 818, L22. Lensed Submillimeter Galaxy HATLAS J090311.6+003906 at z = Abbott, B. P., et al. including Flaminio, R., LIGO Scientific 3.042, ApJ, 808, L4. Collaboration, Virgo Collaboration: 2016, Observation of ALMA Partnership, et al. including Asaki, Y., Hirota, A., Nakanishi, Gravitational Waves from a Binary Black Hole Merger, Phys. Rev. K., Espada, D., Kameno, S., Sawada, T., Takahashi, S., Kurono, Lett., 116, 061102. Y., Tatematsu, K.: 2015, The 2014 ALMA Long Baseline Campaign: Abbott, B. P., et al. including Flaminio, R., LIGO Scientific Observations of Asteroid 3 Juno at 60 Kilometer Resolution, ApJ, Collaboration, Virgo Collaboration: 2016, GW150914: Implications 808, L2. for the Stochastic Gravitational-Wave Background from Binary Black Alonso-Herrero, A., et al. including Imanishi, M.: 2016, A mid-infrared Holes, Phys.
    [Show full text]
  • Report from the Dark Energy Task Force (DETF)
    Fermi National Accelerator Laboratory Fermilab Particle Astrophysics Center P.O.Box 500 - MS209 Batavia, Il l i noi s • 60510 June 6, 2006 Dr. Garth Illingworth Chair, Astronomy and Astrophysics Advisory Committee Dr. Mel Shochet Chair, High Energy Physics Advisory Panel Dear Garth, Dear Mel, I am pleased to transmit to you the report of the Dark Energy Task Force. The report is a comprehensive study of the dark energy issue, perhaps the most compelling of all outstanding problems in physical science. In the Report, we outline the crucial need for a vigorous program to explore dark energy as fully as possible since it challenges our understanding of fundamental physical laws and the nature of the cosmos. We recommend that program elements include 1. Prompt critical evaluation of the benefits, costs, and risks of proposed long-term projects. 2. Commitment to a program combining observational techniques from one or more of these projects that will lead to a dramatic improvement in our understanding of dark energy. (A quantitative measure for that improvement is presented in the report.) 3. Immediately expanded support for long-term projects judged to be the most promising components of the long-term program. 4. Expanded support for ancillary measurements required for the long-term program and for projects that will improve our understanding and reduction of the dominant systematic measurement errors. 5. An immediate start for nearer term projects designed to advance our knowledge of dark energy and to develop the observational and analytical techniques that will be needed for the long-term program. Sincerely yours, on behalf of the Dark Energy Task Force, Edward Kolb Director, Particle Astrophysics Center Fermi National Accelerator Laboratory Professor of Astronomy and Astrophysics The University of Chicago REPORT OF THE DARK ENERGY TASK FORCE Dark energy appears to be the dominant component of the physical Universe, yet there is no persuasive theoretical explanation for its existence or magnitude.
    [Show full text]
  • Analysis and Measurement of Horn Antennas for CMB Experiments
    Analysis and Measurement of Horn Antennas for CMB Experiments Ian Mc Auley (M.Sc. B.Sc.) A thesis submitted for the Degree of Doctor of Philosophy Maynooth University Department of Experimental Physics, Maynooth University, National University of Ireland Maynooth, Maynooth, Co. Kildare, Ireland. October 2015 Head of Department Professor J.A. Murphy Research Supervisor Professor J.A. Murphy Abstract In this thesis the author's work on the computational modelling and the experimental measurement of millimetre and sub-millimetre wave horn antennas for Cosmic Microwave Background (CMB) experiments is presented. This computational work particularly concerns the analysis of the multimode channels of the High Frequency Instrument (HFI) of the European Space Agency (ESA) Planck satellite using mode matching techniques to model their farfield beam patterns. To undertake this analysis the existing in-house software was upgraded to address issues associated with the stability of the simulations and to introduce additional functionality through the application of Single Value Decomposition in order to recover the true hybrid eigenfields for complex corrugated waveguide and horn structures. The farfield beam patterns of the two highest frequency channels of HFI (857 GHz and 545 GHz) were computed at a large number of spot frequencies across their operational bands in order to extract the broadband beams. The attributes of the multimode nature of these channels are discussed including the number of propagating modes as a function of frequency. A detailed analysis of the possible effects of manufacturing tolerances of the long corrugated triple horn structures on the farfield beam patterns of the 857 GHz horn antennas is described in the context of the higher than expected sidelobe levels detected in some of the 857 GHz channels during flight.
    [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]
  • Updated Design of the CMB Polarization Experiment Satellite Litebird
    Journal of Low Temperature Physics (2020) 199:1107–1117 https://doi.org/10.1007/s10909-019-02329-w Updated Design of the CMB Polarization Experiment Satellite LiteBIRD H. Sugai, et al. [full author details at the end of the article] Received: 30 August 2019 / Accepted: 26 December 2019 / Published online: 27 January 2020 © The Author(s) 2020 Abstract Recent developments of transition-edge sensors (TESs), based on extensive experi- ence in ground-based experiments, have been making the sensor techniques mature enough for their application on future satellite cosmic microwave background (CMB) polarization experiments. LiteBIRD is in the most advanced phase among such future satellites, targeting its launch in Japanese Fiscal Year 2027 (2027FY) with JAXA’s H3 rocket. It will accommodate more than 4000 TESs in focal planes of refective low-frequency and refractive medium-and-high-frequency telescopes in order to detect a signature imprinted on the CMB by the primordial gravitational waves predicted in cosmic infation. The total wide frequency coverage between 34 and 448 GHz enables us to extract such weak spiral polarization patterns through the precise subtraction of our Galaxy’s foreground emission by using spectral dif- ferences among CMB and foreground signals. Telescopes are cooled down to 5 K for suppressing thermal noise and contain polarization modulators with transmis- sive half-wave plates at individual apertures for separating sky polarization signals from artifcial polarization and for mitigating from instrumental 1/f noise. Passive cooling by using V-grooves supports active cooling with mechanical coolers as well as adiabatic demagnetization refrigerators. Sky observations from the second Sun– Earth Lagrangian point, L2, are planned for 3 years.
    [Show full text]
  • Arxiv:2006.06594V1 [Astro-Ph.CO]
    Mitigating the optical depth degeneracy using the kinematic Sunyaev-Zel'dovich effect with CMB-S4 1, 2, 2, 1, 3, 4, 5, 6, 5, 6, Marcelo A. Alvarez, ∗ Simone Ferraro, y J. Colin Hill, z Ren´eeHloˇzek, x and Margaret Ikape { 1Berkeley Center for Cosmological Physics, Department of Physics, University of California, Berkeley, CA 94720, USA 2Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA 3Department of Physics, Columbia University, New York, NY, USA 10027 4Center for Computational Astrophysics, Flatiron Institute, New York, NY, USA 10010 5Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto ON, M5S 3H4, Canada 6David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto ON, M5S 3H4, Canada The epoch of reionization is one of the major phase transitions in the history of the universe, and is a focus of ongoing and upcoming cosmic microwave background (CMB) experiments with im- proved sensitivity to small-scale fluctuations. Reionization also represents a significant contaminant to CMB-derived cosmological parameter constraints, due to the degeneracy between the Thomson- scattering optical depth, τ, and the amplitude of scalar perturbations, As. This degeneracy subse- quently hinders the ability of large-scale structure data to constrain the sum of the neutrino masses, a major target for cosmology in the 2020s. In this work, we explore the kinematic Sunyaev-Zel'dovich (kSZ) effect as a probe of reionization, and show that it can be used to mitigate the optical depth degeneracy with high-sensitivity, high-resolution data from the upcoming CMB-S4 experiment.
    [Show full text]
  • Dark Energy and CMB
    Dark Energy and CMB Conveners: S. Dodelson and K. Honscheid Topical Conveners: K. Abazajian, J. Carlstrom, D. Huterer, B. Jain, A. Kim, D. Kirkby, A. Lee, N. Padmanabhan, J. Rhodes, D. Weinberg Abstract The American Physical Society's Division of Particles and Fields initiated a long-term planning exercise over 2012-13, with the goal of developing the community's long term aspirations. The sub-group \Dark Energy and CMB" prepared a series of papers explaining and highlighting the physics that will be studied with large galaxy surveys and cosmic microwave background experiments. This paper summarizes the findings of the other papers, all of which have been submitted jointly to the arXiv. arXiv:1309.5386v2 [astro-ph.CO] 24 Sep 2013 2 1 Cosmology and New Physics Maps of the Universe when it was 400,000 years old from observations of the cosmic microwave background and over the last ten billion years from galaxy surveys point to a compelling cosmological model. This model requires a very early epoch of accelerated expansion, inflation, during which the seeds of structure were planted via quantum mechanical fluctuations. These seeds began to grow via gravitational instability during the epoch in which dark matter dominated the energy density of the universe, transforming small perturbations laid down during inflation into nonlinear structures such as million light-year sized clusters, galaxies, stars, planets, and people. Over the past few billion years, we have entered a new phase, during which the expansion of the Universe is accelerating presumably driven by yet another substance, dark energy. Cosmologists have historically turned to fundamental physics to understand the early Universe, successfully explaining phenomena as diverse as the formation of the light elements, the process of electron-positron annihilation, and the production of cosmic neutrinos.
    [Show full text]
  • Science from Litebird
    Prog. Theor. Exp. Phys. 2012, 00000 (27 pages) DOI: 10.1093=ptep/0000000000 Science from LiteBIRD LiteBIRD Collaboration: (Fran¸coisBoulanger, Martin Bucher, Erminia Calabrese, Josquin Errard, Fabio Finelli, Masashi Hazumi, Sophie Henrot-Versille, Eiichiro Komatsu, Paolo Natoli, Daniela Paoletti, Mathieu Remazeilles, Matthieu Tristram, Patricio Vielva, Nicola Vittorio) 8/11/2018 ............................................................................... The LiteBIRD satellite will map the temperature and polarization anisotropies over the entire sky in 15 microwave frequency bands. These maps will be used to obtain a clean measurement of the primordial temperature and polarization anisotropy of the cosmic microwave background in the multipole range 2 ` 200: The LiteBIRD sensitivity will be better than that of the ESA Planck satellite≤ by≤ at least an order of magnitude. This document summarizes some of the most exciting new science results anticipated from LiteBIRD. Under the conservatively defined \full success" criterion, LiteBIRD will 3 measure the tensor-to-scalar ratio parameter r with σ(r = 0) < 10− ; enabling either a discovery of primordial gravitational waves from inflation, or possibly an upper bound on r; which would rule out broad classes of inflationary models. Upon discovery, LiteBIRD will distinguish between two competing origins of the gravitational waves; namely, the quantum vacuum fluctuation in spacetime and additional matter fields during inflation. We also describe how, under the \extra success" criterion using data external to Lite- BIRD, an even better measure of r will be obtained, most notably through \delensing" and improved subtraction of polarized synchrotron emission using data at lower frequen- cies. LiteBIRD will also enable breakthrough discoveries in other areas of astrophysics. We highlight the importance of measuring the reionization optical depth τ at the cosmic variance limit, because this parameter must be fixed in order to allow other probes to measure absolute neutrino masses.
    [Show full text]
  • Rhodri Evans
    Rhodri Evans The Cosmic Microwave Background How It Changed Our Understanding of the Universe Astronomers’ Universe More information about this series at http://www.springer.com/series/6960 Rhodri Evans The Cosmic Microwave Background How It Changed Our Understanding of the Universe 123 Rhodri Evans School of Physics & Astronomy Cardiff University Cardiff United Kingdom ISSN 1614-659X ISSN 2197-6651 (electronic) ISBN 978-3-319-09927-9 ISBN 978-3-319-09928-6 (eBook) DOI 10.1007/978-3-319-09928-6 Springer Cham Heidelberg New York Dordrecht London Library of Congress Control Number: : 2014957530 © Springer International Publishing Switzerland 2015 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifically the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfilms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. Exempted from this legal reservation are brief excerpts in connection with reviews or scholarly analysis or material supplied specifically for the purpose of being entered and executed on a computer system, for exclusive use by the purchaser of the work. Duplication of this publication or parts thereof is permitted only under the provisions of the Copyright Law of the Publisher’s location, in its current version, and permission for use must always be obtained from Springer. Permissions for use may be obtained through RightsLink at the Copyright Clearance Center. Violations are liable to prosecution under the respective Copyright Law.
    [Show full text]
  • High Redshift Quasar Hunting with the Dark Energy Survey
    High Redshift Quasar Hunting with the Dark Energy Survey Quasars in the Epoch of Reionisation Sophie Reed Supervisors: Richard McMahon, Manda Banerji 1 Why? ★ Theories of black hole formation and evolution z = 6 - 15 z = 2 WORDS Epoch of peak of galaxy Reionization and quasar ★ Metal abundances in the early universe activity ★ Gas distribution and reionisationv z = 20 - 30 z = 6 - 8 Start of z = 1100 first stars Reionization matter-radiation “Population III” decoupling (CMB) 2 Quasar Spectrum at z ~ 6 Spectrum of a z = 5.86 quasar from Venemans et al 2007 Continuum break across rest frame Lyman-alpha (λrest = 121.6nm) gives distinctive colours 3 Quasar Spectrum at z ~ 6 480 nm 640 nm 780 nm 920 nm 990 nm 1252 nm 2147 nm 4 The Dark Energy Survey (DES) First Light September 2012 Very large area when completed: ~5000 deg2, currently have ~2000 deg2 Deep imaging: 10 σ limits for i and z are AB = 23.4 and AB = 23.2 Sophisticated camera, DECam Credit: DES Collaboration 5 DECam Mosaic of 62 2k by 4k CCDs (0.27” pixels) Multi waveband imaging: Visible (400 nm) to Near IR (1050 nm), g, r, i, z and Y bands covered Much more sensitive to red light than SDSS Credit: DES Collaboration 6 DES - SDSS Comparison SDSS was most sensitive to bluer light in the r band DES is most sensitive to redder light in the z band u g r i z Y 7 The VISTA Hemisphere Survey (VHS) Will cover 10,000 deg2 in the infrared when completed VHS-DES (J, H and K) overlaps DES and is deeper VHS-ATLAS (Y, J, H and K) is a shallower survey 8 Currently Known Objects Lots of quasars known
    [Show full text]
  • Macquarie University Researchonline
    Macquarie University ResearchOnline This is the published version of: Anand Sivaramakrishnan ; David Lafrenière ; K. E. Saavik Ford ; Barry McKernan ; Anthony Cheetham ; Alexandra Z. Greenbaum ; Peter G. Tuthill ; James P. Lloyd ; Michael J. Ireland ; René Doyon ; Mathilde Beaulieu ; André Martel ; Anton Koekemoer ; Frantz Martinache ; Peter Teuben " Non- redundant Aperture Masking Interferometry (AMI) and segment phasing with JWST-NIRISS," in Space telescopes and instrumentation 2012 : optical, infared, and millimeter wave 1-6 July 2012 Amsterdam, Netherlands, edited by Mark C. Clampin, Giovanni G. Fazio, Howard A. MacEwen, Jacobus M. Oschmann, Proceedings of SPIE Vol. 8442 (SPIE, Bellingham, WA, 2012) Article CID Number 84422S. Access to the published version: http://dx.doi.org/10.1117/12.925565 Copyright: Copyright 2012 Society of Photo Optical Instrumentation Engineers. One print or electronic copy may be made for personal use only. Systematic reproduction and distribution, duplication of any material in this paper for a fee or for commercial purposes, or modification of the content of the paper are prohibited. Non-Redundant Aperture Masking Interferometry (AMI) and Segment Phasing with JWST-NIRISS Anand Sivaramakrishnana,j, David Lafreni`ereb, K. E. Saavik Fordc,j,k, Barry McKernanc,j,k, Anthony Cheethamd, Alexandra Z. Greenbaume, Peter G. Tuthilld, James P. Lloydf, Michael J. Irelandg, Ren´eDoyonb, Mathilde Beaulieub, Andr´eMartela, Anton Koekemoera, Frantz Martinacheh, Peter Teubeni a Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, United States b D´epartement de Physique, Universit´ede Montr´eal,Montr´eal,Qc, H3C 3J7, Canada c Dept. of Science, Borough of Manhattan Community College, City University of New York, 199 Chambers Street, NY 10007 United States d School of Physics, University of Sydney, NSW 2006, Australia e Johns Hopkins University, Department of Physics & Astronomy, 366 Bloomberg Center, 3400 N.
    [Show full text]
  • Cosmology from Cosmic Shear and Robustness to Data Calibration
    DES-2019-0479 FERMILAB-PUB-21-250-AE Dark Energy Survey Year 3 Results: Cosmology from Cosmic Shear and Robustness to Data Calibration A. Amon,1, ∗ D. Gruen,2, 1, 3 M. A. Troxel,4 N. MacCrann,5 S. Dodelson,6 A. Choi,7 C. Doux,8 L. F. Secco,8, 9 S. Samuroff,6 E. Krause,10 J. Cordero,11 J. Myles,2, 1, 3 J. DeRose,12 R. H. Wechsler,1, 2, 3 M. Gatti,8 A. Navarro-Alsina,13, 14 G. M. Bernstein,8 B. Jain,8 J. Blazek,7, 15 A. Alarcon,16 A. Ferté,17 P. Lemos,18, 19 M. Raveri,8 A. Campos,6 J. Prat,20 C. Sánchez,8 M. Jarvis,8 O. Alves,21, 22, 14 F. Andrade-Oliveira,22, 14 E. Baxter,23 K. Bechtol,24 M. R. Becker,16 S. L. Bridle,11 H. Camacho,22, 14 A. Carnero Rosell,25, 14, 26 M. Carrasco Kind,27, 28 R. Cawthon,24 C. Chang,20, 9 R. Chen,4 P. Chintalapati,29 M. Crocce,30, 31 C. Davis,1 H. T. Diehl,29 A. Drlica-Wagner,20, 29, 9 K. Eckert,8 T. F. Eifler,10, 17 J. Elvin-Poole,7, 32 S. Everett,33 X. Fang,10 P. Fosalba,30, 31 O. Friedrich,34 E. Gaztanaga,30, 31 G. Giannini,35 R. A. Gruendl,27, 28 I. Harrison,36, 11 W. G. Hartley,37 K. Herner,29 H. Huang,38 E. M. Huff,17 D. Huterer,21 N. Kuropatkin,29 P. Leget,1 A. R. Liddle,39, 40, 41 J.
    [Show full text]