DOCSLIB.ORG

Crowdsourcing Quality Control for Dark Energy Survey Images

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Crowdsourcing Quality Control for Dark Energy Survey Images BNL-113170-2016-JA Crowdsourcing quality control for Dark Energy Survey images P. Melchior, E. Sheldon, A. Drlica-Wagner, E. S. Ryko, T. M. C. Abbott, F. B. Abdalla, S. Allam, A. Benoit-L´evy, D. Brooks, E. Buckley-Geer, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Crocce, C. B. D’Andrea, L. N. da Costal, S. Desait, P. Doel, A. E. Evrard, D. A. Finley, B. Flaugher, J. Frieman, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, K. Honscheid, D. J. James, M. Jarvisa, K. Kuehn, T. S. Lia, M. A. G. Maial, M. Marcha, J. L. Marshall, B. Nord, R. Ogando, A. A. Plazas, A. K. Romera, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, R. C. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, V. Vikram, A. R. Walker, W. Wester, Y. Zhang Submitted to Astronomy and Computing October 2016 Physics Department Brookhaven National Laboratory U.S. Department of Energy USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25) Notice: This manuscript has been authored by employees of Brookhaven Science Associates, LLC under Contract No. DE-SC0012704 with the U.S. Department of Energy. The publisher by accepting the manuscript for publication acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. DISCLAIMER 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, nor any of their contractors, subcontractors, or their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or any third party’s use or the results of such use of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or any agency thereof or its contractors or subcontractors. The views and opinions of authors expressed herein do not necessarily state or reflect those of the United States Government or any agency thereof. BNL-113170-2016-JA Crowdsourcing quality control for Dark Energy Survey images P. Melchiora,b, E. Sheldonc, A. Drlica-Wagnerd, E. S. Rykoffe,f, T. M. C. Abbottg, F. B. Abdallah,i, S. Allamd, A. Benoit-Levy´ j,h,k, D. Brooksh, E. Buckley-Geerd, A. Carnero Roselll,m, M. Carrasco Kindn,o, J. Carreterop,q, M. Croccep, C. B. D’Andrear,s, L. N. da Costal,m, S. Desait,u, P. Doelh, A. E. Evrardv,w, D. A. Finleyd, B. Flaugherd, J. Friemand,x, E. Gaztanagap, D. W. Gerdesw, D. Grueny,z, R. A. Gruendln,o, K. Honscheida,b, D. J. Jamesg, M. Jarvisaa, K. Kuehnab, T. S. Liac, M. A. G. Maial,m, M. Marchaa, J. L. Marshallac, B. Nordd, R. Ogandol,m, A. A. Plazasad, A. K. Romerae, E. Sanchezaf, V. Scarpined, I. Sevilla-Noarbeaf,n, R. C. Smithg, M. Soares-Santosd, E. Suchytaaa, M. E. C. Swansono, G. Tarlew, V. Vikramag, A. R. Walkerg, W. Westerd, Y. Zhangw aCenter for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA bDepartment of Physics, The Ohio State University, Columbus, OH 43210, USA cBrookhaven National Laboratory, Bldg 510, Upton, NY 11973, USA dFermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA eKavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA fSLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA gCerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile hDepartment of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK iDepartment of Physics and Electronics, Rhodes University, PO Box 94, Grahamstown, 6140, South Africa jCNRS, UMR 7095, Institut d’Astrophysique de Paris, F-75014, Paris, France kSorbonne Universit´es,UPMC Univ Paris 06, UMR 7095, Institut d’Astrophysique de Paris, F-75014, Paris, France lLaborat´orioInterinstitucional de e-Astronomia - LIneA, Rua Gal. Jos´eCristino 77, Rio de Janeiro, RJ - 20921-400, Brazil mObservat´orioNacional, Rua Gal. Jos´eCristino 77, Rio de Janeiro, RJ - 20921-400, Brazil nDepartment of Astronomy, University of Illinois, 1002 W. Green Street, Urbana, IL 61801, USA oNational Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA pInstitut de Ci`enciesde l’Espai, IEEC-CSIC, Campus UAB, Carrer de Can Magrans, s/n, 08193 Bellaterra, Barcelona, Spain qInstitut de F´ısicad’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra (Barcelona) Spain rInstitute of Cosmology & Gravitation, University of Portsmouth, Portsmouth, PO1 3FX, UK sSchool of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK tExcellence Cluster Universe, Boltzmannstr. 2, 85748 Garching, Germany uFaculty of Physics, Ludwig-Maximilians University, Scheinerstr. 1, 81679 Munich, Germany vDepartment of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA wDepartment of Physics, University of Michigan, Ann Arbor, MI 48109, USA xKavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA yMax Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, 85748 Garching, Germany zUniversit¨ats-Sternwarte, Fakult¨atf¨urPhysik, Ludwig-Maximilians Universit¨atM¨unchen, Scheinerstr. 1, 81679 M¨unchen, Germany aaDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA abAustralian Astronomical Observatory, North Ryde, NSW 2113, Australia acGeorge P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA adJet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA aeDepartment of Physics and Astronomy, Pevensey Building, University of Sussex, Brighton, BN1 9QH, UK afCentro de Investigaciones Energ´eticas,Medioambientales y Tecnol´ogicas(CIEMAT), Madrid, Spain agArgonne National Laboratory, 9700 South Cass Avenue, Lemont, IL 60439, USA Abstract We have developed a crowdsourcing web application for image quality control employed by the Dark Energy Survey. Dubbed the “DES exposure checker”, it renders science-grade images directly to a web browser and allows users to mark problematic features from a set of predefined classes. Users can also generate custom labels and thus help identify previously unknown problem classes. User reports are fed back to hardware and software experts to help mitigate and eliminate recognized issues. We report on the implementation of the application and our experience with its over 100 users, the majority of which are professional or prospective astronomers but not data management experts. We discuss aspects of user training and engagement, and demonstrate how problem reports have been pivotal to rapidly correct artifacts which would likely have been too subtle or infrequent to be recognized oth- erwise. We conclude with a number of important lessons learned, suggest possible improvements, and recommend this collective exploratory approach for future astronomical surveys or other extensive data sets with a sufficiently large user base. We also release open-source code of the web application and host an online demo version at http://des-exp-checker.pmelchior.net. Keywords: surveys, Information systems: Crowdsourcing, Human-centered computing: Collaborative filtering 1. Introduction The application, dubbed the “DES exposure checker”, is geared for a professional user base of several hundred scien- Large astronomical surveys produce vast amounts of data tists and seeks to identify flaws in the DES images that will be for increasingly demanding science applications. At the same used for most science analyses. Problems discovered with this time, the complexity of the instruments, operations, and the application can then be fixed in hardware or in subsequent data subsequent data analyses renders glitches and flaws inevitable, processing runs. Our approach ties in with other quality control particularly during the early phases of experiments. Thus, mech- efforts, which automatically analyze the latest exposures and anisms that facilitate the discovery and reporting of problems in flag cases of e.g. bad observing conditions (Honscheid et al., the data, whether they originate from unexpected instrumen- 2012; Diehl et al., 2014), and allow the inspection of final coad- tal behavior or insufficient treatment in software, are impor- ded data products, both images and object catalogs (Balbinot tant components of a data quality program. Due to the often et al., 2012). Our concept profits from the experience of a prior unexpected nature of these features, algorithmic approaches to ad hoc crowdsourcing effort in DES. During the so-called Sci- identify artifacts are generally infeasible and human inspection ence Verification phase in 2012, flaws in DES imaging have remains necessary. Human-generated reports can then be fed been identified by a small “eyeball squad”, whose reports were back to algorithm developers and hardware experts to mitigate relayed to DES operations and data management experts on a and eliminate
Load more

Recommended publications
  • 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]
  • 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]
  • 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]
  • 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]
  • Cosmic Visions Dark Energy: Science
    Cosmic Visions Dark Energy: Science Scott Dodelson, Katrin Heitmann, Chris Hirata, Klaus Honscheid, Aaron Roodman, UroˇsSeljak, Anˇze Slosar, Mark Trodden Executive Summary Cosmic surveys provide crucial information about high energy physics including strong evidence for dark energy, dark matter, and inflation. Ongoing and upcoming surveys will start to identify the underlying physics of these new phenomena, including tight constraints on the equation of state of dark energy, the viability of modified gravity, the existence of extra light species, the masses of the neutrinos, and the potential of the field that drove inflation. Even after the Stage IV experiments, DESI and LSST, complete their surveys, there will still be much information left in the sky. This additional information will enable us to understand the physics underlying the dark universe at an even deeper level and, in case Stage IV surveys find hints for physics beyond the current Standard Model of Cosmology, to revolutionize our current view of the universe. There are many ideas for how best to supplement and aid DESI and LSST in order to access some of this remaining information and how surveys beyond Stage IV can fully exploit this regime. These ideas flow to potential projects that could start construction in the 2020's. arXiv:1604.07626v1 [astro-ph.CO] 26 Apr 2016 2 1 Overview This document begins with a description of the scientific goals of the cosmic surveys program in x2 and then x3 presents the evidence that, even after the surveys currently planned for the 2020's, much of the relevant information in the sky will remain to be mined.
    [Show full text]
  • Arxiv:0910.5224V1 [Astro-Ph.CO] 27 Oct 2009
    Baryon Acoustic Oscillations Bruce A. Bassett 1,2,a & Ren´ee Hlozek1,2,3,b 1 South African Astronomical Observatory, Observatory, Cape Town, South Africa 7700 2 Department of Mathematics and Applied Mathematics, University of Cape Town, Rondebosch, Cape Town, South Africa 7700 3 Department of Astrophysics, University of Oxford Keble Road, Oxford, OX1 3RH, UK a [email protected] b [email protected] Abstract Baryon Acoustic Oscillations (BAO) are frozen relics left over from the pre-decoupling universe. They are the standard rulers of choice for 21st century cosmology, provid- ing distance estimates that are, for the first time, firmly rooted in well-understood, linear physics. This review synthesises current understanding regarding all aspects of BAO cosmology, from the theoretical and statistical to the observational, and includes a map of the future landscape of BAO surveys, both spectroscopic and photometric . † 1.1 Introduction Whilst often phrased in terms of the quest to uncover the nature of dark energy, a more general rubric for cosmology in the early part of the 21st century might also be the “the distance revolution”. With new knowledge of the extra-galactic distance arXiv:0910.5224v1 [astro-ph.CO] 27 Oct 2009 ladder we are, for the first time, beginning to accurately probe the cosmic expansion history beyond the local universe. While standard candles – most notably Type Ia supernovae (SNIa) – kicked off the revolution, it is clear that Statistical Standard Rulers, and the Baryon Acoustic Oscillations (BAO) in particular, will play an increasingly important role. In this review we cover the theoretical, observational and statistical aspects of the BAO as standard rulers and examine the impact BAO will have on our understand- † This review is an extended version of a chapter in the book Dark Energy Ed.
    [Show full text]
  • Dark Energy Survey Year 3 Results: Multi-Probe Modeling Strategy and Validation
    DES-2020-0554 FERMILAB-PUB-21-240-AE Dark Energy Survey Year 3 Results: Multi-Probe Modeling Strategy and Validation E. Krause,1, ∗ X. Fang,1 S. Pandey,2 L. F. Secco,2, 3 O. Alves,4, 5, 6 H. Huang,7 J. Blazek,8, 9 J. Prat,10, 3 J. Zuntz,11 T. F. Eifler,1 N. MacCrann,12 J. DeRose,13 M. Crocce,14, 15 A. Porredon,16, 17 B. Jain,2 M. A. Troxel,18 S. Dodelson,19, 20 D. Huterer,4 A. R. Liddle,11, 21, 22 C. D. Leonard,23 A. Amon,24 A. Chen,4 J. Elvin-Poole,16, 17 A. Fert´e,25 J. Muir,24 Y. Park,26 S. Samuroff,19 A. Brandao-Souza,27, 6 N. Weaverdyck,4 G. Zacharegkas,3 R. Rosenfeld,28, 6 A. Campos,19 P. Chintalapati,29 A. Choi,16 E. Di Valentino,30 C. Doux,2 K. Herner,29 P. Lemos,31, 32 J. Mena-Fern´andez,33 Y. Omori,10, 3, 24 M. Paterno,29 M. Rodriguez-Monroy,33 P. Rogozenski,7 R. P. Rollins,30 A. Troja,28, 6 I. Tutusaus,14, 15 R. H. Wechsler,34, 24, 35 T. M. C. Abbott,36 M. Aguena,6 S. Allam,29 F. Andrade-Oliveira,5, 6 J. Annis,29 D. Bacon,37 E. Baxter,38 K. Bechtol,39 G. M. Bernstein,2 D. Brooks,31 E. Buckley-Geer,10, 29 D. L. Burke,24, 35 A. Carnero Rosell,40, 6, 41 M. Carrasco Kind,42, 43 J. Carretero,44 F. J. Castander,14, 15 R.
    [Show full text]
  • Arxiv:2002.11464V1 [Physics.Gen-Ph] 13 Feb 2020 a Function of the Angles Θ and Φ in the Sky Is Shown in Fig
    Flat Space, Dark Energy, and the Cosmic Microwave Background Kevin Cahill Department of Physics and Astronomy University of New Mexico Albuquerque, New Mexico 87106 (Dated: February 27, 2020) This paper reviews some of the results of the Planck collaboration and shows how to compute the distance from the surface of last scattering, the distance from the farthest object that will ever be observed, and the maximum radius of a density fluctuation in the plasma of the CMB. It then explains how these distances together with well-known astronomical facts imply that space is flat or nearly flat and that dark energy is 69% of the energy of the universe. I. COSMIC MICROWAVE BACKGROUND RADIATION The cosmic microwave background (CMB) was predicted by Gamow in 1948 [1], estimated to be at a temperature of 5 K by Alpher and Herman in 1950 [2], and discovered by Penzias and Wilson in 1965 [3]. It has been observed in increasing detail by Roll and Wilkinson in 1966 [4], by the Cosmic Background Explorer (COBE) collaboration in 1989{1993 [5, 6], by the Wilkinson Microwave Anisotropy Probe (WMAP) collaboration in 2001{2013 [7, 8], and by the Planck collaboration in 2009{2019 [9{12]. The Planck collaboration measured CMB radiation at nine frequencies from 30 to 857 6 GHz by using a satellite at the Lagrange point L2 in the Earth's shadow some 1.5 10 km × farther from the Sun [11, 12]. Their plot of the temperature T (θ; φ) of the CMB radiation as arXiv:2002.11464v1 [physics.gen-ph] 13 Feb 2020 a function of the angles θ and φ in the sky is shown in Fig.
    [Show full text]
  • Dark Energy Survey Year 1 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing
    University of North Dakota UND Scholarly Commons Physics Faculty Publications Department of Physics & Astrophysics 8-27-2018 Dark Energy Survey year 1 results: Cosmological constraints from galaxy clustering and weak lensing T. M. C. Abbott F. B. Abdalla A. Alarcon J. Aleksic S. Allam See next page for additional authors Follow this and additional works at: https://commons.und.edu/pa-fac Part of the Astrophysics and Astronomy Commons, and the Physics Commons Recommended Citation Abbott, T. M. C.; Abdalla, F. B.; Alarcon, A.; Aleksic, J.; Allam, S.; Allen, S.; Amara, A.; Annis, J.; Asorey, J.; Avila, S.; Bacon, D.; Balbinot, E.; Banerji, M.; Banik, N.; and Barkhouse, Wayne, "Dark Energy Survey year 1 results: Cosmological constraints from galaxy clustering and weak lensing" (2018). Physics Faculty Publications. 13. https://commons.und.edu/pa-fac/13 This Article is brought to you for free and open access by the Department of Physics & Astrophysics at UND Scholarly Commons. It has been accepted for inclusion in Physics Faculty Publications by an authorized administrator of UND Scholarly Commons. For more information, please contact [email protected]. Authors T. M. C. Abbott, F. B. Abdalla, A. Alarcon, J. Aleksic, S. Allam, S. Allen, A. Amara, J. Annis, J. Asorey, S. Avila, D. Bacon, E. Balbinot, M. Banerji, N. Banik, and Wayne Barkhouse This article is available at UND Scholarly Commons: https://commons.und.edu/pa-fac/13 DES-2017-0226 FERMILAB-PUB-17-294-PPD Dark Energy Survey Year 1 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing T. M. C. Abbott,1 F.
    [Show full text]
  • The Dark Energy Survey Data Release 1, DES Collaboration
    DES-2017-0315 FERMILAB-PUB-17-603-AE-E DRAFT VERSION JANUARY 9, 2018 Typeset using LATEX twocolumn style in AASTeX61a THE DARK ENERGY SURVEY DATA RELEASE 1 T. M. C. ABBOTT,1 F. B. ABDALLA,2, 3 S. ALLAM,4 A. AMARA,5 J. ANNIS,4 J. ASOREY,6, 7, 8 S. AVILA,9, 10 O. BALLESTER,11 M. BANERJI,12, 13 W. BARKHOUSE,14 L. BARUAH,15 M. BAUMER,16, 17, 18 K. BECHTOL,19 M. R. BECKER,16, 17 A. BENOIT-LÉVY,20, 2, 21 G. M. BERNSTEIN,22 E. BERTIN,20, 21 J. BLAZEK,23, 24 S. BOCQUET,25 D. BROOKS,2 D. BROUT,22 E. BUCKLEY-GEER,4 D. L. BURKE,17, 18 V. BUSTI,26, 27 R. CAMPISANO,26 L. CARDIEL-SAS,11 A. CARNERO ROSELL,28, 26 M. CARRASCO KIND,29, 30 J. CARRETERO,11 F. J. CASTANDER,31, 32 R. CAWTHON,33 C. CHANG,33 C. CONSELICE,34 G. COSTA,26 M. CROCCE,31, 32 C. E. CUNHA,17 C. B. D’ANDREA,22 L. N. DA COSTA,26, 28 R. DAS,35 G. DAUES,29 T. M. DAVIS,7, 8 C. DAVIS,17 J. DE VICENTE,36 D. L. DEPOY,37 J. DEROSE,17, 16 S. DESAI,38 H. T. DIEHL,4 J. P. DIETRICH,39, 40 S. DODELSON,41 P. DOEL,2 A. DRLICA-WAGNER,4 T. F. EIFLER,42, 43 A. E. ELLIOTT,44 A. E. EVRARD,35, 45 A. FARAHI,35 A. FAUSTI NETO,26 E. FERNANDEZ,11 D. A. FINLEY,4 B. FLAUGHER,4 R. J. FOLEY,46 P.
    [Show full text]
  • Minutes of the Meeting of the Astronomy and Astrophysics Advisory Committee 20-21 September 2018
    Minutes of the Meeting of the Astronomy and Astrophysics Advisory Committee 20-21 September 2018 Members attending: Dieter Hartmann Rachel Bean John O’Meara (Chair) Andrew Connolly Kelsey Johnson Constance Rockosi Ian Dell’Antonio Mansi Kasliwal Eliza Kempton Shane Larson Agency personnel: Richard Green, NSF-AST Pedro Marronetti, NSF-PHY Diana Phan, NSF-AST Vladimir Papatashvili, NSF-Polar Chris Davis, NSF-AST James Ulvestad, NSF-OD Elizabeth Pentecost, NSF-AST R. Chris Smith, NSF-MPS OAD Richard Barvainis, NSF-AST Paul Hertz, NASA Matt Benacquista, NSF-AST Rita Sambruna, NASA Glen Langston, NSF-AST Evan Scannapieco, NASA Peter Kurczynski, NSF-AST Jim Green, NASA Joseph Pesce, NSF-AST Kartik Sheth, NASA Ken Johnston, NSF-AST Daniel Evans, NASA David Boboltz, NSF-AST Bill Latter, NASA Ralph Gaume, NSF-AST Terri Brandt, NASA Edward Ajhar, NSF-AST Kathy Turner, DOE James Neff, NSF-AST Eric Linder, DOE James Whitmore, NSF-PHY Drew Baden, DOE Jean Cottam Allen, NSF-PHY Others: Rachel Osten, STScI Kevin Stevenson, STScI Philip Puxley, AURA Scott Gaudi, OSU David Charbonneau, Harvard/CfA Peter Plavchan, George Mason U Steve Ritz, UCSC Alexey Vikhlinin, Harvard/CfA Lindsey Millken, Lewis-Burke Jeremy Weirich, AURA Michael Ledford, Lewis-Burke Marcia Smith Monty Di Biasi, SwRI Emily Gibson Sarah Lipscy, Ball Aerospace Wil Thomas Ben Kallen, Lewis-Burke Julianne Arnold Jeff Foust, Space News Mike Henry Ashlee Wilkins, AAS MEETING CONVENED 9:00 AM, 20 SEPTEMBER 2018 The Chair called the meeting to order and welcomed all new Committee members. Introductions were made. The minutes from the June 27, 2018 meeting were approved by the Committee.
    [Show full text]
  • The Dark Energy Survey
    The Dark Energy Survey • Aimed at precision measurements of Dark Energy • 5000 sq-degree 4-bandpass sky survey – g,r,i,z i=24, z=23.6 – Photometric redshifts for South Pole Telescope SZ cluster survey to z > 1. – Cluster counting via SZ, optical, WL – Weak lensing: shear-shear and shear-galaxy power spectra – Galaxy angular power spectra – SN light curves: 1 hour per night for 60 nights over 5 years • The Dark Energy Camera –CTIO 4m prime focus – 2 degree FOV corrector – 66 CCD, 500 megapixel focal plane array – Full depletion LBNL CCDs – ~500 nights over 5 years Jim Annis Fermilab The Dark Energy Survey • Physics of the Universe • NOAO Long Range Plan – “immediate priority is heavily weighted – CTIO 4m aimed at wide field imaging towards investigation of Dark Energy” • DOE Office of Science •CTIO – HEP performs experiments that explore – Announcement of opportunity the fundamental nature of matter, – Major instrumentation in return for up energy, space, and time, often leading to 30% telescope time over 5 years to the development of cutting edge technology – DOE teams most often centered at one of the National Labs, almost always • The System and Surveys including university-based researchers – 4m telescope: imaging surveys • Fermilab – 8m telescopes: spectroscopic surveys – Dark Matter: SDSS and CDMS – Experiment driven collaborations – Dark Energy: DES and JDEM provide instrumentation/software • DES collaboration – Surveys provide the best science for the – Fermilab, University of Illinois, most researchers at the least cost NOAO, NCSA, University of Chicago, LBNL, Carnegie Jim Annis Fermilab We aim at ~5% precision on Dark Energy Cluster Counting Weak Lensing Supernova w w w Ω Ω ΩM DE M δ w ~ 5% and δ ΩDE ~ 3% The Planck satellite will provide tighter input CMB measurements, and the constraints will improve slightly.
    [Show full text]