Sample records for kanareykin euclid techlabs

  1. TechLab

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    TechLab Inside the Museum Exhibitions Norris Bradbury Museum Lobby Defense Gallery Research Gallery History Gallery TechLab Virtual Exhibits invisible utility element TechLab...

  2. TechLab

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645U.S. DOE Office of ScienceandMesa del SolStrengthening a solidSynthesis of 2D AlloysTrails News Home | ORNL |TechLab

  3. EDITED--LS-332-DWA_FEL_August16

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    32 August 2012 A Compact Soft X-ray Free-Electron Laser Facility based on a Dielectric Wakefield Accelerator C. Jing, P. Schoessow, A. Kanareykin, Euclid Techlabs LLC, Solon, OH...

  4. Euclid Programming

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    Programming Programming Compiling and linking programs on Euclid. Compiling Codes How to compile and link MPI codes on Euclid. Read More Using the ACML Math Library How to...

  5. Euclid File Systems

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    File storage File storage Disk Quota Change Request Form Euclid File Systems Euclid has 3 kinds of file systems available to users: home directories, scratch directories and...

  6. Running jobs on Euclid

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    Running jobs Running jobs Overview and Basic Description Euclid is a single node system with 48 processors. It supports both multiprocessing (MPI) and multithreading programming...

  7. Compiling Codes on Euclid

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    Compiling Codes Compiling Codes Overview Open Mpi is the the only MPI library available on Euclid. This implementation of MPI-2 is described at Open MPI: Open Source High...

  8. Using the ACML Math Library on Euclid

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    ACML Math Library Using the ACML Math Library The AMD ACML math library is available on Euclid. This library is described at the ACML Math Library. To compile and link with it,...

  9. Cosmology and fundamental physics with the Euclid satellite

    E-Print Network [OSTI]

    Luca Amendola; Stephen Appleby; David Bacon; Tessa Baker; Marco Baldi; Nicola Bartolo; Alain Blanchard; Camille Bonvin; Stefano Borgani; Enzo Branchini; Clare Burrage; Stefano Camera; Carmelita Carbone; Luciano Casarini; Mark Cropper; Claudia deRham; Cinzia di Porto; Anne Ealet; Pedro G. Ferreira; Fabio Finelli; Juan Garcia-Bellido; Tommaso Giannantonio; Luigi Guzzo; Alan Heavens; Lavinia Heisenberg; Catherine Heymans; Henk Hoekstra; Lukas Hollenstein; Rory Holmes; Ole Horst; Knud Jahnke; Thomas D. Kitching; Tomi Koivisto; Martin Kunz; Giuseppe La Vacca; Marisa March; Elisabetta Majerotto; Katarina Markovic; David Marsh; Federico Marulli; Richard Massey; Yannick Mellier; David F. Mota; Nelson Nunes; Will Percival; Valeria Pettorino; Cristiano Porciani; Claudia Quercellini; Justin Read; Massimiliano Rinaldi; Domenico Sapone; Roberto Scaramella; Constantinos Skordis; Fergus Simpson; Andy Taylor; Shaun Thomas; Roberto Trotta; Licia Verde; Filippo Vernizzi; Adrian Vollmer; Yun Wang; Jochen Weller; Tom Zlosnik

    2012-06-06T23:59:59.000Z

    Euclid is a European Space Agency medium class mission selected for launch in 2019 within the Cosmic Vision 2015-2025 programme. The main goal of Euclid is to understand the origin of the accelerated expansion of the Universe. Euclid will explore the expansion history of the Universe and the evolution of cosmic structures by measuring shapes and redshifts of galaxies as well as the distribution of clusters of galaxies over a large fraction of the sky. Although the main driver for Euclid is the nature of dark energy, Euclid science covers a vast range of topics, from cosmology to galaxy evolution to planetary research. In this review we focus on cosmology and fundamental physics, with a strong emphasis on science beyond the current standard models. We discuss five broad topics: dark energy and modified gravity, dark matter, initial conditions, basic assumptions and questions of methodology in the data analysis. This review has been planned and carried out within Euclid's Theory Working Group and is meant to provide a guide to the scientific themes that will underlie the activity of the group during the preparation of the Euclid mission.

  10. The Euclid space-time diagram of the theory of relativity

    E-Print Network [OSTI]

    W. LiMing

    2014-06-03T23:59:59.000Z

    A conventional space-time diagram is $r-ct$ one, which satisfies the Minkowski geometry. This geometry conflict the intuition from the Euclid geometry. In this work an Euclid space-time diagram is proposed to describe relativistic world lines with an exact Euclid geometry. The relativistic effects such as the dilation of moving clocks, the contraction of moving length, and the twin paradox can be geometrically expressed in the Euclid space-time diagram. It is applied to the case of a satellite clock to correct the gravitational effect. It is found that this Euclid space-time diagram is much more intuitive than the conventional space-time diagram.

  11. Euclid Announcements

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  12. Euclid Programming

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  13. Euclid Timeline

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  14. Constraining neutrino properties with a Euclid-like galaxy cluster survey

    SciTech Connect (OSTI)

    Cerbolini, M. Costanzi Alunno; Sartoris, B.; Borgani, S. [Universitá di Trieste, Dipartimento di Fisica, via Valerio, 2, 34127 Trieste (Italy); Xia, Jun-Qing [Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Science, P.O.Box 918-3, Beijing 100049, P.R.China (China); Biviano, A.; Viel, M., E-mail: costanzi@oats.inaf.it, E-mail: sartoris@oats.inaf.it, E-mail: xiajq@ihep.ac.cn, E-mail: borgani@oats.inaf.it, E-mail: viel@oats.inaf.it, E-mail: biviano@oats.inaf.it [INAF-Osservatorio Astronomico di Trieste, via Tiepolo 11, 34143 Trieste (Italy)

    2013-06-01T23:59:59.000Z

    We perform a forecast analysis on how well a Euclid-like photometric galaxy cluster survey will constrain the total neutrino mass and effective number of neutrino species. We base our analysis on the Monte Carlo Markov Chains technique by combining information from cluster number counts and cluster power spectrum. We find that combining cluster data with Cosmic Microwave Background (CMB) measurements from Planck improves by more than an order of magnitude the constraint on neutrino masses compared to each probe used independently. For the ?CDM+m{sub ?} model the 2? upper limit on total neutrino mass shifts from ?m{sub ?} < 0.35 eV using cluster data alone to ?m{sub ?} < 0.031 eV when combined with Planck data. When a non-standard scenario with N{sub eff}?3.046 number of neutrino species is considered, we estimate an upper limit of N{sub eff} < 3.14 (95%CL), while the bounds on neutrino mass are relaxed to ?m{sub ?} < 0.040 eV. This accuracy would be sufficient for a 2? detection of neutrino mass even in the minimal normal hierarchy scenario (?m{sub ?} ? 0.05 eV). In addition to the extended ?CDM+m{sub ?}+N{sub eff} model we also consider scenarios with a constant dark energy equation of state and a non-vanishing curvature. When these models are considered the error on ?m{sub ?} is only slightly affected, while there is a larger impact of the order of ? 15% and ? 20% respectively on the 2? error bar of N{sub eff} with respect to the standard case. To assess the effect of an uncertain knowledge of the relation between cluster mass and optical richness, we also treat the ?CDM+m{sub ?}+N{sub eff} case with free nuisance parameters, which parameterize the uncertainties on the cluster mass determination. Adopting the over-conservative assumption of no prior knowledge on the nuisance parameter the loss of information from cluster number counts leads to a large degradation of neutrino constraints. In particular, the upper bounds for ?m{sub ?} are relaxed by a factor larger than two, ?m{sub ?} < 0.083 eV (95%CL), hence compromising the possibility of detecting the total neutrino mass with good significance. We thus confirm the potential that a large optical/near-IR cluster survey, like that to be carried out by Euclid, could have in constraining neutrino properties, and we stress the importance of a robust measurement of masses, e.g. from weak lensing within the Euclid survey, in order to full exploit the cosmological information carried by such survey.

  15. A new HST/Herschel deep field at the North Ecliptic Pole: preparing the way for JWST, SPICA and Euclid

    E-Print Network [OSTI]

    Serjeant, Stephen; Burgarella, Denis; Clements, Dave; De Zotti, Gianfranco; Goto, Tomo; Hatsukade, Bunyo; Hopwood, Rosalind; Hwang, Narae; Inami, Hanae; Jeong, Woong-Seob; Kim, Seong Jin; Krumpe, Mirko; Lee, Myung Gyoon; Malkan, Matt; Matsuhara, Hideo; Miyaji, Takamitsu; Oyabu, Shinki; Pearson, Chris; Takeuchi, Tsutomu; Vaccari, Mattia; Valtchanov, Ivan; van der Werf, Paul; Wada, Takehiko; White, Glenn

    2012-01-01T23:59:59.000Z

    We propose a co-ordinated multi-observatory survey at the North Ecliptic Pole. This field is the natural extragalactic deep field location for most space observatories (e.g. containing the deepest Planck, WISE and eROSITA data), is in the continuous viewing zones for e.g. Herschel, HST, JWST, and is a natural high-visibility field for the L2 halo orbit of SPICA with deep and wide-field legacy surveys already planned. The field is also a likely deep survey location for the forthcoming Euclid mission. It is already a multi-wavelength legacy field in its own right (e.g. AKARI, LOFAR, SCUBA-2): the outstanding and unparalleled continuous mid-IR photometric coverage in this field and nowhere else enables a wide range of galaxy evolution diagnostics unachievable in any other survey field, by spanning the wavelengths of redshifted PAH and silicate features and the peak energy output of AGN hot dust. We argue from the science needs of Euclid and JWST, and from the comparative multiwavelength depths, that the logical ...

  16. This book is compiled to provide a printer-friendly e-book for you who want to read Euclid's Elements in the original Greek language. The Greek text is borrowed from Perseus Digital Library 1

    E-Print Network [OSTI]

    Beligiannis, Apostolos

    Digital Library 1 and as for the drawings I have reproduced with a geometrical drawing language named on David Joyce's Euclid's Elements Web Page 3 . At the Perseus Digital Library each word is linked. But the digitalized version, and especially the morphological tools serviced on Perseus Digital Library are protected

  17. Process Limits on Euclid

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    Process Limits Process Limits Limit Hard Soft core file size (blocks) 0 unlimited data seg size (kbytes) unlimited unlimited scheduling priority 0 0 file size (blocks) unlimited...

  18. Compiling Codes on Euclid

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645 3,625govInstrumentstdmadapInactiveVisiting theCommercialization and Innovation2010 2010About Us >Effective

  19. Process Limits on Euclid

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645U.S. DOE Office of Science (SC)IntegratedSpeedingTechnical News, informationPriority FirmTechxx by ASME 31

  20. Running jobs on Euclid

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645U.S. DOE Office of Scienceand Requirements RecentlyElectronicResourcesjobs Running jobs Quick Instructions

  1. Getting Started on Euclid

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645U.S. DOE Office of Science (SC) Environmental AssessmentsGeoffrey(SC) Getting More ElectricityStarted

  2. Euclid Email Announcements Archive

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645U.S. DOE Office of Science (SC) Environmental Assessments (EA) /Email Announcements Archive Email Announcements

  3. Euclid File Systems

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645U.S. DOE Office of Science (SC) Environmental Assessments (EA) /Email Announcements Archive Email AnnouncementsFile

  4. Euclid Known Problems

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645U.S. DOE Office of Science (SC) Environmental Assessments (EA) /Email Announcements Archive EmailKnown Problems Known

  5. Euclid Software and Tools

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645U.S. DOE Office of Science (SC) Environmental Assessments (EA) /Email Announcements Archive EmailKnown

  6. Euclid Updates and Status

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645U.S. DOE Office of Science (SC) Environmental Assessments (EA) /Email Announcements Archive EmailKnownTimelineStatus

  7. LEES EUCLIDES! I Jan Hogendijk

    E-Print Network [OSTI]

    Hogendijk, Jan P.

    worden vergeleken, maar niet met elkaar worden vermenigvuldigd. In de rest van dit stuk zullen we af en

  8. Euclid Hardware and Software Configuration

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645U.S. DOE Office of Science (SC) Environmental Assessments (EA) /Email Announcements Archive Email

  9. ` Barbara R. Snyder 10900 Euclid Avenue

    E-Print Network [OSTI]

    Rollins, Andrew M.

    and the Nobel Prize-winning creator of the "bubble chamber" ­ a development essential for a series of subsequent ­ and a $10,000 prize. And, finally, Carbon Origins, designers of reusable rockets that carry science

  10. 1607 Matteo Ricci EuclidElements

    E-Print Network [OSTI]

    Siu, M.K.

    ;6 Thomas Jefferson, 1743-1826 (Bedini, 1990) ... Tacitus Thucydides (Jefferson, 1984) 1776 Declaration

  11. Euclid, Ohio: Energy Resources | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page onYou are now leaving Energy.gov You are now leaving Energy.gov You are beingZealand JumpConceptual Model,DOEHazelPennsylvania: Energy Resources(RECP) in DevelopingEtowah,

  12. Using the ACML Math Library on Euclid

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645U.S. DOE Office of ScienceandMesa del SolStrengthening aTurbulence mayUndergraduateAboutUserHadoopon-package memoryACML

  13. Euclid, NERSC's Sunfire Shared Memory Analytics System

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level: National5Sales for4,645U.S. DOE Office of Science (SC) Environmental Assessments (EA) /Email Announcements Archive EmailKnownTimelineStatus

  14. 2009 Update UCSF Planning Group GearyEuclid

    E-Print Network [OSTI]

    Lim, Wendell

    2727 Mariposa Street 19 3360 Geary Boulevard 20 250 Executive Park Boulevard 8 Hunters Point 9 Oyster

  15. PGI version 11.3 available on Euclid

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    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative1 First Use of Energy for All Purposes (Fuel and Nonfuel), 2002; Level:Energy: Grid Integration Redefining What's Possible for RenewableSpeedingBiomass and4/26/11: eliza18 emergency3 , 2

  16. South Euclid, Ohio: Energy Resources | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page onYou are now leaving Energy.gov You are now leaving Energy.gov YouKizildere IRaghuraji Agro Industries Pvt LtdShawangunk, NewSingaporeSonix Japan

  17. Virtual Exhibits

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    Virtual Exhibits Inside the Museum Exhibitions Norris Bradbury Museum Lobby Defense Gallery Research Gallery History Gallery TechLab Virtual Exhibits invisible utility element...

  18. HISTORY GALLERY

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    History Gallery Inside the Museum Exhibitions Norris Bradbury Museum Lobby Defense Gallery Research Gallery History Gallery TechLab Virtual Exhibits invisible utility element...

  19. Museum Lobby

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    Museum Lobby Inside the Museum Exhibitions Norris Bradbury Museum Lobby Defense Gallery Research Gallery History Gallery TechLab Virtual Exhibits invisible utility element Museum...

  20. Defense Gallery

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    Defense Gallery Inside the Museum Exhibitions Norris Bradbury Museum Lobby Defense Gallery Research Gallery History Gallery TechLab Virtual Exhibits invisible utility element...

  1. The State Energy Program Helps Promote that Bigger IS Better in Euclid, Ohio

    Broader source: Energy.gov [DOE]

    Highlighting how one Ohio-based manufacturer is saving energy and money through the Energy Department's State Energy Program.

  2. An intertextual study of Euclides Da Cunha's Os serto?es, R.B. Cunninghame Graham's A Brazilian mystic, and Mario Vargas Llosa's La guerra del fin del mundo 

    E-Print Network [OSTI]

    Erickson, Sandra Sassetti Fernandes

    1990-01-01T23:59:59.000Z

    known) fictions inspired by Q~~m. In" rr I fin I m n de Mario Vargas Llosa: un estudio transtextual, " Marcos Leopoldo Bernucci discussed a variety of texts used by Llosa in the writing of ~Lrr~. In this study Bernucci examined the relationship... American Case Studies, " and Marcos Leopoldo Bernucci, " ' de Mario Vargas Llosa: Un estudio transtextual. " , and is suggested in Llosa's text itself by Gall's phrenology, a major theme of Hegel's P~hn~m~~nlggy. Both in regard to ~~ and La~~rr we...

  3. An intertextual study of Euclides Da Cunha's Os serto?es, R.B. Cunninghame Graham's A Brazilian mystic, and Mario Vargas Llosa's La guerra del fin del mundo

    E-Print Network [OSTI]

    Erickson, Sandra Sassetti Fernandes

    1990-01-01T23:59:59.000Z

    . Newman Dr. Stephen J. Miller. L rr I fin I m n is not just a story about the saga of Canudos, but rather a "tree of stories, " composed of several metatexts telling that story. Structurally it illustrates two Hegelian themes, namely, the dialectics..., represents the achievement of historical consciousness in the Hegelian sense; at another level, ~~rr illustrates the full dialectical structure of its principal metatext, Quad~. DEDICATION To my parents, Lourdinha and Paulo Pires Fernandes, as a token...

  4. acid-assisted phosphine catalysis: Topics by E-print Network

    Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

    Washington University School of Medicine, 660 S. Euclid Avenue, St. Louis, MO 63110 Marshall, Garland R. 37 Catalytic Hydrogenolysis of Biphenylene with Platinum, Palladium,...

  5. SSL Workshop - Walmart

    Energy Savers [EERE]

    *Timeline *Euclid *Opportunities 2 "LEDs have become an integral part of our energy efficiency model for our stores and play a key role in achieving our overall sustainability...

  6. Alcune difficolt con il caro vecchio Teorema di Prospettive per una ricerca

    E-Print Network [OSTI]

    Spagnolo, Filippo

    razionale. L'ipotesi di Zeuthen ha avuto molta fortuna ed è stata ripresa dagli studiosi anche recentemente2 . La dimostrazione data da Euclide nella I,47 ebbe varia fortuna nella didattica del teorema di

  7. Increasing the transformer ratio at the Argonne wakefield accelerator.

    SciTech Connect (OSTI)

    Power, J.G.; Conde, M.; Liu, W.; Yusof, Z.; Gai, W.; Jing, C.; Kanareykin, A. (High Energy Physics); (Euclid Techlabs, LLC)

    2011-01-01T23:59:59.000Z

    The transformer ratio is defined as the ratio of the maximum energy gain of the witness bunch to the maximum energy loss experienced by the drive bunch (or a bunch within a multidrive bunch train). This plays an important role in the collinear wakefield acceleration scheme. A high transformer ratio is desirable since it leads to a higher overall efficiency under similar conditions (e.g. the same beam loading, the same structure, etc.). One technique to enhance the transformer ratio beyond the ordinary limit of 2 is to use a ramped bunch train. The first experimental demonstration observed a transformer ratio only marginally above 2 due to the mismatch between the drive microbunch length and the frequency of the accelerating structure [C. Jing, A. Kanareykin, J. Power, M. Conde, Z. Yusof, P. Schoessow, and W. Gai, Phys. Rev. Lett. 98, 144801 (2007)]. Recently, we revisited this experiment with an optimized microbunch length using a UV laser stacking technique at the Argonne Wakefield Accelerator facility and measured a transformer ratio of 3.4. Measurements and data analysis from these experiments are presented in detail.

  8. Introduzione In questo libretto sono illustrati i quesiti di informatica che sono stati

    E-Print Network [OSTI]

    Monga, Mattia

    5 1. Trettrerob`ot 6 2. Sul pianeta Alber 8 3. Euclide 10 4. Analisi grammaticale 12 5. Pseudo 2009 #12;Parte I. Quesiti nel volantino #12;Quesito 1: Trettrerob`ot Trettrerobot e in grado di corrispondere ad ogni porzione di frase un movi- mento di Trettrerobot: ad esempio A3 fa procedere il robot di 3

  9. New Book Information Crossroads in the History

    E-Print Network [OSTI]

    Sriraman, Bharath

    and for mathematics education courses aimed at teachers. CONTENTS: TOPICS IN HISTORY AND DIDACTICS OF CALCULUS infinitesimals and formal mathematical analysis, Mikhail Katz (Israel) & David Tall (UK). The didactical nature AND DIDACTICS OF GEOMETRY AND NUMBER. Euclid's Book on the Regular Solids: Its Place in the Elements and Its

  10. The activities of the Department are sup-ported by a combination of government

    E-Print Network [OSTI]

    projects funds from na- tional, international and EU programmes and fully commercial industrial contracts) Materials Science Materials Engineering Materials Technology Symposium EUCLID, EUREKA BRITE-EURAM, JOULE, EU$ Project funding 35.144.000 4.604.000 Government funding Income 34.988.000 4.583.000 Central Risø

  11. UNCORRECTED 2 Spall strength of a zirconium-based bulk metallic glass under

    E-Print Network [OSTI]

    Rollins, Andrew M.

    of Mechanical and Aerospace Engineering, Case Western Reserve University, 10900 Euclid Avenue, Glennan 616 B. Introduction 40 Bulk amorphous metals, also referred to as bulk metallic 41 glasses (BMG), are alloys in which super-cooling of a liquid 42 alloy produces a metastable phase, thus preventing forma- 43 tion

  12. Updated by Malana Bey 6/2013 Postbaccalaureate Research Education

    E-Print Network [OSTI]

    Yang, Sichun

    1 Updated by Malana Bey 6/2013 Postbaccalaureate Research Education Program (PREP) Scholar Handbook Education Program Office of Graduate Education, Ground floor TG-1 CWRU School of Medicine, 10900 Euclid://gradresed.meds.cwru.edu/PREP/index.html #12;2 Updated by Malana Bey 6/2013 Topic Table of Contents Page # Checklist ­ what to do when you

  13. 2001 The Society for the Study of Evolution. All rights reserved. Evolution, 55(12), 2001, pp. 25762600

    E-Print Network [OSTI]

    Cheverud, James M.

    structure relatively stable during evolutionary diversification of South American monkeys. Key words, 660 South Euclid Avenue, Campus Box 8108, Saint Louis, Missouri, 63110 5E-mail: cheverud habits. Finally, common patterns and levels of morphological integration are found among Plat- yrrhine

  14. SPARC Japan>> 20(2008)93()

    E-Print Network [OSTI]

    Hattori, Tetsuya

    2008-01-01T23:59:59.000Z

    1 SPARC Japan>> 20(2008)93() National Institute of Informatics 20(2008)93() RIMS 4 SPARC Japan 2008 SPARC JapanSPARC Japan UniBio Press J-STAGE Project Euclid SPARC Japan 3 (2000) ( 144 63 74 5 2 3 676 1 396 2 105 206 55 ISIJCRNCR 3,676 1,396 2,105 206

  15. MATERIALS RESEARCH DEPARTMENT 2000 A n n u a l R e p o r t 2 0 0 0

    E-Print Network [OSTI]

    MATERIALS RESEARCH DEPARTMENT 2000 35 A n n u a l R e p o r t 2 0 0 0 Finances Finances), 13% BRITE-EURAM, JOULE, EU-Fusion, 23% EUCLID,EUREKA, 5% Research areas (hours) Materials Science, 37% Materials Technology, 41% Materials engineering, 22% 36 501 000 DKK 4 551 000 USS 36 598 000 DKK 4 563 000

  16. Experimental and Molecular Pathology 71, 4054 (2001) doi:10.1006/exmp.2001.2380, available online at http://www.idealibrary.com on

    E-Print Network [OSTI]

    Burnstock, Geoffrey

    2001-01-01T23:59:59.000Z

    Experimental and Molecular Pathology 71, 40­54 (2001) doi:10.1006/exmp.2001.2380, available online, School of Medicine, Case Western Reserve University, 10900 Euclid Avenue, Cleveland, Ohio 44106 in humans and other animals (Verbeuren et al., 1986, macrophages and smooth muscle showed a different

  17. Reprint from the Bulletin of the Belgian Mathematical Society Simon Stevin Lagrangian submanifolds in 3-dimensional

    E-Print Network [OSTI]

    Li, Haizhong

    of Project Euclid (Cornell University Library), an aggregation of electronic journals. It is available online classification of the Lagrangian submanifolds in 3-dimensional complex space forms with isotropic cubic tensor. 1 Mathematics Subject Classification : Primary 53C20; Secondary 53C42. Key words and phrases : Lagrangian

  18. This article appeared in a journal published by Elsevier. The attached copy is furnished to the author for internal non-commercial research

    E-Print Network [OSTI]

    Simon, Dan

    maintenance schedules. Reliable health eval- uations are used to anticipate future maintenance needs.elsevier.com/locate/aescte A comparison of filtering approaches for aircraft engine health estimation Dan Simon Cleveland State University, Department of Electrical Engineering, Stilwell Hall Room 332, 2121 Euclid Avenue, Cleveland, OH 44115, USA

  19. ADAPTIVE FILTERING FOR DETECTING MYOCARDIAL INFARCTION USING NONINVASIVE CONDUCTING POLYMER COMPOSITE SENSORS

    E-Print Network [OSTI]

    Simon, Dan

    , is the leading cause of death among firefighters in the United States [1]. The need to carry heavy equipment long) (1) (3) (1) (1) Cleveland State University, 2121 Euclid Ave, Cleveland, Ohio 44115 (2) Arcon software produces a diagnostic-friendly ECG signal and then determines the patient's heart rate. When

  20. Probing Neutrino Hierarchy and Chirality via Wakes

    E-Print Network [OSTI]

    Hong-Ming Zhu; Ue-Li Pen; Xuelei Chen; Derek Inman

    2014-12-04T23:59:59.000Z

    The relic neutrinos are expected to acquire a bulk relative velocity with respect to the dark matter at low redshifts, and downstream of dark matter halos neutrino wakes are expected to develop. We propose a method of measuring the neutrino mass based on this mechanism. The neutrino wake will cause a dipole distortion of the galaxy-galaxy lensing pattern. This effect could be detected by combining upcoming lensing surveys, e.g. the LSST and Euclid surveys with a low redshift galaxy survey or a 21cm intensity mapping survey which can map the neutrino flow field. The data obtained with LSST and Euclid should enable us to make positive detection if the three neutrino masses are Quasi-Degenerate, and a future high precision 21cm lensing survey would allow the normal hierarchy and inverted hierarchy cases to be distinguished, and even the right handed Dirac neutrinos may be detectable.

  1. Aquifer behavior with reinjection 

    E-Print Network [OSTI]

    Bonet, Euclides Jose

    1967-01-01T23:59:59.000Z

    AQUIFER BEHAVIOR WITH REINJECTION A Thesis By EUCLIDES JOSE BONET Submitted to the Graduate College of the Texas ARUM University in partial fulfillment of the requirements for the degree of MASTER OF SCIENCE May, f967 Major Subject... Petroleum Engineering AQUIFER BEHAVIOR WITH REINJECTION A Thesis By E UC LI DES JOSE BONE T Approved as to style and content by: (Chairman of Committee) (Member) (Member) May, 1967 ACKNOWLEDGMENT Thanks are due to Petroleo Brasilerio S...

  2. A Life in Letters: Personal Essays

    E-Print Network [OSTI]

    Fangman, Ellen Mary

    2008-12-16T23:59:59.000Z

    on the battlefield, while I waged a different kind of warfare as I struggled with growing into a woman’s body. This essay is a sort of loving “slap in the face” at the men who knew nothing of what it meant to carry a tampon and bleed over miles of mountainous... these oft- feeble, oft-boisterous people we call our “selves.” In humorous tones, I write to Edna St. Vincent Millay, asking her to intercede for me with her favorite geometrician, Euclid, that I might be relieved of a recurring nightmare that involves...

  3. Beyond the plane-parallel and Newtonian approach: wide-angle redshift distortions and convergence in general relativity

    SciTech Connect (OSTI)

    Bertacca, Daniele; Maartens, Roy [Physics Department, University of the Western Cape, Cape Town 7535 (South Africa); Raccanelli, Alvise [Jet Propulsion Laboratory, California Institute of Technology, Pasadena CA 91109 (United States); Clarkson, Chris, E-mail: daniele.bertacca@pd.infn.it, E-mail: Roy.Maartens@port.ac.uk, E-mail: Alvise@caltech.edu, E-mail: Clarkson@maths.uct.ac.za [Centre for Astrophysics, Cosmology and Gravitation and Department of Mathematics and Applied Mathematics, University of Cape Town, Cape Town 7701 (South Africa)

    2012-10-01T23:59:59.000Z

    We extend previous analyses of wide-angle correlations in the galaxy power spectrum in redshift space to include all general relativistic effects. These general relativistic corrections to the standard approach become important on large scales and at high redshifts, and they lead to new terms in the wide-angle correlations. We show that in principle the new terms can produce corrections of nearly 10% on Gpc scales over the usual Newtonian approximation. General relativistic corrections will be important for future large-volume surveys such as SKA and Euclid, although the problem of cosmic variance will present a challenge in observing this.

  4. Future cosmological sensitivity for hot dark matter axions

    E-Print Network [OSTI]

    Archidiacono, Maria; Hamann, Jan; Hannestad, Steen; Raffelt, Georg; Wong, Yvonne Y Y

    2015-01-01T23:59:59.000Z

    We study the potential of a future, large-volume photometric survey to constrain the axion mass $m_a$ in the hot dark matter limit. Future surveys such as Euclid will have significantly more constraining power than current observations for hot dark matter. Nonetheless, the lowest accessible axion masses are limited by the fact that axions lighter than $\\sim 0.15$ eV decouple before the QCD epoch, assumed here to occur at a temperature $T_{\\rm QCD} \\sim 170$ MeV; this leaves an axion population of such low density that its late-time cosmological impact is negligible. For larger axion masses, $m_a \\gtrsim 0.15$ eV, where axions remain in equilibrium until after the QCD phase transition, we find that a Euclid-like survey combined with Planck CMB data can detect $m_a$ at very high significance. Our conclusions are robust against assumptions about prior knowledge of the neutrino mass. Given that the proposed IAXO solar axion search is sensitive to $m_a\\lesssim 0.2$ eV, the axion mass range probed by cosmology is n...

  5. Recovery of fluctuation spectrum evolution from tomographic shear spectra

    SciTech Connect (OSTI)

    Bonometto, Silvio A.; Mezzetti, Marino, E-mail: bonometto@oats.inaf.it, E-mail: mezzetti@oats.inaf.it [Department of Physics, Astronomy Unit, Trieste University, Via Tiepolo 11, I 34143 Trieste (Italy)

    2013-05-01T23:59:59.000Z

    Forthcoming large angle surveys are planned to obtain high precision tomographic shear data. In principle, they will allow us to recover the spectra of matter density fluctuation, at various redshift, through the inversion of the expressions yielding shear spectra from fluctuation spectra. This was discussed in previous work, where SVD techniques for matrix inversion were also shown to be the optimal tool to this aim. Here we show the significant improvements obtainable by using a 7 bin tomography, as allowed by future Euclid data, and discuss error propagation from shear to fluctuation spectra. We find that the technique is a promising tool, namely for the analysis of baryon physics through high–l shear spectra and to test the consistency between expansion rate and fluctuation growth.

  6. Constraining primordial magnetic fields with future cosmic shear surveys

    SciTech Connect (OSTI)

    Fedeli, C. [Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611 (United States); Moscardini, L., E-mail: cosimo.fedeli@astro.ufl.edu, E-mail: lauro.moscardini@unibo.it [Dipartimento di Astronomia, Università di Bologna, Via Ranzani 1, 40127 Bologna (Italy)

    2012-11-01T23:59:59.000Z

    The origin of astrophysical magnetic fields observed in galaxies and clusters of galaxies is still unclear. One possibility is that primordial magnetic fields generated in the early Universe provide seeds that grow through compression and turbulence during structure formation. A cosmological magnetic field present prior to recombination would produce substantial matter clustering at intermediate/small scales, on top of the standard inflationary power spectrum. In this work we study the effect of this alteration on one particular cosmological observable, cosmic shear. We adopt the semi-analytic halo model in order to describe the non-linear clustering of matter, and feed it with the altered mass variance induced by primordial magnetic fields. We find that the convergence power spectrum is, as expected, substantially enhanced at intermediate/small angular scales, with the exact amplitude of the enhancement depending on the magnitude and power-law index of the magnetic field power spectrum. Specifically, for a fixed amplitude, the effect of magnetic fields is larger for larger spectral indices. We use the predicted statistical errors for a future wide-field cosmic shear survey, on the model of the ESA Cosmic Vision mission Euclid, in order to forecast constraints on the amplitude of primordial magnetic fields as a function of the spectral index. We find that the amplitude will be constrained at the level of ? 0.1 nG for n{sub B} ? ?3, and at the level of ? 10{sup ?7} nG for n{sub B} ? 3. The latter is at the same level of lower bounds coming from the secondary emission of gamma-ray sources, implying that for high spectral indices Euclid will certainly be able to detect primordial magnetic fields, if they exist. The present study shows how large-scale structure surveys can be used for both understanding the origins of astrophysical magnetic fields and shedding new light on the physics of the pre-recombination Universe.

  7. Systematic errors in the measurement of neutrino masses due to baryonic feedback processes: Prospects for stage IV lensing surveys

    E-Print Network [OSTI]

    Aravind Natarajan; Andrew R. Zentner; Nicholas Battaglia; Hy Trac

    2014-09-04T23:59:59.000Z

    We examine the importance of baryonic feedback effects on the matter power spectrum on small scales, and the implications for the precise measurement of neutrino masses through gravitational weak lensing. Planned large galaxy surveys such as the Large Synoptic Sky Telescope (LSST) and Euclid are expected to measure the sum of neutrino masses to extremely high precision, sufficient to detect non-zero neutrino masses even in the minimal mass normal hierarchy. We show that weak lensing of galaxies while being a very good probe of neutrino masses, is extremely sensitive to baryonic feedback processes. We use publicly available results from the Overwhelmingly Large Simulations (OWLS) project to investigate the effects of active galactic nuclei feedback, the nature of the stellar initial mass function, and gas cooling rates, on the measured weak lensing shear power spectrum. Using the Fisher matrix formalism and priors from CMB+BAO data, we show that when one does not account for feedback, the measured neutrino mass may be substantially larger or smaller than the true mass, depending on the dominant feedback mechanism, with the mass error |\\Delta m_nu| often exceeding the mass m_nu itself. We also consider gravitational lensing of the cosmic microwave background (CMB) and show that it is not sensitive to baryonic feedback on scales l < 2000, although CMB experiments that aim for sensitivities sigma(m_nu) < 0.02 eV will need to include baryonic effects in modeling the CMB lensing potential. A combination of CMB lensing and galaxy lensing can help break the degeneracy between neutrino masses and baryonic feedback processes. We conclude that future large galaxy lensing surveys such as LSST and Euclid can only measure neutrino masses accurately if the matter power spectrum can be measured to similar accuracy.

  8. Testing a phenomenologically extended DGP model with upcoming weak lensing surveys

    SciTech Connect (OSTI)

    Camera, Stefano; Diaferio, Antonaldo [Dipartimento di Fisica Generale ''A. Avogadro'', Università di Torino, via P. Giuria 1, 10125 Torino (Italy); Cardone, Vincenzo F., E-mail: camera@ph.unito.it, E-mail: diaferio@ph.unito.it, E-mail: winnyenodrac@gmail.com [Dipartimento di Scienze e Tecnologie per l'Ambiente e il Territorio, Università degli Studi del Molise, Contrada Fonte Lappone, 86090 Pesche (Italy)

    2011-01-01T23:59:59.000Z

    A phenomenological extension of the well-known brane-world cosmology of Dvali, Gabadadze and Porrati (eDGP) has recently been proposed. In this model, a cosmological-constant-like term is explicitly present as a non-vanishing tension ? on the brane, and an extra parameter ? tunes the cross-over scale r{sub c}, the scale at which higher dimensional gravity effects become non negligible. Since the Hubble parameter in this cosmology reproduces the same ?CDM expansion history, we study how upcoming weak lensing surveys, such as Euclid and DES (Dark Energy Survey), can confirm or rule out this class of models. We perform Monte Carlo Markov Chain simulations to determine the parameters of the model, using Type Ia Supernovæ, H(z) data, Gamma Ray Bursts and Baryon Acoustic Oscillations. We also fit the power spectrum of the temperature anisotropies of the Cosmic Microwave Background to obtain the correct normalisation for the density perturbation power spectrum. Then, we compute the matter and the cosmic shear power spectra, both in the linear and non-linear régimes. The latter is calculated with the two different approaches of Hu and Sawicki (2007) (HS) and Khoury and Wyman (2009) (KW). With the eDGP parameters coming from the Markov Chains, KW reproduces the ?CDM matter power spectrum at both linear and non-linear scales and the ?CDM and eDGP shear signals are degenerate. This result does not hold with the HS prescription. Indeed, Euclid can distinguish the eDGP model from ?CDM because their expected power spectra roughly differ by the 3? uncertainty in the angular scale range 700?

  9. Constraining primordial non-Gaussianity with cosmological weak lensing: shear and flexion

    SciTech Connect (OSTI)

    Fedeli, C. [Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611-2055 (United States); Bartelmann, M. [Zentrum für Astronomie, Universität Heidelberg, Albert-Überle-Straße 2, 69120 Heidelberg (Germany); Moscardini, L., E-mail: cosimo.fedeli@astro.ufl.edu, E-mail: bartelmann@uni-heidelberg.de, E-mail: lauro.moscardini@unibo.it [Dipartimento di Astronomia, Università di Bologna, Via Ranzani 1, 40127 Bologna (Italy)

    2012-10-01T23:59:59.000Z

    We examine the cosmological constraining power of future large-scale weak lensing surveys on the model of the ESA planned mission Euclid, with particular reference to primordial non-Gaussianity. Our analysis considers several different estimators of the projected matter power spectrum, based on both shear and flexion. We review the covariance and Fisher matrix for cosmic shear and evaluate those for cosmic flexion and for the cross-correlation between the two. The bounds provided by cosmic shear alone are looser than previously estimated, mainly due to the reduced sky coverage and background number density of sources for the latest Euclid specifications. New constraints for the local bispectrum shape, marginalized over ?{sub 8}, are at the level of ?f{sub NL} ? 100, with the precise value depending on the exact multipole range that is considered in the analysis. We consider three additional bispectrum shapes, for which the cosmic shear constraints range from ?f{sub NL} ? 340 (equilateral shape) up to ?f{sub NL} ? 500 (orthogonal shape). Also, constraints on the level of non-Gaussianity and on the amplitude of the matter power spectrum ?{sub 8} are almost perfectly anti-correlated, except for the orthogonal bispectrum shape for which they are correlated. The competitiveness of cosmic flexion constraints against cosmic shear ones depends by and large on the galaxy intrinsic flexion noise, that is still virtually unconstrained. Adopting the very high value that has been occasionally used in the literature results in the flexion contribution being basically negligible with respect to the shear one, and for realistic configurations the former does not improve significantly the constraining power of the latter. Since the shear shot noise is white, while the flexion one decreases with decreasing scale, by considering high enough multipoles the two contributions have to become comparable. Extending the analysis up to l{sub max} = 20,000 cosmic flexion, while being still subdominant, improves the shear constraints by ? 10% when added. However on such small scales the highly non-linear clustering of matter, the impact of baryonic physics, and the non-Gaussian part of the covariance matrix make any error estimation uncertain. By considering lower, and possibly more realistic, values of the flexion intrinsic shape noise results in flexion constraining power being a factor of ? 2 better than that of shear, and the bounds on ?{sub 8} and f{sub NL} being improved by a factor of ? 3 upon their combination.

  10. Accounting for baryonic effects in cosmic shear tomography: Determining a minimal set of nuisance parameters using PCA

    SciTech Connect (OSTI)

    Eifler, Tim; Krause, Elisabeth; Dodelson, Scott; Zentner, Andrew; Hearin, Andrew; Gnedin, Nickolay

    2014-05-28T23:59:59.000Z

    Systematic uncertainties that have been subdominant in past large-scale structure (LSS) surveys are likely to exceed statistical uncertainties of current and future LSS data sets, potentially limiting the extraction of cosmological information. Here we present a general framework (PCA marginalization) to consistently incorporate systematic effects into a likelihood analysis. This technique naturally accounts for degeneracies between nuisance parameters and can substantially reduce the dimension of the parameter space that needs to be sampled. As a practical application, we apply PCA marginalization to account for baryonic physics as an uncertainty in cosmic shear tomography. Specifically, we use CosmoLike to run simulated likelihood analyses on three independent sets of numerical simulations, each covering a wide range of baryonic scenarios differing in cooling, star formation, and feedback mechanisms. We simulate a Stage III (Dark Energy Survey) and Stage IV (Large Synoptic Survey Telescope/Euclid) survey and find a substantial bias in cosmological constraints if baryonic physics is not accounted for. We then show that PCA marginalization (employing at most 3 to 4 nuisance parameters) removes this bias. Our study demonstrates that it is possible to obtain robust, precise constraints on the dark energy equation of state even in the presence of large levels of systematic uncertainty in astrophysical processes. We conclude that the PCA marginalization technique is a powerful, general tool for addressing many of the challenges facing the precision cosmology program.

  11. 4MOST - 4-metre Multi-Object Spectroscopic Telescope

    E-Print Network [OSTI]

    de Jong, Roelof S; Chiappini, Cristina; Depagne, Éric; Haynes, Roger; Johl, Diane; Schnurr, Olivier; Schwope, Axel; Walcher, Jakob; Dionies, Frank; Haynes, Dionne; Kelz, Andreas; Kitaura, Francisco S; Lamer, Georg; Minchev, Ivan; Müller, Volker; Nuza, Sebastián E; Olaya, Jean-Christophe; Piffl, Tilmann; Popow, Emil; Steinmetz, Matthias; Ural, U?ur; Williams, Mary; Winkler, Roland; Wisotzki, Lutz; Ansorgb, Wolfgang R; Banerji, Manda; Solares, Eduardo Gonzalez; Irwin, Mike; Kennicutt, Robert C; King, David; McMahon, Richard; Koposov, Sergey; Parry, Ian R; Walton, Nicholas A; Finger, Gert; Iwert, Olaf; Krumpe, Mirko; Lizon, Jean-Louis; Vincenzo, Mainieri; Amans, Jean-Philippe; Bonifacio, Piercarlo; Cohen, Mathieu; Francois, Patrick; Jagourel, Pascal; Mignot, Shan B; Royer, Frédéric; Sartoretti, Paola; Bender, Ralf; Grupp, Frank; Hess, Hans-Joachim; Lang-Bardl, Florian; Muschielok, Bernard; Böhringer, Hans; Boller, Thomas; Bongiorno, Angela; Brusa, Marcella; Dwelly, Tom; Merloni, Andrea; Nandra, Kirpal; Salvato, Mara; Pragt, Johannes H; Navarro, Ramón; Gerlofsma, Gerrit; Roelfsema, Ronald; Dalton, Gavin B; Middleton, Kevin F; Tosh, Ian A; Boeche, Corrado; Caffau, Elisabetta; Christlieb, Norbert; Grebel, Eva K; Hansen, Camilla; Koch, Andreas; Ludwig, Hans-G; Quirrenbach, Andreas; Sbordone, Luca; Seifert, Walter; Thimm, Guido; Trifonov, Trifon; Helmi, Amina; Trager, Scott C; Feltzing, Sofia; Korn, Andreas; Boland, Wilfried

    2012-01-01T23:59:59.000Z

    The 4MOST consortium is currently halfway through a Conceptual Design study for ESO with the aim to develop a wide-field (>3 square degree, goal >5 square degree), high-multiplex (>1500 fibres, goal 3000 fibres) spectroscopic survey facility for an ESO 4m-class telescope (VISTA). 4MOST will run permanently on the telescope to perform a 5 year public survey yielding more than 20 million spectra at resolution R~5000 ({\\lambda}=390-1000 nm) and more than 2 million spectra at R~20,000 (395-456.5 nm & 587-673 nm). The 4MOST design is especially intended to complement three key all-sky, space-based observatories of prime European interest: Gaia, eROSITA and Euclid. Initial design and performance estimates for the wide-field corrector concepts are presented. We consider two fibre positioner concepts, a well-known Phi-Theta system and a new R-Theta concept with a large patrol area. The spectrographs are fixed configuration two-arm spectrographs, with dedicated spectrographs for the high- and low-resolution. A ful...

  12. Do we need model-dependent covariances when we test cosmological models with galaxy power spectra?

    E-Print Network [OSTI]

    Kalus, B; Samushia, L

    2015-01-01T23:59:59.000Z

    We consider the shape of the posterior distribution to be used when fitting cosmological models to power spectra measured from galaxy surveys. At very large scales, Gaussian posterior distributions in the power do not approximate the posterior distribution $\\mathcal P_R$ we expect for a Gaussian density field $\\delta_\\mathbf{k}$, even if we vary the covariance matrix according to the model to be tested. We compare alternative posterior distributions with $\\mathcal P_R$, both mode-by-mode and in terms of expected $f_\\mathrm{NL}$-measurements. Marginalising over a Gaussian posterior distribution $\\mathcal P_f$ with fixed covariance matrix yields a posterior mean value of $f_\\mathrm{NL}$ which, for a data set with the characteristics of Euclid, will be underestimated by $\\triangle f_\\mathrm{NL}=0.4$, while for the data release 9 (DR9) of the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS) it will be underestimated by $\\triangle f_\\mathrm{NL}=19.1$. The inverse cubic normal dist...

  13. Cosmological tests of modified gravity: constraints on $F(R)$ theories from the galaxy clustering ratio

    E-Print Network [OSTI]

    Julien Bel; Philippe Brax; Christian Marinoni; Patrick Valageas

    2015-04-23T23:59:59.000Z

    The clustering ratio $\\eta$, a large-scale structure observable originally designed to constrain the shape of the power spectrum of matter density fluctuations, is shown to provide a sensitive probe of the nature of gravity in the cosmological regime. We apply this analysis to $F(R)$ theories of gravity using the luminous red galaxy (LRG) sample extracted from the spectroscopic Sloan Digital Sky Survey (SDSS) data release 7 and 10 catalogues. We find that General Relativity (GR), complemented with a Friedmann-Robertson-Walker (FRW) cosmological model with parameters fixed by the Planck satellite, describes extremely well the clustering of galaxies up to $z\\sim 0.6$. On large cosmic scales, the absolute amplitude of deviations from GR, $|f_{R_0 }|$, is constrained to be smaller than $4.6 \\times 10^{-5}$ at the $95\\%$ confidence level. This bound makes cosmological probes of gravity almost competitive with the sensitivity of Solar System tests, although still one order of magnitude less effective than astrophysical tests. We also extrapolate our results to future large surveys like Euclid and show that the astrophysical bound will certainly remain out of reach for such a class of modified-gravity models that only differ from $\\Lambda$CDM at low redshifts.

  14. I. Apples to apples $A^2$: photometric redshift predictions for next-generation surveys

    E-Print Network [OSTI]

    Ascaso, Begoña; Benítez, Narciso

    2015-01-01T23:59:59.000Z

    This is the first of a series of papers where we compare the expected performance of two of the largest stage IV next-generation surveys in the optical and infrared (LSST and Euclid), with a particular focus on cluster surveys. In this first paper, we introduce the mock catalogues we have utilized in this work, an N-body simulation+semi-analytical cone with a posterior modification with PhotReal, a technique which modifies the original photometry to make it more realistic by using an empirical library of spectral templates. We have confirmed the reliability of the mock catalogue by comparing the obtained color-magnitude relation, the luminosity and mass function and the angular correlation function with those of real data. We also analyze the behavior of the expected photometric redshifts for each different survey, in terms of photometric redshift resolution, photometric redshift bias and fraction of outliers. In addition, we discuss the benefits of using the BPZ \\emph{odds} photometric redshift quality param...

  15. Remarks on an attempted axiomatisation of Quantum Mechanics, due to Lucien Hardy, and Ten Theses on Hilbert's Sixth Problem and Quantum Measurement

    E-Print Network [OSTI]

    Joseph F. Johnson

    2006-06-15T23:59:59.000Z

    From the standpoint of Hilbert's Sixth Problem, which is the axiomatisation of Physics, the famous paper of Lucien Hardy's, Quantum Theory from Five Reasonable Axioms, is not relevant. The present paper argues that Hardy does not give a physical definition of `limit', and if we assume the usual mathematical definition of limit of a sequence, he fails to define a sequence in physical terms to which the usual definition is applicable. We argue that one should not, in fact, try to define probability in terms of the usual notion of limit of a sequence of results of a measurement because of seemingly insurmountable difficulties in axiomatising the notion of function or sequence in this context. Von Plato's and the authour's work (see http:arxiv.org/abs/quant-ph/0502124 and euclid.unh.edu/~jjohnson/axiomatics.html for larger context and further references) on the definition of physical probability needs to be used in this context. We conclude with ten theses on quantum measurement, from the standpoint of the Hilbert problem.

  16. Counting voids to probe dark energy

    E-Print Network [OSTI]

    Pisani, Alice; Hamaus, Nico; Alizadeh, Esfandiar; Biswas, Rahul; Wandelt, Benjamin D; Hirata, Christopher M

    2015-01-01T23:59:59.000Z

    We show that the number of observed voids in galaxy redshift surveys is a sensitive function of the equation of state of dark energy. Using the Fisher matrix formalism we find the error ellipses in the $w_0-w_a$ plane when the equation of state of dark energy is assumed to be of the form $w_{CPL}(z)=w_0 +w_a z/(1+z)$. We forecast the number of voids to be observed with the ESA Euclid satellite and the NASA WFIRST mission, taking into account updated details of the surveys to reach accurate estimates of their power. The theoretical model for the forecast of the number of voids is based on matches between abundances in simulations and the analytical prediction. To take into account the uncertainties within the model, we marginalize over its free parameters when calculating the Fisher matrices. The addition of the void abundance constraints to the data from Planck, HST and supernova survey data noticeably tighten the $w_0-w_a$ parameter space. We thus quantify the improvement in the constraints due to the use of...

  17. On geometry influence on the behavior of a quantum mechanical scalar particle with intrinsic structure in external magnetic and electric fields

    E-Print Network [OSTI]

    O. V. Veko; K. V. Kazmerchuk; E. M. Ovsiyuk; V. V. Kisel; V. M. Red'kov

    2014-11-07T23:59:59.000Z

    Relativistic theory of the Cox's scalar not point-like particle with intrinsic structure is developed on the background of arbitrary curved space-time. It is shown that in the most general form, the extended Proca-like tensor first order system of equations contains non minimal interaction terms through electromagnetic tensor F_{\\alpha \\beta} and Ricci tensor R_{\\alpha \\beta}. In relativistic Cox's theory, the limiting procedure to non-relativistic approximation is performed in a special class of curved space-time models. This theory is specified in simple geometrical backgrounds: Euclid's, Lobachevsky's, and Rie\\-mann's. Wave equation for the Cox's particle is solved exactly in presence of external uniform magnetic and electric fields in the case of Minkowski space. Non-trivial additional structure of the particle modifies the frequency of a quantum oscillator arising effectively in presence if external magnetic field. Extension of these problems to the case of the hyperbolic Lobachevsky space is examined. In presence of the magnetic field, the quantum problem in radial variable has been solved exactly; the quantum motion in z-direction is described by 1-dimensional Schr\\"{o}dinger-like equation in an effective potential which turns out to be too difficult for analytical treatment. In the presence of electric field, the situation is similar. The same analysis has been performed for spherical Riemann space model.

  18. Constraining inflation with future galaxy redshift surveys

    SciTech Connect (OSTI)

    Huang, Zhiqi; Vernizzi, Filippo [CEA, Institut de Physique Théorique, 91191 Gif-sur-Yvette cédex (France); Verde, Licia, E-mail: zhiqi.huang@cea.fr, E-mail: liciaverde@icc.ub.edu, E-mail: filippo.vernizzi@cea.fr [Institute of Sciences of the Cosmos (ICCUB), University of Barcelona, Marti i Franques 1, Barcelona 08024 (Spain)

    2012-04-01T23:59:59.000Z

    With future galaxy surveys, a huge number of Fourier modes of the distribution of the large scale structures in the Universe will become available. These modes are complementary to those of the CMB and can be used to set constraints on models of the early universe, such as inflation. Using a MCMC analysis, we compare the power of the CMB with that of the combination of CMB and galaxy survey data, to constrain the power spectrum of primordial fluctuations generated during inflation. We base our analysis on the Planck satellite and a spectroscopic redshift survey with configuration parameters close to those of the Euclid mission as examples. We first consider models of slow-roll inflation, and show that the inclusion of large scale structure data improves the constraints by nearly halving the error bars on the scalar spectral index and its running. If we attempt to reconstruct the inflationary single-field potential, a similar conclusion can be reached on the parameters characterizing the potential. We then study models with features in the power spectrum. In particular, we consider ringing features produced by a break in the potential and oscillations such as in axion monodromy. Adding large scale structures improves the constraints on features by more than a factor of two. In axion monodromy we show that there are oscillations with small amplitude and frequency in momentum space that are undetected by CMB alone but can be measured by including galaxy surveys in the analysis.

  19. Additive structure of Z(.) mod m_k (squarefree) and Goldbach's Conjecture

    E-Print Network [OSTI]

    N. F. Benschop

    2009-10-08T23:59:59.000Z

    The product m_k of the first k primes (2..p_k) has neighbours m_k +/- 1 with all prime divisors beyond p_k, implying there are infinitely many primes [Euclid]. All primes between p_k and m_k are in the group G_1 of units in semigroup Z_{m_k}(.) of mutiplication mod m_k. Due to the squarefree modulus Z_{m_k} is a disjoint union of 2^k groups, with as many idempotents - one per divisor of m_k, which form a Boolean lattice BL. The generators of Z_{m_k} and the additive properties of its lattice are studied. It is shown that each complementary pair in BL adds to 1 mod m_k and each even idempotent e in BL has successor e+1 in G_1. It follows that G_1+G_1 \\equiv E, the set of even residues in Z_{m_k}, so each even residue is the sum of two roots of unity, proving "Goldbach for Residues" mod m_k ("GR"). . . . Induction on k by extending residues mod m_k with "carry" a 1) successive 2n are in overlapping intervals, while the smallest composite unit in G_1 mod m_k is p_{k+1}^2, yielding "GC": Each 2n > 4 is the sum of two odd primes.

  20. Wide Angle Effects in Galaxy Surveys

    E-Print Network [OSTI]

    Yoo, Jaiyul

    2013-01-01T23:59:59.000Z

    Current and future galaxy surveys cover a large fraction of the entire sky with a significant redshift range, and the recent theoretical development shows that general relativistic effects are present in galaxy clustering on very large scales. This trend has renewed interest in the wide angle effect in galaxy clustering measurements, in which the distant-observer approximation is often adopted. Using the full wide-angle formula for computing the redshift-space correlation function, we show that compared to the sample variance, the deviation in the redshift-space correlation function from the simple Kaiser formula with the distant-observer approximation is negligible in the SDSS and is completely irrelevant in future galaxy surveys such as Euclid and the BigBOSS, if the theoretical prediction from the Kaiser formula is averaged over the survey volume and the non-uniform distribution of cosine angle between the line-of-sight and the pair separation directions is properly considered. We also find small correctio...

  1. Supermassive population III supernovae and the birth of the first quasars

    SciTech Connect (OSTI)

    Whalen, Daniel J.; Smidt, Joseph [T-2, Los Alamos National Laboratory, Los Alamos, NM 87545 (United States); Even, Wesley; Fryer, Chris L. [CCS-2, Los Alamos National Laboratory, Los Alamos, NM 87545 (United States); Heger, Alexander [Monash Centre for Astrophysics, Monash University, Victoria 3800 (Australia); Chen, K.-J. [School of Physics and Astronomy, University of Minnesota, Twin Cities, Minneapolis, MN 55455 (United States); Stiavelli, Massimo [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Xu, Hao [Center for Astrophysics and Space Sciences, UC San Diego, La Jolla, CA 92093 (United States); Joggerst, Candace C. [XTD-3, Los Alamos National Laboratory, Los Alamos, NM 87545 (United States)

    2013-11-20T23:59:59.000Z

    The existence of supermassive black holes as early as z ? 7 is one of the great, unsolved problems in cosmological structure formation. One leading theory argues that they are born during catastrophic baryon collapse in z ? 15 protogalaxies that form in strong Lyman-Werner UV backgrounds. Atomic line cooling in such galaxies fragments baryons into massive clumps that are thought to directly collapse to 10{sup 4}-10{sup 5} M {sub ?} black holes. We have now discovered that some of these fragments can instead become supermassive stars that eventually explode as thermonuclear supernovae (SNe) with energies of ?10{sup 55} erg, the most energetic explosions in the universe. We have calculated light curves and spectra for supermassive Pop III SNe with the Los Alamos RAGE and SPECTRUM codes. We find that they will be visible in near-infrared all-sky surveys by Euclid out to z ? 10-15 and by WFIRST and WISH out to z ? 15-20, perhaps revealing the birthplaces of the first quasars.

  2. Quintessence versus phantom dark energy: the arbitrating power of current and future observations

    SciTech Connect (OSTI)

    Novosyadlyj, B.; Sergijenko, O. [Astronomical Observatory of Ivan Franko National University of Lviv, Kyryla i Methodia str., 8, Lviv, 79005 (Ukraine); Durrer, R. [Université de Genève, Département de Physique Théorique and CAP, 24 quai Ernest-Ansermet, CH-1211 Genève 4 (Switzerland); Pelykh, V., E-mail: novos@astro.franko.lviv.ua, E-mail: olka@astro.franko.lviv.ua, E-mail: ruth.durrer@unige.ch, E-mail: pelykh@iapmm.lviv.ua [Ya. S. Pidstryhach Institute for Applied Problems of Mechanics and Mathematics, Naukova str., 3-b, Lviv, 79060 (Ukraine)

    2013-06-01T23:59:59.000Z

    We analyze the possibility to distinguish between quintessence and phantom scalar field models of dark energy using observations of luminosity distance moduli of SNe Ia, CMB anisotropies and polarization, matter density perturbations and baryon acoustic oscillations. Among the present observations only Planck data on CMB anisotropy and SDSS DR9 data on baryon acoustic oscillations may be able to decide between quintessence or phantom scalar field models, however for each model a set of best-fit parameters exists, which matches all data with similar goodness of fit. We compare the relative differences of best-fit model predictions with observational uncertainties for each type of data and we show that the accuracy of SNe Ia luminosity distance data is far from the one necessary to distinguish these types of dark energy models, while the CMB data (WMAP, ACT, SPT and especially Planck) are close to being able to reliably distinguish them. Also an improvement of the large-scale structure data (future releases of SDSS BOSS and e.g. Euclid or BigBOSS) will enable us to surely decide between quintessence and phantom dark energy.

  3. Cosmological parameter constraints from SDSS luminous red galaxies: a new treatment of large-scale clustering

    E-Print Network [OSTI]

    Ariel G. Sanchez; M. Crocce; A. Cabre; C. M. Baugh; E. Gaztanaga

    2009-08-19T23:59:59.000Z

    We apply a new model for the spherically averaged correlation function at large pair separations to the measurement of the clustering of luminous red galaxies (LRGs) made from the SDSS by Cabre and Gaztanaga(2009). Our model takes into account the form of the BAO peak and the large scale shape of the correlation function. We perform a Monte Carlo Markov chain analysis for different combinations of datasets and for different parameter sets. When used in combination with a compilation of the latest CMB measurements, the LRG clustering and the latest supernovae results give constraints on cosmological parameters which are comparable and in remarkably good agreement, resolving the tension reported in some studies. The best fitting model in the context of a flat, Lambda-CDM cosmology is specified by Omega_m=0.261+-0.013, Omega_b=0.044+-0.001, n_s=0.96+-0.01, H_0=71.6+-1.2 km/s/Mpc and sigma_8=0.80+-0.02. If we allow the time-independent dark energy equation of state parameter to vary, we find results consistent with a cosmological constant at the 5% level using all data sets: w_DE=-0.97+-0.05. The large scale structure measurements by themselves can constrain the dark energy equation of state parameter to w_DE=-1.05+-0.15, independently of CMB or supernovae data. We do not find convincing evidence for an evolving equation of state. We provide a set of "extended distance priors" that contain the most relevant information from the CMB power spectrum and the shape of the LRG correlation function which can be used to constrain dark energy models and spatial curvature. Our model should provide an accurate description of the clustering even in much larger, forthcoming surveys, such as those planned with NASA's JDEM or ESA's Euclid mission.

  4. CLUSTER LENSING PROFILES DERIVED FROM A REDSHIFT ENHANCEMENT OF MAGNIFIED BOSS-SURVEY GALAXIES

    SciTech Connect (OSTI)

    Coupon, Jean; Umetsu, Keiichi [Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box 23-141, Taipei 10617, Taiwan (China); Broadhurst, Tom, E-mail: coupon@asiaa.sinica.edu.tw [Department of Theoretical Physics, University of Basque Country UPV/EHU, P.O. Box 644, E-48080 Bilbao (Spain)

    2013-07-20T23:59:59.000Z

    We report the first detection of a redshift-depth enhancement of background galaxies magnified by foreground clusters. Using 300,000 BOSS survey galaxies with accurate spectroscopic redshifts, we measure their mean redshift depth behind four large samples of optically selected clusters from the Sloan Digital Sky Survey (SDSS) surveys, totaling 5000-15,000 clusters. A clear trend of increasing mean redshift toward the cluster centers is found, averaged over each of the four cluster samples. In addition, we find similar but noisier behavior for an independent X-ray sample of 158 clusters lying in the foreground of the current BOSS sky area. By adopting the mass-richness relationships appropriate for each survey, we compare our results with theoretical predictions for each of the four SDSS cluster catalogs. The radial form of this redshift enhancement is well fitted by a richness-to-mass weighted composite Navarro-Frenk-White profile with an effective mass ranging between M{sub 200} {approx} 1.4-1.8 Multiplication-Sign 10{sup 14} M{sub Sun} for the optically detected cluster samples, and M{sub 200} {approx} 5.0 Multiplication-Sign 10{sup 14} M{sub Sun} for the X-ray sample. This lensing detection helps to establish the credibility of these SDSS cluster surveys, and provides a normalization for their respective mass-richness relations. In the context of the upcoming bigBOSS, Subaru Prime Focus Spectrograph, and EUCLID-NISP spectroscopic surveys, this method represents an independent means of deriving the masses of cluster samples for examining the cosmological evolution, and provides a relatively clean consistency check of weak-lensing measurements, free from the systematic limitations of shear calibration.

  5. WEAK LENSING MEASUREMENT OF GALAXY CLUSTERS IN THE CFHTLS-WIDE SURVEY

    SciTech Connect (OSTI)

    Shan Huanyuan; Tao Charling [Department of Physics and Tsinghua Center for Astrophysics, Tsinghua University, Beijing, 100084 (China); Kneib, Jean-Paul; Jauzac, Mathilde; Limousin, Marceau [Laboratoire d'Astrophysique de Marseille, CNRS-Universite de Provence, 38 rue Frederic Joliot-Curie, F-13388 Marseille Cedex 13 (France); Fan Zuhui [Department of Astronomy, Peking University, Beijing, 100871 (China); Massey, Richard [Institute for Astronomy, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ (United Kingdom); Rhodes, Jason [California Institute of Technology, MC 350-17, 1200 East California Boulevard, Pasadena, CA 91125 (United States); Thanjavur, Karun [Canada France Hawaii Telescope, 65-1238 Mamalahoa Hwy, Kamuela, HI 96743 (United States); McCracken, Henry J., E-mail: shanhuany@gmail.com [Institude d'Astrophysique de Paris, UMR 7095, 98 bis Boulevard Arago, F-75014 Paris (France)

    2012-03-20T23:59:59.000Z

    We present the first weak gravitational lensing analysis of the completed Canada-France-Hawaii Telescope Legacy Survey (CFHTLS). We study the 64 deg{sup 2} W1 field, the largest of the CFHTLS-Wide survey fields, and present the largest contiguous weak lensing convergence 'mass map' yet made. 2.66 million galaxy shapes are measured, using the Kaiser Squires and Broadhurst Method (KSB) pipeline verified against high-resolution Hubble Space Telescope imaging that covers part of the CFHTLS. Our i'-band measurements are also consistent with an analysis of independent r'-band imaging. The reconstructed lensing convergence map contains 301 peaks with signal-to-noise ratio {nu} > 3.5, consistent with predictions of a {Lambda}CDM model. Of these peaks, 126 lie within 3.'0 of a brightest central galaxy identified from multicolor optical imaging in an independent, red sequence survey. We also identify seven counterparts for massive clusters previously seen in X-ray emission within 6 deg{sup 2} XMM-LSS survey. With photometric redshift estimates for the source galaxies, we use a tomographic lensing method to fit the redshift and mass of each convergence peak. Matching these to the optical observations, we confirm 85 groups/clusters with {chi}{sup 2}{sub reduced} < 3.0, at a mean redshift (z{sub c} ) = 0.36 and velocity dispersion ({sigma}{sub c}) = 658.8 km s{sup -1}. Future surveys, such as DES, LSST, KDUST, and EUCLID, will be able to apply these techniques to map clusters in much larger volumes and thus tightly constrain cosmological models.

  6. Non-linear evolution of the cosmic neutrino background

    SciTech Connect (OSTI)

    Villaescusa-Navarro, Francisco; Viel, Matteo [INAF/Osservatorio Astronomico di Trieste, Via Tiepolo 11, 34143, Trieste (Italy); Bird, Simeon [Institute for Advanced Study, 1 Einstein Drive, Princeton, NJ, 08540 (United States); Peña-Garay, Carlos, E-mail: villaescusa@oats.inaf.it, E-mail: spb@ias.edu, E-mail: penya@ific.uv.es, E-mail: viel@oats.inaf.it [Instituto de Física Corpuscular, CSIC-UVEG, E-46071, Paterna, Valencia (Spain)

    2013-03-01T23:59:59.000Z

    We investigate the non-linear evolution of the relic cosmic neutrino background by running large box-size, high resolution N-body simulations which incorporate cold dark matter (CDM) and neutrinos as independent particle species. Our set of simulations explore the properties of neutrinos in a reference ?CDM model with total neutrino masses between 0.05-0.60 eV in cold dark matter haloes of mass 10{sup 11}?10{sup 15} h{sup ?1}M{sub s}un, over a redshift range z = 0?2. We compute the halo mass function and show that it is reasonably well fitted by the Sheth-Tormen formula, once the neutrino contribution to the total matter is removed. More importantly, we focus on the CDM and neutrino properties of the density and peculiar velocity fields in the cosmological volume, inside and in the outskirts of virialized haloes. The dynamical state of the neutrino particles depends strongly on their momentum: whereas neutrinos in the low velocity tail behave similarly to CDM particles, neutrinos in the high velocity tail are not affected by the clustering of the underlying CDM component. We find that the neutrino (linear) unperturbed momentum distribution is modified and mass and redshift dependent deviations from the expected Fermi-Dirac distribution are in place both in the cosmological volume and inside haloes. The neutrino density profiles around virialized haloes have been carefully investigated and a simple fitting formula is provided. The neutrino profile, unlike the cold dark matter one, is found to be cored with core size and central density that depend on the neutrino mass, redshift and mass of the halo, for halos of masses larger than ? 10{sup 13.5}h{sup ?1}M{sub s}un. For lower masses the neutrino profile is best fitted by a simple power-law relation in the range probed by the simulations. The results we obtain are numerically converged in terms of neutrino profiles at the 10% level for scales above ? 200 h{sup ?1}kpc at z = 0, and are stable with respect to box-size and starting redshift of the simulation. Our findings are particularly important in view of upcoming large-scale structure surveys, like Euclid, that are expected to probe the non-linear regime at the percent level with lensing and clustering observations.

  7. Measuring the neutrino mass from future wide galaxy cluster catalogues

    SciTech Connect (OSTI)

    Carbone, Carmelita; Moscardini, Lauro; Cimatti, Andrea [Dipartimento di Astronomia, Alma Mater Studiorum-Università di Bologna, via Ranzani 1, I-40127 Bologna (Italy); Fedeli, Cosimo, E-mail: carmelita.carbone@unibo.it, E-mail: cosimo.fedeli@astro.ufl.edu, E-mail: lauro.moscardini@unibo.it, E-mail: a.cimatti@unibo.it [Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611 (United States)

    2012-03-01T23:59:59.000Z

    We present forecast errors on a wide range of cosmological parameters obtained from a photometric cluster catalogue of a future wide-field Euclid-like survey. We focus in particular on the total neutrino mass as constrained by a combination of the galaxy cluster number counts and correlation function. For the latter we consider only the shape information and the Baryon Acoustic Oscillations (BAO), while marginalising over the spectral amplitude and the redshift space distortions. In addition to the cosmological parameters of the standard ?CDM+? model we also consider a non-vanishing curvature, and two parameters describing a redshift evolution for the dark energy equation of state. For completeness, we also marginalise over a set of ''nuisance'' parameters, representing the uncertainties on the cluster mass determination. We find that combining cluster counts with power spectrum information greatly improves the constraining power of each probe taken individually, with errors on cosmological parameters being reduced by up to an order of magnitude. In particular, the best improvements are for the parameters defining the dynamical evolution of dark energy, where cluster counts break degeneracies. Moreover, the resulting error on neutrino mass is at the level of ?(M{sub ?}) ? 0.9 eV, comparable with that derived from present Ly? forest measurements and Cosmic Microwave background (CMB) data in the framework of a non-flat Universe. Further adopting Planck priors and reducing the number of free parameters to a ?CDM+? cosmology allows to place constraints on the total neutrino mass of ?(M{sub ?}) ? 0.08 eV, close to the lower bound enforced by neutrino oscillation experiments. Finally, in the optimistic case where uncertainties in the calibration of the mass-observable relation were so small to be neglected, the combination of Planck priors with cluster counts and power spectrum would constrain the total neutrino mass down to ?(M{sub ?}) ? 0.034 eV, i.e. the minimum neutrino mass predicted by oscillation experiments would be detected in a ?CDM framework. We thus show that galaxy clusters from future wide galaxy surveys will be an excellent tool for studying cosmology and fundamental physics.

  8. OPTICAL/NEAR-INFRARED SELECTION OF RED QUASI-STELLAR OBJECTS: EVIDENCE FOR STEEP EXTINCTION CURVES TOWARD GALACTIC CENTERS?

    SciTech Connect (OSTI)

    Fynbo, J. P. U.; Krogager, J.-K.; Vestergaard, M.; Geier, S. [Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen O (Denmark); Venemans, B. [Max-Planck Institute for Astronomy, Koenigstuhl 17, D-69117 Heidelberg (Germany); Noterdaeme, P. [CNRS-UPMC, UMR7095, Institut d'Astrophysique de Paris, 98bis Bd. Arago, F-75014 Paris (France); Moller, P. [European Southern Observatory, Karl-Schwarzschildstrasse 2, D-85748 Garching bei Muenchen (Germany); Ledoux, C. [European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19 (Chile)

    2013-01-15T23:59:59.000Z

    We present the results of a search for red QSOs using a selection based on optical imaging from the Sloan Digital Sky Survey (SDSS) and near-infrared imaging from UKIDSS. Our main goal with the selection is to search for QSOs reddened by foreground dusty absorber galaxies. For a sample of 58 candidates (including 20 objects fulfilling our selection criteria that already have spectra in the SDSS), 46 (79%) are confirmed to be QSOs. The QSOs are predominantly dust-reddened except for a handful at redshifts z {approx}> 3.5. However, the dust is most likely located in the QSO host galaxies (and for two, the reddening is primarily caused by Galactic dust) rather than in the intervening absorbers. More than half of the QSOs show evidence of associated absorption (BAL absorption). Four (7%) of the candidates turned out to be late-type stars, and another four (7%) are compact galaxies. We could not identify the remaining four objects. In terms of their optical spectra, these QSOs are similar to the QSOs selected in the FIRST-2MASS Red Quasar Survey except they are on average fainter, more distant, and only two are detected in the FIRST survey. As per the usual procedure, we estimate the amount of extinction using the SDSS QSO template reddened by Small-Magellanic-Cloud-(SMC) like dust. It is possible to get a good match to the observed (rest-frame ultraviolet) spectra, but it is not possible to match the observed near-IR photometry from UKIDSS for nearly all the reddened QSOs. The most likely reasons are that the SDSS QSO template is too red at optical wavelengths due to contaminating host galaxy light and because the assumed SMC extinction curve is too shallow. Three of the compact galaxies display old stellar populations with ages of several Gyr and masses of about 10{sup 10} M{sub Sun} (based on spectral energy distribution modeling). The inferred stellar densities in these galaxies exceed 10{sup 10} M{sub Sun} kpc{sup -2}, which is among the highest measured for early-type galaxies. Our survey has demonstrated that selection of QSOs based on near-IR photometry is an efficient way to select QSOs, including reddened QSOs, with only small contamination from late-type stars and compact galaxies. This will be useful with ongoing and future wide-field near-IR surveys such as the VISTA and EUCLID surveys.

  9. Final Technical Report: Intensive Quenching Technology for Heat Treating and Forging Industries

    SciTech Connect (OSTI)

    Aronov, Michael A.

    2005-12-21T23:59:59.000Z

    Intensive quenching (IQ) process is an alternative way of hardening (quenching) steel parts through the use of highly agitated water and then still air. It was developed by IQ Technologies, Inc. (IQT) of Akron, Ohio. While conventional quenching is usually performed in environmentally unfriendly oil or water/polymer solutions, the IQ process uses highly agitated environmentally friendly water or low concentration water/mineral salt solutions. The IQ method is characterized by extremely high cooling rates of steel parts. In contrast to conventional quenching, where parts cool down to the quenchant temperature and usually have tensile or neutral residual surface stresses at the end of quenching. The IQ process is interrupted when the part core is still hot and when there are maximum compressive stresses deep into the parts, thereby providing hard, ductile, better wear resistant parts. The project goal was to advance the patented IQ process from feasibility to commercialization in the heat-treating and forging industries to reduce significantly energy consumption and environmental impact, to increase productivity and to enhance economic competitiveness of these industries as well as Steel, Metal Casting and Mining industries. To introduce successfully the IQ technology in the U.S. metal working industry, the project team has completed the following work over the course of this project: A total of 33 manufacturers of steel products provided steel parts for IQ trails. IQT conducted IQ demonstrations for 34 different steel parts. Our customers tested intensively quenched parts in actual field conditions to evaluate the product service life and performance improvement. The data obtained from the field showed the following: Service life (number of holes punched) of cold-work punches (provided by EHT customer and made of S5 shock-resisting steel) was improved by two to eight times. Aluminum extrusion dies provided by GAM and made of hot work H-13 steel outperformed the standard dies by at least 50%. Dies provided by an AST customer, made of plain carbon 1045 steel and used for pellet manufacturing outperformed the standard dies by more than 100%. Concrete crusher liner wear plates provided by an EHT customer and made of 1045 steel, had the same surface hardness as the plates made of more expensive, pre-hardened high alloy HARDOX-500 material supplied by a Swedish company and used currently by the EHT customer. The 1045 material intensively quenched wear plates are currently in the field. Concrete block molding machine wear plates provided by an IQT customer and made of 8620 steel were processed at the AST production IQ system using a 40% reduced carburization cycle. An effective case depth in the intensively quenched wear plates was the same as in the standard, oil quenched parts. Base keys provided by an EHT customer and made of 8620 steel were processed using a 40% reduced carburization cycle. The intensively quenched parts showed the same performance as standard parts. IQT introduced the IQ process in heat treat practices of three commercial heat-treating shops: Akron Steel Treating Co., Summit Heat Treating Co. and Euclid Heat Treating Co. CWRU conducted a material characterization study for a variety of steels to develop a database to support changing/modification of recognized standards for quenching steel parts. IQT conducted a series of IQ workshops, published seven technical papers and participated in ASM Heat Treating Society conference and exposition and in Furnace North America Show. IQT designed and built a fully automated new IQ system installed at the Center for Intensive Quenching. This system includes the following major components: a stand-alone 1,900-gallon IQ water system, a 24'' x 24'' atmosphere pit furnace, and an automated load transfer mechanism. IQT established a ''Center for Intensive Quenching'' at the AST facilities. The 4,000 square feet Center includes the following equipment: High-velocity single part quenching IQ unit developed and built previously under EMTEC CT-65 project. The unit is equipped w