Dark Energy Survey Year 1 results: curved-sky weak lensing mass map

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Stellar population synthesis at the resolution of 2003

G. Bruzual, S. Charlot (2003)

We present a new model for computing the spectral evolution of stellar populations at ages between 100,000 yr and 20 Gyr at a resolution of 3 A across the whole wavelength range from 3200 to 9500 A for a wide range of metallicities. These predictions are based on a newly available library of observed stellar spectra. We also compute the spectral evolution across a larger wavelength range, from 91 A to 160 micron, at lower resolution. The model incorporates recent progress in stellar evolution theory and an observationally motivated prescription for thermally-pulsing stars on the asymptotic giant branch. The latter is supported by observations of surface brightness fluctuations in nearby stellar populations. We show that this model reproduces well the observed optical and near-infrared colour-magnitude diagrams of Galactic star clusters of various ages and metallicities. Stochastic fluctuations in the numbers of stars in different evolutionary phases can account for the full range of observed integrated colours of star clusters in the Magellanic Clouds. The model reproduces in detail typical galaxy spectra from the Early Data Release (EDR) of the Sloan Digital Sky Survey (SDSS). We exemplify how this type of spectral fit can constrain physical parameters such as the star formation history, metallicity and dust content of galaxies. Our model is the first to enable accurate studies of absorption-line strengths in galaxies containing stars over the full range of ages. Using the highest-quality spectra of the SDSS EDR, we show that this model can reproduce simultaneously the observed strengths of those Lick indices that do not depend strongly on element abundance ratios [abridged].

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Mapping the dark matter with weak gravitational lensing

Nick Kaiser, Gordon K. Squires (1993)

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The cosmological simulation code GADGET-2

Volker Springel (2005)

We discuss the cosmological simulation code GADGET-2, a new massively parallel TreeSPH code, capable of following a collisionless fluid with the N-body method, and an ideal gas by means of smoothed particle hydrodynamics (SPH). Our implementation of SPH manifestly conserves energy and entropy in regions free of dissipation, while allowing for fully adaptive smoothing lengths. Gravitational forces are computed with a hierarchical multipole expansion, which can optionally be applied in the form of a TreePM algorithm, where only short-range forces are computed with the `tree'-method while long-range forces are determined with Fourier techniques. Time integration is based on a quasi-symplectic scheme where long-range and short-range forces can be integrated with different timesteps. Individual and adaptive short-range timesteps may also be employed. The domain decomposition used in the parallelisation algorithm is based on a space-filling curve, resulting in high flexibility and tree force errors that do not depend on the way the domains are cut. The code is efficient in terms of memory consumption and required communication bandwidth. It has been used to compute the first cosmological N-body simulation with more than 10^10 dark matter particles, reaching a homogeneous spatial dynamic range of 10^5 per dimension in a 3D box. It has also been used to carry out very large cosmological SPH simulations that account for radiative cooling and star formation, reaching total particle numbers of more than 250 million. We present the algorithms used by the code and discuss their accuracy and performance using a number of test problems. GADGET-2 is publicly released to the research community.

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Author and article information

Journal

Title: Monthly Notices of the Royal Astronomical Society

Publisher: Oxford University Press (OUP)

ISSN (Print): 0035-8711

ISSN (Electronic): 1365-2966

Publication date Created: April 2018

Publication date Created: April 11 2018

Publication date Created: January 04 2018

Publication date Other: April 2018

Publication date (Print): April 11 2018

Publication date (Electronic): January 04 2018

Volume: 475

Issue: 3

Pages: 3165-3190

Affiliations

[1 ]Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA

[2 ]DEDIP/DAP, IRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France

[3 ]Université Paris Diderot, AIM, Sorbonne Paris Cité, CEA, CNRS, F-91191 Gif-sur-Yvette, France

[4 ]Institut de Ciències de l'Espai, IEEC-CSIC, Campus UAB, Facultat de Ciències, Torre C5 par-2, E-08193 Bellaterra, Barcelona, Spain

[5 ]Institute of Cosmology & Gravitation, University of Portsmouth, Portsmouth, PO1 3FX, UK

[6 ]Jodrell Bank Center for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester, M13 9PL, UK

[7 ]Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544, USA

[8 ]Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona) Spain

[9 ]Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA

[10 ]New York University, CCPP, New York, NY 10003, USA

[11 ]Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK

[12 ]Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK

[13 ]Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr. 1, D-81679 Munich, Germany

[14 ]LSST, 933 North Cherry Avenue, Tucson, AZ 85721, USA

[15 ]Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA

[16 ]Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA

[17 ]CNRS, UMR 7095, Institut d'Astrophysique de Paris, F-75014, Paris, France

[18 ]Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK

[19 ]Sorbonne Universités, UPMC Univ Paris 06, UMR 7095, Institut d'Astrophysique de Paris, F-75014, Paris, France

[20 ]Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil

[21 ]Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil

[22 ]Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Madrid, Spain

[23 ]Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA

[24 ]SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA

[25 ]Department of Physics, ETH Zurich, Wolfgang-Pauli-Strasse 16, CH-8093 Zurich, Switzerland

[26 ]Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA

[27 ]Department of Physics, The Ohio State University, Columbus, OH 43210, USA

[28 ]Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA

[29 ]University of Arizona, Department of Physics, 1118 E. Fourth St., Tucson, AZ 85721, USA

[30 ]Brookhaven National Laboratory, Bldg 510, Upton, NY 11973, USA

[31 ]Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, D-85748 Garching, Germany

[32 ]Argonne National Laboratory, 9700 South Cass Avenue, Lemont, IL 60439, USA

[33 ]Institute for Astronomy, University of Edinburgh, Edinburgh EH9 3HJ, UK

[34 ]Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile

[35 ]Department of Physics and Electronics, Rhodes University, PO Box 94, Grahamstown, 6140, South Africa

[36 ]Department of Astronomy, University of Illinois, 1002 W. Green Street, Urbana, IL 61801, USA

[37 ]National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA

[38 ]Department of Physics, IIT Hyderabad, Kandi, Telangana 502285, India

[39 ]Excellence Cluster Universe, Boltzmannstr. 2, D-85748 Garching, Germany

[40 ]Instituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid, E-28049 Madrid, Spain

[41 ]Astronomy Department, University of Washington, Box 351580, Seattle, WA 98195, USA

[42 ]Santa Cruz Institute for Particle Physics, Santa Cruz, CA 95064, USA

[43 ]Australian Astronomical Observatory, North Ryde, NSW 2113, Australia

[44 ]Departamento de Física Matemática, Instituto de Física, Universidade de São Paulo, CP 66318, São Paulo, SP, 05314-970, Brazil

[45 ]Institució Catalana de Recerca i Estudis Avançats, E-08010 Barcelona, Spain

[46 ]Department of Physics and Astronomy, Pevensey Building, University of Sussex, Brighton, BN1 9QH, UK

[47 ]Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA

[48 ]School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK

[49 ]Instituto de Física Gleb Wataghin, Universidade Estadual de Campinas, 13083-859, Campinas, SP, Brazil

[50 ]Computer Science and Mathematics Division, Oak Ridge National Laboratory, Oak Ridge, TN 37831

Article

DOI: 10.1093/mnras/stx3363

SO-VID: 14c8e45f-1051-49e4-89a7-3cbbd3fc1f10

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Dark Energy Survey Year 1 results: curved-sky weak lensing mass map

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Most cited references 68

Stellar population synthesis at the resolution of 2003

Mapping the dark matter with weak gravitational lensing

The cosmological simulation code GADGET-2

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Cited by 15

Most referenced authors 3,089