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1. Probing Dark Energy via Weak Gravitational Lensing with the SuperNova Acceleration Probe (SNAP)

Author

Greg Aldering, M. Hoff, Ralph C. Bohlin, S. L. Mufson, Andrew Szymkowiak, L. Gladney, O. Le Fevre, D. Cole, Nick Mostek, N. Palaio, Susana E. Deustua, Wolfgang Lorenzon, P. Limon, M. L. Lampton, Dragan Huterer, Scott Dodelson, N. Kuznetsova, Alain Mazure, H. Shuka, S. T. Holland, F. Stabenau, Josh Frieman, Roger Smith, Guofeng Wang, T. Davies, B. Besuner, Martin White, A. Weinstein, Roger F. Malina, Jason Rhodes, J. Annis, R. Lafever, G. Kushner, J. Albert, H. Lin, Saul Perlmutter, Lars Bergström, G. Smadja, R. Pain, Eric V. Linder, B. Krieger, John Peoples, A. D. Tomasch, B. Bigelow, J. Musser, Peter Nugent, A. Refregier, William W. Craig, L. Marian, H. von der Lippe, Michael Seiffert, D. E. Groom, Keith Taylor, Timothy A. McKay, Eric Prieto, Chris Bebek, C. R. Bower, D. Peterson, Albert Stebbins, G. Tarle, Stephen Bailey, J. I. Lamoureux, Christopher Stoughton, J.-P. Walder, F. DeJongh, Alex G. Kim, W. Emmet, Eugene D. Commins, V. Scarpine, M. Frerking, Gary Bernstein, A. Goobar, Douglas L. Tucker, Michael Schubnell, C. T. Day, Andre Tilquin, D. Figer, Shawn McKee, Edvard Mörtsell, Rahman Amanullah, M. Deharveng, Dominique Fouchez, W. C. Wester, D. Rabinowitz, M.E. Huffer, R. Nakajima, J. Snyder, T. Dobson, Armin Karcher, Stéphane Basa, Michael L. Brown, David H. Pankow, Steven E. Kahn, Anne Ealet, C. Juramy, Steve Kent, A. S. Fruchter, S. C. Loken, G. Goldhaber, Bhuvnesh Jain, Alain Bonissent, M. Aumeunier, Philip J. Marshall, J. P. Marriner, M. E. Levi, E. Barrelet, P. Jelinsky, Michael Sholl, A. L. Spadafora, L. Hui, T. Diehl, B. Mcginnis, Richard Ellis, B. Mobqsher, V. Lebrun, S. Allam, William Carithers, George F. Smoot, Richard Massey, Roger Blandford, Pierre Astier, W. Althouse, William F. Kolbe, D. W. Gerdes, D. Rusin, Natalie A. Roe, Ramon Miquel, N. Morgan, H. Heetderks, Manfred Bester, D. Vincent, M. Campbell, C. Baltay, Hakeem M. Oluseyi, Flores, Sylvie, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), SNAP, Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Point spread function, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, law.invention, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], law, 0103 physical sciences, 010306 general physics, Weak gravitational lensing, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Redshift, Galaxy, Supernova, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Dark energy, Joint Dark Energy Mission
Abstract

SNAP is a candidate for the Joint Dark Energy Mission (JDEM) that seeks to place constraints on the dark energy using two distinct methods. The first, Type Ia SN, is discussed in a companion white paper. The second method is weak gravitational lensing, which relies on the coherent distortions in the shapes of background galaxies by foreground mass structures. The excellent spatial resolution and photometric accuracy afforded by a 2-meter space-based observatory are crucial for achieving the high surface density of resolved galaxies, the tight control of systematic errors in the telescope's Point Spread Function (PSF), and the exquisite redshift accuracy and depth required by this project. These are achieved by the elimination of atmospheric distortion and much of the thermal and gravity loads on the telescope. The SN and WL methods for probing dark energy are highly complementary and the error contours from the two methods are largely orthogonal., 17 pages, 6 figures; White paper to the Dark Energy Task Force

Published
2005

2. Weak lensing from space I: instrumentation and survey strategy

Author

S. Harris, H. von der Lippe, Dominique Fouchez, Lars Bergström, C. T. Day, Alex G. Kim, B. Bigelow, Chris Bebek, Myron Campbell, A. L. Spadafora, Saul Perlmutter, Eric Prieto, R. Pratt, M. L. Lampton, S.E. Holland, G. Smadja, A. S. Fruchter, Armin Karcher, B. Krieger, J.-P. Walder, N. Morgan, Gary Bernstein, Peter Nugent, C. Baltay, Eric V. Linder, Shawn McKee, Ariel Goobar, Justin Albert, William E. Johnston, Timothy A. McKay, Hakeem M. Oluseyi, N. Palaio, Susana E. Deustua, Greg Aldering, J. Bercovitz, Nick Mostek, George F. Smoot, David Rabinowitz, Roger F. Malina, Pierre Astier, David Bacon, Keith Taylor, C. R. Bower, William F. Kolbe, R. Lafever, Andrew Szymkowiak, H. Heetderks, David H. Pankow, A. D. Tomasch, G. Kushner, J. A. Musser, Wolfgang Lorenzon, Peter Harvey, D. Rusin, Natalie A. Roe, W. Emmet, Anne Ealet, Roger Smith, S. C. Loken, Ramon Miquel, Edvard Mörtsell, Gerson Goldhaber, E. Barrelet, R. DiGennaro, Alain Bonissent, M. E. Levi, Andre Tilquin, S. L. Mufson, Alexandre Refregier, M. Eriksson, Michael Sholl, Manfred Bester, Richard S. Ellis, Bhuvnesh Jain, D. W. Gerdes, William Carithers, Richard Massey, L. Gladney, D. Vincent, Guofeng Wang, Alain Mazure, Michael Schubnell, Carl W. Akerlof, Rahman Amanullah, Eugene D. Commins, Reynald Pain, Donald E. Groom, J. F. Genat, K. Robinson, Gregory Tarle, Dragan Huterer, Michael E. Brown, J. I. Lamoureux, Ralph C. Bohlin, J. Snyder, N. Kuznetsova, Jason Rhodes, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), California Institute of Technology (CALTECH), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Mathematics [Berkeley], University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), School of Engineering [Edinburgh], University of Edinburgh, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Department of Physics, Stockholm University, Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Dispositifs et Instrumentation en Optoélectronique et micro-ondes (DIOM), Université Jean Monnet - Saint-Étienne (UJM), Dept Mat Sci & Engn, Zhejiang University, California Institute of Technology (CALTECH)-NASA, University of California [Berkeley], University of California-University of California, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Harvard University [Cambridge]-Smithsonian Institution, DIOM (DIOM), and Université Jean Monnet [Saint-Étienne] (UJM)

Subjects
Point spread function, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, law.invention, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Spitzer Space Telescope, law, 0103 physical sciences, Dark energy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Instrumentation, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Supernova
Abstract

A wide field space-based imaging telescope is necessary to fully exploit the technique of observing dark matter via weak gravitational lensing. This first paper in a three part series outlines the survey strategies and relevant instrumental parameters for such a mission. As a concrete example of hardware design, we consider the proposed Supernova/Acceleration Probe (SNAP). Using SNAP engineering models, we quantify the major contributions to this telescope's Point Spread Function (PSF). These PSF contributions are relevant to any similar wide field space telescope. We further show that the PSF of SNAP or a similar telescope will be smaller than current ground-based PSFs, and more isotropic and stable over time than the PSF of the Hubble Space Telescope. We outline survey strategies for two different regimes - a ``wide'' 300 square degree survey and a ``deep'' 15 square degree survey that will accomplish various weak lensing goals including statistical studies and dark matter mapping., 25 pages, 8 figures, 1 table, replaced with Published Version

Published
2004
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3. Wide-field surveys from the SNAP mission

Author

Alex G. Kim, Carl W. Akerlof, Greg Aldering, R. Amanullah, Pierre Astier, E. Barrelet, Christopher Bebek, Lars Bergstrom, J. Bercovitz, Gary M. Bernstein, M. Bester, A. Bonissent, C. Bower, William C. Carithers, Jr., Eugene D. Commins, C. Day, Susana E. Deustua, R. DiGennaro, A. Ealet, Richard S. Ellis, M. Eriksson, Andrew Fruchter, Jean-Francois Genat, Gerson Goldhaber, Ariel Goobar, Donald E. Groom, Stewart E. Harris, Peter R. Harvey, Henry D. Heetderks, Steven E. Holland, Dragan Huterer, Armin Karcher, William F. Kolbe, B. Krieger, Robin E. Lafever, J. Lamoureux, Michael L. Lampton, Michael E. Levi, Daniel S. Levin, Eric V. Linder, Stewart C. Loken, Roger Malina, R. Massey, Timothy McKay, Shawn P. McKee, Ramon Miquel, E. Mortsell, N. Mostek, Stuart Mufson, J. A. Musser, Peter E. Nugent, Hakeem M. Oluseyi, Reynald Pain, Nicholas P. Palaio, David H. Pankow, Saul Perlmutter, R. Pratt, Eric Prieto, Alexandre Refregier, Jason Rhodes, Kem E. Robinson, N. Roe, Michael Sholl, Michael S. Schubnell, G. Smadja, George F. Smoot, Anthony Spadafora, Gregory Tarle, Andrew D. Tomasch, H. von der Lippe, D. Vincent, J.-P. Walder, Guobin Wang, Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Flores, Sylvie, Tyson, J. Anthony, and Wolff, Sidney

Subjects
media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Acceleration, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Angular resolution, 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, media_common, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Sampling (statistics), Supernova, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Sky, Magnitude (astronomy)
Abstract

The Supernova/Acceleration Probe (SNAP) is a proposed space-borne observatory that will survey the sky with a wide-field optical/near-infrared (NIR) imager. The images produced by SNAP will have an unprecedented combination of depth, solid-angle, angular resolution, and temporal sampling. For 16 months each, two 7.5 square-degree fields will be observed every four days to a magnitude depth of AB=27.7 in each of the SNAP filters, spanning 3500-17000\AA. Co-adding images over all epochs will give AB=30.3 per filter. In addition, a 300 square-degree field will be surveyed to AB=28 per filter, with no repeated temporal sampling. Although the survey strategy is tailored for supernova and weak gravitational lensing observations, the resulting data will support a broad range of auxiliary science programs., Comment: This paper will be published in SPIE Proceedings Vol. 4836 and is made available as an electronic preprint with permission of SPIE. One print or electronic copy may be made for personal use only. Systematic or multiple reproduction, distribution to multiple locations via electronic or other means, duplication of any material in this paper for a fee or for commercial purposes, or modification of the content of the paper are prohibited

Published
2002

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