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Ultimate wide field Imaging: The Large Synoptic Sky Survey Marek Kowalski Physikalisches Institut Universitt Bonn

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Disclaimer This is not a for the LSST collaboration talk (but all plots/numbers are from LSST public domain)

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LSST Institutions Adler Planetarium, Brookhaven National Laboratory (BNL), California Institute of Technology, Carnegie Mellon University, Cornell University, Drexel University, George Mason University, Google, Harvard-Smithsonian Center for Astrophysics, Institut de Physique Nuclaire et de Physique des Particules (IN2P3), Johns Hopkins University, Kavli Institute for Particle Astrophysics and Cosmology (KIPAC) - Stanford University, Las Cumbres Observatory Global Telescope Network, Lawrence Livermore National Laboratory (LLNL), Los Alamos National Laboratory (LANL), National Optical Astronomy Observatory, Princeton University, Purdue University, Research Corporation for Science Advancement, Rutgers, SLAC National Accelerator Laboratory, Space Telescope Science Institute, Texas A & M University, The Pennsylvania State University, The University of Arizona, University of California at Davis, University of California at Irvine, University of Illinois at Urbana-Champaign, University of Michigan, University of Pennsylvania, University of Pittsburgh, University of Washington, Vanderbilt University

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The survey 6-band Survey: ugrizy 3201080 nm Sky area covered: > 20,000 deg2, 0.2 arcsec / pixel 10-Year Duration: Yields 27.7 AB magnitude @ 5 Each 9.6 sq.deg FOV revisited ~ 1000 times Frequent revisits: 2 x 15 s, 25 AB mag/visit Photometric precision: 0.01 mag absolute 10 % of the time will be devoted to deep drilling

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LSST @ Cerro Pachon 10 km away from CTIO/Cerro Tolo; 0.67 mean seeing; 80% clear nights

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The Telescope 8.4 m diameter 9.6 sq.deg FOV 3.2x10 9 pixels 15 s exposures 2 s readout time

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Optic design for 3.5 deg FoV 8.4 m (primary) 5 m (tertiary) 6.7 m effective diameter

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The Camera

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Simulation Simulation is used to evaluate analysis pipeline & algorithms as well as optimize system sensitivity

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Simulation Example: 4k X4k LSST CCD 15 sec exposures in gr&i

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Sky coverage

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Data managment (challenge) 15 TB per night 5.6 PB image data/yr 0.6 PB catalog data /yr 60 seconds alert latency

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LSST Science Book Contents: Introduction LSST System Design System Performance Education and Public Outreach The Solar System Stellar Populations Milky Way and Local Volume Structure The Transient and Variable Universe Galaxies Active Galactic Nuclei Supernovae Strong Lenses Large-Scale Structure Weak Lensing Cosmological Physics Version 2.0, arXiv:0912.0201 http://www.lsst.org/lsst/scibook

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Transient events

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Cosmic transients Example: orphan afterglows

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Supernovae

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Supernovae of Type Ia Example lightcurves from the MAIN survey

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Supernovae of Type Ia Example lightcurves from the DEEP survey

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SN Ia photometric redshifts (from simulations) z =0.007 =0.16

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SN cosmology: BAO & D l Example: equation of state w(z)=w 0 +w a xz(1+z) -1

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Large scale structure Total: ~10 10 galaxies 4x10 9 golden galaxies with i < 25 mag

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Large scale structure Total: ~10 10 galaxies 4x10 9 golden galaxies with i < 25 mag Photometric redshift errors: z 0 (1+z) with 0 0.02

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Large scale structure Total: ~10 10 galaxies 4x10 9 golden galaxies with i < 25 mag Photometric redshift errors: z 0 (1+z) with 0 0.02 Power-weighted eff. volume:

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Strong lensing Galaxy-galaxy lensing from the CFHTLS 4 deg 2 CFHTLS LSST 10 yr stack 170deg 2 CFHTLS single visit Galaxy-Galaxy lenses: ~10 4 (compared to 15 from CFHTLS) Galaxy-lensed Quasars: ~2600 (compared to 32 from SDSS) Galaxy lensed Supernovae: 330 (none identified so far) Cluster lensed galaxies: ~10 3 (1 multiple image system)

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Strong lensing Example application: Time delay & H 0 e.g. S. Suyu et al., ApJ 2010 H 0 =70.63.1 kms -1 Mpc -1 Fassnacht et al 2002 Today: individual objectsLSST: ~ several hundred obj

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Weak lensing Example: lensing power spectra from galaxies Multiple images of same field with different instrument roation, dither position, seeing,..., reduces systematics errors z