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Ultimate w ide f ield Imaging : The Large Synoptic Sky Survey

Ultimate w ide f ield Imaging : The Large Synoptic Sky Survey. Marek Kowalski Physikalisches Institut Universit ät Bonn. Disclaimer. This is not a “for the LSST collaboration” talk ( but all plots /numbers are from LSST public domain). LSST Institutions.

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Ultimate w ide f ield Imaging : The Large Synoptic Sky Survey

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  1. UltimatewidefieldImaging:The Large Synoptic Sky Survey Marek Kowalski Physikalisches Institut Universität Bonn

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

  3. LSST Institutions Adler Planetarium, BrookhavenNational Laboratory (BNL), CaliforniaInstitute of Technology, Carnegie Mellon University, Cornell University, Drexel University,George Mason University, Google, Harvard-Smithsonian Center forAstrophysics, Institut de PhysiqueNucléaire et de Physique des Particules (IN2P3), Johns Hopkins University, KavliInstitute forParticleAstrophysics and Cosmology (KIPAC) - Stanford University,Las CumbresObservatory Global TelescopeNetwork, Lawrence Livermore National Laboratory (LLNL), Los Alamos National Laboratory (LANL), National OpticalAstronomyObservatory, Princeton University, PurdueUniversity, Research Corporation for Science Advancement, Rutgers, SLAC National Accelerator Laboratory, SpaceTelescope Science Institute, Texas A & M University, ThePennsylvania State University, TheUniversity 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

  4. Thesurvey • 6-band Survey: ugrizy 320–1080 nm • Sky area covered: > 20,000 deg2, 0.2 arcsec / pixel • 10-Year Duration: Yields 27.7 AB magnitude @ 5σ • 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

  5. LSST @ Cerro Pachon10 km awayfrom CTIO/Cerro Tolo;0.67“ meanseeing; 80% clearnights

  6. TheTelescope 8.4 m diameter 9.6 sq.degFOV 3.2x109pixels 15 s exposures 2 s readout time

  7. Opticdesignfor 3.5 degFoV 8.4 m (primary) – 5 m (tertiary) 6.7 m effectivediameter

  8. The Camera

  9. The Camera

  10. Simulation Simulation isused to evaluateanalysispipeline & algorithms as well as optimizesystemsensitivity

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

  12. Sky coverage

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

  14. LSST Science Book Version 2.0, arXiv:0912.0201 http://www.lsst.org/lsst/scibook • Contents: – Introduction – LSST System Design – System Performance – Education and Public Outreach – The Solar System – Stellar Populations – Milky Way and LocalVolumeStructure – TheTransient and Variable Universe – Galaxies – ActiveGalacticNuclei – Supernovae – StrongLenses – Large-ScaleStructure – WeakLensing – CosmologicalPhysics

  15. Transientevents

  16. Cosmictransients Example: orphanafterglows

  17. Supernovae

  18. Supernovae of Type Ia ExamplelightcurvesfromtheMAIN survey

  19. Supernovae of Type Ia ExamplelightcurvesfromtheDEEP survey

  20. SN Iaphotometricredshifts(fromsimulations) σz=0.007 σμ=0.16

  21. SN cosmology: BAO & DlExample: equation of state w(z)=w0+waxz(1+z)-1

  22. Large scalestructure Total: ~1010 galaxies 4x109 „golden“ galaxies with i < 25 mag

  23. Large scalestructure Total: ~1010 galaxies 4x109 „golden“ galaxies with i < 25 mag Photometricredshifterrors: σz≈σ0(1+z)withσ0 ≈0.02

  24. Large scalestructure • Total: ~1010 galaxies • 4x109 „golden“ galaxies with i < 25 mag • Photometricredshifterrors: σz≈σ0 (1+z) withσ0 ≈0.02 • Power-weightedeff. volume:

  25. Stronglensing Galaxy-Galaxylenses: ~104 (compared to 15 from CFHTLS) Galaxy-lensed Quasars: ~2600 (compared to 32 from SDSS) Galaxylensed Supernovae: 330 (noneidentified so far) Cluster lensedgalaxies: ~103 (≥1 multiple image system) Galaxy-galaxylensingfromthe CFHTLS 4 deg2 CFHTLS ⇔ LSST 10 yrstack deg2 CFHTLS ⇔ singlevisit

  26. Stronglensing Today: individualobjects LSST: ~ severalhundredobj Fassnacht et al 2002 e.g. S. Suyu et al., ApJ 2010 ⇒ H0=70.6±3.1 kms-1Mpc-1 Exampleapplication: Time delay & H0

  27. Weaklensing Example: lensing power spectrafromgalaxies z<0.7 0.7<z<1.2 z>1.2 Multiple images of samefieldwith differentinstrumentroation,ditherposition,seeing,...,reducessystematicserrors

  28. Cosmologicalparameters Example: equation of state w(z)=w0+waz(1+z)-1

  29. Neutrino massconstraints factor 4 improvementover Planck alone mtotal≥0.05eV

  30. Neutrino massconstraints* - total versuslightestneutrinomass factor 4 improvementover Planck alone *assuming Planck priors;

  31. ProjectTimeline

  32. Conclusion & Outlook LSST is ranked first in the 2010 decadal survey with a strong recommendation for immediate submission of funding application to NSF & DOE Strong US collaboration has formed, France joined but no German groups involved (yet) Extraordinary science opportunities for astronomy, cosmology & physics Very detailed, up-to-date information on the project: http://www.lsst.org/lsst/scibook

  33. Backup

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