Transcript of Ultimate wide field Imaging: The Large Synoptic Sky Survey Marek Kowalski Physikalisches Institut...
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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