LSST Program and Development Status

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LSST Program and Development Status

• Kirk Gilmore
• SLAC/KIPAC/LSST

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Overview of Financial Data FY2008
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Overview of Financial Data 2007-2010
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LSST 2010
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Summary of LSST project progress since last DOE
Program Review

• Recent Project and Camera DevelopmentsA. 20M
  award from Charles Simonyi 10M from Bill Gates
  - Primary/Tertiary mirror fabricationB. 1.5M
  from Keck Foundation and 1.2M from Eric Schmidt
  (Google CEO) Total 2.7M - Sensor prototyping
  (RFP)C. Conceptual Design Review in September
  07 (CoDR-NSF)D. IN2P3 (France) involvement is
  evolving (600K MS in 08/09 in-kind FTE)E.
  AAS in Austin - 28 Posters (on http//www.lsst.org
  ) SPIE in Marseille - 12 Papers on LSST
• Camera ScheduleA. Currently in RD - 53
  people/14 institutions and universitiesB.
  Anticipated transition to MIE (construction) in
  2010C. Telescope first light 2014D. System
  first light 2015E. Full science in 2016
• Camera BudgetA. Working primarily with SLAC MS
  B. Using budget to support reviews via
  prototyping and analysis MS and labor and
  FPT to outside institutionsC. IN2P3 ramping up
• ScienceA. Science collaborations (10) starting
  to engage and establish projectsB. Science
  Requirements Document established
• 5. LSST Project/camera related EventsA.
  P5B. LSST Project All-hands meeting in May
  (150 people)B. PDR (NSF) 2nd qtr FY09 CD-1
  (DOE) same time

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LSST is motivated by massively parallel
astrophysics to answer a wide range of todays
pressing questions in cosmology and fundamental
physics
Astronomy
LSST From Science Drivers to Reference Design
to anticipated Data Products Ivezic et.
al. 2008 Astro-ph 0805.2366
Endorsed by several NAS panels and reports on
astronomy and high energy physics 2000-2002
Community Committee Developed Towards the LSST
Design Reference Mission Strauss et. al. 2004
LSST Science Requirements Document LSST Science
Council www.lsst.org 2006
LSST
Physics
LSST probes 100x fainter enables the
exploration of the time domain.
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LSST Science Requirements focus on 4
Representative and Divergent Programs
Dark Energy-Dark Matter
Exploring our Solar System
LSST enables multiple investigations into our
understanding of the universe
LSST will find 90 of hazardous NEOs down to 140
m in 10 yrs
Movie of the Universe time domain
Mapping the Milky Way
Discovering the transient and unknown on multiple
time scales
LSST will map the rich and complex structure of
our Galaxy.
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Key LSST Mission Dark Energy
Precision measurements of all four dark energy
signatures in a single data set. Separately
measure geometry and growth of dark matter
structure vs cosmic time.

• Weak gravitational lensing correlations
• (multiple lensing probes!)
• Baryon acoustic oscillations
• Counts of dark matter clusters
• Supernovae to redshift 0.8
• (complementary to JDEM)
• Probe anisotropy! LSST unique

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LSST Science Collaborations

1. Supernovae M. Wood-Vasey (CfA)
2. Weak lensing D. Wittman (UCD) B. Jain (Penn)
3. Stellar Populations Abi Saha (NOAO)
4. Active Galactic Nuclei Niel Brandt (Penn State)
5. Solar System Steve Chesley (JPL)
6. Galaxies Harry Ferguson (STScI)
7. Transients/variable stars Shri Kulkarni
   (Caltech)
8. Large-scale Structure/BAO Hu Zhan (UCD)
9. Milky Way James Bullock (UCI) Beth Willman
   (CfA)
10. Strong gravitational lensing Phil Marshall
    (UCSB)

200 signed on already, from member institutions
and project team.
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The LSST Project is a Complete SystemImage,
Analysis, Archive, Publish and Outreach
Camera
Telescope and Site
Cerro Pachon La Serena
Education and Public Outreach
Data Management
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24 LSSTC US Institutional Members

• Brookhaven National Laboratory
• California Institute of Technology
• Carnegie Mellon University
• Columbia University
• Google Inc.
• Harvard-Smithsonian Center for Astrophysics
• Johns Hopkins University
• Las Cumbres Observatory
• Lawrence Livermore National Laboratory
• National Optical Astronomy Observatory
• Princeton University
• Purdue University

• Research Corporation
• Rutgers University
• Stanford Linear Accelerator Center
• Stanford University KIPAC
• The Pennsylvania State University
• University of Arizona
• University of California, Davis
• University of California, Irvine
• University of Illinois at Champaign-Urbana
• University of Pennsylvania
• University of Pittsburgh
• University of Washington

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LSST has submitted an NSF proposal for 242 M of
Construction funding

• Construction proposal submitted in February 2007
• 60 Month Construction and Commissioning
• Ready for MREFC Funds in FY2010 - Expect in FY
  2011
• Proposed as Public Private Partnership to Share
  costs
• NSF MREFC - 242 M
• DOE HEP - 50 M
• Private - 100 M
• Current Design and Development
• NSF 4yr Award 14.2 M
• DOE Lab Participation
• Partner In-Kind
• Private Donation
• Operations and Maintenance
• Summit, Base, Archive, Data Centers 45 M/yr
  (2016)

(FY06 with Contingency)
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The LSST build plan is set
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Data Management is a distributed system that
leverages world-class facilities and
cyber-infrastructure
Archive Center NCSA, Champaign, IL 100 to 250
TFLOPS, 75 PB
Data Access Centers U.S. and Chile 45 TFLOPS, 87
PB
Mountain Summit/Base Facility Cerro Pachon, La
Serena, Chile 25 TFLOPS, 150 TB
Long-Haul Communications Chile - U.S. 2.5 Gbps
avg, 10 Gbps peak
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• Four Main Science Themes for LSST
• 1. Constraining Dark Energy and Dark Matter
• 2. Taking an Inventory of the Solar System
• 3. Exploring the Transient Optical Sky
• 4. Mapping the Milky Way
• Major Implications to the Camera
• Large Etendue
• Excellent Image Quality and Control of PSF
  Systematics
• High Quantum Efficiency over the Range 320
  1,050 nm
• Fast Readout

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LSST Camera Deliverable Org Chart
SLAC/LSST MS to outside institutions via
Financial Plan Transfer
Calibration Burke (SLAC) WBS 3.5.1
Electronics Oliver (Harvard) WBS 3.5.8
Optics Olivier (LLNL) WBS 3.5.5
Cryostat Assembly Schindler (SLAC) WBS 3.5.7
Utilities Nordby (SLAC) WBS 3.5.2
Sensor/Raft Development Radeka/OConnor (BNL) WBS
3.5.4
Camera Body Mechanisms Nordby (SLAC) WBS 3.5.3
Data Acq. Control Schalk (UCSC) WBS 3.5.6
Sensors/Filters Pain/Antilogus (IN2P3) LPNHE,
LAL, APC, LPSC, LMA
Corner Raft WFS/Guider Olivier (LLNL) WBS 3.5.9

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The LSST Camera Team 72 People from 16
Institutions

Brandeis University J. Besinger, K.
Hashemi Brookhaven National Lab S. Aronson, C.
Buttehorn, J. Frank, J. Haggerty, I. Kotov, P.
Kuczewski, M. May, P. OConnor, S. Plate, V.
Radeka, P. Takacs Florida State University
Horst Wahl Harvard University N. Felt, J.
Geary (CfA), J. Oliver, C. Stubbs IN2P3 - France
R. Ansari, P. Antilogus, E. Aubourg, S.
Bailey, A. Barrau, J. Bartlett, R. Flaminio, H.
Lebbolo, M. Moniez, R. Pain, R. Sefri, C. de la
Taille, V. Tocut, C. Vescovi Lawrence Livermore
National Lab S. Asztalos, K. Baker, S. Olivier,
D. Phillion, L. Seppala, W. Wistler Oak Ridge
National Laboratory C. Britton, Paul
Stankus Ohio State University K. Honscheid, R.
Hughes, B. Winer
Purdue University K. Ardnt, Gino Bolla,
J, Peterson, Ian Shipsey Rochester Institute of
Technology D. Figer Stanford Linear Accelerator
Center - G. Bowden, P. Burchat
(Stanford), D. Burke, M. Foss, K. Fouts, K.
Gilmore, G. Guiffre, M. Huffer, S. Kahn
(Stanford), E. Lee, S. Marshall, M. Nordby, M.
Perl, A. Rasmussen, R. Schindler, L. Simms
(Stanford), T. Weber University of California,
Berkeley J.G. Jernigan University of
California, Davis P. Gee, A. Tyson University
of California, Santa Cruz T. Schalk University
of Illinois, Urbana-Champaign J. Thaler
University of Pennsylvania M. Newcomer, R. Van
Berg
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Major camera risk mitigation scheduled prior to
construction are buying down risk
RD Effort Plan Status
Demonstrate sensor performance Establish all specs are met Flatness, high fill factor, electrical parameters, mechanical packaging Study phase sensors received and being evaluated. Prototype contracts being generated.
Efficient sensor procurement Establish cost, yield and performance of sensors POs being drafted that address risk areas. Prototype phase starting
Establish reliability of shutter and filter mechanisms Build prototype mechanisms and test Design completed. Procurement of parts begun
Evaluate outgassing properties of cryostat components Contamination control demonstrated in engineering cryostat Contamination testing started. Materials selection process begun.
75cm filter w/multilayer coatings produced with non-uniformity of lt1 . Fabrication of samples in large coating chamber to evaluate uniformity of filter transmission Passbands defined. Total system throughput modeled. Some witness samples already produced. RFP to potential vendors ready.
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BNL and sensor group are providing leadship for
schedule driven sensor development

• Request for proposals for prototype
  science CCDs
• issued Feb. 2008
• contract award June/July 2008
• 5 high-resistivity, thick CCDs from study
  program have been extensively
  characterized
• design models validated
• behavior of dark current, quantum efficiency,
  and point spread function vs. thickness,
  temperature, and electric field
• flatness and surface morphology
• antireflection coating
• CCD controllers for 4 new test labs under
  construction
• UC Davis, SLAC, Paris, Purdue
• allows full-speed testing of segmented sensors
• Components for CCD/electronics chain testing
  in assembly (Raft/Tower electronics
  prototype by end of year

X-ray images
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• RFP for Prototyping Filters in 08

Specs
Half-Maximum Transmission Wavelength

• 75 cm dia.
• Curved surface
• Filter is concentric about the chief ray so
  that all portions of the filter see the same
  angle of incidence range, 14.2º to 23.6º

• Filter RFP being sent out to selected
  vendors
• Filter prototyping will qualify vendors to
  fabricate science filters

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Contamination test chamber at SLAC
Other major efforts using SLAC resources
Camera Controls
Main Chamber
MAIN
FORE
Working is proceeding on plans to deliver a
prototype test stand by end of calendar year
2008 - Goal by PDR
Fore or Preparation Chamber
cold finger
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IN2P3 - France RD support for camera development
CNRS - National Center for Scientific
Research IN2P3 - National Institute for Nuclear
Physics and Particle PhysicsAPC - Lab for
Astroparticles and Cosmology (Paris) -
Calibration/CCS CC-IN2P3 - Computing Center of
IN2P3 (Lyon) - Computing Facilities LAL - Lab of
Linear Accelerator (Orsay) - Electronics LMA -
Lab of Advanced Materials (Lyon) - Filters LPSC -
Lab for Subatomic Physics and Cosmology
(Grenoble) - Calibration LPNHE - Lab for Nuclear
Physics and High Energy (Paris) - Sensors/Elec.
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Camera construction costs by sub-system