LSST Project Status
Kirk Gilmore
LSST Camera Scientist
October 1, 2008
Project activities since the NSF CoDR
– Activity focused on preparation for PDR and CD-1
– Full review of project baseline, schedule, and cost estimates
– Business preparation for LSSTC to receive funds directly
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Primary/tertiary mirror cast in March, 2008 with private funds
Secondary mirror blank acquisition from Corning
LSSTC membership has grown to 24 members
Completed favorable agreement for site in Chile
Sensor prototype contracts with $3M in private funding
First significant international participation by IN2P3
Third LSST All Hands Meeting at NCSA with significant
scientific and technical progress reported
Penn
October 1, 2008
2
LSST mirror casting “high fire” celebration was held
March 29 at the UofA
Penn
October 1, 2008
3
Primary mirror casting will reach room temperature
in about 30 days
LSST Casting Schedule
1200
High Temperature 3/29/08 20:21
Temperature (C)
1000
800
600
Start Rotation 3/28/08 22:36
Anneal
400
200
Start Casting 3/23/08 16:00
0
3/23 3/30 4/6 4/13 4/20 4/27 5/4 5/11 5/18 5/25 6/1
6/8 6/15 6/22 6/29 7/6 7/13
Date
112 Day casting cycle
Penn
October 1, 2008
4
Preliminary design of the dome has been a focus this
period – working closely with EIE (VLT vendor)
Revised vent openings
Wind screen is tighter at
corners and more efficient
Structural support up front
and new door in back
Penn
October 1, 2008
5
3-D view of El Peñón summit (at top)
& calibration hill (in the right foreground)
With platforms
prepared
Penn
October 1, 2008
6
One of the best accomplishments on Site since CoDR is
courtesy of Google Earth – Now in Hi Res!
Penn
October 1, 2008
7
Effort on site has focused on civil engineering and
characterization of conditions
• Civil Engineering contract in place with ARCADIS
Geotécnica to design rough excavation process
• Engineers on site May 8th to kick-off effort
Penn
October 1, 2008
8
Two of the study contract CCD devices
Both 100mm thick, high resistivity bulk silicon,fully depleted
E2V
STA/ITL
2K x 4K, 13.5mm pixels, 2 outputs
4K x 4K, 10mm pixels, 16 outputs
Penn
October 1, 2008
9
Imaging data from study contract devices
e2V
STA/ITL
2K x 512, 13.5mm pixels,
single output mode
4K x 4K, 10mm pixels, 16 outputs
4cm
Penn
October 1, 2008
10
Summary of study phase
Science driver
Technology Advance
Criterion
Vendor
1
Vendor
2
Broadband, high QE
Thick silicon, fully depleted
QE(1000nm) > 30%
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Transparent back contact
QE(400nm) > 40%

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Low charge diffusion
< 3.2mm rms
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Small pixel size
10mm (0.2")
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Low read noise
< 5 e- rms
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Low dark current
< 2 e-/pix/s
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Low persistence
< 10-4
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High full well
> 90,000 e-
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Flat silicon surface
< 5mm p-v
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TTP-controlled package
< 6.5mm over raft
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Multiport output
(4K)2, 16 output
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High fill factor die & pkg
> 93%
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Seeing-limited image quality
High throughput
 meets LSST spec
 does not meet spec
– not addressed
? not yet measured
Penn
October 1, 2008
11
Calypso at Kitt Peak is available to validate
LSST calibration for photometric accuracy
Penn
October 1, 2008
12
LSST is driving the new Mike Stonebreaker
startup Scientifica for XLDB
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“Big science” unhappy with commercial RDBMS Systems
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Astronomy, High Energy Physics, Fusion, Bio, BioMed, Chemistry, Remote
sensing, etc.
Scientists forced to “roll their own” database systems to suit their specific needs
for new projects OR limit scale of their science to limitations of commercial RDBM
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Realization that “Roll your own DB” is long term suicide– many Terabytes
moving to Petabytes
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Shouldn’t limit Science based on capabilities of existing commercial DB
systems which were designed 25 years ago
Recognition that Opensource is framework to aggregate requirements and
resources to build DB system for Big Science for long term
Penn
October 1, 2008
13
Core Partners – Computer Science/DBMS
Mike
Stonebraker (MIT)
Dave
Dewitt (Wisconsin -> Microsoft)
Jignesh
Dave
Patel (Wisconsin)
Maier (Portland State)
Stan
Zdonik (Brown)
Sam
Madden (MIT)
Ugur
Cetintemel (Brown)
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Partners -- Other
Talking
to:
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E-Bay
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Amazon
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Yahoo
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Google
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Microsoft
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A few enabling characteristics of Scientifica
•Open Source
•MatLab-like syntax
•User extendable operations
•Provenance embedded
•Scalable to Petabytes
•Embedded Computations
•Data are tagged with uncertainty parameters
•Cloud computing with fault tolerance
Penn
October 1, 2008
16
Community Development & NewCo
Beta Ships
Alpha System
Add Partners?
Design Specification
Finalize Founding Partners
Formalize Company
Begin Recruiting
Begin Coding
Q3
Q4
2008
Q1
Q2
Q3
Q4
2009
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The current LSST timeline
FY-07
FY-08
FY-09
FY-10
FY-11
FY-12
FY-13
FY-14
FY-15
FY-16
FY-17
NSF D&D Funding
MREFC Proposal Submission
NSF CoDR
MREFC Readiness
NSF PDR
NSB
NSF CDR
NSF MREFC Funding
Telescope First Light
NSF + Privately Supported Construction (8.5 years)
System First Light
Commissioning
ORR
Operations
DOE Operating
Funds
Privately Supported camera R&D
DOE MIE Funding
DOE + Privately Supported Fabrication (5 years)
DOE R&D Funding
Sensor Procurement Starts
DOE CD-3
DOE CD-4
Camera Delivered to Chile
Camera Ready to Install
DOE CD-2
DOE CD-0
DOE CD-1
Penn
October 1, 2008
18
LSST Science, Data Policy, Collaborations
Tony Tyson
LSST Director
UC Davis
NSF
June 11, 2008
NSF
June 11, 2008
20
Relative Survey Power
320
15 sec exposures
240
2000 exposures per field
200
20,000 square degrees
2
2
Etendue (m deg )
280
160
120
80
40
0
LSST
PS4
PS1
Subaru
CFHT
SDSS
MMT
NSF
June 11, 2008
DES
x0.3
4m
VST
VISTA
IR
SNAP
x2
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One quarter the diameter of the moon
DSS: digitized photographic plates
NSF
June 11, 2008
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Sloan Digital Sky Survey
NSF
June 11, 2008
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Deep Lens Survey
NSF
June 11, 2008
24
LSST imaging & operations simulations
Sheared HDF raytraced +
perturbation + atmosphere +
wind + optics + pixel
Figure : Visits numbers per field for the 10 year simulated survey
LSST Operations, including real
weather data: coverage + depth
Performance verification using Subaru imaging
NSF
June 11, 2008
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Comparing HST with Subaru
ACS: 34 min (1 orbit)
PSF: 0.1 arcsec (FWHM)
NSF
June 11, 2008
2 arcmin
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Comparing HST with Subaru
Suprime-Cam: 20 min
PSF: 0.52 arcsec (FWHM)
NSF
June 11, 2008
27
LSST survey of 20,000 sq deg
• 3 billion galaxies with redshifts
• Time domain:
1 million supernovae
1 million galaxy lenses
5 million asteroids
new phenomena
NSF
June 11, 2008
28
LSST Science Charts New Territory
Probing Dark Matter
And Dark Energy
Mapping the Milky Way
Finding Near Earth Asteroids
NSF
June 11, 2008
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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
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(multiple lensing probes!)
Baryon acoustic oscillations
Counts of dark matter clusters
Supernovae to redshift 0.8
(complementary to JDEM)
Probe anisotropy! LSST unique
NSF
June 11, 2008
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Dark Energy Error vs Etendue-Time
Separate DE Probes
Combined
NSF
June 11, 2008
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Comparison of Stage-IV facilities for DE
NSF
June 11, 2008
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Testing more general dark energy models
growth
distance
NSF
June 11, 2008
Zhan, Knox, Tyson 2008
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Formation of our Galaxy and Group
SDSS
LSST
NSF
June 11, 2008
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Moving objects: Solar System near and far
Deep Lens Survey
NSF
June 11, 2008
35
Near Earth Objects
• Inventory of solar system is incomplete
• LSST would get orbits of nearly all NEOs
larger than 150m
• Demanding project: requires mapping the sky
down to 24th magnitude every few days,
individual exposures not to exceed 15 sec
NSF
June 11, 2008
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PHA completeness
NSF
June 11, 2008
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Optical flashes
difference
Deep Lens Survey
NSF
June 11, 2008
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Unknown Unknowns
NSF
June 11, 2008
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Massively Parallel Astrophysics
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Dark matter/dark energy via weak lensing
Dark energy via baryon acoustic oscillations
Dark energy via supernovae
Galactic Structure encompassing local group
Dense astrometry over 20000 sq.deg: rare moving objects
Gamma Ray Bursts and transients to high redshift
Gravitational micro-lensing
Strong galaxy & cluster lensing: physics of dark matter
Multi-image lensed SN time delays: separate test of cosmology
Variable stars/galaxies: black hole accretion
QSO time delays vs z: independent test of dark energy
Optical bursters to 25 mag: the unknown
5-band 27 mag photometric survey: unprecedented volume
Solar System Probes: Earth-crossing asteroids, Comets, TNOs
Planetary transits
LSST Overview: Astro-ph/0805.2366
NSF
June 11, 2008
40
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.
New Science Opportunities
Go beyond survey for known phenomena.
Consider discovery potential for
“unknown unknowns”
Design survey to maximize opportunity in
unexplored parts of flux-time-color-position
space.
Opportunities enabled via open data.
NSF
June 11, 2008
42
Value
What makes LSST and its data products uniquely valuable?
• Unprecedented survey (2000 x SDSS plus time domain)
20 billion objects
• High precision, high uniformity
• Open source, open data
• Bridge to CS, Math, Stat
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Cyber-enabled Discovery and Innovation
Promotes and enables research
Leverages existing facilities
Needed now
Movie of the universe opens new windows
Broader impact
NSF
June 11, 2008
43
LSST Repeatedly Ranked High Priority
• NRC 2000 Astronomy Decadal Survey
• NRC New Frontiers in the Solar System
• NRC Quarks-to-Cosmos
• SAGENAP
• Quantum Universe
• Physics of the Universe
• Dark Energy Task Force + P5 + HEPAP
NSF
June 11, 2008
44
US Federal Agency participation
LSST Telescope / Site / Data System:
NSF AST Wide range of astronomy and physics from LSST.
Open data / open source. Breakthrough Astronomy.
LSST Camera:
DOE HEP Dark energy. Multiple unique wide-deep probes.
Possible 100x - 1000x increase in sensitivity over DETF “Stage III”
Share of operations:
NASA Potentially Hazardous Asteroid survey mandated by Congress.
Future share of operations?
NSF
June 11, 2008
45
P5 report at HEPAP May 2008
NSF
June 11, 2008
46
24 LSSTC US Institutional Members
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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
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NSF
June 11, 2008
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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Foreign participation
• IN2P3 France (camera focal plane & electronics)
• All Europe interested (synergy with VLT spectroscopy)
German consortium
Astronet document assumes LSST data
ESO plans LSST data access & spectroscopic facility
UK consortium
Liverpool meeting next month
• Chilean astronomy community joining
NSF
June 11, 2008
48
Transformative Data Products
• Calibration and Quality Assessment
Database must be high quality
The utility of our data will be enabled. Avoid releasing garbage!
• Open Data / Open Source
Transient alerts - world public instantly
Validated metadata releases
2008 NRC study: Data Integrity in the Petascale Era
NSF
June 11, 2008
49
IT CEOs at LSST High Fire event
NSF
June 11, 2008
50
Readiness
1. LSST will transform astronomy and accordingly has broad support
(community, science collaborations, member institutions, etc.)
2. It will have a major impact on many other fields: high energy
physics, the congressional mandate on asteroids, the database
initiative, science education
3. The cost / performance risk to the NSF is low
4. We are actively exploring sharing operations costs
5. We are ready
NSF
June 11, 2008
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