The Large Synoptic Survey Telescope (LSST) Presentation to the Experimental Program Advisory Committee at SLAC November 14, 2003 LSST Camera Project SLAC EPAC Meeting Nov.
Download ReportTranscript The Large Synoptic Survey Telescope (LSST) Presentation to the Experimental Program Advisory Committee at SLAC November 14, 2003 LSST Camera Project SLAC EPAC Meeting Nov.
LSST Camera Project
The Large Synoptic Survey Telescope (LSST)
Presentation to the Experimental Program Advisory Committee at SLAC November 14, 2003 SLAC EPAC Meeting Nov. 14-15, 2003 1
The Large Synoptic Survey Telescope
•
The LSST will be a large, wide-field ground-based telescope designed to survey the entire visible sky every few nights.
•
This project concept has been strongly endorsed by three
separate National Academy committee reports: Astronomy and
Astrophysics in the New Millennium, New Frontiers in the Solar
System, and Connecting Quarks with the Cosmos. •
LSST will enable a wide variety of complementary scientific investigations, utilizing a common database. These range from searches for small bodies in the solar system to precision astrometry of the outer regions of the galaxy to systematic monitoring for transient phenomena in the optical sky.
•
Of particular interest to HEP, LSST will constrain models of dark energy vs. cosmic time by measuring the dark matter power spectral density via weak lensing.
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 2
SLAC Involvement in LSST
•
The Kavli Institute for Particle Astrophysics and Cosmology (KIPAC) has chosen to emphasize dark matter and dark energy as key focus areas for its experimental program at SLAC.
•
We believe it is essential to probe the standard cosmological model on multiple “fronts”, i.e. not only constraining parameters, but testing for internal consistency via disparate measurement techniques.
•
LSST is an excellent complement to SNAP. By participating in BOTH projects, we believe that SLAC will be ideally positioned to play a key role in the next wave of cosmological discovery.
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 3
Outline of Presentations
•
Probing Dark Energy with LSST – A. Tyson
•
The Design and Development of the LSST Camera – W. Althouse
•
LSST Project Organization – S. Kahn LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 4
LSST probes of DE
1.
Number counts vs. redshift:
N(M,z) *Comoving Volume element
dV/dzd
*Growth rate of density perturbations
(z) Counts of mass clusters: 3-D tomography
2.
Shear Tomography
: <
g(
z
1
)
g(
z
2
)> 3. Sachs-Wolfe effect:
g(
z)>
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 6
mass structure vs time
LSST Camera Project 3 billion lyr SLAC EPAC Meeting Nov. 14-15, 2003 7 billion lyr 7
Weak Gravitational Lensing
• •
Over 250,000 resolved hi-redshift galaxies per square degree Each is moved on the sky and distorted LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 8
Strong lensing
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 9
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 10
Mass Cluster @ z = 0.5
Cluster Tomography
Source Redshift Distribution Distant Source Galaxies Foreground Source D lens D source Lens Strength z source Lens Strength z lens = 0.5
The blue galaxy is sheared more than the red galaxy.
The green galaxy is not sheared.
z source
Tomographic mass slices in z
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 12
Observed mass: 2x2 degree field
z = .7
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 13
DLS 1055-05
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 14
mass – baryon correlation?
DLS mass map CXO .5-4 keV
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 15
Mass Cluster Counting
•
The mass function is steep and exponentially sensitive to errors in
M
limit (z) and uncertainty in M(observables,z).
•
Measure mass function, determine
M
limit (z) from LSST cluster survey, devise a test that is insensitive to the limiting mass. LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 16
Cluster Counting
• Goal: Determine cosmological parameters by comparing the observed distribution of clusters to predictions from theory/N-body simulations • However cluster mass is not an observable. Instead we measure: SZ decrement X-rays (L X or T X ) Optical Richness Galaxy v Shear g
No baryon bias
• To interpret the observations we must know
M
( observables,z ) Completeness( observables,z )
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 17
QCDM or LCDM?
Normalized Cluster Redshift Distribution QCDM LCDM
• Redshift distributions differ at a high statistical significance • Lensing kernel is broader for LCDM and probes a broader range of z and M than QCDM •
w precision 2%
• Unlike other cluster counting surveys, this test is ROBUST against uncertainties in mass limit.
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 18
Cosmic shear vs redshift
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 19
LSST shear tomography +
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 20
Precision on DE P/
r
P/
r
= w
0 + w a
(1 a) a = (1+ z) -1
SUGRA L CDM
SNAP SN + Planck LSST WL + WMAP
SNAP WL + Planck
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 21
LSST Weak Lensing survey
Low z WL LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 22
Weak Lensing with LSST Summary
• • • •
An incisive probe of new physics: 3-D tomography / Dark Energy Multiple probes break degeneracies Probes dark energy in multiple ways: w and dw/dz from shear-shear and cluster dN/dz.
m ,
x curves.
Comparison with CMB and with SN1a tests fundamental assumptions LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 23
Controlling Systematics
• • • • •
Need baryon unbiased estimates of cluster mass
shear survey
Minimize delivered PSF shear Chop shear signal multiple ways Large sample of mass clusters Explore mass function
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 24
Figure of Merit
Volume surveyed (number of objects found) to some S/N at some magnitude limit, per unit time:
Science goals Apparatus & Eff.
N t
2 obj
A Ω QE ε (S/N)
2 sky
(
)
site & optics A – aperture
e
– camera FOV QE – det. Eff.
– observing eff.
F
sky – sky flux
– seeing footprint LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 25
Optical Throughput Required
LSST LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 26
Unexplained optical bursts
Deep Lens Survey
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 27
Massively Parallel Astrophysics
LSST DATA PUBLIC
Simultaneously address:
– – – – – – – – – – – – –
Dark matter/dark energy via weak lensing Dark matter/dark energy via supernovae Galactic Structure encompassing local group Dense astrometry over 30000 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 LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 28
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 29
LSST Optics
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 30
Camera Configuration
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 31
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 32
Camera Components
• • • • •
Focal plane array
– –
10 μm pixels
2.3 Gpixels
0.2 arcsecond/pixel (~ 1 / 3 55 cm diameter
3 ° FOV seeing-limited PSF)
– –
integrated front-end electronics 16 bits/pixel, 2 sec readout time
Parallel readout
2.3 GB/sec Housings (environmental control) Filters Optics Mechanisms
– – –
L2 position varies with wavelength (filter) Filters insertion mechanical shutter LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 33
Camera Challenges
• • • • • •
Detector requirements:
–
10 μm pixel size
– – –
Pixel full-well > 90,000 e – Low noise (< 5 e High QE 400 – rms), fast (< 2 sec) readout ( – 1000 nm
< –30 C)
–
All of above exist, but not simultaneously in one detector Focal plane position precision of order 3 μm Package large number of detectors, with integrated readout electronics, with high fill factor and serviceable design Large diameter filter coatings Constrained volume (camera in beam)
–
Makes shutter, filter exchange mechanisms challenging Constrained power dissipation to ambient
–
To limit thermal gradients in optical beam
–
Requires conductive cooling with low vibration LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 34
Camera Challenges (con’d)
• •
Key challenge: Detector technology Main choices: CCD, hybrid CMOS
–
CCDs:
• • • •
Monolithic Si array Routinely used for visible astronomical applications Have been made in high-resistivity, thick format (to achieve sensitivity at 1 μm wavelength) with 15 μm pixel density Slow readout: need ~10 μs per pixel to achieve noise level
–
Hybrid CMOS:
•
Hybrid array uses thin planar detector with pixelated back contact “bump bonded” to CMOS readout multiplexer
•
Routinely used for infrared astronomy (with different photo conversion material)
• • •
Avoids need for mechanical shutter Can integrate substantial electronics on-chip Low power (< 1/100 of CCD) & Fast readout LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 35
Camera Challenges (con’d)
•
Control of systematics
–
Lensing studies exploit subtle, systematic image distortions caused by dark matter
–
Time dependent or environmentally induced distortion in the measuring system (telescope + camera) could mask the lensing signature
–
May place unusual demands on camera development, particularly testing to ensure acceptable control/knowledge of end-to-end transfer function LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 36
LSST Management Plan
•
In March 2003, four organizations (U. of Washington, U. of Arizona, the
Research Corporation, and NOAO) formed the LSST Corporation (LSSTC), a non-profit 501C3 Arizona corporation. •
The purpose of LSSTC is to pursue a shared vision for the nature of the LSST endeavor, and a commitment to advance the project through technical, scientific, and/or financial contributions. LSSTC plans to expand its institutional membership as the project progresses.
•
As presently envisioned, funding for the construction of the LSST will come from NSF, DOE, and private donors. Significant commitments of private funding are already in hand. A proposal to NSF for design & development phase funding will be submitted in December 2003.
•
While LSST is a distributed project, there is a single management plan. All participating organizations will be coordinated and accountable to the LSST Director and Project Manager, who are appointed by the LSSTC Board of Directors.
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 37
DOE Participation in LSST
•
A collaboration of DOE-funded institutions has been formed to pursue participation in LSST. This collaboration has been working closely with other LSST participants under the coordination of the LSST Director and Project Manager.
•
The DOE “deliverable” will be the LSST camera system.
•
SLAC will lead the development of the camera, with significant contributions coming from BNL, LLNL, and DOE-funded university groups (e.g. Harvard, UIUC).
•
Scientists and engineers at these institutions will also participate in the data acquisition system, the development of pipeline software, and the scientific interpretation of the results.
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 38
External Review Board
LSST Project Organization
LSST Corporation Board of Directors
John Schaefer, President
Research Corporation, University of Washington, National Optical Astronomical Observatory, University of Arizona
Executive Advisory Committee
Arthur Bienenstock
Science Assurance System Scientist
Christopher Stubbs
Data: Kem Cook Camera: Steve Kahn Tel/Site: Chuck Claver System Engineering Jacques Sebag LSST Director
Anthony Tyson
Project Manager Donald Sweeney Array Technology
Don Figer, Mike Lesser
Science Advisory Board
Zeljko Ivezic, Philip Pinto
Science Working Groups Project Support
•
Change Control Board
•
Risk Management
•
Project Controls
•
Performance Assurance
•
Administration SW Architecture
Jim Gray, Robert Lupton
Public Outreach Michael Shara, Doug Isbell Data Management
Kem Cook, Sci.
tbd , Mgr.
LSST Camera Project Camera Steve Kahn, Sci.
Bill Althouse, Mgr.
Telescope/Site
Charles Claver, Sci.
Larry Daggert, Mgr.
SLAC EPAC Meeting Nov. 14-15, 2003 39
LSST Camera Project Organization
• • •
Camera Project Support Project Controls & Risk Mgmt Performance & Safety Assur.
Administration Camera S. Kahn, Sci Lead W. Althouse, Proj Mgr System Engineering T. Thurston Lead Mech. Engr T. Decker, LLNL Lead Elect. Engr J. Oliver, Harvard Data Bus W. Althouse (act.) Focal Plane Assy M. May, BNL Optics J. Taylor, LLNL S. Olivier, LLNL Mechanisms L. Hale, LLNL Housing & Structure T. Thurston Camera I&T W. Craig Array, FE Elex V. Radeka, BNL Array Testing D. Figer, STScI M. Lesser, Steward Obs.
Opto-Mech Assy T. Decker, LLNL All SLAC unless otherwise noted LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 40
LSST Design Phase Schedule
OCT 04 OCT 05 OCT 06 OCT 07
Activity / Milestone
FY05 FY 06 FY 07 Optical Design Frozen Science Requirements Document Complete(SRD) Final Site Selection Functional Performance Requirements Doc (FPRD) Interface Requirement Documents Complete (IRD) Order Primary Mirror Glass D & D Funding Begins Conceptual Design Review Order Primary Mirror casting Submit Construction Proposal Mount Design RFQ Place Mount Design contract Dome Design RFQ Select Array Type Preliminary Design Review Construction Funding Approved Site Construcion Begins Order Focal Plane Arrays Place Dome Design / Fab contract
First light Dec. 2011 LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 41
g(
z)>
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 6
mass structure vs time
LSST Camera Project 3 billion lyr SLAC EPAC Meeting Nov. 14-15, 2003 7 billion lyr 7
Weak Gravitational Lensing
• •
Over 250,000 resolved hi-redshift galaxies per square degree Each is moved on the sky and distorted LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 8
Strong lensing
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 9
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 10
Mass Cluster @ z = 0.5
Cluster Tomography
Source Redshift Distribution Distant Source Galaxies Foreground Source D lens D source Lens Strength z source Lens Strength z lens = 0.5
The blue galaxy is sheared more than the red galaxy.
The green galaxy is not sheared.
z source
Tomographic mass slices in z
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 12
Observed mass: 2x2 degree field
z = .7
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 13
DLS 1055-05
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 14
mass – baryon correlation?
DLS mass map CXO .5-4 keV
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 15
Mass Cluster Counting
•
The mass function is steep and exponentially sensitive to errors in
M
limit (z) and uncertainty in M(observables,z).
•
Measure mass function, determine
M
limit (z) from LSST cluster survey, devise a test that is insensitive to the limiting mass. LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 16
Cluster Counting
• Goal: Determine cosmological parameters by comparing the observed distribution of clusters to predictions from theory/N-body simulations • However cluster mass is not an observable. Instead we measure: SZ decrement X-rays (L X or T X ) Optical Richness Galaxy v Shear g
No baryon bias
• To interpret the observations we must know
M
( observables,z ) Completeness( observables,z )
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 17
QCDM or LCDM?
Normalized Cluster Redshift Distribution QCDM LCDM
• Redshift distributions differ at a high statistical significance • Lensing kernel is broader for LCDM and probes a broader range of z and M than QCDM •
w precision 2%
• Unlike other cluster counting surveys, this test is ROBUST against uncertainties in mass limit.
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 18
Cosmic shear vs redshift
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 19
LSST shear tomography +
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 20
Precision on DE P/
r
P/
r
= w
0 + w a
(1 a) a = (1+ z) -1
SUGRA L CDM
SNAP SN + Planck LSST WL + WMAP
SNAP WL + Planck
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 21
LSST Weak Lensing survey
Low z WL LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 22
Weak Lensing with LSST Summary
• • • •
An incisive probe of new physics: 3-D tomography / Dark Energy Multiple probes break degeneracies Probes dark energy in multiple ways: w and dw/dz from shear-shear and cluster dN/dz.
m ,
x curves.
Comparison with CMB and with SN1a tests fundamental assumptions LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 23
Controlling Systematics
• • • • •
Need baryon unbiased estimates of cluster mass
shear survey
Minimize delivered PSF shear Chop shear signal multiple ways Large sample of mass clusters Explore mass function
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 24
Figure of Merit
Volume surveyed (number of objects found) to some S/N at some magnitude limit, per unit time:
Science goals Apparatus & Eff.
N t
2 obj
A Ω QE ε (S/N)
2 sky
(
)
site & optics A – aperture
e
– camera FOV QE – det. Eff.
– observing eff.
F
sky – sky flux
– seeing footprint LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 25
Optical Throughput Required
LSST LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 26
Unexplained optical bursts
Deep Lens Survey
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 27
Massively Parallel Astrophysics
LSST DATA PUBLIC
Simultaneously address:
– – – – – – – – – – – – –
Dark matter/dark energy via weak lensing Dark matter/dark energy via supernovae Galactic Structure encompassing local group Dense astrometry over 30000 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 LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 28
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 29
LSST Optics
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 30
Camera Configuration
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 31
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 32
Camera Components
• • • • •
Focal plane array
– –
10 μm pixels
2.3 Gpixels
0.2 arcsecond/pixel (~ 1 / 3 55 cm diameter
3 ° FOV seeing-limited PSF)
– –
integrated front-end electronics 16 bits/pixel, 2 sec readout time
Parallel readout
2.3 GB/sec Housings (environmental control) Filters Optics Mechanisms
– – –
L2 position varies with wavelength (filter) Filters insertion mechanical shutter LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 33
Camera Challenges
• • • • • •
Detector requirements:
–
10 μm pixel size
– – –
Pixel full-well > 90,000 e – Low noise (< 5 e High QE 400 – rms), fast (< 2 sec) readout ( – 1000 nm
< –30 C)
–
All of above exist, but not simultaneously in one detector Focal plane position precision of order 3 μm Package large number of detectors, with integrated readout electronics, with high fill factor and serviceable design Large diameter filter coatings Constrained volume (camera in beam)
–
Makes shutter, filter exchange mechanisms challenging Constrained power dissipation to ambient
–
To limit thermal gradients in optical beam
–
Requires conductive cooling with low vibration LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 34
Camera Challenges (con’d)
• •
Key challenge: Detector technology Main choices: CCD, hybrid CMOS
–
CCDs:
• • • •
Monolithic Si array Routinely used for visible astronomical applications Have been made in high-resistivity, thick format (to achieve sensitivity at 1 μm wavelength) with 15 μm pixel density Slow readout: need ~10 μs per pixel to achieve noise level
–
Hybrid CMOS:
•
Hybrid array uses thin planar detector with pixelated back contact “bump bonded” to CMOS readout multiplexer
•
Routinely used for infrared astronomy (with different photo conversion material)
• • •
Avoids need for mechanical shutter Can integrate substantial electronics on-chip Low power (< 1/100 of CCD) & Fast readout LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 35
Camera Challenges (con’d)
•
Control of systematics
–
Lensing studies exploit subtle, systematic image distortions caused by dark matter
–
Time dependent or environmentally induced distortion in the measuring system (telescope + camera) could mask the lensing signature
–
May place unusual demands on camera development, particularly testing to ensure acceptable control/knowledge of end-to-end transfer function LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 36
LSST Management Plan
•
In March 2003, four organizations (U. of Washington, U. of Arizona, the
Research Corporation, and NOAO) formed the LSST Corporation (LSSTC), a non-profit 501C3 Arizona corporation. •
The purpose of LSSTC is to pursue a shared vision for the nature of the LSST endeavor, and a commitment to advance the project through technical, scientific, and/or financial contributions. LSSTC plans to expand its institutional membership as the project progresses.
•
As presently envisioned, funding for the construction of the LSST will come from NSF, DOE, and private donors. Significant commitments of private funding are already in hand. A proposal to NSF for design & development phase funding will be submitted in December 2003.
•
While LSST is a distributed project, there is a single management plan. All participating organizations will be coordinated and accountable to the LSST Director and Project Manager, who are appointed by the LSSTC Board of Directors.
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 37
DOE Participation in LSST
•
A collaboration of DOE-funded institutions has been formed to pursue participation in LSST. This collaboration has been working closely with other LSST participants under the coordination of the LSST Director and Project Manager.
•
The DOE “deliverable” will be the LSST camera system.
•
SLAC will lead the development of the camera, with significant contributions coming from BNL, LLNL, and DOE-funded university groups (e.g. Harvard, UIUC).
•
Scientists and engineers at these institutions will also participate in the data acquisition system, the development of pipeline software, and the scientific interpretation of the results.
LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 38
External Review Board
LSST Project Organization
LSST Corporation Board of Directors
John Schaefer, President
Research Corporation, University of Washington, National Optical Astronomical Observatory, University of Arizona
Executive Advisory Committee
Arthur Bienenstock
Science Assurance System Scientist
Christopher Stubbs
Data: Kem Cook Camera: Steve Kahn Tel/Site: Chuck Claver System Engineering Jacques Sebag LSST Director
Anthony Tyson
Project Manager Donald Sweeney Array Technology
Don Figer, Mike Lesser
Science Advisory Board
Zeljko Ivezic, Philip Pinto
Science Working Groups Project Support
•
Change Control Board
•
Risk Management
•
Project Controls
•
Performance Assurance
•
Administration SW Architecture
Jim Gray, Robert Lupton
Public Outreach Michael Shara, Doug Isbell Data Management
Kem Cook, Sci.
tbd , Mgr.
LSST Camera Project Camera Steve Kahn, Sci.
Bill Althouse, Mgr.
Telescope/Site
Charles Claver, Sci.
Larry Daggert, Mgr.
SLAC EPAC Meeting Nov. 14-15, 2003 39
LSST Camera Project Organization
• • •
Camera Project Support Project Controls & Risk Mgmt Performance & Safety Assur.
Administration Camera S. Kahn, Sci Lead W. Althouse, Proj Mgr System Engineering T. Thurston Lead Mech. Engr T. Decker, LLNL Lead Elect. Engr J. Oliver, Harvard Data Bus W. Althouse (act.) Focal Plane Assy M. May, BNL Optics J. Taylor, LLNL S. Olivier, LLNL Mechanisms L. Hale, LLNL Housing & Structure T. Thurston Camera I&T W. Craig Array, FE Elex V. Radeka, BNL Array Testing D. Figer, STScI M. Lesser, Steward Obs.
Opto-Mech Assy T. Decker, LLNL All SLAC unless otherwise noted LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 40
LSST Design Phase Schedule
OCT 04 OCT 05 OCT 06 OCT 07
Activity / Milestone
FY05 FY 06 FY 07 Optical Design Frozen Science Requirements Document Complete(SRD) Final Site Selection Functional Performance Requirements Doc (FPRD) Interface Requirement Documents Complete (IRD) Order Primary Mirror Glass D & D Funding Begins Conceptual Design Review Order Primary Mirror casting Submit Construction Proposal Mount Design RFQ Place Mount Design contract Dome Design RFQ Select Array Type Preliminary Design Review Construction Funding Approved Site Construcion Begins Order Focal Plane Arrays Place Dome Design / Fab contract
First light Dec. 2011 LSST Camera Project SLAC EPAC Meeting Nov. 14-15, 2003 41