LSST Project Status
Kirk Gilmore
LSST Camera Scientist (Manager/Sys Eng)
Stanford/SLAC/KIPAC
Penn
October 1, 2008
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Penn
October 1, 2008
2
The LSST Project is a Complete System:
Image, Analysis, Archive, Publish and Outreach
Camera
Telescope and Site
Cerro Pachon
La Serena
Education and Public Outreach
3
Data Management
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
4
Summary of LSST project progress
since last DOE Program Review
1.
Recent Project and Camera Developments
A. $20M award from Charles Simonyi & $10M from Bill Gates - Primary/Tertiary mirror fabrication
B. $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 M&S in 08/09 + in-kind FTE)
E. AAS in Austin - 28 Posters (on http://www.lsst.org)
SPIE in Marseille - 12 Papers on LSST
2.
Camera Schedule
A.
B.
C.
D.
E.
3.
Currently in R&D - 72 people/16 institutions and universities
Anticipated transition to MIE (construction) in 2010/2011
Telescope first light 2014
System first light 2015
Full science in 2016
Camera Budget
A. Working primarily with SLAC M&S
B. Using budget to support reviews via prototyping and analysis:
M&S and labor and FPT to outside institutions
C. IN2P3 ramping up
4.
Science
A. Science collaborations (10) starting to engage and establish projects
B. Science Requirements Document established
5.
LSST Project/camera related Events
A.
B.
C.
D.
P5
LSST Project All-hands meeting in May (~150 people)
PDR (NSF) 2nd qtr FY09; CD-1 (DOE) ~same time
Decadal Survey…
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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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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
6
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
7
IN2P3 - France R&D support for camera
development
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CNRS - National Center for Scientific Research
IN2P3 - National Institute for Nuclear Physics and Particle Physics
APC - 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.
8
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.
Meeting in December in Seattle - Science council and reps from Collaborations
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)
Sensor Procurement Starts
DOE CD-3
DOE R&D Funding
DOE CD-4
Camera Delivered to Chile
Camera Ready to Install
DOE CD-2
DOE CD-0
DOE CD-1
Penn
October 1, 2008
10
LSST mirror casting “high fire” celebration was held
March 29 at the UofA
Penn
October 1, 2008
11
LSST Primary Mirror Blank, September 2008
12
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
13
Ultra-large Data Management: LSST
•
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100+ petabyte system
Multi-dimensional data set
Large user base ranging from professional astronomers to general public.
Complex analytics
SLAC is responsible for delivering the LSST database and data access system
SciDB - a new open source data management system
for data-intensive scientific analytics
– Design led by world-class database researchers
• Mike Stonebraker, David DeWitt
SLAC's involvement
– Actively helped define SciDB
– Coordinates input from all sciences
SLAC has a chance to make big positive impact on complex scientific analytics and
beyond
14
Comparing HST with Subaru
ACS: 34 min (1 orbit)
PSF: 0.1 arcsec (FWHM)
2 arcmin
15
Comparing HST with Subaru
Suprime-Cam: 20 min
PSF: 0.52 arcsec (FWHM)
16
Dark Matter Simulations at KIPAC
17
simulation by A. Kravtsov
Full LSST endto-end photon
Simulation
Sky->Atmosphere->
Optics->Detector
12 million objects,
billions of raytraced
photons
Peterson, Meert,
Nichols, Grace,
Bankert (Purdue)
Jernigan (Berkeley)
Connolly (U Wash)
Rasmussen (SLAC)
Gilmore (SLAC)
Focal Plane Flatness model and whisker plot
19
LSST filter design
• R Pass band (552 nm -691 nm) optimization with
tantala Ta2O5 and silica SiO2
 Edge slopes = 1% < 5%
 Out band transmittance = 0.01 %
 In band transmittance = 99.75 %
 More than 100 layers on each substrate side
 Single layer thickness between few 10’s nm and few 100’s nm
 Total thickness = 20 µm
 No periodicity in the stack
20
Optical Design: Reference Design Parameters
•
•
•
Camera optical element prescription is established by V3 of the observatory
optical design
– Optical design of camera lenses and filters is integrated with optical design
of telescope mirrors to optimize performance
– 3 refractive lenses with clear aperture diameters of 1.55m, 1.02m and 0.70m
– 6 interchangeable, broad-band, interference filters with clear aperture
diameters of 0.76m
Why are transmissive optics required?
– L3 required as vacuum barrier (6 cm thick) for focal plane cryostat
– Filters required for science program
– L1 & L2 required to minimize chromatic effect of L3 and filters
Baseline LSST optical design produces image quality with 80% encircled
energy <0.3 arc-second
Camera Optical Element Design Requirements
Clear Aperture Dims
Surface 1 vertex to FPA
Surface 2 vertex to FPA
Center thick.
Clear aperture rad.
Surface 1 spherical rad.
Surface 2 spherical rad.
Sagitta of Surface 1
Sagitta of Surface 2
Thick. at Clr Aperture
Lenses
L1
L2
L3
1031.950
537.080
88.500
949.720
507.080
28.500
82.230
30.000
60.000
775.000
551.000
346.000
2824.000 1.000E+15
3169.000
-5021.000 -2529.000 -13360.000
108.424
0.000
18.945
-60.172
-60.754
-4.481
33.977
90.754
45.536
*All dimensions in mm except as noted
u
149.500
123.300
26.200
375.000
5624.000
-5513.000
12.516
-12.769
26.453
"Approx Physical Dims" are for reference only
g
149.500
128.360
21.140
375.000
5624.000
-5564.000
12.516
-12.651
21.275
Filters
r
i
149.500
149.500
131.700
133.800
17.800
15.700
375.000
375.000
5624.000 5624.000
-5594.000 -5612.000
12.516
12.516
-12.583
-12.543
17.867
15.727
z
149.500
135.300
14.200
375.000
5624.000
-5624.000
12.516
-12.516
14.200
y
149.500
136.000
13.500
375.000
5624.000
-5624.000
12.516
-12.516
13.500
21
Optical Design: Filter Reference Design
Blue
Side
330
400
552
691
818
960
U
G
R
I
Z
Y
Half-Maximum Transmission Wavelength
Red
Comments
Side
400 Blue side cut-off depends on AR coating
552 Balmer break at 400 nm
691 Matches SDSS
818 Red side short of sky emission at 826 nm
922 Red side stop before H 2O bands
1070 Red cut-off before detector cut-off
• 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
LSST Ideal Filters
100.0
Uniform deposition
required at 1% level
over entire filter
Transmission
80.0
60.0
u
g
r
i
z
Y
40.0
20.0
0.0
300
400
500
600
700
800
Wavelength (nm)
900
1000
1100
1200
22
LSST system throughput parameters
LSST System Throughput
100.0
System Throughput (%)
90.0
atmo
80.0
optics
70.0
60.0
50.0
40.0
30.0
g
r
i
z
y
u
detector
20.0
10.0
0.0
300
400
500
600
700
800
900
1000
1100
Wavelength (nm)
23
LSST system spectral throughput in the
six filter bands
System throughput (%)
Includes sensor QE, atmospheric
attenuation, optical transmission functions
Wavelength (nm)
24
Leak Update
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Orig Design
Updated
Design
25
Y-Band Options (Y2, Y3 and Y4)
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SED’s for a z=7 quasar and a T-dwarf (SDSS and UKIDSS)
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OH Emission
• Source - Bright airglow produced by a
chemical reaction of hydrogen and ozone in the Earth’s upper
atmosphere
• Band system is due in part to emission from vibrationally excited
OH radicals produced by surface interactions with ground-state
oxygen atoms.
• Emission can vary 10-20% over a 10 minute period
• Ramsey and Mountain (1992) have reported measurements of
the nonthermal emission of the hydroxyl radical and examined
the temporal and spatial variability of the emission.
28
Comparison of Y1, Y2, and Y3
% Transmittance
50
40
30
20
10
0
800
850
900
950
1000
1050
1100
1150
1200
-10
Wavelength
Y1 930.1060
Y2 970.1020
Y3 970.open
redshifted elliptical
combined sky sed
Atmosphere
29
LSST system spectral throughput in the
six filter bands
System throughput (%)
Includes sensor QE, atmospheric
attenuation, optical transmission functions
Wavelength (nm)
30
By Num of Exposures
S/N Calculations in Y-band
By Seeing
Seeing = 0.500
n
source type
400 elliptical-galaxy
400 elliptical-galaxy
400 elliptical-galaxy
Seeing = 0.750
n
source type
400 elliptical-galaxy
400 elliptical-galaxy
400 elliptical-galaxy
Seeing = 1.000
n
source type
400 elliptical-galaxy
400 elliptical-galaxy
400 elliptical-galaxy
Seeing = 1.250
n
source type
400 elliptical-galaxy
400 elliptical-galaxy
400 elliptical-galaxy
z Y1
Y2
Y3
0 16.51 14.26 17.11
1 16.55 14.30 17.36
2 15.88 14.15 17.54
z Y1
Y2
Y3
0 11.08 9.59 11.49
1 11.11 9.62 11.65
2 10.65 9.52 11.78
z
0
1
2
Y1
8.32
8.34
8.00
Y2
7.21
7.23
7.15
Y3
8.63
8.75
8.85
z
0
1
2
Y1
6.66
6.68
6.41
Y2
5.77
5.79
5.73
Y3
6.91
7.01
7.08
n
source type
z
25 elliptical-galaxy 1
50 elliptical-galaxy 1
75 elliptical-galaxy 1
100 elliptical-galaxy 1
125 elliptical-galaxy 1
150 elliptical-galaxy 1
175 elliptical-galaxy 1
200 elliptical-galaxy 1
225 elliptical-galaxy 1
250 elliptical-galaxy 1
275 elliptical-galaxy 1
300 elliptical-galaxy 1
325 elliptical-galaxy 1
350 elliptical-galaxy 1
375 elliptical-galaxy 1
400 elliptical-galaxy 1
Y1
2.09
2.95
3.61
4.17
4.66
5.11
5.52
5.90
6.26
6.60
6.92
7.22
7.52
7.80
8.08
8.34
Y2
1.81
2.56
3.13
3.62
4.04
4.43
4.78
5.11
5.42
5.72
6.00
6.26
6.52
6.77
7.00
7.23
Y3
2.19
3.10
3.79
4.38
4.89
5.36
5.79
6.19
6.57
6.92
7.26
7.58
7.89
8.19
8.48
8.75
By Source
n
400
400
400
400
400
400
400
400
400
source type
z
elliptical-galaxy 0
elliptical-galaxy 1
elliptical-galaxy 2
spiral-galaxy 0
spiral-galaxy 1
spiral-galaxy 2
G5V
0
G5V
1
G5V
2
Y1
8.32
8.34
8.00
8.34
7.74
8.25
8.39
8.33
7.86
Y2
Y3
7.21 8.63
7.23 8.75
7.15 8.85
7.21 8.61
7.30 7.75
7.20 8.66
7.25 8.48
31
7.22 8.65
7.12 9.00
LSST camera consists of the cryostat and body
Back Flange
Valve Box
Filter Carousel
Cryostat
Filter
Filter Auto Changer
L1/L2 Assembly
Utility Trunk
Shutter
32
The LSST Camera Team: 72 People from
16 Institutions
Brandeis University
Purdue University
J. Besinger, K. Hashemi
K. Ardnt, Gino Bolla, J, Peterson, Ian Shipsey
Brookhaven National Lab
Rochester Institute of Technology
S. Aronson, C. Buttehorn, J. Frank, J. Haggerty,
D. Figer
I. Kotov, P. Kuczewski, M. May, P. O’Connor, S. Stanford Linear Accelerator Center Plate, V. Radeka, P. Takacs
G. Bowden, P. Burchat (Stanford), D. Burke, M. Foss,
Florida State University
K. Fouts, K. Gilmore, G. Guiffre, M. Huffer, S. Kahn
Horst Wahl
(Stanford), E. Lee, S. Marshall, M. Nordby, M. Perl, A.
Rasmussen, R. Schindler, L. Simms (Stanford), T.
Harvard University
Weber
N. Felt, J. Geary (CfA), J. Oliver, C. Stubbs
University of California, Berkeley
IN2P3 - France
J.G. Jernigan
R. Ansari, P. Antilogus, E. Aubourg, S. Bailey, A.
Barrau, J. Bartlett, R. Flaminio, H. Lebbolo, M. University of California, Davis
Moniez, R. Pain, R. Sefri, C. de la Taille, V.
P. Gee, A. Tyson
Tocut, C. Vescovi
University of California, Santa Cruz
Lawrence Livermore National Lab
T. Schalk
S. Asztalos, K. Baker, S. Olivier, D. Phillion, L.
Seppala, W. Wistler
University of Illinois, Urbana-Champaign
Oak Ridge National Laboratory
J. Thaler
C. Britton, Paul Stankus
University of Pennsylvania
Ohio State University
M. Newcomer, R. Van Berg
K. Honscheid, R. Hughes, B. Winer
33
Camera Lead
Scientist
Kahn (SLAC)
Camera
Organizational
Chart
Camera Project Camera Project
Scientist
Manager
Gilmore (SLAC)
Fouts (SLAC)
WBS 3.1
Project Control
Price
(SLAC)
WBS 3.1
Systems
Engineering
Gilmore (act.)
(SLAC)
WBS 3.2
Performance, Safety and
Environmental Assurance
(SLAC)
WBS 3.3 / 3.4
Electronics
Oliver
(Harvard)
WBS 3.5.8
Optics
Olivier
(LLNL)
WBS 3.5.5
Sensor/Raft
Development
Radeka/O’Connor
(BNL)
WBS 3.5.4
Camera Integration
& Test Planning
Nordby
(SLAC)
WBS 3.6
Camera Body &
Mechanisms
Nordby
(SLAC)
WBS 3.5.3
Cryostat
Assembly
Schindler
(SLAC)
WBS 3.5.7
Observatory Integ., Test
& Commission Support
(SLAC)
WBS 3.7
Calibration
Burke
(SLAC)
WBS 3.5.1
Camera Data
Acq. & Control
Schalk
(UCSC)
WBS 3.5.6
Sensor,Elect,
Mech. Dev.
Antilogus
(IN2P3)
LPNHE LAL APC
Corner Raft
WFS/Guider
Olivier
(LLNL)
WBS 3.5.9
Camera Utilities
Nordby
(SLAC)
WBS 3.5.2
34
LSST focal plane layout
4KX4K
Science CCD
10mm pixels
3X3
CCD
“RAFT”
CCD is divided into 16 1Mpix
segments with individual
readout
Corner area
Wavefront sensing
and guiding
35
From sensors to rafts to raft/towers
- The heart of the system
CCD
thermal straps
FEE boards
PACKAGED
CCD
cooling
planes
connector
CCD
housing
(cold mass)
carrier
alignment
pins
TOWER
RAFT
• 3 x 3 submosaic of CCDs
• front end electronics
• thermal management components
baseplate
3-pt. mount
flex cables
• Tower is an autonomous,
fully-testable 144 Mpixel
camera
36
Sensor development on the schedule
critical path
–
–
–
–
–
–
–
High QE to 1000nm
• Thick silicon - 100µm thick and BB AR
coating
PSF << 0.7” (0.2”)
• High resistivity substrate (> 5
kohm∙cm)
• Small pixel size (0.2” = 10 µm)
Fast f/1.2 focal ratio
• Sensor flatness < 5µm p-v
Wide FOV
• ~ 3200 cm2 focal plane
• > 189 Science-sensor mosaic
High throughput
• > 90% fill factor
• 4-side buttable package, sub-mm
gaps
Fast readout (1 s)
• Segmented sensors - ~3200 total
output ports
• 150 I/O connections per sensor
Low read noise
• < ~ 5 rms electrons
R&D Program
• Funding secured by Keck Foundation to
keep development moving.
• Three phase development - Study phase
sensor evaluation begun at BNL - Prototype
phase RFP being prepared
37
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
38
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
39
Summary of study phase
Science driver
Technology Advance
Criterion
Vendor
1
Vendor
2
Broadband, high QE
Thick silicon, fully depleted
QE(1000nm) > 30%


Transparent back contact
QE(400nm) > 40%


Low charge diffusion
< 3.2mm rms
?
?
Small pixel size
10mm (0.2")
―

Low read noise
< 5 e- rms
―
?
Low dark current
< 2 e-/pix/s


Low persistence
< 10-4

?
High full well
> 90,000 e-


Flat silicon surface
< 5mm p-v

?
TTP-controlled package
< 6.5mm over raft
―
―
Multiport output
(4K)2, 16 output
―

High fill factor die & pkg
> 93%
―
―
Seeing-limited image quality
High throughput
 meets LSST spec
 does not meet spec
– not addressed
? not yet measured
Penn
October 1, 2008
40
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
-50V
• CCD controllers for 4 new test labs under
construction
– UC Davis, SLAC, Paris, Purdue
– allows full-speed testing of segmented sensors
X-ray images
-10V
• Components for CCD/electronics chain testing
in assembly (Raft/Tower electronics:
prototype by end of year
41
Other major camera efforts
FORE
Main
MAIN
Chamber
Contamination test chamber at
SLAC
Fore or
Preparation
Chamber
Camera Controls
Working is proceeding on plans to deliver
a prototype test stand by end of
calendar year 2008 - Goal by PDR
cold
finger
42
A camera integration plan is complete
Cryostat
Utility
Trunk
Camera Body
L1/L2 assy
43
Camera construction costs by sub-system
44
A list of everything I currently know about Dark Energy
45