LSST Project Status

Kirk Gilmore

LSST Camera Scientist (Manager/Sys Eng) Stanford/SLAC/KIPAC Penn October 1, 2008

QuickTime™ and a Microsoft Video 1 decompressor are needed to see this picture.

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 Data Management Education and Public Outreach

3

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

– – – – – – –

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.

2.

3.

4.

5.

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

(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 - Sensor prototyping

Camera Schedule

A. Currently in R&D - 72 people/16 institutions and universities B. Anticipated transition to MIE (construction) in 2010/2011 C. Telescope first light 2014 D. System first light 2015 E. 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

Science

A. Science collaborations (10) starting to engage and establish projects B. Science Requirements Document established

LSST Project/camera related Events

A. P5 B. LSST Project All-hands meeting in May (~150 people) C. PDR (NSF) 2nd qtr FY09; CD-1 (DOE) ~same time D. Decadal Survey…

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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 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

.

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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.

Meeting in December in Seattle - Science council and reps from Collaborations

The current LSST timeline

FY-07 FY-08 FY-09 FY-10 NSF D&D Funding MREFC Proposal Submission NSF CoDR MREFC Readiness NSF PDR NSB NSF CDR FY-11 FY-12 FY-13 FY-14 FY-15 FY-16 FY-17 NSF MREFC Funding NSF + Privately Supported Construction (8.5 years) Telescope First Light 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-2 DOE CD-0 DOE CD-1

Penn October 1, 2008

DOE CD-4 Camera Delivered to Chile Camera Ready to Install

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LSST mirror casting “high fire” celebration was held March 29 at the UofA

Penn October 1, 2008 11

LSST Primary Mirror Blank, September 2008

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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

• • • •

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)

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Dark Matter Simulations at KIPAC

17 simulation by A. Kravtsov

Full LSST end to-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 Ta

2

O

5

and silica SiO

2



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

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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 L1 Lenses L2 L3 u

Surface 1 vertex to FPA Surface 2 vertex to FPA Center thick.

Clear aperture rad.

Surface 1 spherical rad.

1031.950

949.720

82.230

775.000

2824.000

537.080

507.080

30.000

551.000

1.000E+15 88.500

28.500

60.000

346.000

3169.000

149.500

123.300

26.200

375.000

5624.000

Surface 2 spherical rad.

Sagitta of Surface 1 Sagitta of Surface 2 -5021.000

108.424

-60.172

-2529.000 -13360.000

0.000

-60.754

18.945

-4.481

-5513.000

12.516

-12.769

Thick. at Clr Aperture *All dimensions in mm except as noted 33.977

90.754

45.536

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

149.500

131.700

17.800

375.000

5624.000

-5594.000

12.516

-12.583

17.867

i

149.500

133.800

15.700

375.000

5624.000

-5612.000

12.516

-12.543

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

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Optical Design: Filter Reference Design

U G R I Z Y Blue Side

330 400 552 691 818 960

Half-Maximum Transmission Wavelength Red Comments Side

400 Blue side cut-off depends on AR coating 552 691 818 922 1070 Balmer break at 400 nm Matches SDSS Red side short of sky emission at 826 nm Red side stop before H 2 O bands Red cut-off before detector cut-off

LSST Ideal Filters

100.0

80.0

60.0

40.0

20.0

0.0

300 u 400 g 500 r i z Y 600 700 800

Wavelength (nm)

900 1000 1100 1200 • • • 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 Uniform deposition required at 1% level over entire filter 22

LSST system throughput parameters

LSST System Throughput

100.0

90.0

80.0

70.0

60.0

50.0

40.0

30.0

20.0

10.0

0.0

300 u 400 atmo g 500 r i 600 700

Wavelength (nm)

800 z optics y detector 900 1000 1100 23

LSST system spectral throughput in the six filter bands

Includes sensor QE, atmospheric attenuation, optical transmission functions Wavelength (nm)

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Leak Update QuickTime™ and a decompressor are needed to see this picture.

Orig Design QuickTime™ and a decompressor are needed to see this picture.

Updated Design 25

Y-Band Options (Y2, Y3 and Y4) QuickTime™ and a decompressor are needed to see this picture.

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SED’s for a z=7 quasar and a T-dwarf (SDSS and UKIDSS) 27

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.

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Comparison of Y1, Y2, and Y3

50 40 30 20 10 0 800 -10 850 900 950 1000 1050 1100

Y1 930.1060

Y2 970.1020

Y3 970.open

redshifted elliptical combined sky sed Atmosphere

Wavelength 1150

29

1200

LSST system spectral throughput in the six filter bands

Includes sensor QE, atmospheric attenuation, optical transmission functions Wavelength (nm)

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S/N Calculations in Y-band

By Seeing Seeing = 0.500

n source type z Y1 400 elliptical-galaxy Y2 Y3 0 16.51 14.26 17.11

400 elliptical-galaxy 400 elliptical-galaxy 1 16.55 14.30 17.36

2 15.88 14.15 17.54

Seeing = 0.750

n source type z Y1 400 elliptical-galaxy Y2 Y3 0 11.08 9.59 11.49

400 elliptical-galaxy 1 11.11 9.62 11.65

400 elliptical-galaxy Seeing = 1.000 2 10.65 9.52 11.78

n source type z Y1 400 elliptical-galaxy 400 elliptical-galaxy Y2 Y3 0 8.32 7.21 8.63

1 8.34 7.23 8.75

400 elliptical-galaxy Seeing = 1.250

400 elliptical-galaxy 2 8.00 7.15 8.85

n source type z Y1 400 elliptical-galaxy Y2 Y3 0 6.66 5.77 6.91

1 6.68 5.79 7.01

400 elliptical-galaxy 2 6.41 5.73 7.08

By Num of Exposures n source type z Y1 Y2 Y3 25 elliptical-galaxy 50 elliptical-galaxy 75 elliptical-galaxy 100 elliptical-galaxy 125 elliptical-galaxy 150 elliptical-galaxy 175 elliptical-galaxy 200 elliptical-galaxy 225 elliptical-galaxy 250 elliptical-galaxy 275 elliptical-galaxy 300 elliptical-galaxy 325 elliptical-galaxy 350 elliptical-galaxy 375 elliptical-galaxy 400 elliptical-galaxy 1 2.09 1.81 2.19

1 2.95 2.56 3.10

1 3.61 3.13 3.79

1 4.17 3.62 4.38

1 4.66 4.04 4.89

1 5.11 4.43 5.36

1 5.52 4.78 5.79

1 5.90 5.11 6.19

1 6.26 5.42 6.57

1 6.60 5.72 6.92

1 6.92 6.00 7.26

1 7.22 6.26 7.58

1 7.52 6.52 7.89

1 7.80 6.77 8.19

1 8.08 7.00 8.48

1 8.34 7.23 8.75

By Source n source type z Y1 400 elliptical-galaxy Y2 Y3 0 8.32 7.21 8.63

400 elliptical-galaxy 400 elliptical-galaxy 400 spiral-galaxy 1 8.34 7.23 8.75

2 8.00 7.15 8.85

0 8.34 7.21 8.61

400 spiral-galaxy 400 spiral-galaxy 400 G5V 400 G5V 400 G5V 1 7.74 7.30 7.75

2 8.25 7.20 8.66

0 8.39 7.25 8.48

1 8.33 7.22 8.65

2 7.86 7.12 9.00

LSST camera consists of the cryostat and body

Back Flange Filter Carousel Filter Cryostat Filter Auto Changer L1/L2 Assembly Utility Trunk Valve Box Shutter

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The LSST Camera Team: 72 People from 16 Institutions

Brandeis University

J. Besinger, K. Hashemi

Purdue University

K. Ardnt, Gino Bolla, J, Peterson, Ian Shipsey

Brookhaven National Lab Rochester Institute of Technology

S. Aronson, C. Buttehorn, J. Frank, J. Haggerty, I. Kotov, P. Kuczewski, M. May, P. O’Connor, S. Plate, V. Radeka, P. Takacs D. Figer

Stanford Linear Accelerator Center Florida State University

Horst Wahl

Harvard University

N. Felt, J. Geary (CfA), J. Oliver, C. Stubbs 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

IN2P3 - France University of California, Berkeley

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 J.G. Jernigan

University of California, Davis

P. Gee, A. Tyson

Lawrence Livermore National Lab University of California, Santa Cruz

S. Asztalos, K. Baker, S. Olivier, D. Phillion, L. Seppala, W. Wistler T. Schalk

University of Illinois, Urbana-Champaign Oak Ridge National Laboratory

J. Thaler C. Britton, Paul Stankus

Ohio State University

K. Honscheid, R. Hughes, B. Winer

University of Pennsylvania

M. Newcomer, R. Van Berg 33

Camera Organizational Chart

Camera Lead Scientist

Kahn (SLAC)

Camera Project Scientist

Gilmore (SLAC)

Camera Project Manager

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

Camera Integration & Test Planning

Nordby (SLAC) WBS 3.6

Observatory Integ., Test & Commission Support

(SLAC) WBS 3.7

Electronics

Oliver (Harvard) WBS 3.5.8

Sensor/Raft Development

Radeka/O’Connor (BNL) WBS 3.5.4

Optics

Olivier (LLNL) WBS 3.5.5

Cryostat Assembly

Schindler (SLAC) WBS 3.5.7

Camera Body & Mechanisms

Nordby (SLAC) WBS 3.5.3

Camera Data Acq. & Control

Schalk (UCSC) WBS 3.5.6

Calibration

Burke (SLAC) WBS 3.5.1

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

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LSST focal plane layout

4KX4K Science CCD 10

m

m pixels

3X3 CCD “RAFT”

Corner area Wavefront sensing and guiding CCD is divided into 16 1Mpix segments with individual readout

35

From sensors to rafts to raft/towers - The heart of the system

CCD PACKAGED CCD

CCD alignment pins

RAFT

connector 3-pt. mount carrier thermal straps FEE boards cooling planes housing (cold mass) baseplate flex cables • • •

TOWER

3 x 3 submosaic of CCDs front end electronics thermal management components

• 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 cm 2 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 100

m

m thick, high resistivity bulk silicon,fully depleted

E2V

2K x 4K, 13.5

m m pixels, 2 outputs

STA/ITL

4K x 4K, 10 m m pixels, 16 outputs Penn October 1, 2008 38

Imaging data from study contract devices

e2V

2K x 512, 13.5

m

m pixels, single output mode

STA/ITL

4K x 4K, 10

m

m pixels, 16 outputs

4cm Penn October 1, 2008 39

Summary of study phase

Science driver Broadband, high QE Seeing-limited image quality High throughput



meets LSST spec



does not meet spec – not addressed ? not yet measured Technology Advance Thick silicon, fully depleted Transparent back contact Low charge diffusion Small pixel size Low read noise Low dark current Low persistence High full well Flat silicon surface TTP-controlled package Multiport output High fill factor die & pkg Criterion QE(1000nm) > 30% QE(400nm) > 40% < 3.2

m

m rms 10

m

m (0.2") < 5 e rms < 2 e /pix/s < 10 -4 > 90,000 e < 5

m

m p-v < 6.5

m

m over raft (4K) 2 , 16 output > 93% ?

― ―

   

― ― ― Vendor 1

 

?



?

―



― ?



?



Vendor 2

  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 • • 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

-50V -10V

X-ray images

41

Other major camera efforts

FORE Chamber Contamination test chamber at SLAC Camera Controls

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

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