The Large Synoptic Survey Telescope

The Large Synoptic Survey TelescopeThe Large Synoptic Survey Telescope

Presentation to P5April 20, 2006

Tony TysonDirector, LSST

Physics Department, Univ. of California, Davis

Steven KahnDeputy Director and Camera Lead Scientist, LSST

Stanford/SLAC

P5 PresentationApril 20, 2006 SLAC

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Large Synoptic Survey TelescopeLarge Synoptic Survey Telescope

History:

The need for a facility to survey the sky Wide, Fast and Deep, has been recognized for many years.

1996-2000 “Dark Matter Telescope”Emphasized mapping dark matter

2000- “LSST”Emphasized a broad range of science from the same multi-wavelength survey data


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Wide+Deep+Fast: EtendueWide+Deep+Fast: EtenduePrimary mirror

diameterField of view

KeckTelescope

0.2 degrees10 m

3.5 degrees

LSST


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Massively Parallel AstrophysicsMassively Parallel Astrophysics

– Dark matter/dark energy via weak lensing – Dark matter/dark energy via baryon acoustic oscillations– Dark energy via supernovae– Dark energy via counts of clusters of galaxies– 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, trans-

Neptunian objects


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LSST Ranked High PriorityLSST Ranked High Priority

• NRC Astronomy Decadal Survey

• NRC New Frontiers in the Solar System

• NRC Quarks-to-Cosmos

• Quantum Universe

• Physics of the Universe

• SAGENAP

• NSF OIR 2005-2010 Long Range Plan


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NSF LSST Funding TimelineNSF LSST Funding Timeline

2004 R&D proposal to NSF AST

2005 $14.2M LSST R&D grant

2006 LSST NSF MREFC Proposal

2009 NSB approval to begin construction

2013 First light and commissioning


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LSST Probes Dark Energy and Dark MatterLSST Probes Dark Energy and Dark Matter

Weak lensing (multiple probes) Baryon acoustic oscillations Counts of massive clusters vs redshift Supernova cosmology (complementary to JDEM) Mass power spectrum on very large scales tests CDM paradigm Shortest scales of dark matter clumping tests models of dark

matter particle physics

The LSST survey will address all with a single dataset!


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Weak Gravitational Lensing HeritageWeak Gravitational Lensing Heritage

2-degree by 2-degree mass map of one of five Deep Lens Survey fields. All four clusters examined in this field have been verified with spectroscopy and X-ray observations (2005)

1983-2000 Weak gravitational lens experiments using Blanco telescope

2000 First detection of cosmic shear

2000-2005 Deep Lens Survey

1996- Emerging need for an all-sky deep multi-wavelength facility with controllable systematic errors

Today, several distinct groupsworldwide are pursuing weak lens cosmology on a varietyof telescopes.


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Weak Lensing Shear Survey RequirementsWeak Lensing Shear Survey Requirements

Precision weak lensing shear requires deep imaging to 26.5 I mag and good PSF:

New technology telescopesdeliver the requisite imagequality

Fainter


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20 minute exposure on 8 m Subaru telescopePoint spread width 0.52 arcsec (FWHM)

1 arcminute


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Figure of MeritFigure of Merit

Area surveyed (number of objects found) to some SNR at some photon flux limit, per unit time:

2obj

2sky

φ A Ω QE Nt (SNR) φ (δΩ)

A – aperture A – aperture – camera FOV QE – det. Eff. – camera FOV QE – det. Eff. – – observing eff. observing eff. sky – sky flux sky – sky flux – seeing footprint – seeing footprint

site & opticssite & optics

Apparatus & Eff.Apparatus & Eff.Science goalsScience goals


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Relative Etendue (= ARelative Etendue (= A))

0

40

80

120

160

200

240

280

320

Eten

due

(m2 d

eg2 )

LSST PS4 PS1 Subaru CFHT SDSS MMT DES 4m VST VISTAIR

All facilities assumed operating100% in one survey


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Pan-STARRS-4 as an LSST PrecursorPan-STARRS-4 as an LSST Precursor

• The total etendue = 0.15 x LSST.

• To search for asteroids, PS-4 will use an ultra wide-band filter - unsuitable for lensing or for photo-z’s.

• Weak lensing will require separate observing time with narrow band filters.

• Funded partially by the USAF, PS-4 will consist of four 1.8 m telescopes, each with a 1.4 Gpixel camera.

• A single prototype, PS-1, is currently under construction.


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DE Science Drives Short ExposuresDE Science Drives Short Exposures

• Weak lensing requires exquisite control of shape systematics.

• One needs hundreds of exposures per filter per sky patch for chopping.

• Short exposures allow us to optimally weight.• Many exposures with sky rotated on detector permit

another chop.• These require high etendue and short exposures.


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20000 sq.deg WL survey shear 20000 sq.deg WL survey shear power spectrapower spectra

0.001 shear

z

z

Require: shear error < 0.0002

0.01 shear

0.001 shear


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Critical IssuesCritical Issues

WL shear reconstruction errors Show control to better than required precision

using existing new facilities Photometric redshift errors

Develop robust photo-z calibration plan Undertake world campaign for spectroscopy ()

Photometry errors Develop and test precision flux calibration

technique


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Subaru 10 sec ExposuresSubaru 10 sec Exposures

Raw de-trailed PSF corrected

<shear> <shear> = 0.07= 0.07

<shear> <shear> = 0.000013= 0.00001313

arc

min

(l =

100

0)

<shear> <shear> = 0.04= 0.04

Single exposure in 0.65 arcsec seeing

<shear> <shear> < 0.0001< 0.0001


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Residual Subaru Shear CorrelationResidual Subaru Shear Correlation

Cosmic shear signalTest of shear systematics: Use faint stars as proxies for galaxies, and calculate the shear-shear correlation.

Compare with expected cosmic shear signal.

Conclusion: 200 exposures per sky patch will yield negligible PSF induced shear systematics. Wittman (2005)


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Photometric RedshiftsPhotometric RedshiftsCalibration: angular correlation between photo-z and spectroscopic samples enables high precision photo-z: http://www.lsst.org/Science/Phot-z-plan.pdf


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12-band Super Photo-z Training Set12-band Super Photo-z Training Set

Together with angular correlations of galaxies, this training set enables LSST 6-band photo-z error calibration to better than required for precision cosmology

Systematic error:0.003(1+z) calibratableNeed 20,000 spectroscopic redshifts


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2-parameter Errors from LSST WL2-parameter Errors from LSST WL

Two cosmologies

Effect of joint analysis of LSST 2-point and 3-point shear data + Planck CMB

p/= w0 + wa (1-a)


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30,000 LSST Supernovae to z = 130,000 LSST Supernovae to z = 1

Simulated light curvesSimulated Hubble diagram

Deep field sample from LSST


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LSST

Wang et al. 2006, AAS

Precision vs Integrated LuminosityPrecision vs Integrated Luminosity


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Precision vs Integrated LuminosityPrecision vs Integrated Luminosity


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Strong gravitational lensing with multiple images provides a sensitive probe of dark matter mass distributions. LSST will find many of these.

Image of a z=1.7 galaxy being multiply lensed by a z=0.4 mass cluster

Physics of Dark Matter


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Mass in CL0024

Detailed map Detailed map of dark matterof dark matter


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LSST and Fundamental Physics

• Unique experiment for DE physics:– Five separate types of probes from the same experiment.– Precision control of systematics enabled by multiple chops.– Ultra-deep 2 sky coverage.

• Incisive probe of dark matter clumping on scales relevant to the underlying physics.


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LSST Project OrganizationLSST Project Organization

• The LSST is a public/private project with public support through NSF-AST and DOE-OHEP.

• Private support is devoted primarily to project infrastructure and fabrication of the primary/tertiary and secondary mirrors, which are long-lead items.

• NSF support is proposed to fund the telescope. DOE support is proposed to fund the camera.

• Both agencies would contribute to data management and operations.

CameraSteven Kahn, Sci.Kirk Gilmore, Mgr.

Telescope/SiteCharles Claver, Sci.

Victor Krabbendam, Mgr.

System EngineeringWilliam Althouse

Science Working Groups

Data ManagementTimothy Axelrod, Sci.Jeffrey Kantor, Mgr.

Science AdvisoryCommittee (SAC )

Michael Strauss

System Scientist &Chair of Science Council

Zeljko IvezicEd & Pub Outreach

Suzanne Jacoby

DirectorAnthony Tyson

Steve Kahn, Deputy

Project ManagerDonald Sweeney

Victor Krabbendam, Deputy

Board of Directors

Simulation & DataPhilip Pinto

PresidentJohn Schaefer

System CalibrationDavid Burke

LSST Organization Chart


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The LSST CorporationThe LSST Corporation

• The project is overseen by the LSSTC, a 501(c)3 non-profit Arizona corporation based in Tucson.

• LSSTC is the recipient of private funding, and is the Principal Investigator organization for the NSF D&D funding.


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• Brookhaven National Laboratory • Harvard-Smithsonian Center for Astrophysics • Johns Hopkins University • Las Cumbres Observatory, Inc. • Lawrence Livermore National Laboratory • National Optical Astronomy Observatory• Research Corporation • Stanford Linear Accelerator Center • Stanford University –KIPAC • The Pennsylvania State University• University of Arizona • University of California, Davis • University of Illinois at Champaign-Urbana • University of Pennsylvania• University of Washington

There are 15 LSSTC Institutional MembersThere are 15 LSSTC Institutional Members


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Funding and Management ConfigurationFunding and Management Configuration

NOAO

x

LSST Collaboration Institutions

Funding Sources

Relationships established by MoA's

NCSALSSTC Staff

PMO xLSSTC

PMO: Program Management Office

x

SLACBNLLLNL

Universities

Universities

x

DOE NSF

Joint Oversight - tbdLSSTCPrivate

x


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LSST Optical DesignLSST Optical Design

• f/1.23 • <0.20 arcsec FWHM images in six bands: 0.3 - 1 m • 3.5 ° FOV Etendue = 319 m2deg2

LSST optical layout

Polychromatic diffraction energy collection

0.00

0.05

0.10

0.15

0.20

0.25

0.30

0 80 160 240 320Detector position ( mm )

Imag

e di

amet

er (

arc-

sec

)

U 80% G 80% R 80% I 80% Z 80% Y 80%

U 50% G 50% R 50% I 50% Z 50% Y 50%


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Mirror DesignsMirror Designs

8.4 MetersPrimary Surface

Tertiary Surface 0.9 M

• Unique Monolithic Mirror: Primary and Tertiary Surfaces Polished Into Single Substrate

• Cast Borosilicate Design

Mirror Cell (Yellow)

Secondary Mirror

Baffle (Black)

• Thin Meniscus Low Expansion Glass Design for Secondary Mirror

• 102 Support Actuators

Secondary Mirror

Primary/Tertiary Mirror


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Telescope StructureTelescope Structure

Altitude over azimuth configuration


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LSST Site Selection Process – 2 Finalists LSST Site Selection Process – 2 Finalists Selection Upcoming in JuneSelection Upcoming in June

San Pedro Mártir Cerro Pachón


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Camera AssemblyCamera Assembly

Filter in stored location

L1 Lens

L2 Lens

Shutter

L1/L2 Housing

Camera Base Ring

Camera Housing

Cryostat outer cylinderCold Plates

L3 Lens in Cryostat front-end flange

Raft Tower (Raft with Sensors + FEE)

Filter Carousel main bearing

Utility Trunk

Filter in light path

Filter Changer rail paths

Focal Plane fast actuators

BEE Module


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The LSST Focal PlaneThe LSST Focal Plane

Guider Sensors (yellow)

3.5 deg FOV

Illumination Limit

WavefrontSensors (red)

3.2 Gpixels


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Raft TowersRaft Towers

SENSOR

RAFTRAFT TOWER

FEE

Si CCD Sensor

Raft Structure

Raft Assembly

Flex Cable &

FEE Cage

Thermal Straps

Sensor Packages

CCD Carrier

Thermal Strap(s)


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The LSST CCD SensorThe LSST CCD Sensor

Detail of one edge

Detail of output port

32 segments/CCD200 CCDs total6400 Total Outputs


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The Data Management ArchitectureThe Data Management Architecture

Infrastructure Layer

Middleware Layer

Application Layer

Application Layer

• Data Pipelines and Products and the Science Data Archive

Infrastructure Layer

• Computing, storage, and networking hardware and system software at each facility

Middleware Layer

• Distributed processing, data access, user interface, and system operations services


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Infrastructure LayerInfrastructure Layer

Long-Haul Communications

Base Facility Mountain Site

Archive/Data Access Centers


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Project Management Controls StatusProject Management Controls Status

Currently:

• Reference Design nearly complete• Full WBS with dictionary and task breakdown• Schedule is complete• Construction cost allocation complete and cost estimate nearly

complete

To Do:

• Task-based estimate (due May 31)• Integrated cost/schedule • Concept Design Review• Operations document and operations budget• Functional performance requirements document


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ConstructionCommissioning

Operations

Basic timeline for the LSSTBasic timeline for the LSST

• FY2004 – 2008 R&D phase, long-lead items started• FY2009 – 2012 Construction• Dec, 2012 First engineering light• FY2013 Commissioning and early science• FY 2014 - 2024 Operations

FY-05 2006 2007 2008 2009 2010 2011 2012 2013 2014

Design and Development

Submit NSF MREFC ProposalNSF MREFC begins

First light 51 monthsCD-0

NSF D&D

(and early procurement)

Fiscal Years

CD-2 MIECD-1

Coordinating the NSF and DOE SupportCoordinating the NSF and DOE Support• DOE follows: Program and Project Management for the Acquisition of Capital Assets,” DOE

Order 413.3

• NSF follows new policy modeled in-part after DOE model: “Guideline for Planning and Managing the Major Research Equipment and Facilities Construction Account,” November 22, 2005

NSF

DOE


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Funding Requests in Then-Year dollarsFunding Requests in Then-Year dollars

Construction funding request in Then-Year dollars

Total $330M ($298M in 2006 USD)

NSF MREFC $190M DOE $101M Private $39M

Operations starting in FY2013

FY2014 $25.5M (first full year of operation) Total for 10 years of operation $295M


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The LSST Construction CostThe LSST Construction Cost

$116M

Camera

DataMgmt

$10.3

$89.5M

$79.2M

Prog MgmtTelescope/Site

39%

30%

27%

3%$129.7M

Camera

DataMgmt

$11.5

$101.1M

$88.5M

Prog MgmtTelescope/Site

Total Construction Cost in 2006 USD: $297M

Total Construction Cost in THEN-YEAR USD: $330M

FY06 FY07 FY08 FY09 FY10 FY11 FY12 FY13* FY13** FY14 FY… Total Total TotalQ1 only Q2 to Q4 FY15 on R&D MIE Ops/year

$3.1 $4.5 $4.7 $6.1 $6.5 $5.9 $3.4 $0.9 $2.9 $3.7 $3.4 $12.3 $22.7 $3.4Total Labor Contingency $M $2.0 $2.5 $1.0 $0.4 $1.0 $1.2 $1.2 $5.9 $1.2Subtotal of Labor $ w/Contingency $3.1 $4.5 $4.7 $6.1 $8.5 $8.4 $4.4 $1.3 $3.9 $4.9 $4.6 $12.3 $28.6 $4.6

M&S $1.0 $5.0 $6.7 $24.0 $16.0 $3.5 $0.8 $0.3 $2.0 $3.0 $3.0 $12.7 $44.6 $3.0M&S Contingency $0.2 $1.3 $1.8 $8.0 $6.5 $1.3 $0.2 $0.1 $0.5 $0.7 $0.6 $3.3 $16.1 $0.6Subtotal of M&S w/Contingency $1.2 $6.3 $8.5 $32.0 $22.5 $4.8 $1.0 $0.4 $2.5 $3.7 $3.6 $16.0 $60.7 $3.6

$4.1 $9.5 $11.4 $30.1 $22.5 $9.4 $4.2 $1.2 $4.9 $6.7 $6.4 $25.0 $67.3 $6.7Total of Contingencies $0.2 $1.3 $1.8 $8.0 $8.5 $3.8 $1.2 $0.5 $1.5 $1.9 $1.8 $3.3 $22.0 $1.9

5% 14% 16% 27% 38% 41% 29% 39% 31% 29% 28% 13% 33% 29%$4.3 $10.8 $13.2 $38.1 $31.0 $13.2 $5.4 $1.6 $6.4 $8.6 $8.2 $28.3 $89.2 $8.6

$0.3 $0.8 $3.5 $3.9 $2.1 $1.0 $0.4 $1.5 $2.3 $2.5 $1.1 $10.9 $2.5

$4.3 $11.1 $14.0 $41.6 $34.9 $15.2 $6.4 $2.0 $7.8 $10.8 $10.7 $29.4 $100.2 $10.7

$4.3 $15.4 $29.4 $41.6 $76.5 $91.7 $98.2 $100.1 $7.8 $18.6 $29.3 $29.4 $100.1 $10.7

$4.3 $15.4 $29.4 $71.0 $105.9 $121.2 $127.6 $129.5

Notes

*** Total project cost includes R&D, MIE fabrication phase, and commissioning.

Estimates with 3%/yr Escalation (Then-Year $M)

LSST Camera Cost EstimatesFrom LSST Document-1398

TotalsR&D Phase MIE Phase Operations Phase****

Escalated to Then-Year $M

Total Loaded Labor $M

Subtotal of Loaded Labor+M&S

Total

Escalation added to Total (3%/ year)

Contingency as % of Base

Estimates in Base Year 2006 ($M)

****Observatory operations is shared with NSF; budget here is DOE portion only (~40%) of total observatory operations. Staffing includes camera operations, maintainance and participation in data archive center.

*MIE ends after Q1 of FY13. **Operations starts Q2 of FY13.

Cumulative TPC*** (escalated)

Cumulative of phase (escalated)


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SLAC Director’s Review of LSSTSLAC Director’s Review of LSST

• Review held March 8-9, 2006, chaired by Lowell Klaisner.

• The Committee reviewed the technical design of the camera and the cost and schedule of the project as a whole.

• The Committee supported the project moving forward and the investment requested from DOE and SLAC.

• Reviewers identified concern with technical risk associated with the sensor production, and too little float in the technically-limited schedule.

• All issues are being worked by the project now. Fallback options have been identified if the prototype sensors do not meet specifications and an improved integration concept mitigates risk in the schedule.


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Overall SummaryOverall Summary

• The LSST will be a world-leading facility for astronomy and cosmology. A single database will enable a large array of diverse scientific investigations. The project has broad support in the astronomy community, and it is therefore a key component of NSF’s long-term plan for the field.

• Of particular interest to HEP, LSST will measure properties of dark energy via weak lensing, baryon oscillations, Type 1a supernovae, and measurements of clusters of galaxies. It will test models of dark matter through strong lensing. No other existing or proposed ground-based facility has comparable scientific reach.

• The synergy in technical and scientific expertise between the astronomy and HEP communities will be essential to the project’s success.

• A detailed initial design is in place for all major components of the system. With appropriate funding from NSF and DOE, the project is on-track to achieve first light in 2013.

Documents

The Large Synoptic Survey Telescope