LSST Status

Kirk GilmoreLSST Camera ScientistStanford/SLAC/KIPAC

LSST Science Requirements focus on 4 Representative and Divergent

Programs

LSST enables multiple investigations into our understanding of the universe

Dark Energy-Dark Matter Exploring our Solar System

LSST will find 90% of hazardous NEOs

down to 140 m in 10 yrs

“Movie” of the Universe: time domain Mapping the Milky Way

LSST will map the rich and

complex structure of our

Galaxy.

Discovering the transient and unknown on multiple time

scales

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The LSST Project is a Complete System:Image, Analysis, Archive, Publish and Outreach

Telescope and Site

Camera

Data Management

Cerro PachonLa Serena

Education and Public Outreach

Institutional Members LSSTC, September 08

* Brookhaven National Laboratory * California Institute of Technology * Carnegie Mellon University* Chile * Columbia University * Google Inc. * Harvard-Smithsonian Center for

Astrophysics * Johns Hopkins University * Kavli Institute for Particle Astrophysics

and Cosmology at Stanford University * Las Cumbres Observatory Global

Telescope Network, Inc. * Lawrence Livermore National

Laboratory * Los Alamos National Laboratory

* National Optical Astronomy Observatory

* Princeton University * Purdue University * Research Corporation * Rutgers University* Stanford Linear Accelerator Center * The Pennsylvania State University * The University of Arizona * University of California, Davis * University of California, Irvine * University of Illinois at Urbana-

Champaign * University of Pennsylvania * University of Pittsburgh * University of Washington

The LSST Camera Team: 72 People from 16 Institutions

Brandeis University J. Besinger, K. HashemiBrookhaven National Lab

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

Florida State University Horst WahlHarvard University

N. Felt, J. Geary (CfA), J. Oliver, C. StubbsIN2P3 - France 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

Lawrence Livermore National Lab S. Asztalos, K. Baker, S. Olivier, D. Phillion, L. Seppala, W. Wistler

Oak Ridge National Laboratory C. Britton, Paul StankusOhio State University

K. Honscheid, R. Hughes, B. Winer

Purdue University K. Ardnt, Gino Bolla, J, Peterson, Ian ShipseyRochester Institute of Technology

D. FigerStanford Linear Accelerator Center - 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

University of California, Berkeley

J.G. Jernigan

University of California, Davis

P. Gee, A. Tyson

University of California, Santa Cruz

T. Schalk

University of Illinois, Urbana-Champaign

J. Thaler

University of Pennsylvania

M. Newcomer, R. Van Berg

Camera Lead Scientist

Kahn (SLAC)

SystemsEngineeringGilmore (act.)

(SLAC)WBS 3.2

Project ControlPrice

(SLAC)WBS 3.1

ElectronicsOliver

(Harvard)WBS 3.5.8

Sensor/RaftDevelopment

Radeka/O’Connor(BNL)

WBS 3.5.4

OpticsOlivier (LLNL)

WBS 3.5.5

CryostatAssemblySchindler(SLAC)

WBS 3.5.7

CalibrationBurke

(SLAC)WBS 3.5.1

Camera Body & Mechanisms

Nordby(SLAC)

WBS 3.5.3

Camera Data Acq. & Control

Schalk(UCSC)

WBS 3.5.6

Camera Integration & Test Planning

Nordby(SLAC)

WBS 3.6

Performance, Safety and Environmental Assurance

(SLAC)WBS 3.3 / 3.4

Observatory Integ., Test & Commission Support

(SLAC)WBS 3.7

Corner RaftWFS/Guider

Olivier(LLNL)

WBS 3.5.9

Camera UtilitiesNordby (SLAC)

WBS 3.5.2

Sensor,Elect, Mech. Dev.

Antilogus(IN2P3)

LPNHE LAL APC

Camera Organizational

Chart Camera Project Scientist

Gilmore (SLAC)

Camera Project Manager

Fouts (SLAC)

WBS 3.1

LSST camera consists of the cryostat and bodyBack Flange

Filter Carousel

Cryostat

L1/L2 Assembly

Filter Auto Changer

Valve Box

Utility Trunk

Filter

Shutter

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LSST will build on successes and resources available at SLAC for I&T

GLAST - LAT

Built at SLAC

LSST Camera

A camera integration plan is complete

Camera Body

Cryostat

L1/L2 assy

UtilityTrunk

Contamination test chamber at SLAC

Fore or Preparation Chamber

Main Chamber

FORE MAIN Camera Controls

cold finger

Other major efforts using SLAC resources

Working is proceeding on plans to deliver a prototype test stand by end of calendar year 2008 - Goal by PDR

LSST Primary Mirror Blank, September 2008

12

LSST Data Management System

Long-Haul CommunicationsChile - U.S. & w/in U.S.

2.5 Gbps avg, 10 Gbps peakHigh-speed transfer

Fault Tolerance

Archive Center

NCSA, Champaign, IL

100 to 250 TFLOPS, 75 PB

Database & Pipeline Parallelization

Fault Tolerance

Data Access CentersU.S. (2) and Chile (1)45 TFLOPS, 87 PB

Data Access, Mining & VisualizationFault Tolerance

Mountain Summit/Base Facility

Cerro Pachon, La Serena, Chile

10x10 Gbps fiber optics25 TFLOPS, 150 TB

Transient Alerts, Pipeline Parallelization

Fault Tolerance

1 TFLOPS = 10^12 floating point operations/second

1 PB = 2^50 bytes or ~10^15 bytes

simulation by A. Kravtsov

Dark Matter Simulations at KIPAC

Full LSST end-to-end photonSimulation

Sky->Atmosphere->Optics->Detector

12 million objects,billions of raytraced photons

Peterson, Meert, Nichols, Grace,Bankert (Purdue)

Jernigan (Berkeley)Connolly (U Wash)

Rasmussen (SLAC)

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

FY-09 FY-10 FY-11 FY-12 FY-13 FY-14 FY-15 FY-16

The current LSST timeline

FY-17FY-07 FY-08

NSF D&D FundingMREFC Proposal Submission

NSF CoDRMREFC Readiness

NSF PDR

NSBNSF CDR NSF MREFC Funding

Commissioning

Operations

DOE R&D Funding

DOE CD-0DOE CD-1

Telescope First Light

DOE OperatingFunds

Camera Ready to Install

NSF + Privately Supported Construction (8.5 years) System First Light

ORR

DOE MIE Funding

Camera Delivered to ChileSensor Procurement Starts

DOE CD-3

DOE CD-2

DOE + Privately Supported Fabrication (5 years) DOE CD-4

Privately Supported camera R&D

Conclusions

* LSST Camera R&D progressing well toward NSF full LSST PDR, scheduled for early 2009.

* A contemporaneous DOE CD-1 would keep the project on track to enable first light in 2016.

* Significant growth in this program is envisioned beginning if FY10, with LSST replacing GLAST/Fermi as the major development effort in particle astrophysics and cosmology at SLAC.