Overview and Status

Tony TysonLSST Director

December 3, 2011PAC2011 KIAA

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Telescope design

LSST Ver 3.3_Baseline_Design.zmxConfiguration 3 of 6

3D Layout

LSST Ver 3.3 Baseline Design

3/2/2011

X Y

Z

Cross section through telescope and camera

M1M3 primary mirror

Camera

M2 MirrorTeams are focused on details of interfaces:• Weight,• Size,• Heat,• Utilities,• Handling,• Controls.

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1,380 m2 service and maintenance facility

30 m diameter dome

Control room and heat producing equipment

(lower level)

1.2 m diameter atmospheric telescope

Stray light and Wind Screen

350 ton telescope

Calibration Screen

Base Facility

Scope includes the facilities, and hardware to collect the light, control the survey, calibrate conditions, and support all LSST summit and base operations.

Telescope and Site

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Site and facility development is advanced

− ARCADIS Chile has delivered the 50% package.90% package due this year.full procurement package in 2012.Non-Federal funds.

− Early Site Leveling5 month, $1.3 M effort completed and No surprises!

After ~4,000 kg of explosives and ~12,500 m3 of rock removal, Stage I of the El Peñón

summit leveling is completed.

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Mirror fabrication is advanced

− Primary-Tertiary was cast in the spring of 2008.− Fabrication underway at the Steward Observatory

Mirror Lab - completion by the end of 2012.− NSF-MREFC: support hardware.

− Secondary substrate fabricated by Corning in 2009.− Currently in storage waiting for construction. − NSF-MREFC: optical surface finishing and support

hardware.

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Camera

Filter

L1 Lens

Utility Trunk—houses support electronics and utilities

Cryostat—contains focal plane & its electronics

Focal plane

L2 Lens

L3 Lens

Camera ¾ Section

1.65 m(5’-5”)

− 3.2 Gigapixel science array – 63 cm diameter− Wavefront and guide sensors− 2 second readout− 5 filters in camera− Electronics

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Novel design CCDs

ITL− 4 mechanical samples - achieved best flatness of 5.3µm

peak-to-valley (specification = 5 µm P-V).− Prototype of fully-operable sensors: December 2011. − Wafer lot completed at DALSA , probe testing at ITL.e2V− 3 mechanical samples - the device peak-to-valley is

3.44µm and 99% of the surface is within 2.39µm.− Received two partially-operable 4K x 4K samples.− Prototype of fully-operable sensors: October 2011.− Wafer probe tests - 80% of the devices have 16/16

working amplifiers. − New antireflection coating developed with QE > 80% in

griz, > 60% in u.

ITL buttable package

e2v 4K x 4K device in test Dewar

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LSST six filter system

Wavelength (nm)

Rela

tive

syst

em th

roug

hput

(%)

Includes sensor QE, atmospheric attenuation, optical transmission functions

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LSST Observing Cadence

Pairs of 15 second exposures (to 24.5 mag) per visit to a given position in the sky.

Visit the same position again within the hour with another pair of exposures.

Number of 9.6 sq.deg field-of-view visits per night: 900

Detection of transients announced within 60 seconds.Expect 1-2 million alerts per night!

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Two planned LSST surveys

MAIN SURVEYDeep Wide Survey: 18,000 square degrees to a uniform depth of u: 26.7 g: 27.5 r: 27.7 i: 27.0 z: 26.2 y: 24.9

DEEP DRILLING SURVEY10% of time: ~30 selected fields. 300 square degrees Continuous 15 sec exposures. 1hour/night

LSST Wide-Fast-Deep survey LSST Wide-Fast-Deep survey 4 billion galaxies with photometric redshifts

20 trillion photometric measurements of 20 billion objects

> 20PB database

Immediate transient alerts

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LSST Science Charts New Territory

Probing Dark MatterAnd Dark Energy Mapping the Milky Way

Finding Near Earth Asteroids

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Astro2010 Endorsement

LSST ranked as the highest priority large ground-based facility for the next decade.

“The top rank accorded to LSST is a result of (1) its compelling science case and capacity to address so many of the science goals of this survey and (2) its readiness for submission to the MREFC process as informed by its technical maturity, the survey’s assessment of risk, and appraised construction and operations costs. Having made considerable progress in terms of its readiness since the 2001 survey, the committee judged that LSST was the most ‘ready-to-go.”

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LSST Corporation founded in 2003 to build and operate the LSST.

- The University of Arizona- University of Washington- National Optical Astronomy Observatory- Research Corporation for Science

Advancement- Adler Planetarium- Brookhaven National Laboratory (BNL) - California Institute of Technology- Carnegie Mellon University- Chile- Cornell University- Drexel University- Fermi National Accelerator Laboratory - George Mason University- Google, Inc.- Harvard-Smithsonian Center for

Astrophysics- Institut de Physique Nucléaire et de

Physique des Particules (IN2P3)- Johns Hopkins University- Kavli Institute for Particle Astrophysics

and Cosmology (KIPAC) - Stanford University- Las Cumbres Observatory Global

Telescope Network, Inc.

- Lawrence Livermore National Laboratory (LLNL)

- Los Alamos National Laboratory (LANL)- National Radio Astronomy Observatory- Princeton University- Purdue University- Rutgers University- SLAC National Accelerator Laboratory- Space Telescope Science Institute- Texas A & M University- The Pennsylvania State University- University of California at Davis- University of California at Irvine- University of Illinois at Urbana-

Champaign- University of Michigan- University of Pennsylvania- University of Pittsburgh- Vanderbilt University

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LSST Science Collaborations (Michael Strauss, chair; 419 members so far)

Supernovae: Richard Kessler & Michael Wood-Vasey (39 members) Weak Lensing: Bhuvnesh Jain & David Wittman (63 members) Stellar Populations: Kevin Covey & Knut Olsen (56 members) Active Galactic Nuclei: Niel Brandt (26 members)Solar System: Michael Brown & Lynne Jones (31 members) Galaxies: Harry Ferguson (34 members)Transients/variable stars: Josh Bloom & Lucianne Walkowicz (66 members)Large-scale structure/baryon oscillations: Hu Zhan & Eric Gawiser (49 members) Milky Way and Local Volume Structure: Marla Geha & Beth Willman (36 members) Strong Lensing: Phil Marshall (17 members) Informatics and Statistics: Kirk Borne (37 members)

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LSST All Hands Meeting 2010 August

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LSST: Joint DOE/NSF Project

National Science Foundation

– Lead agency• Telescope and site• Data Management

– Successful Review: August, 2011• Earliest possible NSF construction start: March 2014

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Joint DOE/NSF Project

Department of Energy

– Deliver a 3.2 Gpixel camera that meets project requirements– Agency status:

– CD-0: Approve Mission Need: Dark Energy Stage IV Experiment(s)

– CD-1: Select option to move forward and set cost rangeSuccessful Review (LSST): November 1-3, 2011

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Lead Organizations for Subsystems

– SLAC is lead organization for camera– NOAO will provide telescope and site team– NCSA will construct and test archive and data access centers

− Formal agreements define:• Scope of work• Require compliance with Science Requirements Document and flow-

down to system specifications and subsystem requirement• Require compliance with reporting requirements • Require use of LSST document archive

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Summary of LSST project requests for federal construction funding

Engineering first-light 2018Science verification testing begins 2019Full science operations begin 2020

Component Budget (then-year USD)

NSF Base Budget $347,911,000

NSF Contingency $ 81,439,000

DOE Camera Base Budget $113,063,000

DOE Camera Contingency $ 44,937,000

Total $587,350,000

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Integrated Project Schedule with Key Milestones

Fiscal Year

Key Milestones6 years, 7 months

International partner agreements in place for support of operations share

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Operations Plan: Scope

− Conduct survey for 10 years Maintain throughput, Maintain facilities

− Process data to produce near-real time alerts and archives of raw images

− Issue data release annuallyComplete reprocessing of all data obtained to date

− Issue deep co-added images annually− Provide access to computer resources for analyzing data− Assist the community in accessing and using the data− Incorporate or federate community-supplied data products

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Headquarters SiteHeadquarters FacilityObservatory ManagementScience OperationsEducation and Public Outreach

Archive SiteArchive Center

Alert ProductionData Release Production

Long-term Storage (copy 2)Data Access Center

Data Access and User Services

Base SiteBase Facility

Long-term storage (copy 1)Data Access Center

Data Access and User Services

Summit SiteSummit Facility

Telescope and CameraData Acquisition

Crosstalk Correction

One System, Two Continents, Four Sites

Additional Processing Site(s)

Data Release Production

52%

21%

15%

8%

4%

LSST Operations Plan and Total Survey Cost

Operations: 137 FTE’s, $37.2M/yr (2011USD)

Data Management

Observatory Operations

Project Management

EPOCommunitySoftware

Total LSST Survey cost: $1.25B

$9M/yr from International Partners

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Data Policy

− All LSST data and derived data products will be immediately available to US scientists and those in the host country, Chile. Estimate at least 100 PB of processed images and 20 PB database, plus 800 TF of computation.

− Alerts of transient object detection (time, position, color JPG) will be broadcast world-wide within 60 sec. Estimate 1-2 million alerts per night. Full characterization of these events requires access to all data products.

− Other world-wide access to LSST data and data products will be via collaboration. Contributions to the LSST Project and to a fair share of operations is expected.

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Funding LSST operations

− Operations budget:$37.2M/yr (2011 FY$)

− Proposed obligations:NSF: $19M/yrDOE: $ 9M/yr

= $ 28M/yr 75% of recommended budget

− The project must obtain funding for the remaining $9.2M/yr from international partners

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International Partner contributions to LSST operations

− Usage-based model:− Suppose there are N Principal Investigators outside the US and

Chile now who are interested in LSST data in future.− Estimate N_China (PIs now who are interested in LSST data in future )− Chinese contribution = $9M x N_China / N per year, 2020-2030− Other models give similar results for operations sharing

− This can be done on a per-institute basis, or via a multi-institute consortium

A Letter of Intent to support China’s share of operations is needed December 2011

Details negotiated 2012-2014. MOU by 2015.

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Integrated Project Schedule with Key Milestones

Fiscal Year

Key Milestones6 years, 7 months

International partner agreements in place, for support of construction

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International Partner contributions to LSST Construction and Science Capability

As in all science collaborations:− Intellectual involvement early!− Explore possibilities for contribution− Negotiate with LSST Project

− This can be done on a per-institute basis

A draft Memorandum of Understanding is due before 2013. Hopefully sooner.

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Schedule for International Agreements

− December 2011: Letters of Interest for operations support

− April 2012: Memorandum of Understanding (MOU) for share of operations support (best if done as a consortium)

− 2012 – 2014: If possible, a separate MOU for collaboration in R&D and contributions during construction (this can be done on a per-institute basis)

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China – LSST Collaboration

Important to join LSST early

Benefit to other Chinese projects Example: LSST software system will be

valuable to Chinese survey projects

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Three classes of useful LSST spectroscopy

1. Calibration samples for quantities that can be derived from photometric data: photometric redshifts for galaxies, photometric metallicity for stars

2. Supplemental data that cannot be obtained from LSST data: radial velocity, emission and absorption line strengths

3. Identification spectra for transient, weird and unusual objects (SNe, GRB followup, high-z quasars, brown dwarfs)

These differ by the needed sample size, sample depth, required spectral resolution, and the time delay relative to imaging data.

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China – LSST Collaboration

We look forward to collaboration with our Chinese colleagues!

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Data Management

− LSST Data Management system must deal with an unprecedented data volume.– one 6-gigabyte image every 17 seconds– 15 terabytes of raw scientific image data / night– 100-petabyte final image data archive– 20-petabyte final database catalog– 2 million real time events per night every night for 10 years

− The software, framework and database designs are in place for highly reliable open source system.

− Infrastructure is identified and anticipates modest technical advancement consistent with trends.

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LSST data processing pipelines are designed, prototyped and tested in data challenges

− 2011 Data Challenge is fourth major data challenge.– Assessed end-to-end data quality of multi-terabyte dataset.– Validated infrastructure and middleware reliability at 15% capacity.

− Unique database design to address multiple trillion row data sets.

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Opportunities for Collaboration in Data

− Providing input to aspects of the Data Management System design that remain under discussion– Applications/algorithms– User interfaces and tools– Database schema and standard queries– Data quality metrics and tools– Community-supplied data production support capabilities

− Participating actively in the development and test of the data management system architecture– Analyze pre-cursor and simulated data processed by prototype

science pipelines– Determine the data quality and scientific suitability– Identify systematic effects– Identify calibration issues