Overview and Status Tony Tyson LSST Director December 3, 2011 PAC2011 KIAA

2 Telescope design Cross section through telescope and camera M1M3 primary mirror Camera M2 Mirror Teams are focused on details of interfaces: Weight, Size, Heat, Utilities, Handling, Controls.

3 1,380 m 2 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

4 Site and facility development is advanced − ARCADIS Chile has delivered the 50% package. 90% package due this year. full procurement package in Non-Federal funds. − Early Site Leveling 5 month, $1.3 M effort completed and No surprises! After ~4,000 kg of explosives and ~12,500 m 3 of rock removal, Stage I of the El Peñón summit leveling is completed.

5 Mirror fabrication is advanced − Primary-Tertiary was cast in the spring of − Fabrication underway at the Steward Observatory Mirror Lab - completion by the end of − NSF-MREFC: support hardware. − Secondary substrate fabricated by Corning in − Currently in storage waiting for construction. − NSF-MREFC: optical surface finishing and support hardware.

6 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

7 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 − 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 − 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

8 LSST six filter system Wavelength (nm) Relative system throughput (%) Includes sensor QE, atmospheric attenuation, optical transmission functions

9 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!

10 Two planned LSST surveys MAIN SURVEY Deep 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 SURVEY 10% of time: ~30 selected fields. 300 square degrees Continuous 15 sec exposures. 1hour/night

LSST Wide-Fast-Deep survey 4 billion galaxies with photometric redshifts 20 trillion photometric measurements of 20 billion objects > 20PB database Immediate transient alerts

12 LSST Science Charts New Territory Probing Dark Matter And Dark Energy Mapping the Milky Way Finding Near Earth Asteroids

13 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.”

14 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

15 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)

16 LSST All Hands Meeting 2010 August

17 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

18 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 range Successful Review (LSST): November 1-3, 2011

19 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

20 Summary of LSST project requests for federal construction funding Engineering first-light 2018 Science verification testing begins 2019 Full science operations begin 2020 ComponentBudget (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

21 Integrated Project Schedule with Key Milestones Fiscal Year Key Milestones 6 years, 7 months International partner agreements in place for support of operations share

22 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 annually Complete 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

23 Headquarters Site Headquarters Facility Observatory Management Science Operations Education and Public Outreach Archive Site Archive Center Alert Production Data Release Production Long-term Storage (copy 2) Data Access Center Data Access and User Services Base Site Base Facility Long-term storage (copy 1) Data Access Center Data Access and User Services Summit Site Summit Facility Telescope and Camera Data Acquisition Crosstalk Correction One System, Two Continents, Four Sites Additional Processing Site(s) Data Release Production

LSST Operations Plan and Total Survey Cost Operations: 137 FTE’s, $37.2M/yr (2011USD) DataManagement ObservatoryOperations ProjectManagement EPO CommunitySoftware Total LSST Survey cost: $1.25B $9M/yr from International Partners

25 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.

26 Funding LSST operations − Operations budget: $37.2M/yr (2011 FY$) − Proposed obligations: NSF:$19M/yr DOE:$ 9M/yr = $ 28M/yr  75% of recommended budget − The project must obtain funding for the remaining $9.2M/yr from international partners

27 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, − 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 MOU by 2015.

28 Integrated Project Schedule with Key Milestones Fiscal Year Key Milestones 6 years, 7 months International partner agreements in place, for support of construction

29 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 Hopefully sooner.

30 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)

31 China – LSST Collaboration  Important to join LSST early  Benefit to other Chinese projects Example: LSST software system will be valuable to Chinese survey projects

32 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.

33 China – LSST Collaboration We look forward to collaboration with our Chinese colleagues!

34 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.

35 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.

36 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