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DOE Annual Program Review Center for Particle Astrophysics Scott Dodelson

DOE Annual Program Review Center for Particle Astrophysics Scott Dodelson. We study Fundamental Physics. Dark Energy Dark Matter Neutrino Mass Seeds of Primordial Structure. These are arguably the most compelling discoveries to date of Physics Beyond the Standard Model.

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DOE Annual Program Review Center for Particle Astrophysics Scott Dodelson

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  1. DOE Annual Program Review Center for Particle Astrophysics Scott Dodelson

  2. We study Fundamental Physics • Dark Energy • Dark Matter • Neutrino Mass • Seeds of Primordial Structure These are arguably the most compelling discoveries to date of Physics Beyond the Standard Model Center for Particle Astrophysics

  3. Center Projects Chicagoland Observatory for Underground Particle Physics (COUPP) Cryogenic Dark Matter Search (CDMS) Dark Energy Survey (DES) GammeV Pierre Auger Observatory Sloan Digital Sky Survey (SDSS) SuperNova Acceleration Probe (SNAP) Theoretical Astrophysics Center for Particle Astrophysics

  4. COUPP • Competitive sensitivity for spin-dependent scattering, despite high backgrounds. Spin-dependent Spin-independent Center for Particle Astrophysics

  5. Pierre Auger ExpObs >1019.6 132 +/- 9 51 > 1020 30 +/- 2.5 2 Suppression evident at high energy Calibration unc. 18% FD syst. unc. 22% 5165 km2 sr yr ~ 0.8 full Auger year Center for Particle Astrophysics

  6. CDMS Center for Particle Astrophysics

  7. SDSS Tegmark et al. 2006 Center for Particle Astrophysics

  8. SDSS The 8 O’Clock Arc, the brightest known lensed Lyman Break Galaxy (LBG), with a redshift z=2.73 (Allam et al. 2007) 3 newly confirmed lensed arc systems from SDSS, with z=2.0-2.4 Gravity helps reveal a brilliant jewel of the early universeSLOAN DIGITAL SKY SURVEY NEWS RELEASEPosted: November 8, 2006 Discovered via systematic searches of the SDSS data, with ongoing and proposed multi-wavelength follow-up from ground and space-based telescopes S. Allam, H. Lin, T. Diehl, D. Tucker et al. Center for Particle Astrophysics

  9. GammeV Shining Light through a Wall to search for axions and/or chameleons First Results in Poster Session Tonight! Center for Particle Astrophysics

  10. Dark Energy Survey Blanco 4-meter at CTIO • Study Dark Energy using 4 complementary techniques: I. Cluster Counts II. Weak Lensing III. Baryon Acoustic Oscillations IV. Supernovae • Two multiband surveys: 5000 deg2g, r, i, z 9 deg2 repeat (SNe) • Build new 3 deg2 camera and Data Management system 5 year Survey (525 nights) Center for Particle Astrophysics

  11. CCD Readout Filters Shutter DECam • CCD development is on track • 40 2kx4k devices + 10 2kx2k CCDs delivered to Fermilab this summer (May - June 2007) • Estimates of the yield based on these devices are consistent with the cost and schedule estimates • Readout of 4 CCD mosaic meets noise and readout speed requirements (July 2007) • Prototype high-density readout boards (Spain and FNAL) meet requirements • Acquisition of large lenses (STFC and university) • Procurement of glass blanks awarded • Tenders for polishing the blanks due in September • We anticipate a baseline DOE cost for DECam in the range of $24.1M – $26.7 M and a scheduled completion date from April 2011-April 2012 Optical Lenses DECam Focal Plane • 62 2kx4k Image CCDs: 520 MPix • 8 2kx2k focus, alignment CCDs • 4 2kx2k guide CCDs Center for Particle Astrophysics

  12. SNAP Have started internal discussions on FNAL role in SNAP • Science: Weak lensing & SN1A • Calibration Photometric & Astrometric • “Slice” Electronics Manage data prior to transmission • CCD and Front-end Electronics packaging and Testing SiDet is a Production Facility • Software/Simulations/Data Management Experience with Large HEP & SDSS Datasets “On-Track” Plan Center for Particle Astrophysics

  13. SNAP Leadership Plan • Software/Simulations/Data Management • FNAL processes, manages, analyzes, and serves O(Pbyte)-size data samples & has experience with astronomical data from SDSS • We’d like to design and build the data handling, processing, cataloging, archiving, and serving systems • Focal Plane Assembly • Less modest hardware effort • Build & test this Center for Particle Astrophysics

  14. Budget Includes indirect and scientists but not (DES) project costs Experimental RA salaries in CPA starting in June 07. Center for Particle Astrophysics

  15. Organization Center for Particle Astrophysics

  16. Intellectual Environment • Weekly Seminars • Semi-Annual Workshops (Dark Matter, Strong Lensing) • Move to Wilson Hall 6&7 unifies different groups • Weekly Journal Discussion • Weekly Chalk Talk • Weekly SDSS Science Meeting • Quarterly All-Hands Meetings } New in 2007 Center for Particle Astrophysics

  17. Preparing for the Future Center for Particle Astrophysics

  18. Visitors • Learn the field (Bohn, Perera, Riberio, Schramm, Shapiro, Soares-Santos, ~15 summer students) • Support projects (Ahn, Blasi (Auger), Brink (CDMS), Butner (SDSS), Dall’aglio, Depoy (DES), Deustua (SNAP), Hamilton, Jaffe, Lahav (DES), Makler (DES), McElrath, Powell, Smith (SDSS), Taylor, Wayth, Weller (DES), Zhang, Zlosnik, Zurek) • Future projects (Byrum, Habib, Heitman, Meyer, Peterson, Shutt, Timbie, Vassiliev, Winstein) Build a Users Community Center for Particle Astrophysics

  19. Research Associates • Can help drive science (e.g., CDMS) • Separate Ad/Committee (Offer to Ahn accepted to work on Auger) • Moved RAs to Center • Responsibility (organize seminars, chalk talks, web site, workshops) • Monthly Meetings • Be proactive in helping them get jobs Center for Particle Astrophysics

  20. Cosmological Computing • Essential for extracting information about dark energy from upcoming experiments (DES, SNAP) • Local Expertise/Interest • Seed national collaboration, uniting disparate efforts (in supercomputing 2+2<4) Center for Particle Astrophysics

  21. Cosmological Computing • Hire Gnedin (7/05) • Bring idea to Futures Committee (12/06) • Present idea to Directorate (1/07) • Apply for FRA grant; open discussion with KICP (2/07) • Include Computing Division, LQCD, Kravtsov on Task Force (4/07) • Place Requisitions w/ money from FRA, KICP, Theory (7/07) • Submit Task Force Report (8/07) • Begin Discussions with representatives from other Labs (8/07) Need Scientific Talent Full support; refinement Look for funding Leverage FNAL’s resources Center for Particle Astrophysics

  22. Retreat Wed., Nov. 7: ------------ 9:00-9:45 Goals of the Retreat 9:45-10:15 Coffee break 10:15-11:15 UHECR: Beyond Auger South 11:15-11:45 Gravity waves: beyond LIGO 11:45-12:15 Discussion 12:15-1:30 Lunch 1:30-2:30 Computational Astrophysics 2:30-3:30 21 cm observations 3:30-4:00 Break 4:00-5:00 CMB 5:00-6:00 Direct dark matter detection George Williams College, Geneva, WI Thurs., Nov. 8 -------------- 9:00-10:00 Optical cosmology 10:00-10:30 Near-infrared observations 10:30-11:00 Break 11:00-12:00 Indirect Dark matter detection 12:00-12:30 Discussion 12:30-2:00 Lunch 2:00-2:30 Underground laboratory/experiments 2:30-3:00 Discussion 3:00-4:00 Recap/lessons/next steps Center for Particle Astrophysics

  23. Conclusions • Fermilab has a suite of exciting astrophysics projects which are producing results and/or on schedule to add to our knowledge of Physics Beyond the Standard Model • The Fermilab Center for Particle Astrophysics has created a thriving intellectual environment dedicated to the success of its projects • Over the past year, we’ve instituted the structures which will: ● establish FNAL as a User facility for astrophysicists ● ensure that Fermilab will be heavily involved in the science of its projects ● enable the Center to play a leading role in charting the future of the field Center for Particle Astrophysics

  24. Backup Slides Center for Particle Astrophysics

  25. Center for Particle Astrophysics

  26. Cosmological Computing • As of today, CD maintains an 8 core cluster for cosmology • Other groups have many more resources: • Virgo Consortium: 670 CPU SparcIII, 816 CPU Power4 • ITC, Harvard: 316 CPU Opteron, 264 CPU Athlon • LANL: 294 CPU Pentium4 (just for cosmology) • CITA: 270 CPU Xeon cluster • SLAC: 72 CPU SGI Altrix, 128 CPU Xeon cluster • Princeton: 188 CPU Xeon cluster • UWash: 64 CPU Pentium cluster • Using FRA grant and contribution from KICP (UC), CD will host/maintain 560 core cluster for cosmology by December • CD participating in Task Force to unify cosmological computing on a national scale • Crucial to extract fundamental physics from astrophysical observations (SDSS, DES, SNAP)→ Complements/enhances experimental program Center for Particle Astrophysics

  27. Preparing for the Future Can we do better? Center for Particle Astrophysics

  28. The Dark Energy Survey Blanco 4-meter at CTIO • Study Dark Energy using 4 complementary* techniques: I. Cluster Counts II. Weak Lensing III. Baryon Acoustic Oscillations IV. Supernovae •Two multiband surveys: 5000 deg2g, r, i, z 9 deg2 repeat (SNe) •Build new 3 deg2 camera and Data management system 5 year Survey (525 nights) Response to NOAO AO *in (systematics, cosmological parameter degeneracies, Geometry vs. Structure growth) Center for Particle Astrophysics

  29. Overlap with the South Pole Telescope (SPT) SZ survey to measure cluster masses and redshifts • Deep, Multi-band survey: SDSS g,r,i,z (or Z,Y) filters to measure photo-z’s, red sensitive CCDs • Projecting a factor of 4.6 improvement in the Figure of Merit over Stage II projects DES Forecasts: Power of Multiple Techniques Figure of Merit: inverse area of ellipse Ma, Weller, Huterer, etal

  30. DES Collaboration Red = joined in the past 6 months • Fermilab: J. Annis, E. Buckley-Geer, H. T. Diehl, S. Dodelson, J. Estrada, B. Flaugher, J. Frieman, S. Kent, H. Lin, P. Limon, K. W. Merritt, J. Peoples, V. Scarpine, A. Stebbins, C. Stoughton, D. Tucker, W. Wester • University of Illinois at Urbana-Champaign W. Barkhouse, C. Beldica, R. Brunner, I. Karliner, J. Mohr, C Ngeow, R. Plante, T. Qian, P. Ricker, M. Selen, J. Thaler • University of Chicago: J. Carlstrom, S. Dodelson, J. Frieman, M. Gladders, W. Hu, E. Sheldon, R. Wechsler Graduate students: C. Cunha, M. Lima, H. Oyaizu • Lawrence Berkeley National Laboratory: N. Roe, C. Bebek, M. Levi, S. Perlmutter • University of Michigan: R. Bernstein, B. Bigelow, M. Campbell, D. Gerdes, A. Evrard, W. Lorenzon, T. McKay, M. Schubnell, G. Tarle, M. Tecchio • NOAO/CTIO: Tim Abbott, Chris Miller, Chris Smith, Nick Suntzeff, Alistair Walker • Spanish Consortium: Institut d'Estudis Espacials de Catalunya (IEEC/CSIC): Francisco Castander, Pablo Fosalba, Enrique Gaztañaga, Jordi Miralda-Escude; Institut de Fisica d'Altes Energies (IFAE):Enrique Fernández, Manel Martínez, Ramon Miquel; CIEMAT, Madrid: C. Maña, M. Molla, E. Sanchez, J. Garcia-Bellido (UAM) • United Kingdom Consortium: University College London: O. Lahav, D. Brooks, P. Doel, M. Barlow, S. Bridle, S. Viti, J. Weller: University of Cambridge: G. Efstathiou, R. McMahon, W. Sutherland; University of Edinburgh: J. Peacock; University of Portsmouth Institute of Cosmology and Gravitation: R. Crittenden, R. Nichol, W. Percival; University of Sussex: A. Liddle, K. Romer • University of Pennsylvania: M, Bernardi, G. Bernstein, M. Devlin, B. Jain, M. Jarvis, R. Jimenez, L. Gladney, M. Sako, R. Seth, L. Verde • Brazil-DES Consortium:Observatorio Nacional (ON): Staff: L. da Costa, P. S. Pellegrin, M. Maia, C. Benoist; Post-Docs: J. M. Miralles, L. F. Olsen, R. Ogando: Centro Brasileiro de Pesquisas Fisicas (CBPF): M. Makler Universidade Federal do Rio de Janeiro (UFRJ): I. Waga, M. Calvao; Universidade Federal do Rio Grande do Sul (UFRGS): B. Santiago • The Ohio State University: D. DePoy, K. Honscheid, C. Kochanek, P. Martini, D. Terndrup, D. Weinberg, T. Walker • Argonne National Laboratory: S. Kuhlmann, H. Spinka, Rich Talaga Center for Particle Astrophysics

  31. DES Organization • DES consists of three projects and the Science Committee • DECam: Fermilab • Data Management: NCSA • CTIO Facilities Upgrades: CTIO/NOAO • The DES council provides over-site • DES Project Director coordinates the three projects and the science committee Center for Particle Astrophysics

  32. DECam replaces the Prime Focus Cage of the Blanco F8 Mirror Filters Shutter 3556 mm CCD Read out Hexapod Optical Lenses 1575 mm Center for Particle Astrophysics

  33. DES Project Approval Status • July 2006: • Positive recommendation to proceed with DES from P5 to HEPAP • Fermilab Directors review, practice for CD-1 review by DOE • Oct. 2006: NSF and DOE request “end-to-end” description of DES in the form of a proposal. This was competed at the end of Dec.06. • Feb. 2007: DECam is in the FY08 presidents budget request for a construction start in FY08 (a necessary, but not sufficient step as we still need to go successfully through the DOE review process) • May 1-3 2007: joint NSF-DOE review of DES • This will serve as the CD-1 review of the DECam project • Will also review Data management and plans for upgrades to the Blanco • Aim for CD2/3 ~ Nov. 2007 with construction start ~ March 2008 Center for Particle Astrophysics

  34. DOE and NSF Actions on DES in 2007 Actions prior to July 31, 07: • The DOE FY08 Congressional Budget Request contains $3.6 M for DES MIE, but expenditures are contingent on successful scientific and technical readiness reviews by DOE and NSF. • Joint DOE-NSF review of DES held at Fermilab 1-3 May 07 • The Review Committee recommended that DOE pursue CD-1 approval for the DECam project • DECam, Data Management, NOAO, and Science Teams are actively addressing the 58 recommendations • DOE and NSF formed a Joint Oversight Group for DES- it has met ~10 times since late May • DOE awarded DECam $900 K of funds for Dark Energy R&D Center for Particle Astrophysics

  35. DOE and NSF Actions on DES in 2007 cont’d Actions since August 1, 07 • DOE and NSF agreed to proceed to the next stage of DES; continuation of DOE R&D support for DECam, initial NSF support of Data Management at NCSA and NOAO support of CTIO upgrades • NSF-AST recommended funding for DES Data Management: sufficient for full effort for ~ 15 months • Acquisition Strategy submitted to Office of Science for approval and we hope to have CD-1 approval by the end of September • 2nd Joint NSF-DOE review of DES has been scheduled for 29-31 Jan 08. It will serve as the DOE CD-2 review of DES, the NSF review of the 2nd DES proposal to NSF for data management and the review of DES planning for commissioning and operations. Center for Particle Astrophysics

  36. Institutions Participating in the DES Collaboration • Fermilab • University of Illinois at Urbana-Champaign • University of Chicago • Lawrence Berkeley National Laboratory • University of Michigan • NOAO/CTIO • Spain-DES Collaboration: Institut d'Estudis Espacials de Catalunya (IEEC/ICE), Institut de Fisica d'Altes Energies (IFAE), CIEMAT-Madrid: • United Kingdom-DES Collaboration: University College London, University of Cambridge, University of Edinburgh, University of Portsmouth, University of Sussex • The University of Pennsylvania • Brazil-DES Consortium • The Ohio State University • Argonne National Laboratory 17 institutions and 110 participants Center for Particle Astrophysics

  37. The DES Organizationa collaboration perspective Center for Particle Astrophysics

  38. CCD Readout Filters Shutter DECam Summary • To meet the science requirements, within the allocated time period (525 nights) DECam must have: • 3 sq. deg. field of view with excellent image quality • red sensitive CCDs • g,r,i,Z,Y filters • The CCD Procurement is on track • 40 2kx4k devices + 10 2kx2k CCDs delivered to Fermilab this summer (May - June 2007) • Estimates of the yield based on these devices are consistent with the cost and schedule estimates • Readout of 4 CCD mosaic meets noise and readout speed requirements (July 2007) • Prototype high-density readout boards (Spain and FNAL) meet requirements • Acquisition of large optical elements (STFC and university) • Procurement of glass blanks awarded • Tenders for polishing the blanks due in September • We anticipate a baseline DOE cost for DECam in the range of $24.1M – $26.7 M and a scheduled completion date from April 2011-April 2012 Optical Lenses DECam Focal Plane • 62 2kx4k Image CCDs: 520 MPix • 8 2kx2k focus, alignment CCDs • 4 2kx2k guide CCDs Center for Particle Astrophysics

  39. Center for Particle Astrophysics

  40. Center for Particle Astrophysics

  41. Center for Particle Astrophysics

  42. Center for Particle Astrophysics

  43. COUPP 60 Kg Chamber • Construction of a new 60 kg chamber was approved by the PAC and director last fall. • Now under construction-- will run in 2008. Steel Outer Vessel Quartz Inner Vessel

  44. Discrimination strategies • Most particle physics experience in MeV range • Direct detection requires keV scale Sub-K low threshold large mass >$$ Phonons10 meV/ph CDMS EDELWEISS CRESST DAMA ZEPLIN I DEAP CLEAN Initially need both Ionization~ 10 eV/e Scintillation~ 1 keV/γ ZEPLINXENON WArP, ArDM Scintillation high threshold Noble liquids high threshold but large mass <$$ Center for Particle Astrophysics

  45. Compare CDMS with noble liquids Best resolution from SCDMS experiment allows better discovery potential In the end, the tails of the background distributions determine the sensitivity 99% discrimination to below ~10 keV XENON Prototype Best CDMS Ge ZIP gammas overlap starts at ~50 keV counting statistics for more detail see http://www.physics.ucla.edu/hep/dm06/talks/shutt.pdf n-recoils Center for Particle Astrophysics

  46. Fundamental technology differences • Left out of DM SAG presentation is technology risk associated with noble liquid experiments due to x10 intrinsically worse resolution. • See examples of problems in preprints from WARP and ZEPLIN II (hard to review private communication to DM SAG from XENON 10). • Very intricate phenomenology that will take time to understand and calibrate (energy, contamination etc.). • Not wise to lose best technology even if more expensive - we do not want to be in the DAMA situation again. • Since a large fraction of the costs are people, there is only a modest savings between SCDMS and any of the proposed experiments once they mature. • Essential to understand backgrounds and to have very good discrimination. • Example is the degradation of sensitivity in the present ZEPLIN II results from the fact that they have a background that they cannot reject. • A caution against assuming that the new technologies can mature too quickly in this very challenging research. Center for Particle Astrophysics

  47. FNAL has made a splash in CDMS w/ relatively small investment. • RA’s have made a big difference. Center for Particle Astrophysics

  48. CDMS II Continuing to Run at Soudan CDMS is the only direct detection dark matter experiment currently running without backgrounds! 814 kg-day exposure DAMA MSSM Published CDMS limit Xenon10 limit Current sensitivity of CDMS Large calibration data sets High efficiency for collecting data Center for Particle Astrophysics

  49. CDMS Collaboration at Soudan DOE Laboratory Fermilab LBNL DOE University Brown CalTech Florida Minnesota MIT Stanford UC Santa Barbara NSF Case Western Reserve Colorado (Denver) Santa Clara UC Berkeley Canada Queens Center for Particle Astrophysics

  50. Fermilab responsibilities in CDMS II Established roles in CDMS Project Management Project Manager, Financial support people Operations Lead the Soudan operations on both physicist and technical sides Cryogenics Lead the design, construction and testing of the cryogenics systems Electronics, DAQ, Computing Warm electronics, event builder software, online and offline processing Infrastructure Clean rooms, control rooms, computing rooms Analysis Independent analysis chain (based on ROOT, time-domain pulse fitting) Center for Particle Astrophysics

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