SLOAN DIGITAL SKY SURVEY (E885) Stephen Kent (CD/EAG)

1. I. Description/Status of survey II. Science projects with SDSS Galaxies and Large Scale Structure Quasars Milky Way Structures SLOAN DIGITALSKY SURVEY (E885)Stephen Kent (CD/EAG) FNAL Users Meeting June 10, 2002

2. Fermi National Accelerator Laboratory Princeton University University of Chicago Institute for Advanced Study Japanese Promotion Group US Naval Observatory University of Washington Johns Hopkins University Max Planck Institute for Astronomy, Heidelberg Max Planck Institute, Garching New Mexico State University (new) Los Alamos National Laboratory (new) University of Pittsburgh Partner Institutions

3. FNAL ROLE IN SDSS • Participants • EAG (10 Scientists*, 5 CP, 0.4 staff) • Other CD (1 CP, 1 FTE) • TAG (3 scientists) • PPD (5 eng/tech, 2.5 staff) • BD (0.5 FTE) • Students • 3 Thesis (U of Ch.) • Responsibilities • DAQ system, maintenance/upgrade • Data processing HW, some SW, operations • Data distribution • Telescope & Systems engineering (APO) *includes 1 ex-director

4. Goals: 1. Image ¼ of sky in 5 bands (Scope is now reduced by 1/3) 2. Obtain redshifts of 1 million galaxies and quasars Science: Measure large scale structure of a) galaxies in 0.2% of the visible universe b) quasars in 100% of the visible universe Astrophysics/Particle Physics Connection: Large scale structure today arose in universe from processes occurring above T=1027 K (E=1014 Gev). Sloan Digital Sky Survey

5. Detectors/Equipment 2.5 m Telescope Mosaic Imaging Camera “Photometric” telescope 640 Fiber Spectrograph

6. Survey Operations 1. Image Sky 2. Identify Galaxies, Quasars 3. Design Plugplates 4. Obtain Spectra

7. Sloan Digital Sky Survey(CD/EAG, PPD/TAG)Current Status (Jun. 2002) Sloan Digital Sky Survey(CD/EAG, PPD/TAG)Current Status (Jun. 2002) Percent Complete Percent Complete Baseline Baseline IMAGING IMAGING 8452 sq. deg. 8452 sq. deg. 44% as of Apr 15, 2002 44% as of Apr 15, 2002 SPECTROSCOPY SPECTROSCOPY 1688 tiles 1688 tiles 29% as of Apr 15, 2002 29% as of Apr 15, 2002 MT (calibrations) MT (calibrations) 1563 patches 1563 patches 63% as of Apr 15, 2002 63% as of Apr 15, 2002 Operations began: Apr 1, 2000 Operations began: Apr 1, 2000 Operations end: Jun 30, 2005 Operations end: Jun 30, 2005

8. Topics Hi Z Quasars Gravitational Lensing QSO & Galaxy Corr. Function Galaxy Clusters Galaxy Struct./Evol. Milky Way Halo Brown Dwarfs Asteroids Research Results • Publications • 173 total • (103 in refereed journals) • 13 additional based on SDSS data • 28 Ph. D. Theses

9. Early Data Release(Stoughton et al. 2002) 1. 462 Sq. Deg. (5% of total survey) 2. Catalog of 14 million objects (stars, galaxies, quasars, ...) 3. 54,000 spectra Data are publicly available in online databases accesed via STScI

10. What is Cosmology? • Good old days • H0, q0 • Modern Times • H0 • ΩTotal= ΩΛ + ΩMatter+ Ων • σ8, n, w, b • Derived parameters:Γ SDSS will measure ΩBaryon+ ΩCDM SDSS will try to measure

11. Simulations of SDSS Performance ΩM, w Power spectrum (Γ, σ8)

12. The clustering of galaxies that we see today arose from quantum fluctuations laid down at the end of the inflationary epoch in the early universe. Distribution of Galaxies around Sun to z=0.1

13. Distribution of Quasars to z = 2

14. Galaxy Luminosity Function (Blanton et al. 2001)

15. Weak LensingMcKay, Sheldon, et al (2001, 2002) Foreground Galaxy Background galaxy (sheared)

16. Shear and mass Density vs. Radius for ensemble of 31,000 galaxies

17. Weak Lensing Calibration of M/L McKay + Blanton ==> Ω(matter) > 0.16

18. Galaxy Clustering Galaxy-Galaxy 2-point Correlation Function (Zehavi et al. 2002)

19. Power Spectrum 3 Dimensional Power Spectrum Derived from Angular Correlation Function (Dodelson et al. 2002)

20. Galaxy Clusters Cluster members have same “golden” color Abell 1689 Galaxy Cluster

21. z = 0.13 z = 0.06 z = 0.20 Likelihood= 1.9 Likelihood= -7.8 Likelihood= -8.4 N=0 N=19 N=0

22. The maxBcg Cluster Catalog • The 200 sq-degrees currently analyzed gives a catalog of 4000 clusters • Photometric redshift for each cluster good to 0.015 • Mass estimates from total galaxy light • Plot shows all clusters from a wedge 90o wide and 3o high, out to redshifts of 0.7

23. Scaling Mass with N Weak Lensing Number & Mass Functions σ (km/s) log σ = 0.70 log N + 1.75 log M ~ 2.1 log N

24. Parameters of Interest Black line is a fiducial model. Red, orange, green, blue vary the parameter of interest. Dotted lines are a different redshift. Ωm σ8 n fν Ωm= 0.27  .07  .1 σ8 = 1.04  .11  .1 fν = 0.30  .08  +0.1-0.2 (Work in Progress !!!)

25. z=6.28 Quasar (r', i', z')

26. Ly Alpha Trough Lyman Alpha Trough vs. Redshift

27. Optical Depth vs. Redshift

28. End of the Dark Ages

29. Debris in the Milky Way Halo(Yanny, Newberg, Ivesic, Grebel, ...)

32. Monoceros Structure Sagittarius South Stream New Structure? Sagittarius North stream F stars along Celestial Equator

33. Conclusions • SDSS is performing successfully • Producing leading edge science in a wide range of disciplines • 40% of reduced scope survey now done.

34. Cryogenic Dark Matter Search(CDMS)Progress and Status S. Kent for the CDMS collaboration FNAL Users Meeting June 10, 2002

35. CDMS Collaboration • Case Western Reserve University • D.S. Akerib, A. Bolozdynya, D. Driscoll,S. Kamat, T.A. Perera, R.W. Schnee, G.Wang • Fermi National Accelerator Laboratory • M.B. Crisler, R. Dixon, D. Holmgren • Lawrence Berkeley National Laboratory • R.J. McDonald, R.R. Ross, A. Smith • National Institute of Standards and Technology • J. Martinis • Princeton University • T. Shutt • Brown University • R.J. Gaitskell • University of Minnesota • P. Cushman • Santa Clara University • B.A. Young • Stanford University • L. Baudis, P.L. Brink, B. Cabrera, • C. Chang, T. Saab • University of California, Berkeley • M.S. Armel, V. Mandic, P. Meunier, W. Rau, B. Sadoulet • University of California, Santa Barbara • D.A. Bauer, R. Bunker, • D.O. Caldwell, C. Maloney, • H. Nelson, J. Sander, S. Yellin • University of Colorado at Denver • M. E. Huber

36. How it works ½ mwimpv2 ~ 25 kev Measure phonons and ionizations CDMS I: Stanford Tunnel

37. 1334 Photons (external source) 233 Electrons (tagged contamination) 616 Neutrons (external source) CDMS Background Discrimination • Measure simultaneously the phonons and the ionization created by the interactions. • High sensitivity • Discrimination • Ionization Yield (ionization energy per unit recoil energy) depends strongly on type of recoil • Most background sources (photons, electrons, alphas) produce electron recoils • Electron recoils near detector surface result in reduced ionization yield • WIMPs (and neutrons) produce nuclear recoils • Detectors provide near-perfect event-by-event discrimination against otherwise dominant bulk electron-recoil backgrounds, very good (>95%) againstsurface electron-recoil backgrounds

38. Shared-Electrode • 4.6 kg-days for WIMPs • 10 nuclear-recoil candidates > 10 keV • Inner-Electrode • 12.4 kg-days for WIMPs (≠ 10.7 better efficiencies) • 13 nuclear-recoil candidates > 10 keV • 4 multiples: They are not WIMPs but neutrons all single-scatters nuclear recoil candidates NR Band (-3s,+1.28s) 90% eff. NR Band (-3s,+1.28s) 90% efficient CDMS I Enlargement of Sample

39. Enlarged sample • Close to expected sensitivity • (we have that we were lucky • with the first sample • because of anomalously • high number of multiples) • Tests of various assumptions • • Our story is stable • Small statistics fluctuations • • Still strong disagreement • with DAMA • • Still best at low mass • • We temporarily • lost the “lead” • at high mass • <= CDMSII focus Results (to be send soon to PRD)

40. CDMS I->II • Go deep underground (Soudan Mine) • Athermal phonon technology • Even better rejection of background • Increase the mass -> 7kg • Approved in January 2000

41. CDMS II and other efforts

42. Soudan Installation • Takes much longer than we would like • Historically two obstacles: Institutional • Fridge commissioning problems • 1) Institutional • How to build enclosures in a university laboratory, without direct participation from within? • Bureaucratic nightmare ( Building code, DOE) • Difficulties subcontracting through University of Minnesota • Some interference with MINOS construction • Needed enclosures are essentially finished but nearly one year after our initial hope. However, our major accomplishment was learning to work around these difficulties. They did not have much impact on our schedule.

43. 2002 2003 2005 2004 2000 2001 New Scenario 2-4-7 T1 T1 SUF UCB/Case T2 T1-2 Soudan T3-4 T3 T1-4 T5-7 T5 T1-7 Begin Science Begin Soudan 2 Twrs 30% 4 Twrs 60% Full Science Running

44. Conclusions • CDMS I remains the most sensitive WIMP search at low mass • CDMS II well under way • Soudan tower 1 exceeds specifications. • Our measured background level* rejection shows that we should reach the sensitivity we claim. • Impressive validation of our ZIP concept and our fabrication/testing techniques • We are systematically addressing detector yield issues • All other systems are in line • Enclosures at Soudan are ready and we will move electronics in the Spring • We are aggressively addressing our “slow” temperature physics problem • First dark this summer! • The sensitivity gains in the first month should be spectacular • We should decisively enter the Supersymmetry domain

45. The Pierre Auger ProjectStephen Kent, for the Auger Collaboration A Study of The Highest Energy Cosmic Rays 1019 - 1021 eV Energy Spectrum - Direction - Composition Two Large Air Shower Detectors Mendoza Province, Argentina (under construction) Utah, USA FNAL Users Meeting June 10, 2002

46. Cosmic Ray Spectrum Flux (m2 sr s eV)-1 Energy (eV)

47. Possible Sources Supernova ~1015 eV Conventional – Bottoms-Up Hot spots in radio galaxy lobes? Accretion shocks in active galactic nuclei? Colliding galaxies? Associated with gamma ray bursts? Exotic – Top-Down Annihilation of topological defects? Wimpzillas – heavy dark matter Evaporation of mini black holes? New astrophysics? New physics? The highest energy cosmic rays should point back to possible sources (D < 50 Mpc)

48. EM shower Shower core hard muons Shower front A look at Air Showers Shower Max 1011 Particles at surface N Sea level Depth in the Atmosphere

49. Pierre Auger ObservatoryCombines strengths ofSurface Detector Arrayand Fluorescence Detectors Hybrid detector: Independent measurement techniques allow cross calibration and control of systematics More reliable energy and angle measurement Primary mass measured in complementary ways Uniform sky coverage

50. Auger Southern Site