I. Description/Status of survey

II. Science projects with SDSSGalaxies and Large Scale

StructureQuasarsMilky Way Structures

SLOAN DIGITALSKY SURVEY (E885)

Stephen Kent (CD/EAG)

FNAL Users MeetingJune 10, 2002

Partner InstitutionsFermi National Accelerator LaboratoryPrinceton UniversityUniversity of ChicagoInstitute for Advanced StudyJapanese Promotion GroupUS Naval ObservatoryUniversity of WashingtonJohns Hopkins UniversityMax Planck Institute for Astronomy, HeidelbergMax Planck Institute, GarchingNew Mexico State University(new) Los Alamos National Laboratory(new) University of Pittsburgh

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

Sloan Digital Sky SurveyGoals:

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 universeb) 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).

Detectors/Equipment

2.5 m Telescope

Mosaic Imaging Camera

640 Fiber Spectrograph “Photometric” telescope

2. Identify Galaxies, Quasars

3. Design Plugplates 4. Obtain Spectra

Survey Operations

1. Image Sky

Sloan Digital Sky Survey(CD/EAG, PPD/TAG)

Current Status (Jun. 2002)

Percent Complete

44% as of Apr 15, 2002

29% as of Apr 15, 2002

63% as of Apr 15, 2002

IMAGING

SPECTROSCOPY

MT (calibrations)

Baseline

8452 sq. deg.

1688 tiles

1563 patches

Operations began: Apr 1, 2000

Operations end: Jun 30, 2005

Sloan Digital Sky Survey(CD/EAG, PPD/TAG)

Current Status (Jun. 2002)

Percent Complete

44% as of Apr 15, 2002

29% as of Apr 15, 2002

63% as of Apr 15, 2002

IMAGING

SPECTROSCOPY

MT (calibrations)

Baseline

8452 sq. deg.

1688 tiles

1563 patches

Operations began: Apr 1, 2000

Operations end: Jun 30, 2005

Research Results

● Publications● 173 total

● (103 in refereed journals)

● 13 additional based on SDSS data

● 28 Ph. D. Theses

● Topics● Hi Z Quasars

● Gravitational Lensing

● QSO & Galaxy Corr. Function

● Galaxy Clusters

● Galaxy Struct./Evol.

● Milky Way Halo

● Brown Dwarfs

● Asteroids

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

What is Cosmology?

● Good old days

– H0, q

0

● Modern Times

– H0

– ΩTotal

= ΩΛ + Ω

Matter+ Ω

ν

– σ8, n, w, b

– Derived parameters: Γ

ΩBaryon

+ ΩCDM

SDSS will measure

SDSS will try tomeasure

Simulations of SDSS Performance

Power spectrum (Γ, σ8)Ω

M, w

Distribution of Galaxies around Sun to z=0.1

The clustering ofgalaxies that wesee today arosefrom quantumfluctuations laiddown at the end ofthe inflationaryepoch in the earlyuniverse.

Distribution of Quasars to z = 2

GalaxyLuminosityFunction(Blanton et al. 2001)

Weak LensingMcKay, Sheldon, et al (2001, 2002)

Foreground Galaxy

Background galaxy (sheared)

Shear andmass Densityvs. Radius forensemble of31,000 galaxies

Weak Lensing Calibration of M/L

McKay + Blanton ==> Ω(matter) > 0.16

Galaxy-Galaxy2-pointCorrelationFunction(Zehavi et al.2002)

Galaxy Clustering

3 Dimensional Power Spectrum Derived fromAngular Correlation Function (Dodelson et al. 2002)

Power Spectrum

Abell 1689 Galaxy Cluster

Cluster members have same “golden” color

Galaxy Clusters

z = 0.06

z = 0.13

z = 0.20

Likelihood= -7.8

N=0 N=19 N=0

Likelihood= 1.9 Likelihood= -8.4

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

Scaling Mass with N

σ (km/s)

log σ = 0.70 log N + 1.75

Weak Lensing

log M ~ 2.1 log N

Number & Mass Functions

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

fν n

Ωm= 0.27 .07 .1 σ8 = 1.04 .11 .1 fν = 0.30 .08 +0.1-0.2

(Work in Progress !!!)

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

Lyman AlphaTrough vs.Redshift

Ly AlphaTrough

Optical Depth vs. Redshift

End of theDark Ages

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

SagittariusNorth stream

SagittariusSouth Stream

NewStructure?

MonocerosStructure

F stars alongCelestialEquator

Conclusions

● SDSS is performing successfully● Producing leading edge science in a wide range

of disciplines● 40% of reduced scope survey now done.

Cryogenic Dark Matter Search(CDMS)Progress and Status

• S. Kent for the

• CDMS collaboration

FNAL Users MeetingJune 10, 2002

CDMS CollaborationSanta Clara UniversityB.A. Young

Stanford UniversityL. Baudis, P.L. Brink, B. Cabrera, C. Chang, T. Saab

University of California, BerkeleyM.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 DenverM. E. Huber

Case Western Reserve UniversityD.S. Akerib, A. Bolozdynya, D. Driscoll,S. Kamat, T.A. Perera, R.W. Schnee, G.Wang

Fermi National Accelerator LaboratoryM.B. Crisler, R. Dixon, D. Holmgren

Lawrence Berkeley National LaboratoryR.J. McDonald, R.R. Ross, A. Smith

National Institute of Standards and Technology

J. Martinis

Princeton UniversityT. Shutt

Brown UniversityR.J. Gaitskell

University of MinnesotaP. Cushman

How it works½ mwimpv2 ~ 25 kev

Measure phonons and ionizations

CDMS I: Stanford Tunnel

CDMS Background Discrimination

• Detectors provide near-perfect event-by-event discrimination against otherwise dominant bulk electron-recoil backgrounds, very good (>95%) against surface electron-recoil backgrounds

• 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

616 Neutrons (external source)

1334 Photons (external source)

233 Electrons (tagged contamination)

CDMS I Enlargement of Sample– Inner-Electrode– 12.4 kg-days for WIMPs (≠ 10.7 better efficiencies)

13 nuclear-recoil candidates > 10 keV4 multiples: They are not WIMPs but neutrons

NR Band (-3,+1.28) 90% efficient

all single-scattersnuclear recoil candidates

– Shared-Electrode– 4.6 kg-days for WIMPs – 10 nuclear-recoil candidates > 10 keV

NR Band (-3,+1.28) 90% eff.

Results (to be send soon to PRD)

● 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

● Enlarged sample– Close to expected sensitivity– (we have that we were lucky– with the first sample– because of anomalously– high number of multiples)

CDMS I->II● Go deep underground (Soudan Mine)● Athermal phonon technology

– Even better rejection of background● Increase the mass -> 7kg● Approved in January 2000

CDMS II and other efforts

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.

●

New Scenario 2-4-7

UCB/Case T2

T1-4

Full Science Running

T1-7

T1-2 Soudan

4 Twrs 60%BeginScience

T1 SUF

BeginSoudan2 Twrs 30%

T3-4

T5-7

2000 2001 2002 2003 2004 2005

T3

T5

T1

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

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, USAFNAL Users Meeting

June 10, 2002

Cosmic Ray Spectrum

Energy (eV)

Flu

x (

m2 s

r s e

V)-

1

Possible Sources• 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)

Supernova~1015 eV

A look at Air Showers

Shower Max

Depth in the Atmosphere

N

Sea level

1011 Particles at surface

Shower frontShower corehard muons

EM shower

Pierre Auger Observatory

Combines strengths of

Surface 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

Auger Southern

Site

Auger Surface Array

1600 Detector Stations1.5 Km spacing7000 km2 str~40 events/yr > 1020 eV

The Auger Surface Detector

Three 8” PM Tubes

Plastic tank

White light diffusing liner

12 m2 of de-ionized water

Solar panel and electronic box

Commantenna

GPSantenna

Battery box

Auger Fluorescence Detector

33 telescope units3.4 meter dia. Mirrors440 PMTs per camera

Construction Plan

• Years 2000 & 2001 (Engineering Array)• Install ~40 surface detector station array.• Install two fluorescence telescopes.• Install communications and data acquisition.• Complete Auger Campus.

• Year 2002 - 2004• Full production and deployment• Transition to data taking

•

Auger Center Building

Event Display of a hybrid event Surface Array

Summary

• We have some exciting science.• Strong collaboration organized.• We have completed the Engineering Array.• We have passed our major review.• Construction of the full Auger southern site is

underway. Deployment well underway by end of 2002