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