# Presentation: 470568

## I. Description/Status of survey

II. Science projects with SDSS
	Galaxies and Large Scale
		Structure
	Quasars
	Milky Way Structures

- 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

## Partner Institutions

**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**

## 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 Survey

- Goals:
- 	1. Image 1⁄4 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).

## Detectors/Equipment

- 2.5 m Telescope

- Mosaic Imaging Camera

- 640 Fiber Spectrograph

- “Photometric” telescope

## Survey Operations

- 2. Identify Galaxies,
-     Quasars

- 3. Design Plugplates

- 4. Obtain Spectra

- 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**
**H****0****,  q****0**
**Modern Times**
**H****0**
**Ω****Total**** ****= Ω****Λ**** + Ω****Matter****+ ****Ω****ν**** **
**σ****8****,  ****n****,  w, b**
***Derived parameters:***** ****Γ**

**Ω****Baryon****+ Ω****CDM**

**SDSS will measure**

**SDSS will try to**
**measure**

## Simulations of SDSS Performance

- Power spectrum (Γ, σ8)

- ΩM, w

## Distribution of Galaxies around Sun to z=0.1

- 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 Quasars to z = 2

## Galaxy

- Luminosity
- Function
- (Blanton et al.
-  2001)

## Weak LensingMcKay, Sheldon, et al (2001, 2002)

- Foreground Galaxy

- Background galaxy (sheared)

## Shear and

- mass Density
- vs. Radius for
- ensemble of
- 31,000 galaxies

## Weak Lensing Calibration of M/L

- McKay + Blanton ==> Ω(matter) > 0.16

## Galaxy Clustering

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

## Power Spectrum

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

## Galaxy Clusters

- Abell 1689 Galaxy Cluster

- Cluster members have same “golden” color

## z = 0.06

**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 Alpha

- Trough vs.
- Redshift

**Ly Alpha**
**Trough**

## Optical Depth vs. Redshift

## End of the

- Dark Ages

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

## Slide 30

## Slide 31

## Sagittarius

- North stream

- South Stream

- New
- Structure?

- Monoceros
- Structure

- F stars along
- Celestial
- Equator

## 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 Meeting
- June 10, 2002

## CDMS Collaboration

- _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_ _

- _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

## How it works

- 1⁄2 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**

## CDMS I Enlargement of Sample

## Results (to be send soon to PRD)

## 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%

**Begin**
**Science**

- T1    SUF

**Begin**
**Soudan**
- 2 Twrs 30%

- T3-4

- T5-7

- 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 ProjectStephen 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

## Cosmic Ray Spectrum

**Energy (eV)**

**Flux (m****2 ****sr s eV)****-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**
**~10****15**** eV**

## A look at Air Showers

**Shower Max**

**Depth in the Atmosphere**

**N**

**Sea level**

**10****11**** Particles**
** ****at surface**

##        Pierre Auger ObservatoryCombines strengths ofSurface Detector Arrayand 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 Stations***
***1.5 Km spacing***
***7000 km******2****** str***
***~40 events/yr***
***         ******> 10******20****** eV***

## The Auger Surface Detector

**Three  8” ****PM Tubes**

**Plastic tank**

**White light diffusing liner**

**12 m****2**** of ****de-ionized water**

**Solar panel and electronic box**

**Comm****antenna**

**GPS****antenna**

**Battery**** box**

## Auger Fluorescence Detector33 telescope units3.4 meter  dia. Mirrors440 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