f doe annual program review center for particle astrophysics scott dodelson

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DOE Annual Program Review

Center for Particle Astrophysics

Scott Dodelson

September 25, 2007 2

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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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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


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COUPP

• Competitive sensitivity for spin-dependent scattering, despite high backgrounds.

Spin-dependent Spin-independent


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Pierre Auger

Calibration unc. 18%FD syst. unc. 22%

5165 km2 sr yr ~ 0.8 full Auger year

Exp Obs>1019.6 132 +/- 9 51

> 1020 30 +/- 2.5 2

Suppression evident at high energy


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CDMS


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SDSS

Tegmark et al. 2006


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S. Allam, H. Lin, T. Diehl, D. Tucker et al.

Discovered via systematic searches of the SDSS data, with ongoing and proposed multi-wavelength follow-up from ground and space-based telescopes

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 RELEASE

Posted: November 8, 2006

SDSS


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GammeV

Shining Light through a Wall to search for axions and/or chameleons

First Results in Poster Session Tonight!


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Dark Energy Survey

Study Dark Energy using 4 complementary techniques:

I. Cluster Counts II. Weak Lensing III. Baryon Acoustic Oscillations IV. Supernovae Two multiband surveys: 5000 deg2 g, r, i, z 9 deg2 repeat (SNe) Build new 3 deg2 camera and

Data Management system 5 year Survey (525 nights)

Blanco 4-meter at CTIO


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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

DECam Focal Plane

62 2kx4k Image CCDs: 520 MPix8 2kx2k focus, alignment CCDs4 2kx2k guide CCDs

Optical Lenses

CCD Readout Filters Shutter


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SNAP

Science: Weak lensing & SN1A Calibration

Photometric & Astrometric “Slice” Electronics

Manage data prior to transmission CCD and Front-end Electronics

packaging and TestingSiDet is a Production Facility

Software/Simulations/Data ManagementExperience with Large HEP & SDSS

Datasets

Have started internal discussions on FNAL role in SNAP

“On-Track” Plan


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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

SNAP

Leadership Plan


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Budget

Includes indirect and scientists but not (DES) project costsExperimental RA salaries in CPA starting in June 07.


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Organization

Scott Dodelson, Acting Director(Ellie Arroyo), Budget Officer

Scott Dodelson, Acting Director(Ellie Arroyo), Budget Officer

Research AssociatesAaron Chou, Auger

Jeter Hall, CDMSJeff Kubo, SDSS

Gajus Miknaitis, SDSSJason Steffen, Brinson Fellow

Jong-Hee Yoo, CDMS

Research AssociatesAaron Chou, Auger

Jeter Hall, CDMSJeff Kubo, SDSS

Gajus Miknaitis, SDSSJason Steffen, Brinson Fellow

Jong-Hee Yoo, CDMS

Long Term Guests & VisitorsSahar Allam, SDSS

Pasquale Blasi, Auger/TheoryDarren Depoy, DES

Suzanne Deustua, SNAP

Long Term Guests & VisitorsSahar Allam, SDSS

Pasquale Blasi, Auger/TheoryDarren Depoy, DES

Suzanne Deustua, SNAP


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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

Intellectual Environment

New in 2007}


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FuturesMonthly meetings to chart future

Bauer, Diehl, Dodelson, Frieman, Flaugher, Kent, Mantsch, Peoples, Sonnenschein

FellowsSeparated out FCPA Experimental RA’s

Annis, Bauer, Diehl, Flaugher, Mantsch, Merritt, Newman-Holmes, Sonnenschein

SpaceDoubling Time: ~7 years

Bauer, Diehl, Glass, Merritt,Sonnenschein, Stebbins, Stoughton

VisitorsLong- and Short- Term

Annis, Glass, Sonnenschein, Stebbins

Ad-Hoc Reviews/Task ForcesComputing, GammeV, 8 O’clock Arc Follow-up, SNAP Plan, AGIS

participation

Amundson, Annis, Bauer, Carcagno, Diehl, Dodelson, Frieman, Flaugher, Gnedin, Holmgren, Hooper, Lin, Liu, Kowalkowski, Kronfeld, Marriner, McGinnis, Newman-Holmes, Nguyen, Peoples, Petravick, Wilson

Web Page Kubo, Glass, Jackson, Steffen

Preparing for the Future


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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


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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


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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)


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1. Hire Gnedin (7/05)

2. Bring idea to Futures Committee (12/06)

3. Present idea to Directorate (1/07)

4. Apply for FRA grant; open discussion with KICP (2/07)

5. Include Computing Division, LQCD, Kravtsov on Task Force (4/07)

6. Place Requisitions w/ money from FRA, KICP, Theory (7/07)

7. Submit Task Force Report (8/07)

8. Begin Discussions with representatives from other Labs (8/07)

Need Scientific Talent

Look for funding

Leverage FNAL’s resources

Full support; refinement

Cosmological Computing


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Wed., Nov. 7:------------

9:00-9:45 Goals of the Retreat 9:45-10:15 Coffee break10:15-11:15 UHECR: Beyond Auger

South11:15-11:45 Gravity waves: beyond

LIGO11:45-12:15 Discussion12:15-1:30 Lunch1:30-2:30 Computational Astrophysics2:30-3:30 21 cm observations3:30-4:00 Break4:00-5:00 CMB5:00-6:00 Direct dark matter detection

Retreat

Thurs., Nov. 8--------------

9:00-10:00 Optical cosmology10:00-10:30 Near-infrared observations10:30-11:00 Break11:00-12:00 Indirect Dark matter detection 12:00-12:30 Discussion12:30-2:00 Lunch2:00-2:30 Underground laboratory/experiments 2:30-3:00 Discussion3:00-4:00 Recap/lessons/next steps

George Williams College, Geneva, WI


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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

Conclusions


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Backup Slides


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FY07 FY08 Phase C/D

M&S FTE

M&S FTE

M&S/year FTE/year

Electronics $40k 3.5 $200k 3.5 $1000k 10

Calibration 0 0.25

1.5 0 2

Software, Simulations, Data Management 0 0.5 $150k 3 $500k 6

CCD’s $92k 0 $125k 2 $400k 6

Front-End Electronics 0 0 $25k 1 $300k 3

Science 0 0 0 0 0 2

Total One Year Costs $132k 5 $500k 11 $2.2M 29

Total (x5 for full C/D costs) $11M 145


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Cosmological ComputingCosmological Computing

As of today, CD maintains an 8 core cluster for cosmology Other groups have many more resources:o Virgo Consortium: 670 CPU SparcIII, 816 CPU Power4o ITC, Harvard: 316 CPU Opteron, 264 CPU Athlono LANL: 294 CPU Pentium4 (just for cosmology)o CITA: 270 CPU Xeon clustero SLAC: 72 CPU SGI Altrix, 128 CPU Xeon clustero Princeton: 188 CPU Xeon clustero 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


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Can we do better?

Preparing for the Future


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The Dark Energy Survey

• Study Dark Energy using 4 complementary* techniques: I. Cluster Counts II. Weak Lensing III. Baryon Acoustic Oscillations IV. Supernovae

• Two multiband surveys: 5000 deg2 g, 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

Blanco 4-meter at CTIO

*in (systematics, cosmological parameter degeneracies,Geometry vs. Structure growth)

fDES Forecasts: Power of Multiple Techniques

Ma, Weller, Huterer, etal

Figure of Merit: inverse area of ellipse

• 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


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DES Collaboration• 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

Red = joined in the past 6 months


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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


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DECam replaces the Prime Focus Cage of the Blanco

3556 mm

1575 mm

Hexapod

Optical Lenses

F8 Mirror

CCDRead out

Filters Shutter


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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


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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


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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.


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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


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The DES Organizationa collaboration perspective


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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

DECam Focal Plane

62 2kx4k Image CCDs: 520 MPix8 2kx2k focus, alignment CCDs4 2kx2k guide CCDs

Optical Lenses

CCD Readout Filters Shutter


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fCOUPP 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


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Discrimination strategies• Most particle physics experience in MeV range

• Direct detection requires keV scale Phonons

10 meV/ph

Ionization~ 10 eV/e

Scintillation~ 1 keV/γ

CRESST CDMSEDELWEISS

ZEPLINXENON

WArP, ArDM

Sub-K low threshold

large mass >$$

Scintillation high threshold

Noble liquids high threshold but

large mass <$$

Initially need both

DAMAZEPLIN I

DEAPCLEAN


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Compare CDMS with noble liquids In the end,

the tails of the background distributions determine the sensitivity

gammas

n-recoils

XENON PrototypeBest CDMS Ge ZIP

countingstatistics

Best resolution from SCDMS experiment allows better discovery potential

99% discrimination to below ~10 keV

overlap starts at ~50 keV

for more detail see

http://www.physics.ucla.edu/hep/dm06/talks/shutt.pdf


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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.


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FNAL has made a splash in CDMS w/ relatively small investment. RA’s have made a big difference.


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CDMS II Continuing to Run at Soudan

Current sensitivity of CDMS

Xenon10 limitPublished CDMS lim

it

DAMA MSSM

CDMS is the only direct detection dark matter experiment currently running without backgrounds!

814 kg-day exposure

Large calibration data sets

High efficiency for collecting data


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CDMS Collaboration at SoudanDOE LaboratoryFermilabLBNL

DOE UniversityBrownCalTechFloridaMinnesotaMITStanfordUC Santa Barbara

NSFCase Western ReserveColorado (Denver)Santa ClaraUC Berkeley

CanadaQueens


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Fermilab responsibilities in CDMS II

Established roles in CDMSProject Management

Project Manager, Financial support peopleOperations

Lead the Soudan operations on both physicist and technical sidesCryogenics

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 roomsAnalysis

Independent analysis chain (based on ROOT, time-domain pulse fitting)


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New Fermilab responsibilities in SuperCDMS

New roles for SuperCDMSBackgrounds

Collaborating with COUPP on understanding Radon, alpha screeningMay get involved in beta screening with new clean TPC

Shield/Veto

Do mechanical design and construction together with cryogenicsDetectors

Exploring possibilities for automated inspection and repair at SiDetMay also get involved in bonding our sensors to larger crystals

Systems Test

Put everything together at Fermilab and test before taking to SNOLAB

Need more scientist and engineering help to push forward these new areas


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CDMS budget summaryCDMS II Project budget = $18.5M (6 years)Total budget including base funding = $29.5MMost of the operations funding comes from Fermilab

FY2007 ~$0.5M M&S, $1.3M Labor

SuperCDMSProject budget = $16.2M (6 years)Total budget including base funding = $47.3MFNAL operations budget request increased

FY2008 ~$1.1M M&S, $2M Labor


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Progress on SuperCDMS Design

• Pulse tube cryocooler under test in clean room in Lab 3 at Fermilab– Important to

understand vibrations since these are an integral part of the cryogen-free dilution refrigerators we plan to use for SuperCDMS

• New warm electronics prototype for SuperCDMS– Replaces a chain of four

9U-sized boards used for CDMS II

– Fewer connections, lower power draw => more robust


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SuperCDMS Cryogenics Design• Cryogen-free dilution refrigerator

– Much lower operations and maintenance cost

• Larger volume to accommodate more detectors– More robust thermal connections than in CDMS II


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Scientific reach of CDMS at Soudan

CDMS II - Current

CDMS II - Current

CDMS II -projected

CDMS II -projected

EdelweissEdelweissZEPLIN-1

ZEPLIN-1DAMA

SUSY Models

new XENON10 preprint

new XENON10 preprint


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Schedule and Budget summary


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• Variety of techniques search for WIMP dark matter - interesting sensitivity

• Several have the potential to reach 10-44 cm2 soon and 10-

46 cm2 in future

Status of Direction Detection Search

1 ev/kg/month

1 ev/kg/year

1 ev/ton/year

DAMA

KIMS

CRESST

EDELWEISS

ZEPLIN II

WARP

CDMS Soudan 2004+2005

XENON10 APS2007

CDMS Soudan Proj

SuperCDMS SNOLab ProjLUX 300kg Proj1 ev/10 kg/year

f doe annual program review center for particle astrophysics scott dodelson

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