Cosmology and Astrophysics (and Elementary Particle Physics in the 21 st Century) Cosmology and Astrophysics (and Elementary Particle Physics in the 21

Cosmology and AstrophysicsCosmology and Astrophysics(and Elementary Particle Physics(and Elementary Particle Physics

in the 21in the 21stst Century) Century)

Cosmology and AstrophysicsCosmology and Astrophysics(and Elementary Particle Physics(and Elementary Particle Physics

in the 21in the 21stst Century) Century)

Rocky Kolb

• A few generalities• Particle-Astro EPP• EPP Particle-Astro • The role of National Laboratories• Particle-Astro @ Fermilab (illustrates potential and issues)• The world outside of 60510• Structural questions

• What is (and what is not) Particle-Astro?• When does a suite of projects become a program?• How should projects be prioritized & managed?• What is the right slice of Particle Astro in the EPP Pie?

* My views are not endorsed by DOE, NASA, NSF, or Fermilab; but they should be.

My personal viewsMy personal views** My personal viewsMy personal views**

“When we try to pick out anything by itself, we findit hitched to everything else in the universe.”

– John Muir

A few generalitiesA few generalitiesA few generalitiesA few generalities

• Many EPP questions are also Cosmic Questions– Barish/Bagger Report– Physics of the Universe– Beyond Einstein– Quarks to the Cosmos– Quantum Universe

• Recognition at the funding agencies– interagency committees and task forces– jointly funded projects

• Legacy in nuclear astrophysics

• Particle-Astro now expensive enough to be respectable – many projects are too large for a university group or consortium.

Particle-Astro Particle-Astro EPP EPPParticle-Astro Particle-Astro EPP EPPSome historical examples:

• Limits on neutrino properties: Nm,

• Limits on axions from red giants and mass density• First signals of physics beyond standard model

– neutrino oscillations (atmospheric, solar)

– inflation (physics at mass scale ewk)– non-baryonic dark matter (physics at mass scale ewk?)– vacuum energy and acceleration (physics at all scales)

Possible Futures:• Cosmic rays beyond GKZ cutoff• Mass scale and properties of inflaton potential• Direct or indirect detection of dark matter• Properties of dark matter from clustering• Mass-energy density of the vacuum• Axion detection

Particle-Astro Particle-Astro EPP EPPParticle-Astro Particle-Astro EPP EPPNon Science:

Connectionto a closely aligned field of scienceto the public

People smaller cheaper faster projects (by EPP standards)

EPP EPP Particle-Astro Particle-AstroEPP EPP Particle-Astro Particle-AstroSome historical examples:

asymptotic freedom and T TQCD

grand unified theories and inflationproton decay and baryogenesisN and nucleosynthesisHiggs mass limits rule out EWK baryogenesis (?)Phase transitions and topological defectsNeutrino oscillations and leptogenesis

Possible Futures:SUSY and dark matterStrings and dark energyHiggs mass and baryogenesis/phase transitionsExtra dimensionsTheory of Everything should tell us something

EPP EPP Particle-Astro Particle-AstroEPP EPP Particle-Astro Particle-AstroNon Science:

Experiencein large data sets (also space science), e.g., SDSS

in industrial-scale projects, e.g., Pierre Auger Project

People many talented EPP experimentalists to Particle-Astro

$$$Particle-Astro growing part of shrinking budget pie

freeze out

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EPP EPP Particle-Astro Particle-AstroEPP EPP Particle-Astro Particle-Astro

Cold Thermal Relics

Cold thermal relics X A

X A

X X q q

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X

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X S

X q X q

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q q

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• SUSY LSP (neutralino)

• Direct detection (S)

More than a dozen experiments

• Indirect detection (A)

Annihilation in sun, Earth, galactic center, subclumps, . . .

neutrinos, positrons, antiprotons, rays, . . .

• Production at accelerators (P)


EPP EPP Particle-Astro Particle-AstroEPP EPP Particle-Astro Particle-Astro• The details of the relic abundance depend on the details of the SUSY model (spin, co-annihilation, LSP couplings, …)

• Low-energy SUSY has more than 100 parameters

• Analyses: MSSM, pMSSM, CMSSM, mSUGRA, …

• Why should dark side be simplerthan bright side (Lykken)?

• No guarantee that LHC alone willunravel details


Ellis et al., Phys.Lett. B565 176, (2003)

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mSUGRA

• neutrinos (hot dark matter)

• sterile neutrinos, gravitinos (warm dark matter)

• axions, axion clusters

• LKP (lightest Kaluza-Klein particle)

• supermassive wimpzillas

• solitons (Q-balls; B-balls; Odd-balls, Screw-balls….)

• LSP (neutralino, axino, …) (cold dark matter)

axions

axion clusters

6 40

8 25

10 eV (10 g)

10 M (10 g)

Mass range

Noninteracting: wimpzillas

Strongly interacting: B balls

Interaction strength range


The Role of National LaboratoriesThe Role of National LaboratoriesThe Role of National LaboratoriesThe Role of National Laboratories

• Same role played by NASA centers (Goddard, JPL, …)

• Complexity of Particle-Astro projects beyond universities or university consortia

• If National Laboratories did not exist, would they be invented for Particle-Astro projects?

Particle Astrophysics @ FermilabParticle Astrophysics @ FermilabParticle Astrophysics @ FermilabParticle Astrophysics @ Fermilab

• Particle Astrophysics and the Fermilab (EPP) mission

• Rules of engagement

• Fermilab Particle Astrophysics Projects– Theoretical Astrophysics– Sloan Digital Sky Survey– Pierre Auger Project– Cryogenic Dark Matter Search– Dark Energy Survey– SNAP/JDEM

• Particle Astrophysics Center



Fermilab Mission statement:Fermilab advances the understanding of the fundamental nature of matter and energy by providing leadership and resources for qualified researchers to conduct basic research at the frontiers for high energy physics and related fields.

Fermilab Long Range Plan (May 2004):Fermilab should substantially expand its leadership role in Particle Astrophysics, which provides probes of fundamental physics that complement accelerator experiments.

• Participate in projects requiring National Laboratory

• Participate in strength

• Participate with universities and other labs

• Participate where science overlaps with Fermilab mission

• Participate when techniques and talents of staff relevant

• Participate in the science


Rules of engagement

• Lederman and Schramm Kolb and Turner

• Presently 10-15 theoretical astrophysicists 4 FNAL staff (+1 in September) 4 postdocs 1 Schramm fellow students/users/visitors

• Partially (~1/4) funded by a NASA Astrophysics Theory grant

• Since inception, over 1000 papers

• Goals: science, support of Lab projects, world-wide impact

Theoretical Astrophysics Group (since 1983)


1. Alex Szalay, Professor Johns Hopkins University2. Neil Turok, Professor DAMTP, University of Cambridge3. Andreas Albrecht, Professor University of California, Davis4. Keith A. Olive, Professor University of Minnesota5. David Seckel, Associate Professor Bartol Research Institute6. Lars G. Jensen, Associate Professor North Dakota State7. Richard F. Holman, Professor Carnegie-Mellon University8. David P. Bennett, Associate Professor Notre Dame9. Marcelo Gleiser, Professor Dartmouth College10. Albert Stebbins, Scientist II Fermilab11. Edmund J. Copeland, Professor University of Sussex12. Angela V. Olinto, Associate Professor University of Chicago 13. Dongsu Ryu, Professor Chungnam University, Korea 14. Scott Dodelson, Scientist II Fermilab15. Ruth A. Gregory, Academic Staff University of Durham16. David Salopek, Senior Researcher UBC 17. Esteban Roulet, Visiting Professor Valencia, Spain18. Fay Dowker, Lecturer Queen Mary University of London

Theoretical Astrophysics Group (since 1983)

19. James Gelb, Assistant Professor UT, Arlington20. Robert Caldwell, Assistant Professor Dartmouth College21. Stephane Colombi, Scientist Institut d'Astrophysique, Paris22. Igor Tkachev, Researcher CERN23. Andrew Heckler, Assistant Dean, Ohio State University24. Yun Wang, Assistant Professor University of Oklahoma25. Istvan Szapudi, Assistant Professor University of Hawaii26. Antonio Riotto, Professor INFN, Padova27. Will Kinney, Assistant Professor SUNY Buffalo28. Lam Hui, Associate Professor, Columbia University29. Ewan Stewart, Assistant Professor Korea Advanced Inst.30. Zoltan Haiman, Assistant Professor Columbia University31. Pasquale Blasi, Faculty Osservatorio Astrofisico di Arcetri32. Idit Zehavi, Assistant Professor Case Western Reserve 33. Ravi Sheth, Assistant Professor University of Penn34. Patrick Greene, Assistant Professor UT, San Antonio35. John Beacom, Assistant Professor Ohio State University36. Nicole Bell, Assistant Professor, University of Melbourne


http://www.pha.jhu.edu/people/faculty/szalay.html

http://www.damtp.cam.ac.uk/user/ngt1000/

http://www.physics.ucdavis.edu/Cosmology/albrecht/

http://www.physics.umn.edu/directory/olive

http://www.bartol.udel.edu/%7Eseckel

http://www.bartol.udel.edu/%7Eseckel

http://info.phys.cmu.edu/people/faculty/holman/

http://www.dartmouth.edu/artsci/physics/faculty/gleiser.html

http://home.fnal.gov/%7Estebbins/

http://www.sussex.ac.uk/physics/profile578.html

http://astro.uchicago.edu/

http://canopus.chungnam.ac.kr/ryu/

http://canopus.chungnam.ac.kr/ryu/

http://monopole.ph.qmw.ac.uk/%7Edowker/home.html

http://www.dartmouth.edu/artsci/physics/faculty/Caldwell.html

• About 150 scientists

• ParticipantsUniversity of ChicagoFermi National Accelerator LaboratoryInstitute for Advanced StudyJapan Participation GroupJohns Hopkins UniversityKorean Scientist Group (KSG)Los Alamos National LaboratoryMax-Planck-Institute for Astronomy/HeidelbergMax-Planck-Institute for Astrophysics/GarchingNew Mexico State UniversityUniversity of PittsburghUniversity of Portsmouth, Princeton UniversityUnited States Naval ObservatoryUniversity of Washington

• Funding from Sloan Foundation, DOE, NSF, NASA, USNO, Monbusho, Universities, Max Planck

2.5m telescope

640 fiberspectrograph

120MPix camera

Sloan Digital Sky Survey – E885 (since 1991)


• Funding from Sloan Foundation, DOE, NSF, NASA, USNO, Monbusho, Universities, Max Planck


Issue:

Particle-Astro projects (like EPP) are international

Funding partnership of US government agencies, private, and international

Management, oversight issues

• Its 5-year mission: map steradians in 5 colors, find the redshift of 106 galaxies and 200,000 quasars

• Understand the role of dark matter in shaping structure

• Today: imaging 100%; spectro 70% • Metric of success: SDSS-II: Sloan and NSF ($5.4M)

– Legacy (extend SDSS-I)– SEGUE (galactic merging)– SN (low/intermediate redshift)

Sloan Digital Sky Survey – E885 (since 1991)


Pierre Auger Project – E881 (since 1995)

• About 250 scientists• Participants

• Funding from DOE & NSF US ~ 25% & 13 agencies abroad • URA manages

24 fluorescence detectors

1600 surface detectors

ArgentinaItalyAustraliaMexicoBoliviaPolandBrazil Slovenia Czech RepublicSpainFrance United Kingdom Germany USAGreeceVietnam

UCLAMichigan TechCase WesternMinnesotaChicagoNebraskaColoradoNew MexicoColorado StateNortheasternColumbiaOhio StateFermilab ArgonneUtahLouisiana State

Hybrid scheme


• Its mission: spectrum, source, and composition of highest energy cosmic rays

• Already world’s largest array - 30,000 km2 of pampas in Argentina

• Build, calibrate, take data, interpret

• 38 papers at ICRC

Stil

l bug

s

Pierre Auger Project – E881 (since 1995)



Issues:

Note size

Located offshore

US not majority support


• Funding from DOE & NSF US ~ 25% & 13 agencies abroad


• ParticipantsFermilabLBNLBrownMinnesotaStanfordUC Santa BarbaraCase Western ReserveColorado (Denver)Santa ClaraUC BerkeleyCaltechFlorida

• Funding from DOE & NSF Located in Soudan mine(co-located w/ MINOS)


Cryogenic Dark Matter Search – E891 (since 1996)

• Its mission: direct detection of dark matter

• Best limit in the world by a factor of 4

• Probing significant regions of MSSM model space

• Light-mass region largely ruled out

• Another factor of 3-4 at hand in Soudan

CombinedSoudan limits

DAMA NaI/1-4 3region

ZEPLIN I

EDELWEISS

Cryogenic Dark Matter Search – E891 (since 1996)



Issue:

What then?

Planning for next step in direct detection of dark matter?

• Another factor of 3-4 at hand in Soudan

Dark Energy Survey:• 5000 deg2 survey of the southern galactic cap

• constrain w to ~ 5%, begin to constrain dw/dz

• CTIO Blanco 4-m telescope• 2.2 deg. FOV camera $22.5M

• 2005-2009 Construction• 2009-2014 Operations

SNAP (JDEM):• Joint NASA/DOE dark energy space mission• Lot of action, little money• R&D lead by LBNL• Fermilab admitted to SNAP in 2004

On the horizon:• Auger North• SuperCDMS

New Initiatives



Issues:

How do we (FNAL) plan future initiatives?

Is our suite of projects optimal?

• Intellectual center to unify and focus the astrophysics program, enhance effectiveness and recruiting power

• Framework to germinate, develop, advance future efforts

• Internationally recognized center for Particle Astrophysics

• Interdivisional

• Membership open to all Fermilab employees working on existing astrophysics projects and new initiatives

• Assist Users community involved in Center programs

Goals


• Exciting Particle-Astro projects where Fermilab is not involvedICE3, LSST, Veritas, CMB, GLAST, …

• All have some of the issues of FNAL projects

• Some have unique issues

• One size does not fit all

The world outside of 60510The world outside of 60510The world outside of 60510The world outside of 60510

• The grey area

• “I know it when I see it.”

Define Particle AstroDefine Particle AstroDefine Particle AstroDefine Particle Astro

ParticleAstro

Particle-Astro

• There is no roadmapping procedure for Particle-Astro

• There are many great projects, does this make a program?

• Is it perceived as a coherent program or mishmash of projects?

Projects Projects Program ProgramProjects Projects Program Program

• Particle-Astro program is diverse (great strength, but…).

• There is no Particle-Astro PAC!

• Connecting Quarks with the Cosmos did not prioritize

• Will Eleven Science Questions for the New Century be revisited?

• How to set balance accelerator vs. other

Management and PrioritiesManagement and PrioritiesManagement and PrioritiesManagement and Priorities

The Particle-Astro SliceThe Particle-Astro SliceThe Particle-Astro SliceThe Particle-Astro Slice

• Remarkable time in Particle-Astro:Auger, Ice3, JDEM, LSST, CDMS, SDSS, Veritas, WMAP, Planck, GLAST, …, DON’T FORGET THEORY!

• EPP contribution has been substantial

• Money is the limitation for number of projects (true for EPP?)

• Particle-Astro could consume much larger fraction of EPP people and budget

– MOS (Auger North, SuperCDMS, LSST, JDEM, …)– Gravitational Wave Physics (LISA, LIGO, …)– Stronger presence in space science (Con-X, CMBPOL, …)– Next generation telescopes (TMT, GMT, …)

• How should proper balance be set?

astro & non-accelerator accelerator

The Particle-Astro SliceThe Particle-Astro SliceThe Particle-Astro SliceThe Particle-Astro Slice

• Balance should be set by science opportunities

• Balance must be set by budget opportunities

• Must be able to change dynamically

• Need realistic science-driven priorities (revisited periodically)

• ILC is the 1000-kg gorilla

Documents

Cosmology and Astrophysics (and Elementary Particle Physics in the 21 st Century) Cosmology and Astrophysics (and Elementary Particle Physics in the 21