High Energy Physics

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High Energy Physics DOE Office of Science
AMS Technical Interchange Meeting NASA Kennedy
Space CenterJanuary 14, 2004 Dr. Robin
Staffin, Director Office of High Energy
Physics Office of Science Department of Energy
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What is the universe made of?

• Centuries of experimentation and theoretical
  synthesis have culminated in what we call the
  Standard Model
• A quantum field theory describing the
  interaction of point-like fermions (quarks and
  leptons)
• which interact by the exchange of vector bosons
  (photons, W and Z, gluons)
• Provides an understanding of what nucleons,
  atoms, stars, you and me are made of
• But we know it is incomplete
• Theoretically not well behaved above 1TeV. No
  gravity.
• Experimentally there seems to be a lot of stuff
  in the universe which is not made of quarks or
  gluons

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Meanwhile, back in the universe...
We do not know what 96 of the universe is made
of!
3.5
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A Critical Time

• In the course of the next decade, we may discover
  a very different universe (maybe we already have)
• HEP program addresses the following questions
• What is the path to unification (Einsteins
  Dream)?
• What is the origin of mass (Higgs particle)?
• Are there hidden dimensions of space-time?
  (gravity QM)
• What can neutrinos tell us?
• Why all matter and no (apparent) antimatter?
• What is Dark Matter?
• What is Dark Energy?

The field is poised on the threshold of discovery
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Why Accelerators?

• We live in a cold and empty universe only the
  stable relics and leftovers of the big bang
  remain. The unstable particles have decayed
  away with time, and the symmetries have been
  broken as the universe has cooled.
• But every kind of particle that ever existed is
  still there, in the equations that describe the
  particles and forces of the universe. The vacuum
  knows about all of them.
• We can use accelerators to make the equations
  come alive, by pumping sufficient energy into the
  vacuum to create the particles and uncover the
  symmetries that existed in the earliest universe.
• We are exploring 1ps after the big bang.

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Detectors

• Surround the collision points with arrays of
  instrumentation to intercept the particles
  produced
• large (thousands of tons)
• complex (many subsystems, 106 107 channels)
• designed and built by collaborations of
  university and laboratory physicists

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Big collaborations

• Example
• The DØ detector was built and is operated by an
  international collaboration of 670 physicists
  from 80 universities and laboratories in 19
  nations
• university groups predominate 120 graduate
  studentsgt 50 collaborators non-US

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What do HEP physicists actually do?

• Design and build hardware
• Detectors, electronics
• Write software
• Operate the detector
• Interpret data
• Present, refine, discuss our results among
  ourselves
• Publish papers

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Computer programs reconstruct the particle
trajectories and energies in each collision (each
event)
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How we would make a discovery

• Simulations based on the standard model provide a
  good description of standard processes in our
  data
• Models of beyond-the-standard-model particles and
  forces tell us where to look for deviations

???
Example supersymmetry predicts more events with
high-energy jets and unbalanced momentum
Will we see more like this?
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How we work

• Research is conducted at over 100 universities
  and 5 national laboratories ( non-US
  laboratories)
• New proposals from particle physics community
  submitted either through national laboratories or
  directly to DOE-OHEP
• Proposals peer-reviewed by
• Laboratory Program Advisory Committees and/or
  SAGENAP (Scientific Assessment Group for
  Experiments in Non-Accelerator Physics) and/or
  mail review or special panels
• for their significance to
• Scientific relevance does it answer our major
  questions?
• Technological relevance does it
• Capitalize on existing particle physics
  capabilities and result in significant scientific
  gain?
• or
• Enhance capabilities that the particle physics
  community will need?
• DOE/NSF High Energy Physics Advisory Panel and
  its subpanels make recommendations to funding
  agency.
• By Congressional legislation, DOE has joined the
  NASA/NSF Astronomy and Astrophysics Advisory
  Committee (AAAC).

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Elements of Program

• Accelerator based physics our primary tools
• Construction and operation of accelerators and
  detectors and research activities in these
  facilities
• Proton based accelerator Tevatron, LHC, NuMI,
  MiniBooNE
• Electron based accelerator B-FactoriesBaBar and
  Belle
• Non-accelerator physics
• Atmospheric solar neutrinos Super-K, KamLAND
• Particle astrophysics cosmology AMS, LAT
  (GLAST), Auger, VERITAS, SDSS, CDMS-II, CMB
• Theory
• Elementary particle theory
• Major computing efforts simulation, data
  storage, distribution, analysis. E.g. QCD
  Computer
• Technology RD
• RD for accelerator and detector technologies

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FY 2004 Funding Allocation

• Accelerator based physics (proton electron)
  75
• Non-Accelerator physics 7
• Theory 7
• Technology RD 12

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Major Program Thrusts
Unification/Higgs
Unification/Higgs
n Mass, n Mixing
Matter/Antimatter
Unif./Higgs
Dark Matter
Dark Matter
Dark Energy
n Mass/Unification
Blue In operation Orange Approved
Purple Proposed
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High Energy Physics Program

• Goals Ultimate Unification Extra Dimensions
• Operating
• CDF and DZero Fermilab Tevatron (protons) Top
  quark, Higgs, SUSY, extra dimensions
• MiniBooNE Fermilab Main Injector Neutrino
  mixing
• (protons)
• BaBar SLAC B-factory (electrons)
  Matter-antimatter, b quark, CP violation
• Super-K Japan (non-accelerator) Proton decay,
  neutrino mixing
• K2K Japan (accelerator neutrinos) Neutrino
  mixing
• KamLAND Japan (reactor neutrinos) Neutrino
  mixing
• Approved
• ATLAS CMS CERN LHC (protons) Higgs, SUSY,
  extra dimensions
• NUMI/MINOS Fermilab MI (protons) Neutrino
  mixing (long baseline)
• Proposed
• BTeV Fermilab Tevatron Matter-antimatter, b
  quark, CP violation
• Linear Collider International (electrons)
  Higgs, SUSY, extra dimensions

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High Energy Physics Program

• Goal Cosmic Connections
• Operating
• Sloan Digital Sky Survey (w/NASA, NSF, foreign)
  3D sky map, dark energy
• Supernova Cosmology Project, Nearby Supernova
  Factory
• (w/NSF NASA) dark energy
• CMB cosmology
• Approved
• AMS Alpha Magnetic Spectrometer ISS (w/NASA,
  foreign) cosmic antimatter
• Cold Dark Matter Search (CDMS-II) (underground,
  w/NSF) dark matter in cosmic rays
• Large Area Telescope (LAT) GLAST, 2007
  (w/NASA, foreign) gamma rays, dark matter
• Pierre Auger ground array in Argentina (w/NSF,
  foreign) high energy cosmic rays
• VERITAS telescope in Arizona (w/NSF, SAO) high
  energy gamma rays
• Proposed
• SuperNova/Acceleration Probe (SNAP JDEM
  concept) dark energy
• Large-aperture Synoptic Survey Telescope
  (LSST) dark energy
• Enriched Xenon Observatory (EXO)
  neutrino mass
• AXION dark
  matter search

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Sloan Digital Sky Survey (SDSS)

• Scientific purpose fundamental cosmology,
  formation evolution of galaxies and large scale
  structure, dark matter distribution
• uses 2.5m telescope with CCD camera and
  spectrograph
• digitally maps ¼ of the sky and obtains
  spectra for 1 million galaxies and 100,000
  quasars
• Partnership Joint Project, funded by Sloan
  Foundation, DOE, NASA, NSF, and Foreign Agencies.

2.5 m telescope in New Mexico
2.5 m Telescope

• Status
• Data-taking is complete.
• Discovered how galaxies cluster in space, leading
  to new information about evolution of galaxies
  and matter in the universe.

Mosaic Imaging CCD Camera
Mosaic imaging CCD camera
640 Fiber Spectrograph
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Very Energetic Radiation Imaging Telescope Array
System - VERITAS

• Study of celestial sources of very high energy
  gamma-rays in the energy range of 100GeV-10TeV
• Using atmoshperic Cherenkov telescope located at
  Kitt Peak in southern Arizona
• Collaboration between US and UK
• DOE, NSF, Harvard-Smithsonian
• Under construction for completion September 2006.

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The Pierre Auger (Auger)

• Schedule under construction
• 300 surface detectors (out of the 1600 for the
  total array) installed
• 6 fluorescence stations completed

• Scientific purpose Study origin and nature of
  highest energy particles in nature (gt 1018 eV)
• prove existence of extraordinarily energetic
  cosmic rays
• study flux, arrival directions and other
  properties
• Partnership Joint Project, funded by DOE, NSF,
  and Foreign Agencies (total 18 participating
  countries largely from Europe and South America)
  under FNALs management.

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CDMS II

• Scientific purpose Cold Dark Matter Search
• Search for Weakly Interacting Massive Particle by
  tagging true nuclear recoil
• Partnership Joint Project, funded by DOE and NSF
  (total 12 participating institutions).
• Construction completed in 2004, taking data.

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The Gamma-ray Large Area Space Telescope (GLAST)

• Scientific Purpose - measures the energy and
  direction of celestial gamma-rays with good
  resolution over wide field of view to
• study mechanism of particle acceleration in
  astrophysical sources
• determine high energy behavior of gamma ray
  bursts and transient sources
• search for dark matter candidates

• Large Area Telescope (LAT)
• Primary instrument on the NASA GLAST Mission
  managed by SLAC
• Partnership between DOE and NASA plus
  contributions from France, Italy, Japan, Sweden
• Fabrication cost 137M DOE share is 42M
• Schedule
• Fabrication complete in October 2006
• GLAST launch May 2007

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Dark Energy Next Generation Experiment

• Dark Energy - causing the acceleration of the
  expansion of the universe
• - of central importance to HEP program

• High Energy Physics Advisory Panel endorsed the
  proposed SNAP RD and science
• DOE is having discussions on a Joint Dark Energy
  Mission (JDEM) with NASA
• DOE is funding RD for the SuperNova Acceleration
  Probe (SNAP) a leading contender for a dark
  energy mission
• SNAP will use supernova weak lensing
  measurements to precisely measure the nature of
  dark energy over a large redshift range

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AMS - Alpha Magnetic Spectrometer

• Schedule
• gt95 detector fabrication completed
• Expected launch March 2008

• Scientific purpose Search for anti-nuclei
  (anti-Helium) as a component of cosmic radiation
• High quality magnetic spectrometer in space to
  measure cosmic rays outside atmosphere
• Will operate on the International Space Station
• Partnership Joint Project, funded by DOE, NASA,
  and Foreign Agencies (total 16 participating
  countries largely from Europe and Asia)
• Detector fabrication cost gt 240M
• DOE share is 5M

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Describing the universe
Consistentunderstanding?
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Example 1
10-18 m
1026 m
Consistentunderstanding?
Dark Matter
Supersymmetry in accelerators? WIMPs in
underground detectors?
?
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Example 2
10-18 m
1026 m
Consistentunderstanding?
Higgs Field
Dark Energy
NO! gt 1054
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Summary

• We are on the verge of discovering exciting new
  physics
• TeV scale Unification, origin of mass, hidden
  dimensions
• Neutrinos What are they? How do they relate to
  unification? To the universe?
• CP Violation Wheres all the anti-matter?
• Dark Matter and Energy Can we understand the
  other 96 of the universe?
• By the end of the decade, we will have some of
  the answersand probably many new questions

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• Backup Slides

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DOE-HEP Annual Budget(in Millions)
Includes 15.9M for SBIR/STTR in FY 2003,
17.6M in FY 2004, and 17.5M in FY 2005 Request.

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Example How to catch a Top quark
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EXO- Neutrinoless Double Beta Decay

• If neutrinoless double beta decay process exists,
  by measuring it we can determine
• Absolute effective mass scale of neutrinos
• Majorana nature of neutrinos
• Requires 5-10 tons of Xe(136)
• TPC detector identifies electrons
• Background reduced by unique Ba ion
  extraction/identification technique
• 200 kg prototype in preparation (to be at WIPP)
• Candidate for HEP initiative (100M)

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Neutrinos and Proton Decay

• DOE-HEP scientific (universities) participation
  in
• Super Kamiokande
• Water Cherenkov detector to search for proton
  decay and study neutrino interactions
• Located underground in mine in Kamioka, Japan
• 1998 first evidence for neutrino oscillations
• Data taking and analysis continue
• K2K
• Neutrino oscillation studies by sending neutrino
  beam from the KEK 12 GeV accelerator in
  Tsukuba, Japan to the SuperK detector (250km
  away)
• Data taking continues through 2004
• KamLAND
• Detector in the Kamioka mine in Japan
• Study neutrino oscillations by measuring the
  anti-neutrino flux from reactors in Japan and
  Korea
• Data taking and analysis continue
• ICARUS
• Underground detector at Gran Sasso (Italy) to
  search for proton decay and neutrino measurements