James L' Pinfold

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AstroCollider Physics
ASTROPARTICLE PHYSICS AND THE LHC
James L. Pinfold University of Alberta
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Menu

• The LHC and its multi-purpose detectors, for
  high pt physics (and forward physics?)
• Forward physics at the LHC and Cosmic Ray physics
• The cosmic ray energy spectrum
• Understanding cosmic ray air showers the NEEDS
  project
• Exotic physics (already seen in CR emulsions?)
• UHECR and SUSY
• The synergy between astroparticle physics and
  high pT LHC physics
• WMAP SUSY dark matter (MSUGRA, GMSB and split
  SUSY)
• LHC and dark matter (eg neutralino Dark Matter)
• Direct detection of dark matter
• Indirect detection of dark matter
• A brief look at gravitino dark matter
• Extra dimensions
• Collider signatures of Extra Dimensions
• Evidence for Extra Dimensions from the cosmos
• Mini black hole production at the LHC and in
  HECR interactions
• COSMOLHC the direct detection of cosmic rays
  with LHC detectors
• Conclusions

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The LHC Collider
LHC ring 26km in circ.

• SCHEDULE
• LHC install by the end of 2006
• First beam April 2007
• First collisions July 2007
• 2007 First physics 4 fb-1
• 2008-09 Low lumi 20 fb-1/y
• 2010 High lumi 100 fb-1/y

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The LHC Detectors

• PHYSICS TARGETS
• ATLAS, CMS
• - Higgs boson(s)
• - SUSY particles
• ??
• ALICE
• Quark Gluon Plasma
• LHC-B
• CP violation in the B sector
• TOTEM
• Total pp x-section
• MoEDAL
• Monopole search
• (LoI stage only)

CMS
MoEDAL
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Measuring the Forward Region at the LHC
The present LHC coverage
TOTEM

• TOTEM (at the CMS IP) 3 Roman Pot stations at
  both sides of IP to detect leading proton in
  elastic scattering and in diffractive
  interactions plus 2 telescopes (3lt?lt7) to
  study inelastic interactions in forward region
• Similar coverage being planned for ATLAS

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A Benchmark Measurement of stot(pp)
Goal of CMS/TOTEM and ATLAS 1 precision
Measured by TOTEM -t ? (4-mom. transfer)2 ?
(p?scat)2 (p7 TeV) Nel, Ninel nos of elastic
inelastic events (dNel/dt)t0 (extrap.of)
diff. elastic rate at t0 ? ? Reforward amp.
/Imforward amp. 0.10? 0.01
Curves are (log s)?
To achieve 1 accuracy on ?tot need to
Measure Ninel over large rapidity range to
minimize acceptance correction For ? ? 7
acceptance is 99 measure dNel/dt down to -t
2 x 10-2 GeV2 to minimize extrapolation to t0
? Of particular interest for cosmic ray physics
is the measurement of the total inelastic
X-section as well as the ratio of sdiff/sinel
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Forward physics at the LHC and Cosmic Ray Physics
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The LHC HECR Energy Spectrum

• Studies of LHC collisions with pp ( pA, AA)
  x-sections are important in refining our
  understanding the HECR energy spectrum.
• Is there something that colliders can contribute
  to understanding of the knee? For
  example, a new threshold
• The sextet quark model where enhanced WW/ ZZ
  production has a threshold at the knee (1015 eV)
• The Tevatron energy is just too low but the LHC
  could see a clear effect.
• Is the CR spectrum, beyond the GZK cut-off, due
  to physics beyond the SM?
• From monopoles
• From extra dimensions that induce strong n
  x-sections
• Originating from massive relic
  particle decay with MX gt1012 GeV,
• From SUSY particles such as the S0 (uds-gluino)

High energy CRs consist of protons, nuclei,
gammas,
GZK Cut-off
HECR manifest themselves as extended air showers
(EAS)
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Forward Physics - the LHC CRs

• Forward directions ( ?gt5) few particles with
  low pT but very high energy (gt90 of the event
  energy) relevant to HECR
• Collider physics measurement emphasis
• High Transverse energy Jets, Leptons, Leptonic
  secondaries ETmiss
• Cosmic Ray Extended Air Shower (EAS) measurements
  involve primarily
• Total/inelastic x-section fraction of
  diffractive dissociation energy flow particle
  multiplicity distributions hadronic secondaries
• The study of hA interaction is mostly limited to
  fixed target (FT) energies, ?(sNN)hA lt 0.03 TeV
  (new data from RHIC (Au-Au) is at?0.2 TeV) but
  Feynman Scaling breaks down at higher energies
  (eg Tevatron, LHC).
• Uncertainties in the MC prediction of the
  development EAS are due to uncertainties in the
  calculation of hadronic interactions.

ET
E
?
EAS
EAS
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Colliders CR EAS - The NEEDS Meeting

• Major uncertainties in our understanding of
  Cosmic ray observables still exist
• The NEEDS workshop - held in Karlsruhre in 2002 -
  discussed which measurements of hadronic
  interactions are key to our understanding of CR
  physics. Some central questions were
• How important are the uncertainties in our
  knowledge of hadronic interactions in the
  determination of CR flux comp.
• Will planned expts reduce these uncertainties.
• What additional expts are necessary.
• A brief list of some of the most important
  measurements for shower development
• A precise measurement of the stot sinel.
  proton cross-sections
• Energy distribution of the leading nucleon
  in the final state
• Measurement of sdiff/sinel
• Inclusive p-spectra in the frag. region xF gt0.1
• Ideally make these measurements for pp, AA, and
  pA at the LHC.

EG-1 The HECR Energy spectrum
EG-2 World dataltlog massgt
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Cosmic Ray Exotics at the LHC

• Centauro events have been predominantly observed
  in CR emulsion exposures in balloons
• Centauros all characterized by
• Abnormal hadron dominance in multiplicity/energy.
• Low hadron mult. (wrt AA
  collisions of similar energy)
• PT of produced particles more than
  normal (PT1.7 GeV/c)
• Pseudorapidity distributions consistent with
  formation isotropic decay of a
  fireball
• The CASTOR (CMS) proposal makes charge particle
  mult. EM/HAD E-flow up to h 8
• A tungsten/quartz fibre calorimeter
• CASTORs objectives, measure
• EEM/Ehad
• Longitudinal shower evolution
• Search for Centauros, etc.

• L1.5m, 8 sectors 9?

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HECRs and SUSY

• A possible origin of UHECRs is the decay of a
  supermassive particle Mx with mass related to
  the unification mass scale 1024 GeV
• Schematic view of a jet for an initial squark
  from the decay of the X particle
• Particles with mass of order mSUSY decay
  at the 1st vertical line. For mSUSYlt Q lt 0.1
  light QCD DOFs still contribute to the evolution
  of the cascade.
• At the second vertical line, all partons
  hadronize and unstable hadrons leptons decay.
• At best we would only detect on earth one
  particle of the 104s of particles produced in
  the decay of an X-particle.
• Thus, we will only be able to make studies of the
  single-particle inclusive spectra of protons,
  ns, LSPs gs.
• Thus, input from the LHC wouldl be vital to study
  physics at energies up to 1012 GeV.

hep-ph/0210142)
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The Synergy Between Astroparticle Physics and
High pT LHC physics
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WMAP Dark Matter

• Launch of WMAP satellite in June 2001 ?
  1st data, February 2003.
• The vastly increased precision of the WMAP CMB
  data, revealed temperature fluctuations that vary
  by only millionths of a degree.
• Best fit cosmological model (including CB, ACBAR,
  2dF Galaxy Redshift Survey and Lyman alpha
  forest data) give the following energy
  densities (units of the critical density)
• OL 0.730.04 (Vacuum energy)
• Ob 0.0440.004 (baryon density)
• Om 0.270.04 (Matter density
• One can derive the cold dark matter density
• 0.94 lt OCDM h2 lt 0.129 (95 CL) (Cold dark
  matter) normalized Hubble Constant 0.71 0.04
• Little or no hot dark matter

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Constraining Dark Matter Candidates

• Dark matter candidates are legion axions,
  gravitinos, neutralinos, KK particles, Q balls,
  superWIMPs, self-interacting particles, branons
• SUSY DARK MATTER (MSUGRA)
• (5 params m0- common scalar mass m1/2 common
  gaugino mass A0 - common trilinear coupling
  tanb m - Higgsino mass parameter)

mSUGRA A00 ,
Ellis et al., hep-ph/0303043
Co-annihilation region
Focus point region
Forbidden LSP stau
Bulk region
co-annihilation region
bulk region
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Investigating DM at the LHC
SUSY studies at the ATLAS/LHC will proceed in
four steps

• SUSY Discovery phase (inclusive searches) success
  assumed!
• Inclusive Studies (comparison of significance in
  inclusive channels etc).
• First rough predictions of Wch2 within specific
  model framework (e.g. Constrained MSSM / mSUGRA).
• Exclusive studies (calculation of
  model-independent SUSY masses) and interpretation
  within specific model framework.
• Model-independent calculation of LSP mass for
  comparison with e.g. direct searches detailed
  model-dependent calculations of DM quantities
  (Wch2, scp, fsun etc.)
• Less model-dependent interpretation.
• Approach to model-independent measurement of Wch2
  etc. through measurement of all relevant masses
  etc.

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First Step - Inclusive Constraints
ATLAS constraints
Direct Detection
jetsETmissX channel in ATLAS
Dan Tovey
WIMP-N x-section (pb).
Dan Tovey
M0 (GeV)
The next direct DM searches (1tonne) could
probe cosmologically favoured regions (s10-10
pb) not accessible to the LHC 1) Focus point
scenarios (large m0) 2) models with large
tan(b).
5s reach of the inclusive SUSY searches at ATLAS
for mSUGRA with large tanb probing regions
inaccessible to the current DM expts
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Step 2 Inclusive Studies
LHC Point 5 (Physics TDR)

• Assuming that SUSY is revealed at the LHC the
  next step will be to test broad features of the
  potential DM candidate.
• 1st Question is R-Parity Conserved?
• If YES possible DM candidate
• LHC experiments sensitive only to LSP lifetimes lt
  1 ms (ltlt tU 13.7 Gyr)
• 2nd Question is the neutralino the LSP?
• Natural in many MSSM models
• If YES then test for consistency with
  astrophysics
• If NO then what is it?
• e.g. Light Gravitino DM from GMSB models (not
  considered here)

R-Parity Conserved
R-Parity Violated
ATLAS
Non-pointing photons from c01gGg
GMSB Point 1b (Physics TDR)
ATLAS
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Stage 2/3 Model-Dependent DM

• If a viable DM candidate is found initially
  assume specific consistent model
• e.g. CMSSM / mSUGRA.
• Measure model parameters (m0, m1/2, tan(b),
  sign(m), A0 in CMSSM) Stage 2/3.
• Check consistency with accelerator constraints
  (mh, gm-2, bgsg etc.)
• Estimate Wch2 g consistency check with
  astrophysics (WMAP etc.)
• Ultimate test of DM at LHC only possible in
  conjunction with astroparticle experiments
• g measure mc , scp, fsun etc.

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Step 3 - Mass Measurements

• Model parameters estimated using fit to measured
  positions of kinematic end-points observed in the
  chain of decays in SUSY event. Model independent
  estimate of masses will also be made
• At point 5 expected precisions after 30 fb-1 on
  M0, M1/2 Tan b
  are 2.3, 0.9 and 0.5 respectively

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Stage 2/3 Model Parameters

• First indication (Stage 2) of CMSSM parameters
  from inclusive channels
• Compare significance in jets ETmiss n leptons
  channels
• Detailed measurements (Stage 3) from exclusive
  channels when accessible.
• Consider here two specific example points

ATLAS
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Step 3?4 Relic Density Scenarios

• Use parameter measurements to estimate Wch2 ,
  direct detection cross-section etc. (e.g. for 300
  fb-1, SPS1a)
• W c h2 0.1921 ? 0.0053 log10(scp/pb) -
  8.17 ? 0.04

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Direct Searches for WIMPs

• Predicted nuclear recoil energy spectrum depends
  on astrophysics (DM halo model), nuclear physics
  (form-factors, coupling enhancements) and
  particle physics (WIMP mass and coupling).

?p WIMP-nucleon scattering cross-section, f(A)
mass fraction of element A in target, S(A,ER)
exp(-ER/E0r) for recoil energy ER, I(A)
spin/coherence enhancement (model-dep.), F2(A,ER)
nuclear form-factor, g(A) quenching factor
(Ev/ER), ?(Ev)? event identification efficiency.
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Direct DM Searches

• Next generation of tonne-scale direct Dark Matter
  detection experiments should give sensitivity to
  scalar WIMP-nucleon cross-sections 10-10 pb.

(Slide supplied from D. Tovey)
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Indirect Dark Matter Searches

• Indirect neutralino dark matter can be detected
  via neutralino annihilations giving rise to 3
  main signals.
• The 1st of these signals arises from ns
  produced by neutralino annihilation in the
  suns/earths core. These ns detected via CC
  interactions (? ? µ convs) in n-telescopes such
  as AMANDA.
• The planned neutrino telescopes ANTARES IceCube
  are sensitive to Eµ gt 10 GeV Eµ gt 2550 GeV,
  respect.
• The 2nd signal stems from g-rays originating from
  neutralino annihilations in the galactic core
  halo producing hadrons, giving rise to gs
  primarily from p0 decays.
• These signals can be detected by space- based
  detectors such as EGRET or GLAST with
  thresholds as low as 100s of MeV and in
  atmospheric Cerenkov telescopes on the ground,
  with detection thresholds in the range 20?100
  GeV.
• The 3rd signal is provided by hard cosmic ray
  positrons produced in the decays of leptons,
  heavy quarks gauge bosons from neutralino
  annihilations in our galactic halo. A clumpy
  halo is required to get sufficient s/n.
• Space-based anti-matter detectors such as AMS-02
  and PAMELA will provide precise measurements of
  the positron spectrum and may be able to detect a
  possible positron signal from neutralino
  annihilation.
• All of these measurements are prone to large
  systematic uncertainties, for example on
  quantities such as neutralino densities and
  density variations in the core halo of the
  galaxy.

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Putting it All Together
The black contour depicts the exclusion that we
can expect from the planned future direct
detection (DD) dark matter experiments (sSI gt
10-9 pb).
The S/B gt 0.01 contour for halo produced
positrons (blue-green contour) and
The LHC (100 fb-1) can cover the HB/FP region up
to m1/2 700 GeV, which corresponds to a reach
in mgluino of 1.8 TeV
Reach of IceCube ? telescope with Fsun(µ) 40
µs/km2/yr and Eµ gt 25 covering the FP region to
1400GeV
The Tevatron (10 fb-1) could cover the Higgs
annihilation corridor as shown by red dashed line
If SUSY lies in the upper FP region, then it may
be discovered 1st by IceCube ( possibly
Antares), confirmed later by direct DM
detection and the LC1000.
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What if the Graviton is the LSP?

• Assume gravitino is LSP. Early universe behaves
  as usual, WIMP freezes out with desired thermal
  relic density
• Gravitinos are superweakly-interacting massive
  particles superWIMPs as all interactions are
  suppressed by MW/MPl 10-16
• Current scenarios favour a long lifetime for the
  WIMP (1 year) - A year passesthen all WIMPs
  decay to gravitinos
• Are there observable consequences? Well late
  decays, t ? t G can modify light element
  abundances
• Independent 7Li measurements are all low by
  factor of 3 - SuperWIMP DM naturally explains 7Li
  !

MPl2/MW3 year
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Collider Phenomenology

• Each SUSY event produces 2 metastable sleptons
  with a spectacular signature highly-ionizing
  charged tracks
• Current bound (LEP) m l gt 99 GeV
• Tevatron Run II reach m l 150GeV
• LHC reach m l 700 GeV in 1 year
• Slepton trapping
• Sleptons live for roughly a year, so can be
  trapped for the decays to be observed
  later
• LHC 106 sleptons/yr possible, but most are fast.
  By optimizing trap location and
  shape, can catch 100/yr in 1000
  m3we. (a 1000 a year at the LC)
• Measurement of G ? mG
• WG. SuperWIMP contribution to dark matter
• SUSY breaking scale
• Early universe (BBN, CMB) in the lab

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Extra Dimensions

• The broad features of theories of Extra
  Dimensions (EDs) are as follows
• Compactification of the n EDs generates a
  
  KK (Kaluza-Klein) tower of states - a
  generic
  feature of models with
  compactified EDs.
• Most of the ED models fall into 3 classes
• 1st, the large extra dimension (LED)
  
  ADD scenario
  in which
• Gravity propagates in the bulk, the
  
  matter gauge forces live on the
  3-brane.
• There is an emission and exchange of large
  
  KK towers of gravitons finely
  spaced in mass.
• 2nd - In the RS scenario where the hierarchy is
  
  generated by the large curvature
  of the EDs
  
• There exists 1 ED and the TeVPlanck branes
  within
  a 5-D space of constant -ve curvature
  
  that forms the bulk - where gravity can
  propagate.
• All of the SM particles and forces are confined
  
  to the TeV brane
• 3rd - The UED scenario all fields can propagate
  in the bulk and branes do not need to be present

Often assume that EDs have a common size R
(31n ) dimensions
(31) dimensions
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Searching for EDs at Colliders

• Searches for LEDs have usually assumed the ADD
  scenario. EG at LEP graviton emission virtual
  graviton effects from LEDs have been sought
• Hadron collider reach (ADD scenario) for real
  graviton emission and virtual
  graviton effects
• In RS scenario there are KK excitations
  
  of the SM gauge fields with
  masses TeV, that would manifest themselves at
  the LHC as resonances.
• The constraints from data theoretical
  asssumptions/ requirements mean that the RS
  scenario could be ruled out completely at the LHC

N2?7
80 pb-1
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Astrophysical/Cosmological Limits on EDs
Anomalous heating of neutron stars by
gravitionally trapped KK graviton modes
SN cooling via graviton emission
Radiative decay of gravitons to gs, contribute
to the diffuse g back-grounds

• Although some of these limits are stringent they
  are indirect and contain large systematic errors.
  Although the n 2 scenario looks to be in
  trouble.
• Ignoring these limitations we see that the
  astrophysical constraints allow low-gravity
  models with MD 1TeV, n ? 4.
• If extra dimensions are discovered at the LHC it
  would provide useful input to our understanding
  of astrophysics/cosmology.

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Extra Dimensions the Radion

• In the RS scenario the radion field is a scalar
  field which stabilizes the size of the
  extra-dimensions. Parameters radion mass (m? ),
  radion vev (?? ), h-? mixing (?)
• The presence of the radion is one of the key
  phenomenological consequences of theories of
  warped EDs such as RS.
• Similar couplings as SM Higgs but with different
  strengths (? ?gg is enhanced wrt the Higgs ,
  ?WW/ZZ suppressed in some cases) ? ? HH
  important if open. ?? ltlt ?H
• Precise measurements of couplings needed to
  disentangle ?/H. The determination at the LHC
  would be 10.
• The experimental efforts to determine the
  properties of the radion field have a
  cosmological significance since the size of the
  interaction of the radion field with SM particles
  determines whether it can decay quickly enough to
  avoid overclosure by the beginning of BBN.
• The ADD scenario also admits a light radion (10
  MeV gt Mf gt 10-3 eV) that is a potential source of
  dark matter similar to axionic dark matter

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Searching for the Radion at ATLAS
(For 100 fb-1 of data)
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Black Hole Production at the LHC

• Big surprise BH production is not an exotic
  remote possibility, but the dominant effect!
  (Limitationlack of knowledge of quantum gravity
  effects )

• Main idea when the Ecm reaches the
  
  
  
  fundamental Planckscale, a BH is formed
  
  x-section is given by the black disk
  
  s pRS2 1 TeV-2 10-38 m2
  100 pb
• The underlying assumptions rely on 2 simple
  qualitative properties the absence of small
  couplings the democratic nature of BH decays
• Black holes decay immediately (? 10-26 s) by
  Hawking radiation large multiplicity, small
  Etmiss, jets/leptons 5
• Black holes to hadrons/leptons/g,W,Z/Higgs
  75/20/3/2

James Pinfold ATLAS Athens Physics
Workshop 20
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Black Holes in ATLAS
Preliminary studies reach is MD 6 TeV for any
? in one year at low luminosity.
MBH 8 TeV
By testing Hawking formula ? proof that it is BH
measure of MD, ? Precise measurements of MBH
TH needed (TH from lepton g spectra)

• The end of short-distance physics? Naively
  yes, once the event horizon is larger than a
  proton, a HEP collider would only produce BHs!
• But, gravity couples universally, so each new
  particle, which can appear in the BH decay would
  be produced with 1 probability (if its mass is
  less thanTH 100 GeV)
• Time required for a 5s Higgs discovery MP
  1/3/5 TeV 1 hr/1 wk/1yr. SUSY particles would
  also enjoy a similar rapid discovery mode
• Black hole decays open a new window into new
  physics! Hence, rebirth of the short-distance
  physics! Clean BH samples would make LHC a new
  physics factory as well

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Black Hole Production by Cosmic Rays
(Feng and Shapere, hep-ph/0109106)
hep-ph/0311365

• Consider BH production deep in the atmosphere by
  UHE neutrinos - detect them, e.g. in PAO, Ice3
  or AGASSA
• OFO 100 BHs can be detected before the LHC turns
  on
• But can the BH signature be uniquely
  established?

nD6
PAO limit (96 CL)
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COSMOLHC the Direct Detection of Cosmic Rays
with LHC Detectors
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Cosmo-LHC

• The LHC detectors will deploy unprecedented areas
  of precision muon tracking, tracking and
  calorimetry 100m underground
• In the spirit of Cosmo-LEP the LHC detectors
  could be used to detect and measure cosmic ray
  events directly

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Muon Physics Plus with CosmoLHC

• CosmoLHC carrying on CosmoLEP (L3C,
  CosmoALEPH). Topics to study
• Single/inclusive ms (pt spectrum gt20 GeV? 2TeV,
  angular dist. 0 lt q lt 50o, charge ratio, etc.)
• Upward going ms (E spectrum, angular
  distribution, etc.)
• Multi-ms (composition measurements, etc.)
• Muon bundles (evidence for new physics?)
• Isoburst events seen in LVD, KGF (an hyp. is that
  they are due to the decay of WIMPS (Mgt 10 GeV)
  better measured at the LHC.)
• These measurements will yield data on
• Forward physics of hadronic showers
• Primary composition of cosmic rays
• Non-uniformities (sidereal anisotropies, bursts,
  point sources, GRBs)
• New physics (eg anomalous muon bundles)?
• One can also place detectors in coincidence
  (cosmic strings)

L3C
Single muon data
L3C
A muon bundle event
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Concluding Remarks

• There is a considerable and growing synergy
  between collider astroparticle physics A good
  example of this partnership is the search for
  dark matter. Ultimate test of DM at LHC only
  possible in conjunction with astroparticle
  experiments g measure mc , scp,, fsun etc.
• The nature of discovery physics is that it often
  occurs when it is least expected ? astrocollider
  physics maximizes the coverage of possibility
  space

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Extra SLIDES
42
ATLAS
Weight 7K tonnes
46m
25m
Scale
43
LHC- Direct Search for Monopoles

• An LOI for the MoEDAL experiment to search for
  monopoles, dyons other highly ionizing objects
  has been accepted by the LHCC.
• The MoEDAL detector is essentially a partial
  plastic ball deployed around the LHCb vertex
  chamber region.
• Highly ionizing objects are detected by etching
  the plastics ionization damage zones
• Threshold Z/b gt 10. (Z/b for a highly
  relativistic monopole 1500)
• Advantages
• Minimizes assumptions about the nature of the
  monopole or dyon
• Essentially no SM background. In principle 1
  event should be enough for a discovery
• Very Very cost effective

(plastic ball)
Detection medium, plastic track-etch detectors
(CR39)
44
Indirect Search for Monopoles/Dyons
Also searched in cosmic rays
ATLAS, 100 fb-1
Caveat there will be large form factor
suppression in the cross-section if the monopole
is not point-like
45
The Mysteries of an Opaque Universe

• The universe is opaque to UHECR
• In the case of the GZK cut-off a 5x1019 eV
  proton has a mfp of 50 mpc due to interaction
  with photons in the the CMB.
• But no nearby sources have been identified
• How are the protons with energy gt EGZK
  getting to us? There are two
  scenarios
• BOTTOM UP acceleration in AGNs, g-ray
  bursters, etc. Then production of
  a neutral (n, so,etc).
• BOTTOM UP with GZK cut-off relaxed by
  violation of Lorentz Invariance, etc.
• Or TOP DOWN topological defects (cosmic strings,
  monopoles, etc.) or massive relics, etc.

Region restricted by GZK cut-off 100 Mpc
10,000Mpc
Size of observable universe
46
Cosmic Ray Exotica

• Centauro, Mini-Centauros, Chirons, Geminions are
  all characterized by
• Abnormal hadron dominance in multiplicity/energy.
• Low total hadron multiplicity compared to that
  expected for A-A collisions in that energy range
• PT of produced particles higher than normal
• PT 1.7 GeV/c for centauros
• PT of 10-15 GeV/c for chirons
• Pseudorapidity distributions consistent with
  formation and isotropic decay of a fireball with
• Nh 100 MFB for centauros and chirons
• Nh 15 and MFB 35 GeV for mini-centauros
• Anti-Centauros
• Events with abnormal EM dominance
• Long Flying Component
• Unusually penetrating cascades, clusters of
  showers
• Halo Events
• Dense EM cascade containing several hadronic
  cores spaced closely together (small rel. PT)
  in many multi-halo events the halos are aligned,
  where halos are EM showers in jets.
• Muon Bundles
• Events where bundles of muons with very small
  lateral separation as if produced in a process
  with very small PT

A Centauro Model
Does the production of strangelets play a role in
Centauro-type phenomena?
47
Focus Point Region

• Relic density can also be reduced if c has
  significant Higgsino component to enhance

Feng, Matchev, Wilczek (2000)

• Motivates SUSY with multi-TeV g, q, l c/c0
  highly degenerate
• Such SUSY would be missed at LHC, discovered at LC

Baer, Belyaev, Krupovnickas, Tata (2003)
James Pinfold Fermilab June 2005
48
DM Detectors (as of summer 2004)

• CDMS (Stanford/Soudan)
• CDMS I Shallow site (Stanford)
• punch through fast neutrons from cosmic ray µ
  spallation.
• Subtraction by MC checks on multiple scatters
  limit at 3x10-6pb.
• CDMS II underground operation at Soudan mine from
  April 2003
• 56 live days data collected, blind analysis
  completed, limit at 4x10-7pb
• CRYO-ARRAY tonne scale detector in planning
  stages
• XENON (DUSEL)
• RD programme to develop two phase xenon target
  completed
• Proposal submitted for construction of 100kg
  module for 2007 deployment
• Intend tonne scale final detector for deployment
  at DUSEL
• XMASS (Kamioka)
• 3kg two phase xenon dark matter detector in
  operation.
• High background due to radon contamination (200
  Bq/m3!)
• 20kg module under construction

• DAMA (Gran Sasso)
• 9x9.7 kg crystals in shield 7 years data
  analysed
• Annual variation observed in total event rate lt
  6keV ( noise rej.)
• LIBRA (250kg) NaI array construction completed
• Edelweiss (Frejus)
• Ge thermal/ionisation detector. 50 kg.days data
  from 4x320g units
• 2002 no events in recoil region (one on boundary)
  giving 10-6pb limit.
• 2003 data runs see neutron events in nuclear
  recoil region, confirms limit.
• 28x320g array expected operation in 2004 40kg
  array planned
• CRESST (Gran Sasso)
• CRESST I Sapphire bolometer low WIMP mass, spin
  interaction reach
• CRESST II CaWO4 thermal/scint 300g demonstrator
  operated
• Engineering runs completed neutrons observed,
  no shielding
• 10kg (33x330g) stack in construction SQUID
  readout incorporated

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Colour Sextet Quark Model - Notes
Dfirectly rom Mike Albrows talk - GTEV Gluon
Physics at the Tevatron