J James L. Pinfold University of Alberta ASTROPARTICLE PHYSICS AND THE LHC James Pinfold ISMD 2005.

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James L. PinfoldJames L. Pinfold

University of AlbertaUniversity of Alberta

ASTROPARTICLE PHYSICS AND THE LHCASTROPARTICLE PHYSICS AND THE LHCASTROPARTICLE PHYSICS AND THE LHCASTROPARTICLE PHYSICS AND THE LHC

James Pinfold ISMD 2005

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Astro-Collider Physics – The SynergiesAstro-Collider Physics – The Synergies

High PT

Collider PhysicsInvolving ET

miss, jet production, lepton ID, etc Relevant to Dark Matter, Extra Dimensions, etc.

Forward (||>5) Collider Physics

Few particles with low pT but very high energy

( >90% of Eevent) relevant to HECR

Direct Detection of Cosmic Rays in Collider Detectors

AstroparticlePhysics &Cosmology


http://atlas.ch/atlas_photos/fulldetector/fulldetector/atlas_event_cross.html

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The LHC Collider

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

LHC ring ~26km in circ.


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The LHC DetectorsThe LHC DetectorsPHYSICS 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 accepted)

LHCF:Forward pion production X-section measurement (Proposal)

CMS


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Forward Physics at the LHC Forward Physics at the LHC & Astroparticle Physics & Astroparticle Physics

Forward (||>5) Collider Physics

Few particles with low pT but very high energy

( >90% of Eevent) relevant to HECRAstroparticle

Physics &Cosmology



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Measuring the Forward Region at the LHC Measuring the Forward Region at the LHC

• Extended coverage being planned for ATLAS (with pots out to 420m?)Extended coverage being planned for ATLAS (with pots out to 420m?)

• The LHC benchmark measurement in this area is that of The LHC benchmark measurement in this area is that of tottot(pp) to ~1%(pp) to ~1%


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Colliders & CR Extended Air Showers Colliders & CR Extended Air Showers • Major uncertainties in our understanding of

Cosmic ray observables still exist

• The NEEDS workshop (2002) discussed which measurements of hadronic interactions are key to our understanding of CR physics. Eg:

– A precise measure of tot /inel. p-p x-sections

– Energy distribution of the leading nucleon in the final state

– Measurement of diff/inel

– Inclusive -spectra in the frag. region xF >0.1

– Make these measurement for pp, pA, and AA

• To answer these questions ATLAS, CMS TOTEM, CASTOR have been joined by the proposed LHCF Project: “ To Measure Very Forward Particles at the LHC in order to Understand the Highest Energy Cosmic Rays ”

• To achieve its aim LHCF aims to measure the production x-section of pions in p-p collisions at the highest energy (≡ 1017eV CR proton)

EG-1 The HECRenergy spectrum

LHCF Detector

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The LHC & HECR Energy SpectrumThe LHC & HECR Energy Spectrum• Studies of forward LHC collisions with Studies of forward LHC collisions with

pp, pA & AA collisions are needed to pp, pA & AA collisions are needed to refine our understanding of the HECR refine our understanding of the HECR energy spectrum. energy spectrum.

• Can colliders can contribute to our Can colliders can contribute to our understanding of the knee? understanding of the knee? – Eg the Colour Sextet quark model - Eg the Colour Sextet quark model -

enhanced WW/ ZZ production has a enhanced WW/ ZZ production has a threshold at the knee (~10threshold at the knee (~101515 eV) eV)

– The Tevatron energy is just too low The Tevatron energy is just too low but the LHC could see a clear effect.but the LHC could see a clear effect.

• Is the CR spectrum, beyond the GZK Is the CR spectrum, beyond the GZK cut-off, due to physics beyond the SM?cut-off, due to physics beyond the SM?– From monopolesFrom monopoles– From Extra Dimensions inducing From Extra Dimensions inducing

strong strong x-sections x-sections– From massive relic particle (MRP) From massive relic particle (MRP)

decay with Mdecay with MX X >10>1012 12 GeV, GeV, – From SUSY particles such as the SFrom SUSY particles such as the S00

(uds-gluino)(uds-gluino)

GZKCut-off

High energy CRs consist of protons, nuclei, gammas,…


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Cosmic Ray Exotics at the LHCCosmic Ray Exotics at the LHC• Centauro events have been mostly Centauro events have been mostly observed in CR emulsion exposures in observed in CR emulsion exposures in balloons – they are all characterized by:balloons – they are all characterized by:– Abnormal hadron dominance in Abnormal hadron dominance in

multiplicity/energy.multiplicity/energy.

– Low hadron mult. (wrt AA Low hadron mult. (wrt AA collisions of similar energy)collisions of similar energy)

– PPTT of produced particles more of produced particles more than “normal” (Pthan “normal” (PTT~1.7 GeV/c)~1.7 GeV/c)

– .. distributions consistent with distributions consistent with fireball formation & isotropic decay fireball formation & isotropic decay

• The LHC CASTOR (CMS) proposal The LHC CASTOR (CMS) proposal measure charge particle mult. & measure charge particle mult. & EM/HAD E-flow up to |EM/HAD E-flow up to || ~8| ~8 – A tungsten/quartz fibre calorimeterA tungsten/quartz fibre calorimeter

• CASTOR’s objectives, measure:CASTOR’s objectives, measure:

– EEEMEM/E/Ehadhad & Longitudinal shower & Longitudinal shower evolutionevolution

– Search for Centauros, etcSearch for Centauros, etc..–L=1.5m, 8 sectors ~ 9

One of the mysterious "Centauro" events seen by the Brazil Japan collab. in X-ray emulsion chambers on Mt Chacaltaya


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High PT Collider Physics + CosmologyHigh PT Collider Physics + Cosmologyand Astroparticle Physicsand Astroparticle Physics

High PT

Collider PhysicsInvolving ET

miss, jet production, lepton ID, etc Relevant to Dark Matter, Extra Dimensions, etc. Astroparticle

Physics &Cosmology



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Very High Energy Very High Energy CosmicCosmic RaysRays & SUSY & SUSY• A possible origin of UHECRs is the A possible origin of UHECRs is the

decay of a MRP, Mdecay of a MRP, Mx, x, with mass related with mass related to the unification mass scale.to the unification mass scale.

• Schematic view of a ‘jet’ for an initial Schematic view of a ‘jet’ for an initial squark from the decay of the ‘X’ particle squark from the decay of the ‘X’ particle

– Particles with mass of order Particles with mass of order mmSUSYSUSY decay at the 1 decay at the 1stst vertical line. vertical line.

– At the second vertical line, all partons At the second vertical line, all partons hadronize and unstable hadrons + hadronize and unstable hadrons + leptons decay. leptons decay.

• At best we would only detect on earth one At best we would only detect on earth one particle of the ~10particle of the ~1044’s produced in the ‘X-particle’ ’s produced in the ‘X-particle’ decay decay

• Thus we will only be able to study single Thus we will only be able to study single -particle inclusive spectra of p’s, -particle inclusive spectra of p’s, ’s, LSPs & ’s, LSPs & ’s.’s.

• Input from the LHC on SUSY cascade studies Input from the LHC on SUSY cascade studies are vital to study this physics - at energies up to are vital to study this physics - at energies up to 101012 12 GeV.GeV.

hep-ph/0210142)


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WMAP & Dark Matter WMAP & Dark Matter • Launch of WMAP satellite in June 2001 Launch of WMAP satellite in June 2001

1 1stst data, February 2003. data, February 2003.

• The vastly increased precision of the WMAP The vastly increased precision of the WMAP CMB data, revealed temperature fluctuations CMB data, revealed temperature fluctuations that vary by only millionths of a degreethat vary by only millionths of a degree. .

• Best fit cosmological model (including CB, Best fit cosmological model (including CB, ACBAR, 2dF Galaxy Redshift Survey and ACBAR, 2dF Galaxy Redshift Survey and Lyman alpha forest data) give the following Lyman alpha forest data) give the following energy densities (units of the critical density):energy densities (units of the critical density):

– ΩΩ = 0.73 = 0.73±0.04 (Vacuum energy)±0.04 (Vacuum energy)

– ΩΩbb = 0.044 = 0.044±0.004 (baryon density)±0.004 (baryon density)

– ΩΩmm = 0.27 = 0.27±0.04 (Matter density±0.04 (Matter density

• One can derive the cold dark matter densityOne can derive the cold dark matter density

– 0.94 0.94 < < ΩΩCDMCDM h h2 2 < 0.129 (95% CL) (CDM) – < 0.129 (95% CL) (CDM) – normalized Hubble Constant =0.71 normalized Hubble Constant =0.71 ± 0.04± 0.04

• Little or no hot dark matterLittle or no hot dark matter


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mSUGRA A0=0 ,

Ellis et al.,hep-ph/0303043

~

ForbiddenLSP = stau

~0

~

“co-annihilation region”

Disfavoured by BR (b Disfavoured by BR (b s s) ) from CLEO, BaBar BELLE from CLEO, BaBar BELLE BR (b BR (b s s) = (3.2 ) = (3.2 0.5) 0.5) 10 10-4-4

Favoured by cosmologyFavoured by cosmologyassuming 0.1 assuming 0.1 hh2 2 0.3 0.3

Favoured by cosmology Favoured by cosmology assuming 0.094 assuming 0.094 hh2 2 0.129 0.129

i.e. new WMAP resultsi.e. new WMAP results R

~0

0

“bulk region”

b s

q~

Constraining Dark Matter CandidatesConstraining Dark Matter Candidates

Favoured by gFavoured by g-2 (E821) -2 (E821)

• Dark matter candidates are legion: Dark matter candidates are legion: axions, gravitinos, neutralinos, KK axions, gravitinos, neutralinos, KK particles, Q balls, superWIMPs, particles, Q balls, superWIMPs, branons…branons…

• SUSY dark matter (MSUGRA) a good SUSY dark matter (MSUGRA) a good candidate is the neutralino candidate is the neutralino LHC can LHC can explore a lot of the parameter spaceexplore a lot of the parameter space

• MSUGRA would be discovered in one MSUGRA would be discovered in one year at the LHC using jets year at the LHC using jets + E+ ETT

missmiss +X +X

Co-annihilation region

Bulk region

Focus point (FP) region


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Direct Searches for WIMPsDirect Searches for WIMPs• Predicted nuclear recoil energy spectrum depends on astrophysics (DM Predicted nuclear recoil energy spectrum depends on astrophysics (DM

halo model), nuclear physics (form-factors, coupling enhancements) and halo model), nuclear physics (form-factors, coupling enhancements) and particle physics (WIMP mass and coupling).particle physics (WIMP mass and coupling).

p p = WIMP-nucleon scattering cross-section,= WIMP-nucleon scattering cross-section,

f(A) = mass fraction of element A in target,f(A) = mass fraction of element A in target,S(A,ES(A,ERR) ~ exp(-E) ~ exp(-ERR/E/E00r) for recoil energy Er) for recoil energy ERR,,

I(A) = spin/coherence enhancement (model-dep.),I(A) = spin/coherence enhancement (model-dep.),FF22(A,E(A,ERR) = nuclear form-factor,) = nuclear form-factor,

g(A) = quenching factor (Eg(A) = quenching factor (Evv/E/ERR),),

(E(Evv)= event identification efficiency.)= event identification efficiency.

dRdEv

== pp .. AA f(A) f(A) .. S(A,ES(A,ERR)) .. I(A)I(A) .. FF22(A,E(A,ERR)) .. g(A)g(A) .. (E(Evv))


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Direct DM Searches Direct DM Searches Direct DM Searches Direct DM Searches • Next generation of tonne-scale direct Dark Matter detection experiments Next generation of tonne-scale direct Dark Matter detection experiments

should give sensitivity to scalar WIMP-nucleon cross-sections ~ 10should give sensitivity to scalar WIMP-nucleon cross-sections ~ 10 -10-10 pb. pb.

ZEPLIN-MAX

GENIUS

XENON

ZEPLIN-4

ZEPLIN-2

EDELWEISS 2

CRESST-II

ZEPLIN-I

EDELWEISS

CDMSDAMA


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Indirect Dark Matter SearchesIndirect Dark Matter Searches• Indirect neutralino dark matter can be detected via neutralino annihilations, giving rise Indirect neutralino dark matter can be detected via neutralino annihilations, giving rise

to 3 main signals: to 3 main signals: – Neutralino annihilation in the sun’s/earth’s core. These Neutralino annihilation in the sun’s/earth’s core. These ’s detected via CC ’s detected via CC

interactions (interactions (ν ν µ µ conv’s) in conv’s) in -telescopes such as AMANDA. -telescopes such as AMANDA. • The planned neutrino telescopes ANTARES & IceCube are sensitive to The planned neutrino telescopes ANTARES & IceCube are sensitive to EEµµ > > 10 GeV & 10 GeV & EEµµ > >

25–50 GeV, respectively 25–50 GeV, respectively

– ..-rays originating from neutralino annihilations in the galactic core & halo producing -rays originating from neutralino annihilations in the galactic core & halo producing hadrons, which give rise to hadrons, which give rise to ’s mostly from ’s mostly from 00 decays. decays. • Detected by space- based detectors such as EGRET/GLAST with thresholds as low as 100’s Detected by space- based detectors such as EGRET/GLAST with thresholds as low as 100’s

MeV and in atmospheric Cerenkov telescopes, with thresholds in the range 20MeV and in atmospheric Cerenkov telescopes, with thresholds in the range 20100 GeV.100 GeV.

– Hard cosmic ray positrons produced in the decays of leptons, heavy quarks & gauge 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 bosons from neutralino annihilations in our galactic halo. A “clumpy halo” is required to get sufficient s/n.to get sufficient s/n.• Space-based anti-matter detectors such as AMS-02 and PAMELA will provide precise 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 positron signal from measurements of the positron spectrum and may be able to detect a positron signal from neutralino annihilation.neutralino annihilation.

• The predicted detection rates are very dependent on the models of neutralino The predicted detection rates are very dependent on the models of neutralino densities, etc. and thus subject to large systematic uncertainties.densities, etc. and thus subject to large systematic uncertainties.


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Putting it All TogetherPutting it All TogetherThe black contour depicts the exclusion that we can expect from the planned future direct detection (DD) dark matter experiments (σSI > 10-9 pb).

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

The Tevatron (10 fb-1) could cover the Higgs annihilation corridor as shown by red dashed line

Reach of IceCube ν telescope with sun(μ) = 40 μ’s/km2/yr and Eμ > 25covering the FP region to 1400GeV

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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Extra DimensionsExtra Dimensions• A broad features of theories of Extra Dimensions (EDs) is that A broad features of theories of Extra Dimensions (EDs) is that ccompactification of the ompactification of the n n EDs generates a EDs generates a KK (Kaluza-Klein) tower of states KK (Kaluza-Klein) tower of states

• Most of the ED models fall into 3 classesMost of the ED models fall into 3 classes

–11stst - The large extra dimension (LED) - The large extra dimension (LED) ADD scenario in which: ADD scenario in which:•Gravity propagates in the bulk, the Gravity propagates in the bulk, the matter gauge forces live on the 3-brane. matter gauge forces live on the 3-brane.

–22ndnd - The RS scenario, the hierarchy is - The RS scenario, the hierarchy is generated by the large curvature of the EDs: generated by the large curvature of the EDs: •There exists 1 ED + the TeV & Planck branes There exists 1 ED + the TeV & Planck branes within a 5-D space of constant -ve curvature within a 5-D space of constant -ve curvature forming the bulk - where gravity propagates. forming the bulk - where gravity propagates.

•SM particles & forces are confined to the TeV SM particles & forces are confined to the TeV brane brane

– 33rdrd - The UED scenario all fields can - The UED scenario all fields can propagate in the bulk and branes do not need propagate in the bulk and branes do not need to be present to be present

(3+1+n ) dimensions

(3+1) dimensions

Often assume that EDs have a common size R


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Searching for EDs at CollidersSearching for EDs at Colliders• Searches for LEDs have usually assumed the ADD scenario. EG at LEP Searches for LEDs have usually assumed the ADD scenario. EG at LEP

graviton emission & virtual graviton effects from LEDs have been soughtgraviton emission & virtual graviton effects from LEDs have been sought

• Hadron collider reach (ADD scenario) for real graviton emission and Hadron collider reach (ADD scenario) for real graviton emission and virtual graviton effects virtual graviton effects

• In RS scenario there are KK excitations In RS scenario there are KK excitations of the SM gauge fields with masses ~TeV, manifested as of the SM gauge fields with masses ~TeV, manifested as resonances. resonances.

• The constraints from data + theoretical requirements mean that the RS The constraints from data + theoretical requirements mean that the RS scenario could be ruled out completely at the LHCscenario could be ruled out completely at the LHC

N=27 ~80 pb-1


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Astrophysical/Cosmological Limits on EDsAstrophysical/Cosmological Limits on EDs

• Although some of these limits are stringent they are indirect and contain Although some of these limits are stringent they are indirect and contain large systematic errors. Although the n =2 scenario looks like it’s in trouble.large systematic errors. Although the n =2 scenario looks like it’s in trouble.

• Ignoring these limitations we see that the astrophysical constraints allow Ignoring these limitations we see that the astrophysical constraints allow low-gravity models with low-gravity models with MMDD ~1 ~1 TeV, TeV, n n 4.4.

• If EDs are discovered at the LHC it would provide useful input to our If EDs are discovered at the LHC it would provide useful input to our understanding of astrophysics/cosmology.understanding of astrophysics/cosmology.

SN coolingvia gravitonemission

Anomalous heating of neutron stars by gravitionally trapped KK graviton modes

Radiative decay of gravitons to ’s, contribute to thediffuse back-grounds


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Black Hole Production at the LHCBlack Hole Production at the LHC• In theories with large EDs BH production is not an remote possibility, but In theories with large EDs BH production is not an remote possibility, but

could be the dominant effect when the Ecould be the dominant effect when the Ecmcm reaches the “Planck” scale reaches the “Planck” scale

• The Cross-section is given by the black disk; The Cross-section is given by the black disk; σ ~ πRσ ~ πRSS

22 ~ 1 TeV ~ 1 TeV-2-2 ~ 10 ~ 10-38-38 m m2 2 ~100 pb.~100 pb.

• Two qualitative assumptions: the absence of small Two qualitative assumptions: the absence of small couplings; the “democratic” nature of BH decayscouplings; the “democratic” nature of BH decays

• BHs decay to give large multiplicity, small EBHs decay to give large multiplicity, small ETmiss, jets/leptons ~5 , jets/leptons ~5

hadrons/leptons/hadrons/leptons/,W,Z/Higgs ~ 75%/20%/3%/2%,W,Z/Higgs ~ 75%/20%/3%/2%

• BH decays open a window into new physics! Clean BH samples would make LHC BH decays open a window into new physics! Clean BH samples would make LHC a new physics factory. EG SUSY particles produced ~1% levela new physics factory. EG SUSY particles produced ~1% level


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Black Holes at the LHCBlack Holes at the LHC• The LHC reach is MThe LHC reach is MDD ~ 6 TeV for any ~ 6 TeV for any in one year at low luminosity in one year at low luminosity

• Once the event horizon is larger than a proton, the LHC would only Once the event horizon is larger than a proton, the LHC would only produce BHs! An example of an ATLAS BH event is shown below.produce BHs! An example of an ATLAS BH event is shown below.

MBH ~ 8 TeV


ATLAS

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Black Hole Production by Cosmic RaysBlack Hole Production by Cosmic Rays

(Feng and Shapere, hep-ph/0109106)

• Consider BH production deep in the Consider BH production deep in the atmosphere by UHE neutrinos - detect atmosphere by UHE neutrinos - detect them, e.g. in PAO, Ice3 or AGASSAthem, e.g. in PAO, Ice3 or AGASSA

• OFO 100 BHs can be detected before OFO 100 BHs can be detected before the LHC turns onthe LHC turns on

• But can the BH signature be uniquely But can the BH signature be uniquely established?established?

PAO limit (96% CL)

hep-ph/0311365nD=6


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Direct Detection of CRs at the LHCDirect Detection of CRs at the LHCDirect Detection of Cosmic Rays in Collider Detectors

AstroparticlePhysics &Cosmology



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Cosmo-LHCCosmo-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 CosmoLHCMuon Physics Plus with CosmoLHC

• CosmoLHC – carrying on CosmoLEP (L3+C, CosmoALEPH). Topics to study:– Single/inclusive ’s

– Upward going ’s (E spectrum, angular distribution, etc.)

– Multi-’s + Muon bundles

– Isoburst events seen in LVD, KGF (due to the decay of WIMPS with M> 10 GeV??)

• 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 large area coincidence (cosmic strings)

Single muon data

A muon “bundle” event

L3+C

L3+C

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Concluding RemarksConcluding Remarks• There is a considerable and growing synergy between collider & There is a considerable and growing synergy between collider &

astroparticle physics A good example of this partnership is the search for astroparticle physics A good example of this partnership is the search for dark matter. dark matter. Ultimate test of DM at LHC Ultimate test of DM at LHC only possibleonly possible in conjunction with in conjunction with astroparticle experiments astroparticle experiments measure m measure m , , pp,,, , sunsunetc. etc.

• The nature of discovery physics is that it often occurs when it is least The nature of discovery physics is that it often occurs when it is least expected expected astrocollider physics maximizes the coverage of “possibility astrocollider physics maximizes the coverage of “possibility space”space”

J James L. Pinfold University of Alberta ASTROPARTICLE PHYSICS AND THE LHC James Pinfold ISMD 2005.

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Transcript of J James L. Pinfold University of Alberta ASTROPARTICLE PHYSICS AND THE LHC James Pinfold ISMD 2005.