# Presentation: 202035

## AstroCollider Physics

**James L. Pinfold**
**University of Alberta**

**ASTROPARTICLE PHYSICS AND THE LHC**

- 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 p**T** 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

## 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.

## The LHC Detectors

_*PHYSIC*__*S 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**

## Measuring the Forward Region at the LHC 

- Measuring the Forward Region at the LHC

- The present
- LHC
- coverage

- 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 (3<||<7)  to study inelastic interactions in forward region** **
- Similar coverage being planned for ATLAS

**TOTEM**

## A Benchmark Measurement of tot(pp) 

- A Benchmark Measurement of tot(pp)

- Curves are ~ (log s)

**Measured by TOTEM**
**-t ******** (4-mom. transfer)****2**** ******** (p********scat****)****2**** (p=7 TeV)**
**Nel, Ninel : no’s of elastic & inelastic events**
**(dN****el****/dt)|t=0: (extrap.of) diff. elastic rate at t=0**
****** ******** ****Re[forward amp.] /Im[forward amp.] = 0.10******** 0.01**

**Goal of CMS/TOTEM and**
**ATLAS: ~ 1 % precision**

**To achieve  ~ 1%  accuracy on ********tot **** need  to Measure N****inel****  over large rapidity range to minimize acceptance correction**
**For |********| ******** 7   acceptance  is 99 %  measure dN****el****/dt down to  -t ~ 2 x 10****-2 ****GeV****2 **** to minimize extrapolation to t=0**

****** ****Of particular interest for cosmic ray physics is the measurement of the total & inelastic X-section as well as the ratio of ********diff****/********inel**

## Forward physics at the LHC 

- Forward physics at the LHC
- and Cosmic Ray Physics

## 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  x-sections
- Originating from massive relic                particle decay with MX >1012 GeV,
- From SUSY particles such as the S0 (uds-gluino)

- GZK
- Cut-off

**High energy CRs consist of protons, nuclei, gammas,...**

**HECR manifest themselves as **
**extended air showers (EAS) **

## Forward Physics - the LHC & CRs

- Forward directions (| ****|>5): few particles with low pT but very high energy (>90%  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 < 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.

**EAS**

****

**E**

**E****T**

**EAS**

## 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 tot  & inel. proton cross-sections
- Energy distribution of the leading nucleon                 in the final state
- Measurement of diff/inel
- Inclusive -spectra in the frag. region xF >0.1
- Ideally make these measurements for pp, AA, and  pA at the LHC.

**EG-2 World data:<log mass>**

**EG-1 The HECR**
**Energy spectrum**

## 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” (PT~1.7 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 || ~8** **
- A tungsten/quartz fibre calorimeter
** **CASTOR’s objectives, measure:
- EEM/Ehad
- Longitudinal shower evolution
- Search for Centauros, etc.

**L=1.5m, 8 sectors ~ 9******

## HECRs and SUSY

- A possible origin of UHECRs is the decay of a supermassive particle M**x  **with mass related to the unification  mass scale 10**24** GeV
- Schematic view of a ‘jet’ for an initial squark from the decay of the ‘X’ particle
- Particles with mass of order *m*SUSY         decay at the 1st vertical line. For *m*SUSY*< Q < *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 ~104’s 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, ’s, LSPs & ’s.
- Thus, input from the LHC wouldl be vital to study physics at energies up to 1012 GeV.

**hep-ph/0210142)**

## The Synergy Between Astroparticle 

- The Synergy Between Astroparticle
- Physics and High p**T** LHC physics

## WMAP & Dark Matter 

- 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):
- Ω = 0.73±0.04 (Vacuum energy)
- Ωb = 0.044±0.004  (baryon density)
- Ωm = 0.27±0.04 (Matter density
- One can derive the cold dark matter density
- 0.94 < ΩCDM h**2 **< 0.129 (95% CL) (Cold dark matter) – normalized Hubble Constant =0.71 ± 0.04
- Little or no hot dark matter

## Constraining Dark Matter Candidates

**mSUGRA   A****0****=0 ,**

- Ellis et al.,
- hep-ph/0303043

- Forbidden
- LSP = stau

**“****co-annihilation region”**

**“****bulk region”**

- 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; tan;   - Higgsino mass parameter)

**Co-annihilation region**

**Bulk region**

**Focus point region**

## Investigating DM at the LHC

- SUSY Discovery phase (inclusive searches) success assumed!
- Inclusive Studies (comparison of significance in inclusive channels etc).
- First rough predictions of h2 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 (h2, p, sun etc.)
- Less model-dependent interpretation.
- Approach to model-independent measurement of h2 etc. through measurement of all relevant masses etc.

- SUSY studies at the ATLAS/LHC will proceed in four steps:

## First Step - Inclusive  Constraints

- 5 reach of the inclusive SUSY searches  at ATLAS for mSUGRA with large tan   probing regions inaccessible to the  current  DM expts

**M****0**** (GeV)**

**jets+E****T****miss****+X**
**channel in ATLAS**

- The next  direct DM searches (~1tonne) could  probe cosmologically favoured regions (~10-10 pb) not accessible to the LHC: 1) Focus point scenarios (large m0); 2) models with large tan().

**Direct **
**Detection**

**ATLAS **
**constraints**

**WIMP-N **
** ****x-section (pb).**

-  Dan Tovey

-  Dan Tovey

## Step 2 Inclusive Studies

- 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 < 1 s (<< 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)

**Non-pointing**
**photons from ********0****1********G******

**GMSB Point 1b**
**(Physics TDR)**

**ATLAS**

**LHC Point 5**
**(Physics TDR)**

**R-Parity **
**Conserved**

**R-Parity **
**Violated**

**ATLAS**

## 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(), sign(), A0 in CMSSM): Stage 2/3.
- Check consistency with accelerator constraints (mh,       g-2, bs etc.)
- Estimate h2 consistency check with astrophysics         (WMAP etc.)
- Ultimate test of DM at LHC _only possible_ in conjunction with astroparticle experiments
-   measure m , p, sunetc.

## 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, M**1/2**                               & Tan ****are ± 2.3%, ± 0.9% and 0.5% respectively

## 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**

## Step 34 Relic Density Scenarios

- Step 34 Relic Density Scenarios

- Use parameter measurements to estimate h2 , direct detection cross-section etc. (e.g. for 300 fb**-1**, SPS1a)
-  **********h****2**** = 0.1921 ******** 0.0053 &   log****10****(************p****/pb) = - 8.17 ******** 0.04**

## 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,E****R****) ~ exp(-E****R****/E****0****r) for recoil energy E****R****,**
**I(A) = spin/coherence enhancement (model-dep.),**
**F****2****(A,E****R****) = nuclear form-factor,**
**g(A) = quenching factor (E****v****/E****R****),**
******(E****v****)= event identification efficiency.**

## Direct DM Searches 

- 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)

## 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 ’s produced by neutralino annihilation in the sun’s/earth’s core. These ’s detected via CC interactions (*ν *** *μ *conv’s) in -telescopes such as AMANDA.
**The planned neutrino telescopes ANTARES & IceCube  are sensitive to *****E******μ****** > *****10 GeV &  *****E******μ****** > *****25–50 GeV, respect. **
- The 2nd signal stems from -rays originating from neutralino annihilations in the galactic core & halo producing  hadrons, giving rise to ’s primarily from **0 decays.
**These signals can be detected by space- based detectors such as EGRET  or GLAST  with thresholds as low as 100’s 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.

## Putting it All Together

**The black contour depicts the exclusion that we can expect from the planned future direct detection (DD) dark matter experiments (*****σ*****SI**** *****> *****10****-9**** pb).**

**The LHC (100 fb****-1****) can cover the HB/FP region up to m****1/2**** ∼ 700 GeV, which corresponds   to a reach in m****gluino**** 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/km****2****/yr and E****μ**** > 25**
**covering the FP region to 1400GeV**

**The S/B > 0.01 contour for halo produced  positrons (blue-green contour) and**

**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.**

## 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 *M*W/*M*Pl ~ 1016
- Current scenarios favour a long lifetime for the WIMP (~1 year) -  A year passes...then all WIMPs decay to gravitinos
- Are there observable consequences? Well late decays, ****̃* *→ ***** G̃* can modify light element abundances
- Independent 7Li measurements are all low by factor of 3 - SuperWIMP DM naturally explains 7Li !

*M*Pl2/*M*W3 ~ year

## Collider Phenomenology

- Each SUSY event produces 2 metastable sleptons with a  spectacular signature: highly-ionizing charged tracks
- Current bound (LEP): *m* *l**̃* > 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  *m**G*̃
- G̃. SuperWIMP contribution to dark matter
-  SUSY breaking scale
-  Early universe (BBN, CMB) in the lab

## 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 TeV+Planck  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

**(****3+1+n ) dimensions**

**(3+1) dimensions**

**Often assume that EDs have a common size R**

## 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

**N=2********7**

**~80 pb****-1**

## Astrophysical/Cosmological Limits on EDs

- 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 *M****D**** ~1*TeV,  *n **** *4.
- If extra dimensions are discovered at the LHC it would provide useful input to our understanding of astrophysics/cosmology.

**SN cooling**
**via graviton**
**emission**

**Anomalous heating of neutron stars by **
**gravitionally trapped KK graviton modes**

**Radiative decay of gravitons to ********’s, **
**contribute to the**
**diffuse ******** back-grounds **

## Extra Dimensions & the Radion

- 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.   << 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 > M > 10-3 eV) that is a potential source of dark matter similar to axionic dark matter

## Searching for the Radion at ATLAS

- (For 100 fb**-1** of data)

## Black Hole Production at the LHC

- Big surprise: BH production is not an exotic remote possibility, but the dominant effect! (Limitation:lack of knowledge of quantum gravity effects )

- Main idea: when the E**cm** reaches the                                                                                                                                                          fundamental  “Planck”scale, a BH is formed;                                                               x-section is given by the black disk;                                                                          σ ~ πR**S****2** ~ 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

## Black Holes in ATLAS

- 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  5**** 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

** ****M****BH**** ~ 8 TeV **

- Preliminary studies : reach is MD ~ 6 TeV for any  in one year at low luminosity.

- By testing Hawking formula  proof that it  is BH  +  measure of  MD, 
- Precise measurements of MBH & TH needed (TH from lepton & **** spectra)

## Black Hole Production by Cosmic Rays

**(Feng and Shapere, hep-ph/0109106)**

- 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?

**PAO limit (96% CL)**

**hep-ph/0311365**

**n****D****=6**

**Notes:**
Black holes can also be produced in the interactions of UHE cosmic  neutrinos in the atmosphere. As you can see the cross-section for such a process is much enhanced wrt the SM process of neutrino-nucleon scattering. 
In order to overcome the background from conventional cosmic ray air showers one searches for quasi horizontal air showers that to first order can only arise from neutrino interactions in the atmosphere.
Such cosmic ray black hole events should be seen by for example PAO and AGASSA. In fact of the order of 100 BH events might be detected by the PAo before the LHC turns on.
As CR experiments are flux and not energy limited the effect of inesalsticity is les than that at the LHC, reducing rates by a factor of ten rather than a thousand.
The question is can a black hole signature be uniquely established,.

## COSMOLHC – the Direct Detection 

- COSMOLHC – the Direct Detection
- of Cosmic Rays with LHC Detectors

## 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

**Notes:**
The LHC detectors will deploy unprecedented areas, around 5500m2,  of precision muon tracking and calorimetry roughly 100m underground. Such systems would not normally be deployed solely for cosmic ray studies.
In the spirit of Cosmo Lep the LHC detectors could be used to directly measure cosmic rays underground.
Here you can see the L3 detector the L3 experiment at LEP was one of the leading proponents of such studies and even proposed a surface array to work in conjunction with the underground detector

## Muon Physics Plus  with CosmoLHC

- CosmoLHC – carrying on CosmoLEP (L3+C, CosmoALEPH). Topics to study:
- Single/inclusive ’s (pt spectrum >20 GeV 2TeV, angular dist. 0  <  < 50o, charge ratio, etc.)
- Upward going ’s (E spectrum, angular distribution, etc.)
- Multi-’s (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 (M> 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)

**Single muon data**

- A muon “bundle” event

**L3+C**

**L3+C**

## 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 **** measure m**** , ****************p******,****, ****sun****etc. *
- The nature of discovery physics is that it often occurs when it is least expected   astrocollider physics maximizes the coverage of “possibility space”

## Extra SLIDES

## ATLAS

- Scale

- 25m

- 46m

**Weight 7K  tonnes**

## LHC- Direct Search for Monopoles  

- 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 plastic’s “ionization damage” zones
- Threshold Z/b > ~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**

**Detection medium, plastic **
**track-etch detectors (CR39)**

- (plastic ball)

## Indirect Search for Monopoles/Dyons

- ATLAS, 100 fb-1

- Also searched in cosmic rays

- Caveat: there  will be large form factor suppression in the cross-section if the monopole is not point-like

## The Mysteries of an Opaque Universe

- The universe is opaque to UHECR
- In the case of the GZK cut-off  a 5x10**19** 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 > E**GZK**                              getting to us?  There are two scenarios:
- BOTTOM UP: acceleration in AGNs, ****-ray                           bursters, etc. Then production of a neutral (n, s**o**,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.

**10,000Mpc**

- Size of observable universe

**Region restricted**
**by GZK cut-off **
**~100 Mpc**

## Cosmic Ray Exotica  

- 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**
**P****T**** of produced particles higher than “normal” **
**P****T**** ~1.7 GeV/c for centauros**
**P****T****  of 10-15 GeV/c for chirons**
**Pseudorapidity distributions consistent with formation and isotropic decay of a fireball with:**
**N****h**** ~100 & M****FB**** for centauros and chirons**
**N****h**** ~15 and M****FB**** ~ 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.  P****T****)– 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 P****T**

**A Centauro Model**

**Does the production of**
**strangelets play a role**
**in Centauro-type **
**phenomena?**

## Focus Point Region

- Relic density can also be reduced if  has significant Higgsino component to enhance

- Feng, Matchev, Wilczek (2000)

- Baer, Belyaev, Krupovnickas, Tata (2003)

- Motivates SUSY with multi-TeV *g*̃, *q*̃, *l* ̃ ±/0 highly degenerate
- Such SUSY would be missed at LHC, discovered at LC

- James Pinfold  Fermilab June 2005

## DM Detectors (as of summer 2004)

- DAMA (Gran Sasso)
**9x9.7 kg crystals in shield: 7 years data analysed**
**Annual variation observed in *****total *****event rate < 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**

- 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)
**R&D 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**

## Slide 49

- Colour Sextet Quark Model - Notes

- Dfirectly rom Mike Albrow’s talk - “GTEV Gluon Physics at the Tevatron”