1. Ron Settles MPI-Munich
Tsinghua U. January Experience with LEP and its meaning for the Linear Collider
Ron Settles MPI-Munich
13/01/2008
Ron Settles MPI-Munich Tsinghua Jan. 2010

2. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Outline of talks
1 What physics do we want to do, where?
2 What is the best detector?
3 The LCTPC
4 Machine and global issues
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Ron Settles MPI-Munich Tsinghua Jan. 2010

3. Idea of talksdiscussions
Disclaimer: these are personal views and cannot be exhaustive (e.g., there were 81 astro-ph, 9 hep-ex, 53 hep-ph papers the final week of Dec2009 at
There will be some overlap in these talks and with the ones at the TPC school 2007.
For much more complete review of physics and collider options, see website for LHC2FC March 2009 (more details below).
Here LEP/TevatronILC/CLIC opinions are based on ALEPH experience and LC studies.
Feel free to interrupt, make comments and/or corrections…
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Ron Settles MPI-Munich Tsinghua Jan. 2010

4. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Talk #1
What physics do we want to do, where?
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Ron Settles MPI-Munich Tsinghua Jan. 2010

5. International Linear Collider
Where?: ITRP decision 2004: COLD superconducting à la TESLA chosen
International Linear Collider
Baseline:
200 GeV < √s < 500 GeV
Integrated luminosity ~ 500 fb in 4 years
80 % e- beam polarisation
Upgrade to 1TeV, L = 1 ab-1 in 3 years
2 interaction regions
Concurrent running with the LHC from ~2018 !!
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Ron Settles MPI-Munich Tsinghua Jan. 2010

6. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
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Ron Settles MPI-Munich Tsinghua Jan. 2010

7. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Physics we want to do?
For example, from my talk at Arlington WS Jan.2003:
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Ron Settles MPI-Munich Tsinghua Jan. 2010

8. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Need highest luminosity
Precision for 1 ab-1 :
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Ron Settles MPI-Munich Tsinghua Jan. 2010

9. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
10-3
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Ron Settles MPI-Munich Tsinghua Jan. 2010

10. Supersymmetry 1 TeV DIRECT ... AND solves several SM problems:
Energy in GeV
with Supersymmetry
without Supersymmetry
1 TeV
... AND solves several SM problems:
Link to gravity
lightest SUSY particle stable
 Dark matter candidate
Solves fine tuning problems
Predicts light Higgs
Unification of forces
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Ron Settles MPI-Munich Tsinghua Jan. 2010

11. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
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Ron Settles MPI-Munich Tsinghua Jan. 2010

12. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
“Loop corrections” and precision measurements make the ILC sensitive to physics way beyond the c.m. energy of the machine…
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Ron Settles MPI-Munich Tsinghua Jan. 2010

13. …will come back to this in talk#4…
‘Susy’,’New Physics’
stand for
“Susy and/or New Physics or Nothing (depending on what is found at Tevatron and LHC)”
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Ron Settles MPI-Munich Tsinghua Jan. 2010

14. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
INDIRECT
The value of precision…
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Ron Settles MPI-Munich Tsinghua Jan. 2010

15. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Snapshot of the CMB(& polariz.) y after the big bang, when universe became transparent
power spectrum/ multipole expansion
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Ron Settles MPI-Munich Tsinghua Jan. 2010

16. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Power spectrum  BAO
related by Fourier transform
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Ron Settles MPI-Munich Tsinghua Jan. 2010

17. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
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Ron Settles MPI-Munich Tsinghua Jan. 2010

18. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
We also have a chance to understandthis…
…understand the composition of our universe:
NB. Not only WMAP data going into this ΛCDM model.
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Ron Settles MPI-Munich Tsinghua Jan. 2010

19. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
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Ron Settles MPI-Munich Tsinghua Jan. 2010

20. DE may be a fata morgana…
Time runs more slowly in the filaments than in the voids.
Taking this into account (Leith et al, Astrophy.J.672,L91-L94,2008), is ‘dark energy’
a fata morgana?
75% Dark matter
25%
Baryons
…but there
are MANY
models for
DE…
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Ron Settles MPI-Munich Tsinghua Jan. 2010

21. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
…there are MANY models for DE and the cosmos…
…for example…
w = pressure/density = P / ρ
w < phantom energy
w = cosmological constant
w = -2/3 topological defects
w = -1/3 quintenssence, strings
w = dust, baryonic material,
cold dark matter
6. w = +1/3 photons
7. w = + 1 ………………
DE,
acceleration
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Ron Settles MPI-Munich Tsinghua Jan. 2010

22. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
…and everybody is hungry for data…
…for example,
one experimental paper with two events:
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Ron Settles MPI-Munich Tsinghua Jan. 2010

23. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
…hungry for data…
…has generated many phenomenology papers…
-arXiv:
-arXiv:
-arXiv:
-arXiv:
-arXiv:
-arXiv: …
… to name a few…
WIMPS ‘just around the corner’??
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Ron Settles MPI-Munich Tsinghua Jan. 2010

24. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Back to colliders…
Why do we think these indirect, precision meas. will tell us anything??? The that’s why!
CERN Courier, Nov 2005:
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Ron Settles MPI-Munich Tsinghua Jan. 2010

25. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Electroweak combinations:
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Ron Settles MPI-Munich Tsinghua Jan. 2010

26. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Where are we with the Higgs? CERN Courier, Nov 2005
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Ron Settles MPI-Munich Tsinghua Jan. 2010

27. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Electroweak combinations 2007:
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Ron Settles MPI-Munich Tsinghua Jan. 2010

28. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Compare with electroweak combinations 2009   
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Ron Settles MPI-Munich Tsinghua Jan. 2010

29. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Electroweak combinations: slow progress, but still inching forward
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Ron Settles MPI-Munich Tsinghua Jan. 2010

30. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Electroweak combinations: slow progress, but still inching forward
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Ron Settles MPI-Munich Tsinghua Jan. 2010

31. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
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Ron Settles MPI-Munich Tsinghua Jan. 2010

32. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
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Ron Settles MPI-Munich Tsinghua Jan. 2010

33. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
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Ron Settles MPI-Munich Tsinghua Jan. 2010

34. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
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Ron Settles MPI-Munich Tsinghua Jan. 2010

35. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Compare with electroweak with cmssm combo   
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Ron Settles MPI-Munich Tsinghua Jan. 2010

36. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Compare electroweak with cmssm combo   
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Ron Settles MPI-Munich Tsinghua Jan. 2010

37. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Well,
I don’t know what to say more about the Higgs, except…
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Ron Settles MPI-Munich Tsinghua Jan. 2010

38. …except that in addition we have LEP events…
Expt
(GeV)
Decay Channel
(GeV/c2)
ln(1+s/b)
115 GeV/c2 1
ALEPH
206.7
4-jet
114.3
1.73 2
112.9
1.21 3
206.5
110.0
0.64 4 L3
206.4
E-miss
115.0
0.53 5
OPAL
206.6
110.7 6
Delphi
0.49 7
205.0
Lept
118.1
0.47 8
208.1
Tau
115.4
0.41 9
114.5
0.40 10
205.4
112.6
…the Higgs?
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Ron Settles MPI-Munich Tsinghua Jan. 2010

39. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
“Experience with LEP and its meaning for the Linear Collider” OF COURSE, the number of physics scenarios is much larger than I have shown in these few slides, and these are being addressed in one WS after another 
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Ron Settles MPI-Munich Tsinghua Jan. 2010

40. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
LCs
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Ron Settles MPI-Munich Tsinghua Jan. 2010

41. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
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Ron Settles MPI-Munich Tsinghua Jan. 2010

42. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
For many more, see
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Ron Settles MPI-Munich Tsinghua Jan. 2010

43. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
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Ron Settles MPI-Munich Tsinghua Jan. 2010

44. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
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Ron Settles MPI-Munich Tsinghua Jan. 2010

45. Ron Settles MPI-Munich 1.Tsinghua Jan. 2010
Conclusion?
No conclusion…
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Ron Settles MPI-Munich Tsinghua Jan. 2010

46. Next talk: the detector
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Ron Settles MPI-Munich Tsinghua Jan. 2010