1. Wednesday Summary of Working Group I
Initial questions I:
LHC LUMI 2005; ; Arcidosso
Oliver Brüning 1

2. Wednesday Summary of Working Group I
Initial questions II:
LHC LUMI 2005; ; Arcidosso
Oliver Brüning 2

3. Wednesday Summary of Working Group I
main points from Tanaji Sen’s presentation I:
-peak power deposition inside the triplet magnets is a factor
3 to 4 above the quench limit of the triplet magnets 
any IR upgrade scenario requires an upgrade of the TAS
absorber  TAS length and material?
-peak power deposition inside the triplet magnets leaves a
safety factor 4 for the quench limit (including 3mm orbit
errors) for nominal operation  how does the peak power
deposition inside the triplet magnets scale with the orbit
tolerances and how much can we increase the safety factor
for the peak power deposition wih reduced tolerances on the
closed orbit errors?
LHC LUMI 2005; ; Arcidosso
Oliver Brüning 3

4. Wednesday Summary of Working Group I
main points from Tanaji Sen’s presentation II:
-two options for dealing with the increased heat load inside
the triplet magnets:
1) construct more robust triplet magnets that can tolerate
the increased peak heat load:
how does the quench limit of different super conducting
materials vary and are there SC materials that provide higher
tolerances on the peak power deposition inside the magnets?
LHC LUMI 2005; ; Arcidosso
Oliver Brüning 4

5. Wednesday Summary of Working Group I
main points from Tanaji Sen’s presentation III:
-two options for dealing with the increased heat load inside
the triplet magnets:
2) reduce the peak heat load with an upgrade of the TAS
absorber:
how does the peak power deposition scale with the magnetic
field strength and aperture of the magnets?
magnetic TAS: requires integrated field of 10 Tm <-> 20 Tm
LHC LUMI 2005; ; Arcidosso
Oliver Brüning 5

6. Wednesday Summary of Working Group I
main points from Tanaji Sen’s presentation IV:
-peak power deposition inside the triplet magnets depends
on the material of the vacuum chamber
on the orbit tolerances  scaling?
LHC LUMI 2005; ; Arcidosso
Oliver Brüning 6

7. Inner Triplet - baseline
Azimuthally averaged power density isocontours (mW/g) in the inner
triplet of IR5

8. Peak power density - baseline
Peak power density in the first 2 radial bins for the baseline beam tube
in Q1 and an alternative thinner tube.

9. Wednesday Summary of Working Group I
main points from Peter McIntyres’s presentation I:
-power density deposited inside the triplet magnets reduces
with L* if the triplet aperture is kept constant  move triplet
magnets closer to the IP (scaling of losses with magnet field?)
-power deposition inside the triplet magnets increases with
L* with one assumes the magnet diameter is proportional
to L*  move the triplet magnets further away from the IP
-discussion showed that it is still a good idea to reduce L*
but assumption of constant aperture must be revised
LHC LUMI 2005; ; Arcidosso
Oliver Brüning 9

10. Wednesday Summary of Working Group I
main points from Fabrizio Palla’s presentation I:
-CMS detector might offer potential magnet locations for
L* = 14 m with radial space of +/- 0.5 m (currently occupied
by TOTEM and CASTOR)
-ECAL installation is region of high radiation (L* = 3 m)
-evaluate pro & con of a fixed installation (compatibility with
access and vacuum bake out) and a movable installation
(tolerances for magnet and detector movements)
LHC LUMI 2005; ; Arcidosso
Oliver Brüning 10

11. Muon chambers
Need better shielding of YE/4 (likely to be done before SLHC proper)
Need better shielding for ME/1

12. Wednesday Summary of Working Group I
main points from Fabrizio Palla’s presentation II:
-the situation for ATLAS is not as obvious (active area of the
detector extends beyond TAS absorber)  we might have
to look for different IR layout solutions for the two main
experiments
-the time required for an upgrade shut down must be balanced
against a gain in integrated luminotisy  see the talk by
Michael Bieler
LHC LUMI 2005; ; Arcidosso
Oliver Brüning 12

13. Wednesday Summary of Working Group I
main points from Michael Bieler’s presentation I:
-HERA luminosity upgrade features 6 new superconducting
magnets inside the detectors (2m and 3.7m long)
-main problems related to the new installation:
water condenses on the cold magnets and drips into the
detector
magnets are supported by steel cables and move by up
to 1mm during the ramp
BPMs in the IR regions were initially exposed to
synchtoron radiation
LHC LUMI 2005; ; Arcidosso
Oliver Brüning 13

14. Wednesday Summary of Working Group I
main points from Michael Bieler’s presentation II:
-commissioning time for the HERA luminosity upgrade
of 1.5 years to 2 years
 the LHC IR upgrade must be robust in order to allow
a fast commissioning time!
LHC LUMI 2005; ; Arcidosso
Oliver Brüning 14

15. ZEUS Detektor p e Zentrale Driftkammer Mikrovertex-Detektor CTD
Vorwärts-Kalorimeter
Rückwärts-Kalorimeter
Zentrales-Kalorimeter
Solenoid Magnet
Zentrale Driftkammer
CTD
Mikrovertex-Detektor

16. Wednesday Summary of Working Group I
-not all questions could be answered but interests and worries
have been communicated to all parties involved
-many new questions
-interest in scaling laws and concrete layout models for
comparative studies
-reduced L* is not excluded from the experiment (CMS)
point of view
-complicated IR designs that might imply a long
commissioning time!
LHC LUMI 2005; ; Arcidosso
Oliver Brüning 16