1 / 61

Achille Stocchi LAL (Université Paris-Sud / IN2P3)

Super-B Projects. mainly the Physics Program. Achille Stocchi LAL (Université Paris-Sud / IN2P3). Indirect Searches for New Physics at the time of LHC – Conference 22th-24th March 2010. Next generation of Super asymmetric B factory ≡

gelsey
Download Presentation

Achille Stocchi LAL (Université Paris-Sud / IN2P3)

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Super-B Projects mainly the Physics Program Achille Stocchi LAL (Université Paris-Sud / IN2P3) Indirect Searches for New Physics at the time of LHC – Conference 22th-24th March 2010

  2. Next generation of Super asymmetric B factory ≡ L= 1036 cm-2 s-1, >100 times the one of the present B-factory Only way to meet the luminosity requirement is the « italian crab scheme » The « Japanese » machine is converging to this solution SuperB The TDR phase of the project has been approuved (6MEuros/year) Aim for project approuval (during this phase) by 2010 SuperKEKB KEK authorized to use a part of its operating money to start building a damping ring. Equivalent usage of « KEKB upgrade » or « SuperKEKB project » Aim for approuval in 2010.

  3. 25’ Physics Program Why ? The Machine 10’ How ? The Detector

  4. In this seminar I discuss PHYSICS : the Physics Program for a machine with L= 1036 cm-2 s-1 running 5 years. MACHINE : the new collision schemes which make L= 1036 cm-2 s-1 possible. DETECTOR : not included in this talk both collaborations have ambitious detector solutions inspired by Belle/Babar detector experiences

  5. Physics Program (still under construction..) A discovery machine in the LHC era

  6. Beyond the Standard Model with flavour physics The indirect searches look for “New Physics” through virtual effects from new particles in loop corrections 1 ~1970 charm quark from FCNC and GIM-mechanism K0 mm ~1973 3rd generation from CP violation in kaon (eK) KM-mechanism ~1990 heavy top from B oscillations DmB ~2000 success of the description of FCNC and CPV in SM 2 3 4 “Discoveries” and construction of the SM Lagrangian SM FCNCs and CP-violating (CPV) processes occur at the loop level SM quark Flavour Violation (FV) and CPV are governed by weak interactions and are suppressed by mixing angles. SM quark CPV comes from a single sources ( if we neglect q QCD ) New Physics does not necessarily share the SM behaviour of FV and CPV

  7. 4 The test of the SM (in fermion sector) ..Or the « not discovery » of any new physics beyond the SM ~1990-now  a huge number of precise measurements Coherent picture of FCNC and CPV processes in SM Discovery : absence of New Particles up to the ~2×Electroweak Scale !

  8. The problem of particle physics today is : where is the NP scale L ~ 0.5, 1…1016 TeV t t H H t H H t LHC will search on this range The quantum stabilization of the Electroweak Scale suggests that L~ 1TeV Those are arguments of fine tuning…if the NP scale is at 2-3..10 TeV …naturalness is not at loss yet…

  9. Present and future goals of Flavour Physics It is a game of couplings and scales • if NP particles are discovered at LHC we have to be able to study the flavour structure of the NP • (“reconstructing” the NP Lagrangian) • to have the capability to explore NP scale beyond • the LHC reach

  10. Which NP will be ?? Which NP will be ?? Which NP will be ?? Which NP will be ?? Which NP will be ?? Which NP will be ?? Which NP will be ?? Which NP will be ?? Which NP will be ?? The actors in the next decade The actors in the next decade The actors in the next decade The actors in the next decade The actors in the next decade The actors in the next decade The actors in the next decade The actors in the next decade The actors in the next decade Br (Bs mm) Br (Bs mm) Br (Bs mm) Br (Bs mm) Br (Bs mm) Br (Bs mm) Br (Bs mm) Br (Bs mm) Br (Bs mm) Br,ACP (B Xs l l) Br,ACP (B Xs l l) Br,ACP (B Xs l l) Br,ACP (B Xs l l) Br,ACP (B Xs l l) Br,ACP (B Xs l l) Br,ACP (B Xs l l) Br,ACP (B Xs l l) Br,ACP (B Xs l l) Br (B Xsg) Br (B Xsg) Br (B Xsg) Br (B Xsg) Br (B Xsg) Br (B Xsg) Br (B Xsg) Br (B Xsg) Br (B Xsg) NMFV (1-3) NMFV (1-3) NMFV (1-3) NMFV (1-3) NMFV (1-3) NMFV (1-3) NMFV (1-3) NMFV (1-3) NMFV (1-3) MFV MFV MFV MFV MFV MFV MFV MFV MFV Br (K0 p0nn) Br (K0 p0nn) Br (K0 p0nn) Br (K0 p0nn) Br (K0 p0nn) Br (K0 p0nn) Br (K0 p0nn) Br (K0 p0nn) Br (K0 p0nn) b b b b b b b b b MFV-GUT MFV-GUT MFV-GUT MFV-GUT MFV-GUT MFV-GUT MFV-GUT MFV-GUT MFV-GUT Br (m e g) Br (m e g) Br (m e g) Br (m e g) Br (m e g) Br (m e g) Br (m e g) Br (m e g) Br (m e g) Br (B tn , mu) Br (B tn , mu) Br (B tn , mu) Br (B tn , mu) Br (B tn , mu) Br (B tn , mu) Br (B tn , mu) Br (B tn , mu) Br (B tn , mu) RH-currents RH-currents RH-currents RH-currents RH-currents RH-currents RH-currents RH-currents RH-currents NMFV (2-3) NMFV (2-3) NMFV (2-3) NMFV (2-3) NMFV (2-3) NMFV (2-3) NMFV (2-3) NMFV (2-3) NMFV (2-3) (g - 2)m (g - 2)m (g - 2)m (g - 2)m (g - 2)m (g - 2)m (g - 2)m (g - 2)m (g - 2)m Br (K+ p+nn) Br (K+ p+nn) Br (K+ p+nn) Br (K+ p+nn) Br (K+ p+nn) Br (K+ p+nn) Br (K+ p+nn) Br (K+ p+nn) Br (K+ p+nn) H+ - high tanb H+ - high tanb H+ - high tanb H+ - high tanb H+ - high tanb H+ - high tanb H+ - high tanb H+ - high tanb H+ - high tanb Br (t  mmm) Br (t  mmm) Br (t  mmm) Br (t  mmm) Br (t  mmm) Br (t  mmm) Br (t  mmm) Br (t  mmm) Br (t  mmm) Br (B K nn) Br (B K nn) Br (B K nn) Br (B K nn) Br (B K nn) Br (B K nn) Br (B K nn) Br (B K nn) Br (B K nn) ACP (B Xsg) ACP (B Xsg) ACP (B Xsg) ACP (B Xsg) ACP (B Xsg) ACP (B Xsg) ACP (B Xsg) ACP (B Xsg) ACP (B Xsg) Z penguins Z penguins Z penguins Z penguins Z penguins Z penguins Z penguins Z penguins Z penguins LHT Models LHT Models LHT Models LHT Models LHT Models LHT Models LHT Models LHT Models LHT Models Br (B KSp0g) Br (B KSp0g) Br (B KSp0g) Br (B KSp0g) Br (B KSp0g) Br (B KSp0g) Br (B KSp0g) Br (B KSp0g) Br (B KSp0g) Br (t  mg) Br (t  mg) Br (t  mg) Br (t  mg) Br (t  mg) Br (t  mg) Br (t  mg) Br (t  mg) Br (t  mg) ACP(BsJ/ y f) ACP(BsJ/ y f) ACP(BsJ/ y f) ACP(BsJ/ y f) ACP(BsJ/ y f) ACP(BsJ/ y f) ACP(BsJ/ y f) ACP(BsJ/ y f) ACP(BsJ/ y f) Many of these channels could be studied by SuperB

  11. L= 1034 cm-2 s-1 150 fb-1 1.5 ×108 (4s) produced by year L= 1036 cm-2 s-1 15 ab-1 1.5 ×1010 (4s) produced by year B factories have shown that a variety of measurements can be performed in the clean environment. Asymmetric B factory The systematic errors are very rarely irreducible and can almost on all cases be controlled with control samples. (up to..50-100ab-1) High luminosity Many and interesting measurements at different energies (charm/t threshold, U(5S), other Upsilons.. ) and with polarised beam Flavour factories SuperB factory potential discovery evaluated with 75ab-1

  12. Variety of measurements for any observable B physics @ Y(4S) Possible also at LHCb Similar precision at LHCb Example of « SuperB specifics » inclusive in addition to exclusive analyses channels with p0, g’s, n, many Ks…

  13. Charm at Y(4S) and threshold t physics (polarized beams) To be evaluated at LHCb Bs at Y(5S) Bs : Definitively better at LHCb

  14. The Quantum path The indirect searches look for “New Physics” through virtual effects from new particles in loop corrections I’ll show Examples of golden measurements for possible discoveries Key words : Precise measurements  Luminosity 5

  15. Determination of CKM parameters and New Physics 1 Future (SuperB) + Lattice improvements Today This situation will be different @2015 thanks to LHCb players are : g,a,b..,Vub and Lattice ! r = 0.163 ± 0.028 h = 0.344± 0.016 r = ± 0.0028 h = ± 0.0024 Improving CKM is crucial to look for NP Important also in K physics : K p n n , CKM errors dominated the error budget

  16. 2 Leptonic decay B  l n SuperB SuperB -75ab-1 MH~1.2-2.5 TeV for tanb~30-60 MSSM 2HDM-II 75ab-1 2ab-1 LEP mH>79.3 GeV SuperB ATLAS 30fb−1 SuperB excludes SuperB excludes B-factories exclude B-factories exclude ATLAS 30fb−1 ATLAS 30fb−1

  17. MSSM+generic soft SUSY breaking terms 3 New Physics contribution (2-3 families) • Flavour-changing NP effects in the squark propagator • NP scale SUSY mass • flavour-violating coupling ~ g ~ ~ s b s b In the red regions the d are measured with a significance >3s away from zero 1 10-1 10-2 Here the players are : = (0.026 ± 0.005) • (BXs) • (BXsl+l) • ACP(BXs) Arg(d23)LR=(44.5± 2.6)o 1 10 1 TeV

  18. 4 Lepton Flavour Violation in t decays MEG sensitivity meg ~10-13 Preliminary results < 3 10-11 Masurements and origin of LFV Discrimination between SUSY and LHT SO(10) MSSM 107 BR (tmg) LFV from PMNS SuperB LFV from CKM The ratio t lll / t mg is not suppressed in LHT by ae as in MSSM M1/2

  19. 5 CP Violation in charm NOW To be evaluated at LHCb CPV in D system negligible in SM SuperB CPV in D sector is a clear indication of New Physics !

  20. Part of the program could be accomplished if SM theoretical predictions are @ 1% Shown by Vittorio Lubicz at the SuperB Workshop LNF Dec2009 [2011 LHCb] [2009] [2015 SuperB] The expected accuracy has been reached! (except for Vub)

  21. The Machine How it is possible to gain a factor 100 in the luminosity ..? 1034 cm2sec-1  1036 cm2sec-1

  22. σy(z) z Doing that we also meet another condition Lumiy<Lumiy “Hourglass effect” Focalizations with σy<σy If σytoo small w.r.t σz : particle density drops so fast, away from the IP, that Luminosity is in fact reduced. The stronger the focalization, the quicker the de-focalzation ! “The Crab waist scheme” To have large luminosity 1) Single passage : D (disruption) high [profit of beam-beam effects (pinch)] small sx,sy 2) The beam has to be re-utilized in an accumulation ring  to maxime frD “small” 3)To keep D small and small sx,sy we also needsmall sz Crossing angle interaction

  23. And now we need to… Crab the Waist Crossing angle between e+ and e- : bunch overlap length no longerσz, but σx/θ<< σz ! But: Charge density, thus the forces, felt by e+/e- in the crossing region depends on x, y & z simultaneously ! Waist (focalisation) on y z2: another e+ vertical focalisation  another density  another Force z1: one e+ vertical focalisation  a charge density  a force Force depends on x & z or y & z -Coupling between the x, y and z components of the e+/e- trajectories oscillations around the collider In the machine language : Additional betatron-betatron / synchro-betatron resonances

  24. x …and (finally) to crab the waist: sY e- e+ 2Sx/q q 2Sz*q z 2Sz 2Sx Vertical waist has to be a function of x: Crabbed waist realized with a sextupole (in phase with the IP in X and at p/2 in Y slight luminosity increase) Conceptually simple : restore the B-B effects to those we have quadrupoles focalizing in 2D (compensate the effects of the crossing angle)

  25. Example of resonance suppression Much higher luminosity! Crab Waist On: 1. large Piwinski angleF >> 1 2.bycomparable withsx/q Typical case (KEKB, DAFNE): 1. low Piwinski angleF< 1 2.bycomparable withsz

  26. Bhabha Calorimeters gamma monitor Quadrupoles Y-tube QD0 Quadrupole to simulation… Sputnik Soyuz MIR MIR MIR Sputnik Soyuz QD0 Siddharta Detector and MIR shields Calorimeters Shields Test of these new colliding schemes in Frascati From design….

  27. Data averaged on a full day DAFNE Luminosity results by=9mm, Pw_angle=1.9 Luminosity [1028 cm-2 s-1] by=18mm, Pw_angle=0.6 by=25mm, Pw_angle=0.3 Results match the simulation expectations

  28. 1523 1002 4.53E+32 Results of these tests : new 3 years run @ Phi-factory (from May/June) Lpeak expected at about 5.5∙1032 cm-2s-1 Lint (0.5 fb-1/month)

  29. How to extrapolate the Dafne results to SuperB ? Synergy with ILC RINGS LER SR IP LER SR 66 mrad IP LER arc LER arc HER arc HER arc Rings crossing e+ e- RF

  30. SuperBResults of two year work. Parameters as at 18/3/2010 Different solutions to reach 1036 Tau/charm threshold running at 1035 • Baseline + • other 2 options: • Lower y-emittance • Higher currents • (twice bunches)

  31. Conclusions • SuperB (L>1036) is a discovery machine at the TeV scale • (unique player in the reconstruction of the NP Lagrangian) • Give also the opportunity of exploring NP scales of the several TeV • Part of the program could be accomplished if SM theoretical predictions are @ 1% (crucial role of Lattice Calculations) P H Y S I C S  Measurable effects (anyhow) if NP particles with masses at the TeV scale M A C H I N E Machine is challenging and based on new accelerating schemes : “crab waist” : luminosity > 1036 possible ! Success of Frascati tests has proven that they work ! D E T C T O R Detector largely inspired from Babar/Belle ones will be also largely improved

  32. BACKUP MATERIAL

  33. Backup Physics

  34. Let’s consider (reductively) the GOLDEN MATRIX for B physics X X X- CKM X X X X- CKM X The GOLDEN channel for the given scenario Not the GOLDEN channel for the given scenario, but can show experimentally measurable deviations from SM. X « SuperB specifics » inclusive analyses channels with p0, g, n, many Ks… In the following some examples of

  35. N+1 Br(B  K n n) – Z penguins and Right-Handed currents today h SM Only theo. errors e If these quantities are measured @ <~10% deviations from the SM can be observed ~[20-40] ab-1 are needed for observation>>50ab-1 for precise measurement

  36. Example of need of large statistics 10ab-1 75ab-1 Determination of Susy mass insertion parameter (d13)LL with 10 ab-1 and 75 ab-1 Importance of having very large sample >75ab-1

  37. Another example of sensitivity to NP : sin2b from “s Penguins”… W- s b f t s B0d s K0 d d ~ g  5 discovery possible (extrapolating from today) ~ ~ s b s b Many channels can be measured with DS~(0.01-0.04) bs penguin processes bd SuperB (*) theoretical limited

  38. Charm Physics Charm physics using the charm produced at U(4S) Consider that running 2 month at threshold we will collect 500 times the stat. of CLEO-C Charm physics at threshold 0.3 ab-1 Strong dynamics and CKM measurements @threshold(4GeV) x~1%, exclusive Vub ~ few % syst. error on g from Dalitz Model <1o D decay form factor and decay constant @ 1% Dalitz structure useful for g measurement D mixing Rare decays FCNC down to 10-8 Better studied using the high statistics collected at U(4S) @threshold(4GeV) CP Violation in mixing could now addressed

  39. Polarized beams Polarized beam is (SuperB specific) t anomalous moment (g-2) LFV analyses : novel additional handle on backgrounds The anomalous tau momentum influence both the angular distribution and the t polarization. Measure the Re(F2) and Im(F2) of the (g-2) from factor NP effects ~ 10-6 < Polarisation is -an important issue for LFV -opens the possibility of measuring (g-2) -electroweak physics (neutral current) Under study

  40. Electroweak physics at SuperB SuperB could add a measurement here

  41. New excitement on spectroscopy to complete the picture  to better studying the recently discovered particle (quantum numbers, branching fractions…) More data are needed :

  42. Backup Machine

  43. Frascati Site: Potential HER Synch Radiation Beam Lines LER HER

  44. DAFNE Luminosity and Tune Shifts

  45. Baseline IR Design Stable since October

  46. For the baseline QD0 and QF1 magnets we need to keep the ratio of the magnetic field strengths constant in order to maintain good field quality • We want the * values to remain constant to maintain luminosity How do we change the beam energies? • It should be straightforward to develop a procedure to perform an energy scan •  To go to the Tau-charm • region (Ecm ~4 GeV) we • will need to remove most if • not all of the permanent • magnets

  47. Polarisation • In a storage ring, particle spins naturally precess around the vertical fields of the arc dipoles, at a rate determined by the particle energy. • This means that vertical polarisation is naturally preserved, but longitudinal polarisation can be lost without preventive measures. • For SuperB, there are two options to maintain longitudinal polarisation in the beam at the IP: • Use solenoids opposite the IP, to rotate thespin by p around the longitudinal axis. • Use solenoids or vertical bends torotate between vertical and longitudinalspin before and after the IP. • Option 2 will probably work bestfor the multi-GeV SuperB rings,but more studies are needed. • With a source providing ~ 90%polarisation, it is expected that an average polarisation of 80% can be achieved for the e- beam. e+ polarisation would be an upgrade…

  48. Colliding bunches New Superconducting / permanent final focusing quads near the IP e- 2.6 A Nano-Beam SuperKEKB e+ 3.6 A Replace long dipoles with shorter ones (HER). Add / modify rf systems for higher currents. Redesign the HER arcs to reduce the emittance. Low emittance positrons to inject Low emittance gun New positron target / capture section Low emittance electrons to inject ~40 times gain in luminosity TiN coated beam pipe with antechambers

  49. QC1 magnets closer to IP Superconducting & permanent magnets 83 mrad Full crossing

  50. SuperKEKB Parameters as of Feb.15, 2010 Parameters presented at KEKB MAC Review Feb.15-17, 2010

More Related