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Lecture 11: FCNC and
โPenguinโ Diagrams
http://faculty.physics.tamu.edu/kamon/teaching/phys627/1
โPenguinโ Diagrams
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The goal of this lecture is to understand Flavor Changing NeutralCurrents (FCNCs) and its power in probing new physics.
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Goal
Charged & Neutral Currents
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B Mesons
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We focus on a rare decay of Bs today.
๐ฉ๐ เดฅ๐๐
๐ฉ๐๐ เดฅ๐๐
๐ฉ+ เดฅ๐๐
๐ฉ๐+ เดฅ๐๐
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Quark Mixing & CKM Matrix
Square of each matrix element ๐๐๐2
expresses transition probabilitybetween ๐ โ ๐ with W boson exchange.
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Feynman Diagram in Week Interaction
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๐๐พ
Propagator for W boson:
V-A Charged Current:
โ๐๐
2าง๐๐ฟ๐พ
๐๐๐+๐ ๐ฟ
โฒ
โ๐๐
2าง๐๐ฟ๐พ
๐๐๐+๐๐ฟ
Quark Mixing
๐พ๐1
21 โ ๐พ5
๐
๐
๐พโ
๐๐พ๐ฝ๐๐
Dimensionless coupling strength ๐๐พ for leptons ๐๐พ ร (CKM Factor) for quarks
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CC and FCNC for ๐ฉ๐ โ ๐๐๐ฒ๐ฒ
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CC for ๐ โ ๐ transition
FCNC for ๐ โ ๐ transition
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โPenguinโ Diagram
Note: those types of โloopโ diagrams are veryimportant to search effects beyond the standardmodel, because any undiscovered particles cancontribute in the loop as a virtual state !
Doesnโt look like penguin ?
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๐ฒ๐
เดฅ๐ฒ๐
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Other โPenguinโ Diagram in Kaon
เดฅ๐ฒ๐๐ ๐
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Deviation at 2.4๐ - 2.6๐ from the SM Compatible with other anomalies observed in
๐ โ ๐๐๐ transition โน ~4๐ tension with SM
Puzzle with Anomalies in B Decays
New contribution via ๐ โ ๐+๐โ?
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[Q] Convince yourself if the ratios should be unity. Why do we use R?
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Feynman Diagrams in the SM
[Q] Why do we use R?
Simone Bifani, Sebastien Descotes-Genon, Antonio Romero Vidal and Marie-Helene Schune,
โReview of Lepton Universality tests in B decaysโ, arXiv:1809.06229
๐น๐ฒ(โ) =
๐โ๐+
๐โ๐+
= (cancelling QCD corrections)
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Neutrinos in Weak Interaction
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Rich Neutrino Physics
3 neutrino flavors. More? Non-Zero masses. Why so
light? Mass hierarchy?Oscillations. Structure of
mixing angles?Non standard interactions? Cosmology?
Seesaw mechanism is a generic model used to understand the relative sizes of observed neutrino masses, of the order of eV, compared to those of quarks and charged leptons. RH neutrinos?
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Pauli (1930) Discovered by Cowan and Reines
using a nuclear reactor in 1958 Massless Neutrinos in the Standard
Model (โ60s): ๐ต๐ = ๐. ๐๐๐ ยฑ ๐. ๐๐๐(LEP 2006)
Evidence for neutrino mass from SuperK (1998) and SNO (2002)
First evidence that the โminimalโ Standard Model of particle physics is incomplete!
2002 Nobel to pioneers: Davis and Koshiba:
Neutrino Cosmology: o Can be a (hot) dark matter, but it
cannot be the dominant cold dark (non-relativistic) matter components.
o Prediction by the hot Big Bang agrees with observations (e.g., the power spectrum of Cosmic Microwave Background (CMB) anisotropies), which would fail dramatically without a Cosmic Neutrino Background (C๐B) with properties matching closely those predicted by the standard neutrino decoupling process (i.e., involving only weak interactions).
o ๐๐๐๐๐๐ = ฯ๐๐๐๐ โฒ ๐ ๐๐; ๐ต๐๐๐ โ ๐. ๐
o Matter-antimatter asymmetry?
Tiny Neutrinos, Huge Player
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Tiny masses, but a very big player in particle physics andcosmologyโฆ
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Neutrino Flavor Mixing
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๐๐๐๐๐๐
=
๐๐1 ๐๐2 ๐๐3๐๐1 ๐๐2 ๐๐3๐๐1 ๐๐2 ๐๐3
๐1๐2๐3
3 flavors of ๐ in SM
3 mass eigenstate of ๐
PMNS matrix(1962)
โข Pontecorvoโข Makiโข Makagawaโข Sakaga
Atmospheric & accelerator: ๐23~45
ยฐ
โ๐232~2 ร 10โ3 eV2
Interference:๐13~9
ยฐ
and ๐ฟ๐ถ๐= ??
Solar & reactor:๐12~34
ยฐ
โ๐122~8 ร 10โ5 eV2
3-flavor mixing describes (almost) all neutrino oscillation phenomena (3 mixing angles, 2 independent mass splittings, 1 CPV phase). And โmatter effectโ โฆ Neutrino oscillations change when in media in comparison to vacuum oscillations due to the scattering of neutrinos on matter constituents, electrons particularly. This can be easily described by introducing new effective matter mixing angles and squared mass-splittings.
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Neutrino Detections
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Bubble Chambers Emulsion Chambers IceCube
MINOS, NOvA T2KSuper-Kamiokande
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Feynman Diagrams for ๐ฉ๐ โ ๐๐
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[Q] What is inside the circle?
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๐ฉ๐ โ ๐๐ (Contโd)
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XX
[Q] Gluon doesnโt work. What else?
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๐ฉ๐ โ ๐๐ (Contโd)
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[Q] Phone doesnโt work. For bs. Any solution?
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๐ฉ๐ โ ๐๐ (Contโd)
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[Q] FCNC for ๐ โ ๐ transition?
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Standard Model FCNC for ๐ฉ๐ โ ๐๐
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m
m
๐ธ/๐
b
s
_
b
SM
๐
๐พโ
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Supersymmetric FCNC for ๐ฉ๐ โ ๐๐
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m
m
H/A0
b
s
_
c+~
t~
b
SUSY
tan๐ท๐/ cos๐ท
tan๐ท
โ tan๐ฝ ๐
2
Inquiry/classification on superymmetric diagram
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Power of ๐ฉ๐ โ ๐๐
This is one of interesting rare decays to test new physicssuch as SUSY:
Br(Bsmm)SM ~ 3 x 10-9
Br(Bsmm)SUSY ~ Br(Bsmm)SM x (10 ~ 1000)
Within the SM, we will not see any events even with 100 x 1012
collisions at the Tevatron.
In the SUSY models (large tanb), the decay can be enhanced by up to1,000.
But the SUSY particle masses are expected to be of orderof 1000 GeV. But the Bs mass is ~5 GeV.
How can one possibly test SUSY models using Bs mesondecays? This is a main topic of this lecture.
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Why ๐ฉ๐ โ ๐๐ ? [1990โs] LEP results on the measurements of couplings indicate
SUSY with two Higgs doublets gives a possibility of unification offundamental forces. This motivates me to work on a particular channel (โtrileptonโ) at theTevatron.
[1998] There were two SUSY/Higgs workshops at Fermilab toexplore a feasibility and a potential of discovery of Higgs andSUSY at the Tevatron. An importance of large tanb SUSYscenarios is highlighted. This motivated me to work on large tanb scenario of SUSY where tauleptons are the key in SUSY discovery.
[2002] The WMAP measurement of the dark matter content (23%)in the universe strongly indicates a few SUSY scenarios. One ofthem is a scenario at large tanb where one can explore at theTevatron using the Bsmm decays This is the beginning of TAMUโs PPC program.
[2013] Observation at the SM expectation.
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Teruki Kamon 25PPC 2017
CBS comedy โBig Bang Theoryโ
(Season 1 Episode 15)
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The poster was designed during lunch meetings โฆ
PPC 2007 and Big Bang Theory
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Rare ๐ฉ๐ Meson Decay
CKM matrix
b t
s t
Vtb โฆ transition between t and b
Vts โฆ transition between t and s
PLB 538 (2002) 121
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๐ฉ๐ โ ๐๐
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PLB 538 (2002) 121
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FCNC in ๐ฉ๐ โ ๐๐
Br(๐ฉ๐ โ ๐๐ )
2
+
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๐ฉ๐(๐ ) โ ๐๐ Candidate at CDF
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Run 198082 Event 8264441:- M(mm) = 5.375 GeV- ct = 236mm - pT(m
+) = 4.6 GeV- pT(m
-) = 2.4 GeV
m+m-
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1st Round Analysis
PRL 93 (2004) 032001
First 2-side 90%CL Limit
SM Expectation
PRL 93 (2004) 032001PRL 95 (2005) 221805 PRL 100 (2008) 101802PRL 107 (2011) 191801PRD 87 (2013) 072003
PLB 538 (2002) 121
170 pb-1 ~ 8.5 x 1012 collisions
2002 2013
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Data in Bs signal window
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We see an excess over the background-only expectation in the Bs signal region and have set the first two-sided bounds on BR(Bsโ m+m-)
A fit to the data, including all uncertainties, yields
Data in the B0 search window are consistent with background expectation, and the worldโs best limit is extracted:
Conclusion (2011)
81.19.0 108.1)(
-+-
-+ mmsBBR
89109.3)(106.4
--+- mmsBBR at 90% C.L.
..%)90(%9510)0.5(0.6)(90
LCatBBR --+ mm
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3/14: Approval โฆ postponed
6/09: Collaboration Review (I)
6/22: Collaboration Review (II)
6/30: Approved!
7/10: Submission to PRL!!
7/15: Fermilab-Today
7/26: PRL referee report
8/19: Re-submission
9/07: PRL referee report (II)
9/08: RE-Re-submission
9/09: Accepted by PRL!!!
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Results opened atEPS 2011
What we will seebeyond our horizon ?
Stay tuned !
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2011.07.13
PRL 107 (2011) 191802
PRL 107 (2011) 191801
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CDF
CMS
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CMS Event in 2011
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But, on November 2012
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LHCb at HCP2012 ๐ฉ๐ โ ๐๐
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LHCb at HCP2012 ๐ฉ๐ โ ๐๐
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<4.2x10-9
CMS PAS BPH-12-009
LHCb CONF-2012-017
<8.1x10-10
๐ฉ๐ โ ๐๐
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CMS: PRL 111 (2013) 101804
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LHCb 2017
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ATLAS 2016
๐๐2๐
3๐
[Q] LHCb and CMS results are shown in a combined form, while it is notfor ATLAS. What is the reason?
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Collider Detectors
ATLAS CMS CDF II D0 II
Magnetic
field
2 T solenoid +
toroid (0.5 T barrel
1 T endcap)
4 T solenoid +
return yoke
1.4T solenoid 2T solenoid
+ toroid (1.8T)
Tracker Si pixels, strips +
TRT
ฯ/pT โ 5x10-4 pT +
0.01
Si pixels, strips
ฯ/pT โ 1.5x10-4 pT +
0.005
Si strips + drift
chamber
Si strips +
scintillating fiber
EM
calorimeter
Pb+LAr
ฯ/E โ 10%/โE +
0.007
PbWO4 crystals
ฯ/E โ 3%/โE 0.003
Pb+scintillator
ฯ/E โ 13.5%/โE
0.015 in barrel
U+LAr
Hadronic
calorimeter
Fe+scint. / Cu+LAr
(10 ฮป)
ฯ/E โ 50%/โE
0.03
Brass+scintillator
(7 ฮป + catcher)
ฯ/E โ 100%/โE
0.05
Iron+scintillator
ฯ/E โ 50%/โE 0.03
in barrel
U+LAr (Cu or
stainless in outer
hadronic)
Muon ฯ/pT โ 2% @ 50GeV
to 10% @ 1TeV
(ID+MS)
ฯ/pT โ 1% @ 50GeV
to 10% @ 1TeV
(DT/CSC+Tracker)
Rapidities to 1.4 Rapidities to 2.0
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What we learned from ๐ฉ๐ โ ๐๐ ?
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[Q] What can we conclude on SUSY?
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FCNC Processes
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Check List
1) Describe FCNC and list a few key decay modes; draw a few Penguin diagrams
2) Draw Feynman diagrams for ๐ฉ๐ โ ๐๐ in the SM
3) Draw Feynman diagrams for ๐ฉ๐ โ ๐๐ in SUSY. See Br(๐ฉ๐ โ ๐๐ ) being
proportional to tan6b4) Survey 95% and 90% C.L. limits on Br(๐ฉ๐ โ ๐๐ ) from major experiments
(CLEO, BELLE, BABAR, CDF and D0).
5) D0โs muon detector has an excellent coverage. [Check the pseudo-rapidity
coverage for muons in D0 and CDF.] However, D0 limits on Br(๐ฉ๐ โ ๐๐ ) is
weaker than the CDF limits. Why?
6) CLEO, BELLE, BABAR do not have limits on Br(๐ฉ๐ โ ๐๐ ). Why?
7) Below are three CDF papers on search for ๐ฉ๐ โ ๐๐ . Summarize the analysis
and result in each paper by identifying how the analysis technique was
improved.
CDF (171 pb-1) Br < 7.5E-7 [hep-ex/0403032; PRL 93 (2004) 032001 ]
CDF (364 pb-1) Br < 2.0E-7 [hep-ex/0508036; PRL 95 (2005) 221805]
CDF (2000 pb-1) Br < 5.8E-8 [arXiv:0712.1708 [hep-ex] and PRL 100 (2008) 101892]
8) Survey the results from ATLAS, CMS and LHCb
9) How do we measure Br?
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Flavor Changing Neutral Currents (FCNCs) are powerful tool to probe newphysics.
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But, FCNC โฆ
Summary
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Experimentally, โฆ
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Samples of ๐ โs and ๐ฒโs
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Decay-In-Flight
K+ K+
pT = 3 GeVpT = 2 GeV
K+ m+~100 cm
~10 cm
0
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Impact Parameter
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Anatomy of ๐ฉ๐ โ ๐๐
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Anatomy of Amplitude of ๐ฉ๐ โ ๐๐
m
m
H/A0
b
s
_
c+~
t~
tan6b
b
SUSY
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