Era of Discovery with CMS DetectorEra of Discovery with CMS Detector
TAMU Group Teruki Kamon, Alexei Safonov, David
Toback
Special Colloquium, LHC… Alexei Safonov09/17/08 (Next Wednesday)
Precision Cosmology at the Precision Cosmology at the Large Hadron ColliderLarge Hadron Collider
Bhaskar Dutta
Texas A&M University
311th September ’ 08
Based on plenary talks atCosmo’08, IDM’08,Santa Fe’08,DM’08
LHC Days…
4
The mechanism for generating masses
We will try to understand:
The physics behind the scale of W, Z boson mass scale ~ electroweak scale
The origin of dark matter
Do we have any further evidence of grand unification?
Is there any particle physics connection?
Precision Cosmology at the LHC
Mplanck>>MW
The Standard Model (SM) describes all these particles and 3 of 4 forces. We have confirmed the existence of those in the laboratory experiments.
The Standard ModelThe Standard Model
+ Higgs boson
Higgs has not yet been discovered
The mass is constrained from LEP and Tevatron data:
114 GeV<MH<154 GeV
Precision Cosmology at the LHC 5
SM problems and solutionsSM problems and solutionsThe Standard Model :• Cannot provide a dark matter
candidate.• Has a serious Higgs mass
divergence problem due to quantum correction.
• Cannot accommodate masses for neutrinos.
• Cannot provide enough matter-antimatter asymmetry.
Standard Model has fallen!
6Precision Cosmology at the LHC
• Solves the Higgs mass problem in a very elegant way.
• Supersymmetric grand unified models include neutrinos!
Dutta, Mimura, Moahapatra, PRL 100 (2008); 96, (2006) 061801; 94, (2005) 091804; PRD 72 (2005) 075009.
• Can produce correct matter-antimatter asymmtery
Dutta, Kumar, PLB 643 (2006) 284• Can provide Inflation
• Can provide new sources of CP violation, e.g., Bs
Dutta, Kumar, Leblond, JHEP 0707 (2007) 045; Allahverdi, Dutta and Mazumdar, PRL99 (2007) 261301., PRD (2008) to appear.
Dutta, Mimura, PRL 97 (2006) 241802; PRD (Rapid Com) 77 (2008)051701.
Supersymmetry :Provides a candidate for dark matter ~ neutralino.
What is the new model?
Goldberg’ 83; Ellis, Hagelin, Nanopoulos, Olive, Srednicki’84
Particle Physics and Cosmology
SUSY is an interesting class of models to provide a weakly interacting massive neutral particle (M ~ 100 GeV).
SUSY
SUSY
CDM CDM == Neutralino ( ) Neutralino ( )01~
Ast
roph
ysic
sA
stro
phys
ics
8
pb9.0
1~
23.0
2
2
ann
0
ann
2~ 0
1
M
dxv
h fx
LHC
23/04/22 7
LHC
LHCLHC
Precision Cosmology at the LHC
The fundamental law(s) of nature is hypothesized to be symmetric between bosons and fermions.
Fermion Boson
Have they been observed? ➩ Not yet.
Supersymmetrized SMSupersymmetrized SM
Precision Cosmology at the LHC 8
SUSY partner of Z boson: neutralino
SUSY partner of W boson: chargino
Lightest neutralinos are always in the final state! This neutralino is the dark matter candidate!!
SUSY partner of lepton: stau
SUSY Interaction DiagramsSUSY Interaction Diagrams
Precision Cosmology at the LHC 9
The grand unification of forces occur
in SUSY models.
Dream of the UnificationDream of the Unification
☺U(1)Y ForceU(1)Y Force
Precision Cosmology at the LHC
Unification scale can also be pushed to 1017-18 GeVAmeliorates Proton decay problem in the very successful SO(10) modelDutta, Mimura, Mohapatra , Phys.Rev.Lett.100:181801,2008
10
Search for SUSY-upcoming days
11Precision Cosmology at the LHC
Large Hadron Collider- susy particles will be directly produced
Higgs mass in the well motivated SUSY models: < 150 GeV Current experimental bound: 114 - 154 GeV
Direct detection experiment, CDMS, Xenon 100, LUX etc
Indirect detection experiments, e.g., PAMELA has already observed excess of positron excess in cosmic rayFermi Gamma Ray Space Telescope: Sensitive to gamma ray from Dark Matter annihilation
Tevatron search for Bs highest reach on SUSY masses)
Existence of Higgs will be explored
IceCube: Sensitive to neutrinos from DM annihilation
Arnowitt, Dutta, Kamon and Tanaka, Phys.Lett.B538 (2002) 121.
e+
…
The signal : jets + leptons + missing Energy
SUSY at the LHC
(or l+l-, )
DM
DM
Colored particles get produced and decay into weakly interacting stable particles
High energy jet[mass difference is large]
The energy of jets and leptons depend on the sparticle masses which are given by models R-parity conserving
12Precision Cosmology at the LHC
(or l+l-, )
MW,MZ
Excess in ETmiss + Jets R-parity conserving SUSY
Meff Measurement of the SUSY scale at 10-20%.
Excess in Excess in EETTmissmiss + Jets + Jets
Hinchliffe and Paige, Phys. Rev. D 55 (1997) 5520
q
The heavy SUSY particle mass is measured by combining the final state particles
q
q
q01~
01~
g~g~
ETj1 > 100 GeV, ET
j2,3,4 > 50 GeV Meff > 400 GeV (Meff ET
j1+ETj2+ET
j3+ETj4+ ET
miss) ET
miss > max [100, 0.2 Meff]
Precision Cosmology at the LHC 13
Since squarks and gluinos are
heavier than W,Zs
SUSY scale can be measured with an accuracy of 10-20%
This measurement does not tell us whether the model can generate the right amount of dark matter
The dark matter content is measured to be 23% with an accuracy less than 4% at WMAP Question:To what accuracy can we calculate the relic density based on the measurements at the LHC?
Relic Density and Meff
Precision Cosmology at the LHC14
15
2
1CDM
+ ….
A near degeneracy occurs naturally for light stau in mSUGRA.
011 ~~ MMM
Δ
fTMe k/Δ
2
01~
1~+ + ….
Co-annihilation (CA) ProcessGriest, Seckel ’91
Anatomy of Anatomy of annann
pbM
vann 1~~ 2
2
Precision Cosmology at the LHC
Dark Matter Allowed RegionDark Matter Allowed Region
16
GeV 15~5Δ MCo-annihilation
Region
Precision Cosmology at the LHC
4 parameters + 1 signtan <Hu>/<Hd> at MZ
m1/2 Common gaugino mass at MGUT
m0 Common scalar mass at MGUT
A0 Trilinear couping at MGUT
sign() Sign of in W(2) = Hu Hd
MHiggs > 114 GeV Mchargino > 104 GeV 2.2x104 <B(b s ) <4.5x104 (g2)deviation from SM
Key Experimental Constraints
12900940 201
.h. ~
Minimal Supergravity Minimal Supergravity (mSUGRA)(mSUGRA)
<Hd>
<Hu>
<H> =
246 G
eV
SUSY model in the framework of unification:
+
Arnowitt, Chamesdinne, Nath, PRL 49 (1982) 970; NPB 227 (1983) 121. Barbieri, Ferrara, Savoy, PLB 119 (1982) 343.Lykken, Hall, Weinberg, PRD 27 (1983) 2359.
Precision Cosmology at the LHC 17
DM Allowed Regions in mSUGRA
[Stau-Neutralino CA region]
[Focus point region]the lightest neutralino has a larger Higgsino componentFeng, Matchev, Wilczek, PLB482 388,2000. [A-annihilation funnel region]This appears for large values of m1/2
[Bulk region] is almost ruled out
18Precision Cosmology at the LHC
Arnowitt, Dutta, Santoso, NPB 606:59,2001.
Ellis, Falk, Olive, PLB 444:367,1998.
Overdense region
Signals of the Allowed RegionsSignals of the Allowed Regions Neutralino-stau coannihilation region: jets + taus (low energy) + missing energy[Arnowitt, Dutta, Gurrola, Kamon, Krislock, TobackArnowitt, Dutta, Gurrola, Kamon, Krislock, Toback, , PRL, 100, (2008) 231802PRL, 100, (2008) 231802;Arnowitt, Dutta, Kamon, Kolev, TobackArnowitt, Dutta, Kamon, Kolev, Toback,, PLB 639 (2006) 46PLB 639 (2006) 46;;Arnowitt, Aurisano, Dutta, Kamon, Kolev, Simeon, Toback, Wagner; Arnowitt, Aurisano, Dutta, Kamon, Kolev, Simeon, Toback, Wagner; PLB 649 PLB 649 (2007)73(2007)73] Focus point: jets+ leptons +missing energy [Crockett, Dutta, Flanagan, Gurrola, Kamon, Kolev, VanDyke, 08;Crockett, Dutta, Flanagan, Gurrola, Kamon, Kolev, VanDyke, 08;
Tovey, PPC 2007; Baer, Barger, Salughnessy, Summy, Wang , PRD, 75, 095010 (2007)Tovey, PPC 2007; Baer, Barger, Salughnessy, Summy, Wang , PRD, 75, 095010 (2007)]] Bulk region: jets+ leptons +missing energy [Nojiri, Polsello,
Tovey’05] Annihilation funnel: mass of pseudo scalar Higgs = 2 mass of DM Overdense regions: Higgs+Jets, Z+jets, taus+jets+missing energy [Dutta, Gurrola, Kamon, Krislock, [Dutta, Gurrola, Kamon, Krislock, Lahanas, Mavromatos, Nanopoulos, arXiv:0808.1372 ]Lahanas, Mavromatos, Nanopoulos, arXiv:0808.1372 ]
19Precision Cosmology at the LHC
Goal for the analysisGoal for the analysis Establish the “dark matter allowed region” signal
Measure SUSY masses Determine mSUGRA parameters
Predict h2 and compare with CDMh2 20Precision Cosmology at the LHC
Smoking Gun of CA RegionSmoking Gun of CA Region
100%1~
Lu~
01χ~
02χ~
g~
97%
u
u
SUSY
Mas
ses
(CDM)2 quarks+2 ’s
+missing energy
Uniq
ue k
inem
atics
21
Low energy taus exist in theCA regionHowever, one needs to measure the model parameters to predict thedark matter content in this scenario
Precision Cosmology at the LHC
Low EnergyLow Energy and and MM Low energy ’s are an enormous challenge for the detectors
Precision cosmology at the LHC 22
Num
ber
of C
ount
s / 1
GeV
ETvis(true) > 20, 20 GeV
ETvis(true) > 40, 20 GeV
ETvis(true) > 40, 40 GeV
GeV) 5.7(
011
02
M
~~~
Arnowitt, Dutta, Kamon, Kolev, Toback PLB 639 (2006) PLB 639 (2006) 4646
We need to involve the low energy ’sIn our analysis
Low energy
23
We use ISAJET + PGS4PLB 639 (2006) 46PLB 639 (2006) 46
Precision Cosmology at the LHCArnowitt, Dutta, Kamon, Kolev, Toback
EETTmissmiss+2+2+2j Analysis+2j Analysis
OSOSLS MLS M Distribution Distribution
Clean peak even for low M
(GeV) visM
maxpeak MM
24
GeV 6 10 .M
First, our goal is to determine all the masses
Precision Cosmology at the LHC
SUSY Anatomy
Mj
M
pT()
100%1~
Lu~
01χ~
02χ~
g~
97%
u
u
SUSY
Mas
ses
(CDM)
25
Meff
Precision Cosmology at the LHC
MMeffeff , , MMeffeff (b)Distribution (b)Distribution
26Precision Cosmology at the LHC
ETj1 > 100 GeV, ET
j2,3,4 > 50 GeV [No e’s, ’s with pT > 20 GeV] Meff > 400 GeV (Meff ET
j1+ETj2+ET
j3+ETj4+ ET
miss [No b jets; b ~ 50%]) ET
miss > max [100, 0.2 Meff]At Reference Point Meff
peak = 1274 GeV
Arnowitt, Dutta, Gurrola, Kamon, Krislock, Toback, PRL, 100, (2008) 231802
Meff(b)
> 400 GeV(Meff
(b) ET
j1=b+ETj2+ET
j3+ETj4+ ET
miss
[j1 = b jet])
Meff(b)peak = 1026 GeV
MMeffeff((bb)) can be used to determine
A0 and tan
Observables
SM+SUSY Background gets reduced
NN
• Ditau invariant mass: M
• Jet-- invariant mass: Mj
• Jet- invariant mass: Mj
• PT of the low energy • Meff : 4 jets +missing energy• Meff(b) : 4 jets +missing energy
Since we are using 7 variables, we can measure the model parameters and the grand unified scale symmetry (a major ingredient of this model)
1.Sort ’s by ET (ET1 > ET
2 > …)• Use OSLS method to extract pairs from the
decays
All these variables depend on masses model parameters
27Precision Cosmology at the LHC
7 Eqs (as functions of SUSY parameters)
)~,~(
)~,~,,~(
)~,~,,~ (
)~,~,~(
)~,(
)~,~,(
6peakeff
01
025
(2)peak2
01
024
(2)peak1
01
023
(2)peak
012
01
021
peak
L
Lj
Lj
Lj
qgfM
MqfM
MqfM
qfM
MfSlope
MfM
Invert the equations to Invert the equations to determine the massesdetermine the masses
Determining SUSY Masses (10 Determining SUSY Masses (10 fbfb11))
1 ellipse
)91.5( 8.09.5/
)19.3( 2.01.3/0.26.10
;19141;15260
;21831 ;25748
01
02
01
02
~~
~~
~~
~~
theoryMM
theoryMMM
MM
MM
g
g
gqL
10 fb-1
28
Phys. Rev. Lett. 100, (2008) 231802Phys. Rev. Lett. 100, (2008) 231802
Meff(b) = f7(g, qL, t, b)~ ~ ~ ~
Precision Cosmology at the LHC
Arnowitt, Dutta, Gurrola, Kamon, Krislock, TobackArnowitt, Dutta, Gurrola, Kamon, Krislock, Toback
GUT Scale SymmetryWe can probe the physics at the Grand unified theory (GUT) scale
The masses , , unify at the grand unified scale in SUGRA models
01~
m1/2
mas
s
MZMGUTLog[Q]
g~
01~
02~
02~ g~
Gaugino universality test at ~15% (10 fb-1)
Another evidence of a symmetry at the grand unifying scale!
Use the masses measured at the LHC and evolve them to the GUT scale using mSUGRA
29Precision Cosmology at the LHC
[1] Established the CA region by detecting low energy ’s (pT
vis > 20 GeV)
[2] Determined SUSY masses using:M, Slope, Mj, Mj, Meff
e.g., Peak(M) = f (Mgluino, Mstau, M , M ) [3] Predict the dark matter relic density by determining m0, m1/2, tan, and A0
DM Relic Density in mSUGRADM Relic Density in mSUGRA
01~0
2~
30Precision Cosmology at the LHC
[4] We can also predict the dark matter-nucleon scattering cross section but it has large theoretical error
p
Determining mSUGRA ParametersDetermining mSUGRA Parameters
),tan,,(),(
002/14)(
eff
02/13eff
AmmfMmmfM
b
),tan,,(),(
002/12
02/11
AmmfMmmfM j
Solved by inverting the following functions:
140tan160
43505210
0
2/1
0
A
mm
10 fb-1
),tan,( 02/102
~01
AmmZh
1fb 10 L1fb 50
31
Phys. Rev. Lett. 100, (2008) 231802Phys. Rev. Lett. 100, (2008) 231802
Precision Cosmology at the LHC
)fb 30( %7/ 1~~ 0
101
pp
)fb 70( %1.4)fb 30( %2.6/
1
12~
2~ 0
101
hh
Direct Detection
Focus Point (FP)-IIFocus Point (FP)-IIm0 is large, m1/2 can be small, e.g., m0= 3550 GeV, m1/2=314 GeV, tan=10, A0=0
32
M(gluino) = 889 GeV, ΔM(χ3
0- χ10) = 81 GeV,
ΔM(χ20- χ1
0) = 59 GeV, ΔM(χ3
0- χ20) = 22 GeV
Br(g → χ20 tt) = 10.2%
Br(g → χ20 uu) = 0.8%
Br(g → χ30 tt) = 11.1%
Br(g → χ30 uu) = 0.009%
~~~~
---
-
Precision Cosmology at the LHC
33
Dilepton Mass at FP
)( OSDF e
)OSSF( ee
M(ll) (GeV)
Eve
nts/
GeV
GeV 59)()( 01
02 ~M~M GeV 81)()( 0
103 ~M~M
)( OSDFOSSF eee
Tovey, talk at PPC 2007Baer, Barger, Salughnessy, Summy, Wang , PRD 75, 095010 (2007)Crockett, Dutta, Flanagan, Gurrola, Kamon, Crockett, Dutta, Flanagan, Gurrola, Kamon, Kolev, Krislock, VanDyke (2008)Kolev, Krislock, VanDyke (2008)
Precision Cosmology at the LHC
Relic density calculation depends on , tan and m1/2
mm1/21/2 and tan and tan can be can be solved from M(gluino), solved from M(gluino), ΔM (χΔM (χ33
00- χ- χ1100) and ΔM (χ) and ΔM (χ22
00- χ- χ1100))
Errors of (300 fb-1): M(gluino) 4.5%ΔM (χ3
0- χ10) 1.2%
ΔM (χ2
0- χ10) 1.7%
Chargino masses can be measured! Work in
Progress…
tan 22% 0.1%
Bulk Region-IIIThe most part of this region in mSUGRA is experimentally (Higgs mass limit, bs ) ruled out
mSUGRA point:
The error of relic density: 0.108 ± 0.1(stat + sys)
sparticle
mass
97.2
398
189
607
533
End pts value errormll 81.2 0.09
Mlq((max) 365 2.1
Mlq(min) 266.9 1.6
Mllq(max) 425 2.5
Mllq(min) 207 1.9
M(max) 62.2 5.0
Relic density is mostly satisfied by t channel selectron, stau and sneutrino exchange
Perform the end point analysis to determine the masses
01
~
02
~
l~
g~
uL~
m0=70; A0=-300m1/2=250; >0;tan=10;
[With a luminosity 300 fb-1, edge controlled to 1 GeV]
Nojiri, Polsello, Tovey’05
~Includes: (+0.00,−0.002 )M(A); (+0.001, −0.011) tan β; (+0.002,−0.005) m(2)
Precision Cosmology at the LHC 34
Overdense Region-IVOverdense Region-IV
35
m0
The final states contain Z, Higgs, staus
Lahanas, Mavromatos, Nanopoulos, Phys.Lett.B649:83-90,2007.
Dilaton effect creates new parameter space
Precision Cosmology at the LHC
Overdense region (Large ): Too much dark matter
In some models, this overdense region is not really overdense, e.g.,
Allowed region is moved up
Observables involving Z and Higgs
We can solve for masses by using the end-points
Precision Cosmology at the LHC
Observables:Effective mass: Meff (peak): f1(m0,m1/2)
Effective mass with 1 b jet: Meff (b) (peak): f2(m0,m1/2, A0, tan)
Effective mass with 2 b jets: Meff (2b) (peak): f3(m0,m1/2, A0, tan)
Higgs plus jet invariant mass: Mbbj(end-point): f4(m0,m1/2)
4 observables => 4 mSUGRA parametersDutta, Gurrola, Kamon, Krislock, Lahanas, Dutta, Gurrola, Kamon, Krislock, Lahanas, Mavromatos, Nanopoulos, arXiv:0808.1372Mavromatos, Nanopoulos, arXiv:0808.1372
36
Determining mSUGRA ParametersDetermining mSUGRA ParametersSolved by inverting the following functions:
1839tan9501544050472
0
21
0
A
mm
/
),tan,( 02/102
~01
AmmZh
1fb 1000 L
%~h/h ~~ 1502201
01
)tan()tan(
)()(
00214peak )(
eff
00213peak )(
eff
0212peakeff
0211point end
A,,m,mXMA,,m,mXM
m,mXMm,mXM
/bb
/b
/
/jbb
1000 fb-1
37Precision Cosmology at the LHC
2 tau + missing energy dominated regions:Solved by inverting the following Observables:
340tan450
660023440
0
21
0
A
mm
/
),tan,( 02/102
~01
AmmZh
%~h/h ~~ 192201
01
)tan()tan(
)()(
00214peak
00213peak )(
eff
0212peakeff
0211(2)peak
A,,m,mXMA,,m,mXM
m,mXMm,mXM
/
/b
/
/j
500 fb-1
For 500 fb-1 of data
Dutta, Gurrola, Kamon, Krislock, Lahanas, Mavromatos, Nanopoulos, arXiv:0808.1372Dutta, Gurrola, Kamon, Krislock, Lahanas, Mavromatos, Nanopoulos, arXiv:0808.1372 Precision Cosmology at the LHC 38
Dark Matter particle
DM Particle: Direct Detection?
detector
µ
(*) The TAMU group is one of the leading institutions in the US.
(*)
The measurement at the LHC will pinpoint the parameters of SUSY models. We can predict the direct detection probability of dark matter particles.
Complementary
measurements !
39
James White
Precision Cosmology at the LHC
Ongoing/future projects: CDMS, LUX, XENON100, ZEPLINStatus:– DAMA group (Italy) – claims to have observed some events.– CDMS, ZEPLIN, XENON10, Cogent – dispute their claim.
Status - Direct Detection
James White
Close to the current sensitivity
Accomando, Arnowitt, Dutta, Santoso, NPB 585 (2000) 124
10-8 pb
40
Rupak Mohapatra
ZEPLIN
CDMS
DAMA
XENON
Bob Webb
ConclusionConclusion
41
SM of particle physics has fallen.Supersymmetry seems to be natural in the rescue act and the dark matter content of the universe can be explained in this theory.The minimal SUGRA model is consistent with the existing experimental results.
[1] LHC can probe the minimal SUGRA model directly.
All the dark matter allowed regions can be probed at the LHC
The dark matter content can be measured with an accuracy of 6% in the stau-neutralino coannihilation region
This accuracy depends on the final states[2] This analysis can be applied to any SUSY
model Precision Cosmology at the LHC
Conclusion…[3] Direct detection experiments will simultaneously confirm the existence of these models.[4] Indirect detection experiments will also confirm the existence of SUSY models[5] Very exciting time ahead…
42Precision Cosmology at the LHC
Brahma
23/04/22 44
All of these will be supersymmetry phenomenology/model papers
Conclusion…Conclusion…
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