dm@nlkovarik/hap-kovarik.pdf · susy dm dn dt = 3hn ⇥ annv⇤ n2 (n eq) 2 ⇥ public codes...
TRANSCRIPT
DM@NL KAROL KOVAŘÍK
INSTITUT FÜR THEORETISCHE PHYSIK, KIT
2
OUTLINE
1. Introduction DM & particle physics
2. DM@NLO
3. Summary & Outlook
INTRO
3
Indications of Dark Matter
Rotational curves of galaxies
Gravitational lensing
Newtonian drop-off of stars' velocities with distance not supported by data
MG
r2=
v2
r⇥ v � 1⇤
r
Strong evidence for Dark Matter provided from combinedmeasurement of galaxy cluster 1E0657-56 (bullet cluster) by Chandra X-ray observatory & Hubble telescope & VLT
INTRO
4
Dark Matter in numbers
�DE � 0.72672%
23%
5%
Matter density in the Universe
Dark EnergyDark MatterOrdinary Mat. �b � 0.046
�DM � 0.228
The knowledge on the energy content - combination from several sources
Cosmic Microwave Background - WMAP
Supernova Red Shifts - SN1a
Big Bang Nucleosynthesis
Baryonic Acoustic Oscillation
�DM
INTRO
5
Indirect detection of dark matterobserving products of DM annihilations in galactic halo
- difficult to use for a discovery due to huge uncertainties
e±, p�, �, ⇥, ⇥
Pamela, Fermi/GLAST, AMS, ATIC, HESS, Magic, IceCube, Antares...
Direct detection of dark matterdetection of nucleus recoil after scattering with DM- the only way how to access DM outside of collidersCDMS, Xenon, Edelweiss, ALPs, CAST
Dark Matter observables Dark matter relic density �CDMh2
very indirect but precise observable- good for consistency check of DM candidatesCOBE, WMAP, Planck �CDMh2 = 0.1123± 0.0035
6
Superfield Particle Spin Superpartner SpinV1 Bµ 1 B 1
2
V2 W iµ 1 W i 1
2
V3 Gaµ 1 ga 1
2
Q Q = (uL, dL) 12 Q = (uL, dL) 0
U c U c = uR12 U c = u⇥R 0
Dc Dc = dR12 Dc = d⇥R 0
L L = (�L, eL) 12 L = (�L, eL) 0
Ec Ec = eR12 Ec = e⇥R 0
H1 H1 = (H01 ,H�
1 ) 0 H1 = (H01 , H�
1 ) 12
H2 H2 = (H+2 ,H0
2 ) 0 H2 = (H+2 , H0
2 ) 12
~~
squarks q
sleptons l
neutralinos, charginos
neutralinos, charginos
gluinos
INTRO Supersymmetry
good DM candidate new fundamental space-time symmetry ➨ new particles
lightest SUSY particle (LSP) stable
solves hierarchy problem in the Higgs sector
unification of gauge couplings possible
...
INTRO
7
Supersymmetry ? no experimental hints @ colliders
[GeV]0m500 1000 1500 2000 2500 3000
[GeV
]1/
2m
100
200
300
400
500
600
700
800
± l~ LEP2
± 1χ∼ LEP2
No EWSBNon-Convergent RGE's
= L
SPτ∼
) = 500g~m(
) = 1000g~m(
) = 1500g~m(
) = 1000q~m(
) = 1500q~m(
) = 2000
q~m( ) = 2500
q ~m
( )=10βtan( = 0 GeV0A
> 0µ
= 173.2 GeVtm
= 7 TeVs, -1 = 4.98 fbint
CMS Preliminary L
Tα
Jets+MHT
Razor
SS Dilepton
OS Dilepton
Multi-Lepton
MT2
1 Lepton
m2h0 = m2
Z cos
22� +
3g2m4t
8⇡2m2W
log
mt1mt2
m2t
+
X2t
mt1mt2
✓1� X2
t
12mt1mt2
◆�
cMSSM exclusion plotCMS 2011
constraints from Higgsin MSSM SUSY particles contribute to Higgs mass through loops
++ tt
HTTPS://TWIKI.CERN.CH/TWIKI/BIN/VIEW/CMSPUBLIC/PHYSICSRESULTSSUS#PUBLICATIONS
mass [GeV]g~0 500 1000 1500 2000 2500 3000
mas
s [G
eV]
Rc~ , Ru~
0
500
1000
1500
2000
2500
3000 | preLHC)ep(
68% BCR 95% BCR
mass [GeV]g~0 500 1000 1500 2000 2500 3000
mas
s [G
eV]
Rc~ , Ru~
0
500
1000
1500
2000
2500
3000 | CMS)ep(
68% BCR 95% BCR
mass [GeV]g~0 500 1000 1500 2000 2500 3000
mas
s [G
eV]
0 1r¾
0
200
400
600
800
1000
1200 | preLHC)ep(
68% BCR 95% BCR
mass [GeV]g~0 500 1000 1500 2000 2500 3000
mas
s [G
eV]
0 1r¾
0
200
400
600
800
1000
1200 | CMS)ep(
68% BCR 95% BCR
[Sekmen et. al. arXiv: 1109.5119 [hep-ph]]
INTRO
8
SUSY DM
dn�
dt= � 3Hn� � ⇥�annv⇤
�n2
� � (nEQ� )2
⇥
Public codes perform a calculation of the relic density for given model (MSSM)
DarkSUSY micrOMEGAs SuperIso Relic[Bélanger et al. 2006][Gondolo et al. 2004] [Arbey, Mahmoudi 2009]
Total cross-section contains all SM final states�
r10˜
o1˜
Z
oor10˜
r10˜
Z
h0Z
r10˜
r10˜
W
Wri˜r1
0˜
r10˜
f
fH0
Calculate abundance of DM in a particle physics model (MSSM) ≡ solving Boltzmann eq.
�v�⇥ =�
v� e�E1/T e�E2/T d3p1 d3p2�e�E1/T e�E2/T d3p1 d3p2
thermally averaged total cross-section
INTRO
9
SUSY DMtanβ=10, A0=0 GeV , μ>0
m1/
2 (G
eV)
2000
1500
1000
500
2500 40001000m0 (GeV)
r10˜
r10˜
W
Wri˜
3. focus point region - large m0 , near a region with no radiative EWSB
�01 �0
1 ⇥W+W� � 70%�0
1 �01 ⇥ Z0Z0 � 16%
�01 �0
1 ⇥ Z0h0 � 7%�0
1 �01 ⇥ h0h0 � 5%
r10˜
o1˜
Z
oo
2. co-annihilation region - low m0 , small mass difference between LSP & nLSP
�01 l1 ⇥ A0l � 37%
li lj ⇥ l+i l�j � 29%
�01 �0
1 ⇥ l+l� � 12%�0
1 l1 ⇥ Z0l � 11%
r10˜
r10˜
l
lli˜
1. bulk region - low m0-m1/2 , light sleptons
�01 �0
1 ⇥ l l � 39%�0
1 �01 ⇥ bb � 18%
�01 �0
1 ⇥ qq � 18%
[Baer, Belyaev, Krupovnickas, Mustafayev hep-ph/0403214]
INTRO
10
SUSY DM
[Baer, Belyaev, Krupovnickas, Mustafayev hep-ph/0403214]
tanβ=55, A0=0 GeV , μ>0
m1/
2 (G
eV)
2000
1500
1000
500
2500 40001000m0 (GeV)
r10˜
r10˜
q
qHk0
1. Higgs funnel region - Higgs resonances
�01 �0
1 ⇥ bb � 62%�0
1 �01 ⇥ h0A0 � 11%
�01 �0
1 ⇥W±H⇥ � 10%�0
1 �01 ⇥ l l � 9%
r10˜
o1˜
Z
oo
2. co-annihilation region - low m0 , small mass difference between LSP & nLSP
l1¯l1 ⇥W+W� � 24%
l1¯l1 ⇥ l+l� � 20%
l1¯l1 ⇥ Z0Z0 � 13%
l1¯l1 ⇥ h0h0 � 11%
r10˜
r10˜
W
Wri˜
3. focus point region - large m0 , near a region with no radiative EWSB
�01 �0
1 ⇥ tt � 64%�0
1 �01 ⇥ bb � 15%
�01 �0
1 ⇥W+W� � 10%�0
1 �01 ⇥ Z0Z0 � 5%
INTRO
11
SUSY DM after many years of data taking precision will reach %-level with Planck
COBE 1989 WMAP 2002 Planck 2010
�CDMh2 = 0.1123± 0.0035WMAP 7-year data
motivation to improve theoretical precision in identification of preferred parameter space regions
including SUSY-QCD corrections to cross-sections DM@NL
DM@NL 1. Who are we
2. Goals
3. Some results
Public Tool for SUSY-QCD corrections
13
B. Herrmann
J. Harz
Q. Le Boulc’h
K. Kovařík
http://projects.hepforge.org/dmnlo
M. Klasen,
M. Meinecke, P. Steppeler
DM@NL
14
DM@NL Goals of the project
Provide a consistent set of SUSY-QCD corrected cross-sections for relic density calculation
Provide a package which extends public tools micrOMEGAs & DarkSUSY
Extend SUSY-QCD corrections also to direct & indirect detection
�1
�1
Q
Q
�i
�jq
q�i
qjq
V,H�i
qjq
g
qj
qi V,H
V,Hqj
qi
q
q
15
SPhenosparticle masses, couplings
precision observables
micrOmegasintegration of Boltzmann eq.
& much more ...
W.Porod 2003-2012
G. Bélanger, F. Boudjema, A. Pukhov, A. Semenov (2003-2012)
SUSY parameters(mSUGRA, pMSSM)
Input
CalcHEP(co-) annihilation processes
at tree-level
DM@NL all relevant processes with full SUSY-QCD corrections
J. Harz, B. Herrmann, M. Klasen, K. Kovarik, Q. Le Boulc’h,M. Meinecke, P. Steppeler
(2008-2012)
CalcHEP cross-sections replaced by DM@NLO
neutralino relic density
DM@NL Implementation
16
DM@NL Renormalization
Multiple processes require a consistent choice of input parameters
mb,mt,mt1 ,mt2 ,mb1,mb2
, Ab, At, ✓t, ✓brelevant parameters
⇠ mbh0 h0
b
b
b1
b2
⇠ Ab,mb ⇠ Ab, At,mb,mt
b1
t2
H±
input parameters
dependant parameters
mDRb ,mOS
t , ADRb , ADR
t ,mOSt1,mOS
b1,mOS
b2
mt2 , ✓b, ✓t
U q
M2
Q+ (I3Lq �eq s2W ) cos 2�m 2
Z +m2q , mq
�Aq � µ (tan�)�2I3L
q�
mq
�Aq � µ (tan�)�2I3L
q�
M2{U, D} + eq s2W cos 2�m 2
Z +m2q
!(U q
)
†=
✓m2
q1 0
0 m2q2
◆
17
DM@NL
r10˜
r10˜
q
qH0k
r10˜
r10˜
q
qZ0
r10˜
r10˜
q
qqi˜
r10˜
r10˜
q
qqi˜
Tree-Level
r10˜
r10˜
qg
qZ
qr10˜
r10˜
q
gq
Z
qr10˜
r10˜
qg
qHk0
qr10˜
r10˜
q
gq
Hk0
q
r10˜
r10˜
qg
qqi˜
q
r10˜
r10˜
q
g
q
qi˜
q
r10˜
r10˜
q
g
q
qi˜
qi˜i
r10˜
r10˜
q
g
q
qi˜
q
r10˜
r10˜
q
g
q
qi˜
q
r10˜
r10˜
q
g
q
qi˜
qi˜
Virtual one-loop corrections
Real gluon emission corrections
r10˜
r10˜
q
q
Z gq
q
r10˜
r10˜
q
q
Zg
qi˜
qj˜
r10˜
r10˜
q
q
H0k g
q
q
r10˜
r10˜
q
q
H0k g
qi˜
qj˜
r10˜
r10˜
q
q
qi˜
qj˜
q g
r10˜
r10˜
q
q
qi˜
q
qi˜ g
r10˜
r10˜
q
qqi˜
qj˜
q g
r10˜
r10˜
q
qqi˜
q
qi˜ g
r10˜
r10˜
qqqi˜
qj˜
q g
r10˜
r10˜
qqqi˜
q
qi˜ g
r10˜
r10˜
qi˜
qj˜
q g
r10˜
r10˜
qi˜
q
qi˜ g
r10˜
r10˜
q
q
qi˜
qi˜g
r10˜
r10˜
q
q
qi˜qi˜
g
r10˜
r10˜
q
q
qi˜
qj˜qk˜
r10˜
r10˜
q
q
qi˜qj˜
qk˜
r10˜
r10˜
q
q
qi˜
qj˜q g
r10˜
r10˜
q
q
qi˜
qi˜qi˜ g
r10˜
r10˜
q
q
qi˜
qj˜q g
r10˜
r10˜
q
q
qi˜
qi˜qi˜ g
r10˜
r10˜
q
q
q
qi˜
qj˜
g
r10˜
r10˜
q
q
qi˜
q
q
g
r10˜
r10˜
q
q
q
qi˜
qj˜
g
r10˜
r10˜
q
q
qi˜
q
q
g
�1
�1
Q
Q
Neutralino annihilation
B. Herrmann, M. Klasen, K. Kovarik,arXiV:09010481, 09070030
�1
�1
Q
Q
18
DM@NL Neutralino annihilation
(GeV)2M600 800 1000 1200
(GeV
)0
m
100
200
300
400
500
no EWSB
40%
60%
80%
M2 (GeV)600 800 1000
200
300
400
m0
(GeV
)
σtt (G
eV-2)
10-9
10-10
50 150pcm (GeV)
250 (GeV)CM
p0 50 100 150 200 250 300
)-2
v (G
eVan
n)t (tm
-1010
-910
tot
Z
q~/0H
0H
q~
(-1)q~Z/
(-1)0Z/H
(GeV)CM
p0 50 100 150 200 250 300
)-2
v (G
eVan
n)t(tm
-910
-810
-710
-610 one-loopmicrOMEGAstree-level
50 150pcm (GeV)
250
σtt (G
eV-2)
10-7
10-9
10-8
10-6
Parameter values: m0 = 320 GeV, M2 = 700 GeV tanβ = 10, A0 = -350, sgn μ = + x1 = 2/3, x3 = 1/3
Relic density: Ωh2 = 0.114, tt = 79%
_
19
�1
�1
Q
Q
DM@NL Neutralino annihilation
Ωh2
0.05
0.10
0.15
500460 480 (GeV)1/2m460 470 480 490 500 510
2 hC
DM
10.05
0.1
0.15
0.2=500 GeV0m
tree-levelmicrOMEGAsone-loop
m1/2
pcm (GeV)50 150 250
σbb (G
eV-2)
10-11
10-7
(GeV)CM
p0 50 100 150 200 250 300
)-2
v (G
eVan
n)b(b
m
-1110
-1010
-910
-810
-710
-610
one-loopmicrOMEGAstree-level
10-9
480 500 520
480
500
490
m1/2
m0
(GeV)1/2m470 480 490 500 510 520
(GeV
)0
m
480
490
500
510
r=2mA
m
80%
70%
80%
Parameter values: m0 = 500 GeV, M2 = 500 GeV tanβ = 10, A0 = 0, sgn μ = + MHu = 1500 GeV, MHd = 1000 GeV
Relic density: Ωh2 = 0.118, bb = 64% tt = 21%
__
20
DM@NL Neutralino-stop co-annihilation �i
qjq
V,H
Tree-Level
rn0˜
qi˜
q’
rn0˜
qi˜
q’
q
qj˜ ,rn0˜
qi˜
q’
qrk˜
rn0˜
qi˜
q’
Vq
rn0˜
qi˜
q’
V
qj˜ ,rn0˜
qi˜
q’
Vrk˜
Real gluon emission corrections
Virtual one-loop corrections
rn0˜
qi˜
q’
V/q
gqj˜
qrn0˜
qi˜
q’
V/q
gq
qrn0˜
qi˜
q’g
V/q
q
q’rn0˜
qi˜
V/q
q’
g
rm˜
qj˜
rn0˜
qi˜
V/q
q’
g
rm˜q’
rn0˜
qi˜
q’
V/q
g
qj˜ ,
qj˜
rn0˜
qi˜
q’
g
V/q
qj˜ ,
qj˜ ,
rn0˜
qi˜
q’g
V/q
qj˜ ,q’
rn0˜
qi˜
q’
g
V
qj˜ ,
rn˜
q’
qi˜
q’
qi˜
gV/q
q
q’
q
q’
gV/q
qi˜
qj˜ ,
qi˜
qj˜ ,g
V
qi˜
qi˜
qj˜ ,
g
rn˜
q’
qi˜
qj˜ ,
q
gV/q
q
q’
qj˜
qk˜ ,g
V/q
qi˜
qj˜ ,
q
q’
gV/q
qi˜
qj˜ ,
qk˜
ql˜ ,
rn0˜
V/q
qi˜
q’
q
qi˜
q’
g
rn0˜
V/q
qi˜
q’
qj˜
q
qk˜ ,
g
rn0˜
V/q
q’
qi˜
qj˜ ,
q’
qk˜
g
rn0˜
V/q
q’
qi˜
q’
qj˜ ,
q
g
rn0˜
V
q’
qi˜
qj˜ ,
q’
g
21
DM@NL Neutralino-stop co-annihilation �i
qjq
V,H
Parameter scans in pMSSM in regions where co-annihilation is important
Relative contributions of all co-annihilation final states shown
�t ! th0
�t ! tg �t ! tZ0
�t ! tH0 �t ! tA0
�t ! tW±
�t ! tH±
�t ! t�
22
DM@NL Neutralino-stop co-annihilation �i
qjq
V,H
Parameter scans in pMSSM in regions where co-annihilation is important
Relative contributions of all co-annihilation final states shown
�t ! th0
�t ! tg �t ! tZ0
�t ! tH0 �t ! tA0
�t ! tW±
�t ! tH±
�t ! t�
120GeV mh0 130GeV
Exp. constraints
23
DM@NL Neutralino-stop co-annihilation �i
qjq
V,H
Parameter scans in pMSSM in regions where co-annihilation is important
Relative contributions of all co-annihilation final states shown
�t ! th0
�t ! tg �t ! tZ0
�t ! tH0 �t ! tA0
�t ! tW±
�t ! tH±
�t ! t�
120GeV mh0 130GeV
Exp. constraints
0.0946 ⌦�h2 0.1306
24
DM@NL Neutralino-stop co-annihilation �i
qjq
V,H
Parameter scans in pMSSM in regions where co-annihilation is important
Relative contributions of all co-annihilation final states shown
�t ! th0
�t ! tg �t ! tZ0
�t ! tH0 �t ! tA0
�t ! tW±
�t ! tH±
�t ! t�
120GeV mh0 130GeV
Exp. constraints
0.0946 ⌦�h2 0.1306
2.77 · 10�4 BR(b ! s�)
BR(b ! s�) 4.33 · 10�4
25
DM@NL Neutralino-stop co-annihilation �i
qjq
V,H
M1 Mq1,2 Mq3 M˜ Tt mA µ tan�Parameters 306.9 2037.7 709.7 1499.3 1806.5 1495.6 2616.1 9.0
Scenario with a dominant contribution of the lightest Higgs
⌦�h2 �01t1 ! th0 �0
1t1 ! tZ0 �01t1 ! bW+ Sum
Contributions 0.114 38.5% 3.4% 5.9% 47.8%
J. Harz, B. Herrmann, M. Klasen, K. Kovarik, Q. Le Boulc’h arXiV:1212.5241
SUMMARY & OUTLOOK
26
NLO corrections important for correctly identifying
excluded / preferred regions of parameter space
will bring full NLO QCD
corrections to MicrOmegas & DarkSUSY
Dark matter searches complementary to LHC
DM@NL
http://projects.hepforge.org/dmnlo