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˜

qq

qi˜

qj˜

q g

r10˜

r10˜

qq

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’

qq

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