Dark Matter 2003: an update

Rogério RosenfeldInstituto de FísicaTeórica/UNESP

Nova Física do Espaço II Campos do Jordão 18/02/2003

Many activities in 2002/2003. Highlights:

EidelweissNew codes for computing relic abundancesNew candidatesSummary of IDM2002 (September, York)

(last week!) WMAP

006.0047.0 B

Receita de Universo (pós-WMAP) Receita de Universo (pós-WMAP)

02.002.1 tot

07.029.0 M

68.0 BMtot

Matéria escuraMatéria escuranão-bariônicanão-bariônica

Dark matter candidates2002

•NeutrinosNeutrinos

•AxionsAxions

•WIMPSWIMPS

•WIMPZILLASWIMPZILLAS

•PhionsPhions

NeutrinosNeutrinos•Exist and are as abundant as photonsExist and are as abundant as photons ~ 120/cm~ 120/cm33

eVm

CLh

23.0

)%95(0076.02

•Problems with large scale structure:Problems with large scale structure:relativistic particles => free streaming =>relativistic particles => free streaming =>suppression of small scale fluctuations.suppression of small scale fluctuations.

WMAP + 2dFGRS:WMAP + 2dFGRS:

Dark matter candidates2002

•NeutrinosNeutrinos

•AxionsAxions

•WIMPSWIMPS

•WIMPZILLASWIMPZILLAS

•PhionsPhions

PhionsPhions

Self-interacting dark matterSelf-interacting dark matter

solve LCDM problems: central halo densities and solve LCDM problems: central halo densities and number of subhalosnumber of subhalos

WMAP data: significantly lower amplitude of fluctuationsWMAP data: significantly lower amplitude of fluctuationson small scales as compared to LCDM.on small scales as compared to LCDM.

Dark matter candidates2002

•NeutrinosNeutrinos

•AxionsAxions

•WIMPSWIMPS

•WIMPZILLASWIMPZILLAS

•PhionsPhions

??????????

WIMPZILLASWIMPZILLAS

•Decaimento no halo galácticoDecaimento no halo galáctico

•Grande produção de fótons e neutrinos de altas energiasGrande produção de fótons e neutrinos de altas energias90% pions (fotons e neutrinos), 10% protons90% pions (fotons e neutrinos), 10% protonsEvento do Fly’s Eye não é foton!Evento do Fly’s Eye não é foton!

anisotropiasanisotropiasCentro da galáxiaCentro da galáxia

ClumpsClumps

•Auger, HiRes, EUSOAuger, HiRes, EUSO, EGRET, GLAST, EGRET, GLAST

EGRETZ. Fodorhep-ph/0302036

Dark matter candidates2002

•NeutrinosNeutrinos

•AxionsAxions

•WIMPSWIMPS

•WIMPZILLASWIMPZILLAS

•PhionsPhions

??????????

AxionsAxions

•Partículas que surgem em modelos sem violação de CP Partículas que surgem em modelos sem violação de CP em interações fortes (simetria de Peccei-Quinn). em interações fortes (simetria de Peccei-Quinn).

•Candidato há anos Candidato há anos

•Axions são produzidos não-relativisticamenteAxions são produzidos não-relativisticamente (cold dark matter)(cold dark matter)

•Parâmetro fParâmetro faa : escala de quebra de simetria de PQ : escala de quebra de simetria de PQ

AxionsAxions

•Detecção via conversão de axion em 2 fotons dentro de Detecção via conversão de axion em 2 fotons dentro de cavidades ressonantes (cavidades ressonantes (ggaa). ).

•Limites: 10Limites: 10-6-6 eV < m eV < ma a < 10 < 10-2-2 eV eV

SN1987ASN1987A

•Massa: mMassa: ma a = 10 = 10-5-5 eV (10 eV (101212 GeV/ f GeV/ fa a ) )

C. HagmannK. BibberL. RosenbergPDG junho 2002

Dark matter candidates2002

•NeutrinosNeutrinos

•AxionsAxions

•WIMPSWIMPS

•WIMPZILLASWIMPZILLAS

•PhionsPhions

??????????

WIMPSWIMPS

•WWeakly eakly IInteracting nteracting MMassive assive PParticles:articles:Partículas com massa típica de 100 GeV e que interagemPartículas com massa típica de 100 GeV e que interagemfracamente fracamente 23610 cm

•Existem naturalmente em extensões super simétricas do Existem naturalmente em extensões super simétricas do Modelo Padrão: Modelo Padrão: LLightest ightest SSupersymmetric upersymmetric PParticle (article (LSPLSP).).

•Geralmente, Geralmente, LSP = neutralinoLSP = neutralino..

WIMPSWIMPS

• Candidato favorito da academia.Candidato favorito da academia.

aniWIMP

cm

235102

•Abundância cosmológica pode ser calculada no MSSM: Abundância cosmológica pode ser calculada no MSSM:

• Cold Dark Matter Cold Dark Matter (m (mWIMPWIMP>T>Tf f ).).

WIMPSWIMPS

•Detecção direta de WIMPSDetecção direta de WIMPS

Cristal de Ge, NaICristal de Ge, NaI

WIMP do haloWIMP do halo

Núcleo com recuo (calor,luz,som)Núcleo com recuo (calor,luz,som)

WIMPSWIMPS

Edelweiss (1600 metros sob Frejus)Edelweiss (1600 metros sob Frejus)

1 kg de Germanio1 kg de Germanio

WIMPSWIMPS

Edelweiss June 2002 Edelweiss June 2002

Exclusion plot spin independent scattering (CDMS2 included)

K. PretzlSummary IDM2002

Automatic calculations I

Dark matter halo

0.135 ±0.009

Automatic calculations II: micrOMEGAs

tan = 10 tan = 50

micrOMEGAs: G. Belanger et al., IDM2002

EdsjoIDM2002

Data is starting to probe MSSM

Edsjo - IDM2002 - Indirect searches

NewNew dark matter candidates2003

•NeutrinosNeutrinos

•AxionsAxions

•WIMPSWIMPS

•WIMPZILLASWIMPZILLAS

•PhionsPhions

?????????? •VAMPSVAMPS

VAMPSVAMPS

VAVAriable MMass PParticles

zzzzzzzzzzzzzzz

VAMPSVAMPSIdea: connection between dark matter anddark energy (Comelli, Pietroni and Riotto, hep-ph/0302080)

L ~ mL ~ m0022 exp(-2 exp(-2) )

dark energy field (quintessence)

dark matter field(VAMP)

Slowly varying dark energy field acts as a time-dependent mass term for dark matter

mm22

VAMPSVAMPS

Energy density of VAMPS:

= = mm nn

~ ~

exp(-exp(- ) (a ) (a00/a(t))/a(t))33 = =

exp(-exp(- ) exp(- ) exp(- ) ; ) ;

= ln (a(t)/a= ln (a(t)/a00))

Quintessence: exponential potential

~V(~V() = V) = V00 exp( exp( ) )

VAMPSVAMPS

3

IF

//

for all timesfor all times

solves coincidenceproblem

This solution for is an attractor

VAMPSVAMPS

VAMPSVAMPSComelli, Pietroni and Riotto, hep-ph/030280

NewNew dark matter candidates2003

•NeutrinosNeutrinos

•AxionsAxions

•WIMPSWIMPS

•WIMPZILLASWIMPZILLAS

•PhionsPhions

??????????•VAMPSVAMPS

•LKKLKK

Kaluza-Klein towerKaluza-Klein tower

What if there are small extra dimensions?What if there are small extra dimensions?

Klein-Gordon equation for a scalar field in 5-d:Klein-Gordon equation for a scalar field in 5-d:

0, 52

22

25

2

xxtx

Periodic b.c. (R is the radius of compact dimension) :Periodic b.c. (R is the radius of compact dimension) :

R

nxxxx 5

5

2cos,

02

2

2

22

x

R

n

t

EffectiveEffectivemass termmass termin 4-d in 4-d

Kaluza-Klein dark matterKaluza-Klein dark matter

In some models, lightest KK (In some models, lightest KK (LKKLKK) mode (n=1) ) mode (n=1) is stable: dark matter candidate!is stable: dark matter candidate!

Typical mass in the 1-2 TeV range in order to Typical mass in the 1-2 TeV range in order to have right cosmic abundance.have right cosmic abundance.

Kaluza-Klein dark matterKaluza-Klein dark matter

Servant and Tait, hep-ph/0209262

ConclusionsConclusions

•Many new experimental data: WMAP, Edelweiss•Neutrinos ruled out (WMAP)•Phions not well motivated (WMAP)•Wimpzillas in check (EGRET? Photons in UHECR?)•Narrow window for axions•WIMPS are the favorite candidates•New codes to compute WIMPS relic abundances•DAMA region ruled out (Edelweiss)•Next generation of Dark Matter Experiments will test SUSY

Meanwhile, theorists keep using their wild imagination:VAMPS, KK-modes, ...