Dark Matter 2003: an update Rogério Rosenfeld Instituto de FísicaTeórica/UNESP Nova Física do Espaço II Campos do Jordão 18/02/2003

Many activities in 2002/2003. Highlights: Eidelweiss New codes for computing relic abundances New candidates Summary of IDM2002 (September, York) (last week!) WMAP

Receita de Universo (pós-WMAP) Receita de Universo (pós-WMAP) Matéria escura não-bariônica

Dark matter candidates 2002 NeutrinosNeutrinos AxionsAxions WIMPSWIMPS WIMPZILLASWIMPZILLAS PhionsPhions

Neutrinos Exist and are as abundant as photonsExist and are as abundant as photons ~ 120/cm 3 ~ 120/cm 3 Problems with large scale structure:Problems with large scale structure: relativistic particles => free streaming => suppression of small scale fluctuations. WMAP + 2dFGRS:

Dark matter candidates 2002 NeutrinosNeutrinos AxionsAxions WIMPSWIMPS WIMPZILLASWIMPZILLAS PhionsPhions

Phions Self-interacting dark matter solve LCDM problems: central halo densities and number of subhalos WMAP data: significantly lower amplitude of fluctuations on small scales as compared to LCDM.

Dark matter candidates 2002 NeutrinosNeutrinos AxionsAxions WIMPSWIMPS WIMPZILLASWIMPZILLAS PhionsPhions ?????

WIMPZILLAS Decaimento no halo galácticoDecaimento no halo galáctico Grande produção de fótons e neutrinos de altas energiasGrande produção de fótons e neutrinos de altas energias 90% pions (fotons e neutrinos), 10% protons Evento do Flys Eye não é foton! anisotropias Centro da galáxia Clumps Auger, HiRes, EUSO, EGRET, GLASTAuger, HiRes, EUSO, EGRET, GLAST

EGRET Z. Fodor hep-ph/

Dark matter candidates 2002 NeutrinosNeutrinos AxionsAxions WIMPSWIMPS WIMPZILLASWIMPZILLAS PhionsPhions ?????

Axions Partículas que surgem em modelos sem violação de CPPartículas que surgem em modelos sem violação de CP em interações fortes (simetria de Peccei-Quinn). Candidato há anosCandidato há anos Axions são produzidos não-relativisticamenteAxions são produzidos não-relativisticamente (cold dark matter) (cold dark matter) Parâmetro f a : escala de quebra de simetria de PQParâmetro f a : escala de quebra de simetria de PQ

Axions Detecção via conversão de axion em 2 fotons dentro deDetecção via conversão de axion em 2 fotons dentro de cavidades ressonantes (g a ). Limites: eV < m a < eVLimites: eV < m a < eV SN1987A Massa: m a = eV (10 12 GeV/ f a )Massa: m a = eV (10 12 GeV/ f a )

C. Hagmann K. Bibber L. Rosenberg PDG junho 2002

Dark matter candidates 2002 NeutrinosNeutrinos AxionsAxions WIMPSWIMPS WIMPZILLASWIMPZILLAS PhionsPhions ?????

WIMPS Weakly Interacting Massive Particles:Weakly Interacting Massive Particles: Partículas com massa típica de 100 GeV e que interagem fracamente Existem naturalmente em extensões super simétricas doExistem naturalmente em extensões super simétricas do Modelo Padrão: Lightest Supersymmetric Particle (LSP). Geralmente, LSP = neutralino.Geralmente, LSP = neutralino.

WIMPS Candidato favorito da academia. Candidato favorito da academia. Abundância cosmológica pode ser calculada no MSSM:Abundância cosmológica pode ser calculada no MSSM: Cold Dark Matter (m WIMP >T f ). Cold Dark Matter (m WIMP >T f ).

WIMPS Detecção direta de WIMPSDetecção direta de WIMPS Cristal de Ge, NaI WIMP do halo Núcleo com recuo (calor,luz,som)

WIMPS Edelweiss (1600 metros sob Frejus) 1 kg de Germanio

WIMPS Edelweiss June 2002

Exclusion plot spin independent scattering (CDMS2 included) K. Pretzl Summary IDM2002

Automatic calculations I Dark matter halo ±0.009

Automatic calculations II: micrOMEGAs

tan = 10tan = 50 micrOMEGAs: G. Belanger et al., IDM2002

Edsjo IDM2002

Data is starting to probe MSSM

Edsjo - IDM Indirect searches

New New dark matter candidates 2003 NeutrinosNeutrinos AxionsAxions WIMPSWIMPS WIMPZILLASWIMPZILLAS PhionsPhions ????? VAMPSVAMPS

VAMPS VAMP VAriable Mass Particles zzzzzzzzzzzzzzz

VAMPS Idea: connection between dark matter and dark energy (Comelli, Pietroni and Riotto, hep-ph/ ) L ~ m 0 2 exp(-2 ) L ~ m 0 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 m 2

VAMPS Energy density of VAMPS: = m n ~ = m n ~ exp(- ) (a 0 /a(t)) 3 = exp(- ) exp(- ) ; = ln (a(t)/a 0 ) = ln (a(t)/a 0 )

Quintessence: exponential potential ~V( ) = V 0 exp( ) ~V( ) = V 0 exp( ) VAMPS IF / / for all times for all times solves coincidence problem

This solution for is an attractor VAMPS

VAMPS Comelli, Pietroni and Riotto, hep-ph/030280

New New dark matter candidates 2003 NeutrinosNeutrinos AxionsAxions WIMPSWIMPS WIMPZILLASWIMPZILLAS PhionsPhions ????? VAMPSVAMPS LKKLKK

Kaluza-Klein tower What if there are small extra dimensions? Klein-Gordon equation for a scalar field in 5-d: Periodic b.c. (R is the radius of compact dimension) : Effective Effective mass term in 4-d

Kaluza-Klein dark matter In some models, lightest KK (LKK) mode (n=1) is stable: dark matter candidate! Typical mass in the 1-2 TeV range in order to have right cosmic abundance.

Kaluza-Klein dark matter Servant and Tait, hep-ph/

Conclusions 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,...