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) WMAP (last week!) Receita de Universo (pós-WMAP) tot 1.02 0.02 M 0.29 0.07 B 0.047 0.006 Matéria escura não-bariônica tot M B 0.68 Dark matter candidates 2002 •Neutrinos •Axions •WIMPS •WIMPZILLAS •Phions Neutrinos •Exist and are as abundant as photons ~ 120/cm3 •Problems with large scale structure: relativistic particles => free streaming => suppression of small scale fluctuations. WMAP + 2dFGRS: h 0.0076(95% CL) 2 m 0.23 eV Dark matter candidates 2002 •Neutrinos •WIMPS •Axions •WIMPZILLAS •Phions 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 •Neutrinos •WIMPS •Axions ????? •WIMPZILLAS •Phions WIMPZILLAS •Decaimento no halo galáctico anisotropias Centro da galáxia Clumps •Grande produção de fótons e neutrinos de altas energias 90% pions (fotons e neutrinos), 10% protons Evento do Fly’s Eye não é foton! •Auger, HiRes, EUSO, EGRET, GLAST EGRET Z. Fodor hep-ph/0302036 Dark matter candidates 2002 •Neutrinos •WIMPS •Axions ????? •WIMPZILLAS •Phions Axions •Partículas que surgem em modelos sem violação de CP em interações fortes (simetria de Peccei-Quinn). •Candidato há anos •Axions são produzidos não-relativisticamente (cold dark matter) •Parâmetro fa : escala de quebra de simetria de PQ Axions •Massa: •Limites: ma = 10-5 eV (1012 GeV/ fa ) 10-6 eV < ma < 10-2 eV 1 SN1987A •Detecção via conversão de axion em 2 fotons dentro de cavidades ressonantes (gagg). C. Hagmann K. Bibber L. Rosenberg PDG junho 2002 Dark matter candidates 2002 •Neutrinos •WIMPS •Axions ????? •WIMPZILLAS •Phions WIMPS •Weakly Interacting Massive Particles: Partículas com massa típica de 100 GeV e que interagem 36 2 fracamente 10 cm •Existem naturalmente em extensões super simétricas do Modelo Padrão: Lightest Supersymmetric Particle (LSP). •Geralmente, LSP = neutralino. WIMPS • Candidato favorito da academia. • Cold Dark Matter (mWIMP>Tf ). •Abundância cosmológica pode ser calculada no MSSM: WIMP 2 1035 cm2 ani WIMPS •Detecção direta de WIMPS WIMP do halo Cristal de Ge, NaI 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 0.135 ±0.009 Automatic calculations II: micrOMEGAs micrOMEGAs: G. Belanger et al., IDM2002 tanb = 10 tanb = 50 Edsjo IDM2002 Data is starting to probe MSSM Edsjo - IDM2002 - Indirect searches New dark matter candidates 2003 •Neutrinos •WIMPS •Phions ????? •WIMPZILLAS •Axions •VAMPS VAMPS VAriable Mass Particles zzzzzzzzzzzzzzz VAMPS Idea: connection between dark matter and dark energy (Comelli, Pietroni and Riotto, hep-ph/0302080) mc 2 L ~ m0 exp(-2l f) 2 dark energy field (quintessence) 2 c dark matter field (VAMP) Slowly varying dark energy field acts as a time-dependent mass term for dark matter VAMPS Energy density of VAMPS: r c = mc n c ~ exp(-l f ) (a0/a(t))3 = exp(-l f ) exp(-3 x ) ; x = ln (a(t)/a0) VAMPS Quintessence: exponential potential rf ~V(f) = V0 exp( b f ) IF 3 f x x lb solves coincidence problem rf/rc ~ 1 for all times ! VAMPS This solution for f is an attractor VAMPS Comelli, Pietroni and Riotto, hep-ph/030280 New dark matter candidates 2003 •Neutrinos •Phions ????? •WIMPS •VAMPS •WIMPZILLAS •Axions •LKK Kaluza-Klein tower What if there are small extra dimensions? Klein-Gordon equation for a scalar field in 5-d: 2 2 2 2 f x , x5 0 2 x5 t Periodic b.c. (R is the radius of compact dimension) : 2nx5 f x , x5 x cos R 2 2 2n 2 x 0 2 t R 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/0209262 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, ...
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