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Materia Oscura y Neutrinos

L. VillaseñorIFM-UMSNHRed de Altas EnergíasTaxco, Gro. 4-7 de marzo, 2009

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Contenido

Evidencias de materia oscura (MO) Candidatos de MO Detecciones Directas e Indirectas Experimentos Presentes y Futuros Discusión

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A Mexicangroup submitted a proposal to study DM in anunderground labto Conacyt in 2007

R&D money willpossibly be granted in2009

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Evidence for Dark Matter

Fritz Zwicky (1933) measured thevelocities of the individual galaxies. He concluded that“dark” matter is required to hold the cluster

Coma cluster, 350 M ly

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Evidence for Dark Matter Flat Rotation

curves of Galaxies. Rubin and W.K. Ford (1970) “What you see is not what you get.”

Modified Newtonian Dynamics (Moglim 1983) Modified Gravity such as Scalar tensor vector

gravity theory (Moffat 2006)

Alternative Explanations

• vc ~ r 1/2

Local density : 0.3 GeV/cm3

7M. Persic et al. 1996

Measured over and over

Each plot contains 50-100galaxiesaccording to luminosity

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Widths of curves indicate 95% CL for the abundance predictions

Measurements are shown as boxes.

Non baryon dark mass is required!

D. Tytler, J. M. O’Meara, N. Suzuki, and D. Lubin, astro-ph/0001318

BB Nucleogenesis: Determines the present baryon mass density to only ~ 4% of critical density

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Evidence for Dark Matter

Bullet Cluster(Clowe et al., 2006)

two collidingClusters of Galaxies at a distance of about 3.4 billion light years

evidence against Modified Newtonian Dynamics (MOND)

NASA RELEASE 06-297: "These observations provide the strongest evidence yet that most of the matter in the universe is dark"

White – VisibleRed – X RaysBlue - Grav. Lensing

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Evidence for Dark Matter

Lambda-Cold Dark Matter (concordance) model explains cosmic microwave background observations (WMAP), as well as large scale structure observations (Sloan Digital Sky Survey) and supernovae Ia data of the accelerating expansion of the universe.

The Composition of the Universe

Cómo afecta la MO al sistema solar?

Kepler equivocado?

Dentro de la órbita terrestra se espera que haya ~ 10^10 kg

Mientras que la masa del sol es 10^33 kg y de la tierra 10^24 kg

Por lo tanto no se espera ningún efecto detectable.

Particle Candidate for Cold Dark Matter: WIMP Weakly Interacting Massive Particle

Stable, TeV scale, electrically neutral, only weakly interacting

No such candidate in the Standard Model Good candidate: neutralino, Lightest

Supersymmetric Particle (LSP) in SUSY with m ~ 10 GeV to 10 TeV

Linear combination of the zino, the photino and the neutral higgsinos

May be produced at the LHC

Particle Candidate for Dark Matter

But there are many other possibilities (techni-baryons, gravitino, axino, invisible axion, WIMPZILLAS (Godzilla-sized version of WIMPS, ruled out by Auger data), etc)

WIMP Dark Matter Produced in early Universe They are in thermally equilibrium

at high temperature Decouple when expansion rate ~

interaction rate Density left-over from

annihilation depends on cross section

E.W. Kolb and M.S. Turner, The Early Universe

X=m/Temperature (time )

Com

oving number

density

Nequillibrium

Increasing<Av>

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WIMP DETECTIONDirect Detection

of halo particles in terrestrial detectors CDMS-II, ZEPLIN Edelweiss, DAMA, GENIUS, etc

f f

Scattering

(direct) Detection method We can expect is only a collision with

ordinary matter.

Electron recoil does not give enough energy but nuclear recoil gives ~100keV if mDM~O(100GeV).

Dark Matterparticle

Energy deposit

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WIMP DETECTION

f

fAnnihilation

Indirect Detection SuperK, AMANDA,

ICECUBE, GLAST

p

e+

_

•Search for neutrinos, gamma rays, radio waves, antiprotons, positrons in earth- or space-based experiments

Direct and indirect methods are complementary techniques along with a possible discovery at the LHC

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WIMP signatures (DirectDet) Nuclear recoils

Neutrons (produce similar recoils with sigma 1020 higher, 108-9 background reduction needed

Recoil spectrum shape

Exponential (as most bkg) Shape for backgrounds : electron/nuclear recoils

Absence of multiple scattering (against neutron) Uniform rate throughout volume (against surface radioactivity) Directionality of nuclear recoils Annual rate modulation

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WIMP signatures (Direct Det)

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Current direct detection experiments

running 3 to 10 kg Liquid XeLight+ IonizationSurface to GS

XENON

running6 kg Liquid XeLight+ IonizationBoulby mineZEPLIN II

running20 g FreonBubble chamberSNOPICASSO

stopped0.262 kg Al2O3Heat + LightGran SassoCRESST-I

running50 g Al2O3 + 67 g Ge + 54 g CaWO4

Heat + LightCanfrancROSEBUD

stopped 46 kg NaILightBoulby mineNaIAD

running2 to 7 kg Ge + 0.4 to 1.4 Kg Si

Heat + IonizationSoudan mine

CDMS-II

running0.6 to 9.9 kg CaWO4Heat + LightGran SassoCRESST-II

running ???10 to 40 kg Ge in N2IonizationGran SassoGENIUS-TF

running41 kg TeO2HeatGran SassoCUORICINO

In istallation10 to 30 kg GeHeat + IonizationModaneEDELWEISS-II

stopped1 kg GeHeat + IonizationModaneEDELWEISS-I

stopped 1 Kg Ge + 0.2 Kg SiHeat + IonizationStanfordCDMS-I

stopped4 kg Liquid XeLightBoulby mineZEPLIN-I

running250 kg NaILightGran SassoLIBRA

stopped100 kg NaILightGran SassoDAMA

stopped2 kg Ge DiodesIonizationCanfrancIGEX

stopped0.2 kg Ge diodesIonizationGran SassoHDMS

StatusMaterialTechniqueLocationNameDiscrimination

Even

t-by

-ev

ent

Stat

istic

al

Non

e

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B. SadouletKEKTC6

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Based in Gran Sasso lab (3500 mwe)

100 kg of NaI(Tl) Exposure : 107731 kg.d Coincidence between 2 PMTs Pulse shape rejection inefficient

at 2 keVee

NaINaINaINaI

PM

T PM

T

NaI scintillation : DAMA

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NaI scintillation : DAMA

Used annual modulation Claim annual modulation at

6.3σ over 7 annual cycles Mχ ~ 52 GeV/c² σn ~ 7.2 10-6 pb

Not compatible with other experiments (CDMS, ZEPLIN, EDELWEISS)

Future = LIBRA (250 kg of NaI)

Single-hits events residual rates

DM density ~0.3GeV/cc100GeV WIMPs 1 WIMP / 7cm cubic, =105/cm2/sec

Peccei y Quinn (1977)Wilczek lo llamó axion “por limpiar QCD”

Particle Candidate for Cold Dark Matter: AXION

B ~ 5 T Q ~ 200 000 Desde 1995

Límite astrofísico m

a < 2x10-3 eV SN1987a y laboratorios

Límite cosmológico rhoa /rho

o< 1

ma > 10-6 eV Supercuerdas

High Electron Mobility Transistor --> Amplificadores de RF con SQUIs

IceCube

AMANDA’s BIG BROTHER: 1 km3 of Ice 4200 PMTs on 70 Strings 1450-2450 m ~10 Angular Resolution to Mu Neutrinos IceTop Air Shower Array to

Veto Downgoing Muons• Digitized/Time-Stamped at 1 GHz

Each PMT • Started Deploying 2005;• Construction Finished ~2011

Deteccion de anti-neutrinos en Laguna Verde

como propuesta de la RAE

0 50 100 150 200 250 300days

0.0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

inpu

t in

fissi

ons

235U

239Pu

238U

241Pu

ProyectoAngraen Rio

Simulacion con root (50 K antineutrino events)

Azul-- Espectro U235Rojo-- Espectro Pu239

85% U23515% Pu239

Kathy Turner, 24May2006 36

Gamma-ray Large Area Space Telescope GLAST Large Area Telescope (LAT)

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GLAST will have a very broad science menu that includes:• Systems with supermassive black holes (Active Galactic Nuclei)• Gamma-ray bursts (GRBs)• Pulsars• Solar physics• Origin of Cosmic Rays• Probing the era of galaxy formation, optical-UV background light• Solving the mystery of the high-energy unidentified sources• Discovery! Particle Dark Matter? Other relics from the Big Bang? Extra dimensions? Testing Lorentz invariance. New source classes.

•GLAST will search for WIMP annihilation into gamma rays from the galactic center, galactic halo, galactic satellites and extragalactics

• Llaunched in 2008, will survey the gamma-ray sky in the energy range of 20MeV-300 GeV.

• The existence of Nonbaryonic Dark Datter has been definitely established

• CDM is favoured• Supersymmetric particles (in particular, neutralinos)

are still among the best-motivated candidates• New direct and indirect detection experiments will

reach deep into theory parameter space• The various indirect and direct detection

methods are complementary to each other and to LHC

• The hunt is going on – many new experiments coming!

• The dark matter problem may be near its (s)solution…

Conclusion