Neutrino hot dark matter and

hydrodynamics of structure formation:Two “new” features of matter

Dr. Theo M. Nieuwenhuizen Institute for Theoretical Physics

University of Amsterdam

Harvard Smithsonian Center for Astrophysics

22 Jan 2010

Outline

A modeling of lensing in Abell 1689

Mass, properties, name of DM particle

Two types of dark matter

Dark matter condensation on cluster; reionization

Galactic dark matter: Gravitational hydrodynamics

The two types of dark matter

• Total mass of Universe: 4-5% baryons, 20-25 % dark matter,

• 70-75% dark energy

• Galactic dark mater: Oort 1931Detected by rotation curves, dwarf galaxies

• MACHOs: Massive Astrophysical Compact Halo Objects: Hydrodynamics: Milli Brown Dwarfs consisting of baryons

• Cluster dark matter: Zwicky 1932Detected from rotation curves, by lensing

• WIMPs Weakly Interacting Massive Particles• The dark matter of galaxy clusters is non-baryonic.

• Not MACHOs or WIMPs but MACHOs and WIMPs !!

• Abell 1689 galaxy cluster

• Nearby z = 0.184

• Total mass

• Luminous mass

• Baryon poor

• Einstein ring

M 10 31 15

M 10 4.4 11

IncompleteEinstein ringat 100/h kpc

Abell 1689Center

Dark matter acts ascrystal ball

Abell 1689

X-rayemitting gas

T=10 keV =1.16 10^8 K

Threecomponents:

Dark matterGalaxies

Gas

• Galaxycluster

• Abell 370

Strongest

gravitation lens:

20 times stronger than A1689

Hubble, after last repair May 2009

Theory

• Assume that DM comes from non-interacting fermions

in their common gravitational potential

• Mass m, degeneracy g; g = 2 (2s+1) #families

• Isothermal model for fermions

• Isothermal model for Galaxies and X-ray gas

• Virial equilibrium:

• 30% solar metallicity

Cowsik&McClelland 1973Treumann,Kull&Bohringer 2000Nieuwenhuizen 2009

Fit to A1689 lensing data of Tyson and Fischer ApJ 1995 Limousin et al, ApJ 2007

averageprojectedmass

radius

The mass of the dark matter particle

small statistical error 2%

reduced Hubble parameter

Previous estimates and searches: keV, MeV, GeV, TeV: excludedAdditional CDM component: excluded

= number of available modes in cluster

What is the dark matter particle?

The dark matter fraction

Early decouplers have small g: Not gravitinos, neutralinos, X-inos Not bosons, e.g. axions

Match possible to WMAP5 for =12

(anti) neutrinos, left+right-handed, 3 families: g = 2*2*3=12 mass = 1.45 eV

Neutrino oscillations cause small mass differences, 0.001 eV or less

SuperNovae Riess 09: h=0.74,

Macrolensing: h=0.65

Neutrinos in the cluster

Typical speed is non-relativistic, v = 490 km/s

Local density can be enormous: in Abell center: one billion in a few cc

Thermal length visible to the eye

Temperature is low

Smaller than would-be momentum temperature T_p=1.95 KLarger than would-be energy temperature T_E=0.0001 K

The biggest quantum structure in the Universe

normalized density: # neutrinos per cubic thermal wavelength per degree of freedom

N>1: quantum degenerate nu’sN=1: quantum-to-classical crossover

at r = 505 kpc = 1.6 million light year d = 2r = 3.2 million light yearThat is pretty big …

IncompleteEinstein ringat 100/h kpc

Abell 1689Center

Temperature of gas: 10 keV=10^8 K

Log(Mass)

Log(r/kpc)

Cluster radiates in X-rays like a star in light. Radiated energy supplied by contraction, as in stars.Radiation helps to maintain virial equilibrium.

Virial T of alpha-particles overlaps with it.

Virial equilibrium assumed; only amplitude adjusted

Why isothermal (virial) equilibrium?

• Lynden Bell: violent relaxation, faster than collisional

• Relaxation in time-dependent potential:every object (individual particle, galaxy) exchanges

energy with the whole cluster• Iff phase space density becomes uniform, then

Fermi-Dirac distribution• X-ray radiation helps to maintain the virial state,

as in the sun

CDM or HDM?• Cold Dark Matter: heavy particles already clumped at decoupling z=1100

• But light neutrinos are free streaming until trapped by galaxy cluster

• Free streaming

• Crossover when Newton force of baryons matches Hubble force Hp: z = 6 - 7

• Then cosmic voids loose neutrinos and become empty

• This heats the intracluster gas up to 10 keV, so it reionizes, without heavy stars

• Hot Dark Matter paradigm agrees with gravito-hydrodynamics

Gravitational hydrodynamics

• At decoupling: photon mean free path = 10^(-5) pc << horizon (Silk damping)

• Step 1: In the plasma

• Effect of viscosity important below z = 5000• Instability in plasma: proto-voids & proto-galaxy-clusters• Size of proto-voids*(z+1) = 40 Mpc now

• 13.6 eV recombination energy gives CMB T-fluctuationsof sub-Kelvin

Milky Wayregion in Crux

Gravitational hydrodynamics II• At decoupling: galaxies; Jeans clusters 40,000 solar mass

• Some Jeans clusters developed into globular star clustersOthers were used for ordinary stars

• Most still exist and are dark. These Jeans clusters act as isothermal “particles” forming the galactic dark matter

• Explains flattening rotation curves, Tully Fisher relation

• Explains galaxy mergers

• Milli-lensing “CDM” subhalos explained as Jeans clusters

• (Dwarf) galactic DM does NOT exclude neutrino DM

• Antennae galaxies:•

Two colliding galaxiescome within each othersdark matter sphere.

• Along their trajectories they transform severalcold Jeans clusters intoyoung globular star clusters.

NGC-2623: Two galaxies inside each others dark matter?

Jeans clusters warmed: new stars in young star clusters

Tadpole galaxy (HST)

Gravitational hydrodynamics III• At decoupling: fragmentation of Jeans clusters in milli brown dwarfs (MBDs) of terrestrial weight.

• Thousands of frozen MBDs observed in microlensing at unit optical depth (Schild 1996, 1999)

• 40,000 of heated MBDs in planetary nebulae counted in Spitzer infrared. Connected to hydrodynamics by Gibson&Schild 98-08

• Extreme Scattering Events: Earth-Jovian gas clouds observed in radio. Walker&Wardle 98: May be good fraction of galactic mass

• Multiple imaging of pulsars: by MBDs in Jeans clusters

• Explanation of H-alpha forest absorption lines

N,Gibson,Schild,EPL (2009) 0906.5801

Helix planetary nebula• Star exploded

• Became white dwarf

• Ca 40.000 “cometary knots” in radio

• = proto-gas balls

• Ca 1 earth mass

• Galactic dark matter = gas balls of earth mass: Macho’s

Summary • Observed DM of Abell 1689 cluster explained by thermal fermions of eV mass.

keV, MeV, GeV, TeV, PeV excluded. Thermal bosons (axions) excluded.

• Fitting with global dark matter fraction: 6 active + 6 sterile (anti-)neutrinosMass about 1.45 eV, depends on h

• Gas temperature 10^8 K = alpha-particle temp., gas profile matches automatically

• Free flow into potential well occurs at z = 6 - 7. Causes reionization, without heavy stars

• Neutrino Hot Dark Matter challenges Cold Dark Matter (CDM). • Dark matter particle was not (and should not be) observed in searches • ADMX, ANAIS, ArDM, ATIC, BPRS, CAST, CDMS, CLEAN, CRESST, CUORE, CYGNUS, (DAMA),

DAMIC, DEEP, DRIFT, EDELWEISS, ELEGANTS, EURECA, GENIUS, GERDA, GEDEON, FERMI-GLAST, HDMS, ICECUBE, IGEX, KIMS, LEP, LHC, LIBRA, LUX, NAIAD, ORPHEUS, PAMELA, PICASSO, ROSEBUD, SIGN, SIMPLE, UKDM, VERITAS, XENON, XMASS, ZEPLIN. AMANDA, ANTARES, EGRET.

• Neutrino mass tested in 2015 in Katrin search between 0.2 eV – 2 eV

Summary II

• Hydrodynamics is important before and at decoupling

• Predicts structure formation from baryons without CDM trigger

• Explains a wealth of observations

• Hydrodynamic structure formation is top-down

• So CDM cannot be right and its particle has not been found

• Even for the CMB peaks, it offers no explanation for the scatter of unbinned data, or for the regime l=3000-8000. Turbulence does.

• Hydrodynamics connects structure formation to turbulence.

Do non-relativistic neutrinos constitute the dark matter?

Th. M. N.

Europhysics Letters 86 (2009) 59001

Gravitational hydrodynamics of large-scale structure formationTh. M. N., Carl H. Gibson, Rudy E. Schild

Europhysics Letters 88 (2009) 49001

Psalm 118:22

The stone which the builders refused

is become the head stone of the corner

KArlsruhe TRItium Neutrino Experiments