SFB 443 Bosen workshop 2010 Dark Matter -- Astrophysical Evidences and Terrestrial Searches Klaus Eitel, Karlsruhe Institute of Technology, KCETA, IK KIT University of the State of Baden-Württemberg and National Large-scale Research Center of the Helmholtz Association www.kit.edu
Content of the lecture Lecture 1: Lecture 2: Lecture 3: Lecture 4: review of astrophysical evidences for DM cosmological LCDM concordance model structure formation DM in our neighbourhood DM particle candidates: axions, neutralinos,... interaction models of DM with ordinary matter indirect detection (cc annihilation) & production direct detection strategies methods of direct detection general challenges experiments for direct search (I) experiments for direct search (II) results evidences? direct indirect production actual status (and outlook) 2
Astronomical evidences for DM 1933: F. Zwicky postulates the existence of non-luminous gravitationally interacting matter ( Dark Matter ) to explain the peculiar velocities of galaxies in the Coma cluster virial theorem: E kin 1 2 U pot E dark matter ~90% of the COMA cluster? F. Zwicky Helv.Phys.Acta 6 110-127 (1993) Die Rotverschiebung von extragalaktischen Nebeln s Fritz Zwicky (1898-1974) 3
Astronomical evidences for DM rotation curves (orbital speed vs radius) of galaxies orbital velocity ~ 1 a distance to center rotation of M33: Doppler shift at l=21cm, Radio:VLA&WRST 4
Astronomical evidences Kepler s law: rotation velocity v rot of a star of mass m around a central inner mass M r : M r r( r) dv (galactic bulge: r(r)=r 0 =const. r<5kpc outside: r(r)~0 M r =const. v rot ~r -1/2 ) v rot ~ const. r(r)~r -2 outside bulge Dark Matter halo in galaxy Better: luminous matter in DM halo! 5
Astronomical evidences for DM multitude of galaxy rotation curves Vera Rubin spherical halo model with Y. Sufue et al., Central rotation curves of spiral galaxies, Astrophys. J. 523 (1999) 136 146 making up 80% to 90% of the galactic matter 6
Astronomical evidences for DM strong gravitational lensing: DM makes light bend strong lensing of Cl0024+1654 (z = 0.39) viewed by Hubble Space Telescope 33 images of 11 galaxies Astronomy Picture of the Day http://antwrp.gsfc.nasa.gov/apod/ap090823.html 7
Astronomical evidences for DM weak gravitational lensing: DM creates shear image ellipticity shear invert the equation RXJ1347.5-1145 (Bradac et al 2005) DM reconstruction 8
optical depth (fraction of halo mass) Astronomical evidences for DM micro-lensing by baryonic objects (MACHOs) P. Tisserand et al. (EROS-2) Astron.Astrophys.469:387-404,2007 MACHO candidate (Astrophys.J 542:281, 2000) MACHOs in the mass range 6 10 8 M < M < 15M are ruled out as the primary occupants of the Milky Way Halo 9
Astronomical evidences for DM galaxy cluster 1E 0657-56 bullet cluster Chandra X-ray d=1gpc z=0.296 first evidence that DM halo is not made of normal baryons! HST (weak lensing) (Credit: X-ray: NASA/CXC/CfA/M.Markevitch et al. Optical: NASA/STScI; Magellan/U.Arizona/D.Clowe et al. Lensing Map: NASA/STScI; ESO WFI; Magellan/U.Arizona/D.Clowe et al.) 10
Astronomical evidences for DM crossing of two galaxies as an example of the dynamics of DM and hot baryons DM: dissipationless, no interaction during X ing baryons and DM mixed start of crossing baryons: cluster gas is heated through collisions during crossing shock of the cluster gas baryons and DM separated spatial separation of DM and baryons 11
Astronomical evidences for DM 2.7K CMBR (WMAP) WMAP, Astrophys. J Suppl 180:296, 2009 DT/T 10-5 at z 1000 (300.000y after BigBang) k=0 r= r crit W tot = 1 r B 0.04r crit PDG2006 BBN (3 min. after BB) 12
Astronomical evidences for DM smooth structured structure forms by gravitational instability of primordial density fluctuations Jeans: fluctuations grow as 2 3 1 ( t) t R( t) with R( t) (1 z) ( t0, z 0) 1000 ( tdec, z 1000) 10 2 13
Structure formation - observations on large scales (LSS) 2dF Galaxy Redshift Survey 14
Structure formation - observations on large scales (LSS) SDSS Galaxy Redshift Survey Astrophys.J.657:645,2007 15
P(k) DT (mk) P(k) Cold or Hot DM? Galaxy Distribution (2dF, PSCz) Scales 1 200 Mpc 10 6 10 5 10 4 10 3 10 2 0.01 k (h/mpc) 0.10 W 0 = 1 W L = 0.66 W B = 0.04 H 0 = 72 n s = 0.94 W n = 0.00 0.05 0.10 0.15 0.20 0.25 Adapted from S.Hannestad (and G. Raffelt) Lyman-a forest at large redshift z = 2.72 Scales 0.1 10 Mpc 10 10 10 9 10 8 10 7 10 6 10 5 10 4 0.01 0.1 1 10 k (h/mpc) 16 100 80 60 40 20 0 CMBR (WMAP, Maxima, Boomerang, CBI, DASI) 0 200 400 600 800 1000
DT (mk) P(k) P(k) Cold or Hot DM? HDM? extreme case: W L 10 6 10 5 10 4 10 3 10 2 0.01 k (h/mpc) 0.10 taking W n =Σm n /93eV and m n <2.2eV from laboratory*: 10 10 10 9 10 8 10 7 10 6 10 5 10 4 0.01 0.1 1 10 k (h/mpc) 100 80 60 CMBR (WMAP, Maxima, Boomerang, CBI, DASI) W n W b W CDM W n < 0.13 *Mainz n experiment 40 20 0 0 200 400 600 800 1000 17
DT (mk) P(k) P(k) Cold or Hot DM? CDM! LCDM case: WW L L 10 6 10 5 10 4 10 3 10 2 0.01 k (h/mpc) 0.10 taking W n =Σm n /93eV and m n <0.2eV <2.2eV from cosmology: laboratory: 10 10 10 9 10 8 10 7 10 6 10 5 10 4 0.01 0.1 1 10 k (h/mpc) 100 80 60 CMBR (WMAP, Maxima, Boomerang, CBI, DASI) W n W n < 0.13 0.013 40 20 W n W b W CDM W CDM 0 0 200 400 600 800 1000 18
Astronomical evidences for DM are given from: peculiar velocities of galaxy clusters rotation curves of galaxies galaxy cluster crossing (bullet galaxy) strong lensing of galaxy clusters weak lensing (shear) of galaxies NO convincing micro-lensing by MACHOs structure formation in the early universe power spectrum of CMBR CMBR fluctuations and structure growth BBN (abundance of light elements) 19
Cosmological standard model: LCDM concordance model parameters of the LCDM concordance model (PDG 2009): Hubble constant H 0 = h. 100km/s/Mpc; h = 0.705 ± 0.013 total energy density Ω tot = 1.006 ± 0.006 total matter density W m h 2 = 0.136 ± 0.004 baryon density W b h 2 = 0.0227 ± 0.0006 cosmological constant (Dark Energy) W L = 0.726 ± 0.015 total neutrino mass Sm n < 0.62 ev (95% C.L.) t=t 0 (BB+13.6Gyr) W L r crit = 3H 02 /8pG N = 1.05. 10 5 h 2 GeV/cm 3 5.6 GeV/m 3 non-baryonic Cold Dark Matter W b Wnon-b CDM 20
Do we understand structure formation? 1. calculate structure growth on different scales and compare with LSS surveys quantifying density fluctuations power spectra 2. reproduce structure formation in N-body simulations assuming gravitational interaction only be aware: N ~ 10 10 each particle is a macroscopic DM clump 22
structure formation Millenium Simulation Redshift z=18.3 (t = 0.21 Gyr) http://www.mpa-garching.mpg.de/galform/millennium/ 10 10 particles of ~10 9 M DM as seed for clusters and galaxies Dr/r~10-3 after inflation 23
structure formation Millenium Simulation Redshift z=5.7 (t = 1.0 Gyr) 24
structure formation Millenium Simulation Redshift z=1.4 (t = 4.7 Gyr) 25
structure formation Millenium Simulation Redshift z=0 (t = 13.6 Gyr) 26
structure formation MS of a galaxy cluster CDM only CDM with baryonic galaxies superimposed structure formation on large (>clusters) scales can be understood based on CDM fluctuations DM distribution on galactic scales? DM halos to describe rotation curves? 27
Structure formation within LCDM power spectrum from CMB to galaxy clusters compilation by M. Tegmark 28