astroparticle physics 4. astroparticles: rulers of the universe? (or almost...) alberto carramiñana...
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Astroparticle physics
4. Astroparticles: rulers of the Universe? (or almost...)
Alberto CarramiñanaInstituto Nacional de Astrofísica, Óptica y Electrónica
Tonantzintla, Puebla, México
Xalapa, 10 August 2004
The composition of the Universe
• Planets.• Stars: nuclear burning &
degenerate corpses.• Gas, dust (magnetic
fields (cosmic-rays)).• Galaxies: normal, active.• Cosmological
background(s).
• Protons, neutrons baryons.
• Electrons, muons leptons.
• Neutrinos.
• Mesons hadrons quarks.
Early Universe / Cosmic-rays / astrophysical neutrinos /
non baryonic dark matter / dark energy
Oort’s limit
• Statistical study of motion of stars in the Solar neighborhood: first evidence of “missing mass”.
Dark Galactic halo
• Light:
• Mass:– inside solar circle
– halo
– extended halo70% to 90% of the mass of theMilky Way is in the dark halo
Clemens (1985)
MACHOs
• MAMAssive CCompact HHalo OObjects:– white or red dwarfes, neutron stars, black holes...
• Searched (and found!) through microlensing events (Alcock et al. 1993) but– Statistics: too few MACHOs for the Galactic halo.– HST: red dwarfes < 6% of halo mass.– TeV detections of z0.03 AGN bounds on IR
background thermal emission from MACHOs
Galactic rotation curves
• They become flat rigid rotation
• M/L 1 consistently
M87 X-ray halo
• M87: giant elliptical. Brightest Virgo galaxy
• X-ray emission extends up to 300 kpc– thermal fre-free emission
– M(300 kpc) 31013 M
– M/L 750
Dynamics of groups and clusters
• Local group– M31 & Milky Way
M/L 50 to 70
– Magellanic stream M/L
80
• Groups of galaxies M/L 400h
• Clusters of galaxies– Coma cluster
977 km/s M(3 kpc) 3.31015 M,
M/L 660 (Zwicky 1933) X-ray intracluster M 31014 M (baryonic)
– cd galaxies 1013 to 1014 M, M/L 750
• Local supercluster M 81014 Mh-1, M/L 400h
Surveys of Large Scale structure of the Universe
• PSC-z: 15,000 galaxies from IRAS all-sky survey
• 2dF – 6dF: wide field spectrospic survey
• 2Mass: IR photometry of 30 million objects
• SDSS: photometric (100 million) and spectroscopic (> 1 m)
• HDF North & South: deep HST exposures on narrow field UDF
• GOODS: common HST, CXO, Spitzer fields
• ELAIS: from ISO
PSC-z
• Reshift survey for 15,000 galaxies from IRAS point source catalogue
Saunders et al. 2000
2dF Galaxy Survey
• AAO + Cambridge + Durham + Edinburgh
• 220,000 redshifts• Power spectrum of
galaxy clustering up to 300 h-1 Mpc
(Percival et al. 2001, +....) http://www.mso.anu.edu.au/2dFGS/
6dFGs
• First Data release March 2004: 52,000 redshifts (of 150,000)
http://www.mso.edu.au/6DFGs/
Sloan Digital Sky Survey
• Spectrophotometric survey of ¼ of all sky– Photometry for 100 million objects– Spectra for > 1 million objects
• With a 2.5 m robotic survey telescope.
• Data releases:– EDR: 14 million / 83,000 (Stoughton et al. 2002)
– DR1: 53 million / 186,000 (Abazajian et al. 2003)
– DR2: 88 million / 367,000 (Abazajian et al. 2004)
SDSS power spectrum
Large Scale Structure simulations
lss_nbody & nbody_sim
movies by the Virgo Consortium
• CMB = Initial conditions• Work better from CDM and 0
0=1, CDM M=0.3, =0 M=0.3, =0.7Colles (1998)
Cosmic Microwave
Background
Bennett et al. 2003
Local to LSS to CMB
Distant supernovae searches
– Expanding Universe– Seeking for curvature: deceleration parameter
High Redshift Supernova
– Seeking deceleration acceleration!
Cosmology standard model
CMB
Bennett et al. 2003
Cmbgg OmOlCMB
Slides fromMax Tegmarkwebsite
Cmbgg OmOlCMB
+
LSS
Cmbgg OmOl
How much dark matter is there?
Cmbgg OmOlHow much dark matter is there?
Cmbgg OmOlCMB
How much dark matter is there?
Cmbgg OmOlCMB
+
LSS
How much dark matter is there? .
Cmbgg OmOlHubble constant and total matter density
Cmbgg OmOlCMB
Hubble constant and total matter density
Cmbgg OmOlCMB
+
LSS
Hubble constant and total matter density .
Cmbgg OmOlNeutrino fraction
Cmbgg OmOlCMB
Neutrino fraction
Cmbgg OmOlCMB
+
LSS
Neutrino fraction .
Cmbgg OmOlCMB
+
LSS
How much dark energy is there?
flat
closedopen
Cmbgg OmOlCMB
+
LSS
Nature of the dark energy
Cmbgg OmOlCMB
+
LSS
How flat is the Universe?
Cmbgg OmOlCMB
+
LSS
How old is the Universe?
Cmbgg OmOlCMB
+
LSS
Dark matter particles
• Generate and collapse under gravity
• Very weak EM coupling (WIMPs).
• Categories– Hot (relativistic) VS cold (non relativistic)
– Thermal relics VS non relicsFor a thermal relic WIMP
– (1) known; (2) well motivated; (3) speculative
Goldoni, astro-ph/0403064
Dark matter particles
1. known: neutrinos: – thermal relics– too hot; CMB + LSS
ruled out.
2.1 neutralinosLighest super-sym
particle of MSSM
Superposition of neutral higgsinos and gauginos weakly interactive and massive
Thermal coupled relic
Mass range: 40 GeV 4 TeV (WMAP)
Dark matter particles
2.2 axionsNon thermal relics:
produced by cosmic strings or vacuum alignment
Photon coupling?
“Useful range”: eV to meV
Experimentally bounded: about to be found or to be ruled out
3. speculativeself interacting dark
matter particles: to solve cusp and satellite problems
Almost ruled out
WIMPZILLAs
mass 1013 GeV
Goldoni, astro-ph/0403064
The cosmic-ray connection!?
• WIMPZILLAs: produced at the end of inflation:– Stable – mean-life age of Universe: decay beyond
GZK limit
These presentations
Available (soon!) as http://www.inaoep.mx/alberto/cursos/ap2004_1a.ppt http://www.inaoep.mx/alberto/cursos/ap2004_1b.ppt http://www.inaoep.mx/alberto/cursos/ap2004_2.ppt http://www.inaoep.mx/alberto/cursos/ap2004_3.ppt http://www.inaoep.mx/alberto/cursos/ap2004_4.ppt