Astroparticle physics

4. Astroparticles: rulers of the Universe? (or almost...)

Alberto CarramiñanaInstituto Nacional de Astrofísica, Óptica y Electrónica

Tonantzintla, Puebla, México

alberto@inaoep.mx

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

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LSS

Cmbgg OmOlHow much dark matter is there?

Cmbgg OmOlHow much dark matter is there?

Cmbgg OmOlCMB

How much dark matter is there?

Cmbgg OmOlCMB

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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

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LSS

Neutrino fraction .

Cmbgg OmOlCMB

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LSS

How much dark energy is there?

flat

closedopen

Cmbgg OmOlCMB

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LSS

Nature of the dark energy

Cmbgg OmOlCMB

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LSS

How flat is the Universe?

Cmbgg OmOlCMB

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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 MSSMSuperposition of neutral

higgsinos and gauginos weakly interactive and massive

Thermal coupled relicMass 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

meVExperimentally bounded:

about to be found or to be ruled out

3. speculativeself interacting dark

matter particles: to solve cusp and satellite problems

Almost ruled outWIMPZILLAsmass 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

alberto@inaoep.mx