2. Astroparticle physics 4. Astroparticles: rulers of the Universe? (or almost...) Alberto Carramiñana Instituto Nacional de Astrofísica, Óptica y Electrónica Tonantzintla, Puebla, México alberto@inaoep.mx Xalapa, 10 August 2004

3. 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

4. Oort’s limit Statistical study of motion of stars in the Solar neighborhood: first evidence of “missing mass”.

5. Dark Galactic halo Light: Mass: –inside solar circle –halo –extended halo 70% to 90% of the mass of the Milky Way is in the dark halo Clemens (1985)

6. MACHOs MAC HOMAssive Compact Halo Objects: –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 z  0.03 AGN  bounds on IR background  thermal emission from MACHOs

7. Galactic rotation curves They become flat  rigid rotation M/L  1 consistently

8. 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)  3  10 13 M  –M/L  750

9. 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)  3.3  10 15 M , M/L  660 (Zwicky 1933) X-ray intracluster  M  3  10 14 M  (baryonic) –cd galaxies 10 13 to 10 14 M , M/L  750 Local supercluster M  8  10 14 M  h -1, M/L  400h

10. 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

11. PSC-z Reshift survey for 15,000 galaxies from IRAS point source catalogue Saunders et al. 2000

12. 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/

13. 6dFGs First Data release March 2004: 52,000 redshifts (of 150,000) http://www.mso.edu.au/6DFGs/

14. 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)

15. SDSS power spectrum

16. 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,  =0.7 Colles (1998)

17. Cosmic Microwave Background Bennett et al. 2003

18. Local to LSS to CMB

19. Distant supernovae searches –Expanding Universe –Seeking for curvature: deceleration parameter

20. High Redshift Supernova –Seeking deceleration  acceleration!

22. Cosmology standard model

23. CMB Bennett et al. 2003

24. Cmbgg OmOl CMB Slides from Max Tegmark website

25. Cmbgg OmOl CMB + LSS

26. Cmbgg OmOl How much dark matter is there?

27. Cmbgg OmOl How much dark matter is there?

28. Cmbgg OmOl CMB How much dark matter is there?

29. Cmbgg OmOl CMB + LSS How much dark matter is there?.

30. Cmbgg OmOl Hubble constant and total matter density

31. Cmbgg OmOl CMB Hubble constant and total matter density

32. Cmbgg OmOl CMB + LSS Hubble constant and total matter density.

33. Cmbgg OmOl Neutrino fraction

34. Cmbgg OmOl CMB Neutrino fraction

35. Cmbgg OmOl CMB + LSS Neutrino fraction.

36. Cmbgg OmOl CMB + LSS How much dark energy is there? flat closed open

37. Cmbgg OmOl CMB + LSS Nature of the dark energy

38. Cmbgg OmOl CMB + LSS How flat is the Universe?

39. Cmbgg OmOl CMB + LSS How old is the Universe?

40. Cmbgg OmOl CMB + LSS

41. Dark matter particles Generate and collapse under gravity Very weak EM coupling (WIMPs). Categories –Hot (relativistic) VS cold (non relativistic) –Thermal relics VS non relics For a thermal relic WIMP –(1) known; (2) well motivated; (3) speculative Goldoni, astro-ph/0403064

42. Dark matter particles 1. known: neutrinos: –thermal relics –too hot; CMB + LSS ruled out. 2.1 neutralinos Lighest 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)

43. Dark matter particles 2.2 axions Non 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. speculative self interacting dark matter particles: to solve cusp and satellite problems Almost ruled out WIMPZILLAs mass  10 13 GeV Goldoni, astro-ph/0403064

44. The cosmic-ray connection!? WIMPZILLAs: produced at the end of inflation: –Stable –mean-life  age of Universe: decay beyond GZK limit

45. 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