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Delve into the mysteries of the universe, from the Big Bang theory to dark matter and cosmic rays. Celebrate cosmic discoveries and ponder unanswered questions. Join the journey through the cosmos with groundbreaking insights from the Vèmes Rencontres du Vietnam 2004.
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New Views on the Universe Vèmes Rencontres du Vietnam August 2004 Angela V. Olinto Astronomy & Astrophysics Kavli Institute Cosmol. Phys. Enrico Fermi Institute University of Chicago
Much to celebrate! • Success of the Big Bang theory • Flat Universe (Inflationary prediction) • Discovery of Universe’s Acceleration • Discovery of Neutrino mixing mass • Gamma-ray Bursts Cosmolog.+ Counterparts • Black Holes in every galaxy! • TeV Gamma-ray Sources Many questions remain... Vèmes Rencontres du Vietnam 2004
The Big Bang We live in a Homogeneous & Isotropic Universe described by (a Robertson-Walker metric & Friedmann’s equation derived from) Einstein’s General Relativity. It began 13.7 billion years ago, and is composed of... Celebrate Einstein Centennial!
Evidence for Isotropy: The Microwave Sky! T = 2.725 0.002 K
b Big Bang Nucleosynthesis Theory vs. Observations: Remarkable agreement over 10 orders of magnitude in abundance variation Concordance region: b h2 = 0.02 For h=0.7, b = 0.04. Deuterium: strongest constraint 4He
add Inflation and we can explain...
Brief History of the Universe Inflation exponential expansion
Homogeneity & Isotropy Horizon of observer B at time of decoupling A B Big Bang t=0 Us, today Photon Decoupling (Last Scattering Surface) t=300,000 yr CMB naturally appears isotropic
V() Quantum Fluctuations of the `Inflaton’ Field ==> Density Perturbations field V() space field
Today Scale grow 3000 Mpc 1 Mpc stretch inside outside inside Time Before inflation Radiation Domination Matter Domination During inflation Dark Energy Domination
High-Resolution Simulations of Cold Dark Matter (CDM) Halos
CMB Anisotropies tU =380,000 yr, T 10-5 T
WMAP Precision Cosmology
Inflation predicts: FLAT Universe
Dark Energy? total = +DM +b = 0.73, DM = 0.23, b = 0.04
SnIa WMAP (h fix) LSS 2dF
Radiation - Matter - Vacuum (Dark Energy?) (a) a-4 a-3 const a Early Universe today
Expect dq/dz Riess et al. ApJLett 04, HST 16 SNIa
Towards = 1 closed expands forever recollapses open
Much to celebrate! • Success of the Big Bang theory • Flat Universe (Inflationary prediction) • Discovery of Universe’s Acceleration • Discovery of Neutrino mixing mass • Gamma-ray Bursts Cosmolog.+ Counterparts • Black Holes in every galaxy! • TeV Gamma-ray Sources
Official detections by H.E.S.S. Crab Nebula (2003, 3 Tel.) - 54 sigma PKS 2155 (2003, 2 Tel.) - 45 sigma Mrk 421 (2004, 4 Tel.) - 71 sigma PSR B1259 (2004, 4 Tel.) - 8 sigma RX J1713 (2003, 2 Tel.) - 20 sigma Sagittarius A* (2003. 2 Tel.) - 11 sigma Linton, WatsonFest, Leeds July 2004
HESS Galactic Center! Linton, WatsonFest, Leeds July 2004
What is the Dark Matter? F. Zwicky Coma cluster
HESS Galactic Center neutralino m > 10 TeV ??? Linton, WatsonFest, Leeds July 2004
Many questions remain • What is the Dark Matter? • What is the Dark Energy? • What is the origin & max energy of cosmic rays? • Astro-Physics at high energy, curvature, and/or density? • What are the neutrino masses and underlying theory? • Why is there something rather than nothing? • Is there A Fundamental Theory? Quantum Gravity, Large Extra-Dimensions, Strings, M-theory,...? • How did the Universe Begin?
Cosmological Constant Natural scale for : Contrast with: + coincidence… ~M
Many questions remain • What is the Dark Matter? • What is the Dark Energy? • What is the origin & max energy of cosmic rays? • Astro-Physics at high energy, curvature, and/or density? • What are the neutrino masses and underlying theory? • Why is there something rather than nothing? • Is there A Fundamental Theory? Quantum Gravity, Large Extra-Dimensions, Strings, M-theory,...? • How did the Universe Begin?
Cosmic Rays • 1912 discovered by Victor Hess • (after Wilson & others) • Energy range: • ~ 109 eV to > 1020 eV • 1938Pierre Auger discovered • Extensive Air Showers (EAS) ORIGIN? Unknown! soon to be a Century Old Puzzle! at all energies…
HESS 2 smoking guns CR acceleration! Galactic Centre - 11 RX J1713 - 20 Linton, WatsonFest, Leeds July 2004
CRs at the Highest Energies Great Opportunity for Discovery can traverse longer distances than photons can point back to the source should have spectral features
cosmic rays / / / / / / / / / / / n
UHE proton trajectories in Extra Galactic B at the Highest Energies (1020 eV)) - should point to sources (unless Magnetic Fields are stronger &/or Z is larger) Isola, Lemoine, Sigl ‘02 lower bound 2 1019 eV to 3 1020eV, E-2.4 injection, BMpc ~0.3 G, Kolmog
6 doublets 1 triplet above 4 x 1019 eV < 2.5 deg AGASA above 1019 eV Log E>19.4 Log E>19.6
HiRes HiRes-I Monocular Data, E > 1019.5 eV No clustering seen so far! HiRes-I Monocular Data, E > 1018.5 eV Upper limit of 4 doublets (90% c.l.) in HiRes-I monocular dataset. HiRes Stereo
CRs at the Highest Energies can traverse longer distances than photons can point back to the source should have spectral features
-resonance multi-pions High Energy Proton sees Cosmic Microwave Background as High Energy Gamma Rays! WMAP p+cmb + p + 0 n + + Proton Horizon GZK Cutoff Greisen ‘66, Zatsepin & Kuzmin ‘66
GZK feature is source & B dependent… E. Parizot et al. ‘03
AGASA High Energy Spectrum AGASA: ~ 11 events above 1020 eV!!!
Statistics Fluctuations at GZK feature are large for AGASA & HiRes 400 realizations of GZK feature for low statistics DeMarco, Blasi, & A.O. ‘03
Auger (S) x AGASA DeMarco, Blasi, A.O. ‘03
Pierre Auger Project • 2 Giant AirShower Arrays • South – Argentina Funded • North – Not Yet Funded • 1600 particle detectors over • 3000 km2 • + 4 Fluorescence Detectors • Will Measure Direction, • Energy, & Composition of • ~ 60 events/yr E > 1020eV • ~ 6000 events/yr E > 1019eV > 250 scientists from 16 countries Vietnam! J. Cronin and T. Yamamoto