Theory MRC: Episode I
Theory MRC: Episode I particles structures radiations
Theory MRC: Episode I coupp auger veritas sdss capmap spt quiet des
Theory = People Episode I Episode II Fellows: Chris Gordon Dragan Huterer* Hiranya Peiris* Yong-Seon Song* Xiaomin Wang Faculty: [Sean Carroll] Wayne Hu *externally funded It's the year 2005... KICP theorists are still the same. They'll do anything to get what they need. And they need postdocs and grad students. Fellows: Erin Sheldon Risa Wechsler* Andrew Zentner Faculty: [Josh Frieman] Andrey Kravtsov [Angela Olinto]?
Radiations: CMB Anomalies Low multipole alignments [Schwartz, Starkman, Huterer, Copi 2004]
Radiations: CMB Anomalies 2000 Correlated perturbations and low multipole power [Gordon & Hu 2004] ΘΘ l(l+1)c l /2π (µk 2 ) 6000 4000 adiabatic dark energy perturbations 10 l 100
Radiations: CMB Anomalies Explanations of low power distinguished by polarization & cross correlation [Gordon & Hu 2004]
Radiations: Inflation Tachyonic amplification of perturbations [Gordon & Wands 2005]
Radiations: Inflation Quintessential [Rosenfeld & Frieman 2005]
Radiations: Inflation Low entropy initial conditions for as thermal fluctuations in desitter [Carroll & Chen 2005]
Radiations: Inflation Features in the initial power spectrum: Trans-Planckian physics [Easther, Kinney & Peiris 2004; 2005]
Radiations: Inflation Features in the initial power spectrum: curvature features [Kadota, Dodelson, Hu & Stewart 2005] 0.08 0.07 0.06 0.05 0.04 0.03 0.02 0.01 0-0.01-0.02 ξ=20 ξ=25 ξ=30 ξ=35 0.001 0.01 0.1 k (Mpc -1 )
Radiations: Neutrinos CMB B-modes from lensing: non-gaussianity limits information on neutrinos [Smith, Hu, & Kaplinghat 2004] fractional power deviation 0.02 0.01 0-0.01-0.02 realizations Gaussian variance 100 l 1000
Radiations: Reionization 21cm emission removal of foregrounds with CMB techniques [Wang, Tegmark, Santos, & Knox 2005] 32.45 32.4 32.35 32.3 32.5 32.45 32.4 32.35 32.3 32.25 0.04 0.02 0-0.02-0.04 154.5 155 155.5 156
Structures: Dark Energy Dark energy probes in light of the CMB [Hu 2004b] 0.2 0.1 H-1/H-1 D/D H-1/H-1 D/D 0-0.1 G/G G/G (H 0 D)/H 0 D -0.2 (a) w DE =1/3 0.1 (H 0 D)/H 0 D 1 (b) w a =1/2; w 0 =0 0.1 1 0.02 (c) w a =1/2; w 0 =-0.15 (d) w DE =0.05; Ω T =-0.0033 D/D (H 0 D)/H 0 D 0.01 0-0.01-0.02 H-1/H-1 G/G 0.1 1 z H-1/H-1 (H 0 D)/H 0 D D/D G/G 0.1 1 z
Structures: Dark Energy Gravitational instability across phantom divide: internal degrees of freedom [Hu 2004c] -0.8-1 -1.2 true 2 field model w 0.01 D/D 0 H-1/H-1-0.01 (a) w a =0.5, w 0 =-1.15 0.1 z G/G 1 10
Structures: Dark Energy Clustering of the from galaxy-isw correlation [Hu & Scranton 2004] 10-7 z i =0.15 Θg l(l+1)c l /2π 10-8 3 10-9 1 0.15 ce=0.1 / ce=1 0.8 0.6 w=-0.8; c e =1 3 10 100 l
Structures: Dark Energy Ghost-condensate "unified" /energy tested by small scale structure [Giannakis & Hu 2005] 1 T Q (k) 10-14 ε 0 = 10-12 10-16 10-18 dark 0.1 energy numerical fit 0.01 0.1 k (Mpc -1 ) 1
Structures: Dark Energy Self-calibration of cluster counts [Lima & Hu 2005] 0.1 M 0 ρ m dn d lnm b 2 σ2 50 0.01 0.001 w=-1 w=-2/3 selection 10 13 10 14 M (h -1 M ) 10 15
Structures: Dark Energy Measuring both distances and growth tests modified gravity models [Song 2004; Knox, Song, & Tyson 2005]
Structures: Dark Energy Toward realistic forecasts for cosmic shear [Huterer & Takada 2004; Huterer & White 2005; Ma, Hu & Huterer 2005] n(z) 1.0 0.8 0.6 0.4 photo-z degeneracy 0.2 fractional change 0.1 0-0.1 1 2 3 z
Structures: Neutrinos Toward cosmological detection of neutrino mass with clusters [Wang et al 05]