Theory MRC: Episode I. dark matter. theory. inflation. dark energy

Transcription

1 Theory MRC: Episode I

2 Theory MRC: Episode I particles structures radiations

3 Theory MRC: Episode I coupp auger veritas sdss capmap spt quiet des

4 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 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]?

5 Radiations: CMB Anomalies Low multipole alignments [Schwartz, Starkman, Huterer, Copi 2004]

6 Radiations: CMB Anomalies 2000 Correlated perturbations and low multipole power [Gordon & Hu 2004] ΘΘ l(l+1)c l /2π (µk 2 ) adiabatic dark energy perturbations 10 l 100

7 Radiations: CMB Anomalies Explanations of low power distinguished by polarization & cross correlation [Gordon & Hu 2004]

8 Radiations: Inflation Tachyonic amplification of perturbations [Gordon & Wands 2005]

9 Radiations: Inflation Quintessential [Rosenfeld & Frieman 2005]

10 Radiations: Inflation Low entropy initial conditions for as thermal fluctuations in desitter [Carroll & Chen 2005]

11 Radiations: Inflation Features in the initial power spectrum: Trans-Planckian physics [Easther, Kinney & Peiris 2004; 2005]

12 Radiations: Inflation Features in the initial power spectrum: curvature features [Kadota, Dodelson, Hu & Stewart 2005] ξ=20 ξ=25 ξ=30 ξ= k (Mpc -1 )

13 Radiations: Neutrinos CMB B-modes from lensing: non-gaussianity limits information on neutrinos [Smith, Hu, & Kaplinghat 2004] fractional power deviation realizations Gaussian variance 100 l 1000

14 Radiations: Reionization 21cm emission removal of foregrounds with CMB techniques [Wang, Tegmark, Santos, & Knox 2005]

15 Structures: Dark Energy Dark energy probes in light of the CMB [Hu 2004b] H-1/H-1 D/D H-1/H-1 D/D 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 = (c) w a =1/2; w 0 =-0.15 (d) w DE =0.05; Ω T = D/D (H 0 D)/H 0 D H-1/H-1 G/G z H-1/H-1 (H 0 D)/H 0 D D/D G/G z

16 Structures: Dark Energy Gravitational instability across phantom divide: internal degrees of freedom [Hu 2004c] true 2 field model w 0.01 D/D 0 H-1/H (a) w a =0.5, w 0 = z G/G 1 10

17 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 ce=0.1 / ce= w=-0.8; c e = l

18 Structures: Dark Energy Ghost-condensate "unified" /energy tested by small scale structure [Giannakis & Hu 2005] 1 T Q (k) ε 0 = dark 0.1 energy numerical fit k (Mpc -1 ) 1

19 Structures: Dark Energy Self-calibration of cluster counts [Lima & Hu 2005] 0.1 M 0 ρ m dn d lnm b 2 σ w=-1 w=-2/3 selection M (h -1 M ) 10 15

20 Structures: Dark Energy Measuring both distances and growth tests modified gravity models [Song 2004; Knox, Song, & Tyson 2005]

21 Structures: Dark Energy Toward realistic forecasts for cosmic shear [Huterer & Takada 2004; Huterer & White 2005; Ma, Hu & Huterer 2005] n(z) photo-z degeneracy 0.2 fractional change z

22 Structures: Neutrinos Toward cosmological detection of neutrino mass with clusters [Wang et al 05]