Attempts to explain CMB Large-scale Anomalies

Kin-Wang Ng () Academia Sinica, Taiwan

NTU String Group, June 18, 2010

Thanks: Hsien-Chun Wu, I-Chin Wang, Da-Shin Lee, Wolung Lee, Hing-Tong Cho,Yeo-Yie Charng, Shang-Yung Wang

7o resolution

WMAP3 CMB sky map

WMAP1WMAP3

South-North Power AsymmetryEriksen et al 04Eriksen et al 04Park 04 North pole (80o,57o)

Axis of Evil Land & Magueijo 05l=2, quadrupolel=3, octopole

Foreground problem??

Inflation and Primordial Density Fluctuations

WMAP3 and chaotic inflationr : tenor/scalarm 1013 GeV

Inflation and Primordial Density Fluctuationsperiodic universe, more..

A Challenge to Standard Slow-roll inflation!? Slow-roll conditions violated after horizon crossing (Leach et al)General slow-roll condition (Steward) |n-1|~|dn/dlnk|Multi-field (Vernizzi, Tent, Rigopoulos, Yokoyama et al)etc

Chaotic inflation classical fluctuations driven by a white noise (Starobinsky) or by a colored noise (Liguori, Matarrese et al.) coming from high-k inflatonDriven by a colored noise from interacting quantum environment (Wu et al)Others

Our Inflaton-Scalar Interacting ModelSingle-field inflation= 0(Wu et al 07)

Trace out sigma field to obtain :Feynman & Vernon 1963Influence Functional Methodsemi-classical

Dominant passive fluctuations and low CMB quadrupoleassuming no active de Sitter quantum fluctuations

Conclusion I

We propose a new dynamical source for density perturbation: Colored Quantum Noise - give a low CMB quadrupoleCan be applied to trapped inflation (Green et al. 09)Working on running spectral index and non-Gaussianity, both are natural with colored noise

A black hole in inflation Cho, Ng, Wang 09Schwarzschild-de SitterM - black hole massH - Hubble parameterStatic ------> Planar

Inflaton fluctuationsExpansionparameterwhere the source term

SolutionsZero orderFirst order

Power spectrumde Sitterquantum fluctuationsEnd of inflation 0

Possible effects to CMB anisotropyCarroll, Tseng, & Wise 08 preferred point, line, or planee.g. black holes formed via thermal fluctuations

Chen, Gruber,Ng, Scardigli 10

Conclusion IIHints from WMAP data on beyond standard slow-roll inflation !?A fine tuning physics just at 60 e-foldingsMaybe there is a window to see the first few e-foldings of inflation !?From homogeneous to directional effectsOr we are all fooled by probability it is indeed a Gaussian quantum processNongaussianity is an important check

SpeculationsIs it possible not to fine tune inflation duration to 60 efolds?Then there must be something happening during slow-roll inflationFormation rate must not be far below the expansion rate of inflation

String Landscape10500 de Sitter vacuaMetastable, bubble nucleation via tunnelingBarriers of string scale, slow tunneling rateThe spacetime is a hierachy of de Sitter vacuum bubblesMost part in eternal inflationSome regions tunnel down to flat potential for slow-roll infaltionWe sit in a vacuum with a small cosmological constant today

Efficient and rapid tunnelingTye, Shiu,12

Motion of the bubble wallsurfacetensionbubble radius