What Can WMAP Tell Us About The Very Early What Can WMAP Tell Us About The Very Early Universe? New Physics as an Explanation of Universe? New Physics as an Explanation of Suppressed Large Scale Power and Running Suppressed Large Scale Power and Running

Spectral IndexSpectral Index

Speaker : Cheon Hwa SungSpeaker : Cheon Hwa SungYonsei UniversityYonsei University

Mar Bastero-Gil, Katherine Freese and Laura

Mersimi-Houghton

Hep-ph/0306289

1.The purpose of this paper1.The purpose of this paper

The suppression of low "l" modes The suppression of low "l" modes (Large angle) in the CMB data (Large angle) in the CMB data

and and Running of the spectral index of Running of the spectral index of

density perturbations density perturbations can be explained by can be explained by

New physicsNew physics

1.1 The two modifications to 1.1 The two modifications to standard cosmologystandard cosmology

Modifications to the Friedmann equationModifications to the Friedmann equation

Velocity dependent potentialsVelocity dependent potentials

1.2 Our purpose

1)What is the CMB power spectrum ?

2)What is the Inflation Model? (Horizon, flatness, Relic problem)

3)Friedmann Equation (Slowly-Rolling Scalar Fields)

4)What are concerned with between the New physics and these?

5) RS Model..

2. Introduction of this paper2. Introduction of this paper

1. The suppression of large scale power and the 1. The suppression of large scale power and the running of the index, can be explained by running of the index, can be explained by New PhysicsNew Physics

2. The running of the index can be 2. The running of the index can be explained byexplained by New Physics New Physics

The spectral index runs from red on The spectral index runs from red on small scales to blue on large scales small scales to blue on large scales

New Physics!!!

Last Scatteri

ng

New physics is valid beyond, and around the E_c

Fig: [astro-ph/0302217]

2.1 The Explanation of the 2.1 The Explanation of the suppression of large scale suppression of large scale

powerpower From the low “l” suppression of the signal, we could be learning From the low “l” suppression of the signal, we could be learning

about the about the initial conditionsinitial conditions for the part of inflation for the part of inflation

1) Non trivial topology 1) Non trivial topology [astro-ph/0303580, [astro-ph/0303580, gr-qc/9602039, gr-qc/9602039,

Phys. Rev. D58,123006,1998]Phys. Rev. D58,123006,1998]

2) Closed Universe2) Closed Universe [astro-ph/0303245, 03032597, [astro-ph/0303245, 03032597, 03303127]03303127]

이들 이들 ideasideas 가 가 Concordance ModelConcordance Model 과 아주 잘 맞는 과 아주 잘 맞는 Cosmological dataCosmological data 의 의 나머지와 잘 부합할지는 모른다나머지와 잘 부합할지는 모른다 . [astro-ph/0303268]. [astro-ph/0303268]

3) Double Inflation 3) Double Inflation [phys. Rev. D59(1999)107303, [phys. Rev. D59(1999)107303,

astro-ph/0305020]astro-ph/0305020]

The The conclusion 1conclusion 1 The initial conditions for the observable uniThe initial conditions for the observable uni

verse could be determined by the verse could be determined by the New PhNew Physicsysics, which is the relevant theory valid be, which is the relevant theory valid beyond, and around the cutoff scale E_c of efyond, and around the cutoff scale E_c of effective low energy theoriesfective low energy theories

2.2 Potential-driven models2.2 Potential-driven models

We Here consider potential-driven We Here consider potential-driven models of Inflationmodels of Inflation

( ( 거기서 거기서 potentialpotential 은 우주가 가속하기 위해 우주의 은 우주가 가속하기 위해 우주의 에너지 밀도에 에너지 밀도에 dominatedominate 된 된 PotentialPotential 이다이다 . ) . )

PotentialPotential 의 높이는 의 높이는 GUT scaleGUT scale 에 의해 에 의해 결정되어진다결정되어진다 . .

Horizon scale Horizon scale 까지 까지 HomogeneousHomogeneous 한 한 우주를 만들기 위해서는 우주를 만들기 위해서는 roughly 60 e-roughly 60 e-folding of inflationfolding of inflation 이 요청된다이 요청된다 ..

The The conclusion 2conclusion 2 we here consider models in which we here consider models in which

physics beyond the inflationary scale physics beyond the inflationary scale (e.g. GUT scale) is modified by the (e.g. GUT scale) is modified by the introduction of introduction of NEW PhysicsNEW Physics, this , this NEW PhysicsNEW Physics can leave imprints in can leave imprints in the the CMBCMB at scales near and above at scales near and above the Horizon. the Horizon.

Conclusion 1, 2Conclusion 1, 2 에 의해 다음과 같은 결론을 이끌어 에 의해 다음과 같은 결론을 이끌어 낼 수 있다낼 수 있다 ..

Above the 60Above the 60thth e-folding the theory is described e-folding the theory is described by by NEW PhysicsNEW Physics

This is the regime corresponding to all the energy This is the regime corresponding to all the energy scales above E_c scales above E_c

이 관점에 의하면이 관점에 의하면 , the low “l” feature in CBR , the low “l” feature in CBR 는 는 InflationInflation 의 의 initial timeinitial time 에서 차지하는 에서 차지하는 NEW PhyNEW Physicssics 로 부터 발생되어진다로 부터 발생되어진다 . .

E_c E_c 이상의 이상의 energy scaleenergy scale 에서는 에서는 QFTQFT 나나 GRGR 이 이 적용되지 않는다적용되지 않는다 . . 거기서는 거기서는 NEW PhysicsNEW Physics 가 가 요청된다요청된다 . (New physics. (New physics 는 는 V<E_cV<E_c 에서는 에서는 GR, QGR, QFTFT 로 로 approx approx 할 수 있다할 수 있다 . ). )

이 논문에서는이 논문에서는 , Standard Cosmology, Standard Cosmology 의의FormalismFormalism 에서 두 가지 변경을 에서 두 가지 변경을 고려하였다고려하였다 ..

1.1. Modification to the Friedmann EquationModification to the Friedmann Equation

2.2. The Inflation potential is velocity dependeThe Inflation potential is velocity dependent nt

Modified primordial Modified primordial spectrumspectrum

CBR spectrum of anisotropies with the modified primordial spectrum fo the Rand

all Sundrum

점선 : modified

실선 : standard spectrum