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The distribution of the large scale structure of the universe is the next great cosmological data set, following the Cosmic Microwave Background. It will allow us to study in remarkable detail the initial spectrum of fluctuations and the gravitational physics that governs both the homogeneous evolution of the universe as a whole and the local growth of inhomogeneities.

This workshop will focus on the near-future and long term prospects for learning fundamental physics from large scale structure, especially through statistics of the initial curvature fluctuations and tests of general relativity in the history of structure growth.

**Tzu-Ching Chang**, CITA

**Paolo Creminelli**, ICTP Trieste

**Michael Gladders**, University of Chicago

**Chris Hirata**, California Institute of Technology

**Gil Holder**, McGill University

**Wayne Hu**, University of Chicago

**Lam Hui**, Columbia University

**Dragan Huterer**, University of Michigan

**Bhuvnesh Jain**, University of Pennsylvania

**Eiichiro Komatsu**, University of Texas

**Jeffrey Newman**, University of Pittsburgh

**Alberto Nicolis**, Columbia University

**Ue-Li Pen**, CITA

**Fabian Schmidt**, California Institute of Technology

**Roman Scoccimarro**, New York University

**Suzanne Staggs**, Princeton University

**Anze Slosar**, Brookhaven National Laboratory

**James Taylor**, University of Waterloo

**Hy Trac**, Harvard-Smithsonian Center for Astrophysics

**Alexey Vikhlinin**, Harvard-Smithsonian Center for Astrophysics

**Pengjie Zhang**, Shanghai Astronomical Observatory

**Paolo Creminelli, ICTP Trieste**

**Galilean Genesis: an alternative to inflation**

I will discuss an alternative to inflation based on a Galileon field. The model starts in a (contracting or expanding) quasi Minkowski phase and all the energy of the Universe in generated suddenly in a sort of Genesis associated with a strong violation of the Null Energy Condition. The symmetries of the model force any additional scalar field to acquire a scale invariant spectrum of perturbations.

**Michael Gladders, University of Chicago**

Strong Lensing on Galaxy Cluster Scales

The statistics of strong lensing by galaxy clusters are sensitive both to cosmology and the detailed physics that determines the structure of halos. To exploit these sensitivites requires large and well defined samples of lenses on these mass scales. I will report on efforts to provide such samples - we finally now have uniformly selected samples of several hundred lenses to work with.

**Chris Hirata, California Institute of Technology**

**Tidal Alignments & Large Scale Structure**

TBA

**Gil Holder, McGill University**

Fingerprints of structure formation in the microwave background

Non-linear structures in the universe leave characteristic imprints in the cosmic microwave background. These include Compton scattering (Sunyaev-Zeldovich effects) and gravitational lensing. The South Pole Telescope now has a catalog of massive galaxy clusters that were discovered this way, along with a measure of the background fluctuations generated by smaller clusters, that can be used to chart the growth of structure in the universe.

**Wayne Hu, University of Chicago**

**Cosmic Acceleration: Dark Energy vs Modified Gravity**

I will discuss distinctions between dark energy and modified gravity explanations of cosmic acceleration from the horizon scale to the deeply non-linear regime using the modified action f(R) and braneworld DGP models as worked toy examples.

**Lam Hui, Columbia University**

**Robustness and Violations of a Scalar Equivalence Principle**

Modified gravity theories under consideration typically reduce to a scalar-tensor form in the appropriate limits.

I will discuss in what sense a universal scalar coupling is stable against quantum corrections, when the scalar equivalence principle is violated, how to look for such violations, and the connection with cosmic acceleration.

**Dragan** **Huterer, University of Michigan**

Falsifying Paradigms for Cosmic Acceleration

How can we rule out whole classes of dark energy models? And what quantities, at what redshift, and with what accuracy, should be measured in order to rule out these classes of models? I present answers to these questions by discussing an approach that utilizes the principal component parametrization of dark energy. I show results based on current data, and future forecasted data from SNAP and Planck.

**Bhuvnesh Jain**, University of Pennsylvania

**Magnification of high-redshift galaxies**

TBA

**Eiichiro Komatsu, University of Texas**

Bullet Cluster: A Challenge to Lambda-CDM Cosmology

We show that the existence of the bullet cluster, 1E0657-56, is incompatible with the prediction of the standard Lambda CDM cosmology. The probability of finding the large infall velocity (3000 km/s) necessary for explaining the X-ray and weak lensing data of 1E0657-56 is between 3.3x10^{-11} and 3.6x10^{-9}. The existence of the bullet cluster poses a serious challenge to LCDM cosmology, unless a lower infall velocity solution for 1E0657-56 with <1800 km/s is found.

**Jeffrey Newman, University of Pittsburgh**

Optical Surveys of Large-Scale Structure

TBD

**Alberto Nicolis, Columbia University**

**The Galileon as a local modification of gravity**

TBA

**Fabian Schmidt, California Institute of Technology**

**Non-linear structure formation in modified gravity**

Instead of adding another dark component to the energy budget of the Universe, one can ask whether the observed accelerated expansion might in fact be due to the behavior of gravity itself on the largest scales.

In this talk I will focus on two popular modified gravity theories which realize this scenario: f(R) gravity and the DGP model. While these models yield an accelerated expansion, they also affect the formation of structure on much smaller scales. We have studied this with cosmological N-body simulations which consistently solve for the modified gravitational force. I will discuss the effects of modified gravity on dark matter halo properties as well as cosmological observables. For

f(R) gravity, our first simulation-calibrated constraints from the observed abundance of massive clusters improve on previous constraints from the CMB and ISW by a factor of ~1000. This exemplifies the sensitivity of cosmological observables in the non-linear regime as probes of gravity.

**Hy Trac,**** Harvard-Smithsonian Center for Astrophysics**

**Templates for the SZ Angular Power Spectrum**

The Atacama Cosmology Telescope (ACT) has recently measured the CMB angular power spectrum from maps with arcminute resolution at 148 GHz. By fitting to a template for the SZ angular power spectrum, we constrain the model's amplitude A_SZ < 1.63 (95% confidence level) and the amplitude of matter perturbations sigma_8 < 0.86 (95% CL). In this talk, we review the fiducial template and present additional templates for the SZ angular power spectrum based on different models for the hot gas in dark matter halos. We also discuss how the TSZ, KSZ, and SZ power spectra scale with sigma_8.

**Alexey Vikhlinin, Harvard-Smithsonian Center for Astrophysics**

Recent advances and future challenges for using galaxy clusters in cosmology

X-ray surveys and deep Chandra observations recently provided ~10% accurate measurements of the total mass in nearly 100 galaxy clusters at z=0-0.9. These data clearly show the effect of Dark Energy on slow-down of the structure growth at z<1. THe combination of the structure growth measurements with other cosmological observations substantially improves the constraints on the Dark Energy equation of state parameter. More advanced applications include constraints on the deviations from General Relativity on 10-100 Mpc scales. Will the situation improve in the future when samples of 10^3-10^5 clusters are available? I will review the current "bottlenecks", and discuss possible strategies for using future cluster data for "precision cosmology".

**Pengjie Zhang, Shanghai Astronomical Observatory**

Testing gravity at cosmological scales: from linear to nonlinear regimes

Observations are opening new windows to test general relativity at cosmological scales. In this talk, I will discuss how gravity determines the expansion and structure formation of the universe, what smoking guns of gravity in the cosmos we are expecting, what difficulties we are facing to perform unambiguous tests of gravity and what are possible ways to overcome these difficulties.