**Jorge Alfaro **

Lorentz Invariance Violation in the Standard Model induced by Quantum Gravity

The most important problem of fundamental Physics is the quantization of the gravitational field. A main difficulty is the lack of available experimental tests that discriminate among the theories proposed to quantize gravity. Recently we showed that the Standard Model(SM) itself contains tiny Lorentz invariance violation(LIV) terms coming from QG. All terms depend on one arbitrary parameter $\alpha$ that set the scale of QG effects. We discuss several effects,including the Ultra High Energy Cosmic Rays GZK cutoff.

**Giovanni Amelino-Camelia **

**Doubly Special Relativity: Myths, facts, and some key open issues**

**AP Balachandran **

Quantum fields on the Moyal plane

**Steve Giddings**

**High-energy gravitational scattering and locality**

**Florian Girelli **

QG phenomenology and Finsler geometry

Finsler geometry is a natural generalization of Riemannian geometry. I will describe various arguments (analog models, higher order derivatives field theories, symmetry deformation) favoring Finsler geometry as the natural framework to provide an effective description of semi-classical space-time.

**Jerzy Kowalski-Glikman**

**DSR from quantum gravity**

I will describe the steps of derivation of Doubly Special Relativity from ``no gravity limit'' of quantum gravity. Some of the steps are pretty well understood, and some are quite speculative. I will try to honestly point out which are which.

**Markopoulou**

**Emergent locality in quantum gravity **

**John Moffat**

**Finite, non-local quantum gravity**

**Daniel Sudarsky**

Quantum Gravity Phenomenology without violations or modifications of Lorentz Symmetry

**Bill Unruh**

Where do the particles come from?

Analog models of gravity server two purposes, one is giving us hints into ways in which we might be able to alter our theory of gravity, and another is using them to understand features of ordinary gravity. This talk will focus on the second, more conservative role of analogs. Black Hole evaporation is one of the most puzzling features of gravity and quantum theory. The derivation by Hawking is nonsense, in that it uses features of the theory in regimes where we know the theory is wrong.Analog models of gravity have given us a clue that despite the shaky derivation, the effect is almost certainly right. Where then are the particles in black hole evaporation really created? One of the most useful features of analog models is their maleability-- allowing us to change conditions in the model which are impossible to change in the true theory of gravity. In particular one can shift the location and temperature of the horizon for the various incoming frequencies and ask which of the horizon temperatures determines the temperature of the outgoing radiation. Also one can ask which of the velocities of the waves determines the location of the horizon and the concomitant temperature. This talks will examine these questions in the context of the simplest of analogs for a black hole. It may also look at some analytic work in support of the numerical results.

**Luis Urrutia**

Radiative corrections in the electrodynamics sector of the Myers Pospelov Model

**Matt Visser **

Can we hope to justify the Einstein equations in analogue/emergent spacetimes?

Analogue/ emergent spacetimes currently are useful fordescribing kinematic aspects of quantum gravity, that is: How doparticles and fields react to the presence of the analogue/ emergentspacetime? But obtaining suitable Einstein-like dynamics for theanalogue/ emergent spacetime is certainly much more difficult, andmay in most (hopefully not all) analogue models prove to beimpossible. Without providing any definitive solution to thisproblem, I will try to explore the possibilities and summarize thecurrent situation.

**Silke Weinfurtner**

Physical existence of signature change events and consequences of an absolute time in emergent spacetimes from Bose gas hydrodynamics.

We present an example of emergent spacetime as the hydrodynamic limit of a more fundamental microscopic theory. The low-energy, long-wavelength limit in our model is dominated by collective variables that generate an effective Lorentzian metric. This system naturally exhibits a microscopic mechanism allowing us to perform controlled signature change between Lorentzian and Riemannian geometries. We calculate the number of particles produced from a finite-duration Euclidean-signature event, where we take the position that to a good approximation the dynamics is dominated by the evolution of the linearized perturbations, as suggested by Calzetta and Hu [Phys. Rev. A 68 (2003) 043625]. We adapt the ideas presented by Dray et al. [Gen. Rel. Grav. 23 (1991) 967], such that the field and its canonical momentum are continuous at the signature-change event. We investigate the interplay between the underlying microscopic structure and the emergent gravitational field, focussing on its impact on particle production in the ultraviolet regime. In general, this can be thought of as the combination of trans-Planckian physics and signature-change physics. Further we investigate the possibility of using the proposed signature change event as an amplifier for analogue "cosmological particle production" in condensed matter experiments.