General structure of the Meeting.
The main idea is to have few large talks and plenty of time for discussion. Small talks are foreseen to cover many additional topics.
* Monday      14.30-18.30   Talks
* Tuesday     09.00-18.30   Talks + discussion
* Wed’day     09.00-16.30   Talks + discussion + trip to Venice
* Thursday    09.00-18.30   Talks + discussion
* (Friday)       09.30-13.00   (Open session for those who want to stay)
 
Session 1 - Introduction and general overview
We want to discuss different theoretical approaches to understand what experiments can tell about DM. General topics are: definition of observables for DM searches (i.e. photons, e+e- pairs, neutrinos, etc); which  experiments measure those observables and to what accuracy, what are the assumptions that affect results, what are the optimal targets for observations. We also want to make a short introduction on the current status, and briefly mention the concrete case of the Galactic Center.
 
• Introduction to the workshop.
 
• Status of DM searches. Brief discussion of DM characteristics with particular view on the experimental results.
 
* Focus on the Galactic Center. We want to start with a concrete cases. The GC is a laboratory for Multi3 approach and already several studies are performed to combine results.
 
*N-body simulations and DM structures. What is the development of N-body simulations? Which are the correlation between observations at different regions of the halo? 
 
 
Session 2. Indirect detection experiments
There are several experiments that can constrain proposed DM signals coming from the universe. On the other hand, an experimental result is often subject to a set of assumptions which can bias the result.  In this and the following discussion, we would like to discuss both experimental features and underlying physics scenario assumptions that can determine the quality of the result. We want to define not only the observable but also determine their accuracy.
 
* Air Cherenkov telescopes. What is an ACT and on which experimental technique is it based on? How can it
detect DM (the case of dSphs,GC and Galaxy clusters)? Current experiments: HESS, MAGIC and Veritas etc.
Current data and upper limits: discussion of how the derivation of upper limit is model dependent (particle
physics part, astrophysical part and experimental part). Caveat of the measurements. In the case of a future
signal, how (and how well) can they discriminate from background?
 
• The Fermi observatory. What is Fermi. Introduction on the experiment and on its capability as a DM telescope.
Observation so far and caveat of the measurements. Recents results.
 
• Radio and IC signatures. DM constraints from radio and IC observations. How the astrophysics and DM signals can be disentangled. Which are the assumptions behind the theory. WMAP and Fermi haze. INTEGRAL line. Possible global interpretations (theory building of DM). Which DM scenario do they favor?
 
•Cosmic-ray propagation. Propagation of cosmic rays will be a very important topic both as a background for gamma-rays, but also as important physical quantities per se. Description of propagation models. How is it constrained by data and how large are uncertainties? Tools for the description of the cosmic ray propagation (Galprop or semi-analytical solutions). How to extract a signal? How to get constraints? Robustness of the constraint.

•Constraint of DM annihilation rate from the early universe..

• Constraining Decaying Dark Matter
 
 
 
Session 3. Direct detection
implications from experiment of direct detection.
 
•  Direct detection: experiments. The DAMA modulation signal. Presentation of the experiment and of the signal.
Possible interpretation as DM signal? How can it be combined with other direct detection experiments Xenon, CDMS. etc? What can be inferred from indirect detectors?
 
•  The DM interpretation. How to model/simulate the background? Interpretation in terms of DM and upper limits.
Can these be combined with indirect detection? Direct detection: how to derive constraints on DM model from
multiple detections in a direct detection experiment. How different assumptions on DM are bound together: halo
model and particle physics content? How a signal from indirect detection can tell something on the assumption
from direct detection and vice-versa? How the combination of the two approaches can make you independent from
the assumption?
 
We continue in the discussion of the implications from accelerators. Experiments. LHC, Tevatron
 
 
Session 4. Multi-cube approach
In this session we will start with a review of the topics discussed so far in the meeting, trying to put together the
open questions of the measurements. Procedures on how to combine data, which in turn means how to combine assumptions of different measurements and how to define robust range for precision of measurement. We discuss the past effort in combination of results.  Our wish is to perhaps be able to test our knowledge over a bunch of specific candidates to see what we can say from different backgrounds. An example: Star-plot and combination of results Direct detection and indirect detection: combining the two. Which are the assumptions? Is it model dependent?