3. History, Context, the CDM and WIMP crisis and their decline: This Workshop is the Fifth of a new Chalonge series in Meudon dedicated to Warm Dark Matter. The first Workshop of this series (June 2010) allowed to identify and understand the issues of the serious problems faced by Cold Dark Matter (CDM) and CDM + baryons to reproduce the galactic observations. The 2010 and 2011 Workshops served as well to verify and better understand the confusion situation in the CDM research, namely the increasing number of cyclic arguments, and ad-hoc mechanisms and recipes introduced in the CDM + baryon galaxy simulations over most of twenty five years, in trying to deal with the CDM + baryons small scale crisis: Cusped profiles and overabundance of substructures (too many satellites) are predicted by CDM. In contrast, cored profiles and no such overabundant substructures are seen by astronomical observations. The so many galaxy formation and evolution models of CDM + baryons are plagued with ever increasing tailoring or fine tuning and recepes.

On the CDM particle physics side, the situation is no less critical: So far, all the dedicated experimental searches after most of twenty five years to find the theoretically proposed CDM particle candidate (WIMP) have repeatedly failed. The CDM indirect searches (invoking CDM annihilation) to explain cosmic ray positron excesses, are in crisis as well, as wimp annihilation models are plagued with growing tailoring or fine tuning, and in any case, such cosmic rays excesses are well explained and reproduced by natural astrophysical process and sources. The so-called and continously invoked 'wimp miracle' is nothing but being able to solve one equation with three unknowns (mass, decoupling temperature, and annihilation cross section) within wimp models theoretically motivated by SUSY model building twenty five years ago (at that time those models were fashionable and believed for many proposals which is not anymore the case).

After more than twenty five years, and as often in big-sized science, CDM research (CDM+ baryon simulations, direct and indirect WIMP experimental research and model building), has by now its own internal inertia and own organized community, without reproducing the astronomical observations and failing to provide any experimental signal of wimps (except signals compatible with experimental noise). Growing CDM + baryon galaxy simulations involve ever increasing large super-computers and large number of people working with; CDM particle wimp search involved (and involve) large and long-time planned experiments, huge number of people and huge budgets. One should not to be surprised then if a strategic scientific change have not yet operated in the CDM + baryon research and in the wimp research, given the way in which the organization operates, although their real scientific situation is of decline. Wimps are not the DM particle, DM is not Cold because the right DM particle is at the keV scale, DM is Warm.

4. The Workshop addresses the last and fast progresses made in Warm Dark Matter Galaxies in Agreement with Observations. In the tradition of the Chalonge School, an effort of clarification and synthesis will be made by combining in a conceptual framework, theory, analytical, observational and numerical simulation results. The subject will be approached in a threefold way:

(I) Conceptual context: Dark Matter in cosmology and astrophysics: perspective and prospective of the research in the subject: Theory and observations. The emergence of Warm (keV scale) Dark Matter from theory and observations.

(II) Astronomical observations : galaxy structural properties, the universal and non universal properties of galaxies, high quality rotation curves, kinematics, density profiles, gravitational lensing, small and large structures, deep surveys, clusters of galaxies

(III) Computational framework with the equations of physics. Analytical and numerical frameworks. The new important physical ingredient in galaxy structure: quantum mechanics. Classical (non quantum) numerical simulations with Warm Dark Matter and resulting structures. Results versus observations.

Special attention will be payed to the astrophysical understanding of the dark matter problems and its solution, the use of analytic and numerical methods which determine the properties, the density profiles, masses, sizes and evolution, the distribution and the nature of Warm Dark Matter.

TOPICS OF WORKSHOP:

Kinetic theory and the recent progress in solving the Boltzmann-Vlasov equation to obtain the observed universal properties of galaxies.
Warm (keV scale) dark matter N-body simulations in agreement with observations at large and intermediate scales.

The phase-space density of dark matter.

Particle model independent analysis of astrophysical dark matter.

The impact of the mass of the dark matter particle on the small scale structure formation and the choice of the initial conditions.

The radial profiles and the Dark Matter distribution. Observed galactic cored DM profiles

The keV scale Dark Matter (Warm Dark Matter): Observational and theoretical progresses.

Large and small scale structure formation in agreement with observations at small galactic and at large scales.

The serious dark matter candidate: Sterile neutrinos at the keV scale

Active and sterile neutrinos mass bounds from cosmological data and from astrophysical and X ray data and from high precision beta decay experiments.

News on neutrinos and eV scale sterile neutrinos. News from reactor and accelerator experiments on neutrinos and their science implications.

The Thomas Fermi framework to describe the structure and physical states of galaxies in agreement with observations.

The DM distribution function and the equation of state of galaxies. Universal and non universal profiles. Cored density profiles with WDM core sizes in agreement with observations.

Supermassive Black Holes : Theory and Observations. The clarifying and unifying WDM framework for stars, galaxies and cosmology.

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FORMAT OF THE WORKSHOP

Enough time will be available for the discussions.

The Meeting is open to all scientists interested in the subject. Registration is mandatory. Registration information is given below.

The format of the Meeting is intended to allow easy and fruitful mutual contact and communication.

Sessions last for three full days in the beautiful and green Meudon campus of Observatoire de Paris in the historic Castle with the Great Dome building ("Château Grande Coupole") where CIAS (Centre International d´ Ateliers Scientifiques) is located.

All lectures and presentations will take place at the Castle Conference Room (Salle de Conferences du Château) in the historic Castle building.

All Coffee-Tea breaks will take place at the Urania Hall aside the castle conference room in the same building. The Registration desk and the Secretariat of the Workshop take place at the Urania Hall.

Discussions and working sessions all during the workshop will take place at the CIAS rooms aside the Urania Hall.

SOC et LOC :

Norma G.Sanchez, Hector J. de Vega, Peter Biermann, Maria Cristina Falvella

Nicole Letourneur, Dominique Lopes, Sylvain Cnudde, Emmanuel Vergnaud, Djilali Zidani

Informations on the previous Meudon Chalonge Workshops and of the school programmes are available at http://chalonge.obspm.fr (lecturers, lists of participants, lecture pdf files, Highlights and Conclusions, and photos during the Colloquia Workshops).

PROGRAMME and LECTURERS

Peter BIERMANN (MPI-Bonn, Germany & Univ of Alabama, Tuscaloosa, USA)
Warm Dark Matter and its astrophysical signatures.

Dietrich BODEKER (Fakultaet fuer Physik, Universitaet Bielefeld, Germany)
The baryon asymmetry of the Universe from non-relativistic Leptogenesis and heavy neutrinos

Esra BULBUL (Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA)
Recent detection of a new keV emission line in the X-ray spectrum of galaxy clusters

Hector J. DE VEGA (CNRS LPTHE Univ de Paris VI, France)
The Quantum Structure of Galaxies in keV Fermionic Warm Dark Matter

Anastasia FIALKOV(Départment de Physique ENS Paris France)
The cosmic history of the 21-cm line signal from the recombination epoch to the first stars

Loredana GASTALDO (Kirchhoff Institute for Physics KIP, Univ Heidelberg, Germany)
Status report on the ECHO experiment to measure the active neutrino mass and the search of keV sterile neutrino.

The HOLMES Experiment:Andrea GIACHERO (INFN-Universitá di Milano Bicocca, Milan, Italy)The Electron Neutrino Mass by the HOLMES experiment: A Status Report

Shunsaku HORIUCHI (Dept. of Physics & Astronomy, Univ. of California, Irvine, CA, USA)
keV Sterile neutrino Warm Dark Matter bounds from Galaxies of the Local Group.

The KATRIN Experiment:Kai DOLDE & Marc KORZECZEK (NP & KIT, Karlsruhe, Germany)Neutrino Mass Measurements and Sterile Neutrino Detection at KATRIN

Marco LOMBARDI (Dept. of Physics,University of Milano, taly)
Scaling laws in Star and Structure formation: Density Models fitted to Observational Data

Yann MAMBRINI (CNRS LPT Univ Paris-Sud 11 Orsay, France)
Generating X-ray lines from annihilating Warm Dark Matter

Alessandro MELCHIORRI (Univ. Roma 1 La Sapienza,Italy)
Planck Results for neutrinos and their implications

Nicola MENCI (INAF, Osservatorio di Roma, Rome, Italy)
The Evolution of Galaxies and AGN in Warm Dark Matter Cosmology

Andrei MESINGER (Scuola Normale Superiore, Pisa, Italy)
The imprint of Warm Dark Matter on the cosmological 21-cm signal.

Fabio PACUCCI (Scuola Normale Superiore, Pisa, Italy)
Focusing on Warm Dark Matter with lensed high-redshift Galaxies

Sinziana PADUROIU (Observatoire de Geneve, Switzerland)
Numerical Simulations on Structure Formation in Warm Dark Matter Cosmology.

Paolo SALUCCI (SISSA-Astrophysics, Trieste, Italy)
Testing Warm Dark Matter with Galaxy observations at high redshifts

Norma G. SANCHEZ (CNRS LERMA Observatoire de Paris, Paris, France)
The Thomas Fermi keV Warm Dark Matter Galaxy Theory. Quantum macroscopic effects and New Results.

The SOUTH POLE Telescope -SZ Survey:CMB Power Spectrum and cosmological constraints on neutrino masses (active and sterile) and the value of Ho

Takayuki TAMURA (ISAS/JAXA, Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, Japan)

The ASTRO-H X-ray Observatory: Soft X-ray spectrometer, Soft X-ray imager and the possibility to detect the decay of galactic warm dark matter keV sterile neutrinos.

Christopher G.TULLY (Dept. of Physics, Princeton University, NJ, USA)
The challenges of relic neutrino direct detection and status of the PTOLEMY experiment

Patrick VALAGEAS (Inst. de Physique Théorique, Orme d Merisiers, CEA-Saclay, Gif-sur-Yvette France)
Analytic approaches to structures formation in Warm Dark Matter and arge scale structures.

And Other LECTURERS