REVIEW TALKS

ALDO MORSELLI II UNIVERSITA DI ROMA "TOR VERGATA” - ITALY

ARIEL SÁNCHEZ MPE - GERMANY

CARLA BONIFAZI UFRJ - BRAZIL

CHRISTOPHER J. CONSELICE UNIVERSITY OF NOTTINGHAM - UNITED KINGDOM

JODI COOLEY SOUTHERN METHODIST UNIV. - USA

KEN GANGA APC - FRANCE “THE MISSION”

The planck satellite, created to measure the anisotropies in the temperature and polarization of the cosmic microwave background, was launched in may of 2009 and has performed well. Some early, non-cmb results have been published already. The first set of cmb temperature data and papers will be released at the beginning of 2013. The full data set, including polarization, is scheduled to be made public in early 2014. Galactic and other astronomical results will continue to be released during this period. I will review the non-cmb results which have been released to date and give previews of what we hope to be able to do with the cosmological data releases.

MATTHIAS STEINMETZ AIP - GERMANY

NICOLAO FORNENGO UNIVERSITY OF TORINI - ITALY

PAOLO SALUCCI SISSA – ITALY “ IN GALAXIES: LEADS TO ITS NATURE”

In the past years a wealth of observations has revealed the structural properties of the Dark and Luminous mass distribution in galaxies. These have pointed out to an intriguing scenario. In spirals, the investigation of individual and coadded objects has shown that their rotation curves follow, from their centers out to their virial radii, a Universal profile (URC) that arises from a tuned combination of a stellar disk and of a dark halo. The importance of the latter component decreases with galaxy mass. Individual objects have clearly revealed that the dark halos encompassing the luminous discs have a constant density core. Significantly galaxies of other and very differeny Hubble types show similar properties in the dark component. This scenario poses seriuos challenges to "raw" ΛCDM implying that in scenario baryions lead the formation of galaxies. On the other hand, this phenomenology may indicate, for the dark particle, a different nature .

THOMAS SOTIRIOU SISSA - ITALY

YUN WANG THE UNIV. OF OKLAHOMA - USA “OBSERVATIONAL PROBES OF "

The cause for the observed acceleration in the expansion of the is unknown, and referred to as "dark energy" for convenience. Dark energy could be an unknown energy component, or a modification of einstein's general relativity. This dictates The measurements that are optimal in unveiling the nature of dark energy: the cosmic expansion history, and the growth history of cosmic large scale structure. I will examine type ia supernovae and galaxy clustering as dark energy probes, and discuss recent results and future prospects.

TALKS

ALEJANDRO AVILES CERVANTES ICN UNAM The dark degeneracy and interacting cosmic components In this talk I present some properties of the dark degeneracy, which is the fact that what we measure in gravitational experiments is the energy-momentum tensor of the total dark sector, and any split into components (as in dark matter and dark energy) is arbitrary. In fact, just one dark fluid is necessary to obtain exactly the same cosmological and astrophysical phenomenology as the LCDM model. I work explicitly the first-order perturbation theory and show that beyond the linear order the dark degeneracy is preserved under some general assumptions. Then we construct the dark fluid from a collection of interacting fluids. Finally, I shall try to break the degeneracy with a general class of couplings to baryonic matter. Nonetheless, I show that these interactions can also be understood in the context of the LCDM model as between dark matter and baryons.

ANTONIO C. C. GUIMARÃES UFRJ SNIa analysis independent of dark energy models We study alternative ways to describe the cosmic expansion that are independent of dark energy models and even independent of assumptions about the energy contend of the universe and the underlying gravitational theory. One first approach was to use kinematic models for the cosmic expansion, where we found that even very simple models allow for data fittings that are as good as ΛCDM. One second approach was to use cosmographic expansions, from what we found, among other things, that a transient cosmic acceleration is not excluded by the current SNIa data. We also use SNIa data simulations to investigate the bias that is induced by specific parameterizations of the cosmic expansion when used to analyze real data.

CHRIS GAUTHIER APC Non-Parametric Reconstruction of the Primordial Power Spectrum from the CMB In my talk I propose a straightforward and model independent methodology for characterizing the sensitivity of CMB and other experiments to wiggles, irregularities, and features in the primordial power spectrum. Assuming that the primordial cosmological perturbations are adiabatic, I present a function space generalization of the usual Fisher matrix formalism, which is explicitly calculated for a number of CMB experiments. This work is closely related to other work on recovering the inflationary potential and exploring specific models of non-minimal, or perhaps baroque, primordial power spectra. The approach adopted here, however, most directly expresses what the data really is telling us.

CHRISTOPH SAULDER ESO Observational aspects of an One of the biggest mysteries in cosmology is Dark Energy, which is required to explain the accelerated expansion of the universe within the standard model. But maybe one can explain our observations without introducing new physics, by simply taking one step backwards and re-examining one of the basic concepts of cosmology. In standard cosmology, it is assumed that the universe is homogeneous, but this is obviously not true at small scales. Since general relativity, which is the basis of modern cosmology, is a non-linear theory, one can expect some back reactions in the case of an inhomogeneous matter distribution. The magnitude of these back reactions is a topic of hot discussion and estimates are ranging from insignificant to being perfectly able to explain the accelerated expansion of the universe. In the end, the only way to be sure is to test predictions of inhomogeneous cosmological theories, such as timescape cosmology. If it is a valid description of the universe, one expects aside other effects, that there is a dependence of the Hubble parameter on the line of sight density distribution. The of a galaxy, which is located at a certain distance, is expected to be smaller if the environment in the line of sight is mainly high density (clusters or "walls"), rather than mainly low density environment (voids). It should be noted that this effect can be only observed below the scale of homogeneity and therefore, our objects of interest are rather nearby. Using the redshift and an independent distance indicator, like the fundamental plane, one is able to test this prediction. In order to get solid statistics, which can handle the uncertainties in the distance estimate and the natural scatter due to peculiar motions, one has to systematically study a very large number of galaxies. Therefore, the SDSS forms a perfect basis for testing timescape cosmology and similar theories. The preliminary results of this investigation are very interesting.

DAVI CABRAL RODRIGUES UFES Elliptical galaxies kinematics within general relativity with renormalization group effects The renormalization group framework can be applied to Quantum Field Theory on curved space-time, but there is no proof whether the beta-function of the gravitational coupling indeed goes to zero in the far infrared or not. In a recent paper we have shown that the amount of dark matter inside spiral galaxies may be negligible if a small running of the General Relativity coupling G is present. Here we extend the proposed model to elliptical galaxies and present a detailed analysis on the modeling of NGC 4494 (an ordinary elliptical) and NGC 4374 (a giant elliptical). In order to compare our results to a well known alternative model to the standard dark matter picture, we also evaluate NGC 4374 with MOND. In this galaxy MOND leads to a significative discrepancy with the observed velocity dispersion curve and has a significative tendency towards tangential anisotropy. On the other hand, the approach based on the renormalization group and general relativity (RGGR) could be applied with good results to these elliptical galaxies and is compatible with lower mass-to-light ratios (of about the Kroupa IMF type). --- Based on arXiv:1203.2286v2 [astro-ph.CO].

DAVID DELEPINE UNIV. DE GUANAJUATO Heavy Majorana Neutrinos and Delta L=2 B and top decays in B factories Lepton number violation (LNV) can be induced by Majorana neutrinos in four-body decays of the neutral B meson and the top quark. We study the effects of Majorana neutrinos in these |\Delta L|=2 decays in an scenario where a single heavy neutrino can enhance the amplitude via the resonant mechanism. Using current bounds on heavy neutrino mixings, the most optimistic branching ratios turn out to be at the level of 10^{-6} for \bar{B} -> D^+e^-e^-\pi^+ and t -> bl^+l^+W^- decays. Searches for these LNV decays at future facilities can provide complementary constraints on masses and mixings of Majorana neutrinos.

DEBASISH MAJUMDAR SAHA INSTITUTE OF NUCLEAR PHYSICS Gamma Ray and Neutrino Flux from Annihilation of Dark Matter in mAMSB model We consider the lightest supersymmetric particle (LSP), neutralino in minimal anomaly mediated breaking model (mAMSB) to be a possible candidate for weakly interacting massive particles (WIMP) or and investigate its direct and indirect detections. The supersymmetric parametric space for such a model is constrained by the WMAP results for relic densities. The spin independent and spin dependent scattering cross sections for dark matter off nucleon are thus constrained from the WMAP results. They are found to be within the allowed regions of different ongoing direct detection experiments. The annihilation of such dark matter candidates at the galactic centre produce different standard model particles such as gamma rays, neutrinos etc. In this work, we investigate the possible fluxes of such particles from galactic centre. The neutrino flux from the galactic centre and at different locations away from the galactic centre produced by WIMP annihilation in this model are also obtained. We have also studied signals from dark matter annihilations from different angles of observations for different spherically symmetric distribution models in the galaxy. We have compared our gamma ray flux results for different halo models with the HESS experimental data.

GUILLAUME LAMBARD IFIC/CSIC Indirect dark matter search with the ANTARES neutrino telescope Using the ANTARES neutrino telescope, the largest neutrino telescope in the Northern hemisphere, we have studied our ability to search indirectly for an evidence of dark matter annihilations in heavy astrophysical objects as the Sun and the Galactic centre. First limits have been obtained using the data recorded by ANTARES in 2007 and 2008, and compared with neutrino fluxes predicted within a minimal supersymmetric extension of the Standard Model with supersymmetry-breaking scalar and gaugino masses constrained to be universal at the GUT scale, the CMSSM, as well as a minimal Universal Extra-Dimension scenario with one extra compact dimension where all the Standard Model fields propagate into the bulk, the UED. The current limits over the neutrino/muon fluxes coming from dark matter annihilations, the spin-dependent and spin-independent cross-sections, as well as the expected sensitivities predicted after several years of data taking with ANTARES, will be presented for each source.

JONAS FLORIANO GOMES DOS SANTOS FEDERAL UNIVERSITY OF SÃO CARLOS Study of the coupling of the anisotropic stress tensor of neutrinos with primordial gravitational waves We have studied the effects of the anisotropic stress tensor of cosmological neutrinos in the coupled Einstein-Boltzmann system in the LambdaCDM cosmological scenario. Starting from an expansion in multipole for perturbations in the distribution function of photons and a simple approximation for the collision terms of neutrinos, we investigate the coupling of primordial gravitational waves with neutrinos (we are considering only massless neutrinos). The tensor contribution to the variance in the Cosmic Background Radiation (CBR) temperature multipoles (“angular power spectrum”) shows that for the standard scenario with density parameter of neutrinos equal to 0.4052 (where this value is the ratio of neutrinos density to radiation density and the it is relative to three neutrinos family), the stress tensor does not changes significantly the background temperature of photons. However, if we assume a very large amount of neutrinos to cosmological plasma, that is, the density parameter of neutrinos equal to 1, the stress tensor becomes relevant to our problem. By inserting collision terms, we have noted that as the effectives collisions increases, the angular power spectrum is modified considerably, particularly the quadrupole term. In this scenario, the anisotropic stress tensor of neutrinos affects the angular power spectrum mostly in large scale (l≤10).

JUAN PEDRO OCHOA RICOUX BERKELEY LAB Results from the Daya Bay Reactor Neutrino Experiment The precise determination of the mixing angle θ13 is one of the main priorities in the field of neutrino physics. Not only is this parameter inextricably linked to the possibility of observing CP violation in the neutrino sector, but it may also hold the key to other open questions in physics, such as the matter anti- matter asymmetry in the universe. The Daya Bay Reactor Neutrino Experiment has the highest sensitivity to this parameter among all the other experiments that are currently in operation or under construction. The experiment consists of multiple identical detectors placed underground at different baselines from three groups of reactors, a configuration that minimizes systematic uncertainties and cosmogenic backgrounds. The experiment has been making steady progress, and the first results with a six-detector configuration have already been released. The most recent results will be discussed in this talk alongside the current status and future prospects of the experiment.

KENJI KADOTA NAGOYA UNIVERSITY The effects of quark interactions on the dark matter kinetic The studies of the dark matter kinetic decoupling influencing the size of the smallest dark matter halos could provide us the powerful cosmological probe on the nature of the dark matter, in an analogous way that the physics of the decoupling of photons and baryons have been unveiling the properties of our Universe through the cosmic microwave background and the baryon acoustic oscillations. In this talk, the dark matter kinetic decoupling with the emphasis on the DM-quark interactions, in view of the recent data from the LHC and dark matter direct search experiments, will be discussed.

KINGA PARTYKA YALE UNIVERSITY Analysis of CCQE Neutrino Interactions in a Liquid Argon Time Projection Chamber (LArTPC) The Argon Neutrino Test, ArgoNeuT, is a small scale Liquid Argon Time Projection Chamber(LArTPC). ArgoNeuT, an R&D project paving the way for construction of larger detectors, was located 350 feet underground and ran upstream of the MINOS detector in the NuMI beam at Fermi National Accelerator Laboratory from September 2009 to February 2010. ArgoNeuT provides bubble-chamber-like quality images for excellent particle ID and background rejection. ArgoNeuT provides a sample of neutrino events in a LArTPC for the first time in the U.S. and the first time ever in a low-energy beam of 0.1 to 10 GeV. Analysis of ArgoNeuT's Charged Current Quasi-Elastic (CCQE) neutrino sample, in which a neutrino interacts with a neutron and the final state particles are a proton and a muon, will be presented. Vertex activity and calorimetric reconstruction will be addressed for this class of events.

KOICHI MIYAMOTO ICRR, UNIVERSITY OF TOKYO Isocurvature perturbations in Recent cosmological observations, including measurements of the CMB anisotropy and the primordial helium abundance, indicate the existence of an extra radiation component, dubbed "dark radiation", in the Universe beyond the standard three neutrino species. In this paper we explore the possibility that the dark radiation has isocurvatrue fluctuations. A general formalism to evaluate isocurvature perturbations in the dark radiation is provided in the mixed inflaton-curvaton system, where the dark radiation is produced by the decay of both scalar fields. We also derive constraints on the abundance of the dark radiation and the amount of its isocurvature perturbation. These constraints are applied to some particle physics motivated models. Besides, we discuss the non-Gaussianity of the dark radiation isocurvature perturbation, the forecasted constraints on it in the future CMB experiments, and the implication for the particle physics motivated models.

MARIANA PENNA-LIMA CBPF NumCosmo: Numerical Cosmology Library The NumCosmo is an open source C library whose main purposes are to test cosmological models using observational data and to provide a set of tools to perform cosmological calculations. Particularly, the current version has implemented three different probes: cosmic microwave background (CMB), supernovae type Ia (SNeIa) and large scale structure (LSS) information, such as baryonic acoustic oscillations (BAO) and galaxy cluster abundance. The code supports a joint analysis of these data and the parameter space can include cosmological and phenomenological parameters. It is worth emphasizing that NumCosmo and CMB codes were written independently of other implementations such as CMBFAST, CAMB, etc. The library is structured in such way to simplify the inclusion of non- standard cosmological models. Besides the functions related to cosmological quantities, this library also implements mathematical and statistical tools. The former was developed to enable the inclusion of other probes and/or theoretical models and to optimize the codes. The statistical framework comprises algorithms which define likelihood functions, minimization, Monte Carlo, Fisher Matrix and profile likelihood methods.

MICHAEL STURM KARLSRUHE INSTITUTE OF TECHNOLOGY KATRIN, an experiment for determination of the ν-mass: status and outlook Recent results of the measurement of the cosmic microwave background fit remarkably well with the simplest cosmological ΛCDM model. Observations on small (galactic) scales where the current ΛCDM model seems to fail could maybe be explained by a model (WDM). In this context eV or even keV sterile neutrinos are getting again en vogue. Therefore one of the most fundamental tasks over the next years will be the determination of the absolute mass scale of neutrinos. Model-independent results are only provided by kinematic β-decay experiments. The Karlsruhe Tritium Neutrino experiment KATRIN aims at improving the sensitivity in the neutrino mass measurement down to 200 meV/c² (90%C.L.) and so will help to clarify the role of neutrinos in the early universe. KATRIN investigates spectroscopically the electron spectrum from tritium β-decay close to the kinematic endpoint of 18.6 keV. For such a precise mass determination a key parameter is the stability of the source in terms of β-activity and isotopic purity. For that reason KATRIN uses a strong windowless gaseous tritium source of almost pure molecular tritium (95%) with a throughput of 40 g tritium per day stabilized on 0.1% level. The decay electrons are guided adiabatically from the source to the spectrometer by means of superconducting magnets while at the same time the tritium flow rate to the spectrometers has to be reduced by a factor > 1E14. A tandem spectrometer system with an energy resolution of ΔE = 0.93 eV at 18.6 keV is used for energy analysis, followed by a detector-system for counting the transmitted β-decay electrons. Both spectrometers are of the MAC-E-Filter (Magnetic Adiabatic Collimation followed by Electrostatic Filter) type and therefore combine a high energy resolution with a large luminosity. KATRIN is currently under construction at the Karlsruhe Institute of Technology (KIT) Campus North; it will prospectively start data taking in 2015. This talk will give an introduction to direct ν-mass determination from tritium β-decay and an overview of the status of the main components of the KATRIN experiment.

OLGA SUVOROVA INR RAS Limits on spin-dependent WIMP-proton cross-sections from the neutrino experiment of the Baksan Ungerground Scintillator Telescope We searched for an excess in arrival directions of upward through going muons in the neutrino experiment of the Baksan Ungerground Scintillator Telescope towards the Sun relatively to the expectations from neutrinos of atmospheric origin and so far an annihilation signal in the center of the Sun of weakly interactive massive particles (WIMPs). With data sample of 21,15 years l.t. we obtained upper limits at 90% c.l. on cross sections of neutralino elastic scattering off nucleon as a function of neutralino mass. The best value of the limit is 3 *10-4 picobarn in spin-dependent interaction of neutralino on proton for neutralino mass 210 GeV/c2. We compare different experiments of the dark matter search.

OSAMU SETO HOKKAI-GAKUEN UNIVERSITY Simple vector WIMP dark matter Weakly interacting massive particle is a good candidate for dark matter in many new physics models beyond the standard model at the TeV scale. We found for a vector dark matter particle associated with a broken gauge symmetry at the TeV scale, the higgs boson mass is naturally around 120--125 GeV. Near- future prospects of both direct and indirect detection experiments are also discussed.

PAUL BRINK SLAC NATIONAL ACCELERATOR LABORATORY Results and Status of the Cryogenic Dark Matter Search (CDMS) collaboration The Cryogenic Dark Matter Search (CDMS) collaboration uses Ge crystals cooled below 100 mK in its direct detection search at the Soudan Mine, Minnesota. Results from the CDMS II experiment indicated two candidate events but no claim of a WIMP discovery was made. A combined CDMS - EDELWEISS data analysis was performed which extended the WIMP search exclusion results for higher WIMP masses. Further analyses of CDMS II data were extended to lower energy thresholds with the WIMP exclusion limit obtained (no backgrounds subtracted) disfavoring the (background subtracted) CoGeNT results. All three collaborations use Ge as their target material. The CoGeNT results do indicate an annual modulation signal thus motivating a similar study of the CDMS II data, whose results will be discussed. The successor to CDMS II, SuperCDMS has double the Ge mass and more advanced detector instrumentation to allow the improved rejection of surface-electron background events. SuperCDMS is presently in operation at Soudan and we expect to demonstrate a Ge detector technology appropriate for a 100 kg-scale Ge experiment sited at SNOLAB with a WIMP search sensitivity of 3 x 10^-46 cm2 for the WIMP-nucleon spin- independent cross-section.

PIETRO CHIMENTI UFABC Current status of the ANGRA project: monitoring nuclear reactors with antineutrino detectors We will describe the status of the Angra Project, aimed at developing an antineutrino detector for monitoring nuclear reactor activity. Nuclear reactors are intense source of antineutrinos and the thermal power released in the fission process is directly related to the antineutrino flux, making antineutrino detectors good candidates for monitoring nuclear reactors in quasi real time and in a non-intrusive way through counting rates and energy spectrum measurements. The Angra experiment will use the Brazilian nuclear power plant Angra II, with 4 GW of thermal power, as a source of antineutrinos. The Angra neutrino detector was designed following tightly the recommendations of the International Atomic Energy Agency (IAEA) for a possible future use in safeguards; i.e. small footprint, non-flammable target material and easy to deploy. Therefore, a 1ton target water Cherenkov detector placed in a commercial container located at about 30 m of the reactor core is being built. With this configuration a few thousand inverse beta decay antineutrino reactions per day are expected. The final mechanic design project is ready and the detector parts are being presently produced. The front end and the readout electronics are ready and being tested. We will show the status of the detector construction, local background measurements and preliminary results on the performance of the electronics. The deployment in Angra is scheduled by June 2012 and the detector is expected to be commissioned by the end of 2012.

ROBERT FOOT UNIVERSITY OF MELBOURNE Mirror dark matter interpretations of DAMA, CoGeNT, CRESST-II experiments I propose updating my recent paper: http://arxiv.org/abs/1203.2387 which shows that DAMA, CoGeNT and CRESST-II experiments can be explained within mirror and more generic hidden sector dark matter models.

SANDRO DIAS PINTO VITENTI CBPF Quantization of Cosmological Perturbations in a Quantum Background When dealing with cosmological models in scales near the Planck length one needs to consider quantum effects on both background and perturbations. Naturally, such approach is just an approximation of what would be a complete treatment of quantum cosmology. Nevertheless, to apply such approach, one needs to work the second order action for the perturbations without using the background classical equations of motion. This restriction leads to a very complicated second order action. However, it was shown that it is possible to simplify this action performing a series of canonical transformations on the perturbation variables. We then obtain a simplified second order Hamiltonian, extending the known results to a general thermodynamic fluid in a Friedmann background with arbitrary spacelike hypersurfaces.

YU-FENG ZHOU KITPC/ITP-CAS Probing the fourth generation Majorana neutrino dark matter Heavy fourth generation Majorana neutrino can be stable and contribute to a small fraction of the relic density of dark matter (DM) in the Universe. Due to its strong coupling to the standard model particles, it can be probed by the current direct detection experiments even it is a subdominant component of the whole halo DM. Assuming that it contributes to the same fraction of the local halo DM density as that of the DM relic density,we show that the current Xenon100 data constrain the mass of the stable Majorana neutrino to be greater than the mass of the top quark. In the mass range between 200 GeV and a few hundred GeV, the effective spin-independent cross section for the neutrino elastic scattering off nucleon is insensitive to the neutrino mass and is predicted to be $sim 1.5times 10^{-44} cm^2$, which can be reached by the direct DM search experiments soon. In the same mass region the predicted effective spin- dependent cross section for the heavy neutrino scattering off proton is in the range $2times 10^{-40} cm^2sim 2times 10^{-39} cm^2$, which is within the reach of the ongoing IceCube experiment. We demonstrate such properties in a fourth generation model with the stability of the fourth Majorana neutrino protected by an additional generation-dependent U(1) gauge symmetry.