BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:The Strained State Cosmology DTSTART;VALUE=DATE-TIME:20110419T161500Z DTEND;VALUE=DATE-TIME:20110419T163000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-30@cern.ch DESCRIPTION:Speakers: Prof. TARTAGLIA\, Angelo (Politecnico di Torino)\nSp ace-time as a four-dimentional continuum has an evident similarity with or dinary three-dimensional continua\, apart from the Lorentzian signature of the metric tensor. Since it has physical properties related to its intera ction with matter\, the analogy suggests that it can behave as elastic con tinua do\, provided that general covariance is preserved. The theory that will be presented describes how to implement these ideas into a formally c onsistent cosmological scenario. The theory successfully accounts for the accelerated expansion and turns out to be consistent with a number of typi cal cosmological tests such as light elements abundances\, acoustic horizo n of the CMB\, large scale structure formation and SnIa luminosity/redshif t dependence.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=30 &sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=30&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Inflection point inflation with MSSM Higgs fields DTSTART;VALUE=DATE-TIME:20110418T154500Z DTEND;VALUE=DATE-TIME:20110418T160000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-54@cern.ch DESCRIPTION:Speakers: Mr. CHATTERJEE\, Arindam (University of Bonn)\nWe de monstrate that in the simplest CP conserving scenario\, the MSSM higgs fie lds can act as an inflaton\, in the presence of a Planck suppressed non-re normalizable term in the superpotential. The inflation occurs around an in flection point which can match the current WMAP data. Since inflation occu rs at a low scale\, the moduli problem does not appear\, and the supergrav ity corrections remain negligible. However\, there is a fine tuning needed between the MSSM paramaters involved\, at a high \nenergy scale. We use t he Suspect RGE code to show that\, however\, successful EWSB is possible o ver a large parameter space in spite of the fine tuning at a high scale\, and also that the fine tuning at a high scale does not correspond to any f ine tuning at the EWSB scale.\n\nhttp://indico.cern.ch/contributionDisplay .py?contribId=54&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=54&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Dark Matter direct detection DTSTART;VALUE=DATE-TIME:20110421T074500Z DTEND;VALUE=DATE-TIME:20110421T082500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-22@cern.ch DESCRIPTION:Speakers: ARMENGAUD\, Eric (CEA Saclay)\nhttp://indico.cern.ch /contributionDisplay.py?contribId=22&sessionId=4&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=22&sessionId=4& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:A large void versus the cosmological constant: still no verdict. DTSTART;VALUE=DATE-TIME:20110419T150000Z DTEND;VALUE=DATE-TIME:20110419T151500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-43@cern.ch DESCRIPTION:Speakers: Dr. VALKENBURG\, Wessel (ITTK\, RWTH Aachen)\nThe ev idence for the cosmological constant Lambda relies crucially on the postul ate that we do not live in a special place: the cosmological principle. To strengthen the evidence\, we must test that postulate and rule out altern atives. In this talk I will show how a very large spherically symmetric vo id can fit all existing evidence for Lambda simultaneously: the CMB\, BAO\ , SN and H0\, while using only Dark Matter and General Relativity but no L ambda. The purpose is to point out the different roles of assumptions and observations in the evidence for Lambda. Finally I will discuss the tests that should be performed in the future to rule out such a scenario\, putti ng Lambda on a firmer basis.\n\nhttp://indico.cern.ch/contributionDisplay. py?contribId=43&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=43&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Primordial fluctuations and non-Gaussianities in a Galilean theory DTSTART;VALUE=DATE-TIME:20110418T153000Z DTEND;VALUE=DATE-TIME:20110418T154500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-60@cern.ch DESCRIPTION:Speakers: Dr. RENAUX-PETEL\, Sebastien (University of Cambridg e)\nWe consider a multi-scalar-tensor model of gravity in which the action contains higher-order derivatives of the scalar fields without introducin g extra propagating degrees of freedom. In the context of an inflationary era\, we study the background evolution of this model as well as the linea r and non-linear properties of the cosmological fluctuations it generates. Orthogonal non-Gaussianities are shown to arise for the first time in a c oncrete model and new shapes of non-Gaussianities are identified.\n\nhttp: //indico.cern.ch/contributionDisplay.py?contribId=60&sessionId=7&confId=11 4928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=60&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Electroweak Baryogenesis from a Composite Higgs Sector DTSTART;VALUE=DATE-TIME:20110419T125000Z DTEND;VALUE=DATE-TIME:20110419T131000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-61@cern.ch DESCRIPTION:Speakers: RIVA\, Francesco (IFAE)\nOne of the most appealing e xplanation of physics at the electroweak scale is given by composite Higgs models\, where the Higgs boson is a bound state of a new strongly-interac ting dynamics. While the minimal realization of compositeness differs only slightly from the Standard Model (SM)\, non-minimal realizations\, based on larger coset structures\, can have a much richer phenomenology and acco unt for phenomena that can't be explained within the SM\, such as electrow eak baryogenesis (EWBG). In particular\, in models based on the SO(6)/SO(5 ) coset structure (which describe five light degrees of freedom: four belo nging to the Higgs and one belonging to a new light CP-odd scalar singlet) the existence of an extra gauge singlet in the Higgs sector influence the strength of the phase transition and its CP-odd couplings provide the ext ra source of CP violation.\nFurthermore\, at low energy\, this set up cons isting of the Higgs plus a CP-odd singlet coupled to the fermions\, provid es the most minimal scenario capable of explaining the baryon asymmetry.\n \nhttp://indico.cern.ch/contributionDisplay.py?contribId=61&sessionId=7&co nfId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=61&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Can thermal masses constrain the reheating temperature? DTSTART;VALUE=DATE-TIME:20110418T133000Z DTEND;VALUE=DATE-TIME:20110418T135000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-62@cern.ch DESCRIPTION:Speakers: Dr. DREWES\, Marco (Ecole Polytechnique Federale de Lausanne (EPFL))\nIt has been suggested that large thermal masses of the d ecay products can close the phase space for inflaton decay. This can impos e an upper bound on the reheating temperature which does not depend on the inflaton coupling. We study the problem from first principles of nonequil ibrium quantum field theory and discuss under which conditions this intuit ive argument\, based on the kinematics of classical particles\, can be app lied in the dense primordial plasma.\n\nhttp://indico.cern.ch/contribution Display.py?contribId=62&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=62&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:N-body simulations with generic non-Gaussian initial conditions DTSTART;VALUE=DATE-TIME:20110420T125000Z DTEND;VALUE=DATE-TIME:20110420T131000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-63@cern.ch DESCRIPTION:Speakers: Dr. WAGNER\, Christian (ICC\, University of Barcelon a)\nThe statistical nature of the initial conditions of the universe can b e most directly probed by observations of the early universe\, e.g. by the cosmic microwave background. However\, primordial non-Gaussianity can al so leave measurable signatures in the large-scale structure of the late-ti me universe. Observables like the galaxy cluster mass function\, the galax y bias and bispectrum are affected by the departures from Gaussianity in d istinctive ways. In order to derive constraints on primordial non-Gaussian ity from upcoming data of large-scale structure surveys\, accurate theoret ical modeling is needed. To this end\, N-body simulations are indispensabl e\, since the non-linear gravitational evolution has to be taken into acco unt.\nHere\, we introduce a prescription for setting up non-Gaussian initi al conditions for N-body simulations\, where the departures from Gaussiani ty are specified by a given primordial bispectrum. Using this technique\, we are able to run N-body simulations for the local and non-local types o f non-Gaussianity. Results of these simulations regarding the halo mass fu nction and the halo bias are presented and implications for large-scale st ructure probes of non-Gaussianity are discussed.\nMore details can be foun d in arXiv:1006.5793 and arXiv:1102.3229.\n\nhttp://indico.cern.ch/contrib utionDisplay.py?contribId=63&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=63&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Spontaneous Genesis DTSTART;VALUE=DATE-TIME:20110421T123000Z DTEND;VALUE=DATE-TIME:20110421T125000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-64@cern.ch DESCRIPTION:Speakers: Mr. MCCULLOUGH\, Matthew (Oxford University)\nN.A.\n \nhttp://indico.cern.ch/contributionDisplay.py?contribId=64&sessionId=7&co nfId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=64&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Light Dark Matter and Neutrino Telescopes DTSTART;VALUE=DATE-TIME:20110421T160000Z DTEND;VALUE=DATE-TIME:20110421T161500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-65@cern.ch DESCRIPTION:Speakers: Mr. WINKLER\, Martin (Technische Universität Münch en)\nI discuss the possibility of light dark matter as an explanation for the anomalies seen at the direct detection experiments DAMA\, CoGeNT and C RESST. I derive new strong limits on light dark matter from neutrino teles copes. Finally\, I introduce a realization of light dark matter in a singl et extension of the MSSM.\n\nhttp://indico.cern.ch/contributionDisplay.py? contribId=65&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=65&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Gauge Non-Singlet Matter Inflation in Supergravity DTSTART;VALUE=DATE-TIME:20110418T125000Z DTEND;VALUE=DATE-TIME:20110418T131000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-66@cern.ch DESCRIPTION:Speakers: Dr. ANTUSCH\, Stefan (MPI of Physics\, Munich)\nWe d iscuss a novel class of inflation models in supergravity with gauge non-si nglet matter fields as the inflaton. It is based on a ‘tribrid’ struct ure in the superpotential and on a ‘Heisenberg symmetry’ for solving t he η-problem. Inflation ends via a waterfall phase transition\, as in hyb rid inflation. In the context of grand unified theories\, the unified matt er superparticle provides a promising inflaton candidate. We also comment on how a generalization of this model class may be suitable for realising inflation in heterotic orbifold compactifications\, where the Heisenberg s ymmetry is a property of the tree-level Kahler potential of untwisted matt er fields.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=66&se ssionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=66&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Growing neutrino dark energy DTSTART;VALUE=DATE-TIME:20110419T153000Z DTEND;VALUE=DATE-TIME:20110419T154500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-67@cern.ch DESCRIPTION:Speakers: NUNES\, Nelson (U. Heidelberg)\nThe "growing neutrin o scenario" solves the coincidence problem of dark energy by a growing cos mological value of the neutrino mass which emerges from an interaction bet ween a scalar field and the neutrino. The field mediated attraction betwee n neutrinos induces the formation of large scale neutrino lumps in a recen t cosmological epoch. I will show that the non-linearities in the scalar f ield equation of motion stop the further increase of the neutrino mass whe n sufficiently dense and large lumps are formed. Consequently\, the neutri no induced gravitational potential is substantially reduced when compared to linear estimates. I will also demonstrate that inside a lump\, the poss ible time variation of fundamental constants is much smaller than their co smological evolution. This feature may reconcile current geophysical bound s with claimed cosmological variations of the fine structure constant.\n\n http://indico.cern.ch/contributionDisplay.py?contribId=67&sessionId=7&conf Id=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=67&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:New mechanism of generation of cosmological magnetic fields below electroweak scale DTSTART;VALUE=DATE-TIME:20110419T133000Z DTEND;VALUE=DATE-TIME:20110419T135000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-68@cern.ch DESCRIPTION:Speakers: Dr. RUCHAYSKIY\, Oleg (CERN)\nI will present a new m echanism of generation of cosmological magnetic fields below electroweak s cale and discuss their subsequent evolution. The mechanism is a byproduct of oscillations of sterile neutrinos\, also responsible for baryo and lept ogenesis and dark matter production.\n\nhttp://indico.cern.ch/contribution Display.py?contribId=68&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=68&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Unitarizing Higgs inflation DTSTART;VALUE=DATE-TIME:20110418T150000Z DTEND;VALUE=DATE-TIME:20110418T151500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-69@cern.ch DESCRIPTION:Speakers: Dr. LEE\, Hyun Min (CERN)\nWe consider a simple exte nsion of the Standard Model Higgs inflation with one new real scalar field which preserves unitarity up to the Planck scale. The new scalar field (c alled sigma) completes in the ultraviolet the theory of Higgs inflation by linearizing the Higgs kinetic term in the Einstein frame\, just as the no n-linear sigma model is unitarized into its linear version. The unitarity cutoff of the effective theory\, obtained by integrating out the sigma fie ld\, varies with the background value of the Higgs field. In our setup\, b oth the Higgs field and the sigma field participate in the inflationary dy namics\, following the flat direction of the potential. \nWe obtain the sa me slow-roll parameters and spectral index as in the original Higgs inflat ion but we find that the Hubble rate during inflation depends not only on the Higgs self-coupling\, but also on the unknown couplings of the sigma f ield.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=69&session Id=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=69&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Dark Matter Effective Theory DTSTART;VALUE=DATE-TIME:20110421T151500Z DTEND;VALUE=DATE-TIME:20110421T153000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-52@cern.ch DESCRIPTION:Speakers: DEL NOBILE\, Eugenio (Centre for Particle Physics Ph enomenology CP3-Origins)\nA large number of models for Dark Matter have be en put forward in recent years and compared with experimental data. A true model-independent analysis of the possible interaction terms is still not on the horizon. I will present the first step towards a future comprehens ive analysis which starts with constructing a well defined effective theor y for Dark Matter. We can now use our results for direct and indirect sear ches as well as for the study of Dark Matter genesis. Our approach allows for systematic improvements via quantum corrections\, at the effective Lan grangian level. While classifying our terms we made the discovery of the e xistence of interesting flavor-violating operators in the dark sector awai ting to be tested experimentally.\n\nhttp://indico.cern.ch/contributionDis play.py?contribId=52&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=52&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Nonstandard tensor modes from a pseudoscalar inflaton DTSTART;VALUE=DATE-TIME:20110418T123000Z DTEND;VALUE=DATE-TIME:20110418T125000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-53@cern.ch DESCRIPTION:Speakers: SORBO\, Lorenzo (University of Massachusetts\, Amher st)\nIn many models of inflation\, the inflaton is a pseudoscalar field th at is a potential source of parity violation. I will discuss a natural me chanism allowing to transfer parity violation from the inflaton into the C osmic Microwave Background (CMB). A pseudoscalar inflaton naturally intera cts with gauge fields through an axion-like coupling. Through this couplin g\, the rolling inflaton induces the production of quanta of the gauge fie ld\, that in their turn source the tensor components of the metric perturb ations. Due\nto the parity-violating nature of the system\, non-vanishing TB and EB correlation functions in the CMB are generated. I will also disc uss how the \ntensor modes generated this way might be directly detected b y gravitational wave interferometers such as advanced LIGO.\n\nhttp://indi co.cern.ch/contributionDisplay.py?contribId=53&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=53&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:DM/Baryo connection DTSTART;VALUE=DATE-TIME:20110421T094500Z DTEND;VALUE=DATE-TIME:20110421T102500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-24@cern.ch DESCRIPTION:Speakers: MARCH-RUSSELL\, John (Oxford)\nhttp://indico.cern.ch /contributionDisplay.py?contribId=24&sessionId=4&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=24&sessionId=4& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:The anthropic universe DTSTART;VALUE=DATE-TIME:20110422T070000Z DTEND;VALUE=DATE-TIME:20110422T074000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-25@cern.ch DESCRIPTION:Speakers: NOMURA\, Yasunori (UC Berkeley)\nhttp://indico.cern. ch/contributionDisplay.py?contribId=25&sessionId=5&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=25&sessionId=5& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Galileon DTSTART;VALUE=DATE-TIME:20110422T074500Z DTEND;VALUE=DATE-TIME:20110422T082500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-26@cern.ch DESCRIPTION:Speakers: DE RHAM\, Claudia (Université de Genève)\nhttp://i ndico.cern.ch/contributionDisplay.py?contribId=26&sessionId=5&confId=11492 8 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=26&sessionId=5& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Quantum gravity DTSTART;VALUE=DATE-TIME:20110422T090000Z DTEND;VALUE=DATE-TIME:20110422T094000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-27@cern.ch DESCRIPTION:Speakers: PUJOLAS BOIX\, Oriol ()\nhttp://indico.cern.ch/contr ibutionDisplay.py?contribId=27&sessionId=5&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=27&sessionId=5& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Non gaussianities DTSTART;VALUE=DATE-TIME:20110420T094500Z DTEND;VALUE=DATE-TIME:20110420T102500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-20@cern.ch DESCRIPTION:Speakers: SEFUSATTI\, Emiliano (CEA/Saclay)\nhttp://indico.cer n.ch/contributionDisplay.py?contribId=20&sessionId=3&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=20&sessionId=3& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Indirect Detection of Dark Matter: Status and Prospects DTSTART;VALUE=DATE-TIME:20110421T070000Z DTEND;VALUE=DATE-TIME:20110421T074000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-21@cern.ch DESCRIPTION:Speakers: BERGSTROM\, Lars (Stockholm University)\nhttp://indi co.cern.ch/contributionDisplay.py?contribId=21&sessionId=4&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=21&sessionId=4& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Constraining the dark matter density profile of milky way with gam ma-rays with Fermi-LAT DTSTART;VALUE=DATE-TIME:20110421T135000Z DTEND;VALUE=DATE-TIME:20110421T141000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-48@cern.ch DESCRIPTION:Speakers: Dr. BERNAL\, Nicolas (Uni Bonn)\nWe study the abilit ies of the Fermi-LAT instrument on board of the Fermi mission to constrain the dark matter density profile and the effect the uncertainties in the d ark matter distribution could have to constrain dark matter properties\, a s annihilation cross section\, mass and branching ratio into dominant anni hilation channels.\n\nhttp://indico.cern.ch/contributionDisplay.py?contrib Id=48&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=48&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:News from the front of DM theories DTSTART;VALUE=DATE-TIME:20110421T090000Z DTEND;VALUE=DATE-TIME:20110421T094000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-23@cern.ch DESCRIPTION:Speakers: SLATYER\, Tracy (Harvard University)\nhttp://indico. cern.ch/contributionDisplay.py?contribId=23&sessionId=4&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=23&sessionId=4& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Minimal models of inflation -- connecting cosmology and experiment DTSTART;VALUE=DATE-TIME:20110418T141000Z DTEND;VALUE=DATE-TIME:20110418T143000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-46@cern.ch DESCRIPTION:Speakers: Dr. BEZRUKOV\, Fedor (LMU)\nCurrent Standard Model o f elementary particles nicely describes (nearly) all phenomena observed in the laboratories. On cosmological scales the situation is much worse -- reliable experimental observations do not fit into the Standard Model. In the beginning the Universe had a period of inflationary expansion\, now i t is filled with Dark Matter and has baryon asymmetry. All these require explanation beyond the Standard Model. I will argue on the examples of th e model with light inflaton and of Higgs inflation that extending the SM i n a very minimal way leads to explanation of all these experimental facts\ , and connects Universe behaviour at the earliest (inflationary) stage to the possible effects in modern laboratories.\n\nhttp://indico.cern.ch/cont ributionDisplay.py?contribId=46&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=46&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Angular Clustering in Photometric Surveys: a new window for redshi ft distortions. DTSTART;VALUE=DATE-TIME:20110420T133000Z DTEND;VALUE=DATE-TIME:20110420T135000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-47@cern.ch DESCRIPTION:Speakers: Dr. CROCCE\, Martin (ICE)\nNear future cosmology wil l see the advent of wide area photometric galaxy surveys\, such as the DES \, PanSTARRS and LSST that extent to high redshifts (z ~ 2) but with poor radial distance resolution. In such cases splitting the data into redshift bins and looking at angular clustering will become the standard approach to extract cosmological information or\nto study the nature of dark energy through the Baryon Acoustic Oscillations (BAO) probe. In this talk I will present a comprehensive model for this clustering signal at large angular scales as a function of redshift and bin width\, including all relevant e ffects\, namely nonlinear gravitational clustering\, bias\, redshift space distortions and photo-z uncertainties. We also discuss\, and test against simulations\, a model for the full covariance matrix characterizing the a ngular correlation measurements. One interesting outcome is the potential of photometric surveys to yield constrains in the growth of structure thro ugh redshift space distortions. Hence we discuss the prospects for a full shape analysis of the angular correlation function at BAO scales in forthc oming photometric surveys.\n\nhttp://indico.cern.ch/contributionDisplay.py ?contribId=47&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=47&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter direct detection: a closer look at the astrophysical u ncertainties DTSTART;VALUE=DATE-TIME:20110421T131000Z DTEND;VALUE=DATE-TIME:20110421T133000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-44@cern.ch DESCRIPTION:Speakers: Dr. CATENA\, Riccardo (ITP\, Heidelberg)\nAlthough t here are great expectations from the LHC to shed light on physics beyond t he Standard Model and an eventual embedding of a dark matter candidate wit hin it\, a clean handle on the dark matter puzzle will come only from dire ct or indirect detection signals of dark matter particles within dark matt er halos. There are classes of dark matter candidates for which it is inde ed feasible to extract such signals\, for instance measuring the interacti on of a dark matter particle from the local population within a laboratory detector. A direct detection signal scales linearly with the local number density of dark matter particles and depends also on their local velocity distribution. In this talk I will show how Bayesian methods recently redu ced considerably the uncertainties on those quantities. For instance\, giv en a Galactic mass model and assuming a spherically symmetric dark matter halo\, the local dark matter density can be now determined with an accurac y of approximately the 10%. I will also discuss how such an approach\, com bined with Eddington's inversion formula for the phase-space density\, can be used to determine the dark matter local velocity distribution.\n\nhttp ://indico.cern.ch/contributionDisplay.py?contribId=44&sessionId=7&confId=1 14928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=44&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Supercurvaton DTSTART;VALUE=DATE-TIME:20110418T160000Z DTEND;VALUE=DATE-TIME:20110418T161500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-45@cern.ch DESCRIPTION:Speakers: DEMOZZI\, Vittoria (LMU Munich)\nI discuss the curva ton scenario implemented in the context of the simplest model of chaotic i nflation in supergravity. I investigate observational consequences and the oretical features of this model. The non-Gaussianity parameter f_{NL} in t his scenario can be either very small or very large\, and it can take diff erent values in different parts of the universe. Under certain conditions\ , this parameter can take values in the observationally interesting range from O(10) to O(100). This investigation makes a close connection between the fundamental theory of supergravity and the observational measurements. \n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=45&sessionId=7& confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=45&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:White smokes and Dark smokes in cosmology DTSTART;VALUE=DATE-TIME:20110422T094500Z DTEND;VALUE=DATE-TIME:20110422T102500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-28@cern.ch DESCRIPTION:Speakers: CARROLL\, Sean (Caltech)\nhttp://indico.cern.ch/cont ributionDisplay.py?contribId=28&sessionId=5&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=28&sessionId=5& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Anisotropic stress and (background) stability of modified gravity models DTSTART;VALUE=DATE-TIME:20110419T154500Z DTEND;VALUE=DATE-TIME:20110419T160000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-40@cern.ch DESCRIPTION:Speakers: Mr. SALTAS\, Ippocratis (University of Sussex)\nThe existence of an effective anisotropic stress at late times\, which in this case has a purely geometrical origin\, seems to be a characteristic of hi gher order gravity models\, and its detection will be a smoking gun for de partures from General Relativity (GR)\, for example in future weak lensing surveys. However\, no departure from GR has been as yet observed. In my t alk\, I will discuss and investigate the possibility of constructing a cla ss of modified gravity models of the general f(R\,G) type\, able to "hide" from weak lensing experiments by giving a GR-like behavior for the lensin g potentials\, i.e having a zero anisotropic stress. For both a de Sitter and matter background I will identify models with the desired property\, a nd will discuss the difficulties arising from such constructions\, such as instabilities and extreme fine tuning. In particular\, as I will show\, m odels with zero anisotropic stress in a de Sitter spacetime\, suffer from a background singularity\, that makes it impossible to reach de Sitter evo lution. Motivated by the latter fact\, I will proceed to discuss the link between the effective anisotropic stress and the (background) stability of the model as well as the presence of extra degrees of freedom\, which see ms to be a general feature of higher order gravity models.\n\nhttp://indic o.cern.ch/contributionDisplay.py?contribId=40&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=40&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Dark energy with non-adiabatic sound speed DTSTART;VALUE=DATE-TIME:20110419T135000Z DTEND;VALUE=DATE-TIME:20110419T141000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-41@cern.ch DESCRIPTION:Speakers: Dr. BALLESTEROS\, Guillermo (University of Padova)\n I will describe the prospects of detecting dark energy perturbations from Planck and a LSST-like survey. I will also discuss the initial conditions for dark energy perturbations in the radiation and matter epochs\, general izing the usual adiabatic ones to include the sound speed effect.\n\nhttp: //indico.cern.ch/contributionDisplay.py?contribId=41&sessionId=7&confId=11 4928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=41&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Dark energy and inhomogeneity DTSTART;VALUE=DATE-TIME:20110419T141000Z DTEND;VALUE=DATE-TIME:20110419T143000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-4@cern.ch DESCRIPTION:Speakers: CLARKSON\, Chris (University of Cape Town)\nI discus s how the averaging problem confuses our potential understanding of dark e nergy by considering the backreaction from density perturbations to second -order in the concordance model: this effect leads to at least a 10% incre ase in the dynamical value of the deceleration parameter\, and could be si gnificantly higher. Large Hubble-scale inhomogeneity has not been investig ated in much detail\, and could conceivably be the cause of apparent cosmi c acceleration. I discuss void models which defy the Copernican principle in our Hubble patch\, and describe how we can potentially rule out these m odels.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=4&session Id=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=4&sessionId=7&c onfId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Inflation DTSTART;VALUE=DATE-TIME:20110418T070000Z DTEND;VALUE=DATE-TIME:20110418T074000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-7@cern.ch DESCRIPTION:Speakers: SENATORE\, leonardo (stanford university)\nhttp://in dico.cern.ch/contributionDisplay.py?contribId=7&sessionId=1&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=7&sessionId=1&c onfId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Inflation and strings DTSTART;VALUE=DATE-TIME:20110418T090000Z DTEND;VALUE=DATE-TIME:20110418T094000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-9@cern.ch DESCRIPTION:Speakers: WESTPHAL\, Alexander (DESY Hamburg)\nhttp://indico.c ern.ch/contributionDisplay.py?contribId=9&sessionId=1&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=9&sessionId=1&c onfId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:(P)Re-heating DTSTART;VALUE=DATE-TIME:20110418T074500Z DTEND;VALUE=DATE-TIME:20110418T082500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-8@cern.ch DESCRIPTION:Speakers: BARNABY\, Neil ()\nhttp://indico.cern.ch/contributio nDisplay.py?contribId=8&sessionId=1&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=8&sessionId=1&c onfId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Electroweak lights from Dark Matter annihilation DTSTART;VALUE=DATE-TIME:20110421T153000Z DTEND;VALUE=DATE-TIME:20110421T154500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-49@cern.ch DESCRIPTION:Speakers: Dr. URBANO\, Alfredo (IFAE\, Universitat Autonoma di Barcelona & Università del Salento)\nThe computation of the energy spect ra of Standard Model particles originated from\nthe annihilation/decay of dark matter is a foudamental ingredient to investigate the possibility of its indirect detection. We compute how the inclusion of electroweak correc tions\nsigni\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=49& sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=49&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Galilean symmetry in the EFT of inflation: new shapes of non-Gauss ianity DTSTART;VALUE=DATE-TIME:20110418T151500Z DTEND;VALUE=DATE-TIME:20110418T153000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-39@cern.ch DESCRIPTION:Speakers: Dr. D'AMICO\, Guido (NYU)\nWe study the consequences of imposing an approximate Galilean symmetry on the Effective Theory of I nflation\, the theory of small perturbations around the inflationary backg round. This approach allows us to study the effect of operators with two d erivatives on each field\, which can be the leading interactions due to no n-renormalization properties of the Galilean Lagrangian. In this case cubi c non-Gaussianities are given by three independent operators\, containing up to six derivatives\, two with a shape close to equilateral and one peak ing on flattened isosceles triangles. The four-point function is larger th an in models with small speed of sound and potentially observable with the Planck satellite.\n\nhttp://indico.cern.ch/contributionDisplay.py?contrib Id=39&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=39&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Cosmological Perturbations in Horava-Lifshitz Gravity DTSTART;VALUE=DATE-TIME:20110420T152500Z DTEND;VALUE=DATE-TIME:20110420T154000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-75@cern.ch DESCRIPTION:Speakers: Dr. CERIONI\, Alessandro (University of Bologna)\nWe consider the most general action of Horava-Lifshitz Gravity in the presen ce of scalar matter with and without the projectability condition\, determ ine the actual number of propagating degrees of freedom of the linearized theory on the cosmological background and discuss the stability of the ext ra scalar mode that the theory exhibits.\n\nhttp://indico.cern.ch/contribu tionDisplay.py?contribId=75&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=75&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Helical magnetic fields from inflation and their evolution. DTSTART;VALUE=DATE-TIME:20110419T131000Z DTEND;VALUE=DATE-TIME:20110419T133000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-38@cern.ch DESCRIPTION:Speakers: Dr. HOLLENSTEIN\, Lukas (Département de Physique Th éorique\, Université de Genève)\nI discuss the generation of helical ma gnetic fields in single field inflation induced by an axial coupling of th e electromagnetic field to the inflaton. In slow roll\, such a coupling al ways leads to a blue spectrum\, P_B ~ k\, while a short deviation does not result in strong modifications to the shape of the spectrum. Then I consi der the subsequent evolution of the spectrum during the inverse cascade an d viscous damping of the helical magnetic fields. Although power is moved from small to larger scales\, the magnetic fields in this scenario are too weak to provide the seeds for the observed fields in galaxies and cluster s\; except for low scale inflation with very strong axial coupling\, a cas e where the perturbative treatment of the theory may break down. If time p ermits\, I discuss possible ways of amplification of primordial seed magne tic fields at late times through an axial coupling of electromagnetism to a dark energy scalar field.\n\nhttp://indico.cern.ch/contributionDisplay.p y?contribId=38&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=38&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Backreaction in the relativistic Zel’dovich approximation DTSTART;VALUE=DATE-TIME:20110419T151500Z DTEND;VALUE=DATE-TIME:20110419T153000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-73@cern.ch DESCRIPTION:Speakers: WIEGAND\, Alexander (Universitaet Bielefeld)\nZel’ dovich’s approximation is in Newtownian cosmology a practical tool to in vestigate the evolution of mildly nonlinear regions of the Universe. Its e xtension to the relativistic case is important for the investigation of th e backreaction of inhomogeneities on the evolution history of spatial doma ins of the Universe. This talk presents a Lagrangian framework that allows for a one to one correspondence of Newtownian and general relativistic qu antities and provides a non-perturbative backreaction model\, together wit h domain-dependent quantitiative estimates of the backreaction effect.\n\n http://indico.cern.ch/contributionDisplay.py?contribId=73&sessionId=7&conf Id=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=73&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Indirect Search for Dark Matter with the ANTARES Neutrino Telescop e DTSTART;VALUE=DATE-TIME:20110421T141000Z DTEND;VALUE=DATE-TIME:20110421T143000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-72@cern.ch DESCRIPTION:Speakers: BERTIN\, Vincent (Faculte des Sciences de Luminy)\nT he ANTARES Collaboration is now operating the largest water Cherenkov neut rino\ntelescope in the Nothern hemisphere. The apparatus\, completed in Ma y 2008\,\ncomprises 12 detection lines and a multidisciplinary instrumenta tion line \ninstalled at a depth of about 2500 m in the Mediterranean Sea offshore from France.\n\nThe goals of ANTARES are among others the search for astrophysical neutrino \npoint sources and for neutrinos produced in s elf-annihilation of Dark Matter \nparticles. In that respect\, the most pr omising sources of neutrino emission are \nthe Sun and the Galactic Centre \, where Dark Matter particles from the galactic \nhalo are expected to ac cumulate\, which should produce a clean signal much less affected\nby astr ophysical undertainties and/or backgrounds than for indirect detection wit h gamma rays.\n\nPrior to its completion\, ANTARES has been taking data fo r more than a year in an \nintermediate setup with a five and a ten line d etector configuration.\nFirst results on the search for Dark Matter annihi lations in the Sun with the data\nrecorded in 2007 and 2008 are presented\ , as well as sensitivity studies on Dark Matter \nsearches with the full A NTARES detector and the future large undersea cubic-kilometer \nneutrino t elescope studied by the KM3NeT consortium. A comparison with respect to pr edictions on neutrino fluxes from Dark Matter annihilations in the framewo rk of CMSSM and UED models will be presented.\n\nhttp://indico.cern.ch/con tributionDisplay.py?contribId=72&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=72&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Relic gravitational waves from light primordial black holes DTSTART;VALUE=DATE-TIME:20110421T161500Z DTEND;VALUE=DATE-TIME:20110421T163000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-71@cern.ch DESCRIPTION:Speakers: EJLLI\, Damian (University Of Ferrara)\nThe energy d ensity of relic gravitational waves (GWs) emitted by primordial black hole s (PBHs) is calculated. We estimate the intensity of GWs produced at quant um and classical scattering between PBHs\, the classical graviton emission from the PBH binaries in the early Universe\, and the graviton emission d ue to PBH evaporation. If nonrelativistic PBHs dominated in the cosmologic al energy density prior to their evaporation\, the probability of formatio n of dense clusters of PBHs and their binaries in such clusters would be s ignificant and the energy density of the generated gravitational\nwaves in the present day universe could exceed that produced by other known mechan isms. The intensity of these gravitational waves would be maximal in the G Hz frequency band of the spectrum or higher and this makes their observati on very difficult by the existing detectors. However\, the low frequency p art of the spectrum in the range $f\\sim 10^{-4}-10^2$ Hz may be detectabl e by the planned space interferometers DECIGO/BBO.\n\nFor a sufficiently l ong duration of the PBH matter dominated stage the cosmological energy fra ction of GWs from inflation would be noticeably diluted.\n\nhttp://indico. cern.ch/contributionDisplay.py?contribId=71&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=71&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Non-Abelian Discrete Dark Matter DTSTART;VALUE=DATE-TIME:20110421T125000Z DTEND;VALUE=DATE-TIME:20110421T131000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-70@cern.ch DESCRIPTION:Speakers: PRADLER\, Josef (Perimeter Institute for Theoretical Physics)\nWe consider the minimal model in which dark matter is stabilize d by a non-Abelian discrete symmetry. The symmetry group is taken to be D_ 3\, which is the smallest non-Abelian finite group. The minimal model con tains (nontrivial) singlet and doublet scalar representations of D_3 which couple to the Standard Model fields via the Higgs portal. This constructi on predicts two species of dark matter over much of the parameter space. N ontrival interactions under D_3 lead to a novel thermal history of dark ma tter\, while the multi-component nature of dark matter can be tested by fu ture direct detection experiments.\n\nhttp://indico.cern.ch/contributionDi splay.py?contribId=70&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=70&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Framework for performance forecasting and optimization of CMB B-mo de observations in presence of astrophysical foregrounds DTSTART;VALUE=DATE-TIME:20110420T144000Z DTEND;VALUE=DATE-TIME:20110420T145500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-59@cern.ch DESCRIPTION:Speakers: Mr. ERRARD\, Josquin (Laboratoire Astroparticule et Cosmologie)\nWe derived a semi-analytic formalism for performance forecast ing and optimization for future CMB experiments. The formalism accounts fo r statistical uncertainties due to the CMB sky statistics as well as prese nce of the foreground signals. We model the effects of subtraction of thes e using parametric maximum likelihood technique. \nAs an illustration of t his formalism\, we performed in this work both performance forecasting and optimization of future satellite CMB B-mode observations.\n\nhttp://indic o.cern.ch/contributionDisplay.py?contribId=59&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=59&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Gamma-Ray Lines from Radiative Dark Matter Decay DTSTART;VALUE=DATE-TIME:20110421T154500Z DTEND;VALUE=DATE-TIME:20110421T160000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-58@cern.ch DESCRIPTION:Speakers: TRAN\, David (Technical University of Munich)\nThe d ecay of dark matter particles which are coupled predominantly to charged l eptons has been proposed as a possible origin of excess high-energy positr ons and electrons observed by cosmic-ray telescopes PAMELA and Fermi LAT. Even though the dark matter itself is electrically neutral\, the tree-leve l decay of dark matter into charged lepton pairs will generically induce r adiative two-body decays of dark matter at the quantum level. Using an eff ective theory of leptophilic dark matter decay\, we calculate the rates of radiative two-body decays for scalar and fermionic dark matter particles. Due to the absence of astrophysical sources of monochromatic gamma rays\, the observation of a line in the diffuse gamma-ray spectrum would constit ute a strong indication of a particle physics origin of these photons. We estimate the intensity of the gamma-ray line that may be present in the en ergy range of a few TeV if the dark matter decay interpretation of the lep tonic cosmic-ray anomalies is correct and comment on observational prospec ts of present and future Imaging Cherenkov Telescopes\, in particular the CTA.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=58&sessionI d=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=58&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:The EW scale in cosmology DTSTART;VALUE=DATE-TIME:20110418T094500Z DTEND;VALUE=DATE-TIME:20110418T102500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-10@cern.ch DESCRIPTION:Speakers: SHAPOSHNIKOV\, Mikhail ()\nhttp://indico.cern.ch/con tributionDisplay.py?contribId=10&sessionId=1&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=10&sessionId=1& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Constraints on magnetic fields DTSTART;VALUE=DATE-TIME:20110419T074500Z DTEND;VALUE=DATE-TIME:20110419T082500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-13@cern.ch DESCRIPTION:Speakers: DURRER\, Ruth (University of Geneva)\nhttp://indico. cern.ch/contributionDisplay.py?contribId=13&sessionId=6&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=13&sessionId=6& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Hot relics: which ones\, how many\, and how to know more DTSTART;VALUE=DATE-TIME:20110419T070000Z DTEND;VALUE=DATE-TIME:20110419T074000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-12@cern.ch DESCRIPTION:Speakers: WONG\, Yvonne ()\nhttp://indico.cern.ch/contribution Display.py?contribId=12&sessionId=6&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=12&sessionId=6& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Gravitational Waves astronomy DTSTART;VALUE=DATE-TIME:20110419T094500Z DTEND;VALUE=DATE-TIME:20110419T102500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-15@cern.ch DESCRIPTION:Speakers: VECCHIO\, Alberto (Birmingham)\nhttp://indico.cern.c h/contributionDisplay.py?contribId=15&sessionId=6&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=15&sessionId=6& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Recent developments in baryo/lepto-genesis DTSTART;VALUE=DATE-TIME:20110419T090000Z DTEND;VALUE=DATE-TIME:20110419T094000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-14@cern.ch DESCRIPTION:Speakers: RAMSEY-MUSOLF\, Michael (U. Wisconsin-Madison)\nhttp ://indico.cern.ch/contributionDisplay.py?contribId=14&sessionId=6&confId=1 14928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=14&sessionId=6& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:CMB with Planck DTSTART;VALUE=DATE-TIME:20110420T070000Z DTEND;VALUE=DATE-TIME:20110420T074000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-17@cern.ch DESCRIPTION:Speakers: FINELLI\, Fabio (INAF)\nhttp://indico.cern.ch/contri butionDisplay.py?contribId=17&sessionId=3&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=17&sessionId=3& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Matter surveys DTSTART;VALUE=DATE-TIME:20110420T090000Z DTEND;VALUE=DATE-TIME:20110420T094000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-19@cern.ch DESCRIPTION:Speakers: PERCIVAL\, Will (University of Portmsouth)\nhttp://i ndico.cern.ch/contributionDisplay.py?contribId=19&sessionId=3&confId=11492 8 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=19&sessionId=3& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Tests of acceleration DTSTART;VALUE=DATE-TIME:20110420T074500Z DTEND;VALUE=DATE-TIME:20110420T082500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-18@cern.ch DESCRIPTION:Speakers: KUNZ\, Martin (Departement de Physique Theorique-Uni versite de Geneve)\nhttp://indico.cern.ch/contributionDisplay.py?contribId =18&sessionId=3&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=18&sessionId=3& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:The Coincidence Problem in a Phantom Cyclic Model of the Universe DTSTART;VALUE=DATE-TIME:20110419T160000Z DTEND;VALUE=DATE-TIME:20110419T161500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-31@cern.ch DESCRIPTION:Speakers: Ms. CHANG\, Hui-Yiing (Vanderbilt University)\nIn a phantom dark energy model\, the energy density increases with the expansio n of the Universe\, allowing it to go through standard cycles of radiation /matter domination\, followed by a dark energy/inflationary phase. There is a period in each cycle where the dark energy and matter densities are c omparable. Since the cycles repeat infinitely\, the Universe spends a sub stantial portion of its lifetime in such a state\; this significantly amel iorates the coincidence problem.\n\nhttp://indico.cern.ch/contributionDisp lay.py?contribId=31&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=31&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter searches with the Fermi-LAT DTSTART;VALUE=DATE-TIME:20110421T133000Z DTEND;VALUE=DATE-TIME:20110421T135000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-56@cern.ch DESCRIPTION:Speakers: ZAHARIJAS\, Gabrijela (CEA Saclay)\nBecause of its g ood sensitivity and angular resolution\, as well as energy coverage which includes 1-300 GeV range\, the Fermi-LAT is considered to be a prime tool for an indirect search of a signal of a WIMP annihilation. I will review c urrent dark matter search strategies by the Fermi-LAT team\, with a partic ular emphasis on the searches for cosmological DM annihilation in the extr agalactic diffuse emission.\n\nhttp://indico.cern.ch/contributionDisplay.p y?contribId=56&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=56&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter relic density at one loop level - effective coupling a pproach DTSTART;VALUE=DATE-TIME:20110421T150000Z DTEND;VALUE=DATE-TIME:20110421T151500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-37@cern.ch DESCRIPTION:Speakers: Ms. KULKARNI\, Suchita (BCTP and Physics Institute\, Bonn)\nThe lightest neutralino as a cold dark matter candidate has been w idely studied. Generally\, tree-level calculations of its (co-)annihilatio n cross sections are used to predict the relic density\, which leads to co nstraints on the parameter space. It has been known that these cross secti ons can change by order 10% at one loop level. However\, calculating these one loop corrections is computationally demanding and time consuming due to large number of diagrams. On the other hand\, with the launch of the Pl anck satellite the relic density of dark matter will be experimentally det ermined at a percent accuracy. Matching this accuracy requires the inclusi on of at least leading radiative corrections. We use the approach of effec tive couplings in order to reduce the computational stress. In this work\, we estimate the resulting corrections to the predicted neutralino relic d ensity\, and investigate the available parameter space at one loop level.\ n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=37&sessionId=7&c onfId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=37&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Cosmological Implications of Massive Clusters in the Early Univers e DTSTART;VALUE=DATE-TIME:20110420T123000Z DTEND;VALUE=DATE-TIME:20110420T125000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-36@cern.ch DESCRIPTION:Speakers: Dr. HOYLE\, ben (University of Barcelona)\nWe descri be recent observations of massive\, high redshift clusters of galaxies\, a nd show that they appear to be in tension with best fit WMAP 7 LCDM cosmol ogical parameters. We show that we can alleviate the tension by introducin g the non Gaussianity parameter fnl. We discuss other recent work on these massive objects.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribI d=36&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=36&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Imperfect Dark Energy of Kinetic Gravity Braiding DTSTART;VALUE=DATE-TIME:20110418T135000Z DTEND;VALUE=DATE-TIME:20110418T141000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-35@cern.ch DESCRIPTION:Speakers: VIKMAN\, Alexander (CERN)\nIn this talk I will discu ss a new class of cosmological scalar fields. Similarly to gravity\, these theories are described by actions linearly depending on second derivative s. The latter can not be excluded without breaking the generally covariant formulation of the action principle. Despite the presence of these second derivatives the equations of motion are of the second order. Hence there are no new pathological degrees of freedom. Because of this structure of t he theory the scalar field kinetically mixes with the metric- the phenomen on we have called Kinetic Gravity Braiding.\nThese theories have rather un usual cosmological dynamics which may be useful to model Dark Energy and I nflation.\nI will discuss an equivalent hydrodynamical formulation of thes e theories\, stability and causality for the fluid like\nconfigurations an d cosmological applications.\n\nhttp://indico.cern.ch/contributionDisplay. py?contribId=35&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=35&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Supersonic Electroweak Baryogenesis: Achieving Baryogenesis from F ast Bubble Walls DTSTART;VALUE=DATE-TIME:20110419T123000Z DTEND;VALUE=DATE-TIME:20110419T125000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-34@cern.ch DESCRIPTION:Speakers: Dr. NO\, Jose Miguel (IPhT CEA Saclay)\nIt is widely assumed that for the Electroweak Baryogenesis mechanism to be effective i n generating the baryon asymmetry of the Universe\, the first order phase transition bubbles have to expand at a subsonic speed (in order to allow f or the diffusion of CP asymmetric currents in front of the wall). Here we present a new mechanism for Electroweak Baryogenesis that is effective for supersonic bubble walls\, and relies on the formation of small bubbles of symmetric phase in the plasma behind the bubble wall (which is in the bro ken phase) due to the heating of the plasma as the wall passes by.\n\nhttp ://indico.cern.ch/contributionDisplay.py?contribId=34&sessionId=7&confId=1 14928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=34&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Vector fields and Loop Quantum Cosmology DTSTART;VALUE=DATE-TIME:20110418T161500Z DTEND;VALUE=DATE-TIME:20110418T163000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-33@cern.ch DESCRIPTION:Speakers: Mr. ARTYMOWSKI\, Michal (IFT\, University of Warsaw) \nIn the context of the Loop Quantum Cosmology we have analysed the holono my correction to the classical evolution of the simplified Bianchi I model in the presence of vector fields. For the Universe dominated by a massive vector field or by a combination of a scalar field and a vector field a s mooth transition between Kasner-like solution and expanding Bianchi I Univ erse has been demonstrated. In this case a lack of initial singularity and a finite maximal energy density appear already at the level of General Re lativity\, which simulates a classical Big Bounce.\n\nhttp://indico.cern.c h/contributionDisplay.py?contribId=33&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=33&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Non-Gaussianities in halo clustering properties DTSTART;VALUE=DATE-TIME:20110420T131000Z DTEND;VALUE=DATE-TIME:20110420T133000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-55@cern.ch DESCRIPTION:Speakers: Dr. DE SIMONE\, Andrea (Institut de Physique Theoriq ue-Ecole Polytechnique Federale de L)\nUsing excursion set theory\, and it s path-integral formulation\, \nit is possible to analytically compute se veral\nproperties of the dark matter halos\, like their distribution in m ass\,\nformation history\, and merging rate. The inclusion of non-Gaussian \ninitial conditions establishes an interesting connection between\nprimo rdial conditions and observable features of the large-scale universe.\nIn this talk\, I will briefly introduce the computational techniques \nand th en describe the results for halo mass functions and conditional\nprobabili ties with non-Gaussian initial conditions.\n\nhttp://indico.cern.ch/contri butionDisplay.py?contribId=55&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=55&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Modeling the shapes of dark matter halos DTSTART;VALUE=DATE-TIME:20110420T151000Z DTEND;VALUE=DATE-TIME:20110420T152500Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-74@cern.ch DESCRIPTION:Speakers: ROSSI\, Graziano (Korea Institute for Advanced Study (KIAS))\nWe combine the physics of the ellipsoidal collapse model with th e excursion set theory to study the shapes of dark matter halos. In partic ular\, we develop an analytic approximation to the nonlinear evolution tha t is more accurate than the Zeldovich approximation\, and we provide simpl e physical explanations for some empirical fitting formulae obtained from numerical studies. Comparison with simulations is challenging\, as there i s no agreement about how to define a non-spherical gravitationally bound o bject. Nevertheless\, we find that our model matches the conditional minor -to-intermediate axis ratio distribution rather well\, although it disagre es with the numerical results in reproducing the minor-to-major axis ratio distribution. We suggest that some of the disagreement with some previous numerical studies may be alleviated if we consider only isolated halos.\n \nhttp://indico.cern.ch/contributionDisplay.py?contribId=74&sessionId=7&co nfId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=74&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:Cosmological perturbations in the UV-protected inflation DTSTART;VALUE=DATE-TIME:20110418T131000Z DTEND;VALUE=DATE-TIME:20110418T133000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-32@cern.ch DESCRIPTION:Speakers: Dr. WATANABE\, Yuki (LMU Munich)\nIn natural inflati on\, the inflaton is a pseudo-Nambu-Goldstone boson which acquires a mass by explicit breaking of a global symmerty at scale f. In this case\, for s mall field values\, the potential is flat and stable under radiative corre ctions. However\, slow roll conditions enforce f much larger than M_pl mak ing the validity of the whole scenario questionable. In this talk\, we sho w that a coupling of the inflaton kinetic term to the Einstein tensor allo ws f much smaller than M_pl by enhancing the gravitational friction acting on the inflaton during inflation. This new interaction\, keeps the theory perturbative in the whole inflationary trajectory\, preserves the tree-le vel shift invariance of the pseudo-Nambu-Goldstone Boson and avoids the in troduction of any new degrees of freedom with respect to the standard natu ral inflation. We also study the nonlinear cosmological perturbations in t his model. We estimate the non-Gaussianity and show that the local-type no n-Gaussianity satisfies the single-field consistency relation.\n\nhttp://i ndico.cern.ch/contributionDisplay.py?contribId=32&sessionId=7&confId=11492 8 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=32&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:From k-essence to generalised Galileons and beyond... DTSTART;VALUE=DATE-TIME:20110420T145500Z DTEND;VALUE=DATE-TIME:20110420T151000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-57@cern.ch DESCRIPTION:Speakers: Mr. ZAHARIADE\, George (Laboratoire APC)\nWe constru ct the most general scalar field theory whose action depends on derivative s of order two or less and is polynomial in the second derivatives of the field\, under the condition that the equations of motion stay second order on flat space-time. This generalises k-essence\, Galileons\, k-Mouflage\, the kinetically braided scalars\, as well as the Euler hierarchies of Fai rlie et al.\, avoiding at the same time ghost-like degrees of freedom. The covariantization of such models\, as well as future directions\, are also discussed.\n\nhttp://indico.cern.ch/contributionDisplay.py?contribId=57&s essionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=57&sessionId=7& confId=114928 END:VEVENT BEGIN:VEVENT SUMMARY:What galaxy surveys really measure DTSTART;VALUE=DATE-TIME:20110420T135000Z DTEND;VALUE=DATE-TIME:20110420T141000Z DTSTAMP;VALUE=DATE-TIME:20130526T014749Z UID:indico-contribution-114928-50@cern.ch DESCRIPTION:Speakers: Dr. BONVIN\, Camille (University of Cambridge)\nGala xy redshift surveys measure the number of galaxies per solid angle as a fu nction of redshift. This observation is then used to infer the underlying matter power spectrum and learn about structure formation and cosmological parameters. The link between observation and matter density is however no t as simple as it is usually assumed. It is know since a long time that ga laxy number density measurements are affected by redshift-space distortion . In this talk I will show that in addition to this well-known correction\ , various relativistic effects enter in the relation between the observed galaxy number density and the underlying physical quantities\, i.e. densit y perturbation\, peculiar velocity and gravitational potential. I will sho w how to express the observable in terms of gauge invariant variables and I will discuss the various corrections to the standard result. At small re dshift\, the dominant contribution comes from peculiar velocities of galax ies\, whereas at large redshift magnification gives the largest contributi on. These corrections are relevant at large scales and are large enough to be observed in future galaxy redshift surveys.\n\nhttp://indico.cern.ch/c ontributionDisplay.py?contribId=50&sessionId=7&confId=114928 LOCATION:Palais des Papes\, Avignon Chambre du Trésorier URL:http://indico.cern.ch/contributionDisplay.py?contribId=50&sessionId=7& confId=114928 END:VEVENT END:VCALENDAR