\centering\Large Abstracts received up to 2/6//2009

Abstracts received up to 2/6//2009

Torsion balance tests of the Equivalence Principle, the Inverse Square Law and Lorentz Invariance

E.G. Adelberger, T. Cook, J.H. Gundlach, C. Hagedorn, B.R. Heckel, S. Schlamminger and T. Wagner CENPA, University of Washington, Seattle WA, 98195-4290 USA

presented by:Adelberger E.G. email-eric@npl.washington.edu, phone-+! 206 543 4080, fax-+1 206 685 4634

This talk summarizes recent results of sensitive torsion-balance "gravitational" experiments of the Eöt-Wash Group. The Principle of Equivalence (universality of free fall) has been tested using 3 different test-body pairs to a precision of a few parts in 1013. The gravitational inverse-square law has been tested for separations less than 60 mm, establishing an upper limit of 44 mm on the largest possible size of an ëxtra" dimension; ongoing experiments should impove this limit. Tests of Lorentz Invariance with 1023 polarized electrons reveal no effects at a level 10-5 times the benchmark value me2/MPlanck.

Influence of the interplanetary parameters on the 27-day variation of cosmic rays

Rekha Agarwal, Rajesh K. Mishra 1Department of Physics, Govt. Model Science College (Autonomous), Jabalpur (M.P.) 482 001, India 2Computer and IT Section, Tropical Forest Research Institute, P.O. RFRC, Mandla Road, Jabalpur (M.P.) 482 021, India

presented by: Agarwal Rekha email-rm_ jbp@yahoo.co.in, rkm_ 30@yahoo.com, phone-917612601225, fax-917612840484

The observed modulation of galactic cosmic ray intensity on time and spatial scales contains information regarding their transport in the heliosphere. We used the data of cosmic ray neutron monitor as well as interplanetary parameters to identify the correlation between their 27-day variations. The 27-day variation of cosmic ray intensity is found to linearly correlated with the interplanetary magnetic field strength (B), the north south component (Bz) of the interplanetary magnetic field vector and the product of the solar wind speed (V) times B (V x B). The cross correlation function of the 27-day cosmic ray variation versus the solar wind speed shows a negative correlation. However, the 27-day variation of cosmic rays is correlated with the variation in both the x- and y- components of interplanetary magnetic field.

EW Physics @Tevatron

Tim Andeen Northwestern

presented by: Andeen Tim email-, phone-, fax-

The observed correlations for the strange multibaryon states in systems with l-hyperon from pa collision at momentum of 10 gev/c

P.Zh.Aslanyan Joint Institute for Nuclear Research, Dubna

presented by: Aslanyan P.Zh. email-paslanian@jinr.ru, phone- , fax-

The observed well-known resonances S*+(1385) and K*±(892) from PDG are good tests of this method. Exotic strange multibaryon states have been observed in the effective mass spectra of: L p±,L g, L p, L p p, L K0S, K0Sp± subsystems. The measured L/p+ ratio for average multiplicities from pC reaction is approximately two times larger than the L/p+ ratio, simulated by FRITIOF model and than that of experimental pp reactions at the same energy. The mean value of mass for S*-(1385) resonance is shifted till mass of 1370 MeV/c2 and width is two times larger than the same value from PDG. Such kind of behavior for width and invariant mass of S*-(1385) resonance is interpreted as extensive contribution from stopped X-®Lp- and medium effect with mass. There are enhancement production for all observed hyperons.

Searches for dark matter candidates in Upsilon decays in BaBar

the BaBar collaboration

presented by a representative from the BaBar collaboration. Abstract submitted by Owen Long, physics analysis coordinator.  email-owen@slac.stanford.edu, phone-650 926 5287, fax-

Several extensions of the Standard Model, motivated by recent astrophysical observations, predict existence of a relatively light dark matter component, and/or of a light scalar field A0. Due to the large coupling of the A0 to b[`b], radiative decays of the U states can be a significant source of such particles. We present results of direct searches for A0 decaying into both visible and invisible final states. We also present results on a search for invisible decay of the Upsilon meson, observation of which might signal the existence of a low-mass dark matter component. These measurements use data recorded on the U(2S) and U(3S) resonances the BaBar collaboration.

Dark matter from hidden valley

Seungwon Baek, Taeil Hur, Pyungwon Ko Korea Univ, KAIST, KIAS

presented by: Baek Seungwon email-sbaek@korea.ac.kr, phone-+82-2-10-3730-6293, fax-

We consider a hidden sector with a new strong interaction, and a new extra U(1)X under which both the SM and the hidden sector particles are charged. The lightest hadron in the hidden sector, the so-called hidden sector pion, can be a good cold dark matter candidate, and its dynamics at low energy can be described by hidden sector chiral lgrangian. We consider the constraints on the model and compute the relic density of the hidden sector pions, and its elastic scattering cross section on nucleons, both spin-independent and spin-dependent. We also consider the phenomenology of the extra gauge and higgs boson.

A New Method to Standardize Luminosity Distance Measurements of SNe Ia Using Spectral Flux Ratios

Stephen Bailey for the Nearby Supernova Factory Collaboration LPNHE - Paris

presented by: Bailey Stephen email-stephen.bailey@lpnhe.in2p3.fr, phone-+33/0 1 44 27 72 53 , fax-

We present a new method to standardize luminosity distance measurements of Type Ia supernovae (SNe Ia). This method uses spectral flux ratios to standardize observed SN Ia peak magnitudes providing a  6

SNLS 3rd year cosmological results

C. Balland, the SNLS collaboration LPNHE, Tour 43 RdC, 4 Place Jussieu, 75252 Paris Cedex, France

presented by: email-balland@lpnhe.in2p3.fr, phone-33 (0)1 44 27 63 18, fax-33 (0)1 44 27 46 38

Type Ia supernovae (SNe Ia) currently provide the most direct evidence for an accelerating Universe and for the existence of an unknown dark energy driving this expansion. The Supernova Legacy Survey (SNLS) is a five-year project which has delivered around 500 high-redshift SNe Ia light curves and spectra in the redshift range 0.2 < z < 1.0 in order to constrain the dark energy equation of state, w. We present the cosmological results obtained with ~ 240 SNe Ia followed-up during the first 3 years of the survey. This supernova dataset is the largest homogeneous high redshift sample available today. It allows us to test for various systematic uncertainties potentially affecting our measurement and therefore derive robust cosmological constraints.

Is the Carter-Israel conjecture correct?

Cosimo Bambi (1), Katherine Freese (2), Rohta Takahashi (3) (1) IPMU, The University of Tokyo, (2) MCTP, University of Michigan, (3) RIKEN

presented by: Bambi Cosimo email-cosimo.bambi@ipmu.jp, phone-+81-4-7136-4956, fax-+81-4-7136-4973

According to the Carter-Israel conjecture, the end-state of the gravitational collapse of matter is a Kerr-Newman black hole. However, both the theory and observations cannot yet confirm that is correct. In this talk, we discuss the possibility that the final product of the gravitational collapse may be a more compact object which violates the Kerr bound a < M. In particular, we show how near future observations at the sub-mm wavelength of Sgr A* can test this scenario for the black hole candidate in the Galactic Center.

Addressing certain anomalies in early universe particle production

A.W. Beckwith American institute of Beamed energy propulsion

presented by: Beckwith A.W. email-abeckwith@uh.edu, phone-650-322-6768, fax-

The following is a compilation of typical problems in early universe cosmology • At the EXTREMA of any function: dx/dt =0 • But for Big-Bang dS/dt =¥; at S=0 • Hardly Homogeneous Perfect Fluid at  100 Mpc • Yet Hubble Flow Embarrassingly smooth  5 Mpc! • Flatness & Fine Tuning Problem The author asserts that resolving the problems mentioned above involves a re do of conventional models of relic particle production,i.e. specifically relic neutrino production, and early traces of DM. The talk endeavors to predict what, as an example resolving the extremal production problem of entropy tells us about candidates for both neutrino production and DM candidates in the early universe

Composition Studies of Ultra-High Energy Cosmic Rays using Depth of Shower Maximum by the High-Resolution Fly's Eye Observatory

John Belz, for the HiRes Collaboration University of Utah

presented by: John Belz email-belz@cosmic.utah.edu, phone-801-585-9620, fax-801-581-6256

Both the mean value of airshower maximum Xmax and the width of the Xmax distribution are known to be sensitive to the chemical composition of cosmic rays initiating a set of extensive airshowers. Thus, studies of Xmax are an important part of efforts to understand the nature and origin of Ultra-High Energy Cosmic Rays. With the Northern Hemisphere's largest exposure to date to cosmic rays above 1018 eV, the two fluorescence detectors of the High-Resolution Fly's Eye (HiRes) Observatory are uniquely positioned to study this phenomenon. Here, we report the results of recent studies of the depth of airshower maximum Xmax in cosmic-ray induced extensive airshowers observed in stereo by HiRes.

Brane Universe: Global Geometry

Victor Berezin Institute for Nuclear Research Russian Academy of Sciences Moscow Russia

presented by: Berezin Victor email-berezin@ms2.inr.ac.ru, phone-+7 (499) 188-00-10, fax-+7 (499) 135-68-22

The global geometries of bulk vacuum space-times in the brane-universe models are investigated and classified in terms of geometrical invariants. The corresponding Carter-Penrose diagrams and embedding diagrams are constructed. It is shown that for a given energy-momentum tensor induced on the brane there can be different types of global geometries depending on the signs of a bulk cosmological term and surface energy density of the brane (the sign of the latter does not influence the internal cosmological evolution). It is shown that in the Randall-Sundrum scenario it is possible to have an asymmetric hierarchy splitting even with a Z2-symmetric matching of öur" brane to the bulk.

Status of the Telescope Array Fluorescence Detectors

Douglas Bergman Rutgers University

presented by: Douglas Bergman email-bergman@physics.rutgers.edu, phone-001-7324455500 x0052, fax-001-7324454343

The Telescope Array fluorescence detectors have been operating since November 2007. Details of the operations and analysis from the three fluorescence sites will be presented.

VHE gamma-astronomy observations with the ARGO-YBJ detector

Paolo Bernardini on behalf of the ARGO-YBJ Collaboration Dipartimento di Fisica, Università del Salento and Istituto Nazionale di Fisica Nucleare, Lecce, Italy

presented by: Bernardini Paolo email-paolo.bernardini@le.infn.it, phone-+39 0832 297443, fax-+39 0832 325128

Very High Energy gamma ray astronomy and cosmic ray physics are the main goals of the ARGO-YBJ experiment. The detector is located in Tibet (People's Republic of China) and is a full coverage Extensive Air Shower array consisting of a carpet of Resistive Plate Chambers (RPC). Altitude and full coverage ensure an energy threshold of few hundreds of GeV for primary photons detected in shower mode, while the RPC time resolution gives a good pointing accuracy, thus allowing a high sensitivity to g-ray sources. The large field of view and the high duty-cycle allow the continuous monitor of the Northern sky in the declination band (-10°, +70°). The detector operates also in scaler mode in order to look for GRB signal in the range 1-100 GeV in coincidence with GRB detection by satellites. The performances of the detector and the present results concerning VHE g-ray astronomy will be presented.

Thermodynamic equilibrium conditions for mass varying particle structures

Alex E Bernardini Departamento de Física, Universidade Federal de Sao Carlos, PO Box 676, 13565-905, Sao Carlos, SP, Brasil

presented by: Bernardini Alex E. email-alexeb@ufscar.br, phone-55-19-3351-9174, fax-

Assuming that the so-called dynamical mass behaves like an additional extensive thermodynamic degree of freedom leads to modifications on the thermodynamic equilibrium conditions for compact structures composed by mass varying particles. As a natural consequence, such weakly interacting massive particles can form clusters of non-baryonic matter or even astrophysical objects that, at cosmological scales, are held together by gravity and an attractive force mediated by a background scalar field which feels the effects of the space-time curvature. The equilibrium conditions for resultant static, spherically symmetric objects of uniform energy density are derived for the case where the compounding particles share the key features of the mass varying mechanism in cosmological scenarios. Some physically reasonable solutions which results in formation of stable astrophysical lumps are found.

A Cold Clear Window on the Dark Universe - Progress Towards WIMP Detection with the Large Underground Xenon (LUX) Dual Phase Detector at Homestake.

Adam Bernstein (on behalf of the LUX collaboration) - Dan Akerib ,Susie Bedikian ,Adam Bernstein ,Alexander Bolozdynya ,Adam Bradley ,Ronald Bybee ,Sidney Cahn ,Dennis Carr ,Yuen-Dat Chan ,Jeremy Chapman ,Ken Clark ,Tim Classen ,Alessandro Curioni ,Eric Dahl ,Steven Dazeley ,Mike Dragowsky ,Eryk Druszkiewicz ,Carlos Hernandez Faham ,John Felde ,Simon Fiorucci ,Brian Fujikawa ,Richard Gaitskell ,Carter Hall ,Britt Holbrook ,Louis Kastens ,Kareem Kazkaz ,John Kwong ,Richard Lander ,Robert Lanou ,Douglas Leonard ,Kevin Lesko ,David Malling ,Rachel Mannino ,Daniel McKinsey ,Dongming Mei ,James Nikkel ,Patrick Phelps ,Ryan Sacks ,Udo Schroeder ,George Seidel ,Thomas Shutt ,Wojtek Skulski ,Peter Sorensen ,Tyana Stiegler ,Robert Svoboda ,Melinda Sweany ,John Thomson ,Jan Toke ,Mani Tripathi ,Luiz de Viveiros ,Nick Walsh ,Robert Webb ,James White ,Frank Wolfs ,Michael Woods ,Hengkui Wu Lawrence Livermore National Laboratory, Brown University, Case Western, L! awrence Berkeley National Laboratory, Texas A& M University, UC Davis, University of Maryland, University of Rochester, University of South Dakota, Yale University

presented by: Bernstein Adam email-bernstein3@llnl.gov, phone-(925) 422 5918, fax-

If Weakly Interacting Massive Particles exist, the rare feeble recoils they induce in Earthly nuclei would represent a tantalizing brush with the Dark Universe. Here I discuss progress towards direct WIMP detection with the Large Underground Xenon detector (LUX), a dual phase detector to be deployed in the Homestake Mine near Deadwood South Dakota in the United States. LUX, a 300 kg detector, should allow a roughly hundred-fold more sensitive WIMP search than previous efforts. I will discuss the remarkable sensitivity and attractively simple scaling features of dual-phase xenon detectors that make this gain possible, and describe our group's inexorable progress towards deployment of LUX at Homestake.

High energy neutrinos from active celestial objects via leptonic processes

Arunava Bhadra High Energy & Cosmic Ray Research Centre, University of North Bengal, Siliguri, WB, 734013, India

presented by: Bhadra Arunava email-aru_ bhadra@yahoo.com, phone-913532776358, fax-913532699001

The detection of extraterrestrial neutrinos is supposed as confirm signature for the presence of energetic hadrons in high energy astrophysical sources such as young pulsars, active galactic nuclei, gamma-ray bursters etc. Here we show that neutrinos could also be produced in leptonic processes in some astrophysical scenarios. We also estimate the flux of high energy neutrinos originated in such processes.

The shape of galaxy groups and clusters

Monika Biernacka, Elena Panko, Teresa Juszczyk, Piotr Flin Jan Kochanowski University, Odessa National University, Czacki High School

presented by: Biernacka Monika email-bmonika@ujk.kielce.pl, phone-, fax-

Ellipticities for 6188 low - redshift poor and rich galaxy structures have been examined along with their evolution using an optical observational base that is statistically complete. The shape of each structure projected on the celestial sphere was determined using the covariance ellipse method. Analysis of the data indicates that structure ellipticity changes with redshift, being smaller for nearby objects and greater for those located further away. Such a change is also described better by quadratic or exponential relations than by a simple linear scheme. The sample was divided according to structure richness, representing ten richness classes, with the distribution of ellipticities being different for individual classes. The mean redshift of a structure class is a function of richness, with more poorly populated classes exhibiting greater mean redshift than richer galaxy clusters. Further analysis reveals a dependence of the ellipticity - redshift correlation on structure richness. Among rich galaxy clusters there is an anticorrelation between the parameters, the strongest correlation occuring for poorly populated galaxy classes.

Cosmic topology and fundamental forces

J. J. van der Bij Institut fuer Physik, Universitaet Freiburg, H. Herderstr. 3, 79104 Freiburg, Allemagne

presented by: van der Bij J. J. email-jochum@physik.uni-freiburg.de, phone-0049 761 203 5791, fax-0049 761 203 5869

I present an argument, based on the topology of the universe, why there are three generations of fermions. The argument implies that the gauge group of nature is SU(5), but with SO(10) representations of the fermions. On the basis of the argument one expects the presence of a preferred direction in space, that may have been seen already.

No Higgs at the LHC.

J. J. van der Bij Institut fuer Physik, Universitaet Freiburg, H. Herderstr. 3, 79104 Freiburg, Allemagne

presented by: van der Bij J. J. email-jochum@physik.uni-freiburg.de, phone-0049 761 203 5791, fax-0049 761 203 5869

I discuss a recently developed new class of renormalizable models for the Higgs sector. I compare with the LEP data, which are interpreted as a discovery of the Higgs field. I conclude that the LHC will most likely not see a signal for the Higgs particle.

Observations from the Nearby Supernova Factory: improving SNe Ia as cosmological probes.

S.Bongard, G.Aldering, P.Antilogus, C.Aragon, C.Baltay, S.Bailey, C.Buton, M.Childress, N.Chotard, Y.Copin, E.Gangler, S.Loken, P.Nugent, R.Pain, E.Pecontal, R.Pereira, S.Perlmutter, D.Rabinowitz, G.Rigaudier, K.Runge, R.Scalzo, G.Smadja, H.Swift, C.Tao, R.C.Thomas, C.Wu LPNHE, LBNL, Yale University, IPNL, CRAL

presented by: Bongard Sébastien email-bongard@in2p3.fr, phone-+33 1 44 27 41 23, fax-

We present results from the Nearby Supernova Factory (SNfactory) that have important impact on the use of SNe Ia as cosmological probes. The SNfactory is a program of integrated discovery, followup, and analysis of nearby supernovae to address the limiting factors of SN dark energy measurements. In this talk especially concentrate on the information content of spectrophotometry and its impact on control of environmental effects and systematic errors. We present how the SNfactory dataset can be used to build light curves without K corrections in the photometric system best matched for combining with high-z data, thus addressing one of the largest source of systematic errors when using SNe Ia as cosmological probes. We also discuss how such a dataset can be used to find correlations between spectroscopic and photometric properties of SNe Ia. Finally, we show how spectrophotometry gives a handle on host extinction separation from intrinsic effects, and thus constrains one of the most crucial environmental contaminations of cosmological measurements using SNe Ia.

Correlation of the highest energy cosmic rays with nearby extragalactic objects in Pierre Auger Observatory data

C. Bonifazi for the Pierre Auger Collaboration LPNHE - Laboratoire de Physique Nucléaire et des Hautes Energies, Paris, France Observatorio Pierre Auger, Av. San Martín Norte 304, (5613) Malargüe, Mendoza, Argentina

presented by: Bonifazi C. email-bonifazi@lpnhe.in2p3.fr, phone-+33 1 44 27 73 31, fax-

The Pierre Auger Observatory is uniquely designed for the study of the highest energy cosmic rays. It is a giant hybrid detector that measures extensive air showers with a surface array of water-Cherenkov detectors viewed by fluorescence telescopes. Data collected by the observatory provided evidence for anisotropy in the arrival directions of the cosmic rays with the highest energies by their correlation with the positions of relatively nearby active galactic nuclei (AGN). In this work we update the analysis of this correlation and we discuss it in terms of the energy threshold, maximum distance and angular separation with respect to the AGNs.

The Fermi-LAT as an high energy electron spectrometer


presented by: BREGEON Johan email-johan.bregeon@pi.infn.it, phone-+390502214396, fax-

The Fermi Large Area Telescope (LAT), has been surveying the high-energy sky since August 2008. This poster describes how the LAT collaboration is using the LAT as an electron spectrometer to obtain a highly-precise measurement of the flux of primary cosmic-ray electrons from 20 GeV to 1 TeV. All the details of this innovative analysis will be covered: instrument response (particularly the energy resolution), hadron rejection capability, validation of the LAT Monte Carlo simulation with CERN beam test data and flight data, and estimation of the systematic errors associated with each step. The cosmic-ray electron spectrum measured with the LAT and its implications will be presented separately by Alex Moiseev.

Observation of Crab Nebula with the HAGAR telescope system at Hanle in the Himalayas

R. J. Britto for the HAGAR collaboration Tata Institutre of Fundamental Research, Mumbai Indian Institute of Astrophysics, Bangalore

presented by: Britto Richard email-britto@tifr.res.in, phone-+912222782540, fax-+912222804610

We have observed Crab nebula using the recently commissioned wave-front sampling high altitude (4270 m amsl) array, HAGAR, at Hanle in the Ladakh region of the Himalayas. Regular source observations have begun with the complete setup of 7 telescopes since Sept. 2008. HAGAR is the first array of atmospheric Cherenkov telescopes established at a so high altitude and was designed to reach a relatively low threshold with quite a low mirror area (31 sq m). Preliminary values for the angular resolution of the arrival direction estimate was found to be 0.2 +/- 0.15 deg. for a field of view of 3 deg. Estimation of the sensitivity of the experiment is undergoing using several hours of data from the direction of crab nebula, the standard candle source of TeV gamma ray astronomy. Data were acquired using the On-source/Off-source mode and by comparing these sky regions the strength of the gamma-ray signal could be estimated. Gamma-ray events arrive close to telescope axis direction whil! e the cosmic-ray background events arrive from the whole field of view. We discuss our analysis procedures for the estimate of arrival direction, estimate of gamma-ray flux from Crab nebula and the sensitivity of the HAGAR system etc in this paper.

Observation of Blazars 1ES2344+514 and Mkn421 using the HAGAR telescope system

R. J. Britto et al., (on behalf of HAGAR collaboration) Tata Institute of Fundamental Research, Mumbai Indian Institute of Astrophysics, Bangalore

presented by: Britto R. J. email-, phone-, fax-

We have observed 2 blazars 1ES2344+514 and Mkn421 using the recently commissioned high altitude (4270 m amsl) array, HAGAR, at Hanle in the Himalayas. The blazar 1Es2344+514 (z=0.044), one of the bright extra-galactic sources in the TeV gamma-ray catalog, was observed during Sept-Nov, 2008. Observations of the Bl Lac object Mkn421, known to flare up and well studied in many wavelengths, has started in March 2009. Observations were carried out using the On-source/Off-source mode. The event trigger rate was about 10Hz, corresponding to a gamma ray energy threshold of about 200 GeV. The detailed analysis of our data, comparison of day to day variations in flux with those of other wavelenghts whereever possible will be presented in this paper.

On the Dark Matter solution to the cosmic lepton puzzle

P. Brun, T. Delahaye, J. Diemand, F. Donato, D. Maurin, S. Profumo, P. Salati IRFU - CEA Saclay LAPTh, Annecy & Universita di Torino University of California, Santa Cruz Universita di Torino, LPNHE, Paris University of California, Santa Cruz LAPTh, Annecy

presented by: Brun Pierre email-pierre.brun@cea.fr, phone-0169084264, fax-

Recent measurements of cosmic ray leptons by PAMELA, ATIC and HESS revealed interesting excesses. Many authors suggested WIMP Dark Matter (DM) annihilations could be at the origin of these effects. However, natural values for the DM particle parameters lead to a poor leptons production so that models often require signal enhancement effects that we constrain here. Considering DM annihilations are likely to produce antiprotons as well, we use the PAMELA antiproton/proton measurements to constrain possible exotic contribution. We also consider the possibility of an enhancement due to a nearby clump of DM. This scenario appears unlikely when compared to the state-of-the-art cosmological N-body simulations.

Is Rastall's Model a suitable possibility?

Monica Capone Università di Torino and INFN

presented by: Capone Monica email-monica.capone@unito.it, phone-+390116702933, fax-

Following the search for a suitable explanation of the recent phase of accelerated expansion our universe is undergoing, we review the Rastall's Model that is a model based on the request that the stress-energy tensor of whatever source of gravitation be non-conserved. We start by facing the problem of the variationale derivation of Rastall's equations of motion, problem unsolved hitherto, showing that this derivation is not possible either in the metric case, nor in the Palatini one. Then, we examine the type of universe one may realize, also focusing on the possibility to obtain a Cardassian-type model.

Higgs funnel region of supersymmetric dark matter for small tanb with scalar mass nonuniversality

Utpal Chattopadhyay and Debottam Das Indian Association for the Cultivation of Science, Kolkata, India

presented by: Chattopadhyay Utpal email-tpuc@iacs.res.in, phone-+91-33-2473-4971 (x285), fax-+91-33-2473-2805

A non-universal scalar mass supergravity type of model is explored where the first two generation of scalars and the third generation of sleptons may be very massive. Lighter or vanishing third generation of squarks as well as Higgs scalars at the unification scale cause the radiative electroweak symmetry breaking constraint to be less prohibitive. Thus, both FCNC/CP-violation problems as well as the naturalness problem are within control. We identify a large slepton mass effect in the RGE of mHD2 (for the down type of Higgs) that may turn the later negative at the electroweak scale even for a small tanb. A hyperbolic branch/focus point like effect is found for mA2 that may result in very light Higgs spectra. The lightest stable particle is dominantly a bino that pair annihilates via Higgs exchange, giving rise to a WMAP satisfied relic density region for all tanb. Detection prospects of such LSPs in the upcoming dark matter experiments both of direc! t and indirect types (photon flux) are interesting. The Higgs bosons and the third generation of squarks are light in this scenario and these may be easily probed besides charginos and neutralinos in the early runs of LHC.

Search and Study of CH3CN in Interstellar medium

Chaulagain, U. P.; Aryal, B.; Central department of physics, Tribhuvan University, Kathmandu, Nepal

presented by: Chaulagain, U. P. email-lepton.bibesh@gmail.com, phone-009779841532564, fax-

We present the binding energy, rotational constant, rotational frequency and rotational temperature of CH3CN in different basis sets using Gaussian03. A systematic search of the emission region at 115 GHz is carried out using SkyView Virtual Observatory. A region is selected and studied in the context of rotational temperature of CH3CN using ALADIN2.5 software. From the ab-initio (First principle) calculation of CH3CN in the Hartree Fock level of approximation it is found that there is a strong binding between H, C and N in CH3CN, minimum value of the binding energy being 12.79 eV in the basis set 6-311G which agrees within around 8 e in the same basis set 6-31G* is found to be 7.74 K which agrees within around 4

Causality and hidden dimensions in astrophysical light curves

Anton Chernenko IKI

presented by: Chernenko Anton email-anton@cgrsmx.iki.rssi.ru, phone-+7(495)5086984, fax-+7(495)3331389

Relativistically expanding sources produce radiation that manifest rich spectral evolution and diverse light curve structures. Even if individual emitting regions have similar and simple geometry and rest frame spectra, spectral and temporal evolution within any period of observer's time would be very diverse, since many of individual emitters would contribute to this period at different viewing angles, Lorentz factors and at different stages of development.
In this paper I present multi-scale, multi-lag correlation analysis of light curves recorded in different energy ranges: from the optical to hard gamma-rays, which allows one to determine number of emitters and extract properties of each emitter.

Nancay radiotelescope as part of the international Pulsar Timing campaigns

Cognard I, Desvignes G, Dumora D, Ferdman F, Guillemot L, Hessels J, Kramer M, Possenti A, Smith D, Stappers B, Theureau G LCP2E Orleans, France Nancay Obs, France CENBG Gradignan, France Max Planck Institute, Germany Amsterdam Univ, Netherland Manchester Univ, England Cagliari Obs, Italy

presented by: COGNARD Ismael email-icognard@cnrs-orleans.fr, phone-238257908, fax-238631234

Nancay radiotelescope is involved in high precision timing since 20 years. Since 2004, a state of the art instrumentation enables numerous routine observations on more than 200 pulsars using half of the time if this 100-meters class radiotelescope. Two main programs are currently conducted. A set of highly stable millisecond pulsars is monitored as our contribution to the European Pulsar Timing Array in order to probe the cosmological Gravitational Wave Background. A larger set of young and old pulsars is timed for a multi-wavelength approach, complementary to the very successful high energy observations of pulsars done by FERMI.


Francois Corriveau for the ZEUS and H1 collaborations IPP / McGill University

presented by: Corriveau V. email-corriveau@physics.mcgill.ca, phone-1-514-398-6515, fax-1-514-398-8434

HERA is an electron-collider which has terminated its operations in 2007. Large amounts of experimental data are currently being analyzed. A brief review of the highlights of the QCD studies performed by the ZEUS and H1 will be presented, followed by the latest results on the proton structure functions and on as, the coupling constant of the strong interaction.

Sensitivity of the ANTARES and KM3NeT neutrino telescopes to bursts from galactic supernovae

Heide Costantini on behalf of the ANTARES collaboration INFN Genova

presented by: Costantini Heide email-costant@ge.infn.it, phone-+39 010 353 6336, fax-

The ANTARES Mediterranean neutrino telescope, designed and optimized for detection of Cherenkov light from interactions of neutrinos with energy above 100 GeV, could be sensitive to an intense neutrino burst from the core collapse of a massive star in our galaxy. This neutrino flux would produce a global increase of the rate of the detector above the usual background level during the short time interval of the burst (  10 s). The prospects for the detection of supernova signals with ANTARES and with the future km3 Mediterranean telescope KM3NeT will be discussed in this talk.

Non-SUSY @Tevatron

Dave Cutts  Brown

presented by: Cutts Dave email-, phone-, fax-

Twenty years of ground-based gamma-ray astronomy

Bernard DEGRANGE LLR Ecole polytechnique and CNRS/IN2P3

presented by: Degrange Bernard email-degrange@llr.in2p3.fr, phone-01 69 33 55 45, fax-01 69 33 55 08

The discovery of the TeV gamma-ray emission of the Crab nebula by T. Weekes et al. at the Whipple observatory in 1989 was at the origin of the rapid expansion of ground-based gamma-ray astronomy. To date, more than 70 gamma-ray sources emitting at energies greater than 100 GeV have been firmly detected, most of them by Imaging Atmospheric Cherenkov Telescopes. The progress in instrumentation which led to a gain in sensitivity of about two orders of magnitude in 20 years is described. Some highlight results both on galactic and extragalactic sources are given to show that this new field is increasingly involved in the astrophysics of violent phenomena, complementing radio, optical, X-ray and GeV gamma-ray observations. Prospects aiming at ground-based detectors with a milli-Crab sensitivity in the next decade are described.

LHCb Commissioning and Potential Early Results

Marc Deissenroth Physikalisches Institut, Universitaet Heidelberg

presented by: Deissenroth Marc email-deissenroth@physi.uni-heidelberg.de, phone-+496221-549238, fax-

The LHCb (Large Hadron Collider beauty) detector is designed to study B meson decays with very high precision. The construction and installation of the LHCb detector has been finished early summer 2008, followed by intensive testing and commissioning of the system in order to be ready for the first data taking. Despite the horizontal geometry of the spectrometer we were able to collect over 1 million useful cosmic events that allowed a first time and space alignment of most of the subdetectors. Moreover events from beam dumps during the LHC synchronisation tests provided very useful data for further calibration. Here we will present an overview and results from our commissioning activities and an outlook on the second startup end of this year including a brief summary of the potential early physics results.

Higgs @LHC

Marco Delmastro  CERN

presented by: Delmastro Marco email-, phone-, fax-

Fermionic cosmologies

Chimento L., Devecchi F., Forte M., Kremer G., Ribas M. Depto. de Fisica, UFPR, Curitiba-Brazil

presented by: Devecchi F. email-devecchi@fisica.ufpr.br, phone-55 41 3361 3666, fax-

In this work we discuss if fermionic sources could be responsible for accelerated periods during the evolution of a universe where a matter (bosonic) field would answer for decelerated periods. The coupled diff. equations for the laws of motion are integrated numerically. The fermionic self-interaction potential is a function of scalar and pseudo-scalar invariants. It is shown that the fermion could behave like an inflaton field in the early universe and as dark energy for an old universe. In a second part we focus on analytical results, using the idea of form-invariance transformations FIT. These FIT can be used for modelling phantom cosmologies starting with conventional models. Here we reconsider the scalar field case and extend the discussion to fermionic fields, where the phantomization process shows a new class of possible accelerated regimes.

Dark matter annihilation in small-scale clumps

Veniamin Berezinsky, Vyacheslav Dokuchaev and Yury Eroshenko Institute for Nuclear Research of the Russian Academy of Sciences. 60th October Anniversary Prospect 7a, 117312 Moscow, Russia and INFN, Laboratori Nazionali del Gran Sasso, I-67010 Assergi (AQ), Italy

presented by: Dokuchaev Vyacheslav email-dokuchaev@lngs.infn.it, phone-+74959381738, fax-+74959385325

The small-scale clumps of dark matter particles are efficiently disrupted by tidal forces during formation and evolution of the Galaxy. Surviving the remnants of small scale dark matter clumps is considered by modelling the tidal destruction of clumps in the early hierarchical structures formation and by stars in the Galaxy. It is shown that a substantial fraction of clump remnants may survive through the tidal destruction during the lifetime of the Galaxy if a radius of clump core is rather small. The resulting mass function of survived clumps is extended down to the mass of the core of the cosmologically produced clumps with a minimal mass. The dense remnants of clumps provide a suitable contribution to the amplification (boosting) of the dark matter annihilation signal in the Galaxy.

GeV and TeV photon absorption in the external photon fields of a binary supermassive black hole system

Alina Donea Centre for Stellar and Planetary Astrophysics School of Mathematical Sciences Monash University

presented by: Alina Donea email-alina.donea@sci.monash.edu.au, phone-+40 0728776231, fax-+61 3 9905-4403

Gamma-ray absorption due to photon-photon pair production of gamma-ray jet photons travelling in the external photon environment of a binary supermassive black hole system is considered. We investigate to what extent the location of a gamma-ray emitter exposed to the anisotropic radiation field of both accretion disks affects the gamma-ray opacity. The simple model analysed in this paper consists of a primary black hole surrounded by a standard accretion disk in symbiosis with a relativistic jet. The secondary black hole located at a given position nearby has a similar mass (or smaller) and is surrounded by a viscous small-sized accretion disk. We show that for standard parameters of the accretion disks and a separation distance between the two black holes of 0.05 to 0.1 pc (close system), there is still a significant gamma-ray absorption from the secondary disk.

Sneutrino Dark Matter

Bhaskar Dutta Texas A& M University

presented by: Dutta Bhaskar email-dutta@physics.tamu.edu, phone-(979)845-5359, fax-

In this talk, I will discuss sneutrino dark matter in the U(1)B-L extension of the minimal supersymmetric Standard Model where the right-handed sneutrino is a natural candidate for thermal dark matter. The sneutrino dark matter explains recent results from the PAMELA and ATIC experiments in both thermal and non-thermal scenarios of this model. The cosmological moduli and the gravitino problems are solved in the non-thermal scenarios. The annihilation of sneutrinos mainly produces taus (or muons) by the virtue of B-L charges. The sneutrino-nucleon elastic scattering cross section is large enough to be probed by upcoming and future direct detection experiments. We will show that when this model explains the Pamela data, the direct detection experiment can distinguish between the thermal and non-thermal scenarios. In addition, if (at least) one of the neutrinos is dominantly a Dirac fermion, the sneutrino can provide a unified picture of dark matter and inflation.
Based on: PRL.99:261301,2007; arXiv:0812.2196 (PRD); arXiv:0902.3463; To appear

Heavy Flavors Physics @Tevatron

Hal Evans Indiana

presented by: Evans Hal email-, phone-, fax-

Tau Astronomy in Short Times

Daniele Fargion Physics Department, Rome University 1, Sapienza and INFN Rome 1

presented by: Fargion Daniele email-daniele.fargion@roma1.infn.it, phone-00-39-0649914287, fax-00-39-064957697

UHE Neutrino Astronomy is expected soon. UHE Muon Neutrino in ICE-CUBE might reveal PeV astrophysical signals within atmospheric ones. Higher energy astrophysical tau neutrinos, mostly EeV via GZK secondaries, born by flavor mixing and equipartition, hit noise-free the Earth. Their escaping taus lead to loud tau-air-showers. Their detectionin in AUGER is already at the detection edge. Ande may enhance the signal. However UHECR might be, for some author, lightest nuclei and not nucleons. The GZK neutrinos secondaries are not at EeV but at 0.1-0.01 EeV. Their discover may nevertheless come in short time too, because larger rate and surprising detection road.

Study of the polarized foreground emissions for the analysis of the PLANCK CMB data

J.F. Macias-Pérez, L.Fauvet, LPSC Grenoble

presented by: Fauvet L. email-fauvet@lpsc.in2p3.fr, phone-0476284390, fax-

The PLANCK satellite mission which will be launched in April 2009 is dedicated to the measurement of the Cosmic Microwave Background (CMB) anisotropies in temperature and polarization. From this measurement will be accurately constraint the cosmological parameters describing for example the content in energy and matter of the Universe. In particular, it could give access to the BB polarization modes which will allows us to study the epoch of inflation. The presence of diffuse galactic polarized emissions disturb the measurement of the CMB anisotropies, in particular in polarization, and therefor a good knowledge of these emissions is needed to obtain the order of accuracy required for PLANCK. In this context, we have developed and implemented 3D models of the two mains polarized galactic emissions : synchrotron and dust. We have compared these models to the WMAP, ARCHEOPS and Haslam data and obtained the best fit parameters for them. From this, we are able to estimate the contribution of polarized foreground emission to the polarized CMB emission with PLANCK.

Post-Newtonian modelling of compact binary systems: higher order effects of spin and eccentricity; higher order gravitational-wave amplitude corrections

Guillaume Faye

presented by: Faye Guillaume

Modelling accurately compact binary systems in their late inspiralling phase is of cardinal importance in the context of current or future gravitational-wave experiments, both for detection and for data analysis using matched filtering techniques. Up to quite recently, attention has been mainly focused on non-spinning objects in quasi-circular orbit, though the spin-orbit and spin-spin interactions have been known since the early seventies while the radiated energy flux of elliptical systems was obtained up to the second post-Newtonian (2PN) order a few years ago. More emphasis is made now on (i) higher order spin-effects, which have been investigated with various methods, including effective field theory calculations, as well as (ii) higher order PN contributions in the case of non-zero eccentricity. Most notably, the complete 3PN energy flux for quasi-elliptical orbits has been computed and may now be used to construct accurate templates by means of a well-defined procedure. For non-spinning compact bodies in quasi-circular orbit, the 3PN order has been finally reached in the signal amplitude.

Toward an Understanding of Hadron-Hadron Collisions: From Feynman-Field to the LHC

Rick Field University of Florida

presented by: Field Rick email-rfield@phys.ufl.edu, phone-(352) 392-5702, fax-(352) 392-5339

I will discuss the evolution of our understanding of hadron-hadron collisions at high energy starting from the Field-Feynman "black-box" model and ending with the present day QCD Monte-Carlo model extrapolations to the LHC. In addition, I will explain some of what we have learned from studies of "min-bias" collisions and the ünderlying event" in high transverse momentum jet production and in Z-boson production at the Tevatron.

Orientation of galaxy groups in the Local Supercluster

Piotr Flin, Wlodzimierz Godlowski Jan Kochanowski University, Institute of Physics, Kielce, Poland, Opole University, Institute of Physics, Opole, Poland,

presented by: Flin P. email-sfflin@cyf-kr.edu.pl, phone-, fax-48 + (0)41 + 3496443

Tully's "Nearby galaxies catalog" contains the list of galaxies assigned to galaxy groups. We compiled two sets of data, extracting groups containing at least 10 and 20 member galaxies. The first set contained 61 groups, the second one 35. The ellipticity of the structures were determined applying the covariance ellipse method. Distance and coordinates of the group centre were calculated too. We confirm that galaxy group major axes tend to point toward their neighbours in the scale smaller than 20 Mpc. We also study other possible orientation correlations in data.


Gabriella Gaudio  Pavia

presented by: Gaudio Gabriella email-, phone-, fax-

Gamma Ray Burst Discoveries with the Swift Mission

Neil Gehrels NASA/GSFC

presented by: Gehrels Neil email-, phone-, fax-

Gamma-ray bursts (GRBs) are among the most fascinating occurrences in the universe. They are powerful explosions, visible to high redshift, and thought to be the signature of black hole formation. The Swift Observatory has been detecting 100 bursts per year for 4 years and has greatly stimulated the field with new findings. Observations are made of the X-ray and optical afterglow from  1 minute after the burst, continuing for days. Evidence is building that the long and short duration subcategories of GRBs have very different origins: massive star core collapse to a black hole for long bursts and binary neutron star coalescence to a black hole for short bursts. The similarity to Type II and Ia supernovae originating from young and old stellar progenitors is striking. Bursts are providing a new tool to study the high redshift universe. Swift has detected several events at z>5 and one at z=6.7 giving metallicity measurements and other data on galaxies at previously inaccessible distances. The talk will present the latest results from Swift in GRB astronomy.

Status and preliminary results of EDELWEISS-II


presented by: Gerbier Gilles email-eric.armengaud@cea.fr, phone-01 69 08 19 50, fax-

The EDELWEISS II experiment is devoted to the search for the WIMPs that would constitute the Dark Matter halo of our Galaxy. For this purpose, the experiment uses cryogenic germanium detectors in which the collision of a WIMP with an atom produces characteristic signals in terms of ionization and elevation of temperature. We will present preliminary results attesting to the very low radioactive background conditions achieved so far. Novel detectors, with a special electrode design for active rejection of surface events, have been shown to be suited for searches of WIMPs with scattering cross-sections on nucleon well below 10-8 pb. Preliminary results of WIMP search performed with a first set of these detectors will be shown as well.

Extremely Large Telescopes

Roberto Gilmozzi European Southern Observatory

presented by: Gilmozzi Roberto email-rgilmozz@eso.org, phone-+49-89-320060, fax-+49-89-32006838

I will report on the status of the projects for the next generation of extremely large telescopes that should start operations by the end of the next decade, in particular ESO's E-ELT which is undergoing its Phase B detailed design. I will review the science case, ranging from imaging and spectroscopy of extra solar planets to the direct dynamical measurement of the acceleration of the expansion of the universe. I will also discuss the synergies between ELTs and other contemporary future facilities (e.g. ALMA, JWST, SKA).

Some time dependent systematic effects in the Planck temperature angular power spectrum compared to the cosmic variance.

Damien Girard, Cecile Renault, Juan-Francisco Macias-Perez, Laurence Perotto, Francois-Xavier Desert. Laboratoire de Physique Subatomique et de Cosmologie de Grenoble, Laboratoire d'Astrophysique de l'Observatoire de Grenoble

presented by: Girard Damien email-damien.girard@lpsc.in2p3.fr, phone-04 76 15 36 50, fax-

Planck aims at providing the "definitive" temperature angular power spectrum of the relic radiation as errors should be dominated by the cosmic variance up to the fifth peak. It implies a strict control of all possible systematic error sources. Among systematic effects are time dependent ones: cosmic ray hits have a huge short time impact while thermal variability of the HFI instrument and the Planck telescope have a soft but long time influence. Looking to the angular temperature power spectrum, I will check that the Planck sensitivity to the parameters of the standard cosmological model or to some exotic models is not degraded by our treatment of these systematic effects.

Testing nuMSM in accelerator experiments.

Dmitry Gorbunov, Mikhail Shaposhnikov, Sergey Gninenko INR, Moscow; ITPP, Lausanne

presented by: Gorbunov Dmitry email-gorby@ms2.inr.ac.ru, phone-+7(499)7839291, fax-+7(499)1352268

The minimal extension of the Standard Model with three righthanded neutrinos is capable of explaining the active neutrino oscillations, the baryon asymmetry of the Universe and the dark matter. This extension can be tested by searches for cosmic photons in keV-range from decays of relic long-lived lightest sterile neutrinos and by direct seraches for production and decays of two heavier sterile neutrinos in accelerator experiments. There most promising are searches for meson decays to sterile neutrinos and searches for sterile neutrino decays in beam-dump type experiments. Within nuMSM both lower and upper limits exist for the production and decay rates, which makes these searches powerful in testing nuMSM.

Chemical composition of ultra-high energy cosmic rays at energies above 1018 eV from the analysis of Yakutsk muon data.

A.V. Glushkov, I.T. Makarov, M.I. Pravdin, I.E. Sleptsov, D.S. Gorbunov, G.I. Rubtsov, Sergey V. Troitsky  INR, Moscow; Cosmophys. Res. Inst., Yakutsk

presented by: Gorbunov Dmitry email-gorby@ms2.inr.ac.ru, phone-+7(499)7839291, fax-+7(499)1352268

The Yakutsk experiment provides the unique possibility to measure directly and independently two main components of extensive air showers: electromagnetic component and muon component. Large statistics collected for 30 years allows to probe with electromagnetic and muon data the chemical composition of ultra-high energy cosmic rays at energies above 1018 eV. In particular, the high sensitivity to photons gives the possibility to enter GZK-region for the first time. Study of muon rich showers gives the possibility to test various models describing the development of hadronic component of extensive air showers. The results of new analysis will be presented.

An original constraint on the Hubble constant: h>0.74

Aurélien Barrau (1) Alexia Gorecki (1) Julien Grain (2) (1): Laboratoire de Physique Subatomique et de Cosmologie, Université Joseph Fourier, CNRQ/IN2P3/INPG (2)Laboratoire AstroParticle et Cosmologie, Université Paris 7, CNRQ/IN2P3

presented by: Gorecki Alexia email-gorecki@lpsc.in2p3.fr , phone-+33 4 76 28 41 79 , fax-

A new method, based on the absorption of very high-energy gamma-rays by the cosmic infrared background, was developed to constrain the value of the Hubble constant. As this value is both fundamental for cosmology and still not very well measured, such alternative methods are mandatory. Our lower limit at 68% confidence level is H0 > 74km.s-1MPc-1, leading, when combined with the HST results, to H0=76km.s-1MPc-1. Interestingly, this value, which is significantly higher than the usually considered one, is in exact agreement with other independent approaches based on baryonic acoustic oscillations and X-ray data. Future data from HESS-2 and CTA should help improving those results and make our method very effective.

Searches for gravitational waves from compact binary coalescences with LIGO and Virgo

Romain Gouaty, for the LIGO Scientific Collaboration and the Virgo collaboration LAPP, Annecy

presented by: Gouaty Romain email-gouaty@lapp.in2p3.fr, phone-04 50 09 16 72, fax-04 50 27 94 95

The LIGO-Virgo joint scientific collaboration is looking for gravitational waves emitted during the coalescence of massive compact objects (neutron stars, black holes) in the data collected during the S5-VSR1 science run. The analysis is based on a match-filtering technique. Different template families are used: inspiral post-Newtonian templates for low-mass binaries (up to 35 Msun), inspiral-merger-ringdown templates for high-mass binaries (up to 100 Msun), and ring-down templates for perturbed massive black holes (up to 600 Msun). The collaboration pursues all-sky all-time searches as well as externally triggered searches (GRBs). We present an overview of these searches and discuss the prospectives for the upcoming S6-VSR2 run.

MIMAC: a micro-TPC for dark matter directional detection

C. Grignon, J. Billard, G. Bosson, O. Bourrion, O. Guillaudin, C. Koumeir, F. Mayet, D. Santos, A. Allaoua, L. Lebreton, P. Colas, E. Ferrer, I. Giomataris  LPSC

presented by: Grignon Cyril email-cyril.grignon@lpsc.in2p3.fr, phone-04 76 28 40 00, fax-04 76 28 40 04

MiMac is a project of micro-TPC matrix of gaseous chambers (helium, CF4 ...) for direct detection of non-baryonic dark matter. Measurement of both track and ionization energy will allow the electron-recoil discrimination, while access to the directionnality of the tracks will open a unique way to distinguish a geniune WIMP signal from any background. Firsts results of low energy nuclei recoils obtained with a neutron beam will be presented as well as the expected performances of the directional detector.

Discovery of a population of gamma-ray millisecond pulsars with Fermi

L. Guillemot Centre d'Etudes Nucleaires de Bordeaux Gradignan (CENBG)

presented by: Guillemot L. email-guillemo@cenbg.in2p3.fr, phone-33(0) 557120795, fax-

Before the launch of the Fermi Gamma-ray Space Telescope in June 2008, it was uncertain whether millisecond pulsars (MSPs) were gamma-ray emitters. Although some of these fast rotators (periods of ones to tens of milliseconds) have kinetic energy loss rates comparable to those of their younger counterparts, none of them had previously been firmly identified as a pulsed gamma-ray source. The first months of Fermi-LAT data revealed that PSR J0030+0451 is a bright 4.86 ms gamma-ray pulsar. Then a systematic search for radio MSPs in the galactic plane showed that there is a whole population of gamma-ray sources among the known millisecond pulsars. The spectral shapes of the detected MSPs resemble those of young pulsars. However, the gamma-ray light curves may show complexity similar to that seen in radio wavelengths as photon counts accumulate. We will review these results, and show that there are prospects that the Fermi-LAT may detect individual millisecond pulsars in globular! clusters, where millisecond pulsars are known to be abundant.

Analytically solvable model for fusion near coulomb barrier

Rajiv Gupta*, S.S.Malik*, A.K.Jain** * - Guru Nanak Dev University ** -Indian Institute Of Technology, Roorkee

presented by: Gupta Rajiv email-rajiv_ gupta_mirage@yahoo.com, phone-9463789469, fax-

Using the asymmetric two-center shell model potential in parameterized forms,the dynamical solution for the radial and the mass asymmetry coordinates are obtained analytically for the fusion process near the Coulomb barrier. Our semiclassical quantization results for the radial degree of freedom fixes the maximum excitation energy carried by the compound nucleus and agrees reasonably well with the observed value.The shell effects of the colliding partners play an important role in deciding the incident energy for a reaction to take place.Our results show the nucleus Z=122,A=300 as a doubly magic. Our calculations further emphasize that the doubly magic reaction partners prompt the phenomenon of large mass transfer even at low excitation energy.

Detection of ultra-high energy cosmic rays at the Pierre Auger Observatory with radio antennas

S. Harmsma, for the Pierre Auger Collaboration KVI University Groningen, The Netherlands

presented by: Harmsma S. email-harmsma@kvi.nl, phone-+31-50 363 2054, fax-+31 50 363 4003

The Pierre Auger Observatory is used to study air showers induced by cosmic rays at the highest energies. Secondary charged particles are deflected by the Earth's magnetic field emitting radiation, which can be observed in radio bands. As a first step for the 20 km2 Auger Engineering Radio Array (AERA), two small arrays of radio antennas have been built and are being used at Auger. In this research program, we are investigating in more detail the physics processes leading to radio emission at the highest energies, where we take advantage of the data which are available from the other detector systems at the Observatory. Our results lead to the development of new hardware and software which will be used for AERA.

Non-SM Higgs @Tevatron

Jon Hays Imperial College

presented by: Hays Jon email-, phone-, fax-

Observation of Single Top Quark Production at the Tevatron

Ann Heinson, for the DZero and CDF Collaborations UC Riverside

presented by: Heinson Ann email-ann.heinson@ucr.edu, phone-951-827-5712, fax-951-827-3345

I will present the results of searches for electroweak production of single top quarks by the DZero and CDF collaborations at the Fermilab Tevatron proton-antiproton Collider. Both experiments announced first observation of this process in March 2009 with 5.0 standard deviation significance. Two event signatures are used: an isolated electron or muon, missing transverse energy, and jets, or just missing transverse energy and jets. One or two of the jets must be identified as originating from the decay of a B hadron. The measurements are particularly difficult as the signal:background ratios are about 1:20, and sophisticated multivariate pattern recognition tools are applied to separate the signal from the background.

Dark Matter on the Earth as a Window to the Universe

Mikhail Ja. Ivanov Central Institute of Aviation Motors

presented by: Ivanov M.Ja. email-ivanov@ciam.ru, phone-007-495-362-13-86, fax-007-495-362-38-59

Using subbaryonic gaseous Dark Matter approach a new mechanical simulation of atomic and molecule structures has been proposed. The structure of polarized spaces of electrons and protons has been analyzed. Equation, which describes the electric potential distribution in polarized space, is provided. This equation has been solved for cases of electron and proton polarized space. The simulation methods allow to take into account the thermal expansion of van der Waals spheres, the properties of valence linkages as well as spiral molecule structures. Paper contains typical examples, such as hydrocarbons, fullerenes, metalcarbons and so on. New nature of some valence linkages has been demonstrated. On base of this approach some exact solutions for gamma-ray bursts, cosmic jets and black holes are described as typical elements of "Window to the Universe".

Multi-messenger astronomy with Cen A

M. Kachelriess, S. Ostapchenko, R. Tomas NTNU, Trondheim, Norway U Hamburg, Germany

presented by: Kachelriess Michael email-Michael.Kachelriess@ntnu.no, phone-, fax-

Both the FERMI and the H.E.S.S. collaboration have announced recently the detection of the nearest active galactic nucleus, Centaurus A (Cen A). Moreover, the Auger collaboration detected two UHECR events with arrival directions coincident with the position of Cen A. We up-dated our model that predicted successfully the spectral flux of high-energy photons measured by H.E.S.S. and FERMI, and derive restrictions on the source conditions and the acceleration mechanism in Cen A.

Doubly coexisting dark matter candidates and low scale leptogenesis

Sin Kyu Kang (a), H. Sung Cheon (b), C. S. Kim (b) School of Liberal Arts, Seoul National University of Technology (a); Department of Physics, Yonsei University (b)

presented by: Kang Sin Kyu email-skkang@snut.ac.kr, phone-+82-2-970-6277, fax-+82-2978-0573

We examine how a scenario of coexisting two-particle dark mater can be realized in the extended seesaw model, which we have proposed previously to accommodate small neutrino masses and low scale leptogenesis. In this scenario, we now impose the discrete symmetry Z2 ×Z2¢ and introduce new interaction terms with dimension 5 so as for singlet Majorana neutrino S and singlet scalar F to be doubly coexisting dark matter candidates. Depending on the mass spectrum of the two dark matter candidates, the annihilation process either SS® FF or FF® SS is of particular interest because the annihilation cross sections for the processes can be so large that the relic abundance of decaying particle should get lowered, which in turn makes the constraints on its parameter space relaxed, compared with the case of one and only one dark matter candidate. We discuss the implications of the dark matter detection through the sca! ttering off the nucleus of the detecting material on our scenarios for dark matter candidates. We also study the implications for the search of invisible Higgs decay at LHC, which may serve as a probe of our scenario for dark matter

Jean Kaplan, for the QUBIC collaboration

QUBIC collaboration France, Italy, UK, Ireland

presented by: Kaplan Jean email-kaplan@apc.univ-paris7.fr, phone-+33 1 57 27 69 24, fax-+33 1 57 27 60 71

One of the main challenges of B modes detection is the treatment of systematic errors. Comparison of observations subject to different systematics is crucial. Interferometers offer such an alternative to imagers. However, to obtain the required sensitivity, a very large number of baselines is needed, which is extremely difficult to achieve with heterodyne interferometry. Bolometric interferometry copes with this problem using new technics: the interference pattern produced by a few hundred horns is imaged on a bolometer array, and a time modulation of phase shifts insures the separation of visibilities while coherently adding redundant ones. QUBIC, a merging of the US and European collaborations MBI and BRAIN, intends to deploy an interferometer in 2011-12.

Searches for the Non-SUSY at the LHC

Malgorzata Kazana for the ATLAS and CMS collaboration Soltan Institute for Nuclear Studies, Warsaw, Poland

presented by: Malgorzata Kazana email-malgorzata.kazana@cern.ch, phone-+, fax-+

One of the main goals of experiments being installed at the proton-proton Large Hadron Collider (LHC) is a search for signals of new physics in the TeV mass range. Beyond widely studied supersymmetric extensions (SUSY) of the Standard Model alternative models such as Extra Dimensions, Split SUSY or Hidden Valley provide reliable description of particle interactions at high energies and predict new, challenging signatures like high momentum resonances, heavy stable or late decaying massive particles at energies accessible at LHC. The discovery potential of ATLAS (A Toroidal LHC ApparatuS) and CMS(Compact Muon Solenoid) experiments for Non-SUSY searches, based on the full detector simulation and reconstruction with detailed triggering and systematic studies at ÖS= 10 and 14 TeV is presented.

Extensive air showers window on the Universe

J. Kempa Warsaw University of Technology Off-Campus Plock

presented by: Kempa J. email-kempa@pw.plock.pl, phone-0048 24 367 43 96, fax-0048 24 262 64 91

Energy spectrum of cosmic nuclei from the Universe for energies higher than 1 PeV and 1 EeV are still obtained only by extensive air showers technics. In this paper the log-normal distribution as the error function has been used in convolution with the power law spectrum to explain the KASCADE data above the 'knee' and AUGER and Yakutsk data above the EeV energy range. We will argue that the primary energy spectrum of cosmic ray nuclei is overestimated in the energy above 1 PeV up to the highest energies.

A Possible TeV Window on the Universe

Mihail Chizhov, Daniela Kirilova Sofia University and Institute of Astronomy, Bulgarian Academy of Sciences

presented by: Daniela Petrova Kirilova email-mih@phys.uni-sofia.bg, dani_ adm@astro.bas.bg, phone-+359 2 886 831138 , fax-

An extended electroweak model with additional spin-one chiral particles is described. The unusual characteristics of the chiral particles, their experimental constraints and the possibility for their detection at LHC are discussed. Though at low energies they generate centi-weak effective interactions, at high energies they may present a TeV window on the Universe.

Constraining the Dark 2HDM

Maria Krawczyk Institute of Theoretical Physics, University of Warsaw; Hoza 69, 00-681 Warsaw, Poland

presented by: Krawczyk Maria email-krawczyk@fuw.edu.pl, phone-+48 22 55 32 309, fax-+48 22 55 32 373

The Two Higgs Doublet Model with an Z2 symmetry conserved both explicitly and spontaneously, called the Dark 2HDM, contains the SM-like Higgs scalar h and dark scalars DH,DH+,DH-,DA. The lightest dark scalar is a dark matter candidate. The comparison will be presented of such model and the standard 2HDM with an explicit Z2 symmetry. A possible signal of dark scalars at LHC will be discussed.

The ANTARES Underwater Neutrino Telescope

Robert Lahmann for the ANTARES Collaboration University of Erlangen-Nuremberg Erlangen Centre for Astroparticle Physics (ECAP)

presented by: Lahmann Robert email-lahmann@physik.uni-erlangen.de, phone-+49 9131 8527147, fax-+49 9131 8528774

The ANTARES neutrino telescope is located in the Mediterranean Sea, 40 km south of Toulon, at a depth of about 2500 m. It comprises 12 vertical structures, the detection lines, each one equipped with photomultipliers to detect Cherenkov light emitted from the charged particles produced in neutrino interactions. Data taking with the first detection line started in March 2006 and in May 2008 ANTARES was completed. The performance of the detector will be discussed. Physics results from intermediate 5-line and 10-line configurations of ANTARES will be presented, amongst them first results on point source searches. An outlook on the expected physics sensitivity of the complete 12-line detector will conclude the presentation.

The precise timing of millisecond pulsars as a tool for the search of intermediate mass black holes in globular clusters

Tatiana Larchenkova Astro Space Center of P.N.Lebedev Physical Institute

presented by: Larchenkova Tatiana email-tanya@lukash.asc.rssi.ru, phone-+7(495)3333366, fax-+7(495)3332378

We consider the possibility of the detection of intermediate mass black holes (IMBH, 103-104 MSun), whose presence in centers of some globular clusters is assumed from optical and infrared observations, using the precise timing of pulse arrival times of known millisecond pulsars in globular clusters. For several of them, located mostly close to centers of clusters, the expected time delays of their radiation in the gravitational filed of the central black hole are calculated. It is shown that the detection of such a delay by current instruments is it impossible for the mass of the black hole of 103 MSun and quite problematically for the mass of 104 MSun. We also considered the influence of the delay on changes of pulse period and its first derivative and shown that it will be negligible in a comparison with the current accuracy of their measurements. Nevertheless, in a future, with the progress in the observational instruments and technique, this method can become one of a few direct observations of IMBHs.

Study of the Galaxy structure and detection of the invisible matter with use of the millisecond pulsars timing

Tatiana Larchenkova, Alexander Lutovinov Astro Space Center P.N.Lebedev Physical Institute

presented by: Tatiana Larchenkova email-tanya@lukash.asc.rssi.ru, phone-+7(495)3333366, fax-+7(495)3332378

For pulsars in globular clusters, we suggest using observations of the relativistic time delay of their radiation in the gravitational field of a massive body located close to the line of sight to study the distribution of both visible and dark matter in globular clusters and various components of the Galaxy. We have derived the dependences of the event probability on the structure of globular clusters and on the Galactic latitude and longitude of sources and have estimated the rates of such events. We have determined the number of objects near the line of sight toward the pulsar that can produce a modulation of its pulse arrival times characteristic of the effect under consideration; the population of brown dwarfs in the Galactic disk, whose concentration is comparable to that of the disk stars, has been taken into account for the first time. Using the timing of known millisecond pulsars in globular clusters we consider also the possibility of the detection of intermediate mass black holes (IMBH, 103 - 104 MSun), whose presence in centers of some globular clusters is assumed from optical and infrared observations.

KM3NeT: Status and its Potential for discoveries.

Dimitris Lenis Institute of Nuclear Physics, NCSR "Demokritos"

presented by: Lenis Dimitris email-lenis@inp.demokritos.gr, phone-+302106503514, fax-

KM3NeT will be a cubic kilometer–sized European neutrino telescope to be deployed in a deep location of the Mediterranean Sea. We will discuss its main physics goals, as well as some of the technical aspects and possible layouts and sites. We will also describe the potential of the KM3NeT in the search for point sources of high energy neutrinos in the sky (supernova explosions, AGN's, GRB's) and the detection of diffuse cosmic neutrino flux. The possibility of discovery of dark matter signatures and exotic particles present in cosmic radiation will also be considered. The expected sensitivity of KM3NeT for such searches will be compared with the existing flux limits.

Searches for Gravitational Waves Bursts in the first common run between LIGO, GEO600, and Virgo

Nicolas Leroy for LSC and Virgo collaborations Laboratoire de l'Accelerateur Lineaire - IN2P3/CNRS

presented by: Leroy Nicolas email-leroy@lal.in2p3.fr, phone-+33164468373, fax-

Gravitational wave burst analysis targets short (< 1sec), generic or poorly modeled gravitational-wave events. Such events could be emitted from a wide range of sources like core-collapse of massive stars, neutron stars excitations, black-hole mergers or gamma-ray bursts. We present the status of the first joint searches for gravitational-wave bursts in data from the global network of LIGO, GEO600, and Virgo interferometers.

Charm and beauty of HERA

Katerina Lipka for H1 and ZEUS Collaborations DESY Hamburg

presented by: Katerina Lipka email-katerina.lipka@desy.de, phone-+494089981882, fax-

Recent results on charm and beauty production in ep scattering at HERA are presented. Different methods of charm and beauty tagging are discussed. Measurements of the charm fragmentation function and D-meson cross sections in deep inelastic scattering and photoproduction are shown. The extracted charm and beauty contributions, F2c[`c] and F2b[`b], to the inclusive proton structure function F2 in deep inelastic ep scattering at H1 and ZEUS experiments are compared to the perturbative QCD calculations.

Radiative n decay in dense matter

A.Lokhov Moscow State University, Department of Quantum Statistics and Quantum Field Theory

presented by: Lokhov A. email-lokhov.alex@gmail.com, phone-+79262488743, fax-

The process of n radiative decay ni®nj+g in the presence of dense matter is calculated within the method of exact solutions of quantum equations. The method implies that the neutrino wave functions are the solutions of the corresponding effective Dirac equation that exactly accounts for the effects of matter. The obtained rate of the process is analyzed for different values of the background matter density. Applications to astrophysics are discussed.

New insight into Gamma-ray Blazars from the Fermi-LAT

Lott Benoit on behalf of the Fermi collaboration CENBG, CNRS/IN2P3 Université de Bordeaux, France

presented by: Lott Benoit email-lott@cenbg.in2p3.fr, phone-33-0557120890, fax-33-0557120777

Thanks to its unprecedented sensitivity, large field of view and sky survey operating mode, the Fermi Gamma-ray Space Telescope is opening a new era in extragalactic gamma-ray astronomy. In the first months of science operations the Fermi/LAT has already detected more than one hundred gamma-ray sources located away from the galactic plane ( - b - >10), which can confidently be associated with known AGNs. Most of them are blazars not previously detected at GeV energies. In this contribution we review the gamma-ray properties of these sources, their Log N - Log S distribution, and the resulting luminosity function.

X-ray pulsars: a view from current cosmic observatories

Lutovinov Alexander, Tsygankov Sergei Space Research Institute (IKI) Max-Plank Institute for Astrophysics

presented by: Lutovinov Alexander email-aal@iki.rssi.ru, phone-+7(495)3332222, fax-+7(495)3335377

Results of spectral and timing analysis of bright X-ray pulsars obtained in hard X-rays are reviewed. The main attention was dedicated to the study of cyclotron lines and changes of the pulse profile and pulse fraction with the energy and luminosity. For the first time we succeeded a detailed analysis of the cyclotron line energy dependence on the luminosity. We found that for some pulsars it is near linear according to the accretion column theory, but for other one (e.g. 4U0115+63) the picture is much more complicated, but stable and, seemly, reflects fundamental properties of the source. We also searched the connection of the pulse profile and pulse fraction changes with spectral properties of the sources, particularly, with the position of the cyclotron absorption line. A strong dependence of the pulse fraction on the energy and source luminosity was revealed and studied in detail for the first time. The prominent feature in the dependence of the pulse fraction on the energy was discovered near the cyclotron frequency for several bright sources. The obtained results are discussed in terms of current models; some preliminary explanations are proposed.

The cosmology dependence of weak lensing cluster counts

Laura Marian, Robert E. Smith, Gary M. Bernstein Argelander Institute for Astronomy, Institute for Theoretical Physics of the University of Zuerich, University of Pennsylvania

presented by: Marian Laura email-lmarian@astro.uni-bonn.de, phone-49228736788, fax-

We present the main results of a numerical study of weak lensing cluster counting. We examine the scaling with cosmology of the projected-density-peak mass function. Our main conclusion is that the projected-peak and the 3-dimensional mass functions scale with cosmology in an astonishingly close way. This means that, despite being derived from a 2-dimensional field, the weak lensing cluster abundance can be used to constrain cosmology in the same way as the 3-dimensional mass function probed by other types of surveys.

What is the origin of ultra-high energy cosmic rays?

A. Meli(1), J. K. Becker(2), J. J. Quenby(3) (1) Erlangen Center for Astroparticle Physics, University Erlangen-Nuremberg, Germany (2) Institution for Fysik, Goteborgs University, Sweden (3) Blackett Laboratory, Imperial College London, UK

presented by: Meli Athina email-athina.meli@physik.uni-erlangen.de, phone-+4915777754059, fax-

The origin of ultra high energy cosmic rays and their acceleration mechanism is a favourable subject in astroparticle physics. We review the shock acceleration mechanism, focusing on numerical studies concerning proton acceleration efficiency by subluminal and superluminal shocks, in sources such as Active Galactic Nuclei and Gamma Ray Bursts. A diffuse cosmic ray prediction model is presented, and results are compared with the measured flux of cosmic rays at the highest energies. It is shown that while steeper Active Galactic Nuclei spectra provide an excellent fit, Gamma Ray Burst spectra being flatter, can hardly explain the highest energy observed flux. Our model explains well the first evidence of a correlation between the cosmic ray flux above 5.7 x 1010 GeV and the distribution of Active Galactic Nuclei provided by the AUGER experiment. One the other hand, Gamma Ray Bursts seem not to account for the origin of the highest cosmic ray energies, nevertheless, neutrino production is expected in these sources either in mildly or highly relativistic shocks, with further consequences on our understanding by the effects of the superluminal shock acceleration.

On cosmic ray positrons and electrons

Biermann, P. L.(1), Becker, J. K.(2), Meli, A.(3), Rhode, W.(4), Seo, E.(5), Stanev, T.(6) (1) Max Planck Institute for Radioastronomy, Bonn, Germany (2) Institution for Fysik, Goteborgs University, Sweden (3) Erlangen Center for Astroparticle Physics, University of Erlangen-Nuremberg, Germany (4) Department of Physics, University of Dortmund, Germany (5) Department of Physics, Univ. of Maryland, College Park, MD, USA (6) Bartol Research Institute, University of Delaware, Newark, DE, USA

presented by: Meli Athina email-athina.meli@physik.uni-erlangen.de, phone-004915777754059, fax-

We show that the recently discovered cosmic ray electron and cosmic ray positron excess components are attributed to the acceleration in the supernova caused shock in the polar cap of exploding Wolf Rayet and Red Super Giant stars. Considering a spherical surface at some radius around such a star, the magnetic field is radial in the polar cap as opposed to most of 4 p, where the magnetic field is nearly tangential (Parker 1958). This difference yields a flatter spectrum, and also an enhanced positron injection for the cosmic rays accelerated in the polar cap. This reasoning naturally explains the observations. Precise spectral measurements will be the test, as this predicts a simple E-2 spectrum for the new components in the source, steepened to E-3 in observations (Kardashev 1962). Propagation effects such as trapping and bunching can explain smaller wiggles in the spectrum.

Active Galactic Nuclei and their Starved Cosmic Ray Spectra

Meli, A. (1), Biermann, P. L.(2) (1) Erlangen Center for Astroparticle Physics, University of Erlangen-Nuremberg, Germany (2) Max Planck Institute for Radioastronomy, Bonn, Germany

presented by: Meli Athina email-athina.meli@physik.uni-erlangen.de, phone-004915777754059, fax-

It is essential to understand the cosmic ray physics in terms of shock acceleration in relativistic astrophysical environments. One well known astrophysical application is the process of 'Comptonization' in the disks of accreting compact objects (e.g. Katz 1976). Since these spectra evolve by the Compton scattering of a number of subthermal photons in a hot gas of finite optical depth, we draw here an analogy to cosmic ray spectra, by applying numerical solutions for the AGN jet-conical shock acceleration scenario. We show that the acquired maximum energy allowed by an one-shot low energy injection of particles in a relativistic oblique shock, followed by a second oblique relativistic shock acceleration phase, is a straightforward mechanism in achieving efficiently high cosmic ray values in terms of flux and energy. In an 'one-shot double-step' oblique shock acceleration, the first shock establishes a power-law spectrum and the second one pushes the same spectrum up in energy, consequently leaving a deficiency at low energies, but confering efficiency for very high energy cosmic rays.

Neutrino flux predictions for TeV gamma-ray sources

A. Meli, Jung, I., Kappes, A. Erlangen Center for Astroparticle Physics, University of Erlangen-Nuremberg, Germany

presented by: Meli Athina email-athina.meli@physik.uni-erlangen.de, phone-004915777754059, fax-

The TeV gamma-ray radiation observed from extragalactic sources, challenges our understanding of the physical processes in the relativistic jets of these objects. In this contribution we discuss the application of a hadronic relativistic shock acceleration model applied in AGN environments. Together with the measured TeV gamma ray spectra we derive the expected neutrino fluxes from these sources and discuss their detectability in current and future neutrino telescopes.

Testing Gravity in the Laboratory

Meyer, Hinrich University of Wuppertal

presented by: Meyer Hinrich email-Hinrich.Meyer@desy.de, phone-49-40-89983776, fax-

A laboratory experiment to test the Gravitational Law at very low accelerations will be presented. It is based on determining the resonance frequency of a cavity at 21 GHz to very high precision. The reso.-frequency of the cavity is being changed by an external mass being periodically moved close and far. Recent results from this experiment will be shown.

Future Experiments on Leptonic CP Violation

Mauro Mezzetto INFN

presented by: Mezzetto M. email-mezzetto@pd.infn.it, phone-+39 049 8277147, fax-+39 049 8277145

The ultimate goal of neutrino oscillation experiments is the discovery of leptonic CP violation. This will require accelerator neutrino beams of unprecedent performances and gigantic neutrino detectors. The developments of new concepts of neutrino beams: super-beams, beta-beams and neutrino-factories, developments of neutrino detector designs and the expected performances of the facilities will be presented in the talk.

Geometry of Coronal Mass Ejections in context to recent solar cycle

Rajesh K. Mishra and Rekha Agarwal Computer and I.T. Section, Tropical Forest Research Institute, P.O.: RFRC, Mandla Road, Jabalpur (M.P.) India 482 021 and Department of Physics, Govt. Model Science College (Autonomous), Jabalpur (M.P.) 482 001, India

presented by: Mishra Rajesh Kumar email-rkm_ 30@ yahoo.com, phone-917612601225, fax-917612840484

Coronal Mass Ejections disrupt the flow of the solar wind and produce disturbances that strike the Earth with sometimes catastrophic results. Coronal mass ejections are often associated with solar flares and prominence eruptions but they can also occur in the absence of either of these processes. The frequency of CMEs varies with the sunspot cycle. At solar minimum we observe about one CME a week. Near solar maximum we observe an average of 2 to 3 CMEs per day. We have studied different characteristics of coronal mass ejection based on the observation form Large Angel and Spectrometric Coronagraph (LASCO) on board of the Solar and Heliospheric Observatory (SOHO) space craft during the period 1996 –2006. It is note worthy that the rate of occurrence of Class B CMEs is more than class A CME's. The occurrence spectrum of both classes of CMEs follows the trend of the phase of solar cycle and maximum number both types CME's seems to be occurred during maximum solar activity. It i! s also observed that the maximum number of class A, Class B CMEs have speed range 0-500 km/sec. We have observed that maximum number of Class A, Class B CME's occurred in apparent angular width range 00-900. It is also found that the maximum number of class A and class B CME's have occurred when the position angle ranges in 50-1000 and 2500-3000 respectively

Influence of solar eclipses on cosmic ray intensity variations at the Earth's surface

Rajesh K. Mishra1, Rekha Agarwal2  1 Computer and IT Section, Tropical Forest Research Institute, P.O.: RFRC, Mandla Road, Jabalpur (M.P.) 482 021, India 2Department of Physics, Govt. Model Science College (Autonomous), Jabalpur (M.P.) 482 001, India

presented by: Dr. Rajesh K. Mishra email-rm_ jbp@yahoo.co.in, rkm_ 30@yahoo.com , phone-, fax-917612601225

Cosmic ray intensity variation and its dependence on various solar parameters are important for understanding the interplanetary medium. Cosmic ray primaries observed in the interplanetary medium have galactic and extragalactic origins. The intensity of these particles is found to vary inversely with the intensity of solar wind. Solar effect on primary cosmic rays is visible through solar modulation. However, the solar modulation of secondary cosmic rays from the Earth is well understood in terms of 11-/ 22 year variation, diurnal and 27-day variation. Solar modulation of secondary cosmic rays is also observed during a total solar eclipse, which may be considered as different effect. The results of the investigation of the cosmic ray ground based neutron monitor intensity variations during solar eclipses are reported. The characteristics of different solar and heliospheric parameters during these solar eclipses are also presented. An increase in the cosmic ray neutron monito! r intensity from the Earth is evident. We suggest that such observations may reveal the impact of cosmic ray intensities on the climate.

Dipolar Dark Matter

Eduard Masso, Subhendra Mohanty and Soumya Rao Grup de Física Teòrica and Institut de Física d'Altes Energies
Universitat Autonoma de Barcelona, 08193 Bellaterra . Physical Research Laboratory, Ahmedabad 380009, India

presented by: Mohanty Subhendra email-mohanty@prl.ernet.in, phone-, fax-

If dark matter (DM) has non-zero direct or transition, electric or magnetic dipole moment then they can scatter nucleons electromagnetically in direct detection experiments. Using the results from experiments like XENON, CDMS, DAMA and COGENT we put bounds on the electric and magnetic dipole moments of DM. If DM consists of Majorana fermions then they can have only non-zero transition moments between different mass eigenstates. We find that Majorana fermions with mass mc > 38 GeV and mass splitting of the order of (50-200) keV can explain the DAMA signal and the null observations from other experiments and in addition give the observed relic density of DM by dipole-mediated annihilation.

New results on high energy cosmic ray electrons from Fermi LAT and their implications on the existence of nearby cosmic ray sources

Alexander Moiseev, on behalf of the Fermi LAT Collaboration CRESST/NASA Goddard Space Flight Center and University of Maryland

presented by: Moiseev Alexander email-alexander.a.moiseev@nasa.gov, phone-01-301-286-5581, fax-

The Fermi Large Area Telescope (LAT) has been collecting routine science data since August 2008. An important science goal is the measurement and interpretation of the high-energy cosmic-ray electron (CRE) spectrum. Due to low mass and rapid energy losses, CREs can reveal the information about nearby sources of cosmic rays and galactic magnetic field structure, as well to contribute to the understanding of astrophysical dark matter. In this talk I present our high statistics measurement of the CRE spectrum from 20 GeV to around 1 TeV. I also present the interpretation of our result in terms of a standard cosmic-ray propagation model and astrophysical sources for high energy electrons, as well as physics beyond the standard model

Heavy Flavors @Belle and BaBar

Gautier Hamel de Monchenault Saclay

presented by: Monchenault Gautier Hamel de email-, phone-, fax-

Coalescing black hole binaries. Bridging the gap between analytical (effective one-body) models and numerical relativity simulations

Thibault Damour, Alessandro Nagar Institut des Hautes Etudes Scientifiques

presented by: Nagar Alessandro email-nagar@ihes.fr, phone-+33160926657, fax-+33150926669

Coalescing black hole binaries are expected to be among the most promising sources for currently operating ground-based gravitational wave detectors like LIGO/GEO/Virgo. Recent advances in the numerical methods to simulate black hole systems in general relativity have for the first time allowed simulations of complete orbits of two black holes. This opens the possibility to study black hole systems during the most dynamic, non-linear phase of their inspiral,collision, and merger, as well as to provide crucial information (i.e. template waveforms) needed for gravitational wave detection. However, due to the computational cost of each simulation, it is unlikely that Numerical Relativity is able to densely cover the full parameter space. To this aim, one must devise analytical methods to accurately compute waveforms. The Effective-One-Body (EOB) approach to the general relativistic two-body dynamics has proven effective in modeling analytically the full coalescence process (i.e! ., inspiral, plunge, merger and ringdown) and has succeeded in bridging the gap between numerical and analytical knowledge. I will review the state of the art and present the most recent results about how the EOB analytical knowledge can be completed by extracting crucial non-perturbative information out of accurate numerical data. This will show that the EOB formalism is a very promising route to provide accurate representations of general relativistic waveforms which are needed by gravitational wave detectors.

Properties of the Molière simultaneous distribution between the deflection angle and the lateral displacement

Takao Nakatsuka and Kazuhide Okeia Okayama Shoka University, Japan
fDept. of Info. Sciences, Kawasaki Medical School, Japan

presented by: Nakatsuka Takao email-nakatuka@osu.ac.jp, phone-+81-86-252-0642, fax-+81-86-255-6947

Molière simultaneous distribution between the deflection angle qy and the lateral displacement y are investigated analytically. The simultaneous distribution is expressed by power series of B-1 with coefficients of universal functions with the measure of qM, where B and qM are the same expansion parameter and the scale angle as derived for the Molière angular distribution. Central regions of the simultaneous distribution are well explained by the Fermi simultaneous distribution with the scale angle of qM irrespective of B, and peripheral regions of the distribution are explained asymptotically by the single-scattering and the double-scattering.

Ultra-high energy neutrino limits from the Pierre Auger Observatory

Sergio Navas for the Pierre Auger Collaboration University of Granada

presented by: Sergio Navas email-navas@ugr.es, phone-+00 34 958244152, fax-+00 34 958 248529

The Pierre Auger Observatory has the capability of detecting ultra-high energy neutrinos (UHEnu) of all flavours. They interact through charged and neutral currents in the atmosphere (down going) and through the Ëarth-skimming" mechanism (up-going). The main challenge in detecting UHEnu with Auger is to identify a neutrino-induced shower in the overwhelming background of showers initiated by ultra-high energy cosmic rays (UHECR), possibly protons, heavy nuclei or even photons. While these backgrounds interact shortly after entering the atmosphere, neutrinos can generate deep showers, so the method adopted is to search for "very inclined young showers". At ground level, neutrino events would have a significant electromagnetic component leading to a broad time structure of detected signals in the water-Cherenkov detectors, in contrast to nucleonic-induced showers. Using data collected from Jan 04 to Feb 09, we present the analyses based on down-going neutrinos and on up-going tau neutrinos. We also present the observables that are used to identify neutrino candidates and place the corresponding limits on the all-flavour diffuse neutrino fluxes. Finally, we discuss sources of possible backgrounds and systematic uncertainties.

Dual Superconformal Symmetry, Scattering Amplitudes and Wilson Loops

Dung Nguyen, Marcus Spradlin Brown University

presented by: Nguyen Dung email-dung_ nguyen@brown.edu, phone-(1) 401-378-2620, fax-(1) 401-863-2024

In this talk, we will discuss about some fundamental processes: gluon and graviton scattering amplitudes in N=4 Super Yang-Mills and N=8 Super Gravity theories respectively. We will give a brief review of the new dual superconformal symmetry of the scattering amplitude, that leads to simplified structures and a way to calculate the amplitude at higher loop level. Then we will discuss about the calculation of the four-side light-like Wilson loops at two loops to all order in e. At strong coupling, it's been shown that there is a duality between the scattering amplitude and the Wilson loops. At weak coupling, it has been checked for several cases, but our result at two loops indicates this subject should be studied more carefully in the future. Lastly, we will discuss about twistor theory for gravity and give results of some graviton scattering amplitudes in the Link representation.

Cosmic Background Radiation Studiess from the South Pole, Antarctica - recent results from the BICEP experiment and the plan for the next generation instrument

Hien Nguyen JPL, CALTEC

presented by: Nguyen Hien email-htnguyen@jpl.nasa.gov, phone-, fax-

We briefly review the historical development of the observations of CMB from the South Pole, Antarctica, from the late 1980s to the beginning of the millennium, with the present day BICEP experiment. We give a description of the BICEP experiment and its recent result. We also present the plan for BICEP2 and the Keck array, a multi frequency upgrade for the BICEP receivers with faster mapping speed.

Radio Detection of Ultra High Energy Cosmic Rays

Ryan Nichol UCL

presented by: Nichol Ryan email-rjn@hep.ucl.ac.uk, phone-+44 (0)207 679 7266, fax-+44 (0)207 679 7145

The detection of cosmic rays through emissions in the radio regime dates back to the 1960's. In recent years this field has undergone a revival of interest in the experimental community. In this presentation, the radio emission mechanisms in both air and dense media will be discussed and active experiments reviewed. Future prospects for the radio detection of both charged particle and neutrino cosmic rays will be outlined.

Combined energy spectrum of the Pierre Auger Observatory

V. M. Olmos-Gilbaja for the Pierre Auger Collaboration Departamento de Física de Partículas. Universidade de Santiago de Compostela e Instituto Galego de Física de Altas Enerxías

presented by: Olmos-Gilbaja V. M. email-victor.olmos.gilbaja@gmail.com, phone-+34918563100 - 14089, fax-+34981521091

With the southern site of the Pierre Auger Observatory completed, three independent measurements of the flux of ultra high energy cosmic rays have been performed. Both measurements made with the surface detector, using events below and over 60 degrees, and the measurement of the spectrum using hybrid events have been combined to obtain an only measurement of the cosmic ray flux. A flux suppression at the highest energies with a 6 sigma significance has been reported and an extension of the energy spectrum to lower energies where the efficiency of the surface detector is less than 100% has been obtained.

Probing q13 with global neutrino data analysis

G.L. Fogli, E. Lisi, A. Marrone, A. Palazzo, A.M. Rotunno University of Bari, INFN, Bari, CSIC/IFIC-University of Valencia,

presented by: Palazzo Antonio email-antonio.palazzo@ific.uv.es, phone-(+34) 963543515, fax-(+34) 963543488

Pinning down the unknown neutrino mixing angle q13 is one of the most important goals in particle physics in connection with future investigation on CP violation in the leptonic sector. In this context, I shall present the results of an updated global analysis of neutrino oscillation data, focusing on this puzzling parameter. I shall discuss three independent converging hints of q13 > 0. An first one coming from atmospheric neutrino data, a second one coming from the combination of solar and long-baseline reactor neutrino data, and a third one coming from the latest MINOS results in the electron neutrino appearance channel. Their combination provides an intriguing preference for q13 > 0 at the non-negligible statistical significance of 2 sigma (95

Linear Gravity in de Sitter Universe and Power Spectrum in Krein Space Quantization

Farrin Payandeh Payame Noor University, Tehran, Iran

presented by: Payandeh Farrin email-farrin_ payandeh@yahoo.com, phone-0098 9143045267, fax-0098 411 4788506

It has been shown that the negative-norm states or negative-frequency solutions of the field equation are indispensable for a fully covariant quantization (Krein space quantization) of the minimally coupled free scalar field in de Sitter spacetime. The new method of quantization has been applied for the free boson and spinor fields in Minkowski spacetime, and the basic structure of quantum field theory is reformulated in Krein space. The power spectrum of scalar field and spacetime metric perturbations produced in the process of inflation of universe could be calculated by Krein space approach to field quantization, utilizing auxiliary negative frequency states. It is seen that the presence of unphysical negative-frequency states plays the role of an automatic renormalization tool for the theory.

The physics of electroweak-scale non-sterile right-handed neutrinos

Pham Quang Hung University of Virginia Charlottesville, Virginia 22904-4714

presented by: Pham Quang Hung email-pqh@virginia.edu, phone-1-434-924-6819, fax-1-434-924-4576

A model of electroweak non-singlet nR's with mass MZ/2 < mnR < 246 GeV and with implications concerning their production and detection at the LHC will be presented. Lepton-number violating processes such as like-sign dileptons and decays with displaced vertices are characteristic signatures of the model. The construction of this electroweak-scale right-handed neutrino model necessitates the presence of a non-minimal Higgs structure in the Standard Model involving doubly-charged scalars contained in a Higgs triplet. An extension of the model also gives rise to keV sterile neutrinos which could be candidates for Warm Dark Matter with implications concerning structure formation, pulsar kicks, etc...

Status of the EXO double beta decay project

Andreas Piepke for the EXO Collaboration University of Alabama

presented by: Piepke Andreas email-andreas@bama.ua.edu, phone-205 348 6066, fax-

The experimental observation of neutrino oscillations firmly established neutrino mass and mixing. It is not yet clear whether neutrinos are their own anti-particles or not. The investigation of neutrinoless double beta decay allows exploring this question. Combined with nuclear structure calculations double beta decay constrains the absolute neutrino mass scale. EXO is a next generation double beta decay search using isotopically enriched 136Xe. Our collaboration is developing a novel approach to the detection of double beta decay, aiming at the simultaneous detection of the decay electrons and the emerging Ba ion, allowing essentially background free detection of double beta decay, should it exist. The status of the development of a prototype liquid xenon time projection chamber, utilizing 200 kg of enriched Xe, and of the ion tagging technology will be discussed.

Modeling of Ultra High Energy Cosmic Ray Interactions and Atmospheric Cascade

T. Pierog, R. Engel KIT, Karlsruhe, Germany

presented by: Pierog T. email-tanguy.pierog@ik.fzk.de, phone-+497247828134, fax-+49-7247-824075

Main observables of high energy air showers depend on the nature and energy of the primary cosmic ray particles. As a result, simulations of showers initiated by hadronic particles will have a strong dependence on the physics of hadronic interactions at energies well above the one reached even at the LHC. Using a simplified model to describe the hadronic and electromagnetic air shower development, the source of uncertainties in air shower observables can be understood. Then we will consider how realistic description of hadronic interactions and detailed simulations of air showers can be achieved with our current knowledge of particle physics and show the consequences on the interpretation of charged cosmic ray data.

Search for SUSY at the Tevatron

Aliaksandr Pranko (for CDF and D0 Collaborations) Fermilab

presented by: Pranko Aliaksandr email-pronko@fnal.gov, phone-+1-630-840-3638, fax-+1-630-840-2968

We present results of searches for signs of supersymmetry at the Tevatron. The focus of this paper is on results obtained since summer of 2008. No signs of supersymmetry are observed in 1-3 fb-1 of analyzed data. We report kinematic distributions, data and background counts, as well as exclusion limits on production cross sections of supersymmetric particles.

A tensor theory of space-time as a strained material continuum

Angelo Tartaglia, Ninfa Radicella Polytechnic of Turin and INFN section of Turin

presented by: Radicella Ninfa email-ninfa.radicella@polito.it, phone-+390115647380, fax-+390115647399

In this proposal we want to present the Cosmic Defect theory, an alternative theory of gravitation, in the cosmological setting, and then compare it with the observational data coming from SNIa.
In the pletora of alternative theories our attempt is to move from a physical start, inspired by known physics. The inspiration is from the properties of physical continua and the effects produced in them by the presence of texture defects. Actually this is an old theory for three-dimensional continua; we extend it to the four-dimensional continuum represented by space-time. In our view the initial singularity (the Big Bang) is interpreted as a defect in the space-time continuum, inducing everywhere a strained state which manifests itself as what we read as a non-uniform expansion rate of the universe.
This means that the Lagrangian that we use to describe the space-time must contain also an elastic term that accounts for the presence of defects and their consequences. This term is the elastic potential, that we explicitly use in the linear approximation, that is assuming Hooke law to relate stress smn and strain emn by means of the elastic coefficients: We=[1/2]smnemn = [1/2]Cmnabeabemn . The total Lagrangian is then built by adding this potential term to the Einstein-Hilbert kinetic term for the space-time, the Ricci scalar:
L= æ
R+ 1

Cmnrsemners ö


In our work we are interested in cosmological solutions so that we consider a point-defect that induces Robertson-Walker symmetry. This induces everywhere a strain that can be expressed in terms of the scale factor, the only free function we are left with if we assume such a symmetry. Moreover, the elastic coefficients Cmnab drastically simplify by assuming homogeneity and isotropy so that they reduce to two parameters, the so-called Lamé parameters, l and m.
At the end we deal with modified Einstein equations, that reduce to one evolution equation and a constraint equation, in the same way as standard General Relativity case, and the two Lamé coefficients combine to give what is called the elastic modulus: B=l+[2/3]m. Our equations reduce to Einstein equations in absence of defects (when the strain tensor is null) but show a different behaviour: there is an expansion even without matter (when the defect is present) and it seems to be accelerated, at least for a period. So we test our cosmological theory against luminosity data from Supernovae of type Ia. As usual we express our Hubble parameter in terms of the redshift, assuming matter only as dust component, and then integrate it to get the distance modulus m-M, that is what is measured:
m-M=m+5log æ
( 1+z) ó



3( z¢2-1) 2+yz¢3
We integrate with respect to the variable z = 1+z/a0 and perform a three-parameter fit, where the parameters here y, a0 and m are related to the elastic modulus B, to the present amount of matter and the present value of the scale factor a0. We have tested it by using the data of 307 SnIa's from the Superanovae Cosmology Project Union Survey and by minimising the reduced c2 . Considering the different sensitivity with respect to changes in m, which is outside the logarithm, and in a0 and y , which are in the logarithm, the optimization has been performed in two steps. In the first step the optimisation routine has been run with all three parameters giving the a value for m and a first estimate of a0 and y. In the second step m has been fixed to its already found value and the routine has been used again with the two remaining free parameters, thus yielding a far better uncertainty. The final reduced c2 of the fit is 1.017.
The best fit values for the parameters give us a0=1.97, the present amount of dust r0 ~ 3.4×10-27kg/m3 , consistent with the current estimates for barionic matter (with a very huge error, around hundred percent, because of initial errors on the measured luminosity) and the elastic modulus B=( 3±2) ×10-7 Mpc-2. We can use all of them to get the present value of the Hubble parameter and obtain H0=(64±35) [km/(s×Mpc)].

Matter parity as the origin of Dark Matter

Mario Kadastik, Kristjan Kannike, Martti Raidal National Institute For Chemical Physics and Biophysics, Estonia

presented by: Raidal Martti email-martti.raidal@cern.ch, phone-+372 5164854, fax-+372 6440640

We extend the concept of matter parity PM=(-1)3(B-L) to non-supersymmetric theories and argue that PM is the unique explanation to the existence of Dark Matter of the Universe. The argument is general but we motivate it using constraints on GUT particle content from lower-dimensional field theories. The non-supersymmetric Dark Matter must be contained in scalar 16 representation(s) of SO(10), thus the unique low energy Dark Matter candidates are PM-odd complex scalar singlet(s) S and inert scalar doublet(s) H2. We have calculated the thermal relic Dark Matter abundance of the model and shown that its minimal form may be testable at LHC via the SM Higgs boson decays H1® DM  DM. The PAMELA anomaly can be explained with the decays DM® LL induced via seesaw-like operator which is additionally suppressed by Planck scale. Because the SM fermions are odd under matter parity too, Dark Matter sector is just our scalar relative.

Characteristics of high energy cosmic rays observed with CODALEMA: Evidence for a geomagnetic radio emission mechanism.

CODALEMA Collaboration  Laboratoire SUBATECH Nantes IN2P3/CNRS, Université de Nantes, Ecole des Mines de Nantes

presented by: RAVEL Olivier email-ravel@subatech.in2p3.fr, phone-0251858459, fax-

The CODALEMA experiment detects radio transients produced by cosmic ray induced air showers. The main goal of the CODALEMA experiment is to characterize this electromagnetic signal, according to the physical parameters of the shower. The latest results of CODALEMA will be presented; in particular we will present the cosmic ray arrival direction distributions in both EW and NS polarizations. We will show that they are well described, at first order, by a radio emission assuming a linear dependence of the electric field with respect to the cross product of the shower axis with the geomagnetic field. The lateral distribution of the measured electric field will also be discussed.


Romeri Anna Curir Valentina de, Giuseppe Murante Astronomical Observatory of Torino (Italy) Department of Physics . University of Torino (Italy)

presented by: Romeri Anna Curir Anna de email-curir@oato.inaf.it, phone-003911 8101952, fax-003911 8101930

We performed numerical simulation analysing the growth of the bar instability inside stellar-gaseous disks, where the star formation is triggered, and a central black hole(BH)is present. We use N-body-SPH simulations of the same isolated disk-halo mass systems harbouring BHs of different initial masses and energy feedback on the gas. We compare these simulations with the ones of the same disk without BH in the center. We make the same comparison for a disk in a fully cosmological scenario. The BHs grow in different ways according with their initial mass and feedback efficiencies and the impact on the bar ellipticity depends on these parameters. The BH has a mild effect on the bar ellipticity but it is never able to destroy it.

Supernova physics with the SuperNova Legacy Survey (on behalf of the SNLS collaboration)

Vanina Ruhlmann-Kleider DSM/Irfu/SPP

presented by: Ruhlmann-Kleider Vanina email-ruhlmann@ccimap.in2p3.fr, phone-01 69 08 61 57, fax-01 69 08 64 28

The SuperNova Legacy Survey, in operation between 2003 and 2008 at the Canada-France-Hawaii telescope, detected about a thousand type Ia supernovae (SNIa) in the redshift range between 0.2 and 1. Around half of them were confirmed by spectroscopy and served to derive precise cosmology measurements, which is the primary goal of the survey. But the large data sample and the precision of the photometric measurements made other topics accessible. SNIa explosion rates and SN host galaxy properties were compared to better understand the physics of SNIa, such as progenitor scenarios or the effect of progenitor age and metallicity on SNIa luminosity. Besides SNIa, the large sample of SNLS data also contain core-collapse events, the rate of which was measured with great accuracy. Results on these topics, based on the first three years of the survey, will be reviewed.

CMS Commissioning and Potential Early Results

Alexei Safonov Texas A and M

presented by: Safonov Alexei email-, phone-, fax-

Results from the TA Surface Detectors

Hiroyuki Sagawa for the Telescope Array Collaboration Institute for Cosmic Ray Research, University of Tokyo

presented by: Hiroyuki Sagawa email-hsagawa@icrr.u-tokyo.ac.jp, phone-+81-4-7136-3131, fax-+81-4-7136-3131

The Telescope Array (TA) is the largest hybrid detector in the northern hemisphere, which consists of an array of Surface Detectors (SDs) and Fluorescence Detectors (FDs), to explore the origin of Ultra-High Energy (UHE) cosmic rays by measuring energy, arrival direction, mass composition, and other characteristics of UHE cosmic rays. It is located in the desert of Utah, about 200 km southwest of Salt Lake City.
The Telescope Array succeeds to the Akeno Giant Air Shower Array (AGASA) and High Resolution Fly's Eye (HiRes) experiments. The SD array consists of 507 plastic scintillator counters of 3 m2 area deployed in a square grid with 1.2 km spacing, covering about 700 km2. There are three FD stations, overlooking the SD array. To the southeast and southwest are two FD stations which have 12 new telescopes respectively. To the north is the FD station, consisting of 14 telescopes which were taken and refurbished from the HiRes. Having the HiRes telescopes allows for a direct comparison between the HiRes and TA energy scales.
Each surface detector has two layers of 1.2 cm thick scintillator. The light is gathered by wavelength shifting fibers and brought out to a PMT, one for each layer. The electronics with 50 MHz FADC are used to read out the PMTs. The surface detectors are divided into three sub-array which communicate via radios with towers where triggers are formed. The fluorescence detectors run only on clear moonless nights (10%) while the surface detectors run continuously for 24 hours ( ~ 100%). The SD measurement provides the largest statistical sample at the highest energies of any TA detector component, and it provides reasonable accuracy to measure arrival directions of UHE cosmic rays.
The Telescope Array underwent commissioning in 2007 and began routine data collection with full operation in March of 2008. The data set from the SD array corresponds to an exposure of about 60% that of the AGASA experiment. The fluorescence detectors of the three FD stations provide full hybrid coverage of the SD array above about 10 EeV. We have a real-time system that works in the background to monitor a variety of information for SD calibration and maintenance.
For the TA surface detectors, we adopted plastic scintillator which is sensitive to electromagnetic component of air showers and thus less sensitive to hadronic interaction models and mass composition of primary cosmic rays. By using a lateral shower distribution of an air shower detected with the surface detectors, we measure the local particle density at a certain distance from the shower axis. Independently of the fluorescence detectors, we measure energy of air showers from the evaluation of the conversion of the local density to primary energy by Monte Carlo simulation of air showers and the surface detectors. We confirm energy scale by comparing energies measured with the surface detectors and the fluorescence detectors by using hybrid air shower events which are detected simultaneously both with the surface detectors and the fluorescence detectors.
The Telescope Array has a variety of instrumentation to control systematic uncertainties. Here we present the performance and results from the TA surface detectors.

Looking for Anisotropies over Extended Regions of the Sky with Data from the Pierre Auger Observatory

E. M. Santos for the Pierre Auger Collaboration Instituto de Física, Universidade Federal do Rio de Janeiro, Rio de Janeiro, Brazil

presented by: Santos E. M. email-emoura@if.ufrj.br, phone-+55-21-25627727, fax-+55-25627368

We present large scale anisotropy searches with the data collected by the Pierre Auger Observatory surface detector from 1 January 2004 until 31 March 2009. Special care is devoted to systematic effects introduced by the array exposure variations. Both solar and sidereal modulations are studied as a function of the energy threshold. Upper limits at the percent level on the amplitudes of the first harmomic are imposed.

Ultrahigh energy cosmic ray anisotropy search from the High Resolution Fly's Eye

D.R. Bergman, W.F. Hanlon, H. Koers, P. Tinyakov, L.M. Scott, G.B. Thomson Rutgers University, University of Utah, Universite Libre de Bruxelles

presented by: Lauren M. Scott email-lsct@physics.rutgers.edu, phone-732-445-5500 x5032, fax-732-445-6413

The topic of correlations of ultrahigh energy cosmic rays (UHECRs) with astrophysical objects has been of recent importance with increasing statistics from the HiRes and Auger experiments. We will present our recent results with correlations of UHECRs with Active Galactic Nuclei along with our recent work involving correlations with large-scale structure.

QCD at the Tevatron

Sally Seidel, for the CDF and D0 Collaborations The University of New Mexico

presented by: Seidel Sally email-seidel@phys.unm.edu, phone-505-277-2616, fax-505-277-1520

Measurements of QCD processes recorded by the CDF and D0 Experiments at the Tevatron at center of mass energy 1.96 TeV are presented. Searches for new particles and for quark substructure are described. Cross sections for the production of one or more jets, inclusively and restricted to c-jets or b-jets, in association with weak vector bosons, are reported. Cross sections for production of photon plus jet and for inclusive production of photon plus heavy quark jet are described. The kT distribution of particles in jets is measured.

Upper limits on the cosmic-ray photon fraction from the Pierre Auger Observatory

Mariangela Settimo for the Pierre Auger Collaboration University of Salento and INFN Lecce, Italy

presented by: Settimo Mariangela email-mariangela.settimo@le.infn.it, phone-, fax-

The observation of photons with energies above 1018 eV would open a new window to the extreme universe. The Pierre Auger Observatory, designed to investigate the origin and the nature of Ultra High Energy Cosmic Rays, offers a unique opportunity to search for such photons. An overview of the search methods is given and the latest results are presented.

Particle and Cosmological Aspects of the Double Beta Decay

Fedor Simkovic JINR Dubna, Comenius University Bratislava

presented by: Simkovic Fedor email-simkovic@theor.jinr.ru, simkovic@fmph.uniba.sk, phone-7 49621 62473, 421 2 60295543, fax-7 49621 65084, 421 2 65412305

The absolute neutrino mass scale of neutrinos is discussed in the context of the neutrinoless double beta decay. Both, light neutrino and R-parity breaking SUSY mechanisms are subject of interest. A new possibility to study lepton number violation via oscillations plus deexcitations of neutral atoms is addressed. A phenomenological analysis of this process lead to a resonant enhancement of double electron capture that has a Breit-Wigner form. Finally, we show that two-neutrino double beta decay provide a sensitive test of the Pauli exclusion principle and statistics of neutrinos. Cosmological aspects of this and related processes are discussed.

Borexino: low energy solar neutrinos and beyond

O.Smirnov on behalf of the Borexino collaboration JINR, Dubna

presented by: Smirnov O. email-osmirnov@jinr.ru, phone-+7 49621 63518, fax-+7 49621 66666

The main goal of the Borexino experiment is the real-time measurement of the monoenergetic neutrino flux, originating from the electrons capture on Be-7 in the sun's core, with a precision of at least 5achieved, further improvement of the result is expected after tuning of the events reconstruction code using the data from recent calibration campaign.
Due to the very low level of natural radioactivity achieved in Borexino, some other topics in neutrino physics and astrophysics can be addressed, including solar neutrino measurements in the energy range above compton-like edge of the Be-7 electron-recoil spectrum, and antineutrino flux measurements with practicaly no background.

Can nonlinear evolution of LSS influence CMB temperature correlations?

Smith Robert E.(1) Carlos Hernandez-Monteagudo (2) Uros Seljak (1,3) (1) Institute for Theoretical Physics, UZurich. (2) MPA, Garching (3) UC Berkely (LBNL)

presented by: Smith Robert E. email-res@physik.unizh.ch, phone-+41 446355810, fax-+41 44-635-5704

We investigate the impact of nonlinear evolution of the gravitational potentials in the LCDM model, on the Integrated Sachs-Wolfe (ISW) contribution to the CMB temperature power spectrum, and on the cross-power spectrum of the CMB and a set of biased tracers of the mass. Two lines of inquiry are pursued. First, we use of an ensemble of N-body simulations to directly follow the potentials. Second, we employ analytic perturbation theory (PT) methods. To gain a qualitative understanding, we present maps of the time rate of change of potentials at various stages in the simulations. At early times, small scale nonlinear effects are present through the Rees-Sciama (RS) and Birkinshaw-Gull (BG) effects. At later times these are overwhelmed by the ISW. The ISW contribution to the CMB comprises three spectra: the auto-density and momentum spectra, and their cross-spectrum. We use the simulations to estimate these, and evidence for large-scale nonlinearity is present. The predicti! ons from the PT match the results to high precision for k < 0.2. We compute the nonlinear corrections to the angular power spectrum and find them to be < 10% of linear for l < 100. These corrections are swamped by the cosmic variance. On scales l > 100 the departures are more significant, however the CMB signal is more than a factor 103 larger at this scale. Nonlinear ISW, RS and BG effects therefore play no role in shaping the CMB power spectrum for l < 1500. The CMB-density tracer cross-spectrum comprises two spectra: the biased tracer-mass and -momentum cross spectra. We measure these from the simulations for group and cluster scale dark matter haloes. We use the renormalized bias PT to generate predictions, and find good agreement. For the combined cross-spectrum, and at early times, nonlinearity is manifest as a suppression of power. However, at later times, we find evidence that the signal is boosted on small scales. Analytic arguments show that this should ! happen when, Wm < 0.3. On calculation of the angular power spec trum, nonlinear corrections are found to be < 10% for l < 100, but are swamped by cosmic variance. Since the S/N for the ISW is dominated by l < 100, it is therefore highly unlikely that the detection significance can be influenced by such effects. Finally, we compute the cross-correlation coefficient and find that neglecting the time dependence of the bias leads to significant errors. For robust cosmological inferences, this must be included.

Final Results from HiRes/Status of Telescope Array

Pierre Sokolsky University of Utah, Salt Lake City, Utah

presented by: Sokolsky Pierre email-ps@physics.utah.edu, phone-801 581-3538, fax-

Final results from the HiRes atmospheric air-fluorescence experiment will be presented on the the ultra-high energy cosmic ray spectrum, composition and anisotropy. The HiRes spectrum using monocular and stereo shows clear evidence for the existence of the GZK cutoff and an ankle structure below the cut off. Comparison of cosmic ray induced shower properties with simulations indicate a light, mostly protonic composition near the GZK region, consistent with expectations. No evidence for anisotropy from AGN's is found in the Northern hemisphere sky.
The current status of the Telescope Array project, a hybrid experiment composed of a surface array of plastic scintillators and three air-fluorescence telescope stations will be presented. The initial phase of the project is complete and data taking has been proceeding for one year. Expected physics sensitivities and early information on array and telescope performance will be discussed.

The Nuclotron-based Ion Collider fAcility at the Joint Institute for Nuclear Researchh: new Prospects for Heavy Ion Collisions and Spin Physics

A.N. Sissakian, A.S. Sorin Joint Institute for Nuclear Research

presented by: Sorin A.S. email-sorin@theor.jinr.ru, phone-+7 496 21 62109, fax-+7 49621 65084

A status report on the current development of the Nuclotron-Based Ion Collider fAcility (NICA) and the MultiPurpose Particle Detector (MPD) at the Joint Institute for Nuclear Research (JINR), which gives new prospects for heavy ion collisions and spin physics, will be presented.

The composition of UHECRs studied with the fluorescence detector of the Pierre Auger Observatory

Vitor de Souza for the Pierre Auger Collaboration Instituto de Física de São Carlos - USP Observatório Pierre Auger - Argentina

presented by: Souza Vitor de email-vitor.de.souza@gmail.com, phone-55-16-33738727, fax-55-16-33738127

The Pierre Auge Observatory is operating twenty four fluorescence telescopes and 1600 water Cerenkov stations in its Southern site. The fluorescence telescopes measure the longitudinal development of the air showers and are able to determine precisely the depth (Xmax) in which the shower reaches the maximum number of particles. Since (Xmax) depends directly on the primary particle type, we study the cosmic ray composition by analysing the (Xmax) distributions. In this work, we show the evolution of the mean and fluctuations of (Xmax) as a function of energy as measured by the Auger Observatory. The data is compared to simulation predictions in order to estimate the primary cosmic ray composition.

Antimatter and dark matter search in Space with AMS-02

Francesca R. Spada for the AMS Collaboration Istituto Nazionale di Fisica Nucleare (INFN), Rome, Italy

presented by: Spada Francesca R. email-francesca.spada@roma1.infn.it, phone-+39 06 49694212, fax-+39 06 4957697

AMS-02 is a magnetic spectrometer that will operate on the International Space Station. It is designed to measure with very high accuracy the composition of Cosmic Rays near Earth. With a large acceptance (5000 squared cm), an intense magnetic field from a superconducting magnet (0.7 T) and a very efficient particle identification, AMS-02 will provide the highest precision in Cosmic Rays measurements up to the TeV region. In three years, AMS-02 will achieve a sensitivity to the existence of anti-Helium nuclei in the Cosmic Rays of one part in a billion, and provide important information on the nature of Dark Matter. The detector is now being integrated and will soon be ready for launch: we review the status and the discover capabilities.

Radiation reaction and motion of stars around black holes

Alessandro Spallicci, Sofiane Aoudia Université d'Orléans LPC2E - OSUC

presented by: Spallicci Alessandro email-spallicci@cnrs-orleans.fr, phone-0623153584, fax-

The capture of stars by supermassive black holes represents one of the main targets for the LISA (ESA-NASA) space mission. The detection of the waveforms is made highly complex by the huge number of parameters and by the influence of radiation reaction. In the mid of the 90s, the MiSaTaQuWa self-force approach has allowed researchers to investigate the motion of particles around black holes. In this talk, we present current results and the implications for fundamental physics. The Blois meeting occurs the week later the Capra meeting on radiation reaction in Bloomington which occurred last year in Orléans together with a CNRS school on motion http://www.cnrs-orleans.fr/osuc/conf/.

Sources and Propagation of Ultrahigh Energy Cosmic Rays

Todor Stanev Bartol Research Institute and Department of Physics and Astronomy, University of Delaware, Newark DE 19716, U.S.A.

presented by: Todor Stanev email-stanev@bartol.udel.edu, phone-1-302-831-1495, fax-

We will discuss possible sources of the cosmic rays of energy higher than 1018 eV, including active galactic nuclei and gamma ray bursts. We will also discuss the propagation of these high energy particles in extragalactic space and the production of fluxes of secondary gamma rays and neutrinos during the propagation.

MiniBooNE Results as Related to "Windows on the Universe"

Ray Stefanski Fermilab

presented by: Stefanski Ray email-stefanski@fnal.gov, phone-630.840.3872, fax-630.840.6520

The measurement of absolute neutrino and anti-neutrino cross-sections, the observation of a "low energy anomaly" in the neutrino sector, the constraints placed on the LSND effect by a non-observation of neutrino oscillations, the search for neutrino and anti-neutrino appearance, and a for the possible existence of new heavy particles makes MiniBooNE a major contributor to our current view of the Universe. This paper will address specific model constraints set by the MiniBooNE data, and explore expectations for further remaining analysis of the data.

Electromagnetic properties of neutrino: a window to New Physics

Alexander Studenikin Department of Theoretical Physics, Moscow State University

presented by: Studenikin Alexander email-studenik@srd.sinp.msu.ru, phone-(007-495) 939-16-17, fax-(007-495) 932-88-20s

A review on neutrino electromagnetic properties is given. We start with a derivation of the neutrino electromagnetic vertex function in the most general form that follows from the requirement of Lorentz invariance, for both the Dirac and Majorana cases. The problem of the neutrino form factors definition and calculation within different gauge models is considered. In particular, the neutrino electric charge form factor and charge radius, dipole magnetic and electric and anapole form factors are discussed. A detailed analysis of the neutrino magnetic moment in the Standard Model and beyond is given. Available experimental constraints on neutrino electromagnetic properties are also reviewed, and the most important experimental limits on neutrino magnetic moments are considered. The important neutrino electromagnetic processes involving a direct neutrino coupling with photons (such as neutrino radiative decay, neutrino Cherenkov radiation, spin light of neutrino and plasmon! decay into neutrino-antineutrino pair in media) and neutrino resonant spin-flavor precession in a magnetic field, as well as their applications in astrophysics, are discussed. It is shown that studies of the neutrino electromagnetic properties can open a window to New Physics.

Cosmic Ray Studies with the OPERA detector at Gran Sasso

The OPERA Collaboration Universite' Claude Bernard Lyon-I (UCBL) Inst. : Institut de Physique Nucleaire de Lyon (IPNL) Affiliation. : UCBL-CNRS/IN2P3 Addr. : 4 rue E.Fermi, F-69622 Villeurbanne, FRANCE

presented by: Timothee Brugiere email-timothee.brugiere@ipnl.in2p3.fr, phone-+33 4 7243 1059, fax-+33 4 7244 8004

OPERA is a long-baseline neutrino experiment located in the Hall C of the Gran Sasso underground Laboratories at an average depth of 3800 hg/cm2, corresponding to muon energy at surface higher than 1.5 TeV. We present a series of studies carried on using OPERA as a cosmic ray detector. In particular, we report on the final result on the measurement of the atmospheric muon charge ratio with the magnetic spectrometers of the detector, using the data collected in parasitic way during the 2008 CNGS Physics Run. We also report on the analysis of upgoing muons induced by atmospheric neutrinos.

CUORE and CUORICINO Cryogenic Double Beta Decay Experiments

Claudia Tomei for the CUORE Collaboration Laboratori Nazionali del Gran Sasso (INFN) and INFN Sezione di Roma1

presented by: Tomei Claudia email-claudia.tomei@lngs.infn.it, phone-, fax-

Cryogenic bolometers are excellent detectors for the search of neutrinoless double beta decay. The CUORICINO experiment, operating underground at LNGS, has searched for the 0nbb decay of 130Te with an array of such bolometers and has set the most stringent limits on its half-life. Cuoricino was also a prototype for a next generation experiment, CUORE. The expected sensitivity, based on Monte Carlo simulations and extrapolations of the Cuoricino results, indicate that CUORE will be able to test the 0.02-0.05 eV region for the effective neutrino mass, with a high discovery potential in the inverted hierarchy region. In this talk the final results of CUORICINO will be presented with an update on CUORE R&D and prototypes.

News from Virgo: present status and future upgrades

Edwige Tournefier on behalf of the Virgo collaboration LAPP

presented by: Tournefier Edwige email-tournefier@lapp.in2p3.fr, phone-+33 4 50 09 16 75, fax-

The Virgo detector is designed to detect gravitational waves emitted by astrophysical sources in the frequency range from a few Hz to a few kHz.
The first phase of commissioning of the Virgo interferometer allowed us to obtain good stability of the interferometer and a sensitivity close to the design. Consequently a first long science run (VRS1) took place in 2007 in coincidence with the LIGO detectors. Since then, a series of upgrades has taken place (Virgo+ configuration) to further improve the sensitivity with the aim of a longer science run (VSR2) planned for mid 2009 in coincidence with the LIGO S6 run.
In parallel the Advanced Virgo detector is been designed, aiming at a sensitivity 10 times better than for Virgo. The construction phase is expected to start mid 2009.
The present status of Virgo will be presented, including results from VSR1 science run, along with the plans for Advanced Virgo.

Relativistic MHD Wave Scattering in Curved Spacetime

Parker W. Troischt Hartwick College, USA (some work done as a visitor to CITA)

presented by: Dr. Parker W. Troischt email-troischtp@hartwick.edu, phone-607-431-4745, fax-607-431-4734

Relativistic magnetohydrodynamics is important in a wide variety of astrophysical phenomena including: active galactic nuclei, pulsars, accreting black holes and gamma ray bursts. Fundamental to the study of any physical system is a study of its wave modes. We present a physically intuitive Lagrangian fluid formalism of relativistic MHD and apply it to study the propagation and interaction of wave modes in several background spacetimes.

Top Mass @Tevatron

Marco Trovato Pisa

presented by: Trovato Marco email-, phone-, fax-

ATLAS Commissioning and Potential Early Results

Tuan Vu Anh UC Riverside

presented by: Tuan Vu Anh email-, phone-, fax-

Iron 6.5 keV emissoin lines in Cen X-3 spectrum

Tugay A.V., Vasylenko A.A. National Taras Shevchenko University of Kyiv, Faculty of Physics Astronomy and Space Physics Department

presented by: Tugay A.V. email-tugay@univ.kiev.ua, phone-+380674057669, fax-+38 044 526 4507

We analyzed XMM-Newton observation of eclipsing high mass x-ray binary system Cen X-3. The observation was carried out at 27.01.2001 during 68 kiloseconds. This time corresponds to orbital phases between -0.03 to +0.33 (end of eclipse). Iron emission lines Fe K alpha, Fe XXV and Fe XXVI at energies 6.41 keV, 6.69 keV and 6.98 keV were founded out in the spectrum of the source. Intensity variation of these lines during orbital motion was also detected. The largest variation was detected for K alpha line, what agrees with the model of Ebisawa et al. (1996) in which K alpha line appears in hot plasma in accretion disc and highle ionized iron lines form in outer regions of binary system. Also we estimated geometrical parameters of system with the model of relativistic accretion disk and discussed the detection of Fe XXV triplet reported by Iaria et al. (2005).

Gravitino dark matter and high reheating temperature

M Olechowski, S Pokorski, K Turzynski and JD Wells Institute of Theoretical Physics, University of Warsaw (MO, SP, KT), CERN (JDW)

presented by: Turzynski K. email-turzyn@fuw.edu.pl, phone-+48 22 5532300, fax-

Supersymmetry breaking mediated by gauge interactions is regarded an attractive option due to the lack of new sources of flavor changing neutral currents other than those already present in the Standard Model. In models with gauge mediated supersymmetry breaking (GMSB), the dark matter particle is the gravitino. It is produced both thermally in scatterings in the hot plasma and non-thermally from decays of the next to lightest supersymmetric particle (NLSP). If the NLSP is sufficiently abundant during Big Bang Nucleosynthesis (BBN), these decays can alter the abundances of light elements. This, in turn, gives constraints on the gravitino mass and, for the observed dark matter abundance, on the reheating temperature of the Universe. Since sufficiently high reheating temperature is crucial for thermal leptogenesis, one obtains constraints on viable models with GMSB, consistent with thermal leptogenesis.
We study the interplay of these constraints within a recently introduced and interesting class of models with GMSB, known as models with general gauge mediation (GGM). We study the possibility that the NLSP is a stau or a sneutrino in these models. We determine whether it is possible to achieve `compressed' spectra of supersymmetric particles in which gluino is not much heavier than the NLSP, which alleviates the constraints imposed by requiring successful thermal leptogenesis. We study regions of the parameter space of models with GGM and identify regions in which one achieves radiative breaking of electroweak symmetry, satisfies the higgs mass bounds, gravitinos make up the observed amount of dark matter and the reheating temperature is high enough for leptogenesis.

Gravitino dark matter and high reheating temperature

M Olechowski, S Pokorski, K Turzynski and JD Wells Institute of Theoretical Physics, University of Warsaw (MO, SP, KT), CERN (JDW)

presented by: Turzynski K. email-turzyn@fuw.edu.pl, phone-+48 22 5532300, fax-

Supersymmetry breaking mediated by gauge interactions is regarded an attractive option due to the lack of new sources of flavor changing neutral currents other than those already present in the Standard Model. In models with gauge mediated supersymmetry breaking (GMSB), the dark matter particle is the gravitino. It is produced both thermally in scatterings in the hot plasma and non-thermally from decays of the next to lightest supersymmetric particle (NLSP). If the NLSP is sufficiently abundant during Big Bang Nucleosynthesis (BBN), these decays can alter the abundances of light elements. This, in turn, gives constraints on the gravitino mass and, for the observed dark matter abundance, on the reheating temperature of the Universe. Since sufficiently high reheating temperature is crucial for thermal leptogenesis, one obtains constraints on viable models with GMSB, consistent with thermal leptogenesis.
We study the interplay of these constraints within a recently introduced and interesting class of models with GMSB, known as models with general gauge mediation (GGM). We study the possibility that the NLSP is a stau or a sneutrino in these models. We determine whether it is possible to achieve `compressed' spectra of supersymmetric particles in which gluino is not much heavier than the NLSP, which alleviates the constraints imposed by requiring successful thermal leptogenesis. We study regions of the parameter space of models with GGM and identify regions in which one achieves radiative breaking of electroweak symmetry, satisfies the higgs mass bounds, gravitinos make up the observed amount of dark matter and the reheating temperature is high enough for leptogenesis.

How flat can you get? A model comparison perspective on the curvature of the Universe.

Mihran Vardanyan , Roberto Trotta , Joe Silk  Oxford University, Imperial College London, Oxford University

presented by: Vardanyan Mihran email-m.vardanyan1@physics.ox.ac.uk, phone-+44(0)1865 283133, fax-+44(0)1865 273390

The question of determining the spatial geometry of the Universe is of greater relevance than ever, as precision cosmology promises to verify inflationary predictions about the curvature of the Universe. We revisit the question of what can be learnt about the spatial geometry of the Universe from the perspective of a three-way Bayesian model comparison. We show that, given current data, the probability that the Universe is spatially infinite lies between 67and 98choice, we find odds of order 50:1 (200:1) in favour of a flat Universe when compared with a closed (open) model. We also report a robust, prior-independent lower limit to the number of Hubble spheres in the Universe, NU > 5 (at 99with which future CMB and BAO observations will be able to constrain curvature, finding that a cosmic variance limited CMB experiment together with an SKA-like BAO observation will constrain curvature with a precision of about sigma   4.5x10-4. We demonstrate that the risk of 'model confusion' (i.e., wrongly favouring a flat Universe in the presence of curvature) is much larger than might be assumed from parameter errors forecasts for future probes. We argue that a 5-sigma detection threshold guarantees a confusion- and ambiguity-free model selection. Together with inflationary arguments, this implies that the geometry of the Universe is not knowable if the value of the curvature parameter is below |Wcurvature|   10-4, a bound one order of magnitude larger than the size of curvature perturbations,   10-5.
Based on: http://arxiv.org/abs/0901.3354

Test of Lepton Flavour Violation with the NA62 experiment at CERN

Cristina Lazzeroni on behalf of NA62 Collaboration University of Birmingham

presented by: Venditti Stefano email-cristina.lazzeroni@cern.ch, phone-00441214144614, fax-

The SM prediction for the ratio of purely leptonic decay rates of the charged kaon RK=G(Ke2/G(Km2)) has an excellent sub-premille precision. Due to the helicity suppression of the SM contribution, the ratio is sensitive to non-SM effects; in particular, LFV contributions in the MSSM can modify it by a few percent without contradicting any other presently known experimental constraints. Current experimental precision is limited to 4.5%, and is insufficient for a stringent SM test. The NA62 experiment at the CERN SPS is aiming at improving the precision by almost an order of magnitude, using a dedicated data set collected in 2007/08. The status of the analysis will be discussed in detail.

SM Higgs @Tevatron

Rocio Vilar Calabria

presented by: Vilar Rocio email-, phone-, fax-

Limits on Primordial Black Hole evaporation with H.E.S.S.

Matthieu Vivier, on behalf the H.E.S.S. collaboration IRFU/SPP Cea-Saclay

presented by: Vivier Matthieu email-matthieu.vivier@cea.fr, phone-01 69 08 29 55, fax-01 69 08 50 13

Primordial Black Holes (PBHs) are hypothetical black holes that could have formed in the early stages of the Universe. According to Hawking's prediction, PBHs loose mass over cosmological time scales by emitting a thermal spectrum. With decreasing PBH mass, this process becomes increasingly fast, eventually leading to an explosive final evaporation potentially accompanied by bursts of very high energy particles. In this talk, a search for PBH bursts of very-high energy gamma-rays in the H.E.S.S. data set is presented and preliminary limits on the local PBH evaporation rate are derived.

Higgs boson properties and extra quark-lepton generations

Alexander Rozanov, Victor Novikov, Mikhail Vysotsky CPPM (Marseille), ITEP, ITEP

presented by: Vysotsky Mikhail email-vysotsky@itep.ru, phone-7-499-1238393, fax-7-495-1270833

Higgs boson mass, production crossection and decay branching ratios are strongly bounded in the Standard Model. However, the existence of extra quark-lepton generations may dramatically change these quantities.

Top Cross Sections at the Tevatron

Wolfgang Wagner Bergische Universitaet Wuppertal

presented by: Wolfgang Wagner email-wagner@physik.uni-wuppertal.de, phone-+49-202-439-3786, fax-+49-202-439-2811

Since the start of Run II of the Tevatron in 2002 the particle detectors CDF and D0 have recorded collision data corresponding to about 5.5 fb-1, allowing to reconstruct a few thousand top-quark events. Based on these data sets detailed studies of top-quark properties have been performed.
One of the basic measurements in the top-quark sector is the determination of the top-antitop pair production cross section. A comparison with theoretical predictions constitutes a test of perturbative QCD. The study of differential cross sections, for example, the study of the top-antitop invariant mass spectrum provides the opportunity to search for non-standard-model sources of top quarks.
The samples of reconstructed top quarks are also used to investigate production and decay properties, such as the W helicity in top-quark decays,the top-antitop forward-backward asymmetry, and the braching ratio into the dominant decay mode, a W boson and a b-quark.

Matter Dark (Light Higgs) Searches in Bottomonium

Lucas Winstrom  UC Santa Cruz

presented by: Winstrom Lucas email-, phone-, fax-

VHE Cosmic Ray R and E Experiment in Korea

Jongmann Yang Ewha Womans University

presented by: Yang Jongmann email-jyang@ewha.ac.kr, phone-82-2-3277-2330, fax-82-2-3277-2320

In order to measure high-energy cosmic ray air showers utilizing the facility and student-power in high schools around Seoul area, we formulated a collaboration named COREA (COsmic ray Research and Education Array). So far we installed plastic scintillation detector arrays at Kyeonggibuk Science High School and Hansung Science High School. Consisting of four large scintillation plates each, three stations were set up on top of the school buildings with 1 m spacing. All recorded events have been checked for the coincidence by comparing the time difference between any two single events from each station. Detected high-energy air showers using coincidence detection technique have been evaluated to determine the coincidence signals from each site. The simulation of air shower events by AIRES (AIR-shower Extended Simulations) program has been performed to make a comparison with collected shower events. Current status of the array construction plan will be presented.

The determination of the gamma-families fraction originating from Primary Photons.

Yuldashbaev T.S., Kulachmedov N.N., Nuritdinov Kh. Physical-Technical Inst. of Uzbekistan AS

presented by: Yuldashbaev T.S. email-tsju@uzsci.net, phone-(998) 235-36-33, fax-(998) 235-42-91

In the paper it is shown the possibility of the primary gamma radiation studying by the method of the X-ray emulsion chambers (XREC). The different selection criteria of the gamma-families initiated by primary gama rays in XREC were worked out, and the fraction of such families registered by Pamir experiment was estimated.

Observational Signatures of Cosmological Black Holes

Salvatore Capozziello, Cosimo Stornaiolo, Alexander Zakharov Napoli University, ITEP

presented by: Zakharov Alexander email-zakharov@itep.ru, phone-007-495-1279759, fax-

We discuss observational features of cosmological (hypermassive) black holes (CBHs). If really such objects like cosmological black holes exist they may be studied with a standard technique like strong and weak gravitational lensing. Cosmological voids can be explained as the result the collapse of large perturbations into black hole with masses of the order of 1014M\odot and the expansion of the universe. The resulting image of the universe is that it is more homogeneous than expected from present observations. In this paper we discuss some lensing properties related to the CBHs.

Gravitational lensing: from micro to nano

Gabriele Ingrosso, Sebastiano Calchi Novati, Francesco De Paolis, Philippe Jetzer, Achille Nucita, Alexander Zakharov ITEP, Salerno University, Salento University

presented by: Zakharov Alexander email-, phone-, fax-

We discuss different regimes of gravitational lensing depending on gravitational lens masses, in particular, mass scale Modot corresponds to micro, mass scale Modot10-6 corresponds to nano regimes respectively. Therefore, detections of observational features of gravitational (nano-)lensing provide an opportunity to discover objects with Earth and (sub-) Earth masses. We discuss a possibility to discover a low mass planet in Andromeda galaxy with pixel-lensing. Thus, at the moment, gravitational lensing is the only way to find low mass exoplanets in other galaxies. We note an importance to introduce new selection criteria including temporal variability features for continuum and spectral lines to analyze event candidates in details.

PVLAS: Physics results and recent developments of the apparatus

F. Della Valle1, G. Di Domenico2, U. Gastaldi3, E. Milotti1, R. Pengo3, G. Ruoso3, G. Zavattini2 1Physics Department of the University of Trieste and INFN - Trieste Italy, 2Physics Department of the University of Ferrara and INFN - Ferrara Italy, INFN National Laboratories of Legnaro Italy

presented by: Zavattini G. email-zavattini@fe.infn.it, phone-+39 0532 974299, fax-+39 0532 974210

The aim of the PVLAS experiment is to detect for the first time vacuum magnetic linear birefringence in the optical - near infrared energy range. This process is closely connected to low energy photon-photon elastic scattering and is predicted by quantum electrodynamics. At present PVLAS has set the best limits on such processes.
The same apparatus has also been used to set model independent limits on the existence of hypothetical axion like particles coupling to two photons setting a laboratory limit of 2.8 ·106 GeV for axion masses below 1 meV.
Until recently the sensitivity of the apparatus has been limited by external noise sources which have now been accounted for thereby improving the sensitivity by a factor 50. We are presently assembling a complete prototype system, including magnets, with which we aim to further improve our limits.

Search for Nu-tau appearance via neutrino oscillations in the CNGS beam with the OPERA experiment.

Amina ZGHICHE for the OPERA Collaboration LAPP, Universite de Savoie, CNRS/IN2P3, Annecy-le-Vieux, France

presented by: ZGHICHE Amina email-zghiche@lapp.in2p3.fr, phone-33 450091732, fax-334 50 27 94 95

The OPERA neutrino experiment, located in the underground Gran Sasso Laboratory (LNGS), is designed to detect for the first time neutrino oscillation in the appearance mode Nu-mu&# 8594;Nu-tau. The OPERA detector is an emulsion/lead target combined with electronic detectors, installed at the end of the 730 km long-baseline high energy Nu-mu beam from CERN to LNGS (CNGS). Runs with CNGS neutrinos were successfully carried out in 2007 and 2008 with the detector fully operational together with its related facilities for emulsion handling and analysis. In this talk, the experimental setup description will be followed by a report on the collection, reconstruction and analysis of first samples of neutrino interaction events.

Extending the cosmic distance ladder to z=7 and beyond: using SNIa to calibrate GRB standard candles

Shuang-Nan Zhang, Nan Liang Tsinghua University, Beijing, China

presented by: Zhang Shuang-Nan email-zhangsn@tsinghua.edu.cn, phone-+8610-62794220, fax-+8610-62785807

An important concern in the application of gamma-ray bursts (GRBs) to cosmology is that the calibration of GRB luminosity/energy relations depends on the cosmological model, due to the lack of a sufficient low-redshift GRB sample. In this paper, we present a new method to calibrate GRB relations in a cosmology-independent way. Since objects at the same redshift should have the same luminosity distance and since the distance moduli of Type Ia supernovae (SNe Ia) obtained directly from observations are completely cosmology independent, we obtain the distance modulus of a GRB at a given redshift by interpolating from the Hubble diagram of SNe Ia. Then we calibrate seven GRB relations without assuming a particular cosmological model and construct a GRB Hubble diagram to constrain cosmological parameters. The main paper has been published as: ApJ, 685, Issue 1, pp. 354-360.

Contributions to WMAP cleaned temperature maps from SDSS galaxies: implications for the Planck mission

Shuang-Nan Zhang, Jian Wang Tsinghua University

presented by: Zhang Shuang-Nan email-zhangsn@tsinghua.edu.cn, phone-+8610-62794220, fax-+8610-62785807

We have systematically examined the cross-correlations between WMAP temperature maps, the SFD dust extinction map, and SDSS galaxies. We couclude that: (1) the dust extinction map is contaminated by emissions from SDSS galaxies, consistent with previous results; (2) SDSS galaxy number counts are significantly correlated with WMAP temperature maps before foreground cleaning, but the correlation still remains statistically significant even in the published cleaned maps; (3) the SDSS galaxy - WMAP correlations are best explained by contributions from unremoved and over-removed microwave emissions from SDSS galaxies, because the SDSS galaxies contamination to the SFD dust extinction map is not considered in the foreground cleaning process. Finally we will discuss the implications of our findings to the foreground cleaning of the Planck misison, which will sufer more from microwave emissions of galaxies.

Neutrino Oscillation in the Standard Model and beyond

F.del Aguila, J. Syska, R. Szafron, M. Zralek Institute of Physics University of Granada Spain, Institute of Physics University of Silesia Poland

presented by: Zralek M. email-marek.zralek@us.edu.pl, phone-0048 32 228 29 08, fax-004832 2583653

General description of the neutrino oscillation in the Standard Model and beyond (NP)  is presented. The initial neutrino states are not necessary described by the MNS mixing matrix, their states are sometimes mixed, and density matrix approach must be used. All elements of neutrino oscillation experiments, neutrinos production, propagation in a matter, and detection process are modified by NP. The detection rate does not factorize for the oscillation probability and the detection cross section. Dirac and Majorana neutrinos oscillate can oscillate in different way. Depending on the production process neutrinos can oscillate in coherent or incoherent way. Everything is presented on the example of neutrinos coming from muon decay.

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On 17 Jun 2009, 17:46.