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We present the spectral and temporal analysis of the 2004/2005 outburst of the transient X-ray pulsar V0332+53 as observed with Integral. After the discovery of the third cyclotron line in phase averaged spectra (Kreykenbohm et al 2005, Pottschmidt et al 2005), detailed pulse phase spectroscopy revealed remarkably little variability of the cyclotron lines through the 4.4s X-ray pulse (Pottschmidt et al 2005). During the decline of the outburst, the flux was observed to decay exponentially until 2005 Feb 10 and linearly thereafter. The spectrum was found to become harder with time, while the folding energy remained constant. The energy of the fundamental cyclotron line increased with time from 26.5kev in the RXTE observation up to 29.5kev in the last Integral one indicating that the emission region is moving closer to the surface of the neutron star. For a detailed analysis, see Mowlavi et al (2005).

This contribution to the published Proceedings records the opening talk I presented on the first morning of the 2005 International Linear Collider Workshop in Snowmass, CO, August 14 - 27, 2005. It includes a summary of the motivation for the workshop, the scientific goals and charges for the working groups, the initial plans of the accelerator, detector, and physics groups, and the activities of the communication, education, and outreach group. This document also describes organizational aspects of the meeting, particularly the scientific committee structure, the self-organization of the working groups, the composition of the indispensable secretariat and computer support teams, and the sources of funding support. The report serves as an introduction to the proceedings whose individual papers and summary documents must be consulted for an appreciation of the accomplishments and progress made at Snowmass in 2005 toward the realization of an International Linear Collider.

In this note we re-propose the arguments presented in Vio (2005) examining the superiority of the 'bi-parametric scale adaptive filter' (BSAF) when dealing with source detection as claimed by (Lopez-Caniego 2005a) and confirmed in Lopez-Caniego (2005b). We suggest here that the dispute can be easily solved if these authors provide the community with a detailed derivation of a basic equation.

In this document we collect the 18 contributions of the IceCube Collaboration to the 29th International Cosmic Ray Conference (ICRC 2005), Pune, India, Aug. 2005

IceCube is a kilometer scale neutrino observatory now in construction at the South Pole. The construction started in January 2005 with the deployment of 76 sensors on the first string and four surface detector stations. Nine strings and 32 surface detectors are in operation since February 2006. The data based on calibration measurements, muons and artificial light flashes are consistent with performance expectations. This report focuses on design, construction experience and first data from the sensors deployed in January 2005.

The high-frequency peaked BL Lac PKS 2005-489 (z=0.071) was observed in 2003 and 2004 with the H.E.S.S. stereoscopic array of imaging atmospheric-Cherenkov telescopes in Namibia. A signal was detected at the 6.7 sigma level in the 2004 observations (24.2 hrs live time), but not in the 2003 data set (27.3 hrs live time). PKS 2005-489 is the first blazar independently discovered by H.E.S.S. to be an emitter of VHE photons, and only the second such blazar in the Southern Hemisphere. The integral flux above 200 GeV observed in 2004 is (6.9 +/- 1.0 +/- 1.4) x 10$^{-12}$ cm$^{-2}$ s$^{-1}$, corresponding to ~2.5% of the flux observed from the Crab Nebula. The 99% upper limit on the flux in 2003, I(>200 GeV) < 5.2 x 10$^{-12}$ cm$^{-2}$ s$^{-1}$, is smaller than the flux measured in 2004, suggesting an increased level of activity in 2004. However, the data show no evidence for significant variability on any time scale less than a year. An energy spectrum is measured and is characterized by a very soft power law (photon index = 4.0 +/- 0.4).

Lyutikov (astro-ph/0503505) raised a valid point that for shock deceleration of a highly magnetized outflow, the fate of the magnetic fields after shock crossing should be considered. However, his comment that the deceleration radius should be defined by the total energy rather than by the baryonic kinetic energy is incorrect. As strictly derived from the shock jump conditions in Zhang & Kobayashi (2005), during the reverse shock crossing process the magnetic energy is not tapped. As a result, the fireball deceleration radius is defined by the baryonic energy only. The magnetic energy is expected to be transferred to the circumburst medium after the reverse shock disappears. The evolution of the system then mimicks a continuously-fed fireball. As a result, Lyutikov's naive conclusion that the forward shock dynamics is independent on the ejecta content is also incorrect. The shock deceleration dynamics and the reverse shock calculation presented in Zhang & Kobayashi (2005) are robust and correct.

The decline of the high mass X-ray transient V0332+53 during the Dec. 2004 to Feb. 2005 outburst is analysed from the data recorded by INTEGRAL. The flux is shown to decrease exponentially until 2005 Feb. 10, with a decay time scale of \~30 days above 20 keV and ~20 days at lower energies, and to decrease linearly thereafter. The energy spectrum is well modelled throughout the decay by a power law with a folding energy of ~7.5 keV, and with two cyclotron absorption features. The folding energy does not vary significantly over the decay, but the spectrum becomes harder with time. Most importantly, we show that the parameters describing the fundamental cyclotron line around 27 keV do vary with time: its energy and depth increase (by about 17% for the energy in ~6 weeks), while its width decreases. These changes of the cyclotron line parameters are interpreted as resulting from a change in the extent of the cyclotron scattering region. Two quasi-periodic oscillations are also observed at various times during the observations, one at 0.05 Hz and another one near the pulsation frequency around 0.23 Hz.

We present new astrometry of Pluto's three satellites from images taken of the Pluto system during 2002-3 with the High Resolution Camera (HRC) mode of the Advanced Camera for Surveys (ACS) instrument on the Hubble Space Telescope. The observations were designed to produce an albedo map of Pluto but they also contain images of Charon and the two recently discovered satellites, S/2005 P1 and S/2005 P2. Orbits fitted to all three satellites are nearly co-planar and, for Charon and P2, have eccentricities consistent with zero. The orbit of the outermost satellite, P1, has a significant eccentricity of 0.0052 +/- 0.0011. Orbital periods of P1, P2, and Charon are 38.2065 +/- 0.0014, 24.8562 +/- 00013, and 6.3872304 +/- 0.0000011 days, respectively. The total system mass based on Charon's orbit is 1.4570 +/- 0.0009 x 10^22 kg. We confirm previous results that orbital periods are close to the ratio of 6:4:1 (P1:P2:Charon) indicative of mean-motion resonances, but our results formally preclude precise integer period ratios. The orbits of P1 and P2, being about the barycenter rather than Pluto, enable us to measure the Charon/Pluto mass ratio as 0.1165 +/- 0.0055. This new mass ratio implie

The flat-spectrum radio quasar 3C 454.3 is well known to be a highly active and variable source with outbursts occurring across the whole electromagnetic spectrum over the last decades. In spring 2005, 3C 454.3 has been reported to exhibit a strong optical outburst which subsequently triggered multi-frequency observations of the source covering the radio up to gamma-ray bands. Here, we present first results of our near-IR/optical (V, R, I, H band) photometry performed between May 11 and August 5, 2005 with the Rapid Eye Mount (REM) at La Silla in Chile and the Automatic Imaging Telescope (AIT) of the Perugia University Observatory. 3C 454.3 was observed during an exceptional and historical high state with a subsequent decrease in brightness over our 86 days observing period. The continuum spectral behaviour during the flaring and declining phase suggests a synchrotron peak below the near-IR band as well as a geometrical origin of the variations e.g. due to changes in the direction of forward beaming.

This volume contains papers presented at WLPE 2005, 15th International Workshop on Logic-based methods in Programming Environments. The aim of the workshop is to provide an informal meeting for the researchers working on logic-based tools for development and analysis of programs. This year we emphasized two aspects: on one hand the presentation, pragmatics and experiences of tools for logic programming environments; on the other one, logic-based environmental tools for programming in general. The workshop took place in Sitges (Barcelona), Spain as a satellite workshop of the 21th International Conference on Logic Programming (ICLP 2005). This workshop continues the series of successful international workshops on logic programming environments held in Ohio, USA (1989), Eilat, Israel (1990), Paris, France (1991), Washington, USA (1992), Vancouver, Canada (1993), Santa Margherita Ligure, Italy (1994), Portland, USA (1995), Leuven, Belgium and Port Jefferson, USA (1997), Las Cruces, USA (1999), Paphos, Cyprus (2001), Copenhagen, Denmark (2002), Mumbai, India (2003) and Saint Malo, France (2004). We have received eight submissions (2 from France, 2 Spain-US cooperations, one Spain-Argen

We recount problems, questions and conjectures that arose during a problem session of the Third International Conference on Permutation Patterns, University of Florida, March 7-11, 2005.

This is a review of the latest developments in the theory of superdense nuclear matter, formed in relativistic heavy ion collisions or in the core of collapsed stars, as they were reported and discussed at the Quark Matter 2005 conference in Budapest (Hungary).

Summary of the XIth International Conference on Elastic and Diffractive Scattering in Chateau de Blois, France, May 15 - 20, 2005, summarizing both theoretical and experimental presentations and discussions.

I broadly summarize the theoretical contributions in the Electroweak session of the 2005 Moriond meeting under four rubrics: i) neutrinos; ii) cosmology; iii) electroweak interactions; and iv) flavor physics.

At the 2005 world championships there was considerable discussion and a formal protest in the long distance race arising from a perceived advantage obtained by some athletes running together. It is shown that a statistical model presented in previous work [1] is applicable to this event, giving predictions of the final times to with 2-3 minutes. Using the model, we show that pack formation was inevitable in this format. The statistical benefit gained at the elite level from running with other competitors appears to derive both from increase speed through the terrain, and the elimination of large navigational errors.

This article reports world averages for measurements on b-hadron properties obtained by the Heavy Flavor Averaging Group (HFAG) using the available results as of winter 2005 conferences. In the averaging, the input parameters used in the various analyses are adjusted (rescaled) to common values, and all known correlations are taken into account. The averages include lifetimes, neutral meson mixing parameters, semileptonic decay parameters, rare decay branching fractions, and CP violation measurements.

Some aspects of hadron spectroscopy are reviewed as of summer 2005.

This article explains how to add spatial search functions (point-near-point and point in polygon) to Microsoft SQL Server 2005 using C# and table-valued functions. It is possible to use this library to add spatial search to your application without writing any special code. The library implements the public-domain C# Hierarchical Triangular Mesh (HTM) algorithms from Johns Hopkins University. That C# library is connected to SQL Server 2005 via a set of scalar-valued and table-valued functions. These functions act as a spatial index.