Instruction: what is the prompt that generates the input?

Input: A general {\it ab-initio} and non-perturbative method to solve thetime-dependent Schr\"odinger equation (TDSE) for the interaction of a strongattosecond laser pulse with a general atom, i.e., beyond the models ofquasi-one-electron or quasi-two-electron targets, is described. The field-freeHamiltonian and the dipole matrices are generated using a flexible $B$-spline$R$-matrix method. This numerical implementation enables us to constructterm-dependent, non-orthogonal sets of one-electron orbitals for the bound andcontinuum electrons. The solution of the TDSE is propagated in time using theArnoldi-Lanczos method, which does not require the diagonalization of any largematrices. The method is illustrated by an application to the multi-photonexcitation and ionization of Ne atoms. Good agreement with $R$-matrix Floquetcalculations for the generalized cross sections for two-photon ionization isachieved.


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Input: Starting with a field theoretic approach in Minkowski space, thegravitational energy momentum tensor is derived from the Einstein equations ina straightforward manner. This allows to present them as {\it accelerationtensor} = const. $\times$ {\it total energy momentum tensor}. For flat spacecosmology the gravitational energy is negative and cancels the material energy.In the relativistic theory of gravitation a bimetric coupling between theRiemann and Minkowski metrics breaks general coordinate invariance. The case ofa positive cosmological constant is considered. A singularity free version ofthe Schwarzschild black hole is solved analytically. In the interior thecomponents of the metric tensor quickly die out, but do not change sign,leaving the role of time as usual. For cosmology the $\Lambda$CDM model iscovered, while there appears a form of inflation at early times. Here both thetotal energy and the zero point energy vanish.


Instruction: what is the prompt that generates the input?

Input: Recently, an extension of the standard model based on ideas of Lee and Wickhas been discussed. This theory is free of quadratic divergences and hence hasa Higgs mass that is stable against radiative corrections. Here, we address thequestion of whether or not it is possible to couple very heavy particles, withmasses much greater than the weak scale, to the Lee-Wick standard model degreesof freedom and still preserve the stability of the weak scale. We show that inthe LW-standard model the familiar see-saw mechanism for generating neutrinomasses preserves the solution to the hierarchy puzzle provided by the higherderivative terms. The very heavy right handed neutrinos do not destabilize theHiggs mass. We give an example of new heavy degrees of freedom that woulddestabilize the hierarchy, and discuss a general mechanism for coupling otherheavy degrees of freedom to the Higgs doublet while preserving the hierarchy.


Instruction: what is the prompt that generates the input?

Input: We establish the first hardness results for the problem of computing thevalue of one-round games played by a verifier and a team of provers who canshare quantum entanglement. In particular, we show that it is NP-hard toapproximate within an inverse polynomial the value of a one-round game with (i)quantum verifier and two entangled provers or (ii) classical verifier and threeentangled provers. Previously it was not even known if computing the valueexactly is NP-hard. We also describe a mathematical conjecture, which, if true,would imply hardness of approximation to within a constant.  We start our proof by describing two ways to modify classical multi-provergames to make them resistant to entangled provers. We then show that a strategyfor the modified game that uses entanglement can be ``rounded'' to one thatdoes not. The results then follow from classical inapproximability bounds. Ourwork implies that, unless P=NP, the values of entangled-prover games cannot becomputed by semidefinite programs that are polynomial in the size of theverifier's system, a method that has been successful for more restrictedquantum games.


Instruction: what is the prompt that generates the input?

Input: When a source emits a gravity-wave (GW) pulse over a short period of time,the leading edge of the GW signal is redshifted more than the inner boundary ofthe pulse. The GW pulse is distorted by the gravitational effect of theself-energy residing in between these shells. We illustrate this distortion forGW pulses from the final plunge of black hole (BH) binaries, leading to theevolution of the GW profile as a function of the radial distance from thesource. The distortion depends on the total GW energy released and the durationof the emission, scaled by the total binary mass, M. The effect should berelevant in finite box simulations where the waveforms are extracted within aradius of <~ 100M. For characteristic emission parameters at the final plungebetween binary BHs of arbitrary spins, this effect could distort the simulatedGW templates for LIGO and LISA by a fraction of 0.001. Accounting for the wavedistortion would significantly decrease the waveform extraction errors innumerical simulations.


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Input: Determinations of beryllium abundance in stars, together with lithium,provide a key tool to investigate the so far poorly understood extra-mixingprocesses at work in stellar interiors. We measured Be in three openclusters,complementing existing Be surveys, and aiming at gathering a morecomplete empirical scenario of the evolution of Be as a function of stellar ageand temperature. Specifically, we analyzed VLT/UVES spectra of members of NGC2516, the Hyades, and M 67 to determine their Be and Li abundances. In thefirst two clusters we focused on stars cooler than 5400 K, while the M 67sample includes stars warmer than 6150 K, as well as two subgiants and two bluestragglers. We also computed the evolution of Be for a 0.9 Mo star based onstandard evolutionary models. We find different emprical behaviours for starsin different temperature bins and ages. Stars warmer than 6150 K show Bedepletion and follow a Be vs. Li correlation while Be is undepleted in stars inthe ~6150-5600 K range. NGC 2516 members cooler than 5400 K have not depletedany Be, but older Hyades of similar temperature do show some depletion. Be isseverely depleted in the subgiants and blue stragglers. The results for warmstars are in agreement with previous studies, supporting the hypothesis thatmixing in this temperature regime is driven by rotation. The same holds for thetwo subgiants that have evolved from the "Li gap". This mechanism is insteadnot the dominant one for solar-type stars. We show that Be depletion of coolHyades cannot simply be explained by the effect of increasing depth of theconvective zone. Finally, the different Be content of the two blue stragglerssuggests that they have formed by two different processes (i.e., collisions vs.binary merging).


Instruction: what is the prompt that generates the input?

Input: Different types of superfluid ground states have been investigated in systemsof two species of fermions with Fermi surfaces that do not match. This study isrelevant for cold atomic systems, condensed matter physics and quark matter. Inthis paper we consider this problem in the case the fermionic quasi-particlescan transmute into one another and only their total number is conserved. We usea BCS approximation to study superconductivity in two-band metallic systemswith inter and intra-band interactions. Tuning the hybridization between thebands varies the mismatch of the Fermi surfaces and produces differentinstabilities. For inter-band attractive interactions we find a first ordernormal-superconductor and a homogeneous metastable phase with gaplessexcitations. In the case of intra-band interactions, the transition from thesuperconductor to the normal state as hybridization increases is continuous andassociated with a quantum critical point. The case when both interactions arepresent is also considered.


Instruction: what is the prompt that generates the input?

Input: We obtain a first order differential equation for the driving function of thechordal Loewner differential equation in the case where the domain is slit by acurve which is a trajectory arc of certain quadratic differentials. Inparticular this includes the case when the curve is a path on the square,triangle or hexagonal lattice in the upper halfplane or, indeed, in any domainwith boundary on the lattice. We also demonstrate how we use this to calculatethe driving function numerically. Equivalent results for other variants of theLoewner differential equation are also obtained: Multiple slits in the chordalLoewner differential equation and the radial Loewner differential equation. Themethod also works for other versions of the Loewner differential equation. Theproof of our formula uses a generalization of Schwarz-Christoffel mapping todomains bounded by trajectory arcs of rotations of a given quadraticdifferential that is of interest in its own right.


Instruction: what is the prompt that generates the input?

Input: An epidemic multi-strain model with temporary cross-immunity shows chaos,even in a previously unexpected parameter region. Especially dengue fevermodels with strong enhanced infectivity on secondary infection have previouslyshown deterministic chaos motivated by experimental findings ofantibody-dependent-enhancement (ADE). Including temporary cross-immunity insuch models, which is common knowledge among field researchers in dengue, wefind a deterministically chaotic attractor in the more realistic parameterregion of reduced infectivity on secondary infection (''inverse ADE'' parameterregion). This is realistic for dengue fever since on second infection peopleare more likely to be hospitalized, hence do not contribute to the force ofinfection as much as people with first infection.  Our finding has wider implications beyond dengue in any multi-strainepidemiological systems with altered infectivity upon secondary infection,since we can relax the condition of rather high infectivity on secondaryinfection previously required for deterministic chaos. For dengue the findingof wide ranges of chaotic attractors open new ways to analysis of existing datasets.


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Input: We present a detailed analysis of the prompt and afterglow emission of GRB050410 and GRB 050412 detected by Swift for which no optical counterpart wasobserved. The 15-150 keV energy distribution of the GRB 050410 prompt emissionshows a peak energy at 53 keV. The XRT light curve of this GRB decays as apower law with a slope of alpha=1.06+/-0.04. The spectrum is well reproduced byan absorbed power law with a spectral index Gamma_x=2.4+/-0.4 and a low energyabsorption N_H=4(+3;-2)x10^21 cm^(-2) which is higher than the Galactic value.The 15-150 keV prompt emission in GRB 050412 is modelled with a hard(Gamma=0.7+/-0.2) power law. The XRT light curve follows a broken power lawwith the first slope alpha_1=0.7+/-0.4, the break time T_break=254(-41;+79) sand the second slope alpha_2=2.8(-0.8;+0.5). The spectrum is fitted by a powerlaw with spectral index Gamma_x=1.3+/-0.2 which is absorbed at low energies bythe Galactic column. The GRB 050410 afterglow reveals the expectedcharacteristics of the third component of the canonical Swift light curve.Conversely, a complex phenomenology was detected in the GRB 050412 because ofthe presence of the very early break. The light curve in this case can beinterpreted as being the last peak of the prompt emission. The two burstspresent tight upper limits for the optical emission, however, neither of themcan be clearly classified as dark. For GRB 050410, the suppression of theoptical afterglow could be attributed to a low density interstellar mediumsurrounding the burst. For GRB 050412, the evaluation of the darkness is moredifficult due to the ambiguity in the extrapolation of the X-ray afterglowlight curve.


Instruction: what is the prompt that generates the input?

Input: High-resolution spectroscopy of U Gem was obtained during quiescence. We didnot find a hot spot or gas stream around the outer boundaries of the accretiondisk. Instead, we detected a strong narrow emission near the location of thesecondary star. We measured the radial velocity curve from the wings of thedouble-peaked H$\alpha$ emission line, and obtained a semi-amplitude value thatis in excellent agreement with the obtained from observations in theultraviolet spectral region by Sion et al. (1998). We present also a new methodto obtain K_2, which enhances the detection of absorption or emission featuresarising in the late-type companion. Our results are compared with publishedvalues derived from the near-infrared NaI line doublet. From a comparison ofthe TiO band with those of late type M stars, we find that a best fit isobtained for a M6V star, contributing 5 percent of the total light at thatspectral region. Assuming that the radial velocity semi-amplitudes reflectaccurately the motion of the binary components, then from our results: K_em =107+/-2 km/s; K_abs = 310+/-5 km/s, and using the inclination angle given byZhang & Robinson(1987); i = 69.7+/-0.7, the system parameters become: M_WD =1.20+/-0.05 M_sun,; M_RD = 0.42+/-0.04 M_sun; and a = 1.55+/- 0.02 R_sun. Basedon the separation of the double emission peaks, we calculate an outer diskradius of R_out/a ~0.61, close to the distance of the inner Lagrangian pointL_1/a~0.63. Therefore we suggest that, at the time of observations, theaccretion disk was filling the Roche-Lobe of the primary, and that the matterleaving the L_1 point was colliding with the disc directly, producing the hotspot at this location.


Instruction: what is the prompt that generates the input?

Input: Rotating deformed neutron stars are important potential sources forgroundbased gravitational-wave interferometers such as LIGO, GE0600 and VIRGO.One mechanism that may lead to significant non-asymmetries is the internalmagnetic field. It is well known that a magnetic star will not be sphericaland, if the magnetic axis is not aligned with the spin axis, the deformationwill lead to the emission of gravitational waves. The aim of this paper is todevelop a formalism that would allow us to model magnetically deformed stars,using both realistic equations of state and field configurations. As a firststep, we consider a set of simplified model problems. Focusing on dipolarfields, we determine the internal magnetic field which is consistent with agiven neutron star model. We then calculate the associated deformation. Weconclude by discussing the relevance of our results for currentgravitational-wave detectors and future prospects.


Instruction: what is the prompt that generates the input?

Input: Alexander B. Medvinsky \emph{et al} [A. B. Medvinsky, I. A. Tikhonova, R. R.Aliev, B.-L. Li, Z.-S. Lin, and H. Malchow, Phys. Rev. E \textbf{64}, 021915(2001)] and Marcus R. Garvie \emph{et al} [M. R. Garvie and C. Trenchea, SIAMJ. Control. Optim. \textbf{46}, 775-791 (2007)] shown that the minimalspatially extended reaction-diffusion model of phytoplankton-zooplankton canexhibit both regular, chaotic behavior, and spatiotemporal patterns in a patchyenvironment. Based on that, the spatial plankton model is furtherlyinvestigated by means of computer simulations and theoretical analysis in thepresent paper when its parameters would be expected in the case of mixedTuring-Hopf bifurcation region. Our results show that the spiral waves exist inthat region and the spatiotemporal chaos emerge, which arise from the far-fieldbreakup of the spiral waves over large ranges of diffusion coefficients ofphytoplankton and zooplankton. Moreover, the spatiotemporal chaos arising fromthe far-field breakup of spiral waves does not gradually involve the wholespace within that region. Our results are confirmed by means of computationspectra and nonlinear bifurcation of wave trains. Finally, we give someexplanations about the spatially structured patterns from the community level.


Instruction: what is the prompt that generates the input?

Input: In the bootstrap percolation model, sites in an L by L square are initiallyinfected independently with probability p. At subsequent steps, a healthy sitebecomes infected if it has at least 2 infected neighbours. As(L,p)->(infinity,0), the probability that the entire square is eventuallyinfected is known to undergo a phase transition in the parameter p log L,occurring asymptotically at lambda = pi^2/18. We prove that the discrepancybetween the critical parameter and its limit lambda is at least Omega((logL)^(-1/2)). In contrast, the critical window has width only Theta((logL)^(-1)). For the so-called modified model, we prove rigorous explicit boundswhich imply for example that the relative discrepancy is at least 1% even whenL = 10^3000. Our results shed some light on the observed differences betweensimulations and rigorous asymptotics.


Instruction: what is the prompt that generates the input?

Input: The tilt modulus of a defective Abrikosov vortex lattice pinned by materialline defects is computed using the boson analogy. It tends to infinity at longwavelength, which yields a Bose glass state that is robust to the addition ofweak point-pinning centers, and which implies a restoring force per vortex linefor rigid translations about mechanical equilibrium that is independent ofmagnetic field. It also indicates that the Bose glass state breaks into piecesalong the direction of the correlated pinning centers if the latter have finitelength. The critical current is predicted to crossover from two dimensional tothree dimensional behavior as a function of sample thickness along thecorrelated pinning centers in such case. That crossover notably can occur at afilm thickness that is much larger than that expected from point pins ofcomparable strength. The above is compared to the dependence on thickness shownby the critical current in certain films of high-temperature superconductorscurrently being developed for wire technology.


Instruction: what is the prompt that generates the input?

Input: We address two issues in the thermodynamic model for nuclear disassembly.Surprisingly large differences in results for specific heat were seen inpredictions from the canonical and grand canonical ensembles when the nuclearsystem passes from liquid-gas co-existence to the pure gas phase. We are ableto pinpoint and understand the reasons for such and other discrepancies whenthey appear. There is a subtle but important difference in the physicsaddressed in the two models. In particular if we reformulate the parameters inthe canonical model to better approximate the physics addressed in the grandcanonical model, calculations for observables converge. Next we turn to theissue of bimodality in the probability distribution of the largest fragment inboth canonical and grand canonical ensembles. We demonstrate that thisdistribution is very closely related to average multiplicities. Therelationship of the bimodal distribution to phase transition is discussed.


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Input: The near-infrared integral field spectrograph SINFONI at the ESO VLT opens anew window for the study of central supermassive black holes. With a near-IRspatial resolution similar to HST optical and the ability to penetrate dust itprovides the possibility to explore the low-mass end of the M-sigma relation(sigma<120km/s) where so far very few black hole masses were measured withstellar dynamics. With SINFONI we observed the central region of thelow-luminosity elliptical galaxy NGC4486a at a spatial resolution of ~0.1arcsecin the K band. The stellar kinematics was measured with a maximum penalisedlikelihood method considering the region around the CO absorption band heads.We determined a black hole mass of M_BH=1.25^{+0.75}_{-0.79} x 10^7 M_sun (90%C.L.) using the Schwarzschild orbit superposition method including the full2-dimensional spatial information. This mass agrees with the predictions of theM-sigma relation, strengthening its validity at the lower sigma end.


Instruction: what is the prompt that generates the input?

Input: Propagation, transmission and reflection properties of linearly polarizedplane waves and arbitrarily short electromagnetic pulses in one-dimensionaldispersionless dielectric media possessing an arbitrary space-time dependenceof the refractive index are studied by using a two-component, highly symmetricversion of Maxwell's equations. The use of any slow varying amplitudeapproximation is avoided. Transfer matrices of sharp nonstationary interfacesare calculated explicitly, together with the amplitudes of all secondary wavesproduced in the scattering. Time-varying multilayer structures andspatiotemporal lenses in various configurations are investigated analyticallyand numerically in a unified approach. Several new effects are reported, suchas pulse compression, broadening and spectral manipulation of pulses by aspatiotemporal lens, and the closure of the forbidden frequency gaps with thesubsequent opening of wavenumber bandgaps in a generalized Bragg reflector.


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Input: We consider global and gravitational lensing properties of the recentlysuggested Einstein clusters of WIMPs as galactic dark matter halos. Beingtangential pressure dominated, Einstein clusters are strongly anisotropicsystems which can describe any galactic rotation curve by specifying theanisotropy. Due to this property, Einstein clusters may be considered as darkmatter candidates. We analyse the stability of the Einstein clusters againstboth radial and non-radial pulsations, and we show that the Einstein clustersare dynamically stable. With the use of the Buchdahl type inequalities foranisotropic bodies, we derive upper limits on the velocity of the particlesdefining the cluster. These limits are consistent with those obtained fromstability considerations. The study of light deflection shows that thegravitational lensing effect is slightly smaller for the Einstein clusters, ascompared to the singular isothermal density sphere model for dark matter.Therefore lensing observations may discriminate, at least in principle, betweenEinstein cluster and other dark matter models.


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Input: The environment of high-redshift galaxies is characterized by bothwind-driven outflowing gas and gravitationally infalling streams. Toinvestigate such galaxy-IGM interplay we have generated synthetic opticalabsorption line spectra piercing the volume surrounding a starbursting analogof a Lyman Break Galaxy selected in a $z \approx 3$ output from a SPHsimulation, including a detailed treatment of mechanical feedback from winds.Distributions for several observable species (HI, CIII, CIV, SiII, SiIII, SiIV,OVI, OVII, and OVIII) have been derived by post-processing the simulationoutputs. The hot wind material is characterized by the presence ofhigh-ionization species such as OVI, OVII, and OVIII (the latter two observableonly in X-ray bands); the colder ($T<10^{5.5}$ K) infalling streams can beinstead identified by the combined presence of SiII, SiIII, and CIII opticalabsorption together with OVI that surrounds the cooler gas clumps. However,both line profile and Pixel Optical Depth analysis of the synthetic spectrashow that the intergalactic filament in which the wind-blowing galaxy isembedded produces absorption signatures that closely mimic those of the windenvironment. We conclude that may be difficult to clearly identify wind-blowinggalaxies and their complex gaseous environment at high redshift in optical QSOabsorption-line spectra based solely on the observed ion absorption patterns.


Instruction: what is the prompt that generates the input?

Input: We study the effects of frustration in an antiferromagnetic film of FCClattice with Heisenberg spin model including an Ising-like anisotropy. MonteCarlo (MC) simulations have been used to study thermodynamic properties of thefilm. We show that the presence of the surface reduces the ground state (GS)degeneracy found in the bulk. The GS is shown to depend on the surface in-planeinteraction $J_s$ with a critical value at which ordering of type I coexistswith ordering of type II. Near this value a reentrant phase is found. Variousphysical quantities such as layer magnetizations and layer susceptibilities areshown and discussed. The nature of the phase transition is also studied byhistogram technique. We have also used the Green's function (GF) method for thequantum counterpart model. The results at low-$T$ show interesting effects ofquantum fluctuations. Results obtained by the GF method at high $T$ arecompared to those of MC simulations. A good agreement is observed.


Instruction: what is the prompt that generates the input?

Input: This paper addresses the performance of bit-interleaved coded multiplebeamforming (BICMB) [1], [2] with imperfect knowledge of beamforming vectors.Most studies for limited-rate channel state information at the transmitter(CSIT) assume that the precoding matrix has an invariance property under anarbitrary unitary transform. In BICMB, this property does not hold. On theother hand, the optimum precoder and detector for BICMB are invariant under adiagonal unitary transform. In order to design a limited-rate CSIT system forBICMB, we propose a new distortion measure optimum under this invariance. Basedon this new distortion measure, we introduce a new set of centroids and employthe generalized Lloyd algorithm for codebook design. We provide simulationresults demonstrating the performance improvement achieved with the proposeddistortion measure and the codebook design for various receivers with lineardetectors. We show that although these receivers have the same performance forperfect CSIT, their performance varies under imperfect CSIT.


Instruction: what is the prompt that generates the input?

Input: We discuss a universality property of any covariant field theory inspace-time expanded around pp-wave backgrounds. According to this property thespace-time lagrangian density evaluated on a restricted set of fieldconfigurations, called universal sector, turns out to be same around all thepp-waves, even off-shell, with same transverse space and same profiles for thebackground scalars. In this paper we restrict our discussion to tensorialfields only. In the context of bosonic string theory we consider on-shellpp-waves and argue that universality requires the existence of a universalsector of world-sheet operators whose correlation functions are insensitive tothe pp-wave nature of the metric and the background gauge flux. Such resultscan also be reproduced using the world-sheet conformal field theory. We alsostudy such pp-waves in non-polynomial closed string field theory (CSFT). Inparticular, we argue that for an off-shell pp-wave ansatz with flat transversespace and dilaton independent of transverse coordinates the field redefinitionrelating the low energy effective field theory and CSFT with all the massivemodes integrated out is at most quadratic in fields. Because of thissimplification it is expected that the off-shell pp-waves can be identified onthe two sides. Furthermore, given the massless pp-wave field configurations, aniterative method for computing the higher massive modes using the CSFTequations of motion has been discussed. All our bosonic string theory analysescan be generalised to the common Neveu-Schwarz sector of superstrings.


Instruction: what is the prompt that generates the input?

Input: We report on the structural and magnetic properties of thin Ge(1-x)Mn(x)filmsgrown by molecular beam epitaxy (MBE) on Ge(001) substrates at temperatures(Tg) ranging from 80deg C to 200deg C, with average Mn contents between 1 % and11 %. Their crystalline structure, morphology and composition have beeninvestigated by transmission electron microscopy (TEM), electron energy lossspectroscopy and x-ray diffraction. In the whole range of growth temperaturesand Mn concentrations, we observed the formation of manganese richnanostructures embedded in a nearly pure germanium matrix. Growth temperaturemostly determines the structural properties of Mn-rich nanostructures. For lowgrowth temperatures (below 120deg C), we evidenced a two-dimensional spinodaldecomposition resulting in the formation of vertical one-dimensionalnanostructures (nanocolumns). Moreover we show in this paper the influence ofgrowth parameters (Tg and Mn content) on this decomposition i.e. on nanocolumnssize and density. For temperatures higher than 180deg C, we observed theformation of Ge3Mn5 clusters. For intermediate growth temperatures nanocolumnsand nanoclusters coexist. Combining high resolution TEM and superconductingquantum interference device magnetometry, we could evidence at least fourdifferent magnetic phases in Ge(1-x)Mn(x) films: (i) paramagnetic diluted Mnatoms in the germanium matrix, (ii) superparamagnetic and ferromagnetic low-Tcnanocolumns (120 K < Tc < 170 K), (iii) high-Tc nanocolumns (Tc> 400 K) and(iv) Ge3Mn5 clusters.


Instruction: what is the prompt that generates the input?

Input: By combining high-resolution (HST-WFPC2) and wide-field ground based (2.2mESO-WFI) and space (GALEX) observations, we have collected a multi-wavelengthphotometric data base (ranging from the far UV to the near infrared) of thegalactic globular cluster NGC1904 (M79). The sample covers the entire clusterextension, from the very central regions up to the tidal radius. In the presentpaper such a data set is used to study the BSS population and its radialdistribution. A total number of 39 bright ($m_{218}\le 19.5$) BSS has beendetected, and they have been found to be highly segregated in the cluster core.No significant upturn in the BSS frequency has been observed in the outskirtsof NGC 1904, in contrast to other clusters (M 3, 47 Tuc, NGC 6752, M 5) studiedwith the same technique. Such evidences, coupled with the large radius ofavoidance estimated for NGC 1904 ($r_{avoid}\sim 30$ core radii), indicate thatthe vast majority of the cluster heavy stars (binaries) has already sunk to thecore. Accordingly, extensive dynamical simulations suggest that BSS formed bymass transfer activity in primordial binaries evolving in isolation in thecluster outskirts represent only a negligible (0--10%) fraction of the overallpopulation.


Instruction: what is the prompt that generates the input?

Input: In this paper we demonstrate a technique of utilizing magnetically trappedneutral Rb-87 atoms to measure the magnitude and direction of stray electricfields emanating from surface contaminants. We apply an alternating externalelectric field that adds to (or subtracts from) the stray field in such a wayas to resonantly drive the trapped atoms into a mechanical dipole oscillation.The growth rate of the oscillation's amplitude provides information about themagnitude and sign of the stray field gradient. Using this measurementtechnique, we are able to reconstruct the vector electric field produced bysurface contaminants. In addition, we can accurately measure the electricfields generated from adsorbed atoms purposely placed onto the surface andaccount for their systematic effects, which can plague a precisionsurface-force measurement. We show that baking the substrate can reduce theelectric fields emanating from adsorbate, and that the mechanism for reductionis likely surface diffusion, not desorption.


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Input: We consider the problem of coloring the vertices of a large sparse randomgraph with a given number of colors so that no adjacent vertices have the samecolor. Using the cavity method, we present a detailed and systematic analyticalstudy of the space of proper colorings (solutions).  We show that for a fixed number of colors and as the average vertex degree(number of constraints) increases, the set of solutions undergoes several phasetransitions similar to those observed in the mean field theory of glasses.First, at the clustering transition, the entropically dominant part of thephase space decomposes into an exponential number of pure states so that beyondthis transition a uniform sampling of solutions becomes hard. Afterward, thespace of solutions condenses over a finite number of the largest states andconsequently the total entropy of solutions becomes smaller than the annealedone. Another transition takes place when in all the entropically dominantstates a finite fraction of nodes freezes so that each of these nodes isallowed a single color in all the solutions inside the state. Eventually, abovethe coloring threshold, no more solutions are available. We compute all thecritical connectivities for Erdos-Renyi and regular random graphs and determinetheir asymptotic values for large number of colors.  Finally, we discuss the algorithmic consequences of our findings. We arguethat the onset of computational hardness is not associated with the clusteringtransition and we suggest instead that the freezing transition might be therelevant phenomenon. We also discuss the performance of a simple local Walk-COLalgorithm and of the belief propagation algorithm in the light of our results.


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Input: We present the results of a high-resolution X-ray imaging study of thestellar population in the Galactic massive star-forming region RCW49 and itscentral OB association Westerlund 2. We obtained a 40 ks X-ray image of a17'x17' field using the Chandra X-ray Observatory and deep NIR images using theInfrared Survey Facility in a concentric 8'3x8'3 region. We detected 468 X-raysources and identified optical, NIR, and Spitzer Space Telescope MIRcounterparts for 379 of them. The unprecedented spatial resolution andsensitivity of the X-ray image, enhanced by optical and infrared imaging data,yielded the following results: (1) The central OB association Westerlund 2 isresolved for the first time in the X-ray band. X-ray emission is detected fromall spectroscopically-identified early-type stars in this region. (2) Most(86%) X-ray sources with optical or infrared identifications are clustermembers in comparison with a control field in the Galactic Plane. (3) A looseconstraint (2--5 kpc) for the distance to RCW49 is derived from the mean X-rayluminosity of T Tauri stars. (4) The cluster X-ray population consists oflow-mass pre--main-sequence and early-type stars as obtained from X-ray and NIRphotometry. About 30 new OB star candidates are identified. (5) We estimate acluster radius of 6'--7' based on the X-ray surface number density profiles.(6) A large fraction (90%) of cluster members are identified individually usingcomplimentary X-ray and MIR excess emission. (7) The brightest five X-raysources, two Wolf-Rayet stars and three O stars, have hard thermal spectra.


Instruction: what is the prompt that generates the input?

Input: It is known that a macroscopic quantum superposition (MQS), when it isexposed to environment, decoheres at a rate scaling with the separation of itscomponent states in phase space. This is more or less consistent with the wellknown proposition that a more macroscopic quantum state is reduced more quicklyto a classical state in general. Effects of initial mixedness, however, on thesubsequent decoherence of MQSs have been less known. In this paper, we studythe evolution of a highly mixed MQS interacting with an environment, andcompare it with that of a pure MQS having the same size of the central distancebetween its component states. Although the decoherence develops more rapidlyfor the mixed MQS in short times, its rate can be significantly suppressedafter a certain time and becomes smaller than the decoherence rate of itscorresponding pure MQS. In an optics experiment to generate a MQS, our resulthas a practical implication that nonclassicality of a MQS can be stillobservable in moderate times even though a large amount of noise is added tothe initial state.


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Input: In the conventional formulation of N=1 supersymmetry, a vector multiplet issupposed to be in the adjoint representation of a given gauge group. We presenta new formulation with a vector multiplet in the non-adjoint representation ofSO(N) gauge group. Our basic algebra is [ T^I, T^J ] = f^{I J K} T^K, [ T^I,U^i ] = - (T^I)^{i j} U^j, [ U^i, U^j ] = - (T^I)^{i j} T^I, where T^I are thegenerators of SO(N), while U^i are the new 'generators' in certain non-adjointreal representation R of SO(N). We use here the word `generator' in the broadersense of the word. Such a representation can be any real representation ofSO(N) with the positive definite metric, satisfying (T^I)^{i j} = - (T^I)^{j i}and (T^I)^{[ i j |} (T^I)^{| k ] l} \equiv 0. The first non-trivial examplesare the spinorial 8_S and conjugate spinorial 8_C representations of SO(8)consistent with supersymmetry. We further couple the system to chiralmultiplets, and show that a Higgs mechanism can give positive definite (mass)^2to the new gauge fields for U^i. We show an analogous system working with N=1supersymmetry in 10D, and thereby N=4 system in 4D interacting with extramultiplets in the representation R. We also perform superspace reformulation asan independent confirmation.


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Input: Parton showers are widely used to generate fully exclusive final statesneeded to compare theoretical models to experimental observations. While, ingeneral, parton showers give a good description of the experimental data, theprecise functional form of the probability distribution underlying the eventgeneration is generally not known. The reason is that realistic parton showersare required to conserve four-momentum at each vertex. In this paper weinvestigate in detail how four-momentum conservation is enforced in a standardparton shower and why this destroys the analytic control of the probabilitydistribution. We show how to modify a parton shower algorithm such that itconserves four-momentum at each vertex, but for which the full analytic form ofthe probability distribution is known. We then comment how this analyticcontrol can be used to match matrix element calculations with parton showers,and to estimate effects of power corrections and other uncertainties in partonshowers.


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Input: The paper is considering an opportunity for the CERN/GranSasso (CNGS)neutrino complex, concurrent time-wise with T2K and NOvA, to search fortheta_13 oscillations and CP violation. Compared with large water Cherenkov(T2K) and fine grained scintillators (NOvA), the LAr-TPC offers a higherdetection efficiency and a lower backgrounds, since virtually all channels maybe unambiguously recognized. The present proposal, called MODULAr, describes a20 kt fiducial volume LAr-TPC, following very closely the technology developedfor the ICARUS-T60o, and is focused on the following activities, for which weseek an extended international collaboration:  (1) the neutrino beam from the CERN 400 GeV proton beam and an optimised hornfocussing, eventually with an increased intensity in the framework of the LHCaccelerator improvement program;  (2) A new experimental area LNGS-B, of at least 50000 m3 at 10 km off-axisfrom the main Laboratory, eventually upgradable to larger sizes. A location isunder consideration at about 1.2 km equivalent water depth;  (3) A new LAr Imaging detector of at least 20 kt fiducial mass. Such anincrease in the volume over the current ICARUS T600 needs to be carefullyconsidered. It is concluded that a very large mass is best realised with a setof many identical, independent units, each of 5 kt, "cloning" the technology ofthe T600. Further phases may foresee extensions of MODULAr to meet futurephysics goals.  The experiment might reasonably be operational in about 4/5 years, provided anew hall is excavated in the vicinity of the Gran Sasso Laboratory and adequatefunding and participation are made available.


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Input: In this paper, we present a method to optimise rough set partition sizes, towhich rule extraction is performed on HIV data. The genetic algorithmoptimisation technique is used to determine the partition sizes of a rough setin order to maximise the rough sets prediction accuracy. The proposed method istested on a set of demographic properties of individuals obtained from theSouth African antenatal survey. Six demographic variables were used in theanalysis, these variables are; race, age of mother, education, gravidity,parity, and age of father, with the outcome or decision being either HIVpositive or negative. Rough set theory is chosen based on the fact that it iseasy to interpret the extracted rules. The prediction accuracy of equal widthbin partitioning is 57.7% while the accuracy achieved after optimising thepartitions is 72.8%. Several other methods have been used to analyse the HIVdata and their results are stated and compared to that of rough set theory(RST).


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Input: The composite grain is made up of a host silicate spheroid and graphiteinclusions. The extinction efficiencies of the composite spheroidal grains forthree axial ratios are computed using the discrete dipole approximation (DDA).The interstellar extinction curve is evaluated in the spectral region3.40--0.10$\mu m$ using the extinction efficiencies of the composite spheroidalgrains. The model extinction curves are then compared with the average observedinterstellar extinction curve. We also calculate the linear polarization forthe spheroidal composite grains at three orientation angles and find thewavelength of maximum polarization. Further, we estimate the volume extinctionfactor, an important parameter from the point of view of cosmic abundance, forthe composite grain models that reproduce the average observed interstellarextinction. The estimated abundances derived from the composite grain modelsfor both carbon and silicon are found to be lower than that are predicted bythe bare silicate/graphite grain models but these values are still higher thanthat are implied from the recent ISM values.


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Input: Classical and quantum phase transitions involve observables which arenon-analytic as functions of a controlled thermodynamical variable. As occurswith the self-consistent Fermi Golden Rule, one condition to obtain thediscontinuous behavior is the proper evaluation of a classical or quantumthermodynamic limit. We show that in presence of an environment, theoscillatory dynamics of a quantum two-level system, in analogy with a classicaldamped oscillator, can undergo a quantum dynamical phase transition to anon-oscillatory phase. This is obtained from a self-consistent solution of theGeneralized Landauer Buettiker Equations, a simplified integral form of theKeldysh formalism. I argue that working at each side of the transition impliesstanding under different paradigms in the Kuhn's sense of the word. Inconsequence, paradigms incommensurability obtains a sound mathematicaljustification as a consequence of the non-analyticity of the observables. Astrong case is made upon the need to deepen the public's intuition andunderstanding on the abrupt transition from static to dynamical frictionregimes.  Keywords: Self Consistent Fermi Golden Rule, Paradigm Shift, QuantumDynamical Phase Transition, Decoherence, Energy-time Wigner Function,Dissipative Two-level system, Keldysh Formalisma, GeneralizedLandauer-Buettiker Equations, Loschmidt Echo, Mesoscopic Echo, Spin Dynamics,Solid State NMR, Dynamical Quantum Zeno Effect, Liquid Crystal NMR.


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Input: Swift triggered on a precursor to the main burst of GRB 061121 (z=1.314),allowing observations to be made from the optical to gamma-ray bands. Manyother telescopes, including Konus-Wind, XMM-Newton, ROTSE and the FaulkesTelescope North, also observed the burst. The gamma-ray, X-ray and UV/opticalemission all showed a peak ~75s after the trigger, although the optical andX-ray afterglow components also appear early on - before, or during, the mainpeak. Spectral evolution was seen throughout the burst, with the promptemission showing a clear positive correlation between brightness and hardness.The Spectral Energy Distribution (SED) of the prompt emission, stretching from1eV up to 1MeV, is very flat, with a peak in the flux density at ~1keV. Theoptical-to-X-ray spectra at this time are better fitted by a broken, ratherthan single, power-law, similar to previous results for X-ray flares. The SEDshows spectral hardening as the afterglow evolves with time. This behaviourmight be a symptom of self-Comptonisation, although circumstellar densitiessimilar to those found in the cores of molecular clouds would be required. Theafterglow also decays too slowly to be accounted for by the standard models.Although the precursor and main emission show different spectral lags, both areconsistent with the lag-luminosity correlation for long bursts. GRB 061121 isthe instantaneously brightest long burst yet detected by Swift. Using acombination of Swift and Konus-Wind data, we estimate an isotropic energy of2.8x10^53 erg over 1keV - 10MeV in the GRB rest frame. A probable jet break isdetected at ~2x10^5s, leading to an estimate of ~10^51 erg for thebeaming-corrected gamma-ray energy.


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Input: This paper presents the development of a new software in order to manageobjects, robots and mannequins in using the possibilities given by the hapticfeedback of the Phantom desktop devices. The haptic device provides 6positional degree of freedom sensing but three degrees force feedback. Thissoftware called eM-Virtual Desktop is integrated in the Tecnomatix's solutioncalled eM-Workplace. The eM-Workplace provides powerful solutions for planningand designing of complex assembly facilities, lines and workplaces. In thedigital mockup context, the haptic interfaces can be used to reduce thedevelopment cycle of products. Three different loops are used to manage thegraphic, the collision detection and the haptic feedback according to theirsown frequencies. The developed software is currently tested in industrialcontext by a European automotive constructor.


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Input: In spectra of many Seyfert galaxies there is a wide emission line of Fe$K_\alpha$. The line profile with two maxima supposes that the line emerges ininnermost regions of an accretion disk around a black hole, hence, it isnecessary to take into account General Relativity (GR) effects. In order todetermine GR processes which occur in active galactic nuclei (AGN) an inverseproblem of reconstructing the accreting system parameters from the line profilehas to be solved quickly. In this paper we present a numerical approximation ofthe emission line Fe $K_\alpha$ with analytical functions. The approximation isaccomplished for a range of the disk radial coordinate $r$ and the angle$\theta$ between line of sight and perpendicular to the disk and allows one todecrease computing time by $10^6$ times in certain astrophysical problemstaking into account all GR effects. The approximation results are available inthe Internet at http://www.iki.rssi.ru/people/repin/approx


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Input: Effective Field Theory(EFT) is, the unique, model independent and systematiclow-energy version of QCD for processes involving momenta below the pion mass.A low-energy photo-nuclear observable in three-body systems, photonpolarization parameter at thermal neutron energies is calculated by usingpionless EFT up to next-to-next to leading order(N$^2$LO). In order to make acomparative study of this model, we compared our results for photonpolarization parameter with the realistic Argonne $v_{18}$ two-nucleon andUrbana IX or Tucson-Melbourne three-nucleon interactions. Three-body currentsgive small but significant contributions to some of the observables in theneutron-deuteron radiative capture cross section at thermal neutron energies.In this formalism the three-nucleon forces are needed up to N$^2$LO for cut-offindependent results. Our result converges order by order in low energyexpansion and also cut-off independent at this order.


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Input: A game-theoretic framework is used to study the effect of constellation sizeon the energy efficiency of wireless networks for M-QAM modulation. Anon-cooperative game is proposed in which each user seeks to choose itstransmit power (and possibly transmit symbol rate) as well as the constellationsize in order to maximize its own utility while satisfying its delayquality-of-service (QoS) constraint. The utility function used here measuresthe number of reliable bits transmitted per joule of energy consumed, and isparticularly suitable for energy-constrained networks. The best-responsestrategies and Nash equilibrium solution for the proposed game are derived. Itis shown that in order to maximize its utility (in bits per joule), a user mustchoose the lowest constellation size that can accommodate the user's delayconstraint. Using this framework, the tradeoffs among energy efficiency, delay,throughput and constellation size are also studied and quantified. The effectof trellis-coded modulation on energy efficiency is also discussed.


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Input: The prediction of the three-dimensional native structure of proteins from theknowledge of their amino acid sequence, known as the protein folding problem,is one of the most important yet unsolved issues of modern science. Since theconformational behaviour of flexible molecules is nothing more than a complexphysical problem, increasingly more physicists are moving into the study ofprotein systems, bringing with them powerful mathematical and computationaltools, as well as the sharp intuition and deep images inherent to the physicsdiscipline. This work attempts to facilitate the first steps of such atransition. In order to achieve this goal, we provide an exhaustive account ofthe reasons underlying the protein folding problem enormous relevance andsummarize the present-day status of the methods aimed to solving it. We alsoprovide an introduction to the particular structure of these biologicalheteropolymers, and we physically define the problem stating the assumptionsbehind this (commonly implicit) definition. Finally, we review the 'specialflavor' of statistical mechanics that is typically used to study theastronomically large phase spaces of macromolecules. Throughout the whole work,much material that is found scattered in the literature has been put togetherhere to improve comprehension and to serve as a handy reference.


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Input: If the recent PVLAS results on polarization changes of a linearly polarizedlaser beam passing through a magnetic field are interpreted by an axion-likeparticle, it is almost certain that it is not a standard QCD axion. Consideringthis, we study the general effective interactions of photons with spin-zeroparticles without restricting the latter to be a pseudo-scalar or a scalar,i.e., a parity eigenstate. At the lowest order in effective field theory, thereare two dimension-5 interactions, each of which has previously been treatedseparately for a pseudo-scalar or a scalar particle. By following the evolutionin an external magnetic field of the system of spin-zero particles and photons,we compute the changes in light polarization and the transition probability fortwo experimental set-ups: one-way propagation and round-trip propagation. Whilethe first may be relevant for astrophysical sources of spin-zero particles, thesecond applies to laboratory optical experiments like PVLAS. In the one-waypropagation, interesting phenomena can occur for special configurations ofpolarization where, for instance, transition occurs but light polarization doesnot change. For the round-trip propagation, however, the standard results ofpolarization changes for a pseudoscalar or a scalar are only modified by afactor that depends on the relative strength of the two interactions.


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Input: It is proposed that radiation belts similar to the ones in the planetarymagnetosphere can exist for a pulsar with a relatively long period and a strongmagnetic field. In the belts located in the closed field line region near thelight cylinder relativistic pairs are trapped and maintained at a densitysubstantially higher than the local Goldreich-Julian corotation density. Thetrapped plasma can be supplied and replenished by either direct injection ofrelativistic pairs from acceleration of externally-supplied particles in adormant outer gap or in situ ionization of the accreted neutral material in thetrapping region. The radiation belts can be disrupted by waves that are excitedin the region as the result of plasma instabilities or emitted from the surfacedue to starquakes or stellar oscillations. The disruption can cause anintermittent particle precipitation toward the star producing radio bursts. Itis suggested that such bursts may be seen as rotating radio transients (RRATs).


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Input: We present the results of photoionization modeling of nine weak MgII (W_r<0.3Ang) quasar absorption line systems with redshifts 1.4<z<2.4 obtained with theUltraviolet and Visual Echelle Spectrograph on the Very Large Telescope. Thesesystems have been chosen because they provide access to a regime of red-shiftspace that previous weak MgII studies have not looked at. The densities,metallicities, Doppler parameters, and column densities of these systems arecompared to those of other weak MgII systems at lower redshift. There is nosignificant statistical variation in the properties of the absorbers over theredshift range 0.4<z<2.4. The number density per unit redshift is known todecrease for weak MgII absorbers between z~1 and z~2 by a greater amount thanpredicted from cosmological effects and changes in the extragalactic ionizingbackground alone. We suggest that, because the physical properties of theabsorber population are not seen to change significantly across this range,that the evolution in dN/dz is due to a decrease in the activity that givesrise to weak MgII absorption, and not due to a change in the processes thatform weak MgII absorbers. The presence of separate, but aligned (in velocity)low and high density clouds in all single cloud weak MgII absorbers provides animportant diagnostic of their geometry. We discuss possible origins in dwarfgalaxies and in extragalactic analogs to high velocity clouds.


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Input: We consider a two-brane system in a five-dimensional anti-de Sitterspacetime. We study particle creation due to the motion of the physical branewhich first approaches the second static brane (contraction) and then recedesfrom it(expansion). The spectrum and the energy density of the generatedgravitons are calculated. We show that the massless gravitons have a bluespectrum and that their energy density satisfies the nucleosynthesis bound withvery mild constraints on the parameters. We also show that the Kaluza-Kleinmodes cannot provide the dark matter in an anti-de-Sitter braneworld. However,for natural choices of parameters, backreaction from the Kaluza-Klein gravitonsmay well become important. The main findings of this work have been publishedin the form of a Letter [R. Durrer and M. Ruser, Phys. Rev. Lett. 99, 071601(2007), arXiv:0704.0756].


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Input: We report the discovery of a substellar-mass companion to the K0-giant HD17092 with the Hobby-Eberly Telescope. In the absence of any correlation of theobserved 360-day periodicity with the standard indicators of stellar activity,the observed radial velocity variations are most plausibly explained in termsof a Keplerian motion of a planetary-mass body around the star. With theestimated stellar mass of 2.3Msun, the minimum mass of the planet is 4.6MJ. Theplanet's orbit is characterized by a mild eccentricity of e=0.17 and asemi-major axis of 1.3 AU. This is the tenth published detection of a planetarycompanion around a red giant star. Such discoveries add to our understanding ofplanet formation around intermediate-mass stars and they provide dynamicalinformation on the evolution of planetary systems around post-main sequencestars.


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Input: We calculate the thermal conductivity of electrons and muons kappa_{e-mu}produced owing to electromagnetic interactions of charged particles in neutronstar cores and show that these interactions are dominated by the exchange oftransverse plasmons (via the Landau damping of these plasmons innonsuperconducting matter and via a specific plasma screening in the presenceof proton superconductivity). For normal protons, the Landau damping stronglyreduces kappa_{e-mu} and makes it temperature independent. Protonsuperconductivity suppresses the reduction and restores the Fermi-liquidbehavior kappa_{e-mu} ~ 1/T. Comparing with the thermal conductivity ofneutrons kappa_n, we obtain kappa_{e-mu}> kappa_n for T>2 GK in normal matterand for any T in superconducting matter with proton critical temperaturesT_c>3e9 K. The results are described by simple analytic formulae.


Instruction: what is the prompt that generates the input?

Input: In this paper we obtain general integral formulas for probabilities in theasymmetric simple exclusion process (ASEP) on the integer lattice with nearestneighbor hopping rates p to the right and q=1-p to the left. For the most partwe consider an N-particle system but for certain of these formulas we can takethe limit as N goes to infinity. First we obtain, for the N-particle system, aformula for the probability of a configuration at time t, given the initialconfiguration. For this we use Bethe Ansatz ideas to solve the master equation,extending a result of Schuetz for the case N=2. The main results of the paper,derived from this, are integral formulas for the probability, for given initialconfiguration, that the m'th left-most particle is at x at time t. In one ofthese formulas we can take the limit as N goes to infinity, and it gives theprobability for an infinite system where the initial configuration is boundedon one side. For the special case of the totally asymmetric simple exclusionprocess (TASEP) our formulas reduce to the known ones.


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Input: This paper investigates the many-to-one throughput capacity (and by symmetry,one-to-many throughput capacity) of IEEE 802.11 multi-hop networks. It hasgenerally been assumed in prior studies that the many-to-one throughputcapacity is upper-bounded by the link capacity L. Throughput capacity L is notachievable under 802.11. This paper introduces the notion of "canonicalnetworks", which is a class of regularly-structured networks whose capacitiescan be analyzed more easily than unstructured networks. We show that thethroughput capacity of canonical networks under 802.11 has an analytical upperbound of 3L/4 when the source nodes are two or more hops away from the sink;and simulated throughputs of 0.690L (0.740L) when the source nodes are manyhops away. We conjecture that 3L/4 is also the upper bound for generalnetworks. When all links have equal length, 2L/3 can be shown to be the upperbound for general networks. Our simulations show that 802.11 networks withrandom topologies operated with AODV routing can only achieve throughputs farbelow the upper bounds. Fortunately, by properly selecting routes near thegateway (or by properly positioning the relay nodes leading to the gateway) tofashion after the structure of canonical networks, the throughput can beimproved significantly by more than 150%. Indeed, in a dense network, it isworthwhile to deactivate some of the relay nodes near the sink judiciously.


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Input: We discuss the possibility to study oscillations of atmospheric neutrinos inthe ATLAS experiment at CERN. Due to the large total detector mass, asignificant number of events is expected, and during the shutdown phases of theLHC, reconstruction of these events will be possible with very good energy andangular resolutions, and with charge identification. We argue that 500 livedays of neutrino running could be achieved, and that a total of ~160 contained\nu_\mu events and ~360 upward going muons could be collected during this time.Despite the low statistics, the excellent detector resolution will allow for anunambiguous confirmation of atmospheric neutrino oscillations and formeasurements of the leading oscillation parameters. Though our detailedsimulations show that the sensitivity of ATLAS is worse than that of dedicatedneutrino experiments, we demonstrate that more sophisticated detectors, e.g. atthe ILC, could be highly competitive with upcoming superbeam experiments, andmight even give indications for the mass hierarchy and for the value oftheta-13.


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Input: Medvedev and Melott (2007) have suggested that periodicity in fossilbiodiversity may be induced by cosmic rays which vary as the Solar Systemoscillates normal to the galactic disk. We re-examine the evidence for a 62million year (Myr) periodicity in biodiversity throughout the Phanerozoichistory of animal life reported by Rohde & Mueller (2005), as well as relatedquestions of periodicity in origination and extinction. We find that the signalis robust against variations in methods of analysis, and is based onfluctuations in the Paleozoic and a substantial part of the Mesozoic.Examination of origination and extinction is somewhat ambiguous, with resultsdepending upon procedure. Origination and extinction intensity as defined by RMmay be affected by an artifact at 27 Myr in the duration of stratigraphicintervals. Nevertheless, when a procedure free of this artifact is implemented,the 27 Myr periodicity appears in origination, suggesting that the artifact mayultimately be based on a signal in the data. A 62 Myr feature appears inextinction, when this same procedure is used. We conclude that evidence for aperiodicity at 62 Myr is robust, and evidence for periodicity at approximately27 Myr is also present, albeit more ambiguous.


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Input: We investigate faint radio emission from low- to high-luminosity ActiveGalactic Nuclei (AGN) selected from the Sloan Digital Sky Survey (SDSS). Theirradio properties are inferred by co-adding large ensembles of radio imagecut-outs from the FIRST survey, as almost all of the sources are individuallyundetected. We correlate the median radio flux densities against a range ofother sample properties, including median values for redshift, [OIII]luminosity, emission line ratios, and the strength of the 4000A break. Wedetect a strong trend for sources that are actively undergoing star-formationto have excess radio emission beyond the ~10^28 ergs/s/Hz level found forsources without any discernible star-formation. Furthermore, this additionalradio emission correlates well with the strength of the 4000A break in theoptical spectrum, and may be used to assess the age of the star-formingcomponent. We examine two subsamples, one containing the systems with emissionline ratios most like star-forming systems, and one with the sources that havecharacteristic AGN ratios. This division also separates the mechanismresponsible for the radio emission (star-formation vs. AGN). For both cases wefind a strong, almost identical, correlation between [OIII] and radioluminosity, with the AGN sample extending toward lower, and the star-formationsample toward higher luminosities. A clearer separation between the twosubsamples is seen as function of the central velocity dispersion of the hostgalaxy. For systems with similar redshifts and velocity dispersions, thestar-formation subsample is brighter than the AGN in the radio by an order ofmagnitude. This underlines the notion that the radio emission in star-formingsystems can dominate the emission associated with the AGN.


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Input: We point out the evident errors in statistical analysis of the data,performed by Klapdor-Kleingrothaus et al in recently published paper toestablish a limit on the stability of electron with respect to the decay into$\nu+\gamma$. We performed the reestimation of the sensitivity of theexperimental setups to the 256 keV gamma emitted in the hypothetical electrondecay, and show that in [1] the limits on the electron stability and chargenonconservation parameter $\epsilon_{e\nu\gamma}^{2}$ are overestimated by atleast a factor of 5. We have revealed evident errors in the statisticalanalysis, performed by Klapdor-Kleingrothaus et al in a recently publishedpaper [1] to establish a limit on the stability of electron with respect to thedecay into $\nu+\gamma$. The performed reestimation of the sensitivity of theexperimental setups to the 256 keV gamma emitted in the hypothetical electrondecay, has shown that the limits on the electron stability and chargenonconservation parameter $\epsilon_{e\nu\gamma}^{2}$ presented in [1], havebeen overestimated by at least a factor of 5.


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Input: Cooperative diversity systems are wireless communication systems designed toexploit cooperation among users to mitigate the effects of multipath fading. Infairly general conditions, it has been shown that these systems can achieve thediversity order of an equivalent MISO channel and, if the node geometrypermits, virtually the same outage probability can be achieved as that of theequivalent MISO channel for a wide range of applicable SNR. However, much ofthe prior analysis has been performed under the assumption of perfect timingand frequency offset synchronization. In this paper, we derive the estimationbounds and associated maximum likelihood estimators for frequency offsetestimation in a cooperative communication system. We show the benefit ofadaptively tuning the frequency of the relay node in order to reduce estimationerror at the destination. We also derive an efficient estimation algorithm,based on the correlation sequence of the data, which has mean squared errorclose to the Cramer-Rao Bound.


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Input: We present an atlas of the central regions of 75 Seyfert galaxies imaged inthe near-UV with the Advanced Camera for Surveys of the Hubble Space Telescopeat an average resolution of ~10pc. These data complement archival highresolution data from the Space Telescope at optical and near-IR wavelengths,creating an extremely valuable dataset for astronomers with a broad range ofscientific interests. Our goal is to investigate the nature of the near-UVlight in these objects, its relation to the circumnuclear starburst phenomenon,and the connection of this to the evolution and growth of the galaxy bulge andcentral black hole. In this paper, we describe the near-UV morphology of theobjects and characterize the near-UV emission. We estimate the size and theluminosity of the emitting regions and extract the luminosity profile. We alsodetermine the presence of unresolved compact nuclei. In addition, thecircumnuclear stellar cluster population is identified, and the contribution ofthe stellar clusters to the total light, at this wavelength, is estimated. Thesize of the sample allows us to draw robust statistical conclusions. We findthat {Seyfert 1} galaxies are completely dominated by its bright and compactnucleus, that remains point-like at this resolution, while we find almost nounresolved nucleus in Seyfert 2. The Seyfert types 1 and 2 are quite segregatedin an asymmetry vs compactness plot. Stellar clusters are found somewhat morefrequently in Sy2 (in ~70% of the galaxies) than in Sy1 (~57%), and contributemore to the total light in Sy2, but this two differences seem to be mostly dueto the large contribution of the compact nucleus in Sy1, as the luminositydistribution of the clusters is similar in both Sy types.


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Input: The effect of fractal normal-phase clusters on vortex dynamics in apercolative superconductor is considered. The superconductor containspercolative superconducting cluster carrying a transport current and clustersof a normal phase, acting as pinning centers. A prototype of such a structureis YBCO film, containing clusters of columnar defects, as well as the BSCCO/Agsheathed tape, which is of practical interest for wire fabrication. Transitionof the superconductor into a resistive state corresponds to the percolationtransition from a pinned vortex state to a resistive state when the vorticesare free to move. The dependencies of the free vortex density on the fractaldimension of the cluster boundary as well as the resistance on the transportcurrent are obtained. It is revealed that a mixed state of the vortex glasstype is realized in the superconducting system involved. The current-voltagecharacteristics of superconductors containing fractal clusters are obtained andtheir features are studied.


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Input: Several years ago, we proposed a modification of the Standard Model, in whichthe Higgs sector was stabilized by the addition of higher derivative operators,similar to Lee-Wick Electrodynamics. We studied this theory extensively, bothusing continuum Hamiltonian and path integral methods. We also reporteddetailed lattice studies of the higher derivative Higgs sector. In view of somerecent revived interest in our original idea, we are providing here ourextensive notes from the time period on this topic. The key results werealready published in our papers at that time. The many additional details thatwe make available here were previously available only in Chuan Liu's UCSD Ph.D.thesis (1994). Very recently, our idea has been revived by other groups. Inview of the renewed interest, and to perhaps correct some misconceptions in theliterature, we are here making our original extensive notes available to thewider community.


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Input: The composition of the eta and eta' mesons has long been a source ofdiscussion and is of current interest with new experimental results appearing.We investigate what can be learnt from a number of different processes: V to Pgamma and P to V gamma (V and P are light vector and pseudoscalar mesonsrespectively), P to gamma gamma, J/psi,psi' to P gamma, J/psi,psi' to P V, andchi_{c0,2} to PP. These constrain the eta-eta' mixing angle to a consistentvalue, phi approx 42 degrees; we find that the c cbar components are lesssim 5%in amplitude. We also find that, while the data hint at a small gluoniccomponent in the eta', the conclusions depend sensitively on unknown formfactors associated with exclusive dynamics. In addition, we predict BR(psi' toeta' gamma) approx 1 10^{-5} and BR(chi_{c0} to eta eta') approx 2 10^{-5} - 110^{-4}. We provide a method to test the mixing using chi_{c2} to eta eta, eta'eta', and eta eta' modes and make some general observations on chi_{c0,2}decays. We also survey the semileptonic and hadronic decays of bottom andcharmed mesons and find some modes where the mixing angle can be extractedcleanly with the current experimental data, some where more data will allowthis, and some where a more detailed knowledge of the different amplitudes isrequired.


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Input: Although powers of the Young-Jucys-Murphya elements X_i = (1 i) + ... +(i-1i), i = 1, ..., n, in the symmetric group S_n acting on {1, ...,n} do not liein the centre of the group algebra of S_n, we show that transitive powers,namely the sum of the contributions from elements that act transitively on {1,>...,n}, are central. We determine the coefficients, which we call starfactorization numbers, that occur in the resolution of transitive powers withrespect to the class basis of the centre of S_n, and show that they have apolynomiality property. These centrality and polynomiality properties haveseemingly unrelated consequences. First, they answer a question raised by Pakabout reduced decompositions; second, they explain and extend the beautifulsymmetry result discovered by Irving and Rattan; and thirdly, we relate thepolynomiality to an existing polynomiality result for a class of double Hurwitznumbers associated with branched covers of the sphere, which therefore suggeststhat there may be an ELSV-type formula associated with the star factorizationnumbers.


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Input: In this paper we introduce a variant of pushdown dimension called boundedpushdown (BPD) dimension, that measures the density of information contained ina sequence, relative to a BPD automata, i.e. a finite state machine equippedwith an extra infinite memory stack, with the additional requirement that everyinput symbol only allows a bounded number of stack movements. BPD automata area natural real-time restriction of pushdown automata. We show that BPDdimension is a robust notion by giving an equivalent characterization of BPDdimension in terms of BPD compressors. We then study the relationships betweenBPD compression, and the standard Lempel-Ziv (LZ) compression algorithm, andshow that in contrast to the finite-state compressor case, LZ is not universalfor bounded pushdown compressors in a strong sense: we construct a sequencethat LZ fails to compress signicantly, but that is compressed by at least afactor 2 by a BPD compressor. As a corollary we obtain a strong separationbetween finite-state and BPD dimension.


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Input: We consider position measurements using the cross-correlated output of twotunnel junction position detectors. Using a fully quantum treatment, wecalculate the equation of motion for the density matrix of the coupleddetector-detector-mechanical oscillator system. After discussing the presenceof a bound on the peak-to-background ratio in a position measurement using asingle detector, we show how one can use detector cross correlations toovercome this bound. We analyze two different possible experimentalrealizations of the cross correlation measurement and show that in both casesthe maximum cross-correlated output is obtained when using twin detectors andapplying equal bias to each tunnel junction. Furthermore, we show how thedouble-detector setup can be exploited to drastically reduce the addeddisplacement noise of the oscillator.


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Input: The common wisdom that the phonon mechanism of electron pairing in theweak-coupling Bardeen-Cooper-Schrieffer (BCS) superconductors leads toconventional s-wave Cooper pairs is revised. An inevitable anisotropy of soundvelocity in crystals makes the phonon-mediated attraction of electronsnon-local in space providing unconventional Cooper pairs with a nonzero orbitalmomentum in a wide range of electron densities. As a result of this anisotropyquasi-two dimensional charge carriers undergo a quantum phase transition froman unconventional d-wave superconducting state to a conventional s-wavesuperconductor with more carriers per unit cell. In the oppositestrong-coupling regime rotational symmetry breaking appears as a result of areduced Coulomb repulsion between unconventional bipolarons dismissing therebysome constraints on unconventional pairing in the Bose-Einstein condensation(BEC) limit. The conventional phonons, and not superexchange, are shown to beresponsible for the d-wave symmetry of cuprate superconductors, where theon-site Coulomb repulsion is large.


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Input: It has been claimed that the observed magnitude of the vacuum energy densityis consistent with the distribution predicted in anthropic models, in which anensemble of universes is assumed. This calculation is revisited, without makingthe assumption that the CMB temperature is known, and considering in detail thepossibility of a recollapsing universe. New accurate approximations for thegrowth of perturbations and the mass function of dark haloes are presented.Structure forms readily in the recollapsing phase of a model with negativeLambda, so collapse fraction alone cannot forbid Lambda from being large andnegative. A negative Lambda is disfavoured only if we assume that formation ofobservers can be neglected once the recollapsing universe has heated to T > 8K. For the case of positive Lambda, however, the current universe does occupy aextremely typical position compared to the predicted distribution on theLambda-T plane. Contrasting conclusions can be reached if anthropic argumentsare applied to the curvature of the universe, and we discuss the falsifiabilityof this mode of anthropic reasoning.


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Input: We have used the Very Large Array (VLA) to search for radio emission from theglobular cluster G1 (Mayall-II) in M31. G1 has been reported by Gebhardt et al.to contain an intermediate-mass black hole (IMBH) with a mass of ~2 x 10^4solar masses. Radio emission was detected within an arcsecond of the clustercenter with an 8.4 GHz power of 2 x 10^{15} W/Hz. The radio/X-ray ratio of G1is a few hundred times higher than that expected for a high-mass X-ray binaryin the cluster center, but is consistent with the expected value for accretiononto an IMBH with the reported mass. A pulsar wind nebula is also a possiblecandidate for the radio and X-ray emission from G1; future high-sensitivityVLBI observations might distinguish between this possibility and an IMBH. Ifthe radio source is an IMBH, and similar accretion and outflow processes occurfor hypothesized ~ 1000-solar-mass black holes in Milky Way globular clusters,they are within reach of the current VLA and should be detectable easily by theExpanded VLA when it comes on line in 2010.


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Input: We revisit the model of a system made up of a Brownian quantum oscillatorunder the influence of an external classical force and linearly coupled to anenvironment made up of many quantum oscillators at zero or finite temperature.We show that the HPZ master equation for the reduced density matrix derivedearlier [B.L. Hu, J.P. Paz, Y. Zhang, Phys. Rev. D 45, 2843 (1992)] withcoefficients obtained from solutions of integro-differential equations canassume closed functional forms for a fairly general class of spectral densitiesof the environment at arbitrary temperature and coupling strength. As anillustration of these new results we solve the corresponding master equationand calculate, among other physical quantities, the uncertainty function whoselate time behavior can be obtained fully. This produces a formula forinvestigating the standard quantum limit which is central to addressing manytheoretical issues in macroscopic quantum phenomena and experimental concernsrelated to low temperature precision measurements. We find that any initialstate always settles down to a Gaussian density matrix whose covariance isdetermined by the thermal reservoir and whose mean is determined by theexternal force. For more general spectra we show that the solution of themaster equation can be reduced to solving for the motion of a classicalparametric oscillator with parametric frequency determined by the unsolved formaster equation coefficients. States in these systems experience evolution thatis parametrically similar to the simpler evolution explicitly determined for inthe case of Laurent-series spectra.


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Input: We present a theoretical study of the interplay between cyclotron motion andspin splitting of charge carriers in solids. While many of our results applymore generally, we focus especially on discussing the Rashba model describingelectrons in the conduction band of asymmetric semiconductor heterostructures.Appropriate semiclassical limits are distinguished that describe varioussituations of experimental interest. Our analytical fomulae, which take fullaccount of Zeeman splitting, are used to analyse recent magnetic-focusing data.Surprisingly, it turns out that the Rashba effect can dominate the splitting ofcyclotron orbits even when the Rashba and Zeeman spin-splitting energies are ofthe same order. We also find that the origin of spin-dependent cyclotron motioncan be traced back to Zitterbewegung-like oscillatory dynamics of chargecarriers from spin-split bands. The relation between the two phenomena isdiscussed, and we estimate the effect of Zitterbewegung-related corrections tothe charge carriers' canonical position.


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Input: The transition between the low density groups of T Tauri stars and the highdensity clusters around massive stars occurs in the intermediate-mass (IM)range (M$_*$$\sim$2--8 M$_\odot$). High spatial resolution studies of IM youngstellar objects (YSO) can provide important clues to understand the clusteringin massive star forming regions.  Aims: Our aim is to search for clustering in IM Class 0 protostars. The highspatial resolution and sensitivity provided by the new A configuration of thePlateau de Bure Interferometer (PdBI) allow us to study the clustering in thesenearby objects.  Methods: We have imaged three IM Class 0 protostars (Serpens-FIRS 1, IC 1396N, CB 3) in the continuum at 3.3 and 1.3mm using the PdBI. The sources havebeen selected with different luminosity to investigate the dependence of theclustering process on the luminosity of the source.  Results: Only one millimeter (mm) source is detected towards the lowluminosity source Serpens--FIRS 1. Towards CB 3 and IC1396 N, we detect twocompact sources separated by $\sim$0.05 pc. The 1.3mm image of IC 1396 N, whichprovides the highest spatial resolution, reveal that one of these cores issplitted in, at least, three individual sources.


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Input: The topological insulator is an electronic phase stabilized by spin-orbitcoupling that supports propagating edge states and is not adiabaticallyconnected to the ordinary insulator. In several ways it is a spin-orbit-inducedanalogue in time-reversal-invariant systems of the integer quantum Hall effect(IQHE). This paper studies the topological insulator phase in disorderedtwo-dimensional systems, using a model graphene Hamiltonian introduced by Kaneand Mele as an example. The nonperturbative definition of a topologicalinsulator given here is distinct from previous efforts in that it involvesboundary phase twists that couple only to charge, does not refer to edgestates, and can be measured by pumping cycles of ordinary charge. In thisdefinition, the phase of a Slater determinant of electronic states isdetermined by a Chern parity analogous to Chern number in the IQHE case.Numerically we find, in agreement with recent network model studies, that thedirect transition between ordinary and topological insulators that occurs inband structures is a consequence of the perfect crystalline lattice.Generically these two phases are separated by a metallic phase, which isallowed in two dimensions when spin-orbit coupling is present. The sameapproach can be used to study three-dimensional topological insulators.


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Input: The groups G_{k,1} of Richard Thompson and Graham Higman can be generalizedin a natural way to monoids, that we call M_{k,1}, and to inverse monoids,called Inv_{k,1}; this is done by simply generalizing bijections to partialfunctions or partial injective functions. The monoids M_{k,1} have connectionswith circuit complexity (studied in another paper). Here we prove that M_{k,1}and Inv_{k,1} are congruence-simple for all k. Their Green relations J and Dare characterized: M_{k,1} and Inv_{k,1} are J-0-simple, and they have k-1non-zero D-classes. They are submonoids of the multiplicative part of the Cuntzalgebra O_k. They are finitely generated, and their word problem over anyfinite generating set is in P. Their word problem is coNP-complete over certaininfinite generating sets.  Changes in this version: Section 4 has been thoroughly revised, and errorshave been corrected; however, the main results of Section 4 do not change.Sections 1, 2, and 3 are unchanged, except for the proof of Theorem 2.3, whichwas incomplete; a complete proof was published in the Appendix of reference[6], and is also given here.


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Input: Community structure is an important property of complex networks. Anautomatic discovery of such structure is a fundamental task in manydisciplines, including sociology, biology, engineering, and computer science.Recently, several community discovery algorithms have been proposed based onthe optimization of a quantity called modularity (Q). However, the problem ofmodularity optimization is NP-hard, and the existing approaches often sufferfrom prohibitively long running time or poor quality. Furthermore, it has beenrecently pointed out that algorithms based on optimizing Q will have aresolution limit, i.e., communities below a certain scale may not be detected.In this research, we first propose an efficient heuristic algorithm, Qcut,which combines spectral graph partitioning and local search to optimize Q.Using both synthetic and real networks, we show that Qcut can find highermodularities and is more scalable than the existing algorithms. Furthermore,using Qcut as an essential component, we propose a recursive algorithm, HQcut,to solve the resolution limit problem. We show that HQcut can successfullydetect communities at a much finer scale and with a higher accuracy than theexisting algorithms. Finally, we apply Qcut and HQcut to study aprotein-protein interaction network, and show that the combination of the twoalgorithms can reveal interesting biological results that may be otherwiseundetectable.


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Input: The description of the statistical properties of dust emission givesimportant constraints on the physics of the interstellar medium but it is alsoa useful way to estimate the contamination of diffuse interstellar emission inthe cases where it is considered a nuisance. The main goals of this analysis ofthe power spectrum and non-Gaussian properties of 100 micron dust emission are1) to estimate the power spectrum of interstellar matter density in threedimensions, 2) to review and extend previous estimates of the cirrus noise dueto dust emission and 3) to produce simulated dust emission maps that reproducethe observed statistical properties. The main results are the following. 1) Thecirrus noise level as a function of brightness has been previouslyoverestimated. It is found to be proportional to <I> instead of <I>^1.5, where<I> is the local average brightness at 100 micron. This scaling is inaccordance with the fact that the brightness fluctuation level observed at agiven angular scale on the sky is the sum of fluctuations of increasingamplitude with distance on the line of sight. 2) The spectral index of dustemission at scales between 5 arcmin and 12.5 degrees is <gamma>=-2.9 on averagebut shows significant variations over the sky. Bright regions havesystematically steeper power spectra than diffuse regions. 3) The skewness andkurtosis of brightness fluctuations is high, indicative of strongnon-Gaussianity. 4) Based on our characterization of the 100 micron powerspectrum we provide a prescription of the cirrus confusion noise as a functionof wavelength and scale. 5) Finally we present a method based on a modificationof Gaussian random fields to produce simulations of dust maps which reproducethe power spectrum and non-Gaussian properties of interstellar dust emission.


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Input: We have investigated a closed system of equations for the quark propagator,obtained earlier within our general approach to QCD at low energies. It impliesquark confinement (the quark propagator has no pole, indeed), as well as thedynamical breakdown of chiral symmetry (a chiral symmetry preserving solutionis forbidded). This system can be solved exactly in the chiral limit. We haveestablished the space of the smooth test functions (consisting of the Green'sfunctions for the quark propagator and the corresponding quark-gluon vertex) inwhich our generalized function (the confining gluon propagator) becomes acontinuous linear functional. It is a linear topological space $K(c)$ of theinfinitely differentiable functions (with respect to the dimensionless momentumvariable $x$), having compact support in the region $x \leq c$. We develop ananalytical formalism, the so-called chiral perturbtion theory at thefundamental quark level, which allows one to find explicit solution for thequark propagator in powers of the light quark masses. We also develop ananalytical formalism, which allows one to find the solution for the quarkpropagator in the inverse powers of the heavy quark masses. It justifies theuse for the heavy quark propagator its free counterpart up to terms of theorder $1/m_Q^3$, where $m_Q$ is the heavy quark mass. So this solutionautomatically possesses the heavy quark spin-flavor symmetry.


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Input: In this paper we consider module-composed graphs, i.e. graphs which can bedefined by a sequence of one-vertex insertions v_1,...,v_n, such that theneighbourhood of vertex v_i, 2<= i<= n, forms a module (a homogeneous set) ofthe graph defined by vertices v_1,..., v_{i-1}.  We show that module-composed graphs are HHDS-free and thus homogeneouslyorderable, weakly chordal, and perfect. Every bipartite distance hereditarygraph, every (co-2C_4,P_4)-free graph and thus every trivially perfect graph ismodule-composed. We give an O(|V_G|(|V_G|+|E_G|)) time algorithm to decidewhether a given graph G is module-composed and construct a correspondingmodule-sequence.  For the case of bipartite graphs, module-composed graphs are exactly distancehereditary graphs, which implies simple linear time algorithms for theirrecognition and construction of a corresponding module-sequence.


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Input: In many applications, input data are sampled functions taking their values ininfinite dimensional spaces rather than standard vectors. This fact has complexconsequences on data analysis algorithms that motivate modifications of them.In fact most of the traditional data analysis tools for regression,classification and clustering have been adapted to functional inputs under thegeneral name of functional Data Analysis (FDA). In this paper, we investigatethe use of Support Vector Machines (SVMs) for functional data analysis and wefocus on the problem of curves discrimination. SVMs are large margin classifiertools based on implicit non linear mappings of the considered data into highdimensional spaces thanks to kernels. We show how to define simple kernels thattake into account the unctional nature of the data and lead to consistentclassification. Experiments conducted on real world data emphasize the benefitof taking into account some functional aspects of the problems.


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Input: We discuss how, in a Universe restricted to the causal region connected tothe observer, General Relativity implies the quantum nature of physicalphenomena and directly leads to a string theory scenario, whose dynamics isruled by a functional that weights all configurations according to theirentropy. The most favoured configurations are those of minimal entropy. Alongthis class of vacua a four-dimensional space-time is automatically selected;when, at large volume, a description of space-time in terms of classicalgeometry can be recovered, the entropy-weighted sum reduces to the ordinaryFeynman's path integral. What arises is a highly predictive scenario,phenomenologically compatible with the experimental observations andmeasurements, in which everything is determined in terms of the fundamentalconstants and the age of the Universe, with no room for freely-adjustableparameters. We discuss how this leads to the known spectrum of particles andinteractions. Besides the computation of masses and couplings, CKM matrixelements, cosmological constant, expansion parameters of the Universe etc...,all resulting, within the degree of the approximation we used, in agreementwith the experimental observations, we also discuss how this scenario passesthe tests provided by cosmology and the constraints imposed by the physics ofthe primordial Universe.


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Input: We have presented a detailed study of twist-2 and twist-3 light-conedistribution amplitudes of $1^3P_1$ and $1^1P_1$ axial-vector mesons, based onQCD conformal partial wave expansion. Applying equations of motion, thetwist-three two-parton light-cone distribution amplitudes can be expressed interms of leading-twist and twist-three three-parton light-cone distributionamplitudes. The relevant G-parity invariant and violating parameters,containing the corrections due to the SU(3) breaking effects, are evaluatedfrom the QCD sum rule method. The results for axial-vector decay constants of$1^3P_1$ states are presented. The values of tensor decay constants andGegenbauer moments of the leading twist distribution amplitudes for $1^1P_1$states are updated. Using Gell-Mann-Okubo mass formula, the mixing angle forthe $f_8$ and $f_1$ of $1^3P_1$ states is $\theta_{^3P_1}\sim 38^\circ$, andthat for $h_8$ and $h_1$ of $1^1P_1$ states is $\theta_{^1P_1}\sim 10^\circ$.The detailed properties for physical states $f_1(1285), f_1(1420), h_1(1170)$,and $h_1(1380)$ are given. Assuming the mixing angle between $K_{1A}$ and$K_{1B}$ to be $\theta_K=45^\circ$ or $-45^\circ$, we also give the detailedstudy for $K_1(1270)$ and $K_1(1400)$. Using the conformal partial waveexpansion, we obtain the models for light-cone distribution amplitudes,containing contributions up to conformal spin 9/2. It is interesting to notethat some distribution amplitudes have significant asymmetric behaviors, whichshould be phenomenologically attractive.


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Input: Context. Although Blazars are a small fraction of the overall AGN populationthey are expected to be the dominant population of extragalactic sources in thehard X-ray and gamma-ray bands and have been shown to be the largestcontaminant of CMB fluctuation maps. So far the number of known blazars is ofthe order of several hundreds, but the forthcoming AGILE, GLAST and Planckspace observatories will detect several thousand of objects of this type. Aims.In preparation for these missions it is necessary to identify new samples ofblazars to study their multi-frequency characteristics and statisticalproperties. Methods. We compiled a sample of objects with blazar-likeproperties via a cross-correlation between large radio (NVSS, ATCAPMN) and X-ray surveys (RASS) using the SDSS-DR4 and 2dF survey data to spectroscopicallyidentify our candidates and test the validity of the selection method. Results.We present the Radio - Optical - X-ray catalog built at ASDC (ROXA), a list of816 objects among which 510 are confirmed blazars. Only 19% of the candidatesturned out to be certainly non-blazars demonstrating the high efficiency of ourselection method. Conclusions. Our catalog includes 173 new blazaridentifications, or about 10% of all presently known blazars. The relativelyhigh flux threshold in the X-ray energy band (given by the RASS survey)preferentially selects objects with high fx / fr ratio leading to the discoveryof new High Energy Peaked BL Lac (HBLs). Our catalog therefore includes manynew potential targets for GeV-TeV observations.


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Input: If predictions for species extinctions hold, then the `tree of life' todaymay be quite different to that in (say) 100 years. We describe a technique toquantify how much each species is likely to contribute to future biodiversity,as measured by its expected contribution to phylogenetic diversity. Ourapproach considers all possible scenarios for the set of species that will beextant at some future time, and weights them according to their likelihoodunder an independent (but not identical) distribution on species extinctions.Although the number of extinction scenarios can typically be very large, weshow that there is a simple algorithm that will quickly compute this index. Themethod is implemented and applied to the prosimian primates as a test case, andthe associated species ranking is compared to a related measure (the `Shapleyindex'). We describe indices for rooted and unrooted trees, and a modificationthat also includes the focal taxon's probability of extinction, making itdirectly comparable to some new conservation metrics.


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Input: In the past both instrumentalism and empiricism have inspired certainpragmatic elements into the Copenhagen interpretation of quantum mechanics. Therelation of such pragmatisms with the correspondence principle is discussed. Itis argued that neither Bohr nor Heisenberg did take `correspondence' in one ofthese forms, and that it, in particular, was Bohr's classical attitude whichcaused him to apply in an inconsistent way his correspondence principle to theEinstein-Podolsky-Rosen experiment, thus causing much confusion. It isdemonstrated that an empiricist pragmatism is conducive to an explanation ofviolation of the Bell inequalities as a consequence of `complementarity' in thesense of `mutual disturbance in a joint nonideal measurement of incompatibleobservables' rather than as being caused by `nonlocal influences'.