In this paper, we show that Minkowski functionals (MFs) of weak gravitational lensing (WL) convergence maps contain significant non-Gaussian, cosmology-dependent information. To do this, we run a large suite of cosmological ray-tracing N-body simulations to create mock WL convergence maps, and study the cosmological information content of MFs derived from these maps. Our suite consists of 80 independent ${512}^3$ N-body runs, covering seven different cosmologies, varying three cosmological parameters ${\Omega }_m$, $w$, and ${\sigma }_8$ one at a time, around a fiducial lambda cold dark matter model. In each cosmology, we use ray tracing to create a thousand pseudoindependent $12{\mathrm{deg}}^2$ convergence maps, and use these in a Monte Carlo procedure to estimate the joint confidence contours on the above three parameters. We include redshift tomography at three different source redshifts $z_s=1$, 1.5, 2, explore five different smoothing scales ${\theta }_G=1,2,3,5,10\mathrm{arcmin}$, and explicitly compare and combine the MFs with the WL power spectrum. We find that the MFs capture a substantial amount of information from non-Gaussian features of convergence maps, i.e. beyond the power spectrum. The MFs are particularly well suited to break degeneracies and to constrain the dark energy equation of state parameter $w$ (by a factor of $\approx \mathrm{\text{three}}$ better than from the power spectrum alone). The non-Gaussian information derives partly from the one-point function of the convergence (through $V_0$, the “area” MF), and partly through nonlinear spatial information (through combining different smoothing scales for $V_0$, and through $V_1$ and $V_2$, the boundary length and genus MFs, respectively). In contrast to the power spectrum, the best constraints from the MFs are obtained only when multiple smoothing scales are combined.

Electromagnetic (EM) follow-up observations of gravitational wave events will help shed light on the nature of the sources, and more can be learned if the EM follow-ups can start as soon as the gravitational wave event becomes observable. In this paper, we propose a computationally efficient time-domain algorithm capable of detecting inspiral gravitational waves from coalescing binaries of compact objects with nearly no further delay in addition to the time required to condition the data into a time series of calibrated gravitational-wave strain. Our algorithm, if can be expanded to include sky localization, will serve as the first step towards triggering EM observation before the merger. The key to the efficiency of our algorithm arises from the use of chains of so-called infinite impulse response filters, which filter time-series data recursively. Computational cost is further reduced by a template interpolation technique that requires filtering only done for a “coarse bank”, much sparser than the “fine bank” normally required to sufficiently recover the optimal signal-to-noise ratio: the filter chain of each coarse-bank template is divided into several sections, filtering output from these sections are combined appropriately to reconstruct the output of each of the nearby fine-bank templates. The filter construction and interpolation techniques are illustrated in this paper using Newtonian-chirp waveforms, although these will be generalizable to more accurate post-Newtonian waveforms. Towards future detectors with sensitivity extending to lower frequencies, our algorithm’s computational cost is shown to increase rather insignificantly compared to the conventional time-domain correlation method using finite impulse response filters.

With full 2011 LHC data analyzed, there is no indication for deviation from standard model in CP violating phase for $B_s\to J/\psi \varphi$, nor in the forward-backward asymmetry for $B^0\to K^{*0}{\mu }^{+}{\mu }^{-}$. Standard model sensitivity, however, has been reached for the $B_s\to {\mu }^{+}{\mu }^{-}$ rate, and there may be some hint for a suppression. We illustrate that, if a suppressed $\mathcal{B}(B_s\to {\mu }^{+}{\mu }^{-})$ bears out with 2012 data, it would imply a lower bound on the fourth generation quark mixing product $|V_{t^{\prime }s}^{*}{V}_{t^{\prime }b}|$.

We present an alternative approach to low-energy supersymmetry. Instead of imposing $R$-parity we apply the minimal flavor violation (MFV) hypothesis to the $R$-parity violating MSSM. In this framework, which we call MFV SUSY, squarks can be light and the proton long-lived without producing missing energy signals at the LHC. Our approach differs from that of Nikolidakis and Smith in that we impose holomorphy on the MFV spurions. The resulting model is highly constrained and $R$-parity emerges as an accidental approximate symmetry of the low-energy Lagrangian. The size of the small $R$-parity violating terms is determined by the flavor parameters, and in the absence of neutrino masses there is only one renormalizable $R$-parity violating interaction: the baryon-number violating $\overline{u}\overline{d}\overline{d}$ superpotential term. Low-energy observables (proton decay, dinucleon decay, and $n-\overline{n}$ oscillation) pose only mild constraints on the parameter space. LHC phenomenology will depend on whether the LSP is a squark, neutralino, chargino, or slepton. If the LSP is a squark it will have prompt decays, explaining the non-observation of events with missing transverse energy at the LHC.

Recently, the ATLAS and CMS collaborations have announced exciting hints for a standard model-like Higgs boson at a mass of $\approx 125\mathrm{GeV}$. In this paper, we explore the potential consequences for the MSSM and low-scale SUSY-breaking. As is well-known, a 125 GeV Higgs implies either extremely heavy stops ($\gtrsim 10\mathrm{TeV}$), or near-maximal stop mixing. We review and quantify these statements, and investigate the implications for models of low-scale SUSY-breaking such as gauge mediation where the $A$-terms are small at the messenger scale. For such models, we find that either a gaugino must be superheavy or the NLSP is long-lived. Furthermore, stops will be tachyonic at high scales. These are very strong restrictions on the mediation of supersymmetry breaking in the MSSM, and suggest that if the Higgs truly is at 125 GeV, viable models of gauge-mediated supersymmetry breaking are reduced to small corners of parameter space or must incorporate new Higgs-sector physics.

Considering the possibility to build an $e^{+}{e}^{-}$ collider at the energies around the $Z^0$-boson resonance with a planned luminosity as high as $\mathcal{L}\propto {10}^{34}\sim {10}^{36}{\mathrm{cm}}^{-2}{\mathrm{s}}^{-1}$ (super $Z$-factory), we make a detailed discussion on the ($c\overline{b}$)-quarkonium production through $e^{+}+e^{-}\to (c\overline{b})[n]+b+\overline{c}$ within the framework of nonrelativistic QCD. Here $n$ stands for the Fock-states $|(c\overline{b}{)}_{\mathbf{1}}[{}^{1}S_0]⟩$, $|(c\overline{b}{)}_{\mathbf{8}}[{}^{1}S_0]g⟩$, $|(c\overline{b}{)}_{\mathbf{1}}[{}^{3}S_1]⟩$, $|(c\overline{b}{)}_{\mathbf{8}}[{}^{3}S_1]g⟩$, $|(c\overline{b}{)}_{\mathbf{1}}[{}^{1}P_1]⟩$ and $|(c\overline{b}{)}_{\mathbf{1}}[{}^{3}P_J]⟩$ (with $J=(1,2,3)$), respectively. To simplify the hard-scattering amplitude as much as possible and to derive analytic expressions for the purpose of future events simulation, we adopt the “improved trace technology” to do our calculation, which deals with the hard-scattering amplitude directly at the amplitude level other than the conventional way at the squared-amplitude level. Total cross section uncertainties caused by the quark masses are predicted by taking $m_c=1.50\pm 0.30\mathrm{GeV}$ and $m_b=4.90\pm 0.40\mathrm{GeV}$. If all higher ($c\overline{b}$)-quarkonium states decay to the ground-state $B_c(|(c\overline{b}{)}_{\mathbf{1}}[{}^{1}S_0]⟩)$ with 100% efficiency, we obtain ${\sigma }_{e^{+}+e^{-}\to B_c+b+\overline{c}}={5.190}_{-2.419}^{+6.222}\mathrm{pb}$, which shows that about ${10}^5\sim {10}^7{B}_c$ events per operation year can be accumulated in the super $Z$-factory. If taking the collider energy runs slightly off the $Z^0$-peak, i.e. $\sqrt{S}=(1.00\pm 0.05)m_Z$, the total cross section shall be lowered by about one-order from its peak value. Such a super $Z$-factory shall provide another useful platform to study the properties of $B_c$-meson, or even the properties of its excited $P$-wave states, in addition to its production at the hadronic colliders Tevatron and LHC.

Recently, the CDF Collaboration reported the first nonzero measurement of the $B_s\to {\mu }^{+}{\mu }^{-}$ branching fraction. The LHCb, CMS and ATLAS, collaborations have reported upper limits that are in tension with the CDF result. We consider the implications of these measurements for the specific case of the minimal supersymmetric standard model. We also discuss the implications of these measurements for neutralino dark matter and the supersymmetric contribution to the anomalous magnetic moment of the muon.

We discuss the possibility of using electroproduction of $J/\psi$ as a probe of gluon Sivers function by measuring single spin asymmetry (SSA) in experiments with transversely polarized protons and electron beams. We estimate SSA for JLab, HERMES, COMPASS, and eRHIC energies using the color evaporation model of charmonium production and find asymmetry up to 25% for certain choices of model parameters which have been used earlier for estimating SSA in the SIDIS and Drell-Yan processes.

We study the radiative $B\to K{\eta }^{(\prime )}\gamma$ decays, which are important to investigate $CP$ violation, and are also relevant to assess the role of the exclusive modes induced by the $b\to s\gamma$ transition to saturate the inclusive $B\to X_s\gamma$ decay rate. Moreover, these channels do not display the same hierarchy as $B\to K{\eta }^{(\prime )}$ modes, for which the decay into ${\eta }^{\prime }$ is enhanced with respect to one into $\eta$. The three-body radiative decays reverse the role: we find that this experimentally observed behavior (although affected by a large uncertainty in the case of the ${\eta }^{\prime }$) is reproduced in the theoretical analysis. We compute a $B^{*}\to K$ form factor, needed for this study, using light cone QCD sum rules, and discuss a relation expected to hold in the large energy limit for the light meson. Finally, we examine $B\to K\eta \gamma$ in two extensions of the standard model with universal extra dimensions, to investigate the sensitivity of this rare mode to such a kind of new physics effects.

We propose a minimal extension of the standard model by two real singlet fields that could provide a good candidate for light dark matter, and give a strong first order electroweak phase transition. As a result, there are two $CP$ even scalars: one is lighter than $\sim 70\mathrm{GeV}$, and the other one with mass in the range $\sim 280–400\mathrm{GeV}$, and consistent with electroweak precision tests. We show that the light scalar mass can be as small as 25 GeV while still being consistent with the LEP data. The predicted dark matter scattering cross-section is large enough to accommodate CoGeNT and can be probed by future XENON experiment. We also show that for dark matter mass around 2 GeV, the branching fraction of the process ($B^{+}\to K^{+}+2(DM)$) can be accessible in SuperB factories.

Using the covariant spectator theory, we present the results of a valence quark-diquark model calculation of the nucleon structure function $f(x)$ measured in unpolarized deep inelastic scattering and the structure functions $g_1(x)$ and $g_2(x)$ measured in deep inelastic scattering using polarized beams and targets. Parameters of the wave functions are adjusted to fit all the data. The fit fixes both the shape of the wave functions and the relative strength of each component. Two solutions are found that fit $f(x)$ and $g_1(x)$, but only one of these gives a good description of $g_2(x)$. This fit requires the nucleon covariant spectator theory wave functions contain a large $D$-wave component (about 35%) and a small $P$-wave component (about 0.6%). The significance of these results is discussed.

Expressions for the nucleon wave functions in the covariant spectator theory are derived. The nucleon is described as a system with a off-mass-shell constituent quark, free to interact with an external probe, and two spectator constituent quarks on their mass shell. Integrating over the internal momentum of the on-mass-shell quark pair allows us to derive an effective nucleon wave function that can be written only in terms of the quark and diquark (quark-pair) variables. The derived nucleon wave function includes contributions from $S$-, $P$- and $D$-waves.

Using the data for $24.5\times {10}^6$ $\psi (2S)$ produced in $e^{+}{e}^{-}$ annihilations at $\sqrt{s}=3686\mathrm{MeV}$ at the CESR-c $e^{+}{e}^{-}$ collider and $8.6\times {10}^{6}J/\psi$ produced in the decay $\psi (2S)\to {\pi }^{+}{\pi }^{-}J/\psi$, the branching fractions for $\psi (2S)$ and $J/\psi$ decays to pairs of pseudoscalar mesons, ${\pi }^{+}{\pi }^{-}$, $K^{+}{K}^{-}$, and $K_S{K}_L$, have been measured using the CLEO-c detector. We obtain branching fractions $\mathcal{B}(\psi (2S)\to {\pi }^{+}{\pi }^{-})=(7.6\pm 2.5\pm 0.6)\times {10}^{-6}$, $\mathcal{B}(\psi (2S)\to K^{+}{K}^{-})=(74.8\pm 2.3\pm 3.9)\times {10}^{-6}$, $\mathcal{B}(\psi (2S)\to K_S{K}_L)=(52.8\pm 2.5\pm 3.4)\times {10}^{-6}$, and $\mathcal{B}(J/\psi \to {\pi }^{+}{\pi }^{-})=(1.47\pm 0.13\pm 0.13)\times {10}^{-4}$, $\mathcal{B}(J/\psi \to K^{+}{K}^{-})=(2.86\pm 0.09\pm 0.19)\times {10}^{-4}$, $\mathcal{B}(J/\psi \to K_S{K}_L)=(2.62\pm 0.15\pm 0.14)\times {10}^{-4}$, where the first errors are statistical and the second errors are systematic. The phase differences between the amplitudes for electromagnetic and strong decays of $\psi (2S)$ and $J/\psi$ to $0^{-+}$ pseudoscalar pairs are determined by a Monte Carlo method to be $\delta (\psi (2S{)}_{PP}=({110.5}_{-9.5}^{+16.0})°$ and $\delta (J/\psi {)}_{PP}=({73.5}_{-4.5}^{+5.0})°$. The difference between the two is $\Delta \delta \equiv \delta (\psi (2S){)}_{PP}-\delta (J/\psi {)}_{PP}=({37.0}_{-10.5}^{+16.5})°$.

We study unconventional behavior of massless Dirac fermions due to interaction with a U(1) gauge field in three time-space dimensions. At zero chemical potential, the longitudinal and transverse components of gauge interaction are both long ranged. There is no fermion velocity renormalization since the system respects Lorentz invariance. At finite chemical potential, the Lorentz invariance is explicitly broken by the finite Fermi surface. The longitudinal gauge interaction is statically screened and becomes unimportant, whereas the transverse gauge interaction remains long ranged and leads to singular renormalization of fermion velocity. The anomalous dimension of fermion velocity is calculated by means of the renormalization group method. We then examine the influence of singular velocity renormalization on several physical quantities, and show that they exhibit different behavior at zero and finite chemical potential.

In this paper, the $SIM(2)$ superspace formulation of the supersymmetric Yang-Mills gauge theory minimally coupled to chiral superfields is discussed. The super-Poincare invariant supersymmetric Yang-Mills theory is rewritten to $SIM(2)$ superspace formalism and the effects of $SIM(2)$ invariant but Lorentz breaking terms are discussed. Two approaches are investigated. The first is based on the gauge chiral representation of the supersymmetric gauge theory and the second is based on the covariant representation of the supersymmetric gauge theory.

The microscopic spectral density for lattice QCD with two flavors and maximally twisted mass is computed. The results are given for a fixed index of the Dirac operator and include the leading-order $a^2$ corrections to the chiral Lagrangian due to the discretization errors. The computation is carried out within the framework of Wilson chiral perturbation theory.

A thermodynamic analysis of the black hole solutions coming from the Einstein-Maxwell-dilaton theory in 4D is done. By considering the canonical and grand-canonical ensemble, we apply standard method as well as a recent method known as geometrothermodynamics. We are particularly interested in the characteristics of the so called phantom black hole solutions. We will analyze the thermodynamics of these solutions, the points of phase transition and their extremal limit. The thermodynamic stability is also analyzed. We obtain a mismatch between the results of the geometrothermodynamics method when compared with the ones obtained by the specific heat, revealing a weakness of the method, as well as possible limitations of its applicability to very pathological thermodynamic systems. We also found that normal and phantom solutions are locally and globally unstable, except for certain values of the coupled constant of the Einstein-Maxwell-dilaton action. We also show that the anti-Reissner-Nordstrom solution does not possess extremal limit nor phase transition points, contrary to the Reissner-Nordstrom case.

Current cosmological observations, when interpreted within the framework of a homogeneous and isotropic Friedmann-Lemaître-Robertson-Walker (FLRW) model, strongly suggest that the Universe is entering a period of accelerating expansion. This is often taken to mean that the expansion of space itself is accelerating. In a general spacetime, however, this is not necessarily true. We attempt to clarify this point by considering a handful of local and nonlocal measures of acceleration in a variety of inhomogeneous cosmological models. Each of the chosen measures corresponds to a theoretical or observational procedure that has previously been used to study acceleration in cosmology, and all measures reduce to the same quantity in the limit of exact spatial homogeneity and isotropy. In statistically homogeneous and isotropic spacetimes, we find that the acceleration inferred from observations of the distance-redshift relation is closely related to the acceleration of the spatially averaged universe, but does not necessarily bear any resemblance to the average of the local acceleration of spacetime itself. For inhomogeneous spacetimes that do not display statistical homogeneity and isotropy, however, we find little correlation between acceleration inferred from observations and the acceleration of the averaged spacetime. This shows that observations made in an inhomogeneous universe can imply acceleration without the existence of dark energy.

We study the evolution of linear density perturbations in a large spherical void universe which accounts for the acceleration of the cosmic volume expansion without introducing dark energy. The density contrast of this void is not large within the light cone of an observer at the center of the void. Therefore, we describe the void structure as a perturbation with a dimensionless small parameter $\kappa$ in a homogeneous and isotropic universe within the region observable for the observer. We introduce additional anisotropic perturbations with a dimensionless small parameter $ϵ$, whose evolution is of interest. Then, we solve perturbation equations up to order $\kappa ϵ$ by applying second-order perturbation theory in the homogeneous and isotropic universe model. By this method, we can know the evolution of anisotropic perturbations affected by the void structure. We show that the growth rate of the anisotropic density perturbations in the large void universe is significantly different from that in the homogeneous and isotropic universe. This result suggests that the observation of the distribution of galaxies may give a strong constraint on the large void universe model.

The chameleon mechanism appearing in the massive tensor-scalar theory of gravity can effectively reduce locally the nonminimal coupling between the scalar field and matter. This mechanism is invoked to reconcile large-scale departures from general relativity, supposedly accounting for cosmic acceleration, to small-scale stringent constraints on general relativity. In this paper, we carefully investigate this framework on cosmological and solar system scales to derive combined constraints on model parameters, notably by performing a nonambiguous derivation of observables like luminosity distance and local post-Newtonian parameters. The likelihood analysis of type Ia supernovae data and of an admissible domain for the parametrized-post-Newtonian parameters clearly demonstrates that the chameleon mechanism cannot occur in the same region of parameter space as the one necessary to account for cosmic acceleration with the assumed Ratra-Peebles potential and exponential coupling function.