We study the scalarized charged black holes in the Einstein-Maxwell-Scalar (EMS) theory with scalar mass term. In this work, the scalar mass term is chosen to be $m_{\varphi }^2=\alpha /\beta$, where $\alpha$ is a coupling parameter and $\beta$ is a masslike parameter. It turns out that any scalarized charged black holes are not allowed for the case of $\beta \le 4.4$ with $q=0.7(M=0.5,Q=0.35)$ because this case implies the stable Reissner-Nodström (RN) black holes. In the massless limit of $\beta \to \infty$, one recovers the case of the EMS theory. We note that the unstable RN black hole implies the appearance of scalarized charged black holes. The other unstable case of $\beta >4.4$ with $q=0.7$ allows us to obtain the $n=0,1,2,\dots$ scalarized charged black holes for $\alpha (\beta )\ge {\alpha }_{\mathrm{th}}(\beta )$ where ${\alpha }_{\mathrm{th}}(\beta )$ represents the threshold of instability for the RN black hole. Furthermore, it is shown that the $n=0$ black hole is stable against radial perturbations, while the $n=1$ black hole is unstable. This stability result is independent of the mass parameter $\beta$.

In order to perform model-dependent tests of general relativity with gravitational wave observations, we must have access to numerical relativity binary black hole waveforms in theories beyond general relativity (GR). In this study, we focus on order-reduced Einstein dilaton Gauss-Bonnet gravity (EDGB), a higher curvature beyond-GR theory with motivations in string theory. The stability of single, rotating black holes in EDGB is unknown but is a necessary condition for being able to simulate binary black hole systems (especially the early-inspiral and late ringdown stages) in EDGB. We thus investigate the stability of rotating black holes in order-reduced EDGB. We evolve the leading-order EDGB scalar field and EDGB spacetime metric deformation on a rotating black hole background, for a variety of spins. We find that the EDGB metric deformation exhibits linear growth, but that this level of growth exponentially converges to zero with numerical resolution. Thus, we conclude that rotating black holes in EDGB are numerically stable to leading-order, thus satisfying our necessary condition for performing binary black hole simulations in EDGB.

Perhaps the most powerful method for deriving the Newtonian gravitational interaction between two masses is the multipole expansion. Once inner multipoles are calculated for a particular shape, this shape can be rotated, translated, and even converted to an outer multipole with well-established methods. The most difficult stage of the multipole expansion is generating the initial inner multipole moments without resorting to three-dimensional numerical integration of complex functions. Previous work has produced expressions for the low-degree inner multipoles for certain elementary solids. This work goes further by presenting closed-form expressions for all degrees and orders. A combination of these solids, combined with the aforementioned multipole transformations, can be used to model the complex structures often used in precision gravitation experiments.

In this work, using the Gaussian process, we explore the potentiality of future gravitational wave (GW) measurement to probe cosmic opacity through comparing its opacity-free luminosity distance (LD) with the opacity-dependent one from type Ia supernovae (SNIa). GW data points are simulated from the third-generation Einstein Telescope, and SNIa data are taken from the Joint Light Analysis (JLA) or Pantheon compilation. The advantages of using the Gaussian process are that one may match SNIa data with GW data at the same redshift and use all available data to probe cosmic opacity. We obtain that the error bar of the constraint on cosmic opacity can be reduced to ${\sigma }_{\epsilon }\sim 0.011$ and 0.006 at $1\sigma$ confidence level (CL) for JLA and Pantheon, respectively, in a cosmological-independent way. Thus, the future GW measurements can give competitive results on the cosmic opacity test. Furthermore, we propose a method to probe the spatial homogeneity of the cosmic transparency through comparing the reconstructed LD from the mock GW with the reconstructed one from SNIa data in a flat $\mathrm{\Lambda }\mathrm{CDM}$ with the Gaussian process. The result shows that a transparent universe is favored at $1\sigma$ CL, although the best-fit value of cosmic opacity is redshift dependent.

We analyze the constraints on colored scalar bosons imposed by the current LHC data at $\sqrt{s}=13\mathrm{TeV}$. Specifically, we consider an additional electroweak doublet of color-octet scalars, satisfying the principle of minimal flavor violation in order to fulfill the stringent experimental limits on flavor-changing neutral currents. We demonstrate that colored scalars with masses below 800 GeV are already excluded, provided they are not fermiophobic.

We study portal interactions connecting visible and dark sectors, and involving local interactions of a photon, a dark photon and a axionlike particle (ALP) at future $e^{+}{e}^{-}$ colliders. These interactions, mediated by higher-dimensional effective operators, may arise at one loop by kinetic mixing between dark and ordinary photons, or, for massless dark photons, by direct short-distance contributions. We explore these portal interactions for a heavy ALP with masses between about 10 and 230 GeV, and for a massless dark photon, by investigating the sensitivity of the production $e^{+}{e}^{-}\to \gamma \gamma \overline{\gamma }$ to the effective couplings, where the dark photon $\overline{\gamma }$ gives rise to missing momentum in the final state. We will show how an appropriate choice of missing-energy and missing-mass cuts can optimize the signal to standard-model background ratio. Exclusion regions for the effective photon-dark-photon-ALP couplings versus the ALP mass are worked out for a few representative values of the collision energy and integrated luminosity, as presently envisaged by future $e^{+}{e}^{-}$ projects.

The $\epsilon$-regime of dilaton chiral perturbation theory is introduced. We compute the dilaton mass, the chiral condensate and the topological susceptibility in the $\epsilon$-regime, as a function of the fermion mass. The microscopic spectral density of the Dirac operator is obtained from dilaton chiral perturbation theory. Our main result is that the chiral condensate and the spectral density are related to their counterparts from ordinary chiral perturbation theory via a simple scaling relation. This relation originates from the mass dependence of the dilaton potential, and is valid in both the $\epsilon$-regime and the $p$-regime. In the $\epsilon$-regime, moreover, all results agree with the universal predictions to leading order in $\epsilon$.

We use a chiral model for pion interactions, in the inverse amplitude formalism, to perform a simultaneous analysis of lattice QCD results for pion-pion scattering in all three isospin channels. The input is the finite-volume two-pion spectrum computed using lattice QCD from six ensembles on lattices elongated in one of the spatial dimensions. A two-flavor dynamical lattice QCD action is used with two quark masses corresponding to a pion mass of 315 and 224 MeV. The spectrum in the elastic region is subjected to a global fit which takes into account full correlations across isospin, pion mass and decay constant. The parameters from the fit are used to perform a chiral extrapolation to the physical point. The cross-channel fit results in a more precise determination of the parameters of the model when compared with single channel fits. We obtain, $m_{\pi }{a}_0^{I=0}=0.2132(9)$, and $m_{\pi }{a}_0^{I=2}=0.0433(2)$ as well as $m_{\sigma }=443(3)-i221(6)\mathrm{MeV}$ and $m_{\rho }=724(4)-i67(1)\mathrm{MeV}$. Several aspects of scale setting and consistency with previous analyses of lattice QCD results are discussed as well.

The strong decays of the low-lying $\lambda$-mode ${\mathrm{\Lambda }}_b(1D,2S)$ and ${\mathrm{\Sigma }}_b(2S)$ states are studied in a chiral quark model. We find that (i) the newly observed ${\mathrm{\Lambda }}_b(6146/6152)$ resonances in the ${\mathrm{\Lambda }}_b{\pi }^{+}{\pi }^{-}$ spectrum by the LHCb Collaboration might be explained with the $\lambda$-mode ${\mathrm{\Lambda }}_b(1D)$ states in the quark model. It should be emphasized that whether the structure in the ${\mathrm{\Lambda }}_b{\pi }^{+}{\pi }^{-}$ spectrum corresponds to two states or one state should be further clarified with more observations in future experiments. (ii) The ${\mathrm{\Lambda }}_b(2S)$ $|J^P={\frac{1}{2}}^{+},0⟩$ state mainly decays into ${\mathrm{\Sigma }}_b^{*}\pi$ channel, which may be an ideal channel for searching for this ${\mathrm{\Lambda }}_b(2S)$ state in future experiments. (iii) The ${\mathrm{\Sigma }}_b(2S)$ $|J^P={\frac{1}{2}}^{+},1⟩$ and $|J^P={\frac{3}{2}}^{+},1⟩$ dominantly decay into ${\mathrm{\Lambda }}_b\pi$ with $\mathrm{\Gamma }\simeq 3.82\mathrm{MeV}$ and $\mathrm{\Gamma }\simeq 4.72\mathrm{MeV}$, respectively.

We present the matching coefficient for the quark beam function at next-to-next-to-next-to-leading order in perturbative QCD in the generalized large $N_c$-approximation, $N_c\sim N_f\gg 1$. Although several refinements are still needed to make this result interesting for phenomenological applications, our computation shows that a fully-differential description of simple color singlet production processes at a hadron collider at ${\mathrm{N}}^3\mathrm{LO}$ in perturbative QCD is within reach.

Using a $3.19{\mathrm{fb}}^{-1}$ data sample collected at the $\sqrt{s}=4.178\mathrm{GeV}$ with the BESIII detector, we search for the rare decay $D_s^{+}\to p\overline{p}{e}^{+}{\nu }_e$. No significant signal is observed, and an upper limit of $\mathcal{B}(D_s^{+}\to p\overline{p}{e}^{+}{\nu }_e)<2.0\times {10}^{-4}$ is set at the 90% confidence level. This measurement is useful input in understanding the baryonic transition of $D_s^{+}$ mesons.

We study the reaction $e^{+}{e}^{-}\to {\pi }^{+}{\pi }^{-}{\pi }^0{\eta }_c$ for the first time using data samples collected with the BESIII detector at center-of-mass energies $\sqrt{s}=4.226$, 4.258, 4.358, 4.416, and 4.600 GeV. Evidence of this process is found and the Born cross section ${\sigma }^B(e^{+}{e}^{-}\to {\pi }^{+}{\pi }^{-}{\pi }^0{\eta }_c)$, excluding $e^{+}{e}^{-}\to \omega {\eta }_c$ and $\eta {\eta }_c$, is measured to be $({46}_{-11}^{+12}\pm 10)\mathrm{pb}$ at $\sqrt{s}=4.226\mathrm{GeV}$. Evidence for the decay $Z_c(3900{)}^{\pm }\to {\rho }^{\pm }{\eta }_c$ is reported at $\sqrt{s}=4.226\mathrm{GeV}$ with a significance of $3.9\sigma$, including systematic uncertainties, and the Born cross section times branching fraction ${\sigma }^B(e^{+}{e}^{-}\to {\pi }^{\mp }{Z}_c(3900{)}^{\pm })\times \mathcal{B}(Z_c(3900{)}^{\pm }\to {\rho }^{\pm }{\eta }_c)$ is measured to be $(48\pm 11\pm 11)\mathrm{pb}$, which indicates that $e^{+}{e}^{-}\to {\pi }^{\mp }{Z}_c(3900{)}^{\pm }\to {\pi }^{\mp }{\rho }^{\pm }{\eta }_c$ dominates the $e^{+}{e}^{-}\to {\pi }^{+}{\pi }^{-}{\pi }^0{\eta }_c$ process. The $Z_c(3900{)}^{\pm }\to {\rho }^{\pm }{\eta }_c$ signal is not significant at the other center-of-mass energies and the corresponding upper limits are determined. In addition, no significant signal is observed in a search for $Z_c(4020{)}^{\pm }\to {\rho }^{\pm }{\eta }_c$ with the same data samples. The ratios $R_{Z_c(3900)}=\mathcal{B}(Z_c(3900{)}^{\pm }\to {\rho }^{\pm }{\eta }_c)/\mathcal{B}(Z_c(3900{)}^{\pm }\to {\pi }^{\pm }J/\psi )$ and $R_{Z_c(4020)}=\mathcal{B}(Z_c(4020{)}^{\pm }\to {\rho }^{\pm }{\eta }_c)/\mathcal{B}(Z_c(4020{)}^{\pm }\to {\pi }^{\pm }{h}_c)$ are obtained and compared with different theoretical interpretations of the $Z_c(3900{)}^{\pm }$ and $Z_c(4020{)}^{\pm }$.

By studying the space of geodesics in ${\mathrm{AdS}}_3/{\mathrm{CFT}}_2$ and quantizing the geodesic motion, we relate scattering data to boundary entanglement of the CFT vacuum. The basic idea is to use a family of plane waves parametrized by coordinates of the space of geodesics i.e., kinematic space. This idea enables a simple calculation of the Berry curvature living on kinematic space. As a result we recover the Crofton form with a coefficient depending on the scattering energy. In arriving at these results the space of horocycles is used. We show that this new space used in concert with kinematic space incorporates naturally the gauge degrees of freedom responsible for an analog of Berry’s phase. Horocycles also give a new geometric look to the strong subadditivity relation in terms of lambda lengths giving rise to shear coordinates of geodesic quadrangles. A generalization for geodesic polygons then reveals an interesting connection with $A_n$ cluster algebras. Here the cluster variables are the lambda lengths related to the regularized entropies of the boundary via the Ryu-Takayanagi relation. An elaboration of this idea indicates that cluster algebras might provide a natural algebraic means for encoding the gauge invariant entanglement patterns of certain boundary entangled states in the geometry of bulk geodesics. Finally using the language of integral geometry we show how certain propagators connected to the bulk, boundary and kinematic spaces are related to data of elementary scattering problems. We also present some hints how these ideas might be generalized for more general holographic scenarios.

Accurate predictions for the nonlinear matter power spectrum are needed to confront theory with observations in current and near future weak-lensing and galaxy clustering surveys. We propose a computationally cheap method to create an emulator for modified gravity models by utilizing existing emulators for $\mathrm{\Lambda }\mathrm{CDM}$. Using a suite of $N$-body simulations, we construct a fitting function for the enhancement of both the linear and nonlinear matter power spectrum in the commonly studied Hu-Sawicki $f(R)$ gravity model valid for wave numbers $k\lesssim 5–10h{\mathrm{Mpc}}^{-1}$ and redshifts $z\lesssim 3$. We show that the cosmology dependence of this enhancement is relatively weak so that our fit, using simulations coming from only one cosmology, can be used to get accurate predictions for other cosmological parameters. We also show that the cosmology dependence can, if needed, be included by using linear theory, approximate $N$-body simulations (such as comoving lagrangian acceleration) and semianalytical tools like the halo model. Our final fit can easily be combined with any emulator or semianalytical models for the nonlinear $\mathrm{\Lambda }\mathrm{CDM}$ power spectrum to accurately, and quickly, produce a nonlinear power spectrum for this particular modified gravity model. The method we use can be applied to fairly cheaply construct an emulator for other modified gravity models. As an application of our fitting formula, we use it to compute Fisher forecasts for how well galaxy clustering and weak lensing in a Euclid-like survey will be at constraining modifications of gravity.

Consistency between cosmological datasets is essential for ongoing and future cosmological analyses. We first investigate the questions of stability and applicability of some moment-based inconsistency measures to multiple datasets. We show that the recently introduced index of inconsistency (IOI) is numerically stable while it can be applied to multiple datasets. We use an illustrative construction of constraints as well as an example with real datasets (i.e., WMAP versus Planck) to show some limitations of the application of the Karhunen-Loeve decomposition to discordance measures. Second, we perform various consistency analyses using IOI between multiple current datasets while working with the entire common parameter spaces. We find current large-scale-structure (LSS) datasets [Planck cosmic microwave background lensing, Dark Energy Survey (DES) lensing clustering, and sloan digital sky survey, redshift space distorsions] all to be consistent with one another. This is found to not be the case for Planck temperature (temperature auto correlation, TT) versus polarization [temperature and E-mode polarization cross correlation (TE), E-mode polarization auto correlation (EE)] data, where moderate inconsistencies are present. Noteworthy, we find a strong inconsistency between joint LSS probes and Planck with $\mathrm{IOI}=5.27$, and a moderate tension between DES and Planck with $\mathrm{IOI}=3.14$. Next, using the IOI metric, we compare the Hubble constant from five independent probes. We confirm previous strong tensions between local measurement (Supernovae, HO, for the equation of state of dark energy, SH0ES) and Planck as well as between H0 lenses in COSMOGRAIL’s wellspring and Planck, but also find new strong tensions between SH0ES measurement and the joint LSS probes with $\mathrm{IOI}=6.73$ (i.e., $3.7\text{−}\sigma$ in one dimension) as well as between joint LSS and combined probes $\mathrm{SH}0\mathrm{ES}+\mathrm{H}0\mathrm{LiCOW}$ with $\mathrm{IOI}=8.59$ (i.e., $4.1\text{−}\sigma$ in one dimension). Whether because of systematic effects in the datasets or problems with the underlying model, sources of these old and new tensions need to be identified and dealt with.

We investigate the pion electromagnetic half-off-shell form factors, which parametrize the matrix element of the charged pion electromagnetic current with one leg off mass shell and the other leg on mass shell, using an exactly solvable manifestly covariant model of a ($3+1$)- dimensional fermion field theory. The model provides a three-dimensional imaging of the two off-shell pion form factors $F_1$ and $F_2$ as a function of $(Q^2,t)$, which are related to each other, satisfying the Ward-Takahashi identity. The normalization of the renormalized charge form factor $F_1$ is fixed by $F_1(Q^2=0,t=m_{\pi }^2)=1$, while the other form factor $F_2$ vanishes; i.e., $F_2(Q^2,t=m_{\pi }^2)=0$ for any value of $Q^2$ due to the time-reversal invariance of the strong interaction. We define the new form factor $g(Q^2,t)=F_2(Q^2,t)/(t-m_{\pi }^2)$ and find that $g(Q^2,t)$ can be measurable in the on-mass-shell limit. In particular, $g(Q^2=0,t=m_{\pi }^2)$ is related with the pion charge radius. We also compare our form factors with the data extracted from the pion electroproduction reaction for both the off-shell region ($t<0$) and the on-shell limit ($t\to m_{\pi }^2$).

A common lore has arisen that beyond the Standard Model (BSM) particles, which can be searched for at current and proposed experiments, should have flavorless or mostly third-generation interactions with Standard Model quarks. This theoretical bias severely limits the exploration of BSM phenomenology and is especially constraining for extended Higgs sectors. Such limitations can be avoided in the context of spontaneous flavor violation (SFV), a robust and UV complete framework that allows for significant couplings to any up- or down-type quark, while suppressing flavor-changing neutral currents via flavor alignment. In this work we study the theory and phenomenology of extended SFV Higgs sectors with large couplings to any quark generation. We perform a comprehensive analysis of flavor and collider constraints of extended SFV Higgs sectors and demonstrate that new Higgs bosons with large couplings to the light quarks may be found at the electroweak scale. In particular, we find that new Higgses as light as 100 GeV with order $\sim 0.1$ couplings to first- or second-generation quarks, which are copiously produced at the LHC via quark fusion, are allowed by current constraints. Furthermore, the additional SFV Higgses can mix with the SM Higgs, providing strong theory motivation for an experimental program looking for deviations in the light quark–Higgs couplings. Our work demonstrates the importance of exploring BSM physics coupled preferentially to light quarks and the need to further develop dedicated experimental techniques for the LHC and future colliders.

The Fermilab short-baseline neutrino (SBN) experiments, MicroBooNE, ICARUS, and SBND, are expected to have significant sensitivity to light weakly coupled hidden sector particles. Here we study the capability of the SBN experiments to probe dark scalars interacting through the Higgs portal. We investigate production of dark scalars using both the Fermilab booster 8 GeV and NuMI 120 GeV proton beams, simulating kaons decaying to dark scalars and taking into account the beam line geometry. We also investigate strategies to mitigate backgrounds from beam-related neutrino scattering events. We find that SBND, with its comparatively short $\mathcal{O}(100\mathrm{m})$ baseline, will have the best sensitivity to scalars produced from the booster, while ICARUS, with its large detector volume, will provide the best limits on off-axis dark scalar production from NuMI. The SBN experiments can provide leading tests of dark scalars with masses in the 50–350 MeV range in the near term. Our results motivate dedicated experimental searches for dark scalars and other long-lived hidden sector states at these experiments.

Two-Higgs-doublet models (2HDMs) with a flavored $U(1{)}^{\prime }$ gauge symmetry are a popular extension to the Standard Model (SM), yet they currently lack a complete survey. In this paper, we present a full classification of anomaly-free 2HDMs within the SM fermion content, resulting in a total of 11 distinct models. Four of these are relatively well studied, while the rest either partially, or entirely, lack previous treatment. We study these textures under a variety of experimental bounds, focusing mainly on the previously unexplored models. This work is intended to act as a catalog to models worth considering in greater detail.

We propose a one-loop induced radiative seesaw model applying a modular $S_3$ flavor symmetry, which is known as the minimal non-Abelian discrete group. In this scenario, dark matter (DM) candidate is correlated with neutrinos and lepton flavor violations (LFVs). We show several predictions of mixings and phases satisfying LFVs, observed relic density, and neutrino oscillation data.