Motivated by the Belle measurements of the process ${\mathrm{\Lambda }}_c^{+}\to \eta {\pi }^{+}\mathrm{\Lambda }$, we investigate this process by considering the contributions from the $\mathrm{\Lambda }(1670)$, $a_0(980)$, and $\mathrm{\Sigma }(1385)$. In addition, we also consider the predicted low-lying baryon ${\mathrm{\Sigma }}^{*}(1/2^{-})$. Our results involving the ${\mathrm{\Sigma }}^{*}(1/2^{-})$ are favored by fitting to the Belle data of the $\eta \mathrm{\Lambda }$ and ${\pi }^{+}\mathrm{\Lambda }$ invariant mass distributions. Furthermore, we predict the $\eta {\pi }^{+}$ invariant mass distribution and the angular distribution $d\mathrm{\Gamma }/d\cos \theta$, which are significantly different depending on whether or not the contribution from the ${\mathrm{\Sigma }}^{*}(1/2^{-})$ is considered. Finally, we show that, with the contribution from the ${\mathrm{\Sigma }}^{*}(1/2^{-})$, the calculated Dalitz plot agrees with the Belle measurements. Future precise measurements of the process ${\mathrm{\Lambda }}_c^{+}\to \eta {\pi }^{+}\mathrm{\Lambda }$ could shed further light on the existence of the low-lying ${\mathrm{\Sigma }}^{*}(1/2^{-})$.

Branching ratios $\mathrm{BR}(\varphi \to K^{+}{K}^{-})$ and $\mathrm{BR}(\varphi \to K_L^0{K}_S^0)$ are regularly updated in the Review of Particle Physics by the PDG group, and from their 2022 values one finds $R=\varphi \to K^{+}{K}^{-}/K_L^0{K}_S^0=1.448\pm 0.023$, in disagreement with theoretical estimates. To provide new clues about this discrepancy we extract the value of $R$ from recent cross section measurements of processes $e^{+}{e}^{-}\to K^{+}{K}^{-}$ and $e^{+}{e}^{-}\to K_L^0{K}_S^0$. We achieve this by a common description of both charged and neutral data by the Unitary & Analytic model. This new analysis leads to the value $1.553\pm 0.040$ for $R$, which is significantly larger than the value from PDG 2022 branching ratios, and in a relatively good agreement with theoretical estimates.

In this paper, we employ the nonrelativistic quantum chromodynamics (QCD) factorization to conduct a comprehensive examination of the $Z$ boson decay into a pair of $\mathrm{\Upsilon }$ mesons, achieving accuracy at the next-to-leading-order (NLO) in ${\alpha }_s$. Our calculations demonstrate that the quantum electrodynamics (QED) diagrams are indispensable in comparison to the pure QCD diagrams, and the implementation of QCD corrections markedly enhances the QCD results, whereas it substantially diminishes the QED results. To ensure consistency with the experimental methodology, we have taken into account the feed-down transitions originating from higher excited states, which exhibit significant relevance. Combining all the contributions, we arrive at the NLO prediction of ${\mathcal{B}}_{Z\to \mathrm{\Upsilon }(nS)+\mathrm{\Upsilon }(mS)}\sim {10}^{-11}$, which is notably lower than the upper limits set by CMS.

A search is described for the production of a pair of bottom-type vectorlike quarks ($B$ VLQs) with mass greater than 1000 GeV. Each $B$ VLQ decays into a $b$ quark and a Higgs boson, a $b$ quark and a $Z$ boson, or a $t$ quark and a $W$ boson. This analysis considers both fully hadronic final states and those containing a charged lepton pair from a $Z$ boson decay. The products of the $H\to bb$ boson decay and of the hadronic $Z$ or $W$ boson decays can be resolved as two distinct jets or merged into a single jet, so the final states are classified by the number of reconstructed jets. The analysis uses data corresponding to an integrated luminosity of $138{\mathrm{fb}}^{-1}$ collected in proton-proton collisions at $\sqrt{s}=13\mathrm{TeV}$ with the CMS detector at the LHC from 2016 to 2018. No excess over the expected background is observed. Lower limits are set on the $B$ VLQ mass at the 95% confidence level. These depend on the $B$ VLQ branching fractions and are 1570 and 1540 GeV for 100% $B\to bH$ and 100% $B\to bZ$, respectively. In most cases, the mass limits obtained exceed previous limits by at least 100 GeV.

In this paper, we consider finite-temperature holographic renormalization group (RG) flows in $D=3$ $\mathcal{N}=(2,0)$ gauged truncated supergravity coupled to a sigma model with a hyperbolic target space. In the context of the holographic duality, fixed points (CFTs) at finite temperature are described by anti–de Sitter (AdS) black holes. We come from the gravity equations of motion to a 3D autonomous dynamical system, which critical points can be related to fixed points of dual field theories. Near-horizon black hole solutions correspond to infinite points of this system. We use Poincaré transformations to project the system on ${\mathbf{R}}^3$ into the 3D unit cylinder such that the infinite points are mapped onto the boundary of the cylinder. We explore numerically the space of solutions. We show that the exact RG flow at zero temperature is the separatrix for asymptotically AdS black hole solutions if the potential has one extremum, while for the potential with three extrema the separatrices are RG flows between AdS fixed points. We find near-horizon analytical solutions for asymptotically AdS black holes using the dynamical equations. We also present a method for constructing full analytical solutions.

The quantum entanglement measure of concurrence is shown to be directly calculable from a Tomita- Takesaki modular operator framework constructed from the local von Neumann algebras of observables for two quantum systems. Specifically, the Tomita-Takesaki modular conjugation operator $J$ that links two separate systems with respect to their von Neumann algebras is related to the quantum concurrence $C$ of a pure bivariate entangled state composed from these systems. This concurrence relation provides a direct physical meaning to $J$ as both a symmetry operator and a quantitative measure of entanglement. This procedure is then demonstrated for a supersymmetric quantum mechanical system and a real scalar field interacting with two entangled spin-$\frac{1}{2}$ Unruh-DeWitt qubit detectors. For the latter system, the concurrence result is shown to be consistent with some known results on the Bell-CHSH inequality for such a system.

We currently lack good waveform models for many gravitational wave sources. Examples where models are lacking include neutron star post-merger signals, core collapse supernovae, and signals of unknown origin. Wavelet based techniques have proven effective at detecting and characterizing these signals. Here we introduce a new method that uses collections of evolving amplitude-frequency tracks, or “voices,” to model generic gravitational wave signals. The analysis is implemented using trans-dimensional Bayesian inference, building on the earlier wavelet-based BayesWave algorithm. The new algorithm, BayesWaveVoices, outperforms the original for long duration signals.

In this paper, we consider a rotating black hole with electric and magnetic monopole charges that moves in a static homogeneous electromagnetic field. We assume that both the charges and the fields are weak, so that they have no effect on the spacetime geometry, which is described by the Kerr metric. We present exact solutions to Maxwell’s equations describing the field of a charged rotating black hole moving in an external field background. We use these solutions to calculate the energy, momentum, and angular momentum fluxes of the electromagnetic field into the black hole. Using these results, we obtain expressions for the torque and force acting on the moving charged rotating black hole arising as a result of its interaction with the external electromagnetic field. We calculate these quantities both in the frame comoving with the black hole and in the frame of the external background field. We use this result to derive the equations that govern the change in the black hole’s mass and spin as well as the motion of the black hole. We provide exact solutions for specific cases which illustrate the role of charge and spin on the motion of the black hole.

As the fingerprints of black holes, quasinormal modes are closely associated with many properties of black holes. Especially, the ringdown phase of gravitational waveforms from the merger of compact binary components can be described by quasinormal modes. Serving as a model-independent approach, the framework of parametrized quasinormal frequencies offers a universal method for investigating quasinormal modes of diverse black holes. In this work, we first obtain the Schrödinger-like master equation of the axial gravitational perturbation of a holonomy-corrected black hole. We calculate the corresponding quasinormal frequencies using the Wentzel-Kramers-Brillouin approximation and asymptotic iteration methods. We investigate the numerical evolution of an initial wave packet on the background spacetime. Then, we deduce the parametrized expression of the quasinormal frequencies and find that $r_0\le {10}^{-2}$ is a necessary condition for the parametrized approximation to be valid, where $r_0$ is the quantum parameter. We also study the impact of the parameter $r_0$ on the greybody factor and Hawking radiation. With more ringdown signals of gravitational waves detected in the future, our research will contribute to the study of the quantum properties of black holes.

In this paper we present an approach to compute analytical post-Minkowskian corrections to unbound two-body scattering in the self-force formalism. Our method relies on a further low-velocity (post-Newtonian) expansion of the motion. We present a general strategy valid for gravitational and nongravitational self-force, and we explicitly demonstrate our approach for a scalar charge scattering off a Schwarzschild black hole. We compare our results with recent calculations in [, Comparison of post-Minkowskian and self-force expansions: Scattering in a scalar charge toy model, Phys. Rev. D 108, 024025 (2023)], showing complete agreement where appropriate and fixing undetermined scale factors in their calculation. Our results also extend their results by including in our dissipative sector the contributions from the flux into the black hole horizon.

Numerical relativists can now produce gravitational waveforms with memory effects routinely and accurately. The gravitational-wave memory effect contains very low-frequency components, including a persistent offset. The presence of these components violates basic assumptions about time-shift behavior underpinning standard data-analysis techniques in gravitational-wave astronomy. This poses a challenge to the analysis of waveform spectra: how to preserve the low-frequency characteristics when transforming a time-domain waveform to the frequency domain. To tackle this challenge, we revisit the preprocessing procedures applied to the waveforms that contain memory effects. We find inconsistency between the zero-frequency limit of displacement memory and the low-frequency spectrum of the same memory preprocessed using the common scheme in literature. To resolve the inconsistency, we propose a new robust preprocessing scheme that produces the spectra of memory waveforms more faithfully. Using this new scheme, we inspect several characteristics of the spectrum of a memory waveform. In particular, we find a discernible beating pattern formed by the dominant oscillatory mode and the displacement memory. This pattern is absent in the spectrum of a waveform without memory. The difference between the memory and no-memory waveforms is too small to be observed by current-generation detectors in a single binary-black-hole event. Detecting the memory in a single event is likely to occur in the era of next-generation detectors.

Stochastic gravitational-wave backgrounds can be of either cosmological or astrophysical origin. The detection of an astrophysical stochastic gravitational-wave background with ground-based interferometers is expected in the near future. Perhaps even more excitingly, the detection of stochastic backgrounds of cosmological origin by future ground-based interferometers could reveal invaluable information about the early Universe. From this perspective, the astrophysical background is a foreground that can prevent the extraction of this information from the data. In this paper, we revisit a time-frequency domain notching procedure previously proposed to remove the astrophysical foreground in the context of next-generation ground-based detectors, but we consider the more realistic scenario where we remove individually detectable signals by taking into account the uncertainty in the estimation of their parameters. We find that time-frequency domain masks can still efficiently remove the astrophysical foreground and suppress it to about 5% of its original level. Further removal of the foreground formed by unresolvable events (in particular, unresolvable binary neutron stars), which is about 10 times larger than the residual foreground from realistic notching, would require detector sensitivity improvements. Therefore, the main limitation in the search for a cosmological background is the unresolvable foreground itself, and not the residual of the notching procedure.

We constrain cosmology and baryonic feedback scenarios with a joint analysis of weak lensing, galaxy clustering, cosmic microwave background (CMB) lensing, and their cross-correlations (so-called $6\times 2$) using data from the Dark Energy Survey (DES) Y1 and the Planck satellite mission. Noteworthy features of our $6\times 2$ pipeline are: We extend CMB lensing cross-correlation measurements to a band surrounding the DES Y1 footprint (around 25% gain in pairs), and we develop analytic covariance capabilities that account for different footprints and all cross-terms in the $6\times 2$ analysis. We also measure the DES Y1 cosmic shear two-point correlation function (2PCF) down to $0{.}^{\prime }25$, but find that going below $2{.}^{\prime }5$ does not increase cosmological information due to shape noise. We model baryonic physics uncertainties via the amplitude of principal components (PCs) derived from a set of hydrosimulations. Given our statistical uncertainties, varying the first PC amplitude $Q_1$ is sufficient to model small scale cosmic shear 2PCF. For DES $\mathrm{Y}1+\mathrm{Planck}$ $6\times 2$ we find $S_8=0.799\pm 0.016$, comparable to the $5\times 2$ result of DES $\mathrm{Y}3+\mathrm{SPT}/\mathrm{Planck}$ $S_8=0.773\pm 0.016$. Combined with our most informative cosmology priors—baryon acoustic oscillation, big bang nucleosynthesis, type Ia supernovae, and Planck 2018 $\mathrm{EE}+\mathrm{lowE}$, we measure $S_8=0.817\pm 0.011$. Regarding baryonic physics constraints, our $6\times 2$ analysis finds $Q_1=2.8\pm 1.8$. Combined with the aforementioned priors, it improves the constraint to $Q_1=3.5\pm 1.3$. For comparison, the strongest feedback scenario considered in this paper, the cosmo-OWLS AGN ($\mathrm{\Delta }{T}_{\mathrm{heat}}={10}^{8.7}\mathrm{K}$), corresponds to $Q_1=5.84$.

We propose a lightweight deep convolutional neural network (lCNN) to estimate cosmological parameters from simulated three-dimensional dark matter (DM) halo distributions and associated statistics. The training dataset comprises 2000 realizations of a cubic box with a side length of $1000h^{-1}\mathrm{Mpc}$ and interpolated over a cubic grid of ${300}^3$ voxels, with each simulation produced using ${512}^3$ DM particles and ${512}^3$ neutrinos. Under the flat $\mathrm{\Lambda }\mathrm{CDM}$ model, simulations vary standard six cosmological parameters including ${\mathrm{\Omega }}_m$, ${\mathrm{\Omega }}_b$, $h$, $n_s$, ${\sigma }_8$, and $w$, along with the neutrino mass sum $M_{\nu }$. We find that (i) within the framework of lCNN, extracting large-scale structure information is more efficient from the halo density field compared to relying on the statistical quantities including the power spectrum, the two-point correlation function, and the coefficients from wavelet scattering transform; (ii) combining the halo density field with its Fourier-transformed counterpart enhances predictions, while augmenting the training dataset with measured statistics further improves performance; (iii) achieving high accuracy in inferring ${\mathrm{\Omega }}_m$, $h$, and ${\sigma }_8$ by the neural network model, while being inefficient in predicting ${\mathrm{\Omega }}_b$, $n_s$, $M_{\nu }$, and $w$; and (iv) compared to the simple fully connected network trained with three statistical quantities, our CNN yields statistically reduced errors, showing improvements of approximately 23% for ${\mathrm{\Omega }}_m$, 11% for $h$, 8% for $n_s$, and 21% for ${\sigma }_8$. Additionally, in comparison with the likelihood-based analysis on $P(k)$ data, our CNN provides much tighter constraints on parameters, especially on ${\mathrm{\Omega }}_m$ and ${\sigma }_8$. Our study emphasizes this lCNN-based novel approach in extracting large-scale structure information and estimating cosmological parameters.

We show that the Global Navigation Satellite System (GNSS) and gravimeters on Earth and in space can potentially offer the most accurate direct measurement of local density of near-Earth asteroid-mass primordial black holes (PBHs) and dark matter (DM) clumps in the Solar System by means of gravitational influence. Using semianalytical methods and Monte Carlo simulation, this paper revisits the analysis of the trajectories of DM clumps in the Solar System, including both captured objects and hyperbolic trajectories. A link is thus made between the frequency and distance of Earth overflights for a given mass flux, and a direct measure of dark matter clump density in the Solar System. We then model the signature of a close fly-by of a DM object on orbital data from GNSS satellites and gravity measurements from gravimeters. We thus obtain a first assessment of the single probe sensitivity. It paves the way for an exhaustive statistical analysis of 28 years of gravimeters and GNSS data to obtain observational constraints on the density of the PBHs and DM clumps within the Solar System, for the mass range $[{10}^8–{10}^{17}]\mathrm{kg}$. In addition, our methodology offers a possibility of direct detection in cases where DM clumps are endowed with an additional long-range clump-matter fifth force beyond gravity.

Dark energy (and its simplest model, the cosmological constant or $\mathrm{\Lambda }$) acts as a repulsive force that opposes gravitational attraction. Assuming galaxies maintain a steady state over extended periods, the estimated upper limit on $\mathrm{\Lambda }$ studies its pushback to the attractive gravitational force of dark matter. From the SPARC dataset, we select galaxies that are best fitted by the Navarro-Frenk-White and Hernquist density models. Introducing the presence of $\mathrm{\Lambda }$ in these galaxies helps to establish the upper limit on its repulsive force. This upper limit on $\mathrm{\Lambda }$ is around ${\rho }_{(<\mathrm{\Lambda })}\sim {10}^{-25}\mathrm{kg}/{\mathrm{m}}^3$, only two orders of magnitude higher than the one measured by Planck. We show that for galaxies with detectable velocities far from the galaxy core, the upper limit on $\mathrm{\Lambda }$ is lower. Furthermore, we show that galaxies and other systems follow the same principle: for larger orbital periods the upper limit on $\mathrm{\Lambda }$ is lower. Consequently, we address the implications for future measurements on the upper limit and the condition for detecting the impact of $\mathrm{\Lambda }$ on galactic scales.

Naive intuition about scale decoupling breaks down in the presence of fermion masses. Kinematic enhancements can greatly extend the range where one needs to keep a finite mass in calculations to obtain a correct result at even the $\mathcal{O}(1)$ level. Treating a light fermion as massive though, leads to a known but somewhat obscure paradox, a seeming leading-order sensitivity to an arbitrarily small mass. We show how a proper formulation in effective field theory not only resolves the physical conundrum but also answers the very practical question of when fermion masses are required. This has important implications for the development of shower Monte Carlo event generators above the weak scale.

Recently, it was noted that absorptive corrections to the electromagnetic form factor in high-energy proton-proton scattering are important for the theoretical interpretation of the $p^{\uparrow }p$ and $p^{\uparrow }A$ analyzing power $A_{\mathrm{N}}(t)$ measurements with the Hydrogen Jet Target polarimeter (HJET) at RHIC. Here, a concise expression for the absorptive correction was derived within the eikonal approach. The resulting analysis reveals a systematic bias, nearly independent of the beam energy, in the experimental determination of the real-to-imaginary ratio $\rho$ when absorption effects are overlooked in the data analysis. Quantification of this bias, as ${\rho }^{\mathrm{meas}}=\rho +(0.036\pm 0.016{)}_{\mathrm{bias}}$, was achieved using a Regge fit applied to available proton-proton measurements of ${\rho }^{\mathrm{meas}}(s)$ and ${\sigma }_{\mathrm{tot}}^{\mathrm{meas}}(s)$. Considering the potential impact of such an effect on the experimentally determined $A_{\mathrm{N}}(t)$, one may enhance consistency between the HJET and STAR measurements of the hadronic spin-flip amplitude. While the sign of the bias in the value of $\rho$ aligns with the anticipated effective increase in the proton charge radius in $pp$ scattering due to absorption, it amplifies the observed discrepancy between ${\sigma }_{\mathrm{tot}}^{\mathrm{meas}}$ and ${\rho }^{\mathrm{meas}}$ values at $\sqrt{s}=13\mathrm{TeV}$ as measured in the TOTEM experiment. Evaluation (using published TOTEM data) of the measured proton-proton $d\sigma /dt$ dependence on the absorptive corrections indicated that possible soft photon corrections to the hadronic amplitude slope may be essential for such data analysis.

High-energy beams incident on a fixed target may scatter against atomic electrons. To a first approximation, one can treat these electrons as free and at rest. For precision experiments, however, it is important to be able to estimate the size of, and when necessary calculate, subleading corrections. We discuss atomic binding corrections to relativistic lepton-electron scattering. We analyze hydrogen in detail, before generalizing our analysis to multi-electron atoms. Using the virial theorem, and many-body sum rules, we find that the corrections can be reduced to measured binding energies, and the expectation value of a single one-body operator. We comment on the phenomenological impact for neutrino flux normalization and an extraction of hadronic vacuum polarization from elastic muon electron scattering at MUonE.