The semi-inclusive deep-inelastic scattering (SIDIS) is the golden process for investigating the nucleon’s transverse momentum-dependent (TMD) structure. We present the complete expression for SIDIS structure functions in the TMD factorization formalism at the next-to-leading power. All perturbative elements of the factorization theorem—coefficient functions and evolution kernels—are presented at one-loop accuracy. We found several differences with earlier derivations, which are due to accounting for nontrivial kinematics of the quark-gluon interference terms. As a side result, we present the definition and evolution of twist-three TMD fragmentation functions, including the leading-order evolution kernel.

In this work, we demonstrate that the mixing of scalar and vector condensates produces spatially oscillating, but exponentially damped correlation functions in fermionic theories at finite density and temperature. We find a regime exhibiting this oscillatory behavior in a Gross-Neveu-type model that also features vector interactions within the mean-field approximation. The existence of this regime aligns with expectations based on symmetry arguments that are also applicable to QCD at finite baryon density. We compute the phase diagram including both homogeneous phases and regions with spatially oscillating, exponentially damped correlation functions at finite temperature and chemical potential for different strengths of the vector coupling. Furthermore, we find that inhomogeneous condensates are disfavored compared to homogeneous ones akin to previous findings without vector interactions. We show that our results are valid for a broad class of ($2+1$)-dimensional models with local four-fermion interactions.

Using a sample of $448.1\times {10}^6$ $\psi (2S)$ events collected with the BESIII detector, we perform a study of the decay $J/\psi \to K^{+}{K}^{-}$ via $\psi (2S)\to {\pi }^{+}{\pi }^{-}J/\psi$. The branching fraction of $J/\psi \to K^{+}{K}^{-}$ is determined to be ${\mathcal{B}}_{K^{+}{K}^{-}}=(3.072\pm 0.023(\mathrm{stat})\pm 0.050(\mathrm{syst}))\times {10}^{-4}$, which is consistent with previous measurements but with significantly improved precision.

Tests of the no-hair theorem using astrophysical black holes involve the detection of at least two quasinormal modes (QNMs) in the gravitational wave emitted by a perturbed black hole. A detection of two modes—the dominant, $(\ell ,m,n)=(2,2,0)$, mode and its first overtone, the (2, 2, 1) mode—in the postmerger signal of the binary black hole merger GW150914 was claimed by Isi et al. [Testing the no-hair theorem with GW150914, Phys. Rev. Lett. 123, 111102 (2019)], with further evidence provided by Isi and Farr [Revisiting the ringdown of GW150914 (2022)]. However, Cotesta et al. [Analysis of ringdown overtones in GW150914, Phys. Rev. Lett. 129, 111102 (2022)] disputed this claim, finding that evidence for the overtone only appeared if the signal was analyzed before merger, when a QNM description of the signal is not valid. Because of technical challenges, both of these analyses fixed the merger time and sky location of GW150914 when estimating the evidence for the overtone. At least some of the contention can be attributed to fixing these parameters. Here, we surmount this difficulty and fully marginalize over merger time and sky-location uncertainty while doing a postmerger QNM analysis of GW150914. We find that marginalizing over all parameters yields low evidence for the presence of the overtone, with a Bayes factor of $1.10\pm 0.03$ in favor of a QNM model with the overtone versus one without. The arrival time uncertainty of GW150914 is too large to definitively claim detection of the (2, 2, 1) mode.

We report the results of the first search for Standard Model and baryon-number-violating two-body decays of the neutral $B$ mesons to ${\mathrm{\Lambda }}^0$ and ${\mathrm{\Omega }}_c^{(*)0}$ using $711{\mathrm{fb}}^{-1}$ of data collected at the $\mathrm{\Upsilon }(4S)$ resonance with the Belle detector at the KEKB asymmetric-energy $e^{+}{e}^{-}$ collider. We observe no evidence of signal from any such decays and set 95% confidence-level upper limits on the products of $B^0$ and ${\overline{B}}^0$ branching fractions for these two-body decays with $\mathcal{B}({\mathrm{\Omega }}_c^0\to {\pi }^{+}{\mathrm{\Omega }}^{-})$ in the range between $9.5\times {10}^{-8}$ and $31.2\times {10}^{-8}$.

We develop a covariant formalism to investigate the mixed state entanglement between time-dependent boosted subsystems in $\mathrm{T}\overline{\mathrm{T}}$-deformed ${\mathrm{CFT}}_2\mathrm{s}$ through the reflected entropy. To this end we utilize a conformal perturbation theory to obtain the Rényi reflected entropy through the partition function on the replica manifold. The correction to the reflected entropy to the first order in the deformation parameter $\mu$ is then obtained in the replica limit for finite temperature and finite-sized systems. We further perform an analytic continuation of our results to obtain the reflected entropy for timelike subsystems in such $\mathrm{T}\overline{\mathrm{T}}$-deformed ${\mathrm{CFT}}_2\mathrm{s}$. We verify our field theoretic computations for both spacelike and timelike subsystems by obtaining the dual EWCS in the corresponding bulk cutoff ${\mathrm{AdS}}_3$ geometries and find perfect agreement between the two.

This study focuses on the examination of the island rule within the context of four-dimensional Reissner-Nordström-anti-de Sitter (4D RN-AdS) black holes, illuminating the intricate relationship between the entanglement entropy and phase transitions of black holes. The entanglement entropy of 4D RN-AdS black holes follows the anticipated linear growth pattern before ultimately declining to a constant value, in accordance with the well-established Page curve. The novelty of this study lies in the examination of the influence, previously unexplored, of the first-order phase transition on the shape and evolution of the Page curve in situations involving both eternal and evaporating black holes. Despite the morphological alterations of the curve induced by the transition, the inherent unitarity of the system persists. As the evaporation progresses, the Page curve displays diverse configurations, unveiling phenomena that are novel and defies traditional expectations, thereby enriching our comprehension of the thermodynamics of black holes interlinked with quantum information.

In this paper we discuss a generalization of the Adler zero to loop integrands in the planar limit of the $SU(N)$ nonlinear sigma model (NLSM). The Adler zero for integrands is violated starting at the two-loop order and is only recovered after integration. Here we propose a soft theorem satisfied by loop integrands with any number of loops and legs. This requires a generalization of NLSM integrands to an off shell framework with certain deformed kinematics. Defining an algebraic soft limit, we identify a simple nonvanishing soft behavior of integrands, which we call the algebraic soft theorem. We find that the proposed soft theorem is satisfied by the “surface” integrand of Arkani-Hamed and Figueiredo [arXiv:2403.04826], which is obtained from the shifted $\mathrm{Tr}{\phi }^3$ surfacehedron integrand. Finally, we derive an on shell version of the algebraic soft theorem that takes an interesting form in terms of self-energy factors and lower-loop integrands in a mixed theory of pions and scalars.

Alternative to the embedding formalism, we provide a group theoretic approach to the conformal primary basis for the massless field with arbitrary helicity. To this end, we first point out that $sl(2,\mathbb{C})$ isometry gets enhanced to $sl(2,\mathbb{C})\times D$ symmetry for the solution space of the massless field with $D$ the bulk dilatation. Then, associated with $sl(2,\mathbb{C})\times D$ symmetry, we introduce the novel quadratic Casimirs and relevant tensor/spinor fields to derive two explicit constraints on the bulk dilatation and $sl(2,\mathbb{C})$ Casimirs. With this, we further argue that the candidate conformal primary basis can be constructed out of the infinite tower of the descendants of the left and right highest (lowest) conformal primary wave function of $sl(2,\mathbb{C})$ Lie algebra, and the corresponding celestial conformal weights are determined by the bulk scaling dimension through solving out the exact on-shell conformal primary wave functions, where on top of the two kinds of familiar-looking on-shell conformal primary wave functions, we also obtain another set of independent on-shell conformal primary wave functions for the massless field with helicity $|s|\ge 1$. In passing, we also develop the relationship between the four-dimensional Lorentz Lie algebra and two-dimensional conformal Lie algebra from scratch, and present an explicit derivation for the two important properties associated with the conformal primary wave functions.

In this work, we study the implications of GW230529 on gravity theories and the charge of black holes. The GW230529, which was initially released in O4a, is most likely neutron-star-black-hole mergers. We reanalyze the data from the GW230529 event to obtain bounds on the Einstein-dilation-Gauss-Bonnet (EdGB) gravity parameter $\sqrt{{\alpha }_{\text{EdGB}}}$ and the electric charge of compact binary systems. The event places a 90% credible upper bounds on $\sqrt{{\alpha }_{\text{EdGB}}}$ of $\lesssim 0.298\mathrm{km}$. After including high order corrections of EdGB gravity, the bounds improve to $\sqrt{{\alpha }_{\text{EdGB}}}\lesssim 0.260\mathrm{km}$. Analyses of GW230529 also yield a 90% credible upper bounds on the combination of charge-to-mass ratio of the binary components $\zeta \lesssim 0.024$. The constraints are more stringent than those derived from previously observed single gravitational wave merger event.

Direct observation of gravitational waves from binary black hole (BBH) mergers has made it possible to test the laws of black hole thermodynamics using real astrophysical sources. These tests rely on accurate and unbiased parameter estimates from the pre and postmerger portions of a signal. Due to numerical complications, previous analyses have fixed the sky location and coalescence time when independently estimating the parameters of the pre and postmerger signal. Here we overcome the numerical complications and present a novel method of marginalizing over sky location and coalescence time. Doing so, we find that it is not possible to model only the pre or postmerger portions of the signal while marginalizing over timing uncertainty. We surmount this problem by simultaneously yet independently modeling the pre and postmerger signal, with only the sky location and coalescence time being shared between the models. This allows us to marginalize over all parameters. We use our method to measure the change in area $\mathrm{\Delta }{A}_{\text{measured}}=A_f-A_i$ between the final and initial black holes in the BBH merger GW150914. To measure the final black hole’s area $A_f$ we do an analysis using quasinormal modes (QNMs) to model the postmerger signal, and another analysis using the postmerger portion of an inspiral-merger-ringdown (IMR) template. We find excellent agreement with expectations from general relativity. The Hawking area theorem (which states that $A_f\ge A_i$) is confirmed to 95.4% and 99.5% confidence using the QNM and IMR postmerger models, respectively. Both models yield $\mathrm{\Delta }{A}_{\text{measured}}/\mathrm{\Delta }{A}_{\text{expected}}\sim 1$, where $\mathrm{\Delta }{A}_{\text{expected}}$ is the expected change in area derived from fits to numerical relativity simulations.

Assuming a slow-roll inflationary model where conformal invariance of the Maxwell action is broken via a nonminimal kinetic coupling term, we investigate the non-Gaussian three-point cross-correlation function between the primordial curvature perturbation and the primordial magnetic field, under a fairly general choice of initial vacua for both the scalar and the gauge field sectors. Among the possible triangular configurations of the resulting cross-bispectrum, we find that the squeezed limit leads to local-type non-Gaussianity allowing a product form decomposition in terms of the scalar and magnetic power spectra, which is a generic result independent of any specific choice of the initial states. We subsequently explore its detection prospects in the cosmic microwave background (CMB) via correlations between prerecombination $\mu$-type spectral distortions and temperature anisotropies, sourced by such a primordial cross-correlation. Our analysis with several proposed next-generation CMB missions forecasts a low value of the signal-to-noise ratio (SNR) for the $\mu T$ spectrum if both the vacua are assumed to be pure Bunch-Davies. On the contrary, the SNR may be enhanced significantly for non-Bunch-Davies initial states for the magnetic sector within allowed bounds from current CMB data.

In this study, we investigate two widely recognized interacting dark energy (IDE) models and assess their compatibility with observational data, focusing on the growth rate of matter perturbations. We explore IDE models with different equation of state (EOS) parameters for dark energy (DE), including the Chevallier-Polarski-Linder parametrization and a constant value for $w_{\mathrm{de}}$. To constrain the parameters of the IDE models using background data, we employ a Markov chain Monte Carlo (MCMC) analysis. Our results show that both IDE-I and IDE-II models are compatible with observational data, although with slight variations influenced by the homogeneity or clustering of DE. Following that, we investigate the growth of matter perturbations and perform a comprehensive statistical analysis utilizing both the background and growth rate data. The growth rate in IDE models exhibits deviations compared to the $\mathrm{\Lambda }\mathrm{CDM}$ model due to the impact of homogeneity or clustering of DE, as well as the selection of the EOS parameter. However, we find that the IDE models show good compatibility with the growth rate data. Furthermore, we explore how the clustering or homogeneity of DE and the selection of the EOS parameter affect the evolution of the relative difference in the growth rate of IDE models, $\mathrm{\Delta }f$, in comparison to the $\mathrm{\Lambda }\mathrm{CDM}$ model. Lastly, we employ the Akaike and Bayesian information criteria to evaluate and identify the best model that is compatible with the observational data. The selection of the model depends on the homogeneity or clustering of DE, the EOS parameter, and the dataset used. Overall, the IDE-I and IDE-II models exhibit agreement with the data, with slight deviations depending on specific scenarios and parameters.

The conformal flatness approximation to the Einstein equations has been successfully used in many astrophysical applications such as initial data constructions and dynamical simulations. Although it has been shown that full general relativistic strongly differentially rotating equilibrium models deviate by at most a few percentage from their conformally flat counterparts, whether those conformally flat solutions remain stable has not been fully addressed. To further understand the limitations of the conformal flatness approximation, in this work, we construct spatially conformally flat hot hypermassive neutron stars with postmergerlike rotation laws, and perform conformally flat evolutions and analysis over dynamical timescales. We find that enforcing conformally flat spacetime could change the equilibrium of quasitoroidal models with high angular momentum for $J\gtrsim 9G{M}_{\odot }^2/c$ compared to fully general relativistic cases. In contrast, all the quasispherical models considered in this work remain stable even with high angular momentum $J=9G{M}_{\odot }^2/c$. Our investigation suggests that the quasispherical models are suitable initial data for long-lived hypermassive neutron star modeling in conformally flat spacetime.

If the cosmological dark matter (DM) couples to Standard Model (SM) fields, it can decay promptly to SM states in a highly energetic hard process, which subsequently showers and hadronizes to give stable particles including $e^{\pm }$, $\gamma$, $p^{\pm }$, and $\nu \overline{\nu }$ at lower energy. If the DM particle is very heavy, the high-energy $e^{\pm }$, due to the Klein-Nishina cross section suppression, preferentially lose energy via synchrotron emission which, in turn, can be of unusually high energies. Here, we present previously unexplored bounds on heavy decaying DM up to the Planck scale, by studying the synchrotron emission from the $e^{\pm }$ produced in the ambient Galactic magnetic field. In particular, we explore the sensitivity of the resulting constraints on the DM decay width to (i) different SM decay channels, to (ii) the Galactic magnetic field configurations, and to (iii) various different DM density profiles proposed in the literature. We find that constraints from the synchrotron component complement and improve on constraints from very high-energy cosmic-ray and gamma-ray observatories targeting the prompt emission when the DM is sufficiently massive, most significantly for masses in excess of ${10}^{12}\mathrm{GeV}$.

We have studied the ${\mathrm{\Omega }}_c\to {\pi }^{+}({\pi }^0,\eta )\pi {\mathrm{\Xi }}^{*}$ and ${\mathrm{\Omega }}_c\to {\pi }^{+}({\pi }^0,\eta )\overline{K}{\mathrm{\Sigma }}^{*}$ decays, where the final $\pi {\mathrm{\Xi }}^{*}$ or $\overline{K}{\mathrm{\Sigma }}^{*}$ comes from the decay of two resonances around the nominal $\mathrm{\Xi }(1820)$, which are generated from the interaction of coupled channels made of a pseudoscalar and a baryon of the decuplet. The $\pi {\mathrm{\Xi }}^{*}$ mass distributions obtained in the six different reactions studied are quite different, and we single out four of them, which are free of a tree level contribution, showing more clearly the effect of the resonances. The lower mass resonance is clearly seen as a sharp peak, but the higher mass resonance manifests itself through an interference with the lower one that leads to a dip in the mass distribution around 1850 MeV. Such a feature is similar to the dip observed in the $S$-wave $\pi \pi$ cross section around the 980 MeV coming from the interference of the $f_0(500)$ and $f_0(980)$ resonances. Its observation in coming upgrades of present facilities will shed light on the existence of these two resonances and their nature. On the other hand, when the ${\mathrm{\Omega }}_c\to {\pi }^{+}({\pi }^0,\eta )\overline{K}{\mathrm{\Sigma }}^{*}$ reactions are studied, both peaks are observed.

A dynamical mechanism, based on a confining non-Abelian dark symmetry, which generates Majorana masses for hyperchargeless fermions, is proposed. We apply it to the inverse seesaw scenario, which allows us to generate light neutrino masses from the interplay of TeV-scale pseudo-Dirac mass terms and a small explicit breaking of lepton number. A single generation of vectorlike dark quarks, transforming under a $\mathrm{SU}(3{)}_{\mathrm{D}}$ gauge symmetry, is coupled to a real singlet scalar, which serves as a portal between the dark quark condensate and three generations of heavy sterile neutrinos. Such a dark sector and the Standard Model (SM) are kept in thermal equilibrium with each other via sizable Yukawa couplings to the heavy neutrinos. In this framework, the lightest dark baryon, which has spin $3/2$ and is stabilized at the renormalizable level by an accidental dark baryon number symmetry, can account for the observed relic density via thermal freeze-out from annihilations into the lightest dark mesons. These mesons, in turn, decay to heavy neutrinos, which produce SM final states upon decay. This model may be probed by next generation neutrino telescopes via neutrino lines produced from dark matter annihilations.

In this work, we investigate the possibility to address the excess observed around 95 GeV in the $\gamma \gamma$, $\tau \tau$, and $b\overline{b}$ channels as a scalar resonance(s) within the Georgi-Machacek model. In our analysis, we find that the excess can be easily accommodated in the channels ($\gamma \gamma$ and $b\overline{b}$) simultaneously, where the 95 GeV candidate is a single peak resonance (SPR) due to a light $CP$-even scalar. We found that the excess in the $\tau \tau$ channel can be addressed simultaneously with $\gamma \gamma$ and $b\overline{b}$ only if the 95 GeV candidate is a twin peak resonance (TPR), i.e., another $CP$-odd scalar in addition to the $CP$-even scalar. We demonstrate that the nature of the 95 GeV scalar resonance candidate (SPR or TPR) can be probed via the properties of its di-$\tau$ decay.

Stable dark matter particles may arise as pseudo-Goldstone bosons from the confinement of dark quarks interacting via a non-Abelian gauge force. Their relic abundance is determined not by annihilations into visible particles but by dark pion number-changing processes within the dark sector, such as $3{\pi }_D\to 2{\pi }_D$. However, if the dark vector mesons ${\rho }_D$ are light enough for $3{\pi }_D\to {\pi }_D{\rho }_D$ annihilations to be kinematically allowed, this process dominates and significantly delays freeze-out. As a result, the preferred dark matter mass scale increases and bounds from the Bullet Cluster can be evaded.