We present a calculation of the leading-twist (twist-2) generalized transverse momentum distributions (GTMDs) for unpolarized and longitudinally polarized gluons in the proton, using a recently developed light-front gluon spectator model inspired by the soft-wall AdS/QCD prediction. We calculate the gluon GTMDs for nonzero skewness, using overlaps in terms of light-front wave functions. We also compute the gluon Wigner distributions for various polarization configurations of the proton target, including unpolarized, longitudinally polarized, and transversely polarized states. We present these Wigner distributions and the associated spin densities in both the transverse momentum plane and the transverse impact parameter plane. Furthermore, we evaluate the gluon orbital angular momentum and spin-orbit correlations, and extract the generalized parton distribution and transverse momentum-dependent distribution limits of the GTMDs.

Utilizing $(2712.4\pm 14.3)\times {10}^6\psi (3686)$ events collected with the BESIII detector at the BEPCII collider, we search for the hadronic transition process ${\chi }_{c1}\to {\pi }^{+}{\pi }^{-}{\eta }_c$ following the decay $\psi (3686)\to \gamma {\chi }_{c1}$. No significant signal is observed, and an upper limit of $\mathcal{B}({\chi }_{c1}\to {\pi }^{+}{\pi }^{-}{\eta }_c)$ is determined to be $3.1\times {10}^{-4}$ at 90% confidence level, which is 1 order of magnitude more stringent than the previous measurement.

Using a sample of ($2.712\pm 0.014$)$\times {10}^9\psi (3686)$ events collected with the BESIII detector at the BEPCII collider in 2009, 2012, and 2021, the decay $\psi (3686)\to \omega \eta \eta$ is observed for the first time. The branching fraction of the $\psi (3686)\to \omega \eta \eta$ decay is measured to be ($1.65\pm 0.02\pm 0.21$)$\times {10}^{-5}$, where the first uncertainty is statistical and the second systematic.

We report a laboratory search for ultralight dark photon dark matter using a single-site, two-sensor array of commercial scalar optically pumped magnetometers. In the low-frequency regime where the Earth–ionosphere system acts as an electromagnetic transducer, the expected magnetic signal is a narrow-band triplet of frequencies. This signature consists of a central peak at the dark photon’s Compton frequency, accompanied by two sidebands shifted by Earth’s sidereal rotation frequency. Because scalar magnetometers measure field magnitude, the observable signal is the projection of the oscillating dark photon magnetic field onto the direction of the large, local geomagnetic field. This preserves the crucial triplet signature in the resulting time series data. Analyzing 10.5 h of continuous data, we construct a six-channel complex data vector by evaluating the discrete-time Fourier transform for both sensors directly at the three physical frequencies of the signal triplet. Assuming complex-Gaussian noise, we develop a likelihood framework to set robust, frequency-resolved upper limits on the kinetic-mixing parameter $ϵ$, which governs the coupling between Standard Model photons and dark photons. Within the mass range $4\times {10}^{-15}\mathrm{eV}\lesssim m_{A^{\prime }}\lesssim 3\times {10}^{-14}\mathrm{eV}$, we obtain the most stringent direct laboratory limits to date on the kinetic-mixing parameter, which are complementary to existing astrophysical bounds, including those inferred from observations of the Leo T dwarf galaxy.

Recently, there has been a lot of interest in Carroll black holes and in particular whether or not one could find a Carrollian analog of a rotating black hole spacetime. Here we show that every stationary and axisymmetric solution (and thence also a black hole) of Carrollian general relativity in any number of $d>3$ dimensions is necessarily also static (up to a “topological rotation”). The case of $d=3$ dimensions is special. There, the topological rotation is important and one can have a rotating Carroll Bańados-Teitelboim-Zanelli black hole, obtained from a static one by the Carroll boost accompanied by the reidentification of the angular coordinate, similar to what happens in the Lorentzian case. We also find a Carrollian analog of an accelerating black hole, showing that Schwarzschild is not the only possible stationary and axisymmetric Carroll black hole in four dimensions. A generalization of the no go theorem to include Maxwell, dilatonic, and axionic matter fields is also discussed.

We study the no-global-symmetry conjecture in quantum gravity by modeling black holes as nonisometric codes that encode the interior states with global charges into the fundamental states. The fluctuation in the inner products of the charged states can be larger compared to the case without charges. The nonisometric map causes states with different charges to have nonzero overlaps, signaling symmetry violation. The Renyi entropies of the radiation with global charges are found to be consistent with the quantum extremal surface formula. We compute various forms of Renyi relative entropy, as well as the fidelity, to quantify the degree of a global symmetry violation in Hawking radiation, demonstrating that global symmetries are indeed violated. We also comment on the instability of the black hole remnant.

A novel quantum black hole model is derived by incorporating the Lorentzian term within the loop quantum cosmology framework of the quantum Oppenheimer-Snyder (qOS) model. This model features a quantum-corrected metric tensor, representing a deformation of the classical Schwarzschild solution. Investigations into the quasinormal modes reveal that these quantum-corrected black holes exhibit stability against scalar perturbations. Notably, the exponential decay rate within the Lorentzian qOS model demonstrates a significant reduction compared to both the earlier qOS model devoid of this term and the standard Schwarzschild black hole. The higher overtones of the Lorentzian qOS model also differ significantly from those of the earlier qOS model and the standard Schwarzschild black hole, indicating that the near-horizon geometry is substantially modified. The thermodynamic properties with both positive and negative cosmological constant are considered. For the anti–de Sitter case, our analysis reveals that for small black hole masses, the temperature within this loop quantum gravity framework decreases as the mass diminishes, contrasting with classical black hole behavior. Furthermore, a logarithmic term emerges as the leading-order correction to the Bekenstein-Hawking entropy. Additionally, loop quantum gravity (LQG) corrections induce an extra phase transition in the black hole’s heat capacity at smaller radius. While for the de Sitter case, the temperature increases as the mass decreases for small black holes, again differing from classical expectations. Similarly to the anti–de Sitter case, LQG corrections in the de Sitter case also lead to an extra phase transition in the heat capacity at small radius.

In previous works in this series, we focused on Hamiltonian renormalization of free field theories in all spacetime dimensions or interacting theories in spacetime dimensions lower than 4. In this paper, we address the Hamiltonian renormalization of the $U(1{)}^3$ model for Euclidian general relativity in four spacetime dimensions which is self-interacting. The Hamiltonian flow needs as an input a choice of ${}^{*}$ algebra and corresponding representation thereof or state on it at each resolution scale. If one uses as input algebras and states in analogy to those used in the recent exact solutions of this model, then one finds that the flow finds as fixed point those exact solution theories.

Motivated by bulk reconstruction of smeared boundary operators, we study the Krylov complexity of local and nonlocal primary ${\mathrm{CFT}}_d$ operators from the local bulk-to-bulk propagator of a minimally coupled massive scalar field in ${\mathrm{Rindler}\text{−}\mathrm{AdS}}_{d+1}$ space. We derive analytic and numerical evidence on how the degree of nonlocality in the dual ${\mathrm{CFT}}_d$ observable affects the evolution of Krylov complexity and the Lanczos coefficients. Curiously, the near-horizon limit matches with the same observable for conformally coupled probe scalar fields inserted at the asymptotic boundary of ${\mathrm{AdS}}_{d+1}$ space. Our results also show that the evolution of the growth rate of Krylov operator complexity in the ${\mathrm{CFT}}_d$ takes the same form as to the proper radial momentum of a probe particle inside the bulk to a good approximation. The exact equality only occurs when the probe particle is inserted in the asymptotic boundary or in the horizon limit. Our results capture a prosperous interplay between Krylov complexity in the CFT, thermal ensembles at finite bulk locations and their role in the holographic dictionary.

In previous works in this series we focused on Hamiltonian renormalization of free field theories in all spacetime dimensions. In this paper, we address the Hamiltonian renormalization of the self-interacting scalar field in two spacetime dimensions with polynomial potential, called $P(\mathrm{\Phi }{)}_2$. We consider only the finite volume case. The $P(\mathrm{\Phi }{)}_2$ theory is one of the few interacting quantum field theories that can be rigorously constructed nonperturbatively. We find that our Hamiltonian renormalization flow finds this theory indeed as a fixed point.

The remarkable sensitivity achieved by the planned Laser Interferometer Space Antenna (LISA) will allow us to observe gravitational-wave signals from the mergers of massive black hole binaries (MBHBs) with signal-to-noise ratio (SNR) in the hundreds, or even thousands. At such high SNR, our ability to precisely infer the parameters of an MBHB from the detected signal will be limited by the accuracy of the waveform templates we use. In this paper, we explore the systematic biases that arise in parameter estimation if we use waveform templates that do not model radiation in higher-order multipoles. This is an important consideration for the large fraction of high-mass events expected to be observed with LISA. We examine how the biases change for MBHB events with different total masses, mass ratios, and inclination angles. We find that systematic biases due to insufficient mode content are severe for events with total redshifted mass $\gtrsim {10}^6{M}_{\odot }$. We then compare several methods of predicting such systematic biases without performing a full Bayesian parameter estimation. In particular, we show that through direct likelihood optimization it is possible to predict systematic biases with remarkable computational efficiency and accuracy. Finally, we devise a method to construct approximate waveforms including angular multipoles with $\ell \ge 5$ to better understand how many additional modes (beyond the ones available in current approximants) might be required to perform unbiased parameter estimation on the MBHB signals detected by LISA.

Astrophysical black holes are likely to be surrounded by various forms of matter in the form of disks or halos. While a number of studies have examined the impact of an environment on the lensing of light or gravitational waves from cosmological sources, these have, thus far, been carried out in either a Newtonian or post-Newtonian framework where the environment is superimposed on the black-hole spacetime. By using an exact solution in general relativity describing a black hole embedded within a realistic halo of Hernquist matter distribution, we study deflection angles and image amplification in a fully relativistic setup. It is shown that large “bumps,” that also arise at the Newtonian and post-Newtonian levels, track the transition scale set by the halo parameters that control the strong-lensing upturn and can significantly adjust the inferences made for either the source or lens in various contexts. As an application, we consider “echoes” of gravitational waves, sourced by astrophysical lenses rather than being intrinsic to the compact object that produces the signal.

We study an overpopulated gas of gravitationally interacting bosons surrounding a droplet of Bose-Einstein condensate—the Bose star. We argue that kinetic evolution of this gas approaches with time a self-similar attractor solution to the kinetic equation. If the scale symmetry of the equation is broken by external conditions, the attractor solution exists, remains approximately self-similar, but has a slowly drifting scaling dimension. The latter new regime of adiabatic self-similarity can determine growth of dark matter Bose stars in cosmological models.

We theoretically discuss quantum tunneling transport and frictions at a hadron-quark matter interface based on the Schwinger-Keldysh approach combined with the tunneling Hamiltonian, which has been developed in the context of condensed-matter physics. In the inner core of massive neutron stars, it is expected that cold quark matter appears at sufficiently high densities and hence exhibits color superconductivity, surrounded by nucleon superfluids at lower densities. The perturbative expressions of the tunneling current and the friction at the interface are obtained in terms of the nonequilibrium Green’s functions. We demonstrate the dc Josephson current that occurs at the hadron-quark superfluid interface in the present scheme. Our framework can be applied to various conflagrations involving the interfaces relevant to astrophysical phenomena.

Mathematical ambiguities in partial-wave analysis present a significant challenge to the extraction of resonance properties in hadronic reactions. Recent work has shown that while linear photon polarization can resolve continuous ambiguities in the photoproduction of two pseudoscalar mesons, a final complex conjugate ambiguity remains. In this work, we extend the partial-wave formalism to include circular and elliptical photon polarization. We demonstrate that the additional constraints provided by circularly polarized observables, which are sensitive to the imaginary parts of bilinear amplitude products, are sufficient to remove remaining mathematical ambiguities, yielding an improved partial-wave solution. Furthermore, we show that the resulting overconstrained system allows for a novel application: using the reaction dynamics themselves as a polarimeter. Using recent high-statistics data on $\rho (770)$ photoproduction from the GlueX experiment, we illustrate the viability of this technique in determining the degrees of beam polarization from the data. These results will benefit the next generation of photoproduction experiments at facilities such as Jefferson Lab and the future ilectron-Ion collider.

We propose a parametrization of neutrino masses and mixing in the minimal seesaw model (MSM). The MSM, which introduces two heavy sterile neutrinos, is the minimal extension of the Standard Model in addressing the tiny masses of active neutrinos. The parametrization includes 11 free parameters: six neutrino oscillation parameters (two mass-squared differences $\mathrm{\Delta }{m}_{21}^2$, $\mathrm{\Delta }{m}_{31}^2$ three mixing angles ${\theta }_{12}$, ${\theta }_{13}$, ${\theta }_{23}$, and one Dirac phase ${\delta }_{CP}$), one mass parameter in $0\nu 2\beta$ decay $m_{ee}$, and four additional parameters: two heavy neutrino masses $M_1$ and $M_2$, one active-sterile mixing angle ${\theta }_{14}$, and one $CP$-violating phase ${\delta }_{14}$. This parametrization is derived exactly from the most general neutrino mass matrix in the MSM without any approximation. We further discuss its implications in phenomenological studies.

We investigate baryogenesis from dark matter oscillations in the ultraviolet freeze-in regime. We find that the mechanism can simultaneously accommodate the observed abundances of baryons and dark matter for dark matter masses in the 10 keV to 2 MeV range, provided the reheat temperature lies between the temperature of the electroweak phase transition and $\sim 10\mathrm{TeV}$. The mechanism predicts observable consequences due to the presence of a light dark matter component that is relativistic during structure formation, and x-ray bounds on decaying dark matter can set strong constraints depending on the operator mediating dark matter production.

The CMS Collaboration at the Large Hadron Collider (LHC) has observed two four-jet events with a total invariant mass of about 8 TeV; within each event, the jets can be paired into two dijets with invariant masses of 2 TeV each. These are extremely rare events due to the large invariant mass, which implies a very small QCD background, as well as to the dijet structure, which makes it prone to an interpretation in terms of a heavy resonance decaying into two lighter ones. We investigate the possible interpretation of these events in terms of supersymmetry with a single baryon-number and $R$-parity violating term. In this particular scenario, the lighter resonances are identified with the right-handed squarks of the first generation, while the heavy one is interpreted in terms of a down-squark of the second or third generation. We discuss the constraints that shape this interpretation and outline a well-defined scenario for its realization. The resulting predictions can be scrutinized with forthcoming LHC data.

The dynamics of partons inside the light $\rho$ meson is found to be essential for its properties and internal structure, both in free space and in the nuclear medium. In this paper, we systematically investigate the in-medium structure changes of ${\rho }^{+}$ mesons within the covariant Nambu-Jona-Lasinio (NJL) model, utilizing the Schwinger proper-time regularization scheme. We solve the Bethe-Salpeter equations to guarantee the bound meson-state condition. At the quark level, the nuclear medium effects are also derived within the same NJL model to maintain a consistent approach with the in-medium ${\rho }^{+}$ meson electromagnetic form factors. To this end, we analyze the spacelike electromagnetic form factors of the ${\rho }^{+}$ meson in free space and in a nuclear medium. We find that the charge radius and quadrupole moment of the ${\rho }^{+}$ meson increase with increasing nuclear matter density, while the magnetic moment decreases, in agreement with the existing previous theoretical predictions. The enhancement of the ${\rho }^{+}$ meson charge radius at normal density relative to that in free space is about 11% (0.08 fm), while the reduction of ${\rho }^{+}$ meson magnetic moment is about 8% ($0.20{\mu }_N$). Our predictions for the charge radius, magnetic moment, and quadrupole moment of the ${\rho }^{+}$ meson in both free space and nuclear medium, remain challenging to be verified experimentally.