We make a study of the ${\mathrm{\Omega }}_c(3120)$, one of the five ${\mathrm{\Omega }}_c$ states observed by the LHCb Collaboration, which is well reproduced as a molecular state from the ${\mathrm{\Xi }}_c^{*}\overline{K}$ and ${\mathrm{\Omega }}_c^{*}\eta$ channels mostly. The state with $J^P=3/2^{-}$ decays to ${\mathrm{\Xi }}_c\overline{K}$ in the $D$ wave, and we include this decay channel in our approach, as well as the effect of the ${\mathrm{\Xi }}_c^{*}$ width. With all these ingredients, we determine the fraction of the ${\mathrm{\Omega }}_c(3120)$ width that goes into ${\mathrm{\Xi }}_c\pi \overline{K}$, which could be a measure of the ${\mathrm{\Xi }}_c^{*}\overline{K}$ molecular component, but due to a relatively big binding, compared to its analogous $\mathrm{\Omega }(2012)$ state, we find only a small fraction of about 3%, which makes this measurement difficult with present statistics. As an alternative, we evaluate the scattering length and effective range of the ${\mathrm{\Xi }}_c^{*}\overline{K}$ and ${\mathrm{\Omega }}_c^{*}\eta$ channels, which, together with the binding and width of the ${\mathrm{\Omega }}_c(3120)$ state, could give us an answer to the issue of the compositeness of this state when these magnitudes are determined experimentally, something feasible nowadays, for instance, measuring correlation functions.

True muonium (TM)—the bound state of ${\mu }^{+}{\mu }^{-}$—has not been discovered yet. It was demonstrated that searching for TM via $\gamma \gamma$ fusions in heavy ion collisions is feasible due to the enhancement of the atom number. We study the production of the true para-muonium (pTM) in the collisions of linearly polarized photons in the experiments of heavy-ion collisions, calculate the production rate as well as the transverse spectrum of pTM, and explore the discovery potential in nuclear experiments. Our results show that there is a significant correlation between the linearly polarized photon distribution and the transverse momentum distribution of pTM. The optimal kinematic region of the generated pTM is identified, which can provide a theoretical guide to the detection of pTM in experiments.

A quantum cosmological bouncing model may exhibit an ambiguity stemming from the nonclassical nature of the background evolution: Two classically equivalent theories can produce two qualitatively different potentials sourcing the perturbations. It reflects the general ambiguity in quantization of the gravitational field at linear order. We derive explicitly the quantum canonical transformation of linear perturbations involving the quantum background to show how it leads to inequivalent theories. We identify the relevant quantum parameter describing the difference and expand upon the ambiguity by calculating the expected power spectra produced for initial quantum vacuum fluctuations in the contracting phase of both potentials. We find that one spectral index corresponds to all values of this parameter but one, while the other thus represents a set of measure zero.

We discuss the renormalization of Einstein-Hilbert gravity in $d=2+\epsilon$ dimensions. We show that the application of the path-integral approach leads naturally to scheme- and gauge-independent results on shell, but also gives a natural notion of quantum metric off shell, which is the natural argument of the effective action, even at the leading order in perturbation theory. The renormalization group of Newton’s constant is consistent with the asymptotic safety scenario for quantum gravity in that it has a UV-relevant fixed point. We extend the approach to the analysis of curvature square operators, understood as composites operators, which allows for the determination of the spectrum of scaling operators at the scale-invariant fixed point. The analysis suggests that there is one operator that becomes relevant close to $d=4$ dimensions, while other operators previously found in the literature are either marginal or trivial on shell.

Understanding the orbits of spinning bodies in curved spacetime is important for modeling binary black hole systems with small mass ratios. At zeroth order in mass ratio and ignoring its size, the smaller body moves on a geodesic of the larger body’s spacetime. Postgeodesic effects, driving motion away from geodesics, are needed to model the system accurately. One very important postgeodesic effect is the gravitational self-force, which describes the small body’s interaction with its own contribution to a binary’s spacetime. The self-force includes the backreaction of gravitational-wave emission driving inspiral. Another postgeodesic effect, the “spin-curvature force,” is due to the smaller body’s spin coupling to spacetime curvature. In this paper, we combine the leading orbit-averaged backreaction of point-particle gravitational-wave emission with the spin-curvature force to construct the worldline and associated gravitational waveform for a spinning body spiraling into a Kerr black hole. We use an osculating geodesic integrator, which treats the worldline as evolution through a sequence of geodesic orbits, as well as near-identity (averaging) transformations, which eliminate dependence on orbital phases, allowing for very fast computation of generic spinning-body inspirals. The resulting inspirals and waveforms include all critical dynamical effects which govern such systems (orbit and precession frequencies, inspiral, strong-field gravitational-wave amplitudes), and as such form an effective first model for the inspiral of spinning bodies into Kerr black holes. We emphasize that our present calculation is not self-consistent, since we neglect effects which enter at the same order as effects we include. However, our analysis demonstrates that the impact of spin-curvature forces can be incorporated into extreme mass-ratio inspiral waveform tools with relative ease, making it possible to augment these models with this important aspect of source physics. The calculation is sufficiently modular that it should not be difficult to include neglected postgeodesic effects as efficient tools for computing them become available.

We investigate light propagation in the gravitational field of multiple gravitational lenses. Assuming these lenses are sufficiently spaced to prevent interaction, we consider a linear alignment for the transmitter, lenses, and receiver. Remarkably, in this axially symmetric configuration, we can solve the relevant diffraction integrals—result that offers valuable analytical insights. We show that the point-spread function (PSF) is affected by the number of lenses in the system. Even a single lens is useful for transmission either it is used as a part of the transmitter or it acts on the receiver’s side. We show that power transmission via a pair of lenses benefits from light amplification on both ends of the link. The second lens plays an important role by focusing the signal to a much tighter spot; but in practical lensing scenarios, that lens changes the structure of the PSF on scales much smaller than the telescope, so that additional gain due to the presence of the second lens is independent of its properties and is govern solely by the transmission geometry. While evaluating the signal-to-noise ratio (SNR) in various transmitting scenarios, we see that a single-lens transmission performs on par with a pair of lenses. The fact that the second lens amplifies the brightness of the first one, creates a challenging background for signal reception. Nevertheless, in all the cases considered here, we have found practically-relevant SNR values. As a result, we were able to demonstrate the feasibility of establishing interstellar power transmission links relying on gravitational lensing—a finding with profound implications for applications targeting interstellar power transmission.

We report a new method to calculate the quasinormal modes of rotating black holes, using a spectral decomposition to solve the partial differential equations that result from introducing linear metric perturbations to a rotating background. Our approach allows us to calculate a large sector of the quasinormal mode spectrum. In particular, we study the accuracy of the method for the ($l=2$)-led and ($l=3$)-led modes for different values of the $M_z$ azimuthal number, considering the fundamental modes as well as the first two excitations. We show that our method reproduces the Kerr fundamental modes with an accuracy of ${10}^{-6}$ or better for $a/M<0.8$, while it stays below 0.1% for $a/M<0.98$.

The Love numbers of compact objects quantify their tidal deformability against external perturbations. It is expected that the Love numbers of asymptotically flat black holes (BHs) in general relativity are identically zero. We show that quite contrary to common expectations, the tidal Love numbers of asymptotically de Sitter black holes are nonzero.

We study scatterlike interactions between neutrinos and dark matter in light of different combinations of temperature, polarization and lensing data released by three independent CMB experiments—the Planck satellite, the Atacama Cosmology Telescope (ACT), and the South Pole Telescope (SPT)—in conjunction with baryon acoustic oscillation (BAO) measurements. We apply two different statistical methodologies. Alongside the usual marginalization technique, we cross-check all the results through a profile likelihood analysis. As a first step, working under the assumption of massless neutrinos, we perform a comprehensive (re)analysis aimed at assessing the validity of some recent results hinting at a mild preference for nonvanishing interactions from small-scale CMB data. We find compelling resilience in the results already documented in the literature, confirming that interactions with a strength $u_{\nu \mathrm{DM}}\sim {10}^{-5}–{10}^{-4}$ appear to be globally favored by ACT (both alone and in combination with Planck). This result is corroborated by the inclusion of additional data, such as the recent ACT-DR6 lensing likelihood, as well as by the profile likelihood analysis. Interestingly, a fully consistent preference for interactions emerges from SPT, as well, although it is weaker than the one obtained from ACT. As a second step, we repeat the same analysis considering neutrinos as massive particles. Despite the larger parameter space, all the hints pointing towards interactions are confirmed also in this more realistic case. In addition, we report a very mild preference for interactions in $\mathrm{Planck}+\mathrm{BAO}$ alone (not found in the massless case) which aligns with small-scale data. While this latter result is not fully confirmed by the profile likelihood analysis, the profile distribution does confirm that interactions are not disfavored by Planck.

We investigate the process of an ultrarelativistic fluid accreted onto axisymmetric Kerr-Sen black holes in Einstein-Maxwell-dilaton-axion theory. We obtain the solution describing the velocity potential of a stationary irrotational fluid with a stiff equation of state and the solution for the streamlined diagram of the quadrupolar flow. We also investigate how the solution’s coefficients and the stagnation points are affected by the parameters. The injection rate, the ejection rate, and the critical angle are discussed in detail. We find that with an increasing dilaton parameter the ratio of the ejection rate to the injection rate increases and that the radiative efficiency is larger, while the redshift is lower, compared to the Kerr black hole.

Searching for gravitational-wave signals is a challenging and computationally intensive endeavor undertaken by multiple independent analysis pipelines. While detection depends only on observed noisy data, it is sometimes inconsistently defined in terms of source parameters that in reality are unknown, e.g., by placing a threshold on the optimal signal-to-noise ratio (SNR). We present a method to calibrate unphysical thresholds to search results by performing Bayesian inference on real observations using a model that simultaneously parametrizes the intrinsic network optimal SNR distribution and the effect of search sensitivity on it. We find consistency with a fourth-order power law and detection thresholds of ${10.5}_{-2.4}^{+2.1}$, ${11.2}_{-1.4}^{+1.2}$, and ${9.1}_{-0.5}^{+0.5}$ (medians and 90% credible intervals) for events with false-alarm rates less than $1{\mathrm{yr}}^{-1}$ in the first, second, and third LIGO-Virgo-KAGRA observing runs, respectively. Though event selection can only be self-consistently reproduced by physical searches, employing our inferred thresholds allows approximate observation-calibrated selection criteria to be applied when efficiency is required and injection campaigns are infeasible.

This paper concerns the development of a first simplified model to take into account the perturbations produced by the nongravitational forces acting on the satellites of the Galileo FOC constellation and the corresponding first orbital determinations within the G4S_2.0 project. G4S_2.0 has a series of objectives in verifying the gravitational interaction in the weak field limit of the theory of general relativity, exploiting in particular the eccentricity of the orbits of some Galileo FOC satellites and the precise measurements that can be derived from the atomic clocks on board these satellites. The study focused on the model for the acceleration produced by direct solar radiation pressure on the satellites. This is the largest of all nongravitational perturbations. It is therefore necessary to build a sufficiently accurate model for it before being able to seriously consider smaller perturbation effects, such as those related to terrestrial radiation and thermal thrust effects. The work presents new aspects in the literature of navigation satellites. One of these is the determination of the effects in the Keplerian elements produced by the direct solar acceleration obtained from a box-wing model of the satellite. A second aspect is the comparison of these predictions in the orbital elements with the corresponding orbital residuals achieved from an orbit determination of the satellite. The study therefore highlights even more the importance of being able to improve the model of the perturbation originating from solar radiation in the field of global navigation satellite systems. This is very important if one wants to extract gravitational measurements from the orbit and clock-bias measurements of these satellites to verify the predictions of general relativity and compare them with those of alternative theories of gravitation.

This paper introduces the main problems related to the modeling of the effects of nongravitational perturbations on satellites of the Galileo FOC constellation. The problem is addressed from the point of view of the scientific objectives of the Galileo for Science (G4S_2.0) project. These objectives are reflected in a set of fundamental physics measurements that will exploit the orbits and atomic clocks aboard the Galileo satellites, in particular the GSAT-0201 and GSAT-0202 satellites characterized by elliptical orbits, and not by almost circular orbits such as in the case of the remaining satellites of the constellation. The main focus is on the modeling of the direct solar radiation pressure, the largest nongravitational perturbation on GNSS satellites. After an in-depth presentation of the main nongravitational perturbations of interest, and of the models currently in use in the literature for their consideration, the work focuses on the amplitudes of the different effects and, with particular attention, on their intrinsic knowledge. Finally, two different models are introduced for the structure of the Galileo satellite specially developed for the objectives of G4S_2.0. The first is a simple model of the box-wing type, developed on the basis of the information currently available on the characteristics of the satellite. The second is a 3D model of the Galileo spacecraft, somewhat sophisticated due to the richness of the details on the structure and the various elements that make up the surfaces of the satellite. The activities carried out and in progress with these models and those planned with their subsequent updated versions are described.

We continue previous investigations of the (inhomogeneous) phase structure of the Gross-Neveu model in a noninteger number of spatial dimensions ($1\le d<3$) in the limit of an infinite number of fermion species ($N\to \infty$) at (non)zero chemical potential $\mu$ [L. Pannullo, Inhomogeneous condensation in the Gross-Neveu model in noninteger spatial dimensions $1\le d<3$, Phys. Rev. D 108, 036022 (2023)]. In this work, we extend the analysis from zero to nonzero temperature $T$. The phase diagram of the Gross-Neveu model in $1\le d<3$ spatial dimensions is well-known under the assumption of spatially homogeneous condensation with both a symmetry broken and a symmetric phase present for all spatial dimensions. In $d=1$ one additionally finds an inhomogeneous phase, where the order parameter, the condensate, is varying in space. Similarly, phases of spatially varying condensates are also found in the Gross-Neveu model in $d=2$ and $d=3$, as long as the theory is not fully renormalized, i.e., in the presence of a regulator. For $d=2$, one observes that the inhomogeneous phase vanishes, when the regulator is properly removed (which is not possible for $d=3$ without introducing additional parameters). In the present work, we use the stability analysis of the symmetric phase to study the presence (for $1\le d<2$) and absence (for $2\le d<3$) of these inhomogeneous phases and the related moat regimes in the fully renormalized Gross-Neveu model in the $\mu$, $T$-plane. We also discuss the relation between “the number of spatial dimensions” and “studying the model with a finite regulator” as well as the possible consequences for the limit $d\to 3$.

The scalar-leptoquark (sLQ) parameter space is well explored experimentally. The direct pair production searches at the LHC have excluded light sLQs almost model agnostically, and the high-$p_{\mathrm{T}}$ dilepton tail data have put strong bounds on the leptoquark-quark-lepton Yukawa couplings for a wide range of sLQ masses. However, these do not show the complete picture. Previously, Mandal et al. [Single productions of colored particles at the LHC: An example with scalar leptoquarks, J. High Energy Phys. 07 (2015) 028] showed how the dilepton-dijet data from the pair production searches could give strong limits on these couplings. This was possible by including the single-production contribution to the dilepton-dijet signal. In this paper, we take a fresh look at the LHC limits on all sLQs by following the same principle and combine all significant contributions—from pair and single productions, $t$-channel sLQ exchange and its interference with the Standard Model background—to the $\mu \mu jj$ final state and recast the limits. We notice that the sLQ exchange and its interference with the background processes play significant roles in the limits. The $\mu \mu jj$-recast limits are comparable to or, in some cases, significantly better than the currently known limits (from high-$p_{\mathrm{T}}$ dilepton data and direct searches), i.e., the LHC data rules out more parameter space than what is considered in the current literature. For the first time, we also show how including the QED processes can noticeably improve the sLQ mass exclusion limits from the QCD-only limits.

We study the phenomenology of charged Higgs bosons ($H^{\pm }$) and vectorlike quarks (VLQs), denoted as $T$, the latter possessing a charge identical to the top quark one, within the framework of the two-Higgs-doublet model type II (2HDM-II). Upon examining two scenarios, one featuring a singlet ($T$) [$2\mathrm{HDM}\text{−}\mathrm{II}+(T)$] and another a doublet $(TB)$ [$2\mathrm{HDM}\text{−}\mathrm{II}+(TB)$], we discover that the presence of VLQs has a significant effect on the (pseudo)scalar sector of the 2HDM-II. In particular, this leads to a reduction in the strict constraint on the mass of the charged Higgs boson, which is imposed by $B$-physics observables, specifically $B\to X_s\gamma$. The observed reduction stems from modifications in the charged Higgs couplings to the Standard Model top and bottom quarks. Notably, the degree of this reduction varies distinctly between the singlet 2HDM+($T$) and doublet $2\mathrm{HDM}+(TB)$ scenarios. Additionally, our investigation extends to constraints imposed by the oblique parameters $S$ and $T$ on the VLQ mixing angles. Furthermore, to facilitate efficient exploration of the “$2\mathrm{HDM}\text{−}\mathrm{II}+\mathrm{VLQ}$” parameter space, we present results on pair production of VLQs $T$ ($pp\to T\overline{T}$), followed by $T\to H^{\pm }b$ and $H^{\pm }\to tb$ decays, yielding a distinctive $2t4b$ final state. This investigation thus provides valuable insights guiding the search for extended Higgs and quark sectors at the Large Hadron Collider (LHC) at CERN.

Physics beyond the Standard Model that is resonant in one or more dimensions has been a longstanding focus of countless searches at colliders and beyond. Recently, many new strategies for resonant anomaly detection have been developed, where sideband information can be used in conjunction with modern machine learning, in order to generate synthetic datasets representing the Standard Model background. Until now, this approach was only able to accommodate a relatively small number of dimensions, limiting the breadth of the search sensitivity. Using recent innovations in point cloud generative models, we show that this strategy can also be applied to the full phase space, using all relevant particles for the anomaly detection. As a proof of principle, we show that the signal from the R&D dataset from the LHC Olympics is findable with this method, opening up the door to future studies that explore the interplay between depth and breadth in the representation of the data for anomaly detection.

Leptoquarks are theorized particles of either scalar or vector nature that couple simultaneously to quarks and leptons. Motivated by recent measurements of coherent elastic neutrino-nucleus scattering, we consider the impact of scalar leptoquarks coupling to neutrinos on a few complementary processes, from low energy to colliders. In particular, we set competitive constraints on the typical mass and coupling of scalar leptoquarks by analyzing recent COHERENT data. We compare these constraints with bounds from atomic parity violation experiments, deep inelastic neutrino-nucleon scattering and collider data. Our results highlight a strong complementarity between different facilities and demonstrate the power of coherent elastic neutrino-nucleus scattering experiments to probe leptoquark masses in the sub-TeV range. Finally, we also present prospects for improving current bounds with future upgrades of the COHERENT detectors and the planned European Spallation Source.

Two-dimensional QCD with $N_c$ colors and $N_f$ flavors of massless fermions in the fundamental representation is expected to exhibit conformal behavior in the infrared governed by a $u(N_f)$ Wess–Zumino–Witten model with level $N_c$. Using numerical analysis within the lattice formalism with exactly massless overlap fermions, we show the emergence of such behavior in the infrared limit. Both the continuum extrapolated low-lying eigenvalues of the massless Dirac operator and the propagator of scalar mesons exhibit a flow from the ultraviolet to the infrared. We find that the amplitude of the conserved current correlator remains invariant under the flow, while the amplitude of the scalar correlator approaches $N_f$-independent values in the infrared.

In this work, we propose a method to compute the gravitational form factor $D(Q^2)$ in holographic QCD by exploiting the remarkable correspondence between semiclassical light-front QCD and semiclassical field theories in wrapped spacetime in five dimensions. The use of light-front holography bridges physics at large $Q^2$ as attained in light-front QCD and physics at small $Q^2$ where the coupling to scalar and tensor fields, e.g. glueballs, are dominant. As an application, we compute the $D$-term for the pion and compare the results with recent lattice simulations.