The memory burden effect is an explicit resolution to the information paradox by which an evaporating black hole acquires quantum hair, which then suppresses its rate of mass loss with respect to the semiclassical Hawking rate. We show that this has significant implications for particle dark matter that captures in neutron stars and forms black holes that go on to consume the host star. In particular, we show that constraints on the nucleon scattering cross section and mass of spin-0 and spin-$1/2$ dark matter would be extended by several orders of magnitude.

A quantum communication protocol between harmonic oscillator detectors, interacting with a quantum field, is developed in a cosmological expanding background. The aim is to see if the quantum effects arising in an expanding universe, such as the cosmological particle production, could facilitate the communication between two distant parts or if they provide an additive noisy effect. By considering a perfect cosmic fluid, the resulting expansion turns out to increase the classical capacity of the protocol. This increasing occurs for all the cosmological expansions unless the latter is sharpened just before the receiver’s detector interacts with the field. Moreover, the classical capacity turns out to be sensible to the barotropic parameter $w$ of the perfect fluid and to the coupling between the field and the scalar curvature $\xi$. As a consequence, by performing this protocol, one can achieve information about the cosmological dynamics and its coupling with a background quantum field.

This paper reports the first search for stellar-origin binary black holes within the LISA Data Challenges (LDC). The search algorithm and the Yorsh LDC datasets, both previously described elsewhere, are only summarized briefly; the primary focus here is to present the results of applying the search to the challenge of data. The search employs a hierarchical approach, leveraging semicoherent matching of template waveforms to the data using a variable number of segments, combined with a particle swarm algorithm for parameter space exploration. The computational pipeline is accelerated using graphics processing unit (GPU) hardware. The results of two searches using different models of the LISA response are presented. The most effective search finds all five sources in the data challenge with injected signal-to-noise ratios $\gtrsim 12$. Rapid parameter estimation is performed for these sources.

We introduce gas thermodynamics and matter distribution using jax (godmax), a novel code designed to calculate correlations between the cosmological matter distribution and various gas thermodynamic quantities. Utilizing the extensive antilles suite of 200 hydrodynamical simulations with a diverse range of baryonic feedback strengths, we jointly fit the 3D profiles of total matter distribution, electron density, and electron pressure across various halo masses and redshifts. By accommodating significant variations in gas profiles expected due to baryonic feedback, solving exact hydrostatic equilibrium equation, and offering flexible modeling of nonthermal pressure support, godmax has the capability to jointly fit all these profiles within the measurement uncertainties. This advancement provides consistent profiles to enable, for the first time, robust joint halo-model-based modeling of multiple cosmic probes, including the kinetic and thermal Sunyaev-Zel’dovich (tSZ) effect, weak lensing, and x-ray observations. Furthermore, the model accurately captures correlations between the total matter power suppression due to baryonic feedback and local average thermodynamic quantities, such as the baryon fraction and integrated tSZ effect, in high-mass halos, aligning with observations from hydrodynamical simulations. Looking ahead, we forecast the expected constraints on cosmological and baryonic parameters from upcoming weak lensing catalogs from the Legacy Survey of Space and Time and tSZ maps from the Simons Observatory. This analysis underscores the importance of cross-correlations between weak lensing and tSZ signal in enhancing parameter constraints by resolving major systematic uncertainties due to baryonic physics. The godmax code leverages the jax library, resulting in a fully differentiable halo model with native GPU compilation support.

The early dark energy (EDE) model is one of the promising solutions to the Hubble tension. One of the successes of the EDE model is that it can provide a similar fit to the $\mathrm{\Lambda }\mathrm{CDM}$ model for the cosmic microwave background (CMB) power spectrum. In this work, I analyze the phenomenology of the EDE and $\mathrm{\Lambda }\mathrm{CDM}$ parameters on the CMB temperature power spectrum and notice that this cannot hold on all scales. Thus, if the real cosmology is as described by the EDE model, the $\mathrm{\Lambda }\mathrm{CDM}$ parameters will be scale-dependent when fitting the CMB power spectrum with the $\mathrm{\Lambda }\mathrm{CDM}$ model, which can be hints for the EDE model. I examine CMB-S4-like observations through mock data analysis and find that parameter shifts are notable. As observations include smaller scales, I find lower $H_0$, $n_s$, ${\omega }_b$ and higher ${\omega }_m$, $A_s{e}^{-2\tau }$, which will also constitute new tensions with other observations. They can serve as a possible signal for the EDE model.

We present the first analysis using RADES-BabyIAXO cavities as detectors of high-frequency gravitational waves (HFGWs). In particular, we discuss two configurations for distinct frequency ranges of HFGWs: cavity 1, mostly sensitive at a frequency range of 252.8–333.2 MHz, and cavity 2, at 2.504–3.402 GHz, which is a scaled down version of cavity 1. We find that cavity 1 will reach sensitivity to strains of the HFGWs of order $h_1\sim {10}^{-21}$, while cavity 2 will reach $h_2\sim {10}^{-20}$. These represent the best estimations of the RADES-BabyIAXO cavities as HFGW detectors, showing how this setup can produce groundbreaking results in axion physics and HFGWs simultaneously.

In this study, we introduce the concept of classicality and derive Wigner inequalities that depend on two instants, with a potential extension to three instants. We explore the experimental feasibility of testing the violations of these inequalities in both pure and mixed flavor states of $K^0-$, $D^0$-, and $B_s$- meson pairs. Using the Werner noise model, we demonstrate that violations of time-dependent Wigner inequalities can be detected even when background processes constitute up to 50% of the system.

We have shown that the small-$x$ evolution of the off-forward leading-log dipole scattering amplitudes, both pomeron and odderon, in the momentum space can be completely determined by the evolution of the respective forward amplitudes, with rescaled momenta. In position space, if there is translation symmetry (assumption of a large nucleus), the dipole cross section depends on the positions of quarks and antiquarks only through their separation. The present study is an equivalent proposition in the momentum space—where translation symmetry in momentum bifurcates the amplitudes into two translationally symmetric functions along the $\mathit{k}$ line in the $\mathit{k}-\mathbf{\Delta }$ plane. It also shows that high energy evolutions of dipole generalized transverse momentum-dependent distributions can be achieved only by studying the evolution of dipole transverse momentum-dependent distributions at small-$x$.

In this study, applying the effective Lagrangian approach, we investigate the reaction ${\pi }^{-}p\to K^{*}\mathrm{\Sigma }$ to explore the production of the hidden-strange molecular pentaquarks $P_{s\overline{s}}$. Specifically, we analyze two scenarios, where the $J^P$ quantum numbers of $P_{s\overline{s}}$ are $3/2^{-}$ and $1/2^{-}$. Our results show that the contribution from $s$-channel $P_{s\overline{s}}$ exchange dominates the total cross section, surpassing those from $t$-channel $K^{(*)}$ exchange and $u$-channel $\mathrm{\Sigma }$ exchange. Additionally, we present predictions for the differential cross section of the ${\pi }^{-}p\to K^{*}\mathrm{\Sigma }$ process. Finally, we extend the 2-to-2 scattering process to the 2-to-3 Dalitz process and provide theoretical predictions for this scenario. Our findings suggest that the cross section for the ${\pi }^{-}p\to K^{*}\mathrm{\Sigma }\to K^{+}{\pi }^{-}{\mathrm{\Sigma }}^0$ process can reach several tens of $\mu b$ near the threshold, making it highly favorable for experimental measurement. However, the current scarcity of experimental data for the ${\pi }^{-}p\to K^{*}\mathrm{\Sigma }$ reaction at threshold energy limits our ability to determine the properties of the hidden-strange molecular pentaquarks $P_{s\overline{s}}$ and related physical quantities. Therefore, additional experimental measurements of the ${\pi }^{-}p\to K^{*}\mathrm{\Sigma }$ reaction at threshold are strongly encouraged, and correlation studies could be pursued at facilities such as J-PARC, AMBER, and upcoming HIKE and HIAF meson beam experiments.

We extend previous next-to-next-to leading order (NNLO) calculations of the quantum chromodynamics (QCD) pressure at zero temperature and nonzero baryonic densities using the renormalization group optimized perturbation theory (RGOPT), which entails an all-order RG-invariant resummation. First, we consider the approximation of three massless quark flavors, and then we add the running strange quark mass dependence. The resulting pressure displays a sizeably reduced sensitivity to variations of the arbitrary renormalization scale as compared to the state-of-the-art NNLO results. This confirms previous NLO investigations that the RGOPT resummation scheme provides improved convergence properties and reduced renormalization scale uncertainties, thus being a promising prescription to improve perturbative QCD at high and mid range baryonic densities.

In our previous work [S. Bhattacharya et al., Phys. Rev. Lett. 128, 182002 (2022)], we introduced a pioneering observable aimed at experimentally detecting the orbital angular momentum (OAM) of gluons. Our focus was on the longitudinal double spin asymmetry observed in exclusive dijet production during electron-proton scattering. We demonstrated the sensitivity of the $\cos \varphi$ angular correlation between the scattered electron and proton as a probe for gluon OAM at small $x$ and its intricate interplay with gluon helicity. This current work provides a comprehensive exposition, diving further into the aforementioned calculation with added elaboration and in-depth analysis. We reveal that, in addition to the gluon OAM, one also gains access to the spin-orbit correlation of gluons. We supplement our work with a detailed numerical analysis of our observables for the kinematics of the Electron-Ion Collider. In addition to dijet production, we also consider the recently proposed semi-inclusive diffractive deep inelastic scattering process, which potentially offers experimental advantages over dijet measurements. Finally, we investigate quark-channel contributions to these processes and find an unexpected breakdown of collinear factorization.

A search for the production of three Higgs bosons ($HHH$) in the $b\overline{b}b\overline{b}b\overline{b}$ final state is presented. The search uses $126{\mathrm{fb}}^{-1}$ of proton-proton collision data at $\sqrt{s}=13\mathrm{TeV}$ collected with the ATLAS detector at the Large Hadron Collider. The analysis targets both nonresonant and resonant production of $HHH$. The resonant interpretations primarily consider a cascade decay topology of $X\to SH\to HHH$ with masses of the new scalars $X$ and $S$ up to 1.5 and 1 TeV, respectively. In addition to scenarios where $S$ is off-shell, the nonresonant interpretation includes a search for Standard Model $HHH$ production, with limits on the trilinear and quartic Higgs self-coupling set. No evidence for $HHH$ production is observed. An upper limit of 59 fb is set, at the 95% confidence level, on the cross section for Standard Model $HHH$ production.

We determine the scaling dimension ${\mathrm{\Delta }}_n$ for the class of composite operators ${\varphi }^n$ in the $\lambda {\varphi }^4$ theory in $d=4-\epsilon$ taking the double scaling limit $n\to \infty$ and $\lambda \to 0$ with fixed $\lambda n$ via a semiclassical approach. Our results resum the leading power of $n$ at any loop order. In the small $\lambda n$ regime we reproduce the known diagrammatic results and predict the infinite series of higher-order terms. For intermediate values of $\lambda n$ we find that ${\mathrm{\Delta }}_n/n$ increases monotonically approaching a $(\lambda n{)}^{1/3}$ behavior in the $\lambda n\to \infty$ limit. We further generalize our results to neutral operators in the ${\varphi }^4$ in $d=4-\epsilon$, ${\varphi }^3$ in $d=6-\epsilon$, and ${\varphi }^6$ in $d=3-\epsilon$ theories with $O(N)$ symmetry.

Cosmic strings radiate detectable gravitational waves in models featuring high-scale symmetry breaking, e.g., high-scale leptogenesis. In this Letter, for the first time, we show that different flavored regimes of high-scale leptogenesis can be tested with the spectral features in cosmic string-radiated gravitational waves. This is possible if the scalar field that makes right-handed neutrinos massive is feebly coupled to the Standard Model Higgs. Each flavored regime, sensitive to low-energy neutrino experiments, leaves a marked imprint on the gravitational waves spectrum. A three-flavor and a two-flavor regime could be probed by a characteristic fall-off of the gravitational wave spectrum at the LISA-DECIGO-ET frequency bands with preceding scale-invariant amplitudes bounded from above and below. We present gravitational waves windows for flavored regimes of leptogenesis testable in the upcoming experiments. We also provide the first construction of a leptogenesis framework where a testable distinction of flavor regimes is possible without constraining the flavor structure of the theory.

The gravitational time delays of macrolenses can be used to constrain the rest mass of the photon with high accuracy. Assuming a point mass + external shear lens model, we prove that an upper limit of the photon mass can be derived directly from two observables—the time delay $\mathrm{\Delta }t$ and the leading-to-trailing flux ratio $R$ of strongly lensed fast radio bursts (FRBs). Using the observed values of $\mathrm{\Delta }t$ and $R$ of a lensed FRB candidate, i.e., FRB 20190308C, as a reference, we obtain a strict upper limit of the photon mass between $m_{\gamma }<5.3\times {10}^{-42}\mathrm{kg}$, for a given external shear strength of ${\gamma }^{\prime }=0.01$, and $m_{\gamma }<2.1\times {10}^{-41}-2.4\times {10}^{-42}\mathrm{kg}$, within the external shear range of $0<{\gamma }^{\prime }<1$. This provides the most stringent limit to date on the photon mass through gravitational lensing time delays, improving by 1 to 2 orders of magnitude the previous results obtained from lensed active galactic nuclei.

The oscillation modes of neutron star (NS) merger remnants, as encoded by the kHz postmerger gravitational wave (GW) signal, hold great potential for constraining the as-yet undetermined equation of state (EOS) of dense nuclear matter. Previous works have used numerical relativity simulations to derive quasiuniversal relations for the key oscillation frequencies, but most of them omit the effects of a magnetic field. We conduct full general-relativistic magnetohydrodynamics simulations of NSNS mergers with two different masses and two different EOSs (SLy and ALF2) with three different initial magnetic field topologies (poloidal and toroidal only, confined to the interior, and “pulsarlike”: dipolar poloidal extending from the interior to the exterior), with four different magnetic field strengths with maximum values ranging from $5.5\times {10}^{15}$ to $2.2\times {10}^{17}\mathrm{G}$ at the time of insertion. We find that magnetic braking and magnetic effective turbulent viscosity drives the merger remnants towards uniform rotation and increases their overall angular momentum loss. As a result, the $f_2$ frequency of the dominant postmerger GW mode shifts upwards over time. The overall shift is up to $\sim 200\mathrm{Hz}$ for the strongest magnetic field we consider and $\sim 50\mathrm{Hz}$ for the median case and is therefore detectable in principle by future GW observatories, which should include the magnetic field in their analyses. We also explore the impact of the magnetic field on the postmerger electromagnetic emission, and demonstrate that an extremely large magnetic field, or alternatively a significant shear viscosity mechanism, can cause a supramassive NS remnant to collapse to a black hole in less than 100 ms and lead to jet formation, although we do not expect the conditions for such an outcome to be realistic.

We revisit the dynamics of the post-Newtonian (PN) two-body problem for two inspiraling compact bodies. Starting from a matter-only point-mass Hamiltonian, we present an adapted framework based on the Lie series approach, enabling the derivation of complete perturbative solutions within the conservative sector. Our framework supports both circular and eccentric orbits and is applicable to any perturbation respecting rotational invariance and time independence. In the context of the Arnowitt-Deser-Misner canonical formalism, this includes up to at least 3PN order and local terms beyond. We provide an example application at 2PN order, recovering classical periapsis advance and orbital period corrections, alongside the full orbital evolution in time coordinates. We discuss eventual extensions to spinning and time-dependent systems.

In this work, we test an effective-one-body radiation-reaction force for eccentric planar orbits of a test mass in a Kerr background, which contains third-order post-Newtonian (PN) nonspinning and second-order PN spin contributions. We compare the analytical fluxes connected to two different resummations of this force, truncated at different PN orders in the eccentric sector, with the numerical fluxes computed through the use of frequency- and time-domain Teukolsky-equation codes. We find that the different PN truncations of the radiation-reaction force show the expected scaling in the weak gravitational-field regime, and we observe a fractional difference with the numerical fluxes that is $<5\%$, for orbits characterized by eccentricity $0\le e\le 0.7$, central black-hole spin $-0.99M\le a\le 0.99M$ and fixed orbital-averaged quantity $x=⟨M\mathrm{\Omega }{⟩}^{2/3}=0.06$, corresponding to the mildly strong-field regime with semilatera recta $9M<p<17M$. Our analysis provides useful information for the development of spin-aligned eccentric models in the comparable-mass case.

Recently, the temporal evolution of the angles characterizing the spatial configuration of the jet in the supermassive black hole $\mathrm{M}87^{*}$ was measured exhibiting a precessional pattern around the hole’s spin axis. It would be due to the dragging induced by the fact that the hole’s external spacetime is described by the Kerr metric. Here, it is shown that the Lense-Thirring orbital precessions of a test particle moving about a rotating massive object, calculated perturbatively to the first post-Newtonian order, are able to fully reproduce all the measured features of the orientation of the jet axis of $\mathrm{M}87^{*}$. In particular, by assuming that the latter is aligned with the angular momentum of the accretion disk, modeled as an effective particle moving along a circular orbit, the condition that the absolute value of the predicted Lense-Thirring precessional frequency of the disk agrees with the measured value of $0.56\pm 0.02\mathrm{rad}$ per year of the jet’s one is satisfied for a range of physically meaningful values of the hole’s spin parameter, close to unity, and of the effective disk radius, of the order of just over a dozen gravitational radii. Relying upon such assumptions and results, it is possible to predict that the angle between the hole’s spin axis and the jet’s one stays constant over the years, amounting to 1.16°, in agreement with its measured value of $1.25°\pm 0.18°$. Furthermore, also the temporal pattern and the amplitudes of the time series of the jet’s angles are reproduced by the aforementioned Lense-Thirring precessional model.

Recently it was demonstrated that by adding to the Einstein-Hilbert action a series in powers of the curvature invariants with specially chosen coefficients one can obtain a theory of gravity which has spherically symmetric solutions describing regular black holes. Its reduced action depends on a function of one of the basic curvature invariants of the corresponding metric. In this paper we study a generalization of this model to the case when this function depends on all the basic curvature invariants. We show that the metrics which are solutions of such a model possess a universal scaling property. We demonstrate that there exists a special class of such models for which the “master” equation for a basic curvature invariant is a linear second-order ordinary differential equation. We specify a domain in the space of parameters of the model for which the corresponding solutions describe regular static, spherically symmetric black holes and study their properties.