The 100 most-cited articles in Physical review. D/Physical review. D., 2022

We present the first cosmology results from large-scale structure using the full 5000 deg 2 of imaging data from the Dark Energy Survey (DES) Data Release 1.We perform an analysis of large-scale structure combining three two-point correlation functions (3 × 2pt): (i) cosmic shear using 100 million source galaxies, (ii) galaxy clustering, and (iii) the cross-correlation of source galaxy shear with lens galaxy positions, galaxy-galaxy lensing.To achieve the cosmological precision enabled by these measurements has required updates to nearly every part of the analysis from DES Year 1, including the use of two independent galaxy clustering samples, modeling advances, and several novel improvements in the calibration of gravitational shear and photometric redshift inference.The analysis was performed under strict conditions to mitigate confirmation or observer bias; we describe specific changes made to the lens galaxy sample following unblinding of the results and tests of the robustness of our results to this decision.We model the data within the flat ΛCDM and wCDM cosmological models,…

This work, together with its companion paper, Secco, Samuroff et al. [Phys. Rev. D 105, 023515 (2022)], present the Dark Energy Survey Year 3 cosmic-shear measurements and cosmological constraints based on an analysis of over 100 million source galaxies. With the data spanning $4143\text{ }\text{ }{\mathrm{deg}}^{2}$ on the sky, divided into four redshift bins, we produce a measurement with a signal-to-noise of 40. We conduct a blind analysis in the context of the Lambda-Cold Dark Matter ($\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$) model and find a 3% constraint of the clustering amplitude, ${S}_{8}\ensuremath{\equiv}{\ensuremath{\sigma}}_{8}({\mathrm{\ensuremath{\Omega}}}_{\mathrm{m}}/0.3{)}^{0.5}=0.75{9}_{\ensuremath{-}0.023}^{+0.025}$. A $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$-Optimized analysis, which safely includes smaller scale information, yields a 2% precision measurement of ${S}_{8}=0.77{2}_{\ensuremath{-}0.017}^{+0.018}$ that is consistent with the fiducial case. The two low-redshift measurements are statistically consistent with the Planck Cosmic Microwave…

This work and its companion paper, Amon et al. [Phys. Rev. D 105, 023514 (2022)], present cosmic shear measurements and cosmological constraints from over 100 million source galaxies in the Dark Energy Survey (DES) Year 3 data. We constrain the lensing amplitude parameter ${S}_{8}\ensuremath{\equiv}{\ensuremath{\sigma}}_{8}\sqrt{{\mathrm{\ensuremath{\Omega}}}_{\mathrm{m}}/0.3}$ at the 3% level in $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$: ${S}_{8}=0.75{9}_{\ensuremath{-}0.023}^{+0.025}$ (68% CL). Our constraint is at the 2% level when using angular scale cuts that are optimized for the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ analysis: ${S}_{8}=0.77{2}_{\ensuremath{-}0.017}^{+0.018}$ (68% CL). With cosmic shear alone, we find no statistically significant constraint on the dark energy equation-of-state parameter at our present statistical power. We carry out our analysis blind, and compare our measurement with constraints from two other contemporary weak lensing experiments: the Kilo-Degree Survey (KiDS) and Hyper-Suprime Camera Subaru Strategic Program (HSC). We additionally…

A novel kind of generalized global symmetries is uncovered in a large class of familiar 3+1-dimensional gauge theories, including the free Maxwell theory and Yang-Mills gauge theories. These new symmetries, known as the non-invertible global symmetries, do not have inverses and thus go beyond the traditional paradigm of (anti-)unitary transformations. They are implemented by topological duality defects, generalizing the Kramers-Wannier duality defects in 1+1 dimensions. Remarkably, the existence of certain kinds of duality defects is intrinsically incompatible with a trivially gapped phase and hence gives new constraints on renormalization group flows.

We present constraints on the tensor-to-scalar ratio $r$ using a combination of BICEP/Keck 2018 (BK18) and Planck PR4 data allowing us to fit for $r$ consistently with the six parameters of the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ model. We discuss the sensitivity of constraints on $r$ to uncertainties in the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ parameters as defined by the Planck data. In particular, we are able to derive a constraint on the reionization optical depth $\ensuremath{\tau}$ and thus propagate its uncertainty into the posterior distribution for $r$. While Planck sensitivity to $r$ is slightly lower than the current ground-based measurements, the combination of Planck with BK18 and baryon-acoustic-oscillation data yields results consistent with $r=0$ and tightens the constraint to $r<0.032$ at 95% confidence.

We present a full $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ analysis of the BOSS DR12 dataset, including information from the power spectrum multipoles, the real-space power spectrum, the reconstructed power spectrum and the bispectrum monopole. This is the first analysis to feature a complete treatment of the galaxy bispectrum, including a consistent theoretical model and without large-scale cuts. Unlike previous works, the statistics are measured using window-free estimators: this greatly reduces computational costs by removing the need to window-convolve the theory model. Our pipeline is tested using a suite of high-resolution mocks and shown to be robust and precise, with systematic errors far below the statistical thresholds. Inclusion of the bispectrum yields consistent parameter constraints and shrinks the ${\ensuremath{\sigma}}_{8}$ posterior by 13% to reach $<5%$ precision; less conservative analysis choices would reduce the error bars further. Our constraints are broadly consistent with Planck: in particular, we find ${H}_{0}={69.6}_{\ensuremath{-}1.3}^{+1.1}\text{…

Complexity plays an important role in the study of black holes in quantum gravity, and of interacting many-body systems in condensed matter physics. The authors propose a definition of quantum state complexity, which agrees with earlier definitions under certain conditions. They compute the complexity in various models and show physically reasonable behaviors which can be connected with quantum chaos.

We introduce a family of solutions of Einstein's gravity minimally coupled to an anisotropic fluid, describing asymptotically flat black holes with ``hair'' and a regular horizon. These spacetimes can describe the geometry of galaxies harboring supermassive black holes, and are extensions of Einstein clusters to include horizons. They are useful to constrain the environment surrounding astrophysical black holes, using electromagnetic or gravitational-wave observations. We compute the main properties of the geometry, including the corrections to the ringdown stage induced by the external matter and fluxes by orbiting particles. The leading order effect to these corrections is a gravitational-redshift, but gravitational-wave propagation is affected by the galactic potential in a nontrivial way, and may be characterized with future observatories.

We present new ν μ → ν e , ν μ → ν μ , νμ → νe , and νμ → νμ oscillation measurements by the NOvA experiment, with a 50% increase in neutrino-mode beam exposure over the previously reported results.The additional data, combined with previously published neutrino and antineutrino data, are all analyzed using improved techniques and simulations.A joint fit to the ν e , ν μ , νe , and νμ candidate samples within the 3-flavor neutrino oscillation framework continues to yield a best-fit point in the normal mass ordering and the upper octant of the θ 23 mixing angle, with Δm 2 32 ¼ ð2.41 Æ 0.07Þ × 10 -3 eV 2 and sin 2 θ 23 ¼ 0.57 þ0.03 -0.04 .The data disfavor combinations of oscillation parameters that give rise to a large asymmetry in the rates of ν e and νe appearance.This includes values of the charge parity symmetry (CP) violating phase in the vicinity of δ CP ¼ π=2 which are excluded by > 3σ for the inverted mass ordering, and values around δ CP ¼ 3π=2 in the normal ordering which are disfavored at 2σ confidence.

We systematically study the field equations of $f(\mathbb{Q})$ gravity for spherically symmetric and stationary metric-affine spacetimes. Such spacetimes are described by a metric as well as a flat and torsionless affine connection. In the symmetric teleparallel equivalent of general relativity (STEGR), the connection is pure gauge and hence unphysical. However, in the nonlinear extension $f(\mathbb{Q})$, it is promoted to a dynamical field which changes the physics. Starting from a general metric-affine geometry, we construct the most general static and spherically symmetric forms of the metric and the affine connection. We then use these symmetry reduced geometric objects to prove that the field equations of $f(\mathbb{Q})$ gravity admit general relativity (GR) solutions as well as beyond-GR solutions, contrary to what has been claimed in the literature. We formulate precise criteria, under which conditions it is possible to obtain GR solutions and under which conditions it is possible to obtain beyond-GR solutions. We subsequently construct several perturbative corrections to the…

We propose a new entropy construct that generalizes the Tsallis, R\'enyi, Sharma-Mittal, Barrow, Kaniadakis, and loop quantum gravity entropies and reduces to the Bekenstein-Hawking entropy in a certain limit. This proposal is applied to the Schwarzschild black hole and to spatially homogeneous and isotropic cosmology, where it is shown that it can potentially describe inflation and/or holographic dark energy.

Euclidean time windows in the integral representation of the hadronic vacuum polarization contribution to the muon $g\ensuremath{-}2$ serve to test the consistency of lattice calculations and may help in tracing the origins of a potential tension between lattice and data-driven evaluations. In this paper, we present results for the intermediate time window observable computed using $\mathrm{O}(a)$ improved Wilson fermions at six values of the lattice spacings below 0.1 fm and pion masses down to the physical value. Using two different sets of improvement coefficients in the definitions of the local and conserved vector currents, we perform a detailed scaling study which results in a fully controlled extrapolation to the continuum limit without any additional treatment of the data, except for the inclusion of finite-volume corrections. To determine the latter, we use a combination of the method of Hansen and Patella and the Meyer-Lellouch-L\"uscher procedure employing the Gounaris-Sakurai parametrization for the pion form factor. We correct our results for isospin-breaking effects…

A critical point is an important structure in the phase diagram of a thermodynamic system. In this work, we introduce topology to the study of black hole thermodynamics for the first time by following Duan's topological current $\ensuremath{\phi}$-mapping theory. Each critical point is endowed with a topological charge. We find that critical points can be divided into two classes, the conventional and the novel. Further study shows that the first-order phase transition can extend from the conventional critical point, while the presence of the novel critical point cannot serve as an indicator of the presence of the first-order phase transition near it. Moreover, the charged anti--de Sitter black hole and the Born-Infeld anti--de Sitter black hole have different topological charges, which indicates they are in different topological classes from the viewpoint of thermodynamics. These give the first promising study on the topology of black hole thermodynamics. Such approach is also expected to be extended to other black holes, and much more topological information remains to be…

We give a detailed treatment of electromagnetic signals generated by gravitational waves (GWs) in resonant cavity experiments. Our investigation corrects and builds upon previous studies by carefully accounting for the gauge dependence of relevant quantities. We work in a preferred frame for the laboratory, the proper detector frame, and show how to resum short-wavelength effects to provide analytic results that are exact for GWs of arbitrary wavelength. This formalism allows us to firmly establish that, contrary to previous claims, cavity experiments designed for the detection of axion dark matter only need to reanalyze existing data to search for high-frequency GWs with strains as small as $h\ensuremath{\sim}{10}^{\ensuremath{-}22}--{10}^{\ensuremath{-}21}$. We also argue that directional detection is possible in principle using readout of multiple cavity modes. Further improvements in sensitivity are expected with cutting-edge advances in superconducting cavity technology.

Making use of modern supernova simulations which include muon effects, the authors update constraints on light muon-specific (pseudo) scalars and generic axion-like particles. They find that such scalar solutions to the muon g-2 excess are in conflict with astrophysical observations.

With several dozen binary black hole events detected by LIGO-Virgo to date and many more expected in the next few years, gravitational-wave astronomy is shifting from individual-event analyses to population studies. Using the GWTC-2 catalog, we perform a hierarchical Bayesian analysis that for the first time combines several state-of-the-art astrophysical formation models with a population of primordial black holes (PBHs) and constrains the fraction of a putative subpopulation of PBHs in the data. We find that this fraction depends significantly on the set of assumed astrophysical models. While a primordial population is statistically favored against certain competitive astrophysical channels, such as globular clusters and nuclear stellar clusters, a dominant contribution from the stable-mass-transfer isolated formation channel drastically reduces the need for PBHs, except for explaining the rate of mass-gap events like GW190521. The tantalizing possibility that black holes formed after inflation are contributing to LIGO-Virgo observations could only be verified by further reducing…

The present paper applies a refined detection pipeline to publicly available LIGO-Virgo data from the first half of the third observing run (O3a) to identify new binary black hole (BBH) mergers. The study adds ten new BBH mergers to existing catalogs and provides further evidence for the significance level of previously identified events. The new events display interesting new features that include unexplored ranges of the effective spin and mass ratio, they challenge aspects of stellar collapse models, and have implications for BBH formation channels and black hole mass gaps.

We use observations of ultrafaint dwarf (UFD) galaxies to constrain the particle mass of ultralight dark matter. Potential fluctuations created by wave interference in virialized ``fuzzy'' dark matter (FDM) halos dynamically heat stellar orbits in UFDs, some of which exhibit velocity dispersions of $\ensuremath{\lesssim}3\text{ }\text{ }\mathrm{km}/\mathrm{s}$ and sizes $\ensuremath{\lesssim}40\text{ }\text{ }\mathrm{pc}$. Using simulations of FDM halos, and existing measurements of sizes and stellar radial velocities in Segue 1 and Segue 2 UFDs, we derive a lower limit on the dark matter particle mass of ${m}_{\mathrm{FDM}}>3\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}19}\text{ }\text{ }\mathrm{eV}$ at 99% confidence, marginalized over host halo circular velocity. This constraint is conservative as it is derived under the assumption that soliton heating is negligible, and that no other sources of non-FDM dynamical heating of stars operate to increase velocity dispersion. It can potentially be strengthened by future spectroscopic observations of additional stars in…

We study an impact of self-interacting bosonic dark matter (DM) on various observable properties of neutron stars (NSs). The analysis is performed for asymmetric DM with masses from few MeV to GeV, the self-coupling constant of order $\mathcal{O}(1)$ and various DM fractions. Allowing a mixture between DM and baryonic matter, the formation of a dense DM core or an extended dark halo has been explored. We find that both distribution regimes crucially depend on the mass and fraction of DM for sub-GeV boson masses in the strong coupling regime. From the combined analysis of the mass-radius relation and the tidal deformability of compact stars including bosonic DM, we set a stringent constraint on DM fraction. We conclude that observations of $2\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$ NSs together with ${\mathrm{\ensuremath{\Lambda}}}_{1.4}\ensuremath{\le}580$ constraint, set by LIGO/Virgo Collaboration, favor sub-GeV DM particles with low fractions below $\ensuremath{\sim}5%$.

A novel mechanism for the primordial black hole (PBH) production is proposed as a natural and inevitable consequence of general first-order phase transitions without reference to specific underlying particle physics models. We obtain mutual predictions and constraints between primordial black holes and gravitational waves from phase transitions in the general case. For particular interest, our PBHs generated during a PeV-scale phase transition could make up all the dark matter, while PBHs generated during a MeV-scale phase transition could simultaneously account for LIGO-Virgo coalescence events and NANOGrav 12.5-yr result for the corresponding gravitational waves.

We argue that if the Newtonian gravitational field of a body can mediate entanglement with another body, then it should also be possible for the body producing the Newtonian field to entangle directly with on-shell gravitons. Our arguments are made by revisiting a gedankenexperiment previously analyzed by Belenchia et al., which showed that a quantum superposition of a massive body requires both quantized gravitational radiation and local vacuum fluctuations of the spacetime metric in order to avoid contradictions with complementarity and causality. We provide a precise and rigorous description of the entanglement and decoherence effects occurring in this gedankenexperiment, thereby significantly improving upon the back-of-the-envelope estimates given by Belenchia et al. and also showing that their conclusions are valid in much more general circumstances. As a by-product of our analysis, we show that under the protocols of the gedankenexperiment, there is no clear distinction between entanglement mediated by the Newtonian gravitational field of a body and entanglement mediated by…

Simpson-Visser (SV) spacetimes are the simplest globally regular modifications of the Schwarzschild, Reissner-Nordsr\"om and other black hole solutions of general relativity. They smoothly interpolate between these black holes and traversable wormholes. After a brief presentation of the Schwarzschild-like and Reissner-Nordsr\"om-like SV geometries, including their Carter-Penrose diagrams, we show that any static, spherically symmetric SV metric can be obtained as an exact solution to the Einstein field equations sourced by a combination of a minimally coupled phantom scalar field with a nonzero potential $V(\ensuremath{\phi})$ and a magnetic field in the framework of nonlinear electrodynamics with the Lagrangian $\mathcal{L}(F)$, $\mathcal{F}={F}_{\ensuremath{\mu}\ensuremath{\nu}}{F}^{\ensuremath{\mu}\ensuremath{\nu}}$ (in standard notations). Explicit forms of $V(\ensuremath{\phi})$ and $\mathcal{L}(F)$ are presented for the cases of Schwarzschild-like and Reissner-Nordsr\"om-like SV metrics.

We revisit the possibility that the stochastic common-spectrum process recently detected by the NANOGrav pulsar timing array experiment could be due to primordial gravitational waves (GWs). A na\"{\i}ve extrapolation down to interferometer scales of the blue GW spectrum required to explain NANOGrav consistently with cosmic microwave background (CMB) observations would strongly violate upper limits on the stochastic GW background (SGWB) amplitude from Laser Interferometer Gravitational Wave Observatory/Virgo. In combination with the fact that there are over 19 decades in frequency between CMB and interferometer scales, this motivates us to move beyond the commonly adopted approximation of a pure power-law GW spectrum. We consider a broken power-law parametrization for the SGWB spectrum, which turns from blue to red above the break frequency: while phenomenological, this choice maps to various well-motivated early-Universe models, including scenarios featuring noninstantaneous reheating or a nonstandard background expansion following reheating. After a detailed discussion of the…

We give explicit expressions for the finite frequency greybody factor, quasinormal modes, and Love numbers of Kerr black holes by computing the exact connection coefficients of the radial and angular parts of the Teukolsky equation. This is obtained by solving the connection problem of the confluent Heun equation in terms of the explicit expression of irregular Virasoro conformal blocks as sums over partitions via the Alday, Gaiotto, and Tachikawa correspondence. In the relevant approximation limits our results are in agreement with existing literature. The method we use can be extended to solve the linearized Einstein equation in other interesting gravitational backgrounds.

A coupled-channel approach is applied to the charged tetraquark state ${T}_{cc}^{+}$ recently discovered by the LHCb Collaboration. The parameters of the interaction are fixed by a fit to the observed line shape in the three-body ${D}^{0}{D}^{0}{\ensuremath{\pi}}^{+}$ channel. Special attention is paid to the three-body dynamics in the ${T}_{cc}^{+}$ due to the finite life time of the ${D}^{*}$. An approach to the ${T}_{cc}^{+}$ is argued to be self-consistent only if both manifestations of the three-body dynamics, the pion exchange between the $D$ and ${D}^{*}$ mesons and the finite ${D}^{*}$ width, are taken into account simultaneously to ensure that three-body unitarity is preserved. This is especially important to precisely extract the pole position in the complex energy plane whose imaginary part is very sensitive to the details of the coupled-channel scheme employed. The ${D}^{0}{D}^{0}$ and ${D}^{0}{D}^{+}$ invariant mass distributions, predicted based on this analysis, are in good agreement with the LHCb data. The low-energy expansion of the ${D}^{*}D$ scattering amplitude…

In this present work, we study the observational appearance of Kerr-Melvin black hole (KMBH) illuminated by an accretion disk. The accretion disk is assumed to be located on the equatorial plane and to be thin both geometrically and optically. Considering the fact that outside the innermost stable circular orbit (ISCO) the accretion flow moves in prograde or retrograde circular orbit and falls toward the horizon along plunging orbit inside the ISCO, we develop the numerical backward ray-tracing method and obtain the images of KMBH accompanying with the accretion disk for various black hole spins, strengths of magnetic fields, and inclination angles of observers. We present the intensity distribution horizontally and longitudinally and show the profiles of the redshift for the direct and lensed images. Our study suggests that the inner shadow and critical curves can be used to estimate the magnetic field around a black hole without degeneration.

We use redshift-space galaxy clustering data from the BOSS survey to constrain local primordial non-Gaussianity (LPNG). This is of particular importance due to the consistency relations, which imply that a detection of LPNG would rule out all single-field inflationary models. Our constraints are based on the consistently analyzed redshift-space galaxy power spectra and bispectra, extracted from the public BOSS data with optimal window-free estimators. We use a complete perturbation theory model including all one-loop power spectrum corrections generated by LPNG. Our constraint on the amplitude of the local non-Gaussian shape is ${f}_{\mathrm{NL}}^{\text{local}}=\ensuremath{-}33\ifmmode\pm\else\textpm\fi{}28$ at 68% C.L., yielding no evidence for primordial non-Gaussianity. The addition of the bispectrum tightens the ${f}_{\mathrm{NL}}^{\text{local}}$ constraints from BOSS by 20%, and allows breaking of degeneracies with non-Gaussian galaxy bias. These results set the stage for the analysis of future surveys, whose larger volumes will yield significantly tighter constraints on LPNG.

The thermodynamic Euler equation for high-energy states of large-$N$ gauge theories is derived from the dependence of the extensive quantities on the number of colors $N$. This Euler equation relates the energy of the state to the temperature, entropy, number of degrees of freedom and its chemical potential, but not to the volume or pressure. In the context of the gauge/gravity duality we show that the Euler equation is dual to the generalized Smarr formula for black holes in the presence of a negative cosmological constant. We also match the fundamental variational equation of thermodynamics to the first law of black hole mechanics, when extended to include variations of the cosmological constant and Newton's constant.

We construct an inspiral-merger-ringdown eccentric gravitational-wave (GW) model for binary black holes with non-precessing spins within the effective-one-body formalism. This waveform model, SEOBNRv4EHM, extends the accurate quasi-circular SEOBNRv4HM model to eccentric binaries by including recently computed eccentric corrections up to 2PN order in the gravitational waveform modes, notably the $(l,|m|)=(2,2),(2,1),(3,3),(4,4),(5,5)$ multipoles. The waveform model reproduces the zero eccentricity limit with an accuracy comparable to the underlying quasicircular model, with the unfaithfulness of $\ensuremath{\lesssim}1%$ against quasicircular numerical-relativity (NR) simulations. When compared against 28 public eccentric NR simulations from the Simulating eXtreme Spacetimes catalog with initial orbital eccentricities up to $e\ensuremath{\simeq}0.3$ and dimensionless spin magnitudes up to $+0.7$, the model provides unfaithfulness $<1%$, showing that both the $(2,|2|)$-modes and the higher-order modes are reliably described without calibration to NR datasets in the eccentric sector.…

We model the supermassive dark object $M8{7}^{*}$ as a Schwarzschild lens and study the variations in tangential, radial, and total (the product of tangential and radial) magnifications of images (primary, secondary, and relativistic) against the changes in angular source position and the ratio of lens-source to the observer-source distance. Further, we study the behavior of partial derivatives (with respect to the angular source position) of total magnifications of images against the angular source position. Finally, we model supermassive dark objects at centers of 40 galaxies as Schwarzschild lenses and study the variations in tangential, radial, and total magnifications of images against the change in the ratio of mass of the lens to its distance. These studies yield many nonintuitive results which are likely to be significant for next generation Event Horizon Telescope observations. We hypothesize that there exists a distortion parameter such that its signed sum for all images of singular gravitational lensing of a source identically vanishes. We test this with images of…

The observed pattern of linear polarization of the cosmic microwave background photons is a sensitive probe of physics violating parity symmetry under inversion of spatial coordinates. A new parity-violating interaction might have rotated the plane of linear polarization by an angle $\ensuremath{\beta}$ as the cosmic microwave background photons have been traveling for more than 13 billion years. This effect is known as ``cosmic birefringence.'' In this paper, we present new measurements of cosmic birefringence from a joint analysis of polarization data from two space missions, $Planck$ and WMAP. This dataset covers a wide range of frequencies from 23 to 353 GHz. We measure $\ensuremath{\beta}=0.342{\ifmmode^\circ\else\textdegree\fi{}}_{\ensuremath{-}0.091\ifmmode^\circ\else\textdegree\fi{}}^{+0.094\ifmmode^\circ\else\textdegree\fi{}}$ [68% confidence level (CL)] for nearly full-sky data, which excludes $\ensuremath{\beta}=0$ at 99.987% CL. This corresponds to the statistical significance of $3.6\ensuremath{\sigma}$. There is no evidence for frequency dependence of…

Black hole (BH) shadows can be used to probe new physics in the form of ultralight particles via the phenomenon of superradiant instability. By directly affecting the BH mass and spin, superradiance can lead to a time evolution of the BH shadow, which nonetheless has been argued to be unobservable through very-long-baseline interferometry (VLBI) over realistic observation time scales. We revisit the superradiance-induced BH shadow evolution including the competing effects of gas accretion and gravitational wave (GW) emission and, as a first step towards modeling realistic new physics scenarios which predict the existence of multiple ultralight species, we study the system in the presence of two ultralight bosons, whose combined effect could help reduce the shadow evolution time scale. We find that accretion and GW emission play a negligible role in our results (justifying previous simplified analyses), and that contrary to our intuition the inclusion of an additional ultralight boson does not shorten the BH shadow evolution time scale and hence improve detection prospects. However,…

If dark matter interacts with the Standard Model only gravitationally its abundance in the universe could be explained by the evaporation of primordial black holes (PBH) through Hawking radiation which ``democratically'' emits all existing particles. In these two papers, the authors study this scenario in great detail, significantly improving on previous calculations, and eventually include also interactions with the Standard Model. One curious observation is the strong dependence of the necessary density of PBH on the spin of the dark matter particles.

Superradiant instabilities may create clouds of ultralight bosons around rotating black holes, forming so-called "gravitational atoms".It was recently shown that the presence of a binary companion can induce resonant transitions between bound states of these clouds, whose backreaction on the binary's orbit leads to characteristic signatures in the emitted gravitational waves.In this work, we show that the interaction with the companion can also trigger transitions from bound to unbound states of the cloud-a process that we refer to as "ionization" in analogy with the photoelectric effect in atomic physics.The orbital energy lost in the process overwhelms the losses due to gravitational wave emission and contains sharp features carrying information about the energy spectrum of the cloud.Moreover, we also show that if the companion is a black hole, then the part of the cloud impinging on the event horizon will be absorbed.This "accretion" leads to a significant increase of the companion's mass, which alters the dynamical evolution and ensuing waveform of the binary.We argue that a…

Early dark energy (EDE) offers a particularly interesting theoretical approach to the Hubble tension, albeit one that introduces its own set of challenges, including a new ``why then'' problem related to the EDE injection time at matter-radiation equality, and a mild worsening of the large-scale structure (LSS) tension. Both these challenges center on the properties of dark matter, which becomes the dominant component of the Universe at EDE injection and is also responsible for seeding LSS. Motivated by this, we present the potential of couplings between EDE and dark matter to address these challenges, focusing on a mechanism similar to chameleon dark energy theories, deeming this chameleon early dark energy (CEDE). We present relevant background and perturbation equations and study the dynamics of the case of a quartic scalar potential and an exponential coupling.

Recent population studies have searched for a subpopulation of primordial black holes (PBHs) in the gravitational-wave (GW) events so far detected by LIGO/Virgo/KAGRA (LVK), in most cases adopting a phenomenological PBH mass distribution. When deriving such a population from first principles in the standard scenario, however, the equation of state of the Universe at the time of PBH formation may strongly affect the PBH abundance and mass distribution, which ultimately depend on the power spectrum of cosmological perturbations. Here we improve on previous population studies on several aspects: (i) we adopt state-of-the-art PBH formation models describing the collapse of cosmological perturbations across the QCD epoch; (ii) we perform the first Bayesian multipopulation inference on GW data including PBHs and directly using power spectrum parameters instead of phenomenological distributions; (iii) we critically confront the PBH scenario with LVK phenomenological models describing the GWTC-3 catalog both in the neutron-star and in the BH mass ranges, also considering PBHs as a…

Parity-violating physics in the early universe can leave detectable traces in late-time observables. While vector- and tensor-type parity violation can be observed in the $B$-modes of the cosmic microwave background, scalar-type signatures are visible only in the four-point correlation function (4PCF) and beyond. This work presents a blind test for parity violation in the 4PCF of the baryon oscillation spectroscopic survey (BOSS) CMASS sample, considering galaxy separations in the range $[20,160]\text{ }\text{ }{h}^{\ensuremath{-}1}\text{ }\mathrm{Mpc}$. The parity-odd 4PCF contains no contributions from standard $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ physics and can be efficiently measured using recently developed estimators. Data are analyzed using both a nonparametric rank test (comparing the BOSS 4PCFs to those of realistic simulations) and a compressed ${\ensuremath{\chi}}^{2}$ analysis, with the former avoiding the assumption of a Gaussian likelihood. These find similar results, with the rank test giving a detection probability of 99.6% ($2.9\ensuremath{\sigma}$). This…

The terminal wall velocity of a first-order phase transition bubble in the early Universe can be calculated from a set of fluid equations describing the scalar fields and the plasma's state. We rederive these equations from the energy-momentum tensor conservation and the Boltzmann equation, without linearizing in the background temperature and fluid velocity. The resulting equations have a finite solution for any wall velocity. We propose a spectral method to integrate the Boltzmann equation, which is simple, efficient, and accurate. As an example, we apply this new methodology to the singlet scalar extension of the standard model. We find that all solutions are naturally categorized as deflagrations (${v}_{w}\ensuremath{\sim}{c}_{s}$) or ultrarelativistic detonations (${\ensuremath{\gamma}}_{w}\ensuremath{\gtrsim}10$). Furthermore, the contributions from out-of-equilibrium effects are, most of the time, subdominant. Finally, we use these results to propose several approximation schemes with increasing levels of complexity and accuracy. They can be used to considerably simplify the…

The early dark energy (EDE) scenario aims to increase the value of the Hubble constant (${H}_{0}$) inferred from cosmic microwave background (CMB) data over that found in the standard cosmological model ($\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$), via the introduction of a new form of energy density in the early Universe. The EDE component briefly accelerates cosmic expansion just prior to recombination, which reduces the physical size of the sound horizon imprinted in the CMB. Previous work has found that nonzero EDE is not preferred by Planck CMB power spectrum data alone, which yield a 95% confidence level (C.L.) upper limit ${f}_{\mathrm{EDE}}<0.087$ on the maximal fractional contribution of the EDE field to the cosmic energy budget. In this paper, we fit the EDE model to CMB data from the Atacama Cosmology Telescope (ACT) data release 4. We find that a combination of ACT, large-scale Planck TT (similar to WMAP), Planck CMB lensing, and BAO data prefers the existence of EDE at $>99.7%\text{ }\text{ }\mathrm{C}.\mathrm{L}.$:…

We study the strong gravitational lensing effect around rotating black holes in different gravity theories. By calculating the deflection angle of strong gravitational lensing, we evaluate the lensing observables including the image position, separation, magnification, and the time delays between the relativistic images of different rotating black holes. We argue that the differences in image positions, separations between the rotating black hole in modified gravity (MOG) theory and the Kerr black hole in general relativity (GR) are more significant in SgrA* than those in M87*; however the differences in time delays between rotating black holes in MOG and GR are shorter in SgrA* than that in M87*. Our evaluations on lensing observables in the strong gravity regime can help to distinguish the MOG from GR. Furthermore, we investigate the shadow observables of different rotating black holes. Employing the Event Horizon Telescope observations on the angular shadow radius for supermassive M87* and SgrA* black holes, respectively, we estimate the ranges of MOG parameter and obtain its…

We present imrphenomtphm, a phenomenological model for the gravitational-wave signals emitted by the coalescence of quasicircular precessing binary black holes systems. The model is based on the ``twisting up'' approximation, which maps nonprecessing signals to precessing ones in terms of a time-dependent rotation which can be described by three Euler angles and which has been utilized in several frequency-domain waveform models that have become standard tools in gravitational-wave data analysis as well as in several time-domain models. Our model is constructed in the time domain, applying the twisting up approximation to the nonprecessing multimode model imrphenomthm, which allows several improvements over the frequency-domain models; we do not use the stationary phase approximation, we employ a simple approximation for the precessing Euler angles for the ringdown signal, and we implement a new method for computing the Euler angles through the evolution of the spin dynamics of the system, which is more accurate and also computationally efficient.

In this work, we obtain the shadow images of spherically symmetric scalar boson and Proca stars using analytical fittings of numerical solutions, when illuminated by a geometrically thin accretion disk. We chose a sample of four boson and four Proca stars with radii ranging from more compact configurations with $R\ensuremath{\sim}9M$ to more dilute configurations with $R\ensuremath{\sim}20M$, where $M$ is the total mass of the bosonic star. In these configurations, the absence of the light sphere (the locus of unstable bound geodesics) makes the optical appearance of these stars to be dominated by a single luminous ring enclosing a central brightness depression, and no further photon rings are available. We show that if one considers face-on observations and a disk model whose emission is truncated at some finite radius at which the luminosity attains its maximum value, both the size of the shadow, as well as the luminosity and depth of the bright region, are heavily influenced by the emission profile, with the choice of the type and parameters of the bosonic stars in our samples…

Optimal extraction of the non-Gaussian information encoded in the large-scale structure of the Universe lies at the forefront of modern precision cosmology. We propose achieving this task through the use of the wavelet scattering transform (WST), which subjects an input field to a layer of nonlinear transformations that are sensitive to non-Gaussianity in spatial density distributions. In order to assess its applicability in the context of large-scale structure surveys, we apply the WST on the 3D overdensity field obtained by the Quijote simulations, out of which we extract the Fisher information in six cosmological parameters. WST delivers a large improvement in the marginalized errors on all parameters, ranging between $1.2\ensuremath{-}4\ifmmode\times\else\texttimes\fi{}\mathrm{tighter}$ than the corresponding ones obtained from the regular 3D cold dark $\mathrm{matter}+\text{baryon}$ power spectrum, as well as a 50% improvement over the neutrino mass constraint given by the marked power spectrum. Through this first application on 3D cosmological fields, we demonstrate the great…

Emerging high-redshift cosmological probes, in particular quasars (QSOs), show a preference for larger matter densities, ${\mathrm{\ensuremath{\Omega}}}_{m}\ensuremath{\approx}1$, within the flat $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ framework. Here, using the Risaliti-Lusso relation for standardizable QSOs, we demonstrate that the QSOs recover the same Planck-$\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ universe as type Ia supernovae (SN), ${\mathrm{\ensuremath{\Omega}}}_{m}\ensuremath{\approx}0.3$ at lower redshifts $0

Thermodynamics of black holes in anti--de Sitter (AdS) spacetimes typically contain critical points in the phase diagram, some of which correspond to the first order transition ending in a second order one. Following the recent proposal in [Phys. Rev. D 105, 104003 (2022)] on using Duan's $\ensuremath{\phi}$-mapping theory, we classify the critical points of six dimensional charged Gauss-Bonnet black holes in AdS spacetime. We find that the higher derivative curvature terms in the form of Gauss-Bonnet gravity do not change the topological class of critical points in charged black holes in AdS, unlike the case of Born-Infeld corrections noted earlier. The connection between the topological nature of critical points and existence of first order phase transitions breaks down in a certain parameter regime. A resolution is proposed by treating the novel and conventional critical points as phase creation and phase annihilation points, respectively. Examples are provided to support the proposal.

A 10% difference in the scale for the Hubble parameter constitutes a clear problem for cosmology. Here, considering angular distribution of type Ia supernovae (SN) within the Pantheon compilation and working within flat $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ cosmology, we observe a correlation between higher ${H}_{0}$ and the CMB dipole direction, confirming our previous results for strongly lensed quasars [Classical Quantum Gravity 38, 184001 (2021)]. Concretely, we record a $\ensuremath{\sim}1\text{ }\text{ }\mathrm{km}/\mathrm{s}/\mathrm{Mpc}$ variation in ${H}_{0}$ at antipodal points on the sky within the Pantheon sample, which is evident in the Low $z$ subsample ($z\ensuremath{\lesssim}0.075$) and gets enhanced by higher redshift SN. Our work raises the possibility that we may be at the precision required to probe anisotropic Hubble expansions, while providing a concrete prediction for future inferences of ${H}_{0}$.

Measurement of spin-precession in black hole binary mergers observed with gravitational waves is an exciting milestone as it relates to both general relativistic dynamics and astrophysical binary formation scenarios. In this study, we revisit the evidence for spin-precession in GW200129 and localize its origin to data in LIGO Livingston in the 20--50 Hz frequency range where the signal amplitude is lower than expected from a nonprecessing binary given all the other data. These data are subject to known data quality issues as a glitch was subtracted from the detector's strain data. The lack of evidence for spin-precession in LIGO Hanford leads to a noticeable inconsistency between the inferred binary mass ratio and precessing spin in the two LIGO detectors, something not expected from solely different Gaussian noise realizations. We revisit the LIGO Livingston glitch mitigation and show that the difference between a spin-precessing and a nonprecessing interpretation for GW200129 is smaller than the statistical and systematic uncertainty of the glitch subtraction, finding that the…

The lack of evidence for new interactions and particles at the Large Hadron Collider (LHC) has motivated the high-energy physics community to explore model-agnostic data-analysis approaches to search for new physics. Autoencoders are unsupervised machine learning models based on artificial neural networks, capable of learning background distributions. We study quantum autoencoders based on variational quantum circuits for the problem of anomaly detection at the LHC. For a QCD $t\overline{t}$ background and resonant heavy-Higgs signals, we find that a simple quantum autoencoder outperforms classical autoencoders for the same inputs and trains very efficiently. Moreover, this performance is reproducible on present quantum devices. This shows that quantum autoencoders are good candidates for analysing high-energy physics data in future LHC runs.

An improved measurement of the decay B 0 s → µ + µ -and searches for the decays B 0 → µ + µ -and B 0 s → µ + µ -γ are performed at the LHCb experiment using data collected in proton-proton collisions at √ s = 7, 8 and 13 TeV, corresponding to integrated luminosities of 1, 2 and 6 fb -1 , respectively.The B 0 s → µ + µ -branching fraction and effective lifetime are measured to be B(B 0 s → µ + µ -) = 3.09 + 0.46 + 0.15 -0.43 -0.11 × 10 -9 and τ (B 0 s → µ + µ -) = (2.07 ± 0.29 ± 0.03) ps, respectively, where the uncertainties include both statistical and systematic contributions.No significant signal for B 0 → µ + µ -and B 0 s → µ + µ -γ decays is found and the upper limits -9 at 95% confidence level are determined, where the latter is limited to the range m µµ > 4.9 GeV/c 2 .Additionally, the ratio between the B 0 → µ + µ -and B 0 s → µ + µ -branching fractions is measured to be R µ + µ -< 0.095 at 95% confidence level.The results are in agreement with the Standard Model predictions.

We present results of an all-sky search for continuous gravitational waves which can be produced by spinning neutron stars with an asymmetry around their rotation axis, using data from the third observing run of the Advanced LIGO and Advanced Virgo detectors. Four different analysis methods are used to search in a gravitational-wave frequency band from 10 to 2048 Hz and a first frequency derivative from $\ensuremath{-}{10}^{\ensuremath{-}8}$ to ${10}^{\ensuremath{-}9}\text{ }\text{ }\mathrm{Hz}/\mathrm{s}$. No statistically significant periodic gravitational-wave signal is observed by any of the four searches. As a result, upper limits on the gravitational-wave strain amplitude ${h}_{0}$ are calculated. The best upper limits are obtained in the frequency range of 100 to 200 Hz and they are $\ensuremath{\sim}1.1\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}25}$ at 95% confidence level. The minimum upper limit of $1.10\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}25}$ is achieved at a frequency 111.5 Hz. We also place constraints on the rates and abundances of nearby…

We propose a new model-agnostic search strategy for physics beyond the standard model (BSM) at the LHC, based on a novel application of neural density estimation to anomaly detection. Our approach, which we call classifying anomalies through outer density estimation (cathode), assumes the BSM signal is localized in a signal region (defined e.g., using invariant mass). By training a conditional density estimator on a collection of additional features outside the signal region, interpolating it into the signal region, and sampling from it, we produce a collection of events that follow the background model. We can then train a classifier to distinguish the data from the events sampled from the background model, thereby approaching the optimal anomaly detector. Using the LHC Olympics R dataset, we demonstrate that cathode nearly saturates the best possible performance, and significantly outperforms other approaches that aim to enhance the bump hunt (cwola hunting and anode). Finally, we demonstrate that cathode is very robust against correlations between the features and maintains…

Delayed single- and few-electron emissions plague dual-phase time projection chambers, limiting their potential to search for light-mass dark matter. This paper examines the origins of these events in the XENON1T experiment. Characterization of the intensity of delayed electron backgrounds shows that the resulting emissions are correlated, in time and position, with high-energy events and can effectively be vetoed. In this work we extend previous S2-only analyses down to a single electron. From this analysis, after removing the correlated backgrounds, we observe rates $<30\text{ }\mathrm{events}/(\mathrm{electron}\ifmmode\times\else\texttimes\fi{}\mathrm{kg}\ifmmode\times\else\texttimes\fi{}\mathrm{day})$ in the region of interest spanning 1 to 5 electrons. We derive 90% confidence upper limits for dark matter-electron scattering, first direct limits on the electric dipole, magnetic dipole, and anapole interactions, and bosonic dark matter models, where we exclude new parameter space for dark photons and solar dark photons.

In astrophysical environments with a large number of neutrinos, such as supernovae, neutrinos exhibit nonlinear flavor oscillations due to interactions with the dense neutrino background. Characterizing the features of these flavor conversions is a difficult problem. The present paper by Taiki Morinaga makes a significant contribution by establishing rigorously the sufficient and necessary conditions under which so-called fast neutrino flavor instabilities arise.

Large dark matter overdensities can form around black holes of astrophysical and primordial origin as they form and grow. This ``dark dress'' inevitably affects the dynamical evolution of binary systems and induces a dephasing in the gravitational waveform that can be probed with future interferometers. In this paper, we introduce a new analytical model to rapidly compute gravitational waveforms in the presence of an evolving dark matter distribution. We then present a Bayesian analysis determining when dressed black hole binaries can be distinguished from GR-in-vacuum ones and how well their parameters can be measured, along with how close they must be to be detectable by the planned Laser Interferometer Space Antenna (LISA). We show that LISA can definitively distinguish dark dresses from standard binaries and characterize the dark matter environments around astrophysical and primordial black holes for a wide range of model parameters. Our approach can be generalized to assess the prospects for detecting, classifying, and characterizing other environmental effects in gravitational…

We present the results obtained from the full-shape cosmology analysis of the redshift-space power spectra for four galaxy samples of the SDSS-III BOSS DR12 galaxy catalog over $0.2<z<0.75$. For the theoretical template, we use an emulator that was built from an ensemble set of $N$-body simulations, which enables fast and accurate computation of the redshift-space power spectrum of ``halos.'' Combining with the halo occupation distribution to model the galaxy-halo connection, we can compute the redshift-space power spectrum of BOSS-like galaxies in less than a CPU second, for an input model under flat $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ cosmology. In our cosmology inference, we use the monopole, quadrupole, and hexadecapole moments of the redshift-space power spectrum and include seven nuisance parameters, with broad priors, to model uncertainties in the galaxy-halo connection for each galaxy sample, but do not use any information on the abundance of galaxies. We demonstrate a validation of our analysis pipeline using the mock catalogs of BOSS-like galaxies, generated using…

We present angular diameter measurements obtained by measuring the position of baryon acoustic oscillations (BAO) in an optimized sample of galaxies from the first three years of Dark Energy Survey data (DES Y3). The sample consists of 7 million galaxies distributed over a footprint of $4100\text{ }\text{ }{\mathrm{deg}}^{2}$ with $0.6<{z}_{\text{photo}}<1.1$ and a typical redshift uncertainty of $0.03(1+z)$. The sample selection is the same as in the BAO measurement with the first year of DES data, but the analysis presented here uses three times the area, extends to higher redshift, and makes a number of improvements, including a fully analytical BAO template, the use of covariances from both theory and simulations, and an extensive preunblinding protocol. We used two different statistics; angular correlation function and power spectrum, and validate our pipeline with an ensemble of over 1500 realistic simulations. Both statistics yield compatible results. We combine the likelihoods derived from angular correlations and spherical harmonics to constrain the ratio of comoving…

We present simulations of nonequilibrium dynamics of quantum field theories on digital quantum computers. As a representative example, we consider the Schwinger model, a ($1+1$)-dimensional U(1) gauge theory, coupled through a Yukawa-type interaction to a thermal environment described by a scalar field theory. We use the Hamiltonian formulation of the Schwinger model discretized on a spatial lattice. With the thermal scalar fields traced out, the Schwinger model can be treated as an open quantum system and its real-time dynamics are governed by a Lindblad equation in the Markovian limit. The interaction with the environment ultimately drives the system to thermal equilibrium. In the quantum Brownian motion limit, the Lindblad equation is related to a field theoretical Caldeira-Leggett equation. By using the Stinespring dilation theorem with ancillary qubits, we perform studies of both the nonequilibrium dynamics and the preparation of a thermal state in the Schwinger model using IBM's simulator and quantum devices. The real-time dynamics of field theories as open quantum systems and…

We consider the production of matter and radiation during reheating after inflation, restricting our attention solely to gravitational interactions. Processes considered are the exchange of a graviton, ${h}_{\ensuremath{\mu}\ensuremath{\nu}}$, involved in the scattering of the inflaton or particles in the newly created radiation bath. In particular, we consider the gravitational production of dark matter (scalar or fermionic) from the thermal bath as well as from scattering of the inflaton condensate. We also consider the gravitational production of radiation from inflaton scattering. In the latter case, we also derive a lower bound on the maximal temperature of order of ${10}^{12}\text{ }\text{ }\mathrm{GeV}$ for a typical $\ensuremath{\alpha}$-attractor scenario from $\ensuremath{\phi}\ensuremath{\phi}\ensuremath{\rightarrow}{h}_{\ensuremath{\mu}\ensuremath{\nu}}\ensuremath{\rightarrow}$ Standard Model fields (dominated by the production of Higgs bosons). This lower gravitational bound becomes the effective maximal temperature for reheating temperatures,…

This paper points out the importance of the quantum nature of the gravitational interaction with matter in a linearized theory of quantum gravity induced entanglement of masses. We will show how the quantum interaction entangles the steady states of a closed system (eigenstates) of two test masses placed in the harmonic traps, and how such a quantum matter-matter interaction emerges from an underlying quantum gravitational field. We will rely upon quantum perturbation theory highlighting the critical assumptions for generating a quantum matter-matter interaction and showing that a classical gravitational field does not render such an entanglement. We will consider two distinct examples: one where the two harmonic oscillators are static, and the other where the harmonic oscillators are nonstatic. In both cases it is the quantum nature of the gravitons interacting with the harmonic oscillators that are responsible for creating an entangled state with the ground and the excited states of harmonic oscillators as the Schmidt basis. We will compute the concurrence as a criterion for the…

We derive relativistic second-order dissipative fluid-dynamical equations of motion for massive spin-$1/2$ particles from kinetic theory using the method of moments. Besides the usual conservation laws for charge, energy, and momentum, such a theory of relativistic dissipative spin hydrodynamics features an equation of motion for the rank-3 spin tensor, which follows from the conservation of total angular momentum. Extending the conventional method of moments for spin-0 particles, we expand the spin-dependent distribution function near local equilibrium in terms of moments of the momentum and spin variables. We work to next-to-leading order in the Planck constant $\ensuremath{\hbar}$. As shown in previous work, at this order in $\ensuremath{\hbar}$ the Boltzmann equation for spin-$1/2$ particles features a nonlocal collision term. From the Boltzmann equation, we then obtain an infinite set of equations of motion for the irreducible moments of the deviation of the single-particle distribution function from local equilibrium. In order to close this system of moment equations, a…

We investigate constraints on early dark energy (EDE) using ACT DR4, SPT-3G 2018, Planck polarization, and restricted Planck temperature data (at $\ensuremath{\ell}<650$), finding a $3.3\ensuremath{\sigma}$ preference ($\mathrm{\ensuremath{\Delta}}{\ensuremath{\chi}}^{2}=\ensuremath{-}16.2$ for three additional degrees of freedom) for EDE over $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$. The EDE contributes a maximum fractional energy density of ${f}_{\mathrm{EDE}}({z}_{c})=0.16{3}_{\ensuremath{-}0.04}^{+0.047}$ at a redshift ${z}_{c}=3357\ifmmode\pm\else\textpm\fi{}200$ and leads to a CMB inferred value of the Hubble constant ${H}_{0}={74.2}_{\ensuremath{-}2.1}^{+1.9}\text{ }\text{ }\mathrm{km}/\mathrm{s}/\mathrm{Mpc}$. We find that Planck and ACT DR4 data provide the majority of the improvement in ${\ensuremath{\chi}}^{2}$, and that the inclusion of SPT-3G pulls the posterior of ${f}_{\mathrm{EDE}}({z}_{c})$ away from $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$. This is the first time that a moderate preference for EDE has been reported for these combined CMB datasets including…

The detection of $\ensuremath{\sim}50$ coalescing compact binaries with the Advanced LIGO and Virgo detectors has allowed us to test general relativity, constrain merger rates, and look for evidence of tidal effects, compact object spins, higher waveform modes, and black hole ringdowns. An effect that has not yet been confidently detected is binary eccentricity, which might be present in a small fraction of binaries formed dynamically. Here we discuss general limits on eccentricity that can, in-principle, be placed on all types of compact object binaries by a detector operating at the design sensitivity of Advanced LIGO. Using a post-Newtonian model for gravitational-wave phasing valid in the small eccentricity regime, we assess the relative measurement error for eccentricity for a variety of spinning and nonspinning binaries. Errors and correlations involving the mass and spin parameters are also investigated. We find that decreasing the low frequency limit of a detector's observational frequency band is one of the key design factors for increasing the odds of measuring binary…

Based on the assumption that quasars (QSOs) and gamma-ray bursts (GRBs) represent standardizable candles, we provide evidence that the Hubble constant ${H}_{0}$ adopts larger values in hemispheres aligned with the cosmic microwave background (CMB) dipole direction. If substantiated, this trend signals a departure from Friedmann-Lema\^{\i}tre-Robertson-Walker cosmology. In particular, QSOs show a definite trend, whereas our findings in GRBs are consistent with an isotropic universe, but we show in a sample of GRBs calibrated with type Ia supernovae (SNe) that this conclusion may change as one focuses on GRBs more closely (mis)aligned with the CMB dipole direction. The statistical significance in QSOs alone is $\ensuremath{\gtrsim}2\ensuremath{\sigma}$, and when combined with similar trends in strong lensing, type Ia SNe, and calibrated GRBs, this increases to $\ensuremath{\sim}3\ensuremath{\sigma}$. Our findings are consistent with reported discrepancies in the cosmic dipole and anisotropies in galaxy cluster scaling relations. The reported variations in ${H}_{0}$ across the sky…

Using the Bragg-Williams construction of an off-shell free energy, we calculate the topological charge of the Hawking-Page transition point for black holes in anti--de Sitter. A computation following from a related off-shell effective potential in the boundary gauge dual matches the value of topological charge obtained in the bulk. We also work out the topological charges of the equilibrium phases of these systems, which follow from the saddle points of the appropriate free energy. The locally stable and unstable phases turn out to have topological charges opposite to each other, with the total being zero, in agreement with the result obtained from a recent construction [S.-W. Wei, Y.-X. Liu, and R. B. Mann, arXiv:2208.01932].

We present a high statistics study of the isovector nucleon charges and form factors using seven ensembles of $2+1$-flavor Wilson-clover fermions. The axial vector and pseudoscalar form factors obtained on each of these ensembles satisfy the partially conserved axial current relation between them once the lowest energy $N\ensuremath{\pi}$ excited state is included in the spectral decomposition of the correlation functions used for extracting the ground state matrix elements. Similarly, we find evidence that the $N\ensuremath{\pi}\ensuremath{\pi}$ excited state contributes to the correlation functions with the insertion of the vector current, consistent with the vector meson dominance model. The resulting form factors are consistent with the Kelly parametrization of the experimental electric and magnetic data. Our final estimates for the isovector charges are ${g}_{A}^{u\ensuremath{-}d}=1.32(6)(5{)}_{\mathrm{sys}}$, ${g}_{S}^{u\ensuremath{-}d}=1.06(9)(6{)}_{\mathrm{sys}}$, and ${g}_{T}^{u\ensuremath{-}d}=0.97(3)(2{)}_{\mathrm{sys}}$, where the first error is the overall analysis…

$f(Q)$ gravity is the extension of symmetric teleparallel general relativity (STGR), in which both curvature and torsion vanish and gravity is attributed to nonmetricity. This work performs theoretical analyses of static and spherically symmetric solutions with an anisotropic fluid for general $f(Q)$ gravity. We find that the off-diagonal component of the field equation due to a coincident gauge leads to stringent restrictions on the functional form of $f(Q)$ gravity. In addition, although the exact Schwarzschild solution only exists in STGR, we obtain Schwarzschild-like solutions in nontrivial $f(Q)$ gravity and study its asymptotic behavior and deviation from the exact one.

This paper presents the Summed Parallel Infinite Impulse Response (SPIIR) pipeline used for public alerts during the third advanced LIGO and Virgo observation run (O3 run). The SPIIR pipeline uses infinite impulse response (IIR) filters to perform extremely low-latency matched filtering and this process is further accelerated with graphics processing units (GPUs). It is the first online pipeline to select candidates from multiple detectors using a coherent statistic based on the maximum network likelihood ratio statistic principle. Here we simplify the derivation of this statistic using the singular-value-decomposition (SVD) technique and show that single-detector signal-to-noise ratios from matched filtering can be directly used to construct the statistic. Coherent searches are in general more computationally challenging than coincidence searches due to extra search over sky direction parameters. The search over sky directions follows an embarrassing parallelization paradigm and has been accelerated using GPUs. The detection performance is reported using a segment of public data…

In this work, we study the prospect of detecting the stochastic gravitational-wave background with the TianQin Observatory. We consider sources of both astrophysical and cosmological origin, including stellar-mass binary black holes, binary neutron stars, Galactic white dwarves, inflation, first-order phase transitions, and cosmic defects. For the detector configurations, we consider TianQin, TianQin $\mathrm{I}+\text{II}$, and $\mathrm{TianQin}+\text{LISA}$. We study the detectability of stochastic gravitational-wave backgrounds with both the cross correlation and null channel methods, and present the corresponding power-law integrated sensitivity curves. We introduce the definition of the ``joint foreground'' with a network of detectors. With the joint foreground, the number of resolved double white dwarves in the Galaxy will be increased by 5--22% compared with a simple combination of individual detectors. The astrophysical background is expected to be detectable with a signal-to-noise ratio of 100 after 5 years of operation and dominated by the extragalactic double white…

The $W$ boson mass is one of the most important electroweak precision observables for testing the Standard Model (SM) or its extensions. The very recent measured $W$ boson mass at the Collider Detector at Fermilab (CDF) shows about $7\ensuremath{\sigma}$ deviations from the SM prediction, which may challenge the internal consistency of the SM. By performing the global electroweak fit with the new $W$ boson, we present the new values of the oblique parameters: $S=0.06\ifmmode\pm\else\textpm\fi{}0.10$, $T=0.11\ifmmode\pm\else\textpm\fi{}0.12$, $U=0.13\ifmmode\pm\else\textpm\fi{}0.09$, or $S=0.14\ifmmode\pm\else\textpm\fi{}0.08$, $T=0.26\ifmmode\pm\else\textpm\fi{}0.06$ with $U=0$ and the corresponding correlation matrices, which strongly indicates the need for the nondegenerate multiplets beyond the SM. As a proof-of-concept, we show that the new results can be accommodated in the two-Higgs doublet model, where the charged Higgs boson has to be either heavier or lighter than both two heavy neutral Higgs bosons. The collider search for these non-SM Higgs bosons will provide a…

In this paper we extract from a large-$r$ expansion of the vacuum Einstein's equations a dynamical system governing the time evolution of an infinity of higher-spin charges. Upon integration, we evaluate the canonical action of these charges on the gravity phase space. The truncation of this action to quadratic order and the associated charge conservation laws yield an infinite tower of soft theorems. We show that the canonical action of the higher spin charges on gravitons in a conformal primary basis, as well as conformally soft gravitons reproduces the higher spin celestial symmetries derived from the operator product expansion. Finally, we give direct evidence that these charges form a canonical representation of a ${w}_{1+\ensuremath{\infty}}$ loop algebra on the gravitational phase space.

Black hole spectroscopy with gravitational waves is an important tool to measure the mass and spin of astrophysical black holes and to test their Kerr nature. Next-generation ground- and space-based detectors will observe binary black hole mergers with large signal-to-noise ratios and perform spectroscopy routinely. It was recently shown that small perturbations due, e.g., to environmental effects (the ``flea'') to the effective potential governing gravitational-wave generation and propagation in black hole exteriors (the ``elephant'') can lead to arbitrarily large changes in the black hole's quasinormal spectrum, including the fundamental mode, which is expected to dominate the observed signal. This raises an important question: is the black hole spectroscopy program robust against perturbations? We clarify the physical behavior of time-domain signals under small perturbations in the potential, and we show that changes in the amplitude of the fundamental mode in the prompt ringdown signal are parametrically small. This implies that the fundamental quasinormal mode extracted from…

Spin precession is a generic feature of compact binary coalescences that leaves clear imprints in the gravitational waveforms. Building on previous work, we present an efficient time domain inspiral-merger-ringdown effective-one-body model for precessing binary black holes, which incorporates subdominant modes beyond $\ensuremath{\ell}=2$, and the first effective-one-body frequency domain approximant for precessing binary neutron stars. We validate our model against 99 ``short'' numerical relativity precessing waveforms, where we find median mismatches of $5\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}3}$, $7\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}3}$ at inclinations of 0, $\ensuremath{\pi}/3$, and 21 ``long'' waveforms with median mismatches of $4\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}3}$ and $5\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}3}$ at the same inclinations. Further comparisons against the state-of-the-art nrsur7dq4 waveform model yield median mismatches of $4\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}3}$,…

As cosmological data have improved, tensions have arisen. One such tension is the difference between the locally measured Hubble constant ${H}_{0}$ and the value inferred from the cosmic microwave background (CMB). Interacting radiation has been suggested as a solution, but studies show that conventional models are precluded by high-$\ensuremath{\ell}$ CMB polarization data. It seems at least plausible that a solution may be provided by related models that distinguish between high- and low-$\ensuremath{\ell}$ multipoles. When interactions of strongly-coupled radiation are mediated by a force carrier that becomes nonrelativistic, the dark radiation undergoes a ``step'' in which its relative energy density increases as the mediator deposits its entropy into the lighter species. If this transition occurs while CMB-observable modes are inside the horizon, high- and low-$\ensuremath{\ell}$ peaks are impacted differently, corresponding to modes that enter the horizon before or after the step. These dynamics are naturally packaged into the simplest supersymmetric theory, the Wess-Zumino…

Score-based generative models are a new class of generative algorithms that have been shown to produce realistic images even in high dimensional spaces, currently surpassing other state-of-the-art models for different benchmark categories and applications. In this work we introduce caloscore, a score-based generative model for collider physics applied to calorimeter shower generation. Three different diffusion models are investigated using the Fast Calorimeter Simulation Challenge 2022 dataset. caloscore is the first application of a score-based generative model in collider physics and is able to produce high-fidelity calorimeter images for all datasets, providing an alternative paradigm for calorimeter shower simulation.

The detection of gravitational waves from compact binary mergers by the LIGO/Virgo Collaboration has, for the first time, allowed us to test relativistic gravity in its strong, dynamical, and nonlinear regime, thus opening a new arena to confront general relativity (and modifications thereof) against observations. We consider a theory which modifies general relativity by introducing a scalar field coupled to a parity-violating curvature term known as dynamical Chern-Simons gravity. In this theory, spinning black holes are different from their general relativistic counterparts and can thus serve as probes to this theory. We study linear gravito-scalar perturbations of black holes in dynamical Chern-Simons gravity at leading order in spin and (i) obtain the perturbed field equations describing the evolution of the perturbed gravitational and scalar fields, (ii) numerically solve these equations by direct integration to calculate the quasinormal mode frequencies for the dominant and higher multipoles and tabulate them, (iii) find strong evidence that these rotating black holes are…

This paper describes the first all-sky search for long-duration, quasimonochromatic gravitational-wave signals emitted by ultralight scalar boson clouds around spinning black holes using data from the third observing run of Advanced LIGO. We analyze the frequency range from 20 to 610 Hz, over a small frequency derivative range around zero, and use multiple frequency resolutions to be robust towards possible signal frequency wanderings. Outliers from this search are followed up using two different methods, one more suitable for nearly monochromatic signals, and the other more robust towards frequency fluctuations. We do not find any evidence for such signals and set upper limits on the signal strain amplitude, the most stringent being $\ensuremath{\approx}{10}^{\ensuremath{-}25}$ at around 130 Hz. We interpret these upper limits as both an ``exclusion region'' in the boson mass/black hole mass plane and the maximum detectable distance for a given boson mass, based on an assumption of the age of the black hole/boson cloud system.

The outflows from neutrino-cooled black hole accretion disks formed in neutron-star mergers or cores of collapsing stars are expected to be neutron-rich enough to explain a large fraction of elements created by the rapid neutron-capture process, but their precise chemical composition remains elusive. Here, we investigate the role of fast neutrino flavor conversion, motivated by the findings of our post-processing analysis that shows evidence of electron-neutrino lepton-number crossings deep inside the disk, hence suggesting possibly nontrivial effects due to neutrino flavor mixing. We implement a parametric, dynamically self-consistent treatment of fast conversion in time-dependent simulations and examine the impact on the disk and its outflows. By activating the otherwise inefficient, emission of heavy-lepton neutrinos, fast conversions enhance the disk cooling rates and reduce the absorption rates of electron-type neutrinos, causing a reduction of the electron fraction in the disk by 0.03--0.06 and in the ejected material by 0.01--0.03. The rapid neutron-capture process yields are…

With a key improvement, the auxiliary mass flow method is now able to compute Feynman integrals encountered in cutting-edge collider processes. We have successfully applied it to compute some integrals involved in two-loop electroweak corrections to ${e}^{+}{e}^{\ensuremath{-}}\ensuremath{\rightarrow}HZ$, two-loop QCD corrections to $3j$, $W/Z/H+2j$, $t\overline{t}H$ and $4j$ production at hadron colliders, and three-loop QCD corrections to $t\overline{t}$ production at hadron colliders, all of which are crucial for precision frontier in collider physics in the following decade. Our results are important building blocks and benchmarks for future studies of these processes.

We study gravitational perturbations of slowly rotating black holes in a general effective-field-theory extension of general relativity that includes up to eight-derivative terms. We show that two Schr\"odinger-like equations with spin-dependent effective potentials govern the odd- and even-parity master variables. These equations are coupled for parity-violating corrections, and this coupling affects the quasinormal modes even at linear order in the higher-derivative corrections, due to their isospectrality in general relativity. We provide results for the shifts in the fundamental quasinormal mode frequencies at linear order in the spin, which we expect to be valuable for high-precision phenomenology through future gravitational wave observations.

Light primordial black holes may comprise a dominant fraction of the dark matter in our Universe. This paper critically assesses whether planned and future gravitational wave detectors in the ultrahigh-frequency band could constrain the fraction of dark matter composed of subsolar primordial black holes. Adopting the state-of-the-art description of primordial black hole merger rates, we compare various signals with currently operating and planned detectors. As already noted in the literature, our findings confirm that detecting individual primordial black hole mergers with currently existing and operating proposals remains difficult. Current proposals involving gravitational wave to electromagnetic wave conversion in a static magnetic field and microwave cavities feature a technology gap with respect to the loudest gravitational wave signals from primordial black holes of various orders of magnitude. However, we point out that one recent proposal involving resonant LC circuits represents the best option in terms of individual merger detection prospects in the range…

The gravitational form factors (GFFs) of hadrons encode the matrix elements of the energy-momentum tensor of QCD. These quantities describe how energy, spin, and various mechanical properties of hadrons are carried by their quark and gluon constituents. We present the gluon GFFs of the pion, nucleon, $\ensuremath{\rho}$ meson, and $\mathrm{\ensuremath{\Delta}}$ baryon as functions of the squared momentum transfer $t$ in the region $0\ensuremath{\le}\ensuremath{-}t<2\text{ }\text{ }{\mathrm{GeV}}^{2}$, as determined in a lattice QCD study with pion mass ${m}_{\ensuremath{\pi}}=450(5)\text{ }\text{ }\mathrm{MeV}$. By fitting the extracted GFFs using multipole and z-parameter expansion functional forms, we extract various gluon contributions to the energy, pressure, and shear force distributions of the hadrons in the 3D and 2D Breit frames as well as in the infinite momentum frame. We also obtain estimates for the corresponding gluon mechanical and mass radii, as well as the forward-limit gluon contributions to the momentum fraction and angular momentum of the hadrons.

We study the cosmological information content of the redshift-space galaxy bispectrum monopole at one-loop order in perturbation theory. We incorporate all effects necessary for comparison to data: fourth-order galaxy bias, infrared resummation (accounting for the nonlinear evolution of baryon acoustic oscillations), ultraviolet counterterms, nonlinear redshift-space distortions, stochastic contributions, projection, and binning effects. The model is implemented using FFTLog, and validated with the PT Challenge suite of $N$-body simulations, whose large volume allows for high-precision tests. Focusing on the mass fluctuation amplitude, ${\ensuremath{\sigma}}_{8}$, and galaxy bias parameters, we find that including one-loop corrections allow us to significantly extend the range of scales over which the bispectrum can be modeled, and greatly tightens constraints on bias parameters. However, this does not lead to noticeable improvements in the ${\ensuremath{\sigma}}_{8}$ error bar due to the necessary marginalization over a large number of nuisance parameters with conservative priors.…

We reanalyze the GW150914 postmerger data searching for quasinormal modes beyond the fundamental, quadrupolar mode. There is currently an ongoing disagreement in the literature about whether, and to what extent, the data contains evidence for a quasinormal mode overtone. We use a frequency-domain approach to ringdown data analysis that was recently proposed by the authors. Our analysis has several advantages compared to other analyses performed mainly in the time domain; in particular, the source sky position and the ringdown start time are marginalized over (as opposed to simply being fixed) as part of a Bayesian ringdown analysis. We find tentative evidence for an overtone in GW150914, but at a lower significance than reported elsewhere. Our preferred analysis, marginalizing over the uncertainty in the time of peak strain amplitude, gives a posterior on the overtone amplitude peaked away from zero at $\ensuremath{\sim}1.8\ensuremath{\sigma}$.

We analyze the properties that any late-time modification of the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ expansion history must have in order to consistently solve both the ${H}_{0}$ and the ${\ensuremath{\sigma}}_{8}$ tensions. Taking a model-independent approach, we obtain a set of necessary conditions that can be applied to any late-time extension whose main effect is a deviation from the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ background. Our results are fully analytical and merely based on the assumptions that the deviations from the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ background remain small. For the concrete case of a dark energy fluid with equation of state $w(z)$, we derive the following general requirements: (i) Solving the ${H}_{0}$ tension demands $w(z)<\ensuremath{-}1$ at some $z$ (ii) Solving both the ${H}_{0}$ and ${\ensuremath{\sigma}}_{8}$ tensions requires $w(z)$ to cross the phantom divide. Finally, we also allow for small deviations on the effective gravitational constant. In this case, our method is still able to constrain the functional form of…

We study the information content of the angle-averaged redshift space galaxy bispectrum. The main novelty of our approach is the use of a systematic tree-level perturbation theory model that includes galaxy bias, IR resummation, and also accounts for nonlinear redshift space distortions, binning, and projection effects. We analyze data from the perturbation theory challenge simulations, whose cumulative volume of $566\text{ }\text{ }{h}^{\ensuremath{-}3}\text{ }{\mathrm{Gpc}}^{3}$ allows for a precise comparison to theoretical predictions. Fitting the power spectrum and bispectrum of our simulated data, and varying all necessary cosmological and nuisance parameters in a consistent Markov chain Monte Carlo analysis, we find that our tree-level bispectrum model is valid up to ${k}_{\mathrm{max}}=0.08\text{ }\text{ }h\text{ }{\mathrm{Mpc}}^{\ensuremath{-}1}$ (at $z=0.61$). We also find that inclusion of the bispectrum monopole improves constraints on cosmological parameters by (5--15)% relative to the power spectrum. The improvement is more significant for the quadratic bias parameters…

The QCD axion is one of the most compelling candidates to explain the dark matter abundance of the Universe. With its extremely small mass ($\ensuremath{\ll}1\text{ }\text{ }\mathrm{eV}/{c}^{2}$), axion dark matter interacts as a classical field rather than a particle. Its coupling to photons leads to a modification of Maxwell's equations that can be measured with extremely sensitive readout circuits. ${\text{DMRadio-m}}^{3}$ is a next-generation search for axion dark matter below $1\text{ }\text{ }\mathit{\ensuremath{\mu}}\mathrm{eV}$ using a $>4\text{ }\text{ }\mathrm{T}$ static magnetic field, a coaxial inductive pickup, a tunable LC resonator, and a DC-SQUID readout. It is designed to search for QCD axion dark matter over the range $20\text{ }\text{ }\mathrm{neV}\ensuremath{\lesssim}{m}_{a}{c}^{2}\ensuremath{\lesssim}800\text{ }\mathrm{neV}$ ($5\text{ }\text{ }\mathrm{MHz}<\ensuremath{\nu}<200\text{ }\mathrm{MHz}$). The primary science goal aims to achieve Dine-Fischler-Srednicki-Zhitnitsky sensitivity above ${m}_{a}{c}^{2}\ensuremath{\approx}120\text{ }\text{ }\mathrm{neV}$ (30…

The symmetry breaking of grand unified gauge groups in the early Universe often leaves behind relic topological defects such as cosmic strings, domain walls, or monopoles. For some symmetry breaking chains, hybrid defects can form where cosmic strings attach to domain walls or monopoles attach to strings. In general, such hybrid defects are unstable, with one defect ``eating'' the other via the conversion of its rest mass into the other's kinetic energy and, subsequently, decaying via gravitational waves. In this work, we determine the gravitational wave spectrum from 1) the destruction of a cosmic string network by the nucleation of monopoles which cut up and ``eat'' the strings, 2) the collapse and decay of a monopole-string network by strings that eat the monopoles, 3) the destruction of a domain wall network by the nucleation of string-bounded holes on the wall that expand and eat the wall, and 4) the collapse and decay of a string-bounded wall network by walls that eat the strings. We call the gravitational wave signals produced from the eating of one topological defect by…

Ultralight bosons can affect the dynamics of spinning black holes (BHs) via superradiant instability, which can lead to a time evolution of the supermassive BH shadow. We study prospects for witnessing the superradiance-induced BH shadow evolution, considering ultralight vector and tensor fields. We introduce two observables sensitive to the shadow time-evolution: the shadow drift, and the variation in the azimuthal angle lapse associated to the photon ring autocorrelation. The two observables are shown to be highly complementary, depending on the observer's inclination angle. Focusing on the supermassive object Sgr ${\mathrm{A}}^{\ensuremath{\star}}$ we show that both observables can vary appreciably over human timescales of a few years in the presence of superradiant instability, leading to signatures which are well within the reach of the Event Horizon Telescope for realistic observation times (but benefiting significantly from extended observation periods) and paving the way towards probing ultralight bosons in the $\ensuremath{\sim}{10}^{\ensuremath{-}17}\text{ }\text{…

We investigate the Page curve for a nonstandard black hole which is asymptotically nonflat/AdS/dS. For this purpose, we apply the island prescription to the charged linear dilaton black holes and analyze, in detail, the entanglement entropy of Hawking radiation for both the nonextremal case and the extremal case. In the nonextremal case, we find the Page curve consistent with the unitarity principle: at early times the entanglement entropy grows linearly in time without the island and at late times it saturates to double of the Bekenstein-Hawking entropy in the presence of the island. We observe the Page time is universal for all different models studied by our method: ${t}_{\text{Page}}=\frac{3}{\ensuremath{\pi}c}\frac{{S}_{\mathrm{BH}}}{{T}_{H}}$. For the extremal case, the island prescription provides the well-defined entanglement entropy only with the island, which cannot be obtained from the continuous limit of the nonextremal case. This implies that the Page curve may not be reproduced for the extremal case and further investigation is needed.

Seconds-long numerical-relativity simulations for black hole--neutron star mergers are performed for the first time to obtain a self-consistent picture of the merger and post-merger evolution processes. To investigate the case that tidal disruption takes place, we choose the initial mass of the black hole to be $5.4\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$ or $8.1\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$ with a dimensionless spin of 0.75. The neutron-star mass is fixed to be $1.35\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$. We find that after the tidal disruption, dynamical mass ejection takes place over $\ensuremath{\lesssim}10\text{ }\text{ }\mathrm{ms}$, together with the formation of a massive accretion disk. Subsequently, the magnetic field in the disk is amplified by the magnetic winding and magnetorotational instability, establishing a turbulent state and inducing angular momentum transport. The post-merger mass ejection by the magnetically induced viscous effect sets in at $\ensuremath{\sim}300--500\text{ }\text{ }\mathrm{ms}$ after the tidal disruption, at which the…

In this work, we present an extension of the time-domain phenomenological model imrphenomt for gravitational-wave signals from binary black hole coalescences to include subdominant harmonics, specifically the $(l=2,m=\ifmmode\pm\else\textpm\fi{}1)$, $(l=3,m=\ifmmode\pm\else\textpm\fi{}3)$, $(l=4,m=\ifmmode\pm\else\textpm\fi{}4)$, and $(l=5,m=\ifmmode\pm\else\textpm\fi{}5)$ spherical harmonics. We also improve our model for the dominant $(l=2,m=\ifmmode\pm\else\textpm\fi{}2)$ mode and discuss mode mixing for the $(l=3,m=\ifmmode\pm\else\textpm\fi{}2)$ mode. The model is calibrated to numerical relativity solutions of the full Einstein equations up to mass ratio 18 and to numerical solutions of the Teukolsky equations for higher mass ratios. This work complements the latest generation of traditional frequency-domain phenomenological models (imrphenomx) and provides new avenues to develop computationally efficient models for gravitational-wave signals from generic compact binaries.

We study a Friedmann-Lema\^{\i}tre-Robertson-Walker spacetime in the theory of $f(Q)$ gravity, where $Q$ denotes the nonmetricity scalar. It has been previously shown in the literature, that there exist four distinct families of connections, which are compatible with the isometries of the FLRW metric; three for the spatially-flat case and one when the spatial curvature is present. In the spatially-flat case, one connection is dynamically irrelevant and yields the dynamics of the coincident gauge in the Cartesian coordinates. For this, we obtain the general solution of an arbitrary $f(Q)$ theory with a perfect fluid-matter content, and present various examples for specific choices of the $f(Q)$ function. We proceed by studying the effect of the rest of the connections, which are dynamical and affect the equations of the motion. We concentrate in scenarios that depart from the $Q=\mathrm{const}$ case, which just reproduces General Relativity with a cosmological constant, and derive novel vacuum solutions for a power-law $f(Q)$ function.

Using high statistics datasets generated in ($2+1$)-flavor QCD calculations at finite temperature, we present results for low-order cumulants of net-baryon-number fluctuations at nonzero values of the baryon chemical potential. We calculate Taylor expansions for the pressure (zeroth-order cumulant), the net-baryon-number density (first-order cumulant), and the variance of the distribution on net-baryon-number fluctuations (second-order cumulant). We obtain series expansions from an eighth-order expansion of the pressure and compare these to diagonal Pad\'e approximants. This allows us to estimate the range of values for the baryon chemical potential in which these expansions are reliable. We find ${\ensuremath{\mu}}_{B}/T\ensuremath{\le}2.5$, 2.0, and 1.5 for the zeroth-, first-, and second-order cumulants, respectively. We, furthermore, construct estimators for the radius of convergence of the Taylor series of the pressure. In the vicinity of the pseudocritical temperature ${T}_{pc}\ensuremath{\simeq}156.5\text{ }\text{ }\mathrm{MeV}$, we find…

The cosmological information extracted from photometric surveys is most robust when multiple probes of the large scale structure of the Universe are used. Two of the most sensitive probes are the clustering of galaxies and the tangential shear of background galaxy shapes produced by those foreground galaxies, so-called galaxy-galaxy lensing. Combining the measurements of these two two-point functions leads to cosmological constraints that are independent of the way galaxies trace matter (the galaxy bias factor). The optimal choice of foreground, or lens, galaxies is governed by the joint, but conflicting requirements to obtain accurate redshift information and large statistics. We present cosmological results from the full $5000\text{ }\text{ }{\mathrm{deg}}^{2}$ of the Dark Energy Survey's first three years of observations (Y3) combining those two-point functions, using for the first time a magnitude-limited lens sample (MagLim) of 11 million galaxies, especially selected to optimize such combination, and 100 million background shapes. We consider two flat cosmological models, the…

Gravitational-wave observations of black hole ringdowns are commonly used to characterize binary merger remnants and to test general relativity. These analyses assume linear black hole perturbation theory, in particular that the ringdown can be described in terms of quasinormal modes even for times approaching the merger. Here we investigate a nonlinear effect during the ringdown, namely how a mode excited at early times can excite additional modes as it is absorbed by the black hole. This is a third-order secular effect: the change in the black hole mass causes a shift in the mode spectrum, so that the original mode is projected onto the new ones. Using nonlinear simulations, we study the ringdown of a spherically symmetric scalar field around an asymptotically anti--de Sitter black hole, and we find that this ``absorption-induced mode excitation'' is the dominant nonlinear effect. We show that this effect takes place well within the nonadiabatic regime, so we can analytically estimate it using a sudden mass-change approximation. Adapting our estimation technique to asymptotically…

Inspired by the ${T}_{cc}^{+}$ signal discovered by the LHCb Collaboration, we systematically investigate the doubly heavy tetraquark states with the molecule configuration $[{Q}_{1}{\overline{q}}_{2}{]}_{{\mathbf{1}}_{c}}[{Q}_{3}{\overline{q}}_{4}{]}_{{\mathbf{1}}_{c}}$ ($Q=c$ and $b$, $q=u$, $d$, and $s$) in a nonrelativistic quark model. The model involves a color screening confinement potential, meson-exchange interactions, and one-gluon-exchange interactions. The state ${T}_{cc}^{+}$ with $I{J}^{P}=0{1}^{+}$ is a very loosely bound deuteronlike state with a binding energy around 0.34 MeV and a huge size of 4.32 fm. Both the meson exchange force and the coupled channel effect play a pivotal role. Without the meson exchange force, there does not exist the ${T}_{cc}^{+}$ molecular state. In strong contrast, the QCD valence bond forms clearly in the ${T}_{bb}^{\ensuremath{-}}$ system when we turn off the meson-exchange force, which is very similar to the hydrogen molecule in QED. Moreover, the ${T}_{bb}^{\ensuremath{-}}$ becomes a heliumlike QCD-atom if we increase the bottom quark…

Magnetic fields are expected to play a key role in the dynamics and the ejection mechanisms that accompany the merger of two neutron stars. General relativistic magnetohydrodynamic (MHD) simulations offer a unique opportunity to unravel the details of the ongoing physical processes. Nevertheless, current numerical studies are severely limited by the fact that any affordable resolution remains insufficient to fully capture the small-scale dynamo, initially triggered by the Kelvin-Helmholtz instability, and later sourced by several MHD processes involving differential rotation. Here, we alleviate this limitation by using explicit large-eddy simulations, a technique where the unresolved dynamics occurring at the subgrid scales (SGS) is modeled by extra terms, which are functions of the resolved fields and their derivatives. The combination of high-order numerical schemes, high resolutions, and the gradient SGS model allow us to capture the small-scale dynamos produced during the binary neutron star mergers, as shown in previous works. Here, we follow the first 50 milliseconds after the…

In this work we derive simple closed-form expressions for the dynamical friction acting on black holes moving through ultralight (scalar field) dark matter, covering both nonrelativistic and relativistic black hole speeds. Our derivation is based on long known scattering amplitudes in black hole spacetimes, it includes the effect of black hole spin and can be easily extended to vector and tensor light fields. Our results cover and complement recent numerical and previous nonrelativistic treatments of dynamical friction in ultralight dark matter.

If dark matter interacts with the Standard Model only gravitationally its abundance in the universe could be explained by the evaporation of primordial black holes (PBH) through Hawking radiation which ``democratically'' emits all existing particles. In these two papers, the authors study this scenario in great detail, significantly improving on previous calculations, and eventually include also interactions with the Standard Model. One curious observation is the strong dependence of the necessary density of PBH on the spin of the dark matter particles.

The speed of sound of the matter within neutron stars may contain nonsmooth structure related to first- or higher-order phase transitions. Here we investigate what are the observable consequences of structure in the speed of sound, such as bumps, spikes, step functions, plateaus, and kinks. One of the main consequences is the possibility of ultraheavy neutron stars (with masses larger than 2.5 solar masses), mass twins in heavy (with masses larger than 2 solar masses) and ultraheavy neutron stars. These stars pass all observational and theoretical constraints, including those imposed by recent LIGO/Virgo gravitational-wave observations and NICER x-ray observations. We thoroughly investigate other consequences of this structure in the speed of sound to develop an understanding of how nonsmooth features affect astrophysical observables, such as stellar radii, tidal deformability, moment of inertia, and Love number. Our results have important implications for future gravitational wave and x-ray observations of neutron stars and their impact in nuclear astrophysics.