The three-point function of the energy-momentum tensor in a conformal field theory is completely determined by three parameters, called $\mathcal{A}$, $\mathcal{B}$, $\mathcal{C}$. We carry out a holographic calculation of these three parameters in general $d\ge 4$ dimensions from higher curvature gravities up to and including the quartic order. The result is valid both for massless and perturbative higher curvature gravities. It is known that in four dimensional conformal field theory (CFT) the $a$-charge is a linear combination of $\mathcal{A}$, $\mathcal{B}$, $\mathcal{C}$, our result reproduces this but also shows that a similar relation does not exist for general $d>4$. We then compute the Weyl anomaly in $d=6$ and found all the three $c$-charges are linear combinations of $\mathcal{A}$, $\mathcal{B}$, $\mathcal{C}$, which is consistent with that the $a$-charge is not. We also find the previously conjectured relation between $t_2$, $t_4$, $h^{\prime \prime }$ does not hold in general massless gravities.

Black holes in anti–de Sitter spacetime provide an important testing ground for both gravitational and field-theoretic phenomena. In particular, the study of perturbations can be useful to further our understanding regarding certain physical processes, such as superradiance, or the dynamics of strongly coupled conformal field theories through the holographic principle. In this work we continue our systematic study of the ultraviolet instabilities of black-hole quasinormal modes, built on the characterization of the latter as eigenvalues of a (spectrally unstable) nonselfadjoint operator and using the pseudospectrum as a main analysis tool, extending our previous studies in the asymptotically flat setting to anti–de Sitter asymptotics. Very importantly, this step provides a singularly well-suited probe into some of the key structural aspects of the pseudospectrum. This is a consequence of the specific features of the Schwarzschild-anti-de Sitter geometry, together with the existence of a sound characterization by Warnick of quasinormal modes as eigenvalues, that is still absent in asymptotic flatness. This work focuses on such structural aspects, with an emphasis on the convergence issues of the pseudospectrum and, in particular, the comparison between the hyperboloidal and null slicing cases. As a physical by-product of this structural analysis we assess, in particular, the spectral stability of purely imaginary “hydrodynamic” modes, which appear for axial gravitational perturbations, that become dominant when the black-hole horizon is larger than the anti–de Sitter radius. We find that their spectral stability, under perturbations, depends on how close they are to the real axis, or conversely how distant they are from the first oscillatory overtone.

A triangular solution [Phys. Rev. D 107, 044005 (2023)] has recently been found to the planar circular three-body problem in the parametrized post-Newtonian (PPN) formalism, for which they focus on a class of fully conservative theories characterized by the Eddington-Robertson parameters $\beta$ and $\gamma$. The present paper extends the PPN triangular solution to quasielliptic motion, for which the shape of the triangular configuration changes with time at the PPN order. The periastron shift due to the PPN effects is also obtained.

This paper delves into the exploration of suitable boundary conditions for the asymptotically flat scenario of general relativity presented in terms of Ashtekar-Barbero variables. While the standard parity conditions have been extensively studied by Thiemann [Classical Quantum Gravity 12, 181 (1995)] and Campiglia [Classical Quantum Gravity 32, 145011 (2015)], it turns out that they fail to produce nontrivial supertranslations at spatial infinity. We propose new parity conditions for the Ashtekar-Barbero variables that do yield nontrivial supertranslation charges at spatial infinity. We compare our findings with those of Henneaux and Troessaert [J. High Energy Phys. 03 (2018) 147] and demonstrate that the new boundary conditions ensure the finiteness of the symplectic structure. Moreover, when embarking on the quest for appropriate parity conditions, it is essential to ensure that the selected parities remain invariant under hypersurface deformations. Given that working with Ashtekar-Barbero variables provides more asymptotic structure as compared to the Arnowitt-Deser-Misner variables, it is shown that by fixing the Lagrange multiplier corresponding to the Gauss constraint, the invariance of certain parity conditions can be guaranteed.

The Penrose process for the decay of electrically charged particles in a Reissner-Nordström-anti–de Sitter black hole spacetime is studied. To extract large quantities of energy one needs to mount a recursive Penrose process where particles are confined and can bounce back to suffer ever again a decaying process in the black hole electric ergoregion. In an asymptotically anti–de Sitter (AdS) spacetime, two situations of confinement are possible. One situation uses a reflecting mirror at some radius, which obliges the energetic outgoing particles to return to the decaying point. The other situation uses the natural AdS property that sends back at some intrinsic returning radius those outgoing energetic particles. In addition, besides the conservation laws the decaying process must obey, one has to set conditions at the decaying point for the particles debris. These conditions restrain the possible scenarios, but there are still a great number of available scenarios for the decays. Within these, we choose two scenarios, scenario 1 and scenario 2, that pertain to the masses and electric charges of the final particles. Thus, in the mirror situation we find that scenario 1 leads to a black hole energy factory, and scenario 2 ends in a black hole bomb. In the no mirror situation, i.e., pure Reissner-Nordström-AdS, scenario 1 leads again to a black hole energy factory, but scenario 2 yields no bomb. This happens because the volume in which the particles are confined increases to infinity along the chain of decays, leading to a zero value of the extracted energy per unit volume and the bomb is demined. The whole treatment performed here involves no backreaction on the black hole mass and black hole electric charge; nevertheless we speculate that the end state of the recursive process is a Reissner-Nordström-AdS black hole with very short hair, i.e., with one particle at rest at some definite radius.

We forecast the sensitivity of ongoing and future galaxy cluster abundance measurements to detect deviations from the cold dark matter (CDM) paradigm. Concretely, we consider a class of dark sector models that feature an interaction between dark matter and a dark radiation species (IDM-DR). This setup can be naturally realized by a non-Abelian gauge symmetry and has the potential to explain $S_8$ tensions arising within $\mathrm{\Lambda }\mathrm{CDM}$. We create mock catalogs of the ongoing SPT-3G as well as the future CMB-S4 surveys of galaxy clusters selected via the thermal Sunyaev-Zeldovich effect (tSZE). Both datasets are complemented with cluster mass calibration from next-generation weak gravitational lensing data (ngWL) like those expected from the Euclid mission and the Vera C. Rubin Observatory. We consider an IDM-DR scenario with parameters chosen to be in agreement with Planck 2018 data and that also leads to a low value of $S_8$ as indicated by some local structure formation analyses. Accounting for systematic and stochastic uncertainties in the mass determination and the cluster tSZE selection, we find that both $\mathrm{SPT}\text{−}3\mathrm{G}\times \mathrm{ngWL}$ and $\mathrm{CMB}\text{−}\mathrm{S}4\times \mathrm{ngWL}$ cluster data will be able to discriminate this IDM-DR model from $\mathrm{\Lambda }\mathrm{CDM}$, and thus test whether dark matter-dark radiation interactions are responsible for lowering $S_8$. Assuming IDM-DR, we forecast that the temperature of the dark radiation can be determined to about 40% (10%) with $\mathrm{SPT}\text{−}3\mathrm{G}\times \mathrm{ngWL}$ ($\mathrm{CMB}\text{−}\mathrm{S}4\times \mathrm{ngWL}$), considering 68% credibility, while $S_8$ can be recovered with percent-level accuracy. Furthermore, we show that IDM-DR can be discriminated from massive neutrinos, and that cluster counts will be able to constrain the dark radiation temperature to be below $\sim 10\%$ (at 95% credibility) of the cosmic microwave background temperature if the true cosmological model is $\mathrm{\Lambda }\mathrm{CDM}$.

Recent analysis on the stellar kinematics of ultrafaint dwarf (UFD) galaxies has put a stringent upper limit on the self-scattering cross section of dark matter, i.e., $\sigma /m<\mathcal{O}(0.1){\mathrm{cm}}^2/\mathrm{g}$ at the scattering velocity of $\mathcal{O}(10)\mathrm{km}/\mathrm{s}$. Resonant self-interacting dark matter (rSIDM) is one possibility that can be consistent with the UFDs and explain the low central densities of rotation-supported galaxies; the cross section is resonantly enhanced to be $\sigma /m=\mathcal{O}(1){\mathrm{cm}}^2/\mathrm{g}$ around the scattering velocity of $\mathcal{O}(100)\mathrm{km}/\mathrm{s}$ while being suppressed at lower velocities. To further assess this possibility, since the inferred dark matter distribution of halos from astrophysical observations is usually compared to that in constant-cross section SIDM (cSIDM), whether the structures of rSIDM halos can be approximated by the cSIDM halo profiles needs to be clarified. In this work, we employ the gravothermal fluid method to investigate the structural evolution of rSIDM halos in a wide mass range. We find that except for halos in a specific mass range, the present structures of rSIDM halos are virtually indistinguishable from those of the cSIDM halos. For halos in the specific mass range, the resonant self-scattering renders a break in their density profile. We demonstrate how such a density-profile break appears in astrophysical observations, e.g., rotation curves and line-of-sight velocity dispersion profiles. We show that for halos above the specific mass range, the density-profile break disappears through the thermalization before the present. We infer that such distinctive thermalization dynamics might leave imprints on the orbital classes of stars with similar ages and metallicities.

The measurement of eccentricity would provide strong constraints on the formation channel of stellar-mass binary black holes. However, current ground-based gravitational wave detectors will, in most cases, not be able to measure eccentricity due to orbital circularization. Space-based observatories, in contrast, can determine binary eccentricity at 0.01 Hz to $e_{0.01}\gtrsim \mathcal{O}({10}^{-4})$. Directly observing stellar-mass binary black holes with space-based observatories remains a challenging problem. However, observing such systems with ground-based detectors allows the possibility to identify the same signal in archival data from space-based observatories in the years previous. Since ground-based detectors provide little constraints on eccentricity, including eccentricity in the archival search will increase the required number of filter waveforms for the archival search by 5 orders of magnitudes [from $\sim \mathcal{O}({10}^3)$ to $\sim \mathcal{O}({10}^8)$], and will correspondingly need $\sim 8\times {10}^5$ core hours (and $\sim {10}^5\mathrm{GB}$ of memory), even for a mild upper limit on eccentricity of 0.1. In this work, we have constructed the first template bank for an archival search of space-based gravitational wave detectors, including eccentricity. We have demonstrated that, even though the inclusion of eccentricity brings extra computational burden, an archival search including eccentricity will be feasible in the time frame of planned space-based observatories and will provide strong constraints on the eccentricities of stellar-mass binary black holes.

Core-collapse supernovae (CCSNe) are prime candidates for gravitational-wave detectors. The analysis of their complex waveforms can potentially provide information on the physical processes operating during the collapse of the iron cores of massive stars. In this work we analyze the early-bounce rapidly rotating CCSN signals reported in the waveform catalog of Richers et al. 2017. This catalog comprises over 1800 axisymmetric simulations extending up to about 10 ms of postbounce evolution. It was previously established that for a large range of progenitors, the amplitude of the bounce signal, $D·\mathrm{\Delta }h$, is proportional to the ratio of rotational-kinetic energy to potential energy, $T/|W|$, and the peak frequency, $f_{\mathrm{peak}}$, is proportional to the square root of the central rest-mass density, $\sqrt{{\rho }_{\mathrm{c}}}$. In this work, we exploit these relations to suggest that it could be possible to use such waveforms to infer protoneutron star properties from a future gravitational wave observation, but only if the distance and inclination are well known and the rotation rate is sufficiently low. Our approach relies on the ability to describe a subset of the waveforms in the early postbounce phase in a simple form—a master waveform template—depending only on two parameters, $D·\mathrm{\Delta }h$ and $f_{\mathrm{peak}}$. We use this template to perform a Bayesian inference analysis of waveform injections in Gaussian colored noise for a network of three gravitational wave detectors formed by Advanced LIGO and Advanced Virgo. We show that, for a Galactic event ($D\sim 10\mathrm{kpc}$), it is possible to recover the peak frequency and amplitude with an accuracy better than 10% for $\sim 80\%$ and $\sim 60\%$ of the signals, respectively, given known distance and inclination angle. However, inference on waveforms from outside the Richers catalog is not reliable, indicating a need for carefully verified waveforms of the first 10 ms after bounce of rapidly rotating supernovae of different progenitors with agreement between different codes.

In subleading powers of soft-collinear effective theory (SCET), the Lagrangian contains couplings between soft quarks and hard-collinear quarks. Matrix elements of the hard-collinear parts of these couplings are radiative jet functions. In the position-space formulation of SCET, the Lagrangians are constructed from operators that appear to be gauge invariant. Nevertheless, we find violations of gauge invariance arise in the hard-collinear sector because gauge transformations can shift the momentum of a hard-collinear quark field from the hard-collinear sector to the soft sector, where the hard-collinear fields, by definition, have no support. The violations of gauge invariance are manifested in perturbation theory in the hard-collinear sector through the absence of certain Feynman diagrams that would be present in full QCD. A consequence of the absence of these diagrams is that the radiative jet functions that follow directly from the position-space Lagrangians are not gauge invariant, and we demonstrate this through explicit calculations in lower-order perturbation theory. We obtain gauge-invariant Lagrangians by adding to existing position-space Lagrangians terms that are proportional to the soft-quark equation of motion. These gauge-invariant Lagrangians are valid for nonzero, as well as zero, quark masses. We also remark briefly on the gauge invariance of certain Lagrangians that have been constructed in the label-momentum formulation of SCET.

We construct an example of a safe ultraviolet finite supersymmetric renormalizable SO(10) grand unified theory featuring a supersymmetric dynamical breaking mechanism. Our results constitute a step forward towards an ultraviolet safe extension of the Standard Model enjoying the benefits of grand unified theories.

Axionlike particles (ALPs) emerge in many extensions of the Standard Model as pseudo-Goldstone bosons of a spontaneously broken global symmetry. Understanding their phenomenology in high-energy collisions is crucial for optimizing experimental searches and understanding the exploration potential of future experiments. In this paper, we revise the phenomenology of ALPs with universal couplings to fermions. In particular, we analyze the hierarchy and uncertainty of the various ALP production channels depending on the proton collision energy and the placement of the experiment, and provide improved calculations of the hadronic decay modes.

We investigate the enhancement of dark sector particle production within the scattering dominant regime. These particles typically exhibit a slight mixing with Standard Model particles through various portals, allowing for their generation through in-medium oscillation from Standard Model particle sources. Our analysis reveals that in the scattering dominance regime, with a significantly smaller scattering mean free path ${\lambda }_{\mathrm{sca}}$ compared to the absorption mean free path ${\lambda }_{\mathrm{abs}}$, the nonresonant production of sterile states can experience an enhancement by a factor of ${\lambda }_{\mathrm{abs}}/{\lambda }_{\mathrm{sca}}$. This phenomenon is demonstrated within the context of kinetic mixing dark photon production at a reactor, precisely satisfying this condition. By incorporating this collisional enhancement, we find that the current sensitivity to the mixing parameter $\epsilon$ for dark photons in the TEXONO experiment can be significantly improved across a range spanning from tens of eV to MeV. This advancement establishes the most stringent laboratory constraint within this mass spectrum for the dark photon. Sterile neutrino production, however, does not exhibit such enhancement, either due to the failure to meet the scattering dominance criterion or the neutrino damping in resonant production.

We propose a grand unified theory (GUT) pseudo-Nambu-Goldstone boson (pNGB) dark matter (DM) model based on $SU(7)$ gauge symmetry. In the GUT model, the Standard Model (SM) gauge symmetry $G_{\mathrm{SM}}≔SU(3{)}_C\times SU(2{)}_L\times U(1{)}_Y$ and the “dark” gauge symmetry $SU(2{)}_D$ are unified, where the $SU(2{)}_D$ symmetry plays an important role in the stability of DM. The unification of SM fermions and dark sector fermions is partially realized. The gauge symmetry $SU(7)$ is spontaneously broken to $SU(5)\times SU(2)\times U(1)$ gauge symmetry at the GUT scale by the nonvanishing vacuum expectation values of an $SU(7)$ adjoint scalar field, where the $SU(5)$ gauge symmetry is not usual $SU(5)$ GUT gauge symmetry. The symmetry is further broken to $G_{\mathrm{SM}}\times SU(2{)}_D$ at an intermediate scale. Furthermore, the $SU(2{)}_D$ symmetry is broken by the $SU(2{)}_D$ doublet and triplet scalar fields at the TeV scale. In the pNGB DM model based on $G_{\mathrm{SM}}\times SU(2{)}_D$, the residual global $U(1{)}_V$ dark custodial symmetry guarantees DM stability. On the other hand, in the $SU(7)$ pNGB DM model, this global symmetry is explicitly broken by the Yukawa interaction and the effective Majorana mass terms. In the scalar sector, the cubic coupling constants of the $SU(2{)}_D$ doublet and triplet scalar fields are the order parameters of the $U(1{)}_V$ symmetry breaking. To maintain $U(1{)}_V$ symmetry and thus the DM stability, we need to tune Yukawa coupling constants and cubic scalar couplings at high accuracy. We find that the allowed DM mass region is quite restricted as the gauge coupling constant of $SU(2{)}_D$ is determined by the condition of the gauge coupling unification. To satisfy gauge coupling unification and the current experimental constraint on proton lifetime, we find that three generations of $SU(3{)}_C$ adjoint fermions and another three generations of $SU(2{)}_L$ adjoint fermions with the intermediate mass scale are required. We also find that there is no other solution to satisfy simultaneously the gauge coupling unification and the proton decay constraint if one assumes the other symmetry breaking schemes.

Research on the quantum chromodynamics (QCD) phase diagram with lattice field theory methods is dominated by the use of rooted staggered fermions, as they are the computationally cheapest discretization available. We show that rooted staggered fermions at a nonzero baryochemical potential ${\mu }_B$ predict a sharp rise in the baryon density at low temperatures and ${\mu }_B\gtrsim 3m_{\pi }/2$, where $m_{\pi }$ is the Goldstone pion mass. We elucidate the nature of the nonanalyticity behind this sharp rise in the density by a comparison of reweighting results with a Taylor expansion of high order. While at first sight this nonanalytic behavior becomes apparent at the same position where the pion condensation transition takes place in the phase-quenched theory, the nature of the nonanalyticity in the two theories appears to be quite different: While at nonzero isospin density the data are consistent with a genuine thermodynamic (branch-point) singularity, the results at nonzero baryon density point to an essential singularity at ${\mu }_B=0$. The effect is absent for four flavors of degenerate quarks, where rooting is not used. For the two-flavor case, we show numerical evidence that the magnitude of the effect diminishes on finer lattices. We discuss the implications of this technical complication on future studies of the QCD phase diagram.

In this paper QCD at large isospin density is studied, which is known to be in the superfluid state with Cooper pairs carrying the same quantum number as pions. The gap equation derived from the perturbation theory up to the next-to-leading-order corrections is solved. The pairing gap at large isospin chemical potential is found to be enhanced compared to the color-superconducting gap at large baryon chemical potential due to the $\sqrt{2}$ difference in the exponent arising from the stronger attraction in one-gluon exchange in the singlet channel. Then, using the gap function, the contribution of the condensation energy of the superfluid state to the QCD equation of state is evaluated. At isospin chemical potential of a few GeV, where the lattice QCD and the perturbative QCD can be both applied, the effect of the condensation energy becomes dominant even compared to the next-to-leading order corrections to the pressure in the perturbation theory. It resolves the discrepancy between the recent lattice QCD results and the perturbative QCD result.

We calculate the mass spectrum of the S-wave fully heavy tetraquark systems $QQ\overline{Q}\overline{Q}(Q=c,b)$ with both normal $(J^{PC}=0^{++},1^{+-},2^{++})$ and exotic $(J^{PC}=0^{+-},1^{++},2^{+-})$ C-parities using three different quark potential models (AL1, AP1, BGS). The exotic C-parity systems refer to the ones that cannot be composed of two S-wave ground heavy quarkonia. We incorporate the molecular dimeson and compact diquark-antidiquark spatial correlations simultaneously, thereby discerning the actual configurations of the states. We employ the Gaussian expansion method to solve the four-body Schrödinger equation, and the complex scaling method to identify the resonant states. The mass spectra in three different models qualitatively agree with each other. We obtain several resonant states with $J^{PC}=0^{++},1^{+-},2^{++},1^{++}$ in the mass region (6.92,7.30) GeV, some of which are good candidates of the experimentally observed $X(6900)$ and $X(7200)$. We also obtain several exotic C-parity zero-width states with $J^{PC}=0^{+-}$ and $2^{+-}$. These zero-width states have no corresponding S-wave diquarkonium threshold and can only decay strongly to final states with P-wave quarkonia. With the notation $T_{4Q,J(C)}(M)$, we deduce from the root mean square radii that the $X(7200)$ candidates $T_{4c,0(+)}(7173),T_{4c,2(+)}(7214)$ and the state $T_{4c,1(-)}(7191)$ look like molecular states although most of the resonant and zero-width states are compact states.

We compute the pressure from first principles within perturbative QCD at finite baryon density and very high magnetic fields up to two-loops and with physical quark masses. The region of validity for our framework is given by $m_s\ll {\mu }_q\ll \sqrt{eB}$, where $m_s$ is the strange quark mass, ${\mu }_q$ is the quark chemical potential, $e$ is the fundamental electric charge, and $B$ is the magnetic field strength. We include the effects of the renormalization scale in the running coupling, ${\alpha }_s({\mu }_q,\sqrt{eB})$, and running strange quark mass. We also discuss the simplifications that come about in the chiral limit. The effectively negligible contribution of the exchange diagram allows for building a simple analytic model for the equation of state for pure quark magnetars and computing their mass and radius at very large values of $B$. These results provide constraints on the behavior of the maximum mass and associated radius from perturbative QCD. We also discuss the magnetic bag model for extreme magnetic fields.

We investigate the chemical potential effects of the equation of state and the chiral transition in an Einstein-Maxwell-dilaton-scalar system, which is obtained from an improved soft-wall anti–de Sitter/QCD model coupled with an Einstein-Maxwell-dilaton system. The equations of state obtained from the model are in quantitative agreement with the lattice results at both zero and nonzero chemical potentials. The sensible chiral transition behaviors can be realized in the model. The QCD phase diagram with a critical end point has also been obtained from the model.

Study of canonical entropy in electron-proton interactions at $\sqrt{s}=300\mathrm{GeV}$ is presented. The precision data collected by the H1 experiment at the HERA in different ranges of invariant hadronic mass $W$ and the squared four-momentum exchange $Q^2$ in electron-proton $(ep)$ interactions have been analyzed in the ensemble theory approach. The canonical partition function relates to the multiplicity distribution which is often studied in collider experiments. We use the canonical ensemble partition function to explore the dynamics of hadron production in $ep$ interactions by devising different methods to find the entropic parameter and the collision temperature. The inverse slope of the transverse momentum spectrum of produced hadrons also relates to the temperature. In the recent past, the CMS, ATLAS, and ALICE experiments at the LHC have studied the charged hadron transverse momentum and particle distributions in proton-proton and proton-nucleus interactions by using the Tsallis function within this approach. A detailed investigation into the role of the system volume and relation amongst different dynamical parameters reveals interesting results.