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Gravitational-Waves


#astro-ph.HE #gr-qc

Origin | Interest | Match
arXiv logo
arXiv.orgGW231123: a Binary Black Hole Merger with Total Mass 190-265 $M_{\odot}$On 2023 November 23 the two LIGO observatories both detected GW231123, a gravitational-wave signal consistent with the merger of two black holes with masses $137^{+22}_{-17}\, M_\odot$ and $103^{+20}_{-52}\, M_\odot$ (90\% credible intervals), at luminosity distance 0.7-4.1 Gpc and redshift of $0.39^{+0.27}_{-0.24}$, and a network signal-to-noise ratio of $\sim$22.5. Both black holes exhibit high spins, $0.9^{+0.10}_{-0.19}$ and $0.80^{+0.20}_{-0.51}$ respectively. A massive black hole remnant is supported by an independent ringdown analysis. Some properties of GW231123 are subject to large systematic uncertainties, as indicated by differences in inferred parameters between signal models. The primary black hole lies within or above the theorized mass gap where black holes between 60-130 $M_\odot$ should be rare due to pair instability mechanisms, while the secondary spans the gap. The observation of GW231123 therefore suggests the formation of black holes from channels beyond standard stellar collapse, and that intermediate-mass black holes of mass $\sim$200 $M_\odot$ form through gravitational-wave driven mergers.
#astrophhe#grqc
Gravitational-Waves


#astro-ph.HE #astro-ph.GA #gr-qc

Origin | Interest | Match
arXiv logo
arXiv.orgWhere are Gaia's small black holes?Gaia has recently revealed a population of over 20 compact objects in wide astrometric binaries, while LIGO-Virgo-KAGRA (LVK) have observed around 100 compact object binaries as gravitational-wave (GW) mergers. Despite belonging to different systems, the compact objects discovered by both Gaia and the LVK follow a multimodal mass distribution, with a global maximum at neutron star (NS) masses ($\sim 1$-$2\,M_\odot$) and a secondary local maximum at black hole (BH) masses $\sim10\,M_\odot$. However, the relative dearth of objects, or ``mass gap," between these modes is more pronounced among the wide binaries observed by Gaia compared to the GW population, with $9^{+10}_{-6}\%$ of GW component masses falling between $2.5$--$5\,M_\odot$ compared to $\lesssim5\%$ of Gaia compact objects. We explore whether this discrepancy can be explained by the natal kicks received by low-mass BHs. GW progenitor binaries may be more likely to survive natal kicks, because the newborn BH has a more massive companion and/or is in a tighter binary than Gaia progenitor binaries. We compare the survival probabilities of Gaia and GW progenitor binaries as a function of natal kick strength and pre-supernova binary parameters, and map out the parameter space and kick strength required to disrupt the progenitor binaries leading to low-mass BHs in Gaia systems more frequently than those in GW systems.
#astrophhe#astrophga#grqc
DarkMatter


#gr-qc

Origin | Interest | Match
arXiv logo
arXiv.orgPhase space analysis of Rényi Holographic dark energy modelRecent observational evidences point out towards a late time acceleration of the universe. In order to study the accelerated expansion, scientists have incorporated the existence of an exotic matter with negative pressure, termed as dark energy. Afterwards a new idea of dark energy have been studied depending on the holographic principle of quantum gravity, called as the Holographic Dark Energy(HDE). Later on modifying Bekestein-Hawking entropy, different generalized entropies have been proposed, one of them being Rényi entropy which leads to Rényi holographic dark energy model (RHDE). We have considered RHDE model with Hubble horizon as the IR cut off and have studied the cosmological behaviour under non interacting, linear and non-linear interacting scenarios with the help of dynamical systems analysis. We have also investigated the stability of the system around hyperbolic critical points along with the type of fluid description, evolution of equation of state parameter as well as matter and energy density parameters.
#grqc
Gravitational-Waves


#astro-ph.IM #astro-ph.GA #gr-qc

Origin | Interest | Match
arXiv logo
arXiv.orgModeling Non-Gaussianities in Pulsar Timing Array data analysis using Gaussian Mixture ModelsIn Pulsar Timing Array (PTA) data analysis, noise is typically assumed to be Gaussian, and the marginalized likelihood has a well-established analytical form derived within the framework of Gaussian processes. However, this Gaussianity assumption may break down for certain classes of astrophysical and cosmological signals, particularly for a gravitational wave background (GWB) generated by a population of supermassive black hole binaries (SMBHBs). In this work, we present a new method for testing the presence of non-Gaussian features in PTA data. We go beyond the Gaussian assumption by modeling the noise or signal statistics using a Gaussian mixture model (GMM). An advantage of this approach is that the marginalization of the likelihood remains fully analytical, expressed as a linear combination of Gaussian PTA likelihoods. This makes the method straightforward to implement within existing data analysis tools. Moreover, this method extends beyond the free spectrum analysis by producing posterior probability distributions of higher-order moments inferred from the data, which can be incorporated into spectral refitting techniques. We validate the model using simulations and demonstrate the sensitivity of PTAs to non-Gaussianity by computing the Bayes factor in favor of the GMM as a function of the injected excess moments. We apply the method to a more astrophysically motivated scenario where a single SMBHB is resolved on top of a Gaussian GWB and show that significant non-Gaussianities are introduced by the individual source. Finally, we test our model on a realistic GWB generated from a simulated population of SMBHBs.
#astrophim#astrophga#grqc
Gravitational-Waves


#gr-qc

Origin | Interest | Match
arXiv logo
arXiv.orgEstimating High-Order Time Derivatives of Kerr Orbital FunctionalsFunctions of bound Kerr geodesic motion play a central role in many calculations in relativistic astrophysics, ranging from gravitational-wave generation to self-force and radiation-reaction modeling. Although these functions can be expressed as a Fourier series using the geodesic fundamental frequencies, reconstructing them in coordinate time is challenging due to the coupling of the radial and polar motions. In this paper, we compare two strategies for performing such reconstructions and their ability to estimate high-order coordinate-time derivatives of the orbital functional. The first method maps Fourier coefficients from Mino to coordinate time; the second method fits a sampled time series of the function to a truncated coordinate-time Fourier series. While the latter method is prone to overfitting, it yields more accurate reconstructions and derivatives than the mapping, but completely misrepresents the harmonic content of the orbital functional. For the purpose of accurate coordinate-time derivative estimation, we propose a hybrid method: fit for the Mino-time coefficients, differentiate with respect to Mino time, then convert to coordinate time. Applied to the mass quadrupole of a generic Kerr geodesic, this hybrid method recovers the sixth derivative with a fractional residual $\sim10^{-6}$ using only two harmonics. For orbital functionals that depend explicitly on the geodesic orbit expressed in Boyer--Lindquist coordinates, we also provide a recursive procedure for computing coordinate-time derivatives using exact analytic expressions. These results offer a general framework for accurately evaluating high-order time derivatives along Kerr geodesic worldlines, with direct relevance to applications such as extreme-mass-ratio inspiral kludge waveform modeling, where such derivatives are key ingredients for precise gravitational-wave predictions.
#grqc
Gravitational-Waves


#gr-qc #astro-ph.IM #hep-ph

Origin | Interest | Match
arXiv logo
arXiv.orgA general Fourier expansion of post-Newtonian binary dynamics based on quasi-Keplerian frameworkWe have introduced a new Fourier-expansion technique for computing gravitational-wave emission from non-spinning binaries in the post-Newtonian framework. Using this approach, we derived the full set of 3PN dynamical quantities and gravitational-wave Fourier modes and have released the corresponding numerical code as open source. Furthermore, applying the method to the tail contribution of the energy flux, we found that it can be resummed into an exceptionally compact expression. These advances pave the way for more convenient and accurate frequency-domain waveform modeling in the future.
#grqc#astrophim#hepph
Gravitational-Waves


#gr-qc #astro-ph.IM

Origin | Interest | Match
arXiv logo
arXiv.orgToward Low-Latency, High-Fidelity Calibration of the LIGO Detectors with Enhanced Monitoring ToolsAccurate and reliable calibration of the Advanced LIGO detectors has enabled a plethora of gravitational-wave discoveries over the past decade, starting with the ground-breaking discovery, GW150914. Over the past ten years, the calibrated strain data from Advanced LIGO detectors has become available at a lower latency and with more reliability. In this paper, we discuss the relevant history of Advanced LIGO calibration and introduce new tools that have been developed to enable faster and more robust calibrated strain data products in the current observing run. We discuss improvements to the robustness, reliability, and accuracy of the low-latency calibration pipeline as well as the development of a new tool for monitoring the LIGO calibration in real time.
#grqc#astrophim
Gravitational-Waves


#gr-qc #hep-ph #hep-th

Origin | Interest | Match
arXiv logo
arXiv.orgSelf-Gravity in Superradiance Clouds: Implications for Binary Dynamics and Observational ProspectsSpinning black holes could produce ultralight particles via the superradiance instability. These particles form a dense cloud around the host black hole, introducing new opportunities for the detection of ultralight new physics. When the black hole is part of a binary system, the binary can trigger transitions among different states of the cloud configuration. Such transitions backreact on the orbital dynamics, modifying the frequency evolution of the emitted gravitational waves. Based on this observation, black hole binaries were proposed as a way to test the existence of ultralight particles. We investigate the effects of the self-gravity of the cloud on the orbital evolution and on the gravitational wave emission. We find that cloud self-gravity could lead to a density-dependent modification of the energy levels of ultralight particles and that it could alter the order of hyperfine energy levels. The crossing of hyperfine levels prevents binaries from triggering resonant hyperfine transitions and allows them to approach radii that could trigger resonant transitions of fine levels. We study the implications of these findings, especially in the context of future space-borne gravitational wave observatory, the Laser Interferometer Space Antenna (LISA). For quasi-circular, prograde and equatorial orbits, we find that LISA could probe ultralight particles in the mass range $10^{-15}\,{\rm eV} \, - \, 10^{-13}\, {\rm eV}$ through gravitational wave observations.
#grqc#hepph#hepth
Observatories


#gr-qc #astro-ph.HE

Origin | Interest | Match
arXiv logo
arXiv.orgChallenging a binary neutron star merger interpretation of GW230529GW230529_181500 represented the first gravitational-wave detection with one of the component objects' mass inferred to lie in the previously hypothesized mass gap between the heaviest neutron stars and the lightest observed black holes. Given the expected maximum mass values for neutron stars, this object was identified as a black hole, and, with the secondary component being a neutron star, the detection was classified as a neutron star-black hole merger. However, due to the low signal-to-noise ratio and the known waveform degeneracy between the spin and mass ratio in the employed gravitational-wave models, GW230529_181500 could also be interpreted as a merger of two heavy ($\gtrsim 2 \mathrm{M}_\odot$) neutron stars with high spins. We investigate the distinguishability of these scenarios by performing parameter estimation on simulated signals obtained from numerical-relativity waveforms for both neutron star-black hole and binary neutron star systems, with parameters consistent with GW230529_181500, and comparing them to the analysis of the real event data. We find that GW230529_181500 is more likely to have originated from a neutron star-black hole merger, though the possibility of a binary neutron star origin can not be ruled out. Moreover, we use the simulation data to estimate the signatures of potential electromagnetic counterparts emitted by the systems. We find them to be too dim to be located by current wide-field surveys if only the dynamical ejecta is considered, and detectable by the Vera C. Rubin Observatory during the first two days after merger if one accounts for additional disk wind ejecta.
#grqc#astrophhe
NeutronStars


#gr-qc

Origin | Interest | Match
arXiv logo
arXiv.orgHorizon tracking for asynchronous parallel black hole simulationsIn the field of gravitational wave science, next-generation detectors will be substantially more accurate than the current suite of detectors. Numerical relativity simulations of binary black hole (BBH) gravitational waveforms must become faster, more efficient, and more accurate to be used in analyses of these next-generation detections. One approach, which the \texttt{SpECTRE} code employs, is using spectral methods for accuracy along with synchronous task-based parallelism to avoid idle time in simulations and make the most efficient use of computational resources. When writing an asynchronous application, algorithms must be redesigned compared to their synchronous counterparts. To illustrate this process, we present novel methods for dynamically tracking the apparent horizons in evolutions of BBH mergers using a feedback control system, all in the context of asynchronous parallelism. We also briefly detail how these methods can be applied to binary neutron star simulations performed with asynchronous parallelism.
#grqc
NeutronStars


#nucl-th #gr-qc #hep-ph #hep-th

Origin | Interest | Match
arXiv logo
arXiv.orgSpacetime Curvature as a Probe of Exotic Core Phases in Neutron Stars within Modified GravityIn this study, we investigate the effect of Energy-Momentum Squared Gravity (EMSG) on the curvature of neutron stars (NSs) by using three relativistic mean-field (RMF) equations of state (EOSs) and three hadron-quark phase transition (HQPT) EOSs. Neutron stars, with their extreme densities and strong gravitational fields, provide an ideal laboratory for testing General Relativity (GR) in the high-curvature regime and for exploring possible deviations via modified gravity. EMSG extends GR by including nonlinear terms involving the energy-momentum tensor, characterized by a coupling parameter $α$. We focus on the Kretschmann, Ricci, and Weyl curvature scalars, analyzing their dependence on baryon density and radial coordinate for varying values of $α$. Our results indicate that EMSG can significantly alter the curvature profiles of neutron stars. In particular, the magnitude of both Weyl and Kretschmann scalars increases (decreases) for a positive (negative) EMSG parameter, with the former exhibiting a larger dependence. Similarly, the surface curvature (SC) is notably affected by $α$. Interestingly, we further observe distinct discontinuities in the curvature profiles at hadron-quark phase transitions, especially in the soft and intermediate HQPT models. These signatures may provide observable imprints of exotic core phases in neutron stars.
#nuclth#grqc#hepph
Gravitational-Waves


#astro-ph.CO #gr-qc #hep-th

Origin | Interest | Match
arXiv logo
arXiv.orgOscillations and parity violation in gravitational wave background from extra tensor modesSpectator fields which provide additional tensor degrees of freedom, on top of the standard metric tensor perturbations, can produce significant amounts of gravitational waves (GWs). Employing the effective field theory approach for spin-2 fields, we find a universal prediction that linear mixing between the metric and extra tensor modes inevitably induces oscillatory features in the GW spectrum, reminiscent of the so-called neutrino oscillation. Moreover, parity-violating operators in the spin-2 sector can imprint chiral signatures on the resulting GW background. We consider a concrete scenario in which the spin-2 field generates observable chiral GWs with characteristic oscillatory patterns. These results provide a model-independent characterization of the key signatures and observational implications of such scenarios which can be detected with future GW detectors.
#astrophco#grqc#hepth
Gravitational-Waves


#gr-qc #hep-ph #hep-th

Origin | Interest | Match
arXiv logo
arXiv.orgSelf-Gravity in Superradiance Clouds: Implications for Binary Dynamics and Observational ProspectsSpinning black holes could produce ultralight particles via the superradiance instability. These particles form a dense cloud around the host black hole, introducing new opportunities for the detection of ultralight new physics. When the black hole is part of a binary system, the binary can trigger transitions among different states of the cloud configuration. Such transitions backreact on the orbital dynamics, modifying the frequency evolution of the emitted gravitational waves. Based on this observation, black hole binaries were proposed as a way to test the existence of ultralight particles. We investigate the effects of the self-gravity of the cloud on the orbital evolution and on the gravitational wave emission. We find that cloud self-gravity could lead to a density-dependent modification of the energy levels of ultralight particles and that it could alter the order of hyperfine energy levels. The crossing of hyperfine levels prevents binaries from triggering resonant hyperfine transitions and allows them to approach radii that could trigger resonant transitions of fine levels. We study the implications of these findings, especially in the context of future space-borne gravitational wave observatory, the Laser Interferometer Space Antenna (LISA). For quasi-circular, prograde and equatorial orbits, we find that LISA could probe ultralight particles in the mass range $10^{-15}\,{\rm eV} \, - \, 10^{-13}\, {\rm eV}$ through gravitational wave observations.
#grqc#hepph#hepth
NeutronStars


#hep-th #astro-ph.CO #gr-qc #hep-ph

Origin | Interest | Match
arXiv logo
arXiv.orgCan weak-gravity, causality-violation arguments constrain modified gravity?We investigate limitations of causality arguments from flat-spacetime amplitudes, based on the eikonal limit of gravitational scattering, to place constraints on modified gravity. We show that causality constraints are only valid in the weak-gravity regime even for transplanckian scattering, and that such constraints are much less stringent than astrophysical ones, obtained for example from gravitational waves emitted in black hole coalescence. Special attention is given to the weakness of causality constraints on dynamical Chern-Simons gravity, but our results apply to other modified gravity theories as well. In the context of that theory, we also discuss how to obtain a time-delay formula from black hole, neutron stars, and shockwave solutions. For scattering with compact objects, we explicitly show that time delays are greatly suppressed by the ratio of the object's mass to the impact parameter, so time advances only occur greatly outside the cut off of the theory. For the shockwave solution, we find that the time delay is always positive within the regime of validity of the solution. We also comment on the impact of graviton nonlinearities for time-delay calculations in the nonlinear, strong gravity regime. We conclude that amplitude-based causality constraints on modified gravity are typically not stringent relative to other experimental and observational bounds.
#hepth#astrophco#grqc
DarkMatter


#astro-ph.CO #gr-qc #hep-th

Origin | Interest | Match
arXiv logo
arXiv.orgParticle physics models of interacting bosonic dark energy and fermionic dark matter in Einstein scalar Gauss-Bonnet gravityWe explore a cosmological framework in which a Gauss-Bonnet (GB) coupled scalar field, acting as dark energy, interacts with a fermionic dark matter field through a coupling obtained from the point of view of particle physics. This setup is inspired by string/M-theory, and two representative scalar field potentials are investigated: exponential and power-law. A distinctive feature of the GB-coupled models is their potential to alter the propagation speed of gravitational waves (GWs), a property with significant implications in light of recent multi-messenger astrophysical observations. To account for this, we analyze models under two scenarios: one where the GW speed differs from that of light and the other where they are equal, but all consistent with current observational constraints. The dynamical evolution of the system is investigated by reformulating the field equations into an autonomous dynamical system, enabling a detailed analysis of the Universe's long-term behavior, including the radiation-, matter- and dark energy-dominated epochs. We constrain the model parameters using a broad set of recent observational data, including mock high-redshift measurements from the Roman Space Telescope. Our findings indicate that both potentials yield cosmologies that are in excellent agreement with current data, closely tracking the expansion history predicted by the standard \(Λ\)CDM model, while still allowing room for subtle deviations that could be tested by future observations.
#astrophco#grqc#hepth
NeutronStars


#nucl-th #gr-qc #hep-ph #hep-th

Origin | Interest | Match
arXiv logo
arXiv.orgSpacetime Curvature as a Probe of Exotic Core Phases in Neutron Stars within Modified GravityIn this study, we investigate the effect of Energy-Momentum Squared Gravity (EMSG) on the curvature of neutron stars (NSs) by using three relativistic mean-field (RMF) equations of state (EOSs) and three hadron-quark phase transition (HQPT) EOSs. Neutron stars, with their extreme densities and strong gravitational fields, provide an ideal laboratory for testing General Relativity (GR) in the high-curvature regime and for exploring possible deviations via modified gravity. EMSG extends GR by including nonlinear terms involving the energy-momentum tensor, characterized by a coupling parameter $α$. We focus on the Kretschmann, Ricci, and Weyl curvature scalars, analyzing their dependence on baryon density and radial coordinate for varying values of $α$. Our results indicate that EMSG can significantly alter the curvature profiles of neutron stars. In particular, the magnitude of both Weyl and Kretschmann scalars increases (decreases) for a positive (negative) EMSG parameter, with the former exhibiting a larger dependence. Similarly, the surface curvature (SC) is notably affected by $α$. Interestingly, we further observe distinct discontinuities in the curvature profiles at hadron-quark phase transitions, especially in the soft and intermediate HQPT models. These signatures may provide observable imprints of exotic core phases in neutron stars.
#nuclth#grqc#hepph
Gravitational-Waves


#astro-ph.HE #gr-qc

Origin | Interest | Match
arXiv logo
arXiv.orgGW231123: a Binary Black Hole Merger with Total Mass 190-265 $M_{\odot}$On 2023 November 23 the two LIGO observatories both detected GW231123, a gravitational-wave signal consistent with the merger of two black holes with masses $137^{+22}_{-17}\, M_\odot$ and $103^{+20}_{-52}\, M_\odot$ (90\% credible intervals), at luminosity distance 0.7-4.1 Gpc and redshift of $0.39^{+0.27}_{-0.24}$, and a network signal-to-noise ratio of $\sim$22.5. Both black holes exhibit high spins, $0.9^{+0.10}_{-0.19}$ and $0.80^{+0.20}_{-0.51}$ respectively. A massive black hole remnant is supported by an independent ringdown analysis. Some properties of GW231123 are subject to large systematic uncertainties, as indicated by differences in inferred parameters between signal models. The primary black hole lies within or above the theorized mass gap where black holes between 60-130 $M_\odot$ should be rare due to pair instability mechanisms, while the secondary spans the gap. The observation of GW231123 therefore suggests the formation of black holes from channels beyond standard stellar collapse, and that intermediate-mass black holes of mass $\sim$200 $M_\odot$ form through gravitational-wave driven mergers.
#astrophhe#grqc
NeutronStars


#hep-th #astro-ph.CO #gr-qc #hep-ph

Origin | Interest | Match
arXiv logo
arXiv.orgCan weak-gravity, causality-violation arguments constrain modified gravity?We investigate limitations of causality arguments from flat-spacetime amplitudes, based on the eikonal limit of gravitational scattering, to place constraints on modified gravity. We show that causality constraints are only valid in the weak-gravity regime even for transplanckian scattering, and that such constraints are much less stringent than astrophysical ones, obtained for example from gravitational waves emitted in black hole coalescence. Special attention is given to the weakness of causality constraints on dynamical Chern-Simons gravity, but our results apply to other modified gravity theories as well. In the context of that theory, we also discuss how to obtain a time-delay formula from black hole, neutron stars, and shockwave solutions. For scattering with compact objects, we explicitly show that time delays are greatly suppressed by the ratio of the object's mass to the impact parameter, so time advances only occur greatly outside the cut off of the theory. For the shockwave solution, we find that the time delay is always positive within the regime of validity of the solution. We also comment on the impact of graviton nonlinearities for time-delay calculations in the nonlinear, strong gravity regime. We conclude that amplitude-based causality constraints on modified gravity are typically not stringent relative to other experimental and observational bounds.
#hepth#astrophco#grqc
Gravitational-Waves


#gr-qc #astro-ph.IM #hep-ph

Origin | Interest | Match
arXiv logo
arXiv.orgA general Fourier expansion of post-Newtonian binary dynamics based on quasi-Keplerian frameworkWe have introduced a new Fourier-expansion technique for computing gravitational-wave emission from non-spinning binaries in the post-Newtonian framework. Using this approach, we derived the full set of 3PN dynamical quantities and gravitational-wave Fourier modes and have released the corresponding numerical code as open source. Furthermore, applying the method to the tail contribution of the energy flux, we found that it can be resummed into an exceptionally compact expression. These advances pave the way for more convenient and accurate frequency-domain waveform modeling in the future.
#grqc#astrophim#hepph
NeutronStars


#gr-qc #astro-ph.HE

Origin | Interest | Match
arXiv logo
arXiv.orgChallenging a binary neutron star merger interpretation of GW230529GW230529_181500 represented the first gravitational-wave detection with one of the component objects' mass inferred to lie in the previously hypothesized mass gap between the heaviest neutron stars and the lightest observed black holes. Given the expected maximum mass values for neutron stars, this object was identified as a black hole, and, with the secondary component being a neutron star, the detection was classified as a neutron star-black hole merger. However, due to the low signal-to-noise ratio and the known waveform degeneracy between the spin and mass ratio in the employed gravitational-wave models, GW230529_181500 could also be interpreted as a merger of two heavy ($\gtrsim 2 \mathrm{M}_\odot$) neutron stars with high spins. We investigate the distinguishability of these scenarios by performing parameter estimation on simulated signals obtained from numerical-relativity waveforms for both neutron star-black hole and binary neutron star systems, with parameters consistent with GW230529_181500, and comparing them to the analysis of the real event data. We find that GW230529_181500 is more likely to have originated from a neutron star-black hole merger, though the possibility of a binary neutron star origin can not be ruled out. Moreover, we use the simulation data to estimate the signatures of potential electromagnetic counterparts emitted by the systems. We find them to be too dim to be located by current wide-field surveys if only the dynamical ejecta is considered, and detectable by the Vera C. Rubin Observatory during the first two days after merger if one accounts for additional disk wind ejecta.
#grqc#astrophhe
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