Astrometric Effects of Gravitational Wave Backgrounds with non-Luminal Propagation Speeds

A passing gravitational wave causes a deflection in the apparent astrometric positions of distant stars. The effect of the speed of the gravitational wave on this astrometric shift is discussed. A stochastic background of gravitational waves would result in a pattern of astrometric deflections which are correlated on large angular scales. These correlations are quantified and investigated for backgrounds of gravitational waves with sub- and super-luminal group velocities. The statistical properties of the correlations are depicted in two equivalent and related ways: as correlation curves and as angular power spectra. Sub-(super-)luminal gravitational wave backgrounds have the effect of enhancing (suppressing) the power in low-order angular modes. Analytical representations of the redshift-redshift and redshift-astrometry correlations are also derived. The potential for using this effect for constraining the speed of gravity is discussed

Fast post-adiabatic waveforms in the time domain: Applications to compact binary coalescences in LIGO and Virgo

We present a computationally efficient (time-domain) multipolar waveform model for quasi-circular spin-aligned compact binary coalescences. The model combines the advantages of the numerical-relativity informed, effective-one-body (EOB) family of models with a post-adiabatic solution of the equations of motion for the inspiral part of the two-body dynamics. We benchmark this model against other state-of-the-art waveforms in terms of efficiency and accuracy. We find a speed-up of one to two orders of magnitude compared to the underlying time-domain EOB model for the total mass range $2 - 100 M_{\odot}$. More specifically, for a low total-mass system, such as a binary neutron star with equal masses of $1.4 M_{\odot}$, like GW170817, the computational speedup is around 100 times; for an event with total mass $\sim 40 M_\odot$ and mass ratio $\sim 3$, like GW190412, the speedup is by a factor of $\sim 20$, while for a binary system of comparable masses and total mass of $\sim 70 M_{\odot}$, like GW150914, it is by a factor of $\sim 10$. We demonstrate that the new model is extremely faithful to the underlying EOB model with unfaithfulness less than $0.01\%$ across the entire applicable region of parameter space. Finally, we present successful applications of this new waveform model to parameter estimation studies and tests of general relativity

Orbital Complications of Functional Endoscopic Sinus Surgery

Objective: Functional endoscopic sinus surgery (FESS) is an operating procedure for surgical treatment of diseases of the paranasal sinuses. There are precised indications for this surgical intervention. Like any invasive intervention there is a risk of occurrence of complications. Some of the most common are the orbital complications.Methods: By analyzing the available literature, the authors compare and summarize the results of various studies on this subject.Results: Orbital complications are rare but can be with severe consequences, including the complete loss of vision, and even death. Most of them after adequate treatment have not substantial implications but the underestimation can have serious consequences.Conclusion: The first step to avoid complications is prevention. If we have doubts of complications they must be precised instantly and act responsibly towards them. In the presence of this complication, one should be immediately consulted with an ophthalmologist and periodic assessment of IOP and visual acuity

A femtoscopic Correlation Analysis Tool using the Schr\"odinger equation (CATS)

We present a new analysis framework called "Correlation Analysis Tool using the Schr\"odinger equation" (CATS) which computes the two-particle femtoscopy correlation function $C(k)$, with $k$ being the relative momentum for the particle pair. Any local interaction potential and emission source function can be used as an input and the wave function is evaluated exactly. In this paper we present a study on the sensitivity of $C(k)$ to the interaction potential for different particle pairs: p-p, p-$\mathrm{\Lambda}$, $\mathrm{K^-}$-p, $\mathrm{K^+}$-p, p-$\mathrm{\Xi}^-$ and $\mathrm{\Lambda}$-$\mathrm{\Lambda}$. For the p-p Argonne $v_{18}$ and Reid Soft-Core potentials have been tested. For the other pair systems we present results based on strong potentials obtained from effective Lagrangians such as $\chi$EFT for p-$\mathrm{\Lambda}$, J\"ulich models for $\mathrm{K(\bar{K})}$-N and Nijmegen models for $\mathrm{\Lambda}$-$\mathrm{\Lambda}$. For the p-$\mathrm{\Xi}^-$ pairs we employ the latest lattice results from the HAL QCD collaboration. Our detailed study of different interacting particle pairs as a function of the source size and different potentials shows that femtoscopic measurements can be exploited in order to constrain the final state interactions among hadrons. In particular, small collision systems of the order of 1~fm, as produced in pp collisions at the LHC, seem to provide a suitable environment for quantitative studies of this kind.Comment: 16 pages, 13 figures, submitted to EPJ

Laparoscopic vs. open surgical access radical cystectomy with subsequent orthotopic reconstruction in the treatment of invasive urothelial carcinoma of the bladder

Introduction: Radical cystectomy combined with extended lymph node dissection is the treatment of choice for muscle-invasive bladder cancer and can be performed using open, laparoscopic, or robot-assisted surgical access. Aim: To compare the outcomes of laparoscopic (LRC) and open-access (ORC) radical cystectomy in terms of surgery, oncology, functional outcomes, and complications. Materials and methods: We conducted a retrospective study of 200 patients who had all undergone cystectomy for muscle-invasive bladder cancer within the last 4 years. All patients were divided into groups according to the surgical access: LRC in 30 patients and ORC in 170 patients. Oncologic outcomes, expressed as perioperative complications and postoperative results, were analyzed. Results: Overall survival rates were most significantly associated with the histological type, as well as the ‘positive’ lymph nodes and positive resection margin. The average duration of the procedure was shorter in ORC than in LRC (245.5 min and 345.3 min, respectively). Hospital stay was on average 9.18 days in LRC and 12.63 days in ORC, and this duration could vary depending on the type of diversion. The average blood loss in LRC (250-320 ml) was lower than that in ORC (200-720 ml). The complications rate was lower with LRC than with ORC; however, with subsequent orthotopic reconstruction, the functional results were better in ORC. Conclusions: LRC is an alternative option to ORC, considering the fewer complications, less amount of blood loss, and greater surgical precision, as well as shorter hospital stay. Orthotopic diversion has better functional outcomes in ORC

Cosmic topology. Part II. Eigenmodes, correlation matrices, and detectability of orientable Euclidean manifolds

If the Universe has non-trivial spatial topology, observables depend on both the parameters of the spatial manifold and the position and orientation of the observer. In infinite Euclidean space, most cosmological observables arise from the amplitudes of Fourier modes of primordial scalar curvature perturbations. Topological boundary conditions replace the full set of Fourier modes with specific linear combinations of selected Fourier modes as the eigenmodes of the scalar Laplacian. We present formulas for eigenmodes in orientable Euclidean manifolds with the topologies $E_1$ - $E_6$, $E_{11}$, $E_{12}$, $E_{16}$, and $E_{18}$ that encompass the full range of manifold parameters and observer positions, generalizing previous treatments. Under the assumption that the amplitudes of primordial scalar curvature eigenmodes are independent random variables, for each topology we obtain the correlation matrices of Fourier-mode amplitudes (of scalar fields linearly related to the scalar curvature) and the correlation matrices of spherical-harmonic coefficients of such fields sampled on a sphere, such as the temperature of the cosmic microwave background (CMB). We evaluate the detectability of these correlations given the cosmic variance of the observed CMB sky. We find that topologies where the distance to our nearest clone is less than about 1.2 times the diameter of the last scattering surface of the CMB give a correlation signal that is larger than cosmic variance noise in the CMB. This implies that if cosmic topology is the explanation of large-angle anomalies in the CMB, then the distance to our nearest clone is not much larger than the diameter of the last scattering surface. We argue that the topological information is likely to be better preserved in three-dimensional data, such as will eventually be available from large-scale structure surveys.Comment: 79 pages, 9 figure