arXiv subjects

Odylio Denys Aguiar

Publications and source records attributed to Odylio Denys Aguiar.

5 recordsLinked to original sources

arXiv2026

Estimation of the MTOV precision for ET, CE, and NEMO from the post-merger of BNS coalescences

The detection of the gravitational waves produced after the coalescence of two neutron stars is greatly anticipated because it will be able to provide information about matter in extreme conditions, especially if the remnant turns out to go through a hypermassive or a supermassive neutron star state before collapsing into a black hole. Next-generation gravitational wave detectors such as ET, CE, and NEMO are expected to observe high-frequency gravitational wave signals, that is, the post-merger stage of the coalescence of binary neutron stars; then from these signals one can estimate the maximum mass that a spinless neutron star (MTOV ) can have. In this paper, we investigate the problem of the determination of the MTOV precision from the post-merger detected by next-generation observatories. Our results show that only under the most optimistic scenario of signal-to-noise ratio for post-merger signals ($\mathrm{SNR}\geq 8$) and merger rate density (250Gpc-3yr-1), CE achieves marginally a mass precision in the range $δM/2 \approx 0.3-0.8\,M_{\odot}$ for a remnant mass of $2.57\,M_{\odot}$. We clarify that this precision represents the minimum uncertainty, corresponding to the most probable value (main peak) in the final mass distribution, showing that it depends on the value of the final (remnant) mass. Therefore, based on the results obtained in this study, it will still be necessary to improve the sensitivity at high frequencies of future ground-based gravitational wave observatories if one wants to obtain greater precision in the MTOV estimation. One possibility would be to improve the sensitivity in a frequency range that allows us to determine whether or not a black hole was formed in the coalescence.

gr-qc↗

arXiv2025

Poissonian Analysis of Glitches Observed in the LIGO Gravitational Wave Interferometers

This work investigates the temporal distribution of glitches detected by LIGO, focusing on the morphological classification provided by the Gravity Spy project. Starting from the hypothesis that these events follow a Poisson process, we developed a statistical methodology to evaluate the agreement between the empirical distribution of glitches and an ideal Poisson model, using the coefficient of determination ($R^2$) as the main metric. The analysis was applied to real data from the LIGO detectors in Livingston and Hanford throughout the O3 run, as well as to synthetic datasets generated from pure Poisson distributions. The results show that while several morphologies exhibit good agreement with the proposed model, classes such as 1400Ripples, Fast Scattering, and Power Line display significant deviations ($R^2 \leq 0.6$), suggesting that their origins do not strictly follow Poissonian statistics. In some cases, a dependence on the detector or the observing run was also observed. This analysis provides a quantitative basis for distinguishing glitch classes based on their degree of "Poissonness", potentially supporting the development of more effective glitch mitigation strategies in gravitational wave detector data.

gr-qc↗

arXiv2023

Search for gravitational-wave bursts in LIGO data at the Schenberg antenna sensitivity range

The Brazilian Mario Schenberg gravitational-wave detector remained operational until 2016 when it was disassembled. To assess the feasibility of reassembling the antenna, its capability to detect GW within its designed sensitivity parameters needs to be evaluated. Although the antenna is currently disassembled, insights can be gleaned from the O3 data of the LIGO detectors, given the similarities between Schenberg's ultimate sensitivity and the interferometers' sensitivity in the [3150-3260] Hz band. The search focused on signals lasting from ms to seconds, with no assumptions about their morphology, polarization, and arrival sky direction. Data analysis was performed using the coherent WaveBurst pipeline in the frequency range between 512 Hz and 4096 Hz, specifically targeting signals with bandwidths overlapping the Schenberg frequency band. However, the O3 data did not yield statistically significant evidence of GW bursts. This null result allowed for the characterization of the search efficiency in identifying simulated signal morphologies and setting upper limits on the GW burst event rate as a function of strain amplitude. The current search is sensitive to sources emitting isotropically $5\times10^{-6} M_{\odot}c^2$ in GWs from a distance of 10 kiloparsecs with a 50\% detection efficiency at a false alarm rate of 1 per 100 years. Moreover, we revisited estimations of detecting f-modes of neutron stars excited by glitches, setting the upper limit of the f-mode energy for the population of Galactic pulsars to $\sim 8 \times 10^{-8} M_{\odot}c^2$ at 3205 Hz. Our simulations suggest f-modes are an unlikely source of gravitational waves for the aSchenberg. Nevertheless, its potential in probing other types of GW short transients, such from giant flares from magnetars, post-merger phase of binary NSs, or the inspiral of binaries of primordial BHs with sub-solar masses, remains promising.

gr-qc↗

arXiv2015

Development of superconducting Klystron cavity for the Mario Schenberg gravitational wave detector

Superconducting reentrant cavities can be used in parametric transducers for Gravitational Wave antennas. The Mario Schenberg detector, which is being built by the GRAVITON group at Instituto Nacional de Pesquisas Espaciais (INPE), basically consists of a resonant mass (ball) and a set of parametric transducers in order to monitor the fundamental modes of vibration. When coupled to the antenna, the transducer-sphere system will work as a mass-spring system. In this work the main task is the development of parametric transducers consisting of reentrant superconducting cavity with high performance to be implemented in the Mario Schenberg detector. Many geometries, materials and designs have been tested and compared to optimize parameters such as electric and mechanical Q-factor. The aim is the construction of a complete set of nine parametric transducers that, attached to the spherical antenna, will possibly reach the sensitivity $h$ $\sim$ 10$^{-22}$ $Hz$$^{-1/2}$ in the near future.

astro-ph.IM↗

arXiv2010

The Past, Present and Future of the Resonant-Mass Gravitational Wave Detectors

Resonant-mass gravitational waves detectors are reviewed from the concept of gravitational waves and its mathematical derivation, using Einstein's general relativity, to the present status of bars and spherical detectors, and their prospects for the future, which include dual detectors and spheres with non-resonant transducers. The review covers not only the technical aspects of detectors and the science that will be done, but also analyses the subject in a historic perspective, covering the various detection efforts over four decades, starting from Weber's pioneering work.

astro-ph.IM↗