Simultaneous event detection rates by electromagnetic and gravitational wave detectors in the Advanced Era of LIGO and Virgo

We present several estimates of the rate of simultaneous detection of the merging of a binary system of neutron stars in the electromagnetic and the gravitational wave domains, assuming that they produce short GRBs. We have based our estimations on a carefully selected sample of short gamma-ray bursts, corrected from redshift effects. The results presented in this paper are based on actual observation only. In the electromagnetic spectrum, we considered observations by current (Swift and Fermi}) and future (LOFT and SVOM) missions. In the gravitational wave domain, we consider detections by the Advanced Virgo instrument alone and the network of both Advanced LIGO and Advanced Virgo. We discuss on the possible biases present in our sample, and how to fix them. For present missions, assuming a detection in the following years, we find that we should observe simultaneously between 0.11 and 4.2 gravitational wave events per year with Swift} and Fermi} respectively. For future projects (LOFT and SVOM) we can expect less than one common detection per year. We check the consistency of our results with several previously published rate of detection of gravitational waves.Comment: 7 pages, accepted for publication in MNRAS, with note added in proof correcting the rates for Fermi/SVOM experiment. Added tables 5 and 6 that are corrected and replace tables 2 and

Simultaneous detection rates of binary neutron star systems in advanced Virgo/LIGO and GRB detectors

The coalescence of two compact objects is a key target for the new gravitational wave observatories such as Advanced-Virgo (AdV), Advanced-LIGO (aLIGO) and KAGRA. This phenomenon can lead to the simultaneous detection of electromagnetic waves in the form of short GRBs (sGRBs) and gravitational wave transients. This will potentially allow for the first time access to the fireball and the central engine properties. We present an estimation of the detection rate of such events, seen both by a Swift-like satellite and AdV/ALIGO. This rate is derived only from the observations of sGRBs. We show that this rate, if not very high, predicts a few triggers during the whole life time of Advanced LIGO-Virgo. We discuss how to increase it using some dedicated observational strategies. We apply our results to other missions such as the SVOM French-Chinese satellite project or LOFT.Comment: 7 pages, 1 figure, 7th Huntsville Gamma-Ray Burst Symposium, GRB 2013: paper 18 in eConf Proceedings C130414

Jet Geometry and Rate Estimate of Coincident Gamma Ray Burst and Gravitational Wave Observations

Short Gamma-Ray Burst (SGRB) progenitors have long been thought to be coalescing binary systems of two Neutron Stars (NSNS) or a Neutron Star and a Black Hole (NSBH). The August 17$^{\rm th}$, 2017 detection of the GW170817 gravitational-wave signal by Advanced LIGO and Advanced Virgo in coincidence with the electromagnetic observation of the SGRB GRB 170817A confirmed this scenario and provided new physical information on the nature of these astronomical events. We use SGRB observations by the Neil Gehrels Swift Observatory Burst Alert Telescope and GW170817/GRB 170817A observational data to estimate the detection rate of coincident gravitational-wave and electromagnetic observations by a gravitational-wave detector network and constrain the physical parameters of the SGRB jet structure. We estimate the rate of gravitational-wave detections coincident with SGRB electromagnetic detections by the Fermi Gamma-ray Burst Monitor to be between $\sim$ 0.1 and $\sim$ 0.6 yr$^{-1}$ in the third LIGO-Virgo observing run and between $\sim$ 0.3 and $\sim$ 1.8 yr$^{-1}$ for the LIGO-Virgo-KAGRA network at design sensitivity. Assuming a structured model with a uniform ultra-relativistic jet surrounded by a region with power-law decay emission, we find the jet half-opening angle and the power-law decay exponent to be $\theta_c\sim 7\,{}^\circ$ -- $22\,{}^\circ$ and $s\sim 5$ -- $30$ at 1$\sigma$ confidence level, respectively.Comment: 20 pages, 10 figure

Binary compact systems as sources of multimessengers : rate, distribution, emissions

La coalescence d'objets compacts (étoiles à neutrons entre elles ou étoile à neutrons avec un trou noir) émet des ondes gravitationnelles et on pense qu’elle produit un sursaut gamma court. Avec l'arrivée des détecteurs d'ondes gravitationnelles de seconde génération, on s'attend à détecter ce signal, qui est l'un des mieux modélisé.L'observation en coïncidence des ondes gravitationnelles émises par ce système et de l'émission électromagnétique sera une source d'informations considérable pour la compréhension de ces phénomènes, de leur progéniteur et du moteur central. Le but de ma thèse a été d’estimer ce taux de détections en coïncidence attendus en fonction des différents instruments. La première méthode se base sur les observations, j’ai donc sélectionné et étudié un échantillon de 31 sursauts gamma courts possédant une mesure de distance. Après avoir dérivé un taux local isotropique du nombre de sursauts gamma courts pour différents satellites, j’ai utilisé la seconde méthode de Monte Carlo avec la simulation de cette population de sursauts gamma courts. La différence entre les taux dérivés des observations et celui venant des simulations est expliqué par la présence d'une sous-population à bas redshift qui était sous-estimée auparavant. Cette thèse montre la faisabilité d'une étude en coïncidence et les stratégies observationnelles à adopter. La compréhension de notre échantillon de sursauts gamma courts, avec une nouvelle sous-population à bas redshift et basse-luminosité, est cruciale dans la préparation de ces détections simultanées.The coalescence of compact binaries (two neutron stars or a neutron star and a black hole) emits gravitational waves and are thought to produce a short Gamma-Ray Burst (sGRB). With the second generation of gravitational waves detector, the detection in coincidence of both electromagnetic and gravitational emission will open a new window in astrophysics; the multimessenger area. It will allow the understanding of this phenomena, their progenitor and central engine. The goal of this thesis was to made an estimation of the coincident rate for different instruments, using two different method. The first one was based on the oberservations. Thus, I selected a sample of 31 sGRBs of known redshift based on specific criteria. After studying the spectral, temporal and host properties, I derived the isotropic local rate corrected from all known biases. This result was then applied to different satellites and gravitational detectors. After that I simulated this population to confirm this coincident rate with the Monte Carlo simulations. The difference between the two results is explained by a low-redshift population that can't be reproduce by the simulations, and was underestimated before. After tested different parameters for the model, I conclude that this non reproducible population of faint sGRBs at low redshift might be due to an other sort of progenitor. This thesis shows the feasibility of a coincident detection and the observational strategy that should be adopted. The understanding of our sample of sGRB is crucial in the preparation of this coincident detection

Les systèmes binaires compacts comme sources de multimessagers : taux, distribution, émissions

The coalescence of compact binaries (two neutron stars or a neutron star and a black hole) emits gravitational waves and are thought to produce a short Gamma-Ray Burst (sGRB). With the second generation of gravitational waves detector, the detection in coincidence of both electromagnetic and gravitational emission will open a new window in astrophysics; the multimessenger area. It will allow the understanding of this phenomena, their progenitor and central engine. The goal of this thesis was to made an estimation of the coincident rate for different instruments, using two different method. The first one was based on the oberservations. Thus, I selected a sample of 31 sGRBs of known redshift based on specific criteria. After studying the spectral, temporal and host properties, I derived the isotropic local rate corrected from all known biases. This result was then applied to different satellites and gravitational detectors. After that I simulated this population to confirm this coincident rate with the Monte Carlo simulations. The difference between the two results is explained by a low-redshift population that can't be reproduce by the simulations, and was underestimated before. After tested different parameters for the model, I conclude that this non reproducible population of faint sGRBs at low redshift might be due to an other sort of progenitor. This thesis shows the feasibility of a coincident detection and the observational strategy that should be adopted. The understanding of our sample of sGRB is crucial in the preparation of this coincident detection.La coalescence d'objets compacts (étoiles à neutrons entre elles ou étoile à neutrons avec un trou noir) émet des ondes gravitationnelles et on pense qu’elle produit un sursaut gamma court. Avec l'arrivée des détecteurs d'ondes gravitationnelles de seconde génération, on s'attend à détecter ce signal, qui est l'un des mieux modélisé.L'observation en coïncidence des ondes gravitationnelles émises par ce système et de l'émission électromagnétique sera une source d'informations considérable pour la compréhension de ces phénomènes, de leur progéniteur et du moteur central. Le but de ma thèse a été d’estimer ce taux de détections en coïncidence attendus en fonction des différents instruments. La première méthode se base sur les observations, j’ai donc sélectionné et étudié un échantillon de 31 sursauts gamma courts possédant une mesure de distance. Après avoir dérivé un taux local isotropique du nombre de sursauts gamma courts pour différents satellites, j’ai utilisé la seconde méthode de Monte Carlo avec la simulation de cette population de sursauts gamma courts. La différence entre les taux dérivés des observations et celui venant des simulations est expliqué par la présence d'une sous-population à bas redshift qui était sous-estimée auparavant. Cette thèse montre la faisabilité d'une étude en coïncidence et les stratégies observationnelles à adopter. La compréhension de notre échantillon de sursauts gamma courts, avec une nouvelle sous-population à bas redshift et basse-luminosité, est cruciale dans la préparation de ces détections simultanées

Etude électromagnétique des sources possibles de rayonnement gravitationnel

Thès

Target-of-opportunity observations of gravitational-wave events with Vera C. Rubin Observatory

The discovery of the electromagnetic counterpart to the binary neutron star (NS) merger GW170817 has opened the era of gravitational-wave multimessenger astronomy. Rapid identification of the optical/infrared kilonova enabled a precise localization of the source, which paved the way to deep multiwavelength follow-up and its myriad of related science results. Fully exploiting this new territory of exploration requires the acquisition of electromagnetic data from samples of NS mergers and other gravitational-wave sources. After GW170817, the frontier is now to map the diversity of kilonova properties and provide more stringent constraints on the Hubble constant, and enable new tests of fundamental physics. The Vera C. Rubin Observatory's Legacy Survey of Space and Time can play a key role in this field in the 2020s, when an improved network of gravitational-wave detectors is expected to reach a sensitivity that will enable the discovery of a high rate of merger events involving NSs (∼tens per year) out to distances of several hundred megaparsecs. We design comprehensive target-of-opportunity observing strategies for follow-up of gravitational-wave triggers that will make the Rubin Observatory the premier instrument for discovery and early characterization of NS and other compact-object mergers, and yet unknown classes of gravitational-wave events

Search for intermediate mass black hole binaries in the first observing run of Advanced LIGO

International audienceDuring their first observational run, the two Advanced LIGO detectors attained an unprecedented sensitivity, resulting in the first direct detections of gravitational-wave signals produced by stellar-mass binary black hole systems. This paper reports on an all-sky search for gravitational waves (GWs) from merging intermediate mass black hole binaries (IMBHBs). The combined results from two independent search techniques were used in this study: the first employs a matched-filter algorithm that uses a bank of filters covering the GW signal parameter space, while the second is a generic search for GW transients (bursts). No GWs from IMBHBs were detected; therefore, we constrain the rate of several classes of IMBHB mergers. The most stringent limit is obtained for black holes of individual mass 100  M⊙, with spins aligned with the binary orbital angular momentum. For such systems, the merger rate is constrained to be less than 0.93  Gpc−3 yr−1 in comoving units at the 90% confidence level, an improvement of nearly 2 orders of magnitude over previous upper limits

First low-frequency Einstein@Home all-sky search for continuous gravitational waves in Advanced LIGO data

International audienceWe report results of a deep all-sky search for periodic gravitational waves from isolated neutron stars in data from the first Advanced LIGO observing run. This search investigates the low frequency range of Advanced LIGO data, between 20 and 100 Hz, much of which was not explored in initial LIGO. The search was made possible by the computing power provided by the volunteers of the Einstein@Home project. We find no significant signal candidate and set the most stringent upper limits to date on the amplitude of gravitational wave signals from the target population, corresponding to a sensitivity depth of 48.7  [1/Hz]. At the frequency of best strain sensitivity, near 100 Hz, we set 90% confidence upper limits of 1.8×10-25. At the low end of our frequency range, 20 Hz, we achieve upper limits of 3.9×10-24. At 55 Hz we can exclude sources with ellipticities greater than 10-5 within 100 pc of Earth with fiducial value of the principal moment of inertia of 1038  kg m2