The Gravitational Wave Universe Toolbox

Yi, Shuang; Nelemans, G.; Brinkerink, Christiaan D.; Kostrzewa-Rutkowska, Z.; Timmer, Sjoerd T.; Stoppa, Fiorenzo; Rossi, Elena M.; Zwart, Simon F. Portegies

doi:10.1051/0004-6361/202141634

Cited by 12 publications

(12 citation statements)

References 181 publications

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“…https://observing.docs.ligo.org/plan/ 6 Estimated with the GW Universe Toolbox(Yi et al 2022): https://gwuniverse.org.…”

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confidence: 99%

Tidally-induced Magnetar Super Flare at the Eve of Coalescence with Its Compact Companion

Zhang

et al. 2022

ApJL

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In the late inspiral phase of a double neutron star (NS) or NS–black hole system in which one NS is a magnetar, the tidal force on the magnetar arisen from its companion will increase dramatically as the binary approaches. The tidal-induced deformation may surpass the maximum that the magnetar’s crust can sustain just seconds or subseconds before the coalescence. A catastrophic global crust destruction may thus occur, and the magnetic energy stored in the magnetar’s interior will have the opportunity to be released, which would be observed as a superflare with energy 100s of times larger than giant flares of magnetars. Such a mechanism can naturally explain the recently observed precursor of GRB 211211A, including its quasiperiodic oscillation. We predict that in the coming gravitational wave O4/O5 period, there could be a fraction of detected double NS mergers associated with such super flares. If observed, copious information on the structure and magnetic field in an NS interior can be obtained, which is hard to study elsewhere.

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“…https://observing.docs.ligo.org/plan/ 6 Estimated with the GW Universe Toolbox(Yi et al 2022): https://gwuniverse.org.…”

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confidence: 99%

Tidally-induced Magnetar Super Flare at the Eve of Coalescence with Its Compact Companion

Zhang

et al. 2022

ApJL

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“…Here we give a brief summary of the method. For details, we refer to Yi et al (2021). We first calculate a function D(z, m 1 , m 2 ), which represents the detectability of a BBH with redshift z, and primary and secondary masses m 1 , m 2 .…”

Section: Methodsmentioning

confidence: 99%

“…The other ingredient is the merger rate density distribution of BBH in the Universe, ṅ(z, m 1 , m 2 ). In the GW-Universe Toolbox, we integrate two parameterized function forms for ṅ(z, m 1 , m 2 ), namely pop-A and pop-B (see Yi et al 2021 for the description on the population models). For a more sophisticated ṅ(z, m 1 , m 2 ) from population synthesis simulations, see Belczynski et al (2002), Mapelli et al (2017Mapelli et al ( , 2022, Mapelli & Giacobbo (2018), Arca Sedda et al (2021), Banerjee (2022), van Son et al (2022, Singh et al (2021).…”

Section: Methodsmentioning

confidence: 99%

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The Gravitational Wave Universe Toolbox

Stoppa

Nelemans

et al. 2022

A&A

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Context: The GW-Universe Toolbox is a software package that simulates observations of the gravitational wave (GW) Universe with different types of GW detectors, including Earth-based and space-borne laser interferometers and pulsar timing arrays. It is accessible as a website, and can also be imported and run locally as a Python package. Methods: We employ the method used by the GW-Universe Toolbox to generate a synthetic catalogue of detection of stellar-mass binary black hole (BBH) mergers. As an example of its scientific application, we study how GW observations of BBHs can be used to constrain the merger rate as a function of redshift and masses. We study advanced LIGO (aLIGO) and the Einstein Telescope (ET) as two representatives of the second and third generation GW observatories, respectively. We also simulate the observations from a detector that is half as sensitive as the ET at its nominal designed sensitivity, which represents an early phase of the ET. We used two methods to obtain the constraints on the source population properties from the catalogues: the first uses a parameteric differential merger rate model and applies a Bayesian inference on the parameters; the other is non-parameteric and uses weighted Kernel density estimators. Results: Our results show the overwhelming advantages of the third generation detector over those of the second generation for the study of BBH population properties, especially at redshifts higher than ∼2, where the merger rate is believed to peak. With the simulated aLIGO catalogue, the parameteric Bayesian method can still give some constraints on the merger rate density and mass function beyond its detecting horizon, while the non-parametric method loses the constraining ability completely there. The difference is due to the extra information placed by assuming a specific parameterisation of the population model in the Bayesian method. In the non-parameteric method, no assumption of the general shape of the merger rate density and mass function are placed, not even the assumption of its smoothness. These two methods represent the two extreme situations of general population reconstruction. We also find that, despite the numbers of detected events of the half ET can easily be compatible with full ET after a longer observation duration, and the catalogue from the full ET can still give much better constraints on the population properties due to its smaller uncertainties on the physical parameters of the GW events.

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“…Additionally, next to already established high-energy (HE) detectors, such as Fermi/GBM (Meegan et al 2009) and Swift/BAT (Gehrels et al 2004), newer instruments such as Insight-HXMT (Song et al 2022) and GECAM-GRD (Xiao et al 2022;Zhang et al 2019Zhang et al ) (launched in 2017Zhang et al and 2020 will prove extremely useful in the search of sGRBs as electromagnetic (EM) counterparts to GW observations. Previously, we built open-source Python-based software, the Gravitational Wave Universe Toolbox (Yi et al 2022a,b, the GWToolbox or Toolbox hereafter for short) to make GW astrophysics easily accessible. The GWToolbox is available at its own website, or can alternatively be downloaded as a Python package 1 .…”

Section: Introductionmentioning

confidence: 99%

The Gravitational Wave Universe Toolbox

Hendriks

Nelemans

2023

A&A

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Context. In the current multi-messenger astronomy era, it is important that information about joint gravitational wave (GW) and electromagnetic (EM) observations through short gamma-ray bursts (sGRBs) remains easily accessible to each member of the GW-EM community. The possibility for non-experts to execute quick computations of joint GW-sGRB detections should be facilitated. Aims. For this study, we constructed a model for sGRBs and added this to the framework of the previously built Gravitational Wave Universe Toolbox (GWToolbox or Toolbox). We provide expected joint GW-sGRB detection rates for different combinations of GW detectors and high-energy (HE) instruments. Methods. We employed and adapted a generic GRB model to create a computationally low-cost top-hat jet model suitable for the GWToolbox. With the Toolbox, we simulated a population of binary neutron stars (BNSs) observed by a user-specified GW detector such as LIGO, Virgo, the Einstein Telescope (ET), or the Cosmic Explorer (CE). Based on the characteristics of each binary, our model predicts the properties of a resulting sGRB, as well as its detectability for HE detectors such as Fermi/GBM, Swift/BAT, or GECAM.Results. We report predicted joint detection rates for combinations of GW detectors (LIGO and ET) with HE instruments (Fermi/GBM, Swift/BAT, and GECAM). Our findings stress the significance of the impact that ET will have on multi-messenger astronomy. While the LIGO sensitivity is currently the limiting factor regarding the number of joint detections, ET will observe BNSs at such a rate that the vast majority of detected sGRBs will have a GW counterpart observed by ET. These conclusions hold for CE as well. Additionally, since LIGO can only detect BNSs up to a redshift of ∼0.1 where few sGRBs exist, a search for sub-threshold GW signals at higher redshifts using sGRB information from HE detectors has the potential to be very successful and significantly increase the number of joint detections. Equivalently, during the ET era, GW data can assist in finding sub-threshold sGRBs, potentially increasing, for example, the number of joint ET-Fermi/GBM observations by ∼270%. Lastly, we find that our top-hat jet model underestimates the number of joint detections that include an off-axis sGRB. We corrected for this by introducing a second, wider and weaker jet component. We predict that the majority of joint detections during the LIGO/Virgo era will include an off-axis sGRB, making GRB170817A not as unlikely as one would think based on the simplest top-hat jet model. In the ET era, most joint detections will contain an on-axis sGRB.

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The Gravitational Wave Universe Toolbox

Cited by 12 publications

References 181 publications

Tidally-induced Magnetar Super Flare at the Eve of Coalescence with Its Compact Companion

Tidally-induced Magnetar Super Flare at the Eve of Coalescence with Its Compact Companion

The Gravitational Wave Universe Toolbox

The Gravitational Wave Universe Toolbox

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