Toward Rapid Transient Identification and Characterization of Kilonovae

Coughlin, M. W.; Dietrich, Tim; Kawaguchi, Kyohei; Smartt, S. J.; Stubbs, C. W.; Ujevic, Maximiliano

doi:10.3847/1538-4357/aa9114

Cited by 45 publications

(47 citation statements)

References 64 publications

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“…Based on the results from numerical relativity simulations, a rough empirical relation between the dynamical ejecta mass and the mass ratio of the NS binary has been established. Before the detection of GW170817, it has been proposed that such a relation could be used to explore NS-NS binary parameters from kilonova detections (Coughlin et al 2017). The LIGO-Virgo collaboration have employed such a relation to estimate the dynamical ejecta mass by using the GW measurements of GW170817 and used the resulting ejecta mass to estimate its contribution (without the inclusion of the disk wind ejecta) to the corresponding kilonova light curves from various models, but they did not directly invoke electromagnetic observations (Abbott et al 2017e).…”

Section: Conclusion and Discussionmentioning

confidence: 99%

A More Stringent Constraint on the Mass Ratio of Binary Neutron Star Merger GW170817

Cao

Zhang

2017

ApJL

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Recently, the LIGO-Virgo collaboration reported their first detection of gravitational wave (GW) signals from a low mass compact binary merger GW170817, which is most likely due to a double neutron star (NS) merger. With the GW signals only, the chirp mass of the binary is precisely constrained to 1.188 +0.004 −0.002 M , but the mass ratio is loosely constrained in the range 0.4 − 1, so that a very rough estimation of the individual NS masses (1.36 M < M 1 < 2.26 M and 0.86 M < M 2 < 1.36 M ) was obtained. Here we propose that if one can constrain the dynamical ejecta mass through performing kilonova modeling of the optical/IR data, by utilizing an empirical relation between the dynamical ejecta mass and the mass ratio of NS binaries, one may place a more stringent constraint on the mass ratio of the system. For instance, considering that the red "kilonova" component is powered by the dynamical ejecta, we reach a tight constraint on the mass ratio in the range of 0.46 − 0.59. Alternatively, if the blue "kilonova" component is powered by the dynamical ejecta, the mass ratio would be constrained in the range of 0.53 − 0.67. Overall, such a multi-messenger approach could narrow down the mass ratio of GW170817 system to the range of 0.46 − 0.67, which gives a more precise estimation of the individual NS mass than pure GW signal analysis, i.e. 1.61 M < M 1 < 2.11 M and 0.90 M < M 2 < 1.16 M .

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Section: Conclusion and Discussionmentioning

confidence: 99%

A More Stringent Constraint on the Mass Ratio of Binary Neutron Star Merger GW170817

Cao

Zhang

2017

ApJL

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“…Finally, we want to use our analysis to obtain information about the binary parameters, such as the total mass, mass ratio, and tidal deformability. The idea follows the discussion in Coughlin et al (2017): namely that information about the ejecta properties can be translated to constraints on the system parameters by fits such as those from Dietrich & Ujevic (2017). In this work, we improve on the fit of Dietrich & Ujevic (2017), which connects the intrinsic binary parameters with dynamical ejecta properties extracted from full 3D numerical relativity simulations.…”

Section: Inferring Source Propertiesmentioning

confidence: 99%

Constraints on the neutron star equation of state from AT2017gfo using radiative transfer simulations

Coughlin

Dietrich

Doctor

et al. 2018

Monthly Notices of the Royal Astronomical Society

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225

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The detection of the binary neutron star merger GW170817 together with the observation of electromagnetic counterparts across the entire spectrum inaugurated a new era of multimessenger astronomy. In this study, we incorporate wavelength-dependent opacities and emissivities calculated from atomic-structure data enabling us to model both the measured light curves and spectra of the electromagnetic transient AT2017gfo. Best fits of the observational data are obtained by Gaussian Process Regression, which allows us to present posterior samples for the kilonova and source properties connected to GW170817. Incorporating constraints obtained from the gravitational wave signal measured by the LIGO-Virgo Scientific Collaboration, we present a $90{{\ \rm per\ cent}}$ upper bound on the mass ratio q ≲ 1.38 and a lower bound on the tidal deformability of $\tilde{\Lambda } \gtrsim 197$, which rules out sufficiently soft equations of state. Our analysis is a path-finder for more realistic kilonova models and shows how the combination of gravitational wave and electromagnetic measurements allow for stringent constraints on the source parameters and the supranuclear equation of state.

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“…We compare these models to observational data following Coughlin et al (2017), i.e., randomized sets of lightcurves are computed for each model, and a χ 2 value is calculated between each model and the data. For the kilonova model, the priors are taken to be flat between: −5 ≤ log 10 (M ej /M ) ≤ 0, 0 ≤ v ej ≤ 0.3 c, and −9 ≤ log 10 (X lan ) ≤ −1.…”

Section: Data and Analysis Techniquementioning

confidence: 99%

A luminosity distribution for kilonovae based on short gamma-ray burst afterglows

Ascenzi

Coughlin

Dietrich

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The combined detection of a gravitational-wave signal, kilonova, and short gamma-ray burst (sGRB) from GW170817 marked a scientific breakthrough in the field of multi-messenger astronomy. But even before GW170817, there have been a number of sGRBs with possible associated kilonova detections. In this work, we re-examine these "historical" sGRB afterglows with a combination of state-of-the-art afterglow and kilonova models. This allows us to include optical/near-infrared synchrotron emission produced by the sGRB as well as ultraviolet/optical/near-infrared emission powered by the radioactive decay of r-process elements (i.e., the kilonova). Fitting the lightcurves, we derive the velocity and the mass distribution as well as the composition of the ejected material. The posteriors on kilonova parameters obtained from the fit were turned into distributions for the peak magnitude of the kilonova emission in different bands and the time at which this peak occurs. From the sGRB with an associated kilonova, we found that the peak magnitude in H bands falls in the range [-16.2, -13.1] (95% of confidence) and occurs within 0.8−3.6 days after the sGRB prompt emission. In g band instead we obtain a peak magnitude in range [-16.8, -12.3] occurring within the first 18 hr after the sGRB prompt. From the luminosity distributions of GW170817/AT2017gfo, kilonova candidates GRB130603B, GRB050709 and GRB060614 (with the possible inclusion of GRB150101B, GRB050724A, GRB061201, GRB080905A, GRB150424A, GRB160821B) and the upper limits from all the other sGRBs not associated with any kilonova detection we obtain for the first time a kilonova luminosity distribution in different bands.

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Toward Rapid Transient Identification and Characterization of Kilonovae

Cited by 45 publications

References 64 publications

A More Stringent Constraint on the Mass Ratio of Binary Neutron Star Merger GW170817

A More Stringent Constraint on the Mass Ratio of Binary Neutron Star Merger GW170817

Constraints on the neutron star equation of state from AT2017gfo using radiative transfer simulations

A luminosity distribution for kilonovae based on short gamma-ray burst afterglows

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