Kilonova Detectability with Wide-field Instruments

Chase, E. A.; O’Connor, B.; Fryer, Chris L.; Troja, E.; Korobkin, Oleg; Wollaeger, Ryan; Ristić, Marko; Fontes, Christopher J.; Hungerford, Aimee L.; Herring, Angela M.

doi:10.3847/1538-4357/ac3d25

Cited by 49 publications

(36 citation statements)

References 167 publications

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“…This work represents a significant step towards improved modelling for rapidly simulating populations of kNe consistent with BNS merger progenitors and detailed physics, which is necessary to make accurate predictions for detection prospects (Rosswog et al 2017;Scolnic et al 2017;Setzer et al 2019;Almualla et al 2021;Mochkovitch et al 2021;Sagués Carracedo et al 2021;Andreoni et al 2022;Chase et al 2022;Colombo et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Modelling Populations of Kilonovae

Setzer¹,

Peiris²,

Korobkin³

et al. 2022

Preprint

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The 2017 detection of a kilonova coincident with gravitational-wave emission has identified neutron star mergers as the major source of the heaviest elements, and dramatically constrained alternative theories of gravity. Observing a population of such sources has the potential to transform cosmology, nuclear physics, and astrophysics. However, with only one confident detection currently available, modelling the diversity of signals expected from such a population requires improved theoretical understanding. In particular, models which are quick to evaluate, and are calibrated with more detailed multi-physics simulations, are needed to design observational strategies for kilonovae detection, and to obtain rapid-response interpretations of new observations. We use grey-opacity models to construct populations of kilonovae, spanning ejecta parameters predicted by numerical simulations. Our modelling focuses on wavelengths relevant for upcoming optical surveys, such as the Rubin Observatory Legacy Survey of Space and Time (LSST). In these simulations, we implement heating rates that are based on nuclear reaction network calculations. We create a Gaussian-process emulator for kilonova grey opacities, calibrated with detailed radiative transfer simulations. Using recent fits to numerical relativity simulations, we predict how the ejecta parameters from BNS mergers shape the population of kilonovae, accounting for the viewing-angle dependence. Our simulated population of binary neutron star (BNS) mergers produce peak i-band absolute magnitudes −17 ≤ 𝑀 𝑖 ≤ −11. A comparison with detailed radiative transfer calculations indicates that further improvements are needed to accurately reproduce spectral shapes over the full light curve evolution.

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Section: Introductionmentioning

confidence: 99%

Modelling Populations of Kilonovae

Setzer¹,

Peiris²,

Korobkin³

et al. 2022

Preprint

Self Cite

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“…In our simulations we did not find any scenario where an event could not be observed if kilonovae lasted at least two days. The detectability and best strategy to observe kilonovae have been already studied (see, for instance, Cowperthwaite & Berger 2015;Mochkovitch et al 2021;Chase et al 2022). The exact details for the best observation strategy go beyond the scope of our work; still, we can neglect the impact of overlapping events for two reasons.…”

Section: Discussionmentioning

confidence: 99%

The lure of sirens: joint distance and velocity measurements with third generation detectors

Alfradique,

Quartin,

Amendola

et al. 2022

Preprint

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The next generation of detectors will detect gravitational waves from binary neutron stars at cosmological distances, for which around a thousand electromagnetic follow-ups may be observed per year. So far, most work devoted to the expected cosmological impact of these standard sirens employed them only as distance indicators. Only recently their use as tracers of clustering, similar to what already proposed for supernovae, has been studied. Focusing on the expected specifications of the Einstein Telescope (ET), we forecast here the performance on cosmological parameters of future standard sirens as both distance and density indicators, with emphasis on the linear perturbation growth index and on spatial curvature. We improve upon previous studies in a number of ways: a more detailed analysis of available telescope time, the inclusion of more cosmological and nuisance parameters, the Alcock-Paczynski correction, the use of sirens also as both velocity and density tracers, and a more accurate estimation of the distance posterior. We find that the analysis of the clustering of sirens improves the constraints on H 0 by 30% and on Ω k0 by over an order of magnitude, with respect to their use merely as distance indicators. With 5 years of joint ET and Rubin Observatory follow-ups we could reach precision of 0.1 km/s/Mpc in H 0 and 0.02 in Ω k0 using only data in the range 0 < z < 0.5. We also find that the use of sirens as tracers of density, and not only velocity, yields good improvements on the growth of structure constraints.

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“…Although previous optical observations were able to capture the kilonova associated with GW170817, it was already fading and clouded a complete understanding of the nature of the blue ejecta (Cowperthwaite et al 2017;Nicholl et al 2017). Chase et al (2022) provide an in depth review of kilonova detectability prospects across multiple observing bands for a selection of current and planned wide field-of-view observatories.…”

Section: Outlook and Discussionmentioning

confidence: 99%

Observing Scenarios for the Next Decade of Early Warning Detection of Binary Neutron Stars

Magee

Borhanian

2022

ApJ

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We describe representative observing scenarios for early warning detection of binary neutron star mergers with the current generation of ground-based gravitational wave detectors as they approach design sensitivity. We incorporate recent estimates of the infrastructure latency and detector sensitivities to provide up-to-date predictions. We use Fisher analysis to approximate the associated localizations, and we directly compare to Bayestar to quantify biases inherited from this approach. In particular, we show that Advanced LIGO and Advanced Virgo will detect and distribute ≲1 signal with signal-to-noise ratio greater than 15 before a merger in their fourth observing run provided they maintain a 70% duty cycle. This is consistent with previous early warning detection estimates. We estimate that 60% of all observations and 8% of those detectable 20 s before a merger will be localized to ≲100 deg2. If KAGRA is able to achieve a 25 Mpc horizon, 70% of these binary neutron stars will be localized to ≲100 deg2 by a merger. As the Aundha–Hanford–KAGRA–Livingston–Virgo network approaches design sensitivity over the next ∼10 yr, we expect one (six) early warning alerts to be distributed 60 (0) s before a merger. Although adding detectors to the Hanford–Livingston–Virgo network at design sensitivity impacts the detection rate at ≲50% level, it significantly improves localization prospects. Given uncertainties in sensitivities, participating detectors, and duty cycles, we consider 103 future detector configurations so electromagnetic observers can tailor preparations toward their preferred models.

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Kilonova Detectability with Wide-field Instruments

Cited by 49 publications

References 167 publications

Modelling Populations of Kilonovae

Modelling Populations of Kilonovae

The lure of sirens: joint distance and velocity measurements with third generation detectors

Observing Scenarios for the Next Decade of Early Warning Detection of Binary Neutron Stars

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