Constraining properties of neutron star merger outflows with radio observations

Dobie, Dougal; Kaplan, David L.; Hotokezaka, Kenta; Murphy, Tara; Deller, Adam T.; Hallinan, Gregg; Nissanke, S.

doi:10.1093/mnras/staa789

Cited by 15 publications

(12 citation statements)

References 113 publications

(133 reference statements)

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“…Additionally, the relativistic nature of the jetted outflow can be revealed by VLBI observations (Mooley et al 2018a;Ghirlanda et al 2019) that evidence an apparent superluminal motion of the jet head. Detecting this centroid displacement is possible for events that are particularly close or bright or under specific inclination angle conditions (Duque et al 2019;Dobie et al 2020). Doing so further constrains ι and narrows down the measurement of H 0 , as shown in the case of GW170817.…”

Section: Inferring H 0 With Gravitational Waves and Electromagnetic Counterpartsmentioning

confidence: 99%

“…However, currently, these signals crucially lack modeling and observing history. Inclination angle measurements from kilonova data are very model dependent and lack robustness (Doctor 2020;Heinzel et al 2021). Only when the kilonova sample grows will the potential impact of kilonova-derived angle constraints be appreciated.…”

Section: Inferring H 0 With Gravitational Waves and Electromagnetic Counterpartsmentioning

confidence: 99%

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The potential role of binary neutron star merger afterglows in multimessenger cosmology

Mastrogiovanni

Duque

Chassande–Mottin

et al. 2021

A&A

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Binary neutron star mergers offer a new and independent means of measuring the Hubble constant H0 by combining the gravitational-wave inferred source luminosity distance with its redshift obtained from electromagnetic follow-up. This method is limited by the intrinsic degeneracy between the system distance and orbital inclination in the gravitational-wave signal. Observing the afterglow counterpart to a merger can further constrain the inclination angle, allowing this degeneracy to be partially lifted and improving the measurement of H0. In the case of the binary neutron star merger GW170817, afterglow light-curve and imaging modeling thus allowed the H0 measurement to be improved by a factor of three. However, systematic access to afterglow data is far from guaranteed. In fact, though each one allows a leap in H0 precision, these afterglow counterparts should prove rare in forthcoming multimessenger campaigns. We combine models for emission and detection of gravitational-wave and electromagnetic radiation from binary neutron star mergers with realistic population models and estimates for afterglow inclination angle constraints. Using these models, we quantify how fast H0 will be narrowed down by successive multimessenger events with and without the afterglow. We find that because of its rareness and though it greatly refines angle estimates, the afterglow counterpart should not significantly contribute to the measurement of H0 in the long run.

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Section: Inferring H 0 With Gravitational Waves and Electromagnetic Counterpartsmentioning

confidence: 99%

Section: Inferring H 0 With Gravitational Waves and Electromagnetic Counterpartsmentioning

confidence: 99%

The potential role of binary neutron star merger afterglows in multimessenger cosmology

Mastrogiovanni

Duque

Chassande–Mottin

et al. 2021

A&A

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“…To assess the detectability of radio afterglows we use the same power-law jet model as Dobie et al (2020). The kinetic energy is distributed according to…”

Section: Emission From a Power-law Jetmentioning

confidence: 99%

“…We also assume the fraction of shock energy distributed to the electrons and magnetic field of the jet to be 𝜖 𝑒 = 0.1 and 𝜖 𝐵 = 0.01 respectively, based on the canonical GRB microphysics parameters (e.g. Berger 2014, and references therein), which we note are higher than those typically found for GW170817 (see Table 1 of Dobie et al 2020). Our results rely on these parameter assumptions, which are biased towards GW170817-like events and therefore may not represent the general population of compact binary coalescences.…”

Section: Emission From a Power-law Jetmentioning

confidence: 99%

Radio Afterglows from Compact Binary Coalescences: Prospects for Next-Generation Telescopes

Dobie,

Murphy,

Kaplan

et al. 2021

Preprint

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The detection of gravitational waves from a neutron star merger, GW170817, marked the dawn of a new era in time-domain astronomy. Monitoring of the radio emission produced by the merger, including high-resolution radio imaging, enabled measurements of merger properties including the energetics and inclination angle. In this work we compare the capabilities of current and future gravitational wave facilities to the sensitivity of radio facilities to quantify the prospects for detecting the radio afterglows of gravitational wave events. We consider three observing strategies to identify future mergers -widefield follow-up, targeting galaxies within the merger localisation and deep monitoring of known counterparts. We find that while planned radio facilities like the Square Kilometre Array will be capable of detecting mergers at gigaparsec distances, no facilities are sufficiently sensitive to detect mergers at the range of proposed third-generation gravitational wave detectors that would operate starting in the 2030s.

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“…Chen et al 2019). Several works have shown how independent EM observations can constrain the binary viewing angle (Guidorzi et al 2017;Hotokezaka et al 2019;Dobie et al 2020;Dhawan et al 2020), thus providing an external constraint that breaks the inclination angle-distance degeneracy, one of the main sources of uncertainty for the distance precision. When estimated independently of the distance, viewing angle constraints can be as good as ∼ 5 deg for GW170817 when using X-ray and radio data, and ∼ 10 deg from optical-NIR data (Dhawan et al 2020), leading to a factor 2 or better improvement on the distance precision.…”

Section: Experiments Specificsmentioning

confidence: 99%

Probing gravity and growth of structure with gravitational waves and galaxies' peculiar velocity

Palmese,

Kim

2020

Preprint

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The low-redshift velocity field is a unique probe of the growth of cosmic structure and gravity. We propose to use distances from gravitational wave (GW) detections, in conjunction with the redshifts of their host galaxies from wide field spectroscopic surveys (e.g. DESI, 4MOST, TAIPAN), to measure peculiar motions within the local Universe. Such measurement has the potential to constrain the growth rate f σ 8 and test gravity through determination of the gravitational growth index γ, complementing constraints from other peculiar velocity measurements. We find that binary neutron star mergers with associated counterpart at z 0.2 that will be detected by the Einstein Telescope (ET) will be able to constrain f σ 8 to ∼ 3% precision after 10 years of operations when combined with galaxy overdensities from DESI and TAIPAN. If a larger network of third generation GW detectors is available (e.g. including the Cosmic Explorer), the same constraints can be reached over a shorter timescale (∼ 5 years for a 3 detectors network). The same events (plus information from their hosts' redshifts) can constrain γ to σ γ 0.04. This constraint is precise enough to discern General Relativity from other popular gravity models at 3σ. This constraint is improved to σ γ ∼ 0.02 − 0.03 when combined with galaxy overdensities. The potential of combining galaxies' peculiar velocities with gravitational wave detections for cosmology highlights the need for extensive optical to near-infrared follow-up of nearby gravitational wave events, or exquisite GW localization, in the next decade.

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Constraining properties of neutron star merger outflows with radio observations

Cited by 15 publications

References 113 publications

The potential role of binary neutron star merger afterglows in multimessenger cosmology

The potential role of binary neutron star merger afterglows in multimessenger cosmology

Radio Afterglows from Compact Binary Coalescences: Prospects for Next-Generation Telescopes

Probing gravity and growth of structure with gravitational waves and galaxies' peculiar velocity

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