Multi-Messenger Constraints on the Hubble Constant through Combination of Gravitational Waves, Gamma-Ray Bursts and Kilonovae from Neutron Star Mergers

Bulla, Mattia; Coughlin, M. W.; Dhawan, Suhail; Dietrich, Tim

doi:10.3390/universe8050289

Cited by 16 publications

(5 citation statements)

References 168 publications

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“…Distinct polarization features are observed from various LOS directions, with the maximum polarization occurring at θ los = 90°and the minimum polarization occurring at θ los = 0°. While parameter degeneracy is more likely to occur at low P values, systems with larger P values will exhibit a more prominent angular dependence, indicating that the polarimetry is a potential tool for probing angledependent information (Bulla et al 2022).…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems

Wen,

Gao,

et al. 2023

ApJ

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The formation of black hole–neutron star (BH–NS) or BH–BH systems may be accompanied by special supernova (SN) signals, due to the accretion feedback from the companion BH. The additional heating, which is mainly attributed to the Blandford–Payne mechanism, would disrupt the isotropic nature of the luminosity distribution on the surface of the SN ejecta, leading to the appearance of polarization. Here we develop a three-dimensional Monte Carlo polarization simulation code to conduct simulations for these special SNe. We find that the maximum polarization level of ∼2% occurs at the peak time of SN emission in the “close-binary” scenario, while in the “faraway-binary” case maximum polarization (i.e., ∼0.7%) is observed at a considerably later time than the peak of the SN. The magnitude of polarization is dependent on the degree of unevenness in the luminosity distribution and the angle between the line of sight and the equatorial direction. When considering the geometric distortion of SN ejecta at the same time, the magnitude of polarization may either increase (for a oblate ellipsoidal shape) or decrease (for a prolate ellipsoidal shape). The polarization signatures represent a promising auxiliary instrument to facilitate the identification of the companion-fed SNe. Moreover, comparing the event rate of these special SNe with the event rate density of LIGO-Virgo-detected BH–NS/BH systems could further help to distinguish the BH–NS/BH formation channel.

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Section: Conclusion and Discussionmentioning

confidence: 99%

Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems

Wen,

Gao,

et al. 2023

ApJ

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“…The redshift can most easily be determined from the detection of the optical counterpart (KN) caused by a NS merger. The most promising methods for estimating inclination focus either on measuring the GRB afterglow time delay, the color evolution of the early KN light curve, or through polarimetry (Bulla et al 2022). Both the afterglow as well as the early KN evolution are prime targets for high-cadence ULTRASAT observations.…”

Section: Type Ia Supernovae: Ratesmentioning

confidence: 99%

ULTRASAT: A Wide-field Time-domain UV Space Telescope

Shvartzvald,

Waxman,

Gal-Yam

et al. 2024

ApJ

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The Ultraviolet Transient Astronomy Satellite (ULTRASAT) is scheduled to be launched to geostationary orbit in 2027. It will carry a telescope with an unprecedentedly large field of view (204 deg2) and near-ultraviolet (NUV; 230–290 nm) sensitivity (22.5 mag, 5σ, at 900 s). ULTRASAT will conduct the first wide-field survey of transient and variable NUV sources and will revolutionize our ability to study the hot transient Universe. It will explore a new parameter space in energy and timescale (months-long light curves with minutes cadence), with an extragalactic volume accessible for the discovery of transient sources that is >300 times larger than that of the Galaxy Evolution Explorer (GALEX) and comparable to that of the Vera Rubin Observatory’s Legacy Survey of Space and Time. ULTRASAT data will be transmitted to the ground in real time, and transient alerts will be distributed to the community in <15 minutes, enabling vigorous ground-based follow up of ULTRASAT sources. ULTRASAT will also provide an all-sky NUV image to >23.5 AB mag, over 10 times deeper than the GALEX map. Two key science goals of ULTRASAT are the study of mergers of binaries involving neutron stars, and supernovae. With a large fraction (>50%) of the sky instantaneously accessible, fast (minutes) slewing capability, and a field of view that covers the error ellipses expected from gravitational-wave (GW) detectors beyond 2026, ULTRASAT will rapidly detect the electromagnetic emission following binary neutron star/neutron star–black hole mergers identified by GW detectors, and will provide continuous NUV light curves of the events. ULTRASAT will provide early (hour) detection and continuous high-cadence (minutes) NUV light curves for hundreds of core-collapse supernovae, including for rarer supernova progenitor types.

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“…They are the promising sites to study the hydrodynamical interactions and microphysical processes associated with some of the most extreme macroscopic bulk motions in the Universe (Meszaros & Rees 1993;. Recently, it has also been demonstrated that GRB afterglows could serve as probes to study the Universe's expansion rate (see Bulla et al 2022 for a review), thereby helping to unravel the nature of the Hubble tension (see Di Valentino et al 2021 for a review).…”

Section: Introductionmentioning

confidence: 99%

jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow

Wang 王,

Dastidar,

Giannios

et al. 2024

ApJS

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Gamma-ray burst (GRB) afterglows are emissions from ultrarelativistic blast waves produced by a narrow jet interacting with surrounding matter. Since the first multimessenger observation of a neutron star merger, hydrodynamic modeling of GRB afterglows for structured jets with smoothly varying angular energy distributions has gained increased interest. While the evolution of a jet is well described by self-similar solutions in both ultrarelativistic and Newtonian limits, modeling the transitional phase remains challenging. This is due to the nonlinear spreading of a narrow jet to a spherical configuration and the breakdown of self-similar solutions. Analytical models are limited in capturing these nonlinear effects, while relativistic hydrodynamic simulations are computationally expensive, which restricts the exploration of various initial conditions. In this work, we introduce a reduced hydrodynamic model that approximates the blast wave as an infinitely thin two-dimensional surface. Further assuming axial symmetry, this model simplifies the simulation to one dimension and drastically reduces the computational costs. We have compared our modeling to relativistic hydrodynamic simulations and semianalytic methods, and applied it to fit the light curve and flux centroid motion of GRB 170817A. These comparisons demonstrate good agreement and validate our approach. We have developed this method into a numerical tool, jetsimpy, which models the synchrotron GRB afterglow emission from a blast wave with arbitrary angular energy and Lorentz factor distribution. Although the code is built with GRB afterglow in mind, it applies to any relativistic jet. This tool is particularly useful in Markov Chain Monte Carlo studies and is provided to the community.

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Multi-Messenger Constraints on the Hubble Constant through Combination of Gravitational Waves, Gamma-Ray Bursts and Kilonovae from Neutron Star Mergers

Cited by 16 publications

References 168 publications

Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems

Polarization Signature of Companion-fed Supernovae Arising from BH–NS/BH Progenitor Systems

ULTRASAT: A Wide-field Time-domain UV Space Telescope

jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow

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