Multi-messenger Bayesian parameter inference of a binary neutron-star merger. (arXiv:1812.04803v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Coughlin_M/0/1/0/all/0/1">Michael W. Coughlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dietrich_T/0/1/0/all/0/1">Tim Dietrich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Margalit_B/0/1/0/all/0/1">Ben Margalit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Metzger_B/0/1/0/all/0/1">Brian D. Metzger</a>
The combined detection of a binary neutron-star merger in both gravitational
waves (GWs) and electromagnetic (EM) radiation spanning the entire spectrum —
GW170817 / AT2017gfo / GRB170817A — marks a breakthrough in the field of
multi-messenger astronomy. Between the plethora of modeling and observations,
the rich synergy that exists among the available data sets creates a unique
opportunity to constrain the binary parameters, the equation of state of
supranuclear density matter, and the physical processes at work during the
kilonova and gamma-ray burst. However, previous works use simplified lightcurve
models and fits to numerical relativity simulation that do not account for all
of the relevant physical processes. We report, for the first time, Bayesian
parameter estimation combining information from GW170817, AT2017gfo, GRB170817
to obtain truly multi-messenger constraints on the tidal deformability
$tilde{Lambda} in [279,822]$, total binary mass $M in [2.724,2.752]
M_odot$, the radius of a $1.4$ solar mass neutron star $R in [11.1,13.4] rm
km$ (with additional $0.2 rm km$ systematic uncertainty), and an upper bound
on the mass ratio of $q leq 1.29$, all at 90% confidence. Our joint novel
analysis makes use of new phenomenological descriptions of the dynamical
ejecta, debris disk mass, and remnant black hole properties, all derived from a
large suite of numerical relativity simulations.
The combined detection of a binary neutron-star merger in both gravitational
waves (GWs) and electromagnetic (EM) radiation spanning the entire spectrum —
GW170817 / AT2017gfo / GRB170817A — marks a breakthrough in the field of
multi-messenger astronomy. Between the plethora of modeling and observations,
the rich synergy that exists among the available data sets creates a unique
opportunity to constrain the binary parameters, the equation of state of
supranuclear density matter, and the physical processes at work during the
kilonova and gamma-ray burst. However, previous works use simplified lightcurve
models and fits to numerical relativity simulation that do not account for all
of the relevant physical processes. We report, for the first time, Bayesian
parameter estimation combining information from GW170817, AT2017gfo, GRB170817
to obtain truly multi-messenger constraints on the tidal deformability
$tilde{Lambda} in [279,822]$, total binary mass $M in [2.724,2.752]
M_odot$, the radius of a $1.4$ solar mass neutron star $R in [11.1,13.4] rm
km$ (with additional $0.2 rm km$ systematic uncertainty), and an upper bound
on the mass ratio of $q leq 1.29$, all at 90% confidence. Our joint novel
analysis makes use of new phenomenological descriptions of the dynamical
ejecta, debris disk mass, and remnant black hole properties, all derived from a
large suite of numerical relativity simulations.
http://arxiv.org/icons/sfx.gif
