Constraining the Delay Time Distribution of Binary Neutron Stars with the Host Galaxies of Gravitational Wave Events. (arXiv:1904.08436v1 [astro-ph.GA])

Constraining the Delay Time Distribution of Binary Neutron Stars with the Host Galaxies of Gravitational Wave Events. (arXiv:1904.08436v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Safarzadeh_M/0/1/0/all/0/1">Mohammadtaher Safarzadeh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berger_E/0/1/0/all/0/1">Edo Berger</a>

The delay time distribution of (DTD) of binary neutron stars (BNS) remains
poorly constrained, mainly by the small known population of Galactic binaries,
the properties of short gamma-ray burst host galaxies, and inferences from
$r$-process enrichment. In the new era of BNS merger detections through
gravitational waves (GW), a new route to the DTD is the demographics of the
host galaxies, localized through associated electromagnetic counterparts. This
approach takes advantage of the correlation between star formation history
(SFH) and galaxy mass, such that the convolution of the SFH and DTD impacts the
BNS merger rate as a function of galaxy mass. Here we quantify this approach
for a power law DTD governed by two parameters: the power law index ($Gamma$)
and a minimum delay time ($t_{rm min}$). Under the reasonable assumption that
EM counterparts are likely only detectable in the local universe, accessible by
the current generation of GW detectors, we study how many host galaxies at
$zsim 0$ are required to constrain the DTD parameters. We find that the DTD is
mainly imprinted in the statistics of massive galaxies (stellar mass of
$M_*gtrsim 10^{10.5}$ M$_odot$, comparable to the host galaxy of GW170817).
Taking account of relevant uncertainties we find that $mathcal{O}(10^3)$ host
galaxies are required to constrain the DTD; for a fixed value of $t_{rm min}$,
as done in previous analyses of the DTD, $mathcal{O}(10^2)$ host galaxies will
suffice. Such a sample will become available within the next two decades, prior
to the advent of third-generation GW detectors.

The delay time distribution of (DTD) of binary neutron stars (BNS) remains
poorly constrained, mainly by the small known population of Galactic binaries,
the properties of short gamma-ray burst host galaxies, and inferences from
$r$-process enrichment. In the new era of BNS merger detections through
gravitational waves (GW), a new route to the DTD is the demographics of the
host galaxies, localized through associated electromagnetic counterparts. This
approach takes advantage of the correlation between star formation history
(SFH) and galaxy mass, such that the convolution of the SFH and DTD impacts the
BNS merger rate as a function of galaxy mass. Here we quantify this approach
for a power law DTD governed by two parameters: the power law index ($Gamma$)
and a minimum delay time ($t_{rm min}$). Under the reasonable assumption that
EM counterparts are likely only detectable in the local universe, accessible by
the current generation of GW detectors, we study how many host galaxies at
$zsim 0$ are required to constrain the DTD parameters. We find that the DTD is
mainly imprinted in the statistics of massive galaxies (stellar mass of
$M_*gtrsim 10^{10.5}$ M$_odot$, comparable to the host galaxy of GW170817).
Taking account of relevant uncertainties we find that $mathcal{O}(10^3)$ host
galaxies are required to constrain the DTD; for a fixed value of $t_{rm min}$,
as done in previous analyses of the DTD, $mathcal{O}(10^2)$ host galaxies will
suffice. Such a sample will become available within the next two decades, prior
to the advent of third-generation GW detectors.

http://arxiv.org/icons/sfx.gif