The effects of Galactic model uncertainties on LISA observations of double neutron stars. (arXiv:2205.01507v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Storck_A/0/1/0/all/0/1">Anatole Storck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Church_R/0/1/0/all/0/1">Ross Church</a>
The upcoming space-based gravitational wave observatory, LISA, will detect
binaries containing pairs of neutron stars. LISA observations of double neutron
stars, particularly in combination with electromagnetic observations, have the
potential to improve our understanding of neutron star physics and binary
evolution. In this work we assess the effect of changing the model of the Milky
Way on predictions of the population of double neutron star binaries that will
be detected and resolved by LISA. We conclude that the spatial and
gravitational-wave frequency distributions of these binaries are insensitive to
the choice of galactic models, compared to the stochastic variation induced by
the small sample size. In particular, the time-consuming computation of the
binaries’ Galactic orbits is not necessary. However, the distribution of
eccentricities is strongly affected by the choice of star-formation history.
Binaries with eccentricities e>0.1 that can be measured by LISA observations
are all younger than 100 Myr. We caution that comparisons between different
predictions for LISA observations need to use consistent star formation
histories, and that the Galactic star formation history should be taken into
account in the analysis of the observations themselves.
The upcoming space-based gravitational wave observatory, LISA, will detect
binaries containing pairs of neutron stars. LISA observations of double neutron
stars, particularly in combination with electromagnetic observations, have the
potential to improve our understanding of neutron star physics and binary
evolution. In this work we assess the effect of changing the model of the Milky
Way on predictions of the population of double neutron star binaries that will
be detected and resolved by LISA. We conclude that the spatial and
gravitational-wave frequency distributions of these binaries are insensitive to
the choice of galactic models, compared to the stochastic variation induced by
the small sample size. In particular, the time-consuming computation of the
binaries’ Galactic orbits is not necessary. However, the distribution of
eccentricities is strongly affected by the choice of star-formation history.
Binaries with eccentricities e>0.1 that can be measured by LISA observations
are all younger than 100 Myr. We caution that comparisons between different
predictions for LISA observations need to use consistent star formation
histories, and that the Galactic star formation history should be taken into
account in the analysis of the observations themselves.
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