Galaxies-gravitational waves multimessenger cross-correlations: detectability and exploitation as an astrophysical probe. (arXiv:2007.08534v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Scelfo_G/0/1/0/all/0/1">Giulio Scelfo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boco_L/0/1/0/all/0/1">Lumen Boco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lapi_A/0/1/0/all/0/1">Andrea Lapi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Viel_M/0/1/0/all/0/1">Matteo Viel</a>
Gravitational waves astronomy has opened a new opportunity to study the
Universe. Full exploitation of this window can especially be provided by
combining data coming from gravitational waves experiments with luminous
tracers of the Large Scale Structure, like galaxies. In this work we
investigate the cross-correlation signal between gravitational waves resolved
events, as detected by the Einstein Telescope, and actively star-forming
galaxies. The galaxies distribution is computed through their UV and IR
luminosity functions and the gravitational waves events, assumed to be of
stellar origin, are self-consistently computed from the aforementioned galaxies
distribution. We provide a state-of-the-art treatment both on the astrophysical
side, keeping into account the impact of the star formation and chemical
evolution histories of galaxies, and in computing the cross-correlation signal,
for which we include lensing and relativistic effects. We find that, given
enough gravitational waves events and for some Star Formation Rate cuts, the
cross-correlation signal that would be measured is sufficiently strong to
overcome the noise and provide a clear signal. We suggest a possible
application of this methodology, which consists in the possibility of
distinguishing between different astrophysical scenarios and eventually test
theoretical models. We consider a proof-of-concept case in which a metallicity
dependence on the compact objects merger efficiency can be discriminated
against a reference case with no metallicity dependence. When considering
galaxies with a Star Formation Rate $psi > 10 : M_{odot} /rm{yr}$, a
Signal-to-Noise ratio around a value of 2-4 is gained after a decade of
observation time, depending on the observed fraction of the sky. This formalism
can be exploited as an astrophysical probe and could potentially allow to test
and compare different astrophysical scenarios.
Gravitational waves astronomy has opened a new opportunity to study the
Universe. Full exploitation of this window can especially be provided by
combining data coming from gravitational waves experiments with luminous
tracers of the Large Scale Structure, like galaxies. In this work we
investigate the cross-correlation signal between gravitational waves resolved
events, as detected by the Einstein Telescope, and actively star-forming
galaxies. The galaxies distribution is computed through their UV and IR
luminosity functions and the gravitational waves events, assumed to be of
stellar origin, are self-consistently computed from the aforementioned galaxies
distribution. We provide a state-of-the-art treatment both on the astrophysical
side, keeping into account the impact of the star formation and chemical
evolution histories of galaxies, and in computing the cross-correlation signal,
for which we include lensing and relativistic effects. We find that, given
enough gravitational waves events and for some Star Formation Rate cuts, the
cross-correlation signal that would be measured is sufficiently strong to
overcome the noise and provide a clear signal. We suggest a possible
application of this methodology, which consists in the possibility of
distinguishing between different astrophysical scenarios and eventually test
theoretical models. We consider a proof-of-concept case in which a metallicity
dependence on the compact objects merger efficiency can be discriminated
against a reference case with no metallicity dependence. When considering
galaxies with a Star Formation Rate $psi > 10 : M_{odot} /rm{yr}$, a
Signal-to-Noise ratio around a value of 2-4 is gained after a decade of
observation time, depending on the observed fraction of the sky. This formalism
can be exploited as an astrophysical probe and could potentially allow to test
and compare different astrophysical scenarios.
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