Cross-correlating galaxy catalogs and gravitational waves: a tomographic approach. (arXiv:2002.02466v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Calore_F/0/1/0/all/0/1">F. Calore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cuoco_A/0/1/0/all/0/1">A. Cuoco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Regimbau_T/0/1/0/all/0/1">T. Regimbau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sachdev_S/0/1/0/all/0/1">S. Sachdev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Serpico_P/0/1/0/all/0/1">P. D. Serpico</a>
Unveiling the origin of the coalescing binaries detected via gravitational
waves (GW) is challenging, notably if no multi-wavelength counterpart is
detected. One important quantity for diagnostics is their distribution with
respect to the large scale structures of the universe, as encoded, for
instance, in their (linear) biases. We discuss the perspectives of inferring
these quantities via the cross-correlation of galaxy catalogs with mock GW
ones, using both existing and forthcoming galaxy catalogs and using realistic
Monte Carlo simulations of GW events. We find that the bias should be
marginally detectable for a 10-year data taking of current generation detectors
at design sensitivity, at least for binary neutron star mergers. The
forthcoming five detector network would allow for a firmer detection of this
signal and, in combination with future cosmological surveys, would also permit
the detection of the coalescing black hole bias. Such a measurement may also
unveil, for instance, a primordial origin of coalescing black holes. To attain
this goal, we find that it is crucial to adopt a tomographic approach and to
reach a sufficiently accurate localization of GW events. The depth of
forthcoming surveys will be fully exploited by third generation GW detectors,
which will allow one to perform precision studies of the coalescing black holes
bias and attain rather advanced model discrimination capabilities, at a few
percent level.
Unveiling the origin of the coalescing binaries detected via gravitational
waves (GW) is challenging, notably if no multi-wavelength counterpart is
detected. One important quantity for diagnostics is their distribution with
respect to the large scale structures of the universe, as encoded, for
instance, in their (linear) biases. We discuss the perspectives of inferring
these quantities via the cross-correlation of galaxy catalogs with mock GW
ones, using both existing and forthcoming galaxy catalogs and using realistic
Monte Carlo simulations of GW events. We find that the bias should be
marginally detectable for a 10-year data taking of current generation detectors
at design sensitivity, at least for binary neutron star mergers. The
forthcoming five detector network would allow for a firmer detection of this
signal and, in combination with future cosmological surveys, would also permit
the detection of the coalescing black hole bias. Such a measurement may also
unveil, for instance, a primordial origin of coalescing black holes. To attain
this goal, we find that it is crucial to adopt a tomographic approach and to
reach a sufficiently accurate localization of GW events. The depth of
forthcoming surveys will be fully exploited by third generation GW detectors,
which will allow one to perform precision studies of the coalescing black holes
bias and attain rather advanced model discrimination capabilities, at a few
percent level.
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