Calibration of gamma-ray bursts luminosity correlations using gravitational waves as standard sirens. (arXiv:1902.09677v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Y/0/1/0/all/0/1">Yu-Yang Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_F/0/1/0/all/0/1">F. Y. Wang</a> (NJU)
Gamma-ray bursts (GRBs) are a potential tool to probe high-redshift universe.
However, the circularity problem enforces people to find model-independent
methods to study the luminosity correlations of GRBs. Here, we present a new
method which uses gravitational waves as standard sirens to calibrate GRB
luminosity correlations. For the third-generation ground-based GW detectors
(i.e., Einstein Telescope), the redshifts of gravitational wave (GW) events
accompanied electromagnetic counterparts can reach out to $sim 4$, which is
more distant than type Ia supernovae ($zlesssim 2$). The Amati relation and
Ghirlanda relation are calibrated using mock GW catalogue from Einstein
Telescope. We find that the $1sigma$ uncertainty of intercepts and slopes of
these correlations can be constrained to less than 0.2% and 8% respectively.
Using calibrated correlations, the evolution of dark energy equation of state
can be tightly measured, which is important for discriminating dark energy
models.
Gamma-ray bursts (GRBs) are a potential tool to probe high-redshift universe.
However, the circularity problem enforces people to find model-independent
methods to study the luminosity correlations of GRBs. Here, we present a new
method which uses gravitational waves as standard sirens to calibrate GRB
luminosity correlations. For the third-generation ground-based GW detectors
(i.e., Einstein Telescope), the redshifts of gravitational wave (GW) events
accompanied electromagnetic counterparts can reach out to $sim 4$, which is
more distant than type Ia supernovae ($zlesssim 2$). The Amati relation and
Ghirlanda relation are calibrated using mock GW catalogue from Einstein
Telescope. We find that the $1sigma$ uncertainty of intercepts and slopes of
these correlations can be constrained to less than 0.2% and 8% respectively.
Using calibrated correlations, the evolution of dark energy equation of state
can be tightly measured, which is important for discriminating dark energy
models.
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