Actually, the main cosmological contribution from the kilonova binary neutron star (BNS) detection was an independent measurement of the Hubble constant, $H_0$. It came back as 70 km/(sec Mpsec), with uncertianties (68%) of +- 10 approx. The accuracies will improve over time with higher SNRs and a greater number of gravitational wave detections.

The independence is due to the distance-ladder independent measurement of distance using the gravitational wave (GW) parameters and analysis as a standard siren. Using electromagnetic redshifts for the Galaxy, and doing some peculiar velocity adjustments, the Hubble constant is then obtained. Within the accuracy limits it is consistent with Planck CMB measurements. See the LIGO papers, at http://www.nature.com/nature/journal/vaap/ncurrent/pdf/nature24471.pdf and at https://journals.aps.org/prl/pdf/10.1103/PhysRevLett.119.161101

In the longer term, probably in the 2020s space based gravitational observatories with longer arm lengths (currently eLISA is proposed to have about 1 million Kms arm lengths) will allow observations of larger scale and longer wavelength structures such as possible anomalies early after the Big Bang. With those and improved earth based detectors we will be able to see beyond the current electromagnetic wall around tHe radiation decoupling at about 300,000 light years after the BIg Bang. We will be seeing much more energetic physics, and look for primordial structures like branes, or domain walls, or primordial black holes, as well as possible detections of GW waves from inflation, and other exotic phenomena, we will have a chance to probe those scales with GW detections. See eg Actually, the main cosmological contribution from the kilonova binary neutron star (BNS) detection was an independent measurement of the Hubble constant, $H_0$. It came back as 70 km/(sec Mpsec), with uncertianties (68%) of +- 10 approx. The accuracies will improve over time with higher SNRs and a greater number of gravitational wave detections.

The independence is due to the distance-ladder independent measurement of distance using the gravitational wave (GW) parameters and analysis as a standard siren. Using electromagnetic redshifts for the Galaxy, and doing some peculiar velocity adjustments, the Hubble constant is then obtained. Within the accuracy limits it is consistent with Planck CMB measurements. See the LIGO papers, at http://www.nature.com/nature/journal/vaap/ncurrent/pdf/nature24471.pdf and at https://journals.aps.org/prl/pdf/10.1103/PhysRevLett.119.161101

In the longer term, probably in the 2020s space based gravitational observatories with longer arm lengths will allow observations of larger scale and longer wavelength structures such as possible anomalies early after the Big Bang. With those and improved earth based detectors we will be able to see beyond the current electromagnetic wall around tHe radiation decoupling at about 300,000 light years after the BIg Bang. We will be seeing much more energetic physics, and look for primordial structures like branes, domain walls, primordial black holes and inflation eevidence and parameterse, and other exotic matter and phenomena. We will have a chance to probe those scales with GW detections. See eg https://arxiv.org/pdf/1405.0504.pdf

GWS open up a whole new window of observations, a completely new and independent messenger of information to add to all our electromagnetic observations.

Actually, the main cosmological contribution from the kilonova binary neutron star (BNS) detection was an independent measurement of the Hubble constant, $H_0$. It came back as 70 km/(sec Mpsec), with uncertianties (68%) of +- 10 approx. The accuracies will improve over time with higher SNRs and a greater number of gravitational wave detections.

The independence is due to the distance-ladder independent measurement of distance using the gravitational wave (GW) parameters and analysis as a standard siren. Using electromagnetic redshifts for the Galaxy, and doing some peculiar velocity adjustments, the Hubble constant is then obtained. Within the accuracy limits it is consistent with Planck CMB measurements. See the LIGO papers, at http://www.nature.com/nature/journal/vaap/ncurrent/pdf/nature24471.pdf and at https://journals.aps.org/prl/pdf/10.1103/PhysRevLett.119.161101

In the longer term, probably in the 2020s space based gravitational observatories with longer arm lengths (currently eLISA is proposed to have about 1 million Kms arm lengths) will allow observations of larger scale and longer wavelength structures such as possible anomalies early after the Big Bang. With those and improved earth based detectors we will be able to see beyond the current electromagnetic wall around tHe radiation decoupling at about 300,000 light years after the BIg Bang. We will be seeing much more energetic physics, and look for primordial structures like branes, or domain walls, or primordial black holes, as well as possible detections of GW waves from inflation, and other exotic phenomena, we will have a chance to probe those scales with GW detections. See eg https://arxiv.org/pdf/1405.0504.pdf

GWs open up a whole new window of observations, a completely new and independent messenger of information to add to all our electromagnetic observations.

Actually, the main cosmological contribution from the kilonova binary neutron star (BNS) detection was an independent measurement of the Hubble constant, $H_0$. It came back as 70 km/(sec Mpsec), with uncertianties (68%) of +- 10 approx. The accuracies will improve over time with higher SNRs and a greater number of gravitational wave detections.

The independence is due to the distance-ladder independent measurement of distance using the gravitational wave (GW) parameters and analysis as a standard siren. Using electromagnetic redshifts for the Galaxy, and doing some peculiar velocity adjustments, the Hubble constant is then obtained. Within the accuracy limits it is consistent with Planck CMB measurements. See the LIGO papers, at http://www.nature.com/nature/journal/vaap/ncurrent/pdf/nature24471.pdf and at https://journals.aps.org/prl/pdf/10.1103/PhysRevLett.119.161101

In the longer term, probably in the 2020s space based gravitational observatories with longer arm lengths (currently eLISA is proposed to have about 1 million Kms arm lengths) will allow observations of larger scale and longer wavelength structures such as possible anomalies early after the Big Bang. With those and improved earth based detectors we will be able to see beyond the current electromagnetic wall around tHe radiation decoupling at about 300,000 light years after the BIg Bang. We will be seeing much more energetic physics, and look for primordial structures like branes, or domain walls, or primordial black holes, as well as possible detections of GW waves from inflation, and other exotic phenomena, we will have a chance to probe those scales with GW detections. See eg Actually, the main cosmological contribution from the kilonova binary neutron star (BNS) detection was an independent measurement of the Hubble constant, $H_0$. It came back as 70 km/(sec Mpsec), with uncertianties (68%) of +- 10 approx. The accuracies will improve over time with higher SNRs and a greater number of gravitational wave detections.

The independence is due to the distance-ladder independent measurement of distance using the gravitational wave (GW) parameters and analysis as a standard siren. Using electromagnetic redshifts for the Galaxy, and doing some peculiar velocity adjustments, the Hubble constant is then obtained. Within the accuracy limits it is consistent with Planck CMB measurements. See the LIGO papers, at http://www.nature.com/nature/journal/vaap/ncurrent/pdf/nature24471.pdf and at https://journals.aps.org/prl/pdf/10.1103/PhysRevLett.119.161101

In the longer term, probably in the 2020s space based gravitational observatories with longer arm lengths will allow observations of larger scale and longer wavelength structures such as possible anomalies early after the Big Bang. With those and improved earth based detectors we will be able to see beyond the current electromagnetic wall around tHe radiation decoupling at about 300,000 light years after the BIg Bang. We will be seeing much more energetic physics, and if primordial structures like branes or primordial black holes existed, and other exotic phenomena, we will have a chance to probe those scales with GW detections. See eg

Actually, the main cosmological contribution from the kilonova binary neutron star (BNS) detection was an independent measurement of the Hubble constant, $H_0$. It came back as 70 km/(sec Mpsec), with uncertianties (68%) of +- 10 approx. The accuracies will improve over time with higher SNRs and a greater number of gravitational wave detections.

The independence is due to the distance-ladder independent measurement of distance using the gravitational wave (GW) parameters and analysis as a standard siren. Using electromagnetic redshifts for the Galaxy, and doing some peculiar velocity adjustments, the Hubble constant is then obtained. Within the accuracy limits it is consistent with Planck CMB measurements. See the LIGO papers, at http://www.nature.com/nature/journal/vaap/ncurrent/pdf/nature24471.pdf and at https://journals.aps.org/prl/pdf/10.1103/PhysRevLett.119.161101

In the longer term, probably in the 2020s space based gravitational observatories with longer arm lengths (currently eLISA is proposed to have about 1 million Kms arm lengths) will allow observations of larger scale and longer wavelength structures such as possible anomalies early after the Big Bang. With those and improved earth based detectors we will be able to see beyond the current electromagnetic wall around tHe radiation decoupling at about 300,000 light years after the BIg Bang. We will be seeing much more energetic physics, and look for primordial structures like branes, or domain walls, or primordial black holes, as well as possible detections of GW waves from inflation, and other exotic phenomena, we will have a chance to probe those scales with GW detections. See eg Actually, the main cosmological contribution from the kilonova binary neutron star (BNS) detection was an independent measurement of the Hubble constant, $H_0$. It came back as 70 km/(sec Mpsec), with uncertianties (68%) of +- 10 approx. The accuracies will improve over time with higher SNRs and a greater number of gravitational wave detections.

The independence is due to the distance-ladder independent measurement of distance using the gravitational wave (GW) parameters and analysis as a standard siren. Using electromagnetic redshifts for the Galaxy, and doing some peculiar velocity adjustments, the Hubble constant is then obtained. Within the accuracy limits it is consistent with Planck CMB measurements. See the LIGO papers, at http://www.nature.com/nature/journal/vaap/ncurrent/pdf/nature24471.pdf and at https://journals.aps.org/prl/pdf/10.1103/PhysRevLett.119.161101

In the longer term, probably in the 2020s space based gravitational observatories with longer arm lengths will allow observations of larger scale and longer wavelength structures such as possible anomalies early after the Big Bang. With those and improved earth based detectors we will be able to see beyond the current electromagnetic wall around tHe radiation decoupling at about 300,000 light years after the BIg Bang. We will be seeing much more energetic physics, and look for primordial structures like branes, domain walls, primordial black holes and inflation eevidence and parameterse, and other exotic matter and phenomena. We will have a chance to probe those scales with GW detections. See eg https://arxiv.org/pdf/1405.0504.pdf

GWS open up a whole new window of observations, a completely new and independent messenger of information to add to all our electromagnetic observations.