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Ground Based Gravitational Wave Astronomy: Role of Asian and Australia Detectors Results from the first two years of gravitational wave astronomy indicate that binary black holes coalesce within the Hubble volume at a rate of one every 4 minutes, while neutron stars coalesce at a rate of ~ 4 per minute. The origin of the binary black holes is uncertain. They could be remnants of coevolved binaries, they could be dynamically formed, or they could be of primordial origin. Neutron star coalescence has already given a clue to the neutron star equation of state, but sensitivity in the 1-4kHz range is inadequate to properly probe neutron star matter. Equally, the lack of sensitivity at high frequencies prevents black hole quasi-normal modes to be used to obtain black hole angular momentum data which can help distinguish formation mechanisms and provide deeper testing of general relativity near the event horizon. This talk review recent modelling of a pair 8km arm length Advanced LIGO type detectors in the Asia/Australia region. Such detectors could be the first stage of a future third generation detectors. Sensitivity improvements could be based on white light signal recycling and other quantum optic techniques. Modelling shows the significant benefits of expanding the world array of detectors. Even modest improvements will allow gravitational wave astronomy to monitor black hole coalescence across the Hubble volume, and to deeply probe the neutron star matter. This talk will review the various concepts for improved detectors and show that an improved world array is capable of mapping large scale black hole density fluctuations, which in turn may help determine the total population of black holes in the universe.

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