Gravitational Wave Advanced Detector Workshop 2017
Towards the next generation of gravitational wave detectors
7-12 May 2017
Hamilton Island, Queensland
Registration will close at Sat 22 April 2017, 07:00 UTC (Sat 22 April 2017, 5pm Sydney, Fri 21 April 2017, mid-night Los Angeles).
The age of gravitational wave astronomy has dawned, with advanced detectors providing the first detections. The international network will soon begin observations and planning is underway for improvements to the advanced detectors and for building the next generation of detectors. The operational lifespans of the current detectors (aLIGO, aVirgo, KAGRA) is finite, however, and it is becoming important to solidify plans for upgrades to these detectors and to come to consensus on large, next generation detectors, which will benefit significantly from international cooperation. At GWADW 2017 we will focus on these issues as we begin plans for a long period of observational gravitational wave astronomy, that will also include space-based detectors and pulsar timing arrays.
Planning for the design of second generation detectors was primarily guided by a need for a detection with significant emphasis given to maximising the range of the perceived most likely source, that is the coalescence of neutron star binaries. With the first detection and over ten years of additional research the choices for the design of future detectors has become much richer.
The GWADW 2017 workshop will open with a discussion on 'What is the known science case for future generations of detectors?'. From this we envisage exploring questions like 'How does the science case depend on the network of detectors?', 'Is it desirable for the detectors to have the same response?' and 'Will there be an ongoing role for second generation detectors?' and since the LISA mission will possibly be launched around the same time as future detectors come online, 'What will be the interaction of future ground based detectors and space based detectors'. Significant time will be devoted to key design issues for future detectors including control strategies, quantum and thermal noise abatement and extending the range of detectors to lower frequencies.