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"Prospects for Observing and Localizing Gravitational-Wave Transients with Advanced LIGO and Advanced Virgo"

Abbott, B. P. et al.

	Abstract
1	Introduction
2	Commissioning and Observing Phases
	2.1	Commissioning and observing roadmap
	2.2	Envisioned observing schedule
3	Searches for Gravitational-Wave Transients
	3.1	Detection and false alarm rates
	3.2	Sky localization
4	Observing Scenario
	4.1	2015 – 2016 run (O1): aLIGO 40 – 80 Mpc
	4.2	2016 – 2017 run (O2): aLIGO 80 – 120 Mpc, AdV 20 – 60 Mpc
	4.3	2017 – 2018 run (O3): aLIGO 120 – 170 Mpc, AdV 60 – 85 Mpc
	4.4	2019+ runs: aLIGO 200 Mpc, AdV 65 – 130 Mpc
	4.5	2022+ runs: aLIGO (including India) 200 Mpc, AdV 130 Mpc
5	Conclusions
	Acknowledgements
A	Changes Between Versions
	A.1	Updates to detector commissioning
	A.2	Updates to sky localization
	References
	LIGO Scientific Collaboration and Virgo Collaboration
	Footnotes
	Figures
	Tables

Figure 1: aLIGO (left) and AdV (right) target strain sensitivity as a function of frequency. The binary neutron-star (BNS) range, the average distance to which these signals could be detected, is given in megaparsec. Current notions of the progression of sensitivity are given for early, mid and late commissioning phases, as well as the final design sensitivity target and the BNS-optimized sensitivity. While both dates and sensitivity curves are subject to change, the overall progression represents our best current estimates.