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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

1		Another often quoted number is the BNS horizon – the distance at which an optimally oriented and located BNS system would be observed with an SNR of $8$ . The horizon is a factor of 2.26 larger than the range [58 , 13 , 20 ].
2		Data from the fifth and sixth science runs (S5 and S6) of LIGO are publicly available from the LIGO Open Science Center losc.ligo.org [108 ].
3		We do not intend to produce timing-only sky maps, but timing triangulation can be useful for order-of-magnitude estimates of sky-localization accuracy averaged across the population of signals.
4		We expect that on average 50% of sources should be found within a reported 50% confidence region, but this is not the case: between 65% and 85% of detected signals have been found within the 50% confidence regions, depending upon the detector network and signal morphology [51 *].
5		This assumes a black-hole mass of $5M ⊙$ .
6		This is consistent with what was achieved with the initial detectors, where H1 and L1 had duty cycles of 78% and 67% in the S5 observing run [21 ]. Virgo had duty cycles of 81%, 80% and 73% in observing runs VSR1 – 3 respectively [1 ].
7		This study used noise from the sixth science run of initial LIGO, recolored to the expected O1 sensitivity curve. The source catalog, as well as the analysis pipeline, is shared with [99 *].