LIGO Document P1200087-v58

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

Document #:
LIGO-P1200087-v58
Document type:
P - Publications
Other Versions:
LIGO-P1200087-v57
26 Sep 2019, 13:52
LIGO-P1200087-v56
12 Sep 2019, 14:11
LIGO-P1200087-v55
04 Sep 2019, 05:53
LIGO-P1200087-v47
26 Apr 2018, 12:55
LIGO-P1200087-v46
15 Mar 2018, 09:06
LIGO-P1200087-v42
08 Sep 2017, 10:38
LIGO-P1200087-v32
09 Feb 2016, 01:31
LIGO-P1200087-v19
24 Apr 2014, 06:29
Abstract:
We present possible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next decade, with the intention of providing information to the astronomy community to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals, and study the capability of the network to determine the sky location of the source. We report our findings for gravitational-wave transients, with particular focus on gravitational-wave signals from the inspiral of binary neutron star systems, which are the most promising targets for multi-messenger astronomy. The ability to localize the sources of the detected signals depends on the geographical distribution of the detectors and their relative sensitivity, and 90% credible regions can be as large as thousands of square degrees when only two sensitive detectors are operational. Determining the sky position of a significant fraction of detected signals to areas of 520 square degrees requires at least three detectors of sensitivity within a factor of ~2 of each other and with a broad frequency bandwidth. When all detectors, including KAGRA and the third LIGO detector in India, reach design sensitivity, a significant fraction of gravitational-wave signals will be localized to a few square degrees by gravitational-wave observations alone.
Files in Document:
Author Groups:
Keywords:
observing-scenario
Notes and Changes:
Updated the numbers in Table 5 based on fixes/changes to the simulations. Also added some authors.

This is the updated version submitted to the arXiv. We expect at least one more update when we respond to the referee.

Associated with Events:
held on 08 May 2014 in NSF HQ

DCC Version 3.3.0, contact Document Database Administrators