Rapid Bayesian position reconstruction for gravitational-wave transients
Within the next few years, Advanced LIGO and Virgo should detect gravitational waves from binary neutron star and neutron star-black hole mergers. These sources are also predicted to power a broad array of electromagnetic transients. Because the electromagnetic signatures can be faint and fade rapidly, observing them hinges on rapidly inferring the sky location from the gravitational-wave observations. Markov chain Monte Carlo methods for gravitational-wave parameter estimation can take hours or more. We introduce BAYESTAR, a rapid, Bayesian, non-Markov chain Monte Carlo sky localization algorithm that takes just seconds to produce probability sky maps that are comparable in accuracy to the full analysis. Prompt localizations from BAYESTAR will make it possible to search electromagnetic counterparts of compact binary mergers.
© 2016 American Physical Society. Received 28 September 2015; published 14 January 2016. We thank John Veitch and Will Farr for chairing a review of the analysis and code. We thank Britt Griswold for assistance with preparing Fig. 8. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the NSF and operates under Cooperative Agreement No. PHY-0107417. This research was supported by the NSF through a Graduate Research Fellowship to L. S. L. S. thanks the Aspen Center for Physics and NSF Grant No. 1066293 for hospitality during the editing of this paper. Source code for BAYESTAR is available as part of LALInference,17 the open source LIGO/Virgo parameter estimation toolchain, which is in turn part of LALSuite.18 This research made use of Astropy19 , a community-developed core Python package for astronomy. Some of the results in this paper have been derived using HEALPix20 . Some results were produced on the NEMO computing cluster operated by the Center for Gravitation and Cosmology at University of Wisconsin–Milwaukee under NSF Grants No. PHY-0923409 and No. PHY-0600953.
Published - PhysRevD.93.024013.pdf
Submitted - 1508.03634v2.pdf