Template bank for spinning compact binary mergers in the second observation run of Advanced LIGO and the first observation run of Advanced Virgo
Mukherjee, Debnandini; Caudill, Sarah; Magee, Ryan; Messick, Cody; Privitera, Stephen; Sachdev, Surabhi; Blackburn, Kent; Brady, Patrick; Brockill, Patrick; Cannon, Kipp; Chamberlin, Sydney J.; Chatterjee, Deep; Creighton, Jolien D.E.; Fong, Heather; Godwin, Patrick; Hanna, Chad; Kapadia, Shasvath; Lang, Ryan N.; Li, Tjonnie G.F.; Lo, Rico K.L.; Meacher, Duncan; Pace, Alex; Sadeghian, Laleh; Tsukada, Leo; Wade, Leslie; Wade, Madeline; Weinstein, Alan; Xiao, Liting
(2021) Physical Review D, volume 103, issue 8, pp. 1 - 13
(Article)
Abstract
We describe the methods used to construct the aligned-spin template bank of gravitational waveforms used by the Gstreamer and Ligo Algorithm Library (GstLAL)-based pipeline to analyze data from the second observing run of Advanced Laser Interferometer Gravitational Wave Observatory (LIGO) and the first observing run of Advanced Virgo. The bank
... read more
expands upon the parameter space covered during Advanced LIGO's first observing run, including coverage for merging compact binary systems with total mass between 2 M and 400 M and mass ratios between 1 and 97.988. Thus the systems targeted include merging neutron star-neutron star systems, neutron star-black hole binaries, and black hole-black hole binaries expanding into the intermediate-mass range. Component masses less than 2 M have allowed (anti-)aligned spins between ±0.05, while component masses greater than 2 M have allowed (anti-)aligned between ±0.999. The bank placement technique combines a stochastic method with a new grid-bank method to better isolate noisy templates, resulting in a total of 677,000 templates.
show less
Download/Full Text
Keywords: Physics and Astronomy (miscellaneous)
ISSN: 2470-0010
Publisher: American Institute of Physics
Note: Funding Information: We thank the LIGO-Virgo Scientific Collaboration for access to data. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation (NSF) and operates under cooperative agreement PHY-0757058. We thank Satya Mohapatra for the helpful comments and suggestions. We also thank Graham Woan for helping with the review of the template bank used for the O2. We gratefully acknowledge the support by NSF Grant No. PHY-1607585 for J. C., P. B., D. C. and D. M. D. M. was also partly supported by PHY 14-54389, ACI 16-42391, OAC 18-41480. S. C. is supported by the research program of the Netherlands Organisation for Scientific Research (NWO). S. S. was supported in part by the Eberly Research Funds of Penn State, The Pennsylvania State University, University Park, PA 16802, USA. H. F. was supported by the Natural Sciences and Engineering Research Council of Canada (NSERC). C. H. was supported in part by the NSF through Grant No. PHY-1454389. Funding for this project was provided by the Charles E. Kaufman Foundation of The Pittsburgh Foundation. T. G. F. L. was partially supported by a grant from the Research Grants Council of the Hong Kong (Project No. CUHK 14310816 and CUHK 24304317) and the Direct Grant for Research from the Research Committee of the Chinese University of Hong Kong. M. W. was supported by NSF Grant No. PHY-1607178. We thank the computational resources provided by Leonard E. Parker Center for Gravitation, Cosmology and Astrophysics at the University of Wisconsin-Milwaukee and supported by National Science Foundation Grants No. PHY-1626190 and No. PHY-1700765. We are also grateful for the computational resources provided by The Pennsylvania State University’s Institute for CyberScience Advanced Cyber-Infrastructure (ICS-ACI). The authors are also grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grants No. PHY-0757058 and No. PHY-0823459. Publisher Copyright: © 2021 American Physical Society.
(Peer reviewed)
