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On the properties of the massive binary black hole merger GW170729

Chatziioannou, Katerina and Barkett, Kevin and Blackman, Jonathan and Giesler, Matthew and Hemberger, Daniel and Scheel, Mark A. and Szilágyi, Béla and Teukolsky, Saul A. (2019) On the properties of the massive binary black hole merger GW170729. . (Unpublished) http://resolver.caltech.edu/CaltechAUTHORS:20190821-153756552

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Abstract

We present a detailed investigation into the properties of GW170729, the gravitational wave with the most massive and distant source confirmed to date. We employ an extensive set of waveform models, including new improved models that incorporate the effect of higher-order waveform modes which are particularly important for massive systems. We find no indication of spin-precession, but the inclusion of higher-order modes in the models results in an improved estimate for the mass ratio of (0.3−0.8) at the 90\% credible level. Our updated measurement excludes equal masses at that level. We also find that models with higher-order modes lead to the data being more consistent with a smaller effective spin, with the probability that the effective spin is greater than zero being reduced from 99% to 94%. The 90\% credible interval for the effective spin parameter is now (−0.01−0.50). Additionally, the recovered signal-to-noise ratio increases by ∼0.3 units compared to analyses without higher-order modes. We study the effect of common spin priors on the derived spin and mass measurements, and observe small shifts in the spins, while the masses remain unaffected. We argue that our conclusions are robust against systematic errors in the waveform models. We also compare the above waveform-based analysis which employs compact-binary waveform models to a more flexible wavelet- and chirplet-based analysis. We find consistency between the two, with overlaps of ∼0.9, typical of what is expected from simulations of signals similar to GW170729, confirming that the data are well-described by the existing waveform models. Finally, we study the possibility that the primary component of GW170729 was the remnant of a past merger of two black holes and find this scenario to be indistinguishable from the standard formation scenario.


Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription
https://arxiv.org/abs/1903.06742arXivDiscussion Paper
Additional Information:We thank Christopher Berry, Thomas Dent, Tristano DiGirolamo, Bhooshan Gadre, Roland Haas, Nathan Johnson-McDaniel, Riccardo Sturani, and Aaron Zimmerman for helpful comments and suggestions. This research has made use of data, software and/or web tools obtained from the Gravitational Wave Open Science Center (https://www.gw-openscience.org), a service of LIGO Laboratory, the LIGO Scientific Collaboration and the Virgo Collaboration. LIGO is funded by the U.S. National Science Foundation. Virgo is funded by the French Centre National de Recherche Scientifique (CNRS), the Italian Istituto Nazionale della Fisica Nucleare (INFN) and the Dutch Nikhef, with contributions by Polish and Hungarian institutes. JCB acknowledges support from Australian Research Council Discovery Project DP180103155. MH was supported by Science and Technology Facilities Council (STFC) grant ST/L000962/1 and European Research Council Consolidator Grant 647839. Parts of this research were conducted by the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), through project number CE170100004. ROS and JL are supported by National Science Foundation (NSF) PHY-1707965 and PHY-1607520. PS acknowledges support from the NWO Veni grant no. 680-47-460 and the Science and Technology Facilities Council grant ST/N000633/1. MH acknowledges support from the Swiss National Science Foundation (SNSF) Grant IZCOZ0 177057. LS was supported by the Young Elite Scientists Sponsorship Program by the China Association for Science and Technology (2018QNRC001), and partially supported by the National Science Foundation of China (11721303), and XDB23010200. The GT authors gratefully acknowledge the NSF for financial support from Grants No. PHY 1806580, PHY 1809572, and TG-PHY120016. Computational resources were provided by XSEDE and the Georgia Tech Cygnus Cluster. The RIT authors gratefully acknowledge the NSF for financial support from Grants No. PHY-1607520, No. PHY-1707946, No. ACI-1550436, No. AST-1516150, No. ACI-1516125, No. PHY-1726215. This work used the Extreme Science and Engineering Discovery Environment (XSEDE) [allocation TG-PHY060027N], which is supported by NSF grant No. ACI-1548562. Computational resources were also provided by the NewHorizons, BlueSky Clusters, and Green Prairies at the Rochester Institute of Technology, which were supported by NSF grants No. PHY-0722703, No. DMS-0820923, No. AST-1028087, No. PHY-1229173, and No. PHY-1726215. The SXS authors at Caltech acknowledge the Sherman Fairchild Foundation, and NSF grants PHY-1708212 and PHY-1708213. GL, NA, and AG are supported by NSF PHY-1606522, PHY-1654359, PHY-1654359. Computations were done using the orca cluster supported in part by PHY-1429873 and by Cal State Fullerton. AG is also supported in part by Nancy Goodhue-McWilliams. The authors are grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grants PHY-0757058 and PHY-0823459. Some of the computational work for this manuscript was also carried out on the computer cluster Vulcan at the Max Planck Institute for Gravitational Physics in Potsdam. Plots have been made with matplotlib [106] and corner [107].
Group:LIGO, TAPIR
Funders:
Funding AgencyGrant Number
Centre National de Recherche Scientifique (CNRS)UNSPECIFIED
Istituto Nazionale di Fisica Nucleare (INFN)UNSPECIFIED
NikhefUNSPECIFIED
Australian Research CouncilDP180103155
Science and Technology Facilities Council (STFC)ST/L000962/1
European Research Council (ERC)647839
Australian Research CouncilCE170100004
NSFPHY-1707965
NSFPHY-1607520
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)680-47-460
Science and Technology Facilities Council (STFC)ST/N000633/1
Swiss National Science Foundation (SNSF)IZCOZ0 177057
China Association for Science and Technology2018QNRC001
National Natural Science Foundation of China11721303
National Natural Science Foundation of ChinaXDB23010200
NSFPHY-1806580
NSFPHY-1809572
NSFTG-PHY120016
NSFPHY-1607520
NSFPHY-1707946
NSFACI- 1550436
NSFAST-1516150
NSFACI-1516125
NSFPHY-1726215
NSFTG-PHY060027N
NSFACI-1548562
NSFPHY-0722703
NSFDMS-0820923
NSFAST-1028087
NSFPHY-1229173
Sherman Fairchild FoundationUNSPECIFIED
NSFPHY-1708212
NSFPHY-1708213
NSFPHY-1606522
NSFPHY-1654359
NSFPHY-1429873
California State University, FullertonUNSPECIFIED
Nancy Goodhue-McWilliamsUNSPECIFIED
NSFPHY-0757058
NSFPHY-0823459
Record Number:CaltechAUTHORS:20190821-153756552
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20190821-153756552
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:98090
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:21 Aug 2019 22:58
Last Modified:21 Aug 2019 22:58

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