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Optimizing LIGO with LISA forewarnings to improve black-hole spectroscopy

Tso, Rhondale and Gerosa, Davide and Chen, Yanbei (2019) Optimizing LIGO with LISA forewarnings to improve black-hole spectroscopy. Physical Review D, 99 (12). Art. No. 124043. ISSN 2470-0010. https://resolver.caltech.edu/CaltechAUTHORS:20190625-111507915

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Abstract

The early inspiral of massive stellar-mass black-hole binaries merging in LIGO’s sensitivity band will be detectable at low frequencies by the upcoming space mission LISA. LISA will predict, with years of forewarning, the time and frequency with which binaries will be observed by LIGO. We will, therefore, find ourselves in the position of knowing that a binary is about to merge, with the unprecedented opportunity to optimize ground-based operations to increase their scientific payoff. We apply this idea to detections of multiple ringdown modes, or black-hole spectroscopy. Narrow-band tunings can boost the detectors’ sensitivity at frequencies corresponding to the first subdominant ringdown mode and largely improve our prospects to experimentally test the Kerr nature of astrophysical black holes. We define a new consistency parameter between the different modes, called δGR, and show that, in terms of this measure, optimized configurations have the potential to double the effectiveness of black-hole spectroscopy when compared to standard broadband setups.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1103/physrevd.99.124043DOIArticle
https://arxiv.org/abs/1807.00075arXivDiscussion Paper
ORCID:
AuthorORCID
Tso, Rhondale0000-0003-4464-0117
Gerosa, Davide0000-0002-0933-3579
Chen, Yanbei0000-0002-9730-9463
Additional Information:© 2019 American Physical Society. Received 29 June 2018; published 25 June 2019. We especially thank Jamie Rollins and Christopher Wipf for sharing their Python port of the GWINC software. We thank Joshua Smith for providing the GWINC Cosmic Explorer configuration file. D. G. and Y. C. thank Christian Ott for important suggestions on the early developments of this idea. We also thank Rana Adhikari, Emanuele Berti, Jonathan Blackman, Neil Cornish, Matthew Evans, Daniel D’Orazio, Matthew Giesler, Zoltan Haiman, Evan Hall, Kevin Kuns, Lionel London, Belinda Pang, Alberto Sesana, Ulrich Sperhake, and Salvatore Vitale for fruitful discussions. R. T. is supported by the National Science Foundation Graduate Research Fellowship Program under Grant No. DGE-1144469, the Ford Foundation Predoctoral Fellowship, and the Gates Foundation. D. G. is supported by NASA through Einstein Postdoctoral Fellowship Grant No. PF6-170152 awarded by the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under Contract No. NAS8-03060. Y. C. is supported by NSF Grants No. PHY-1708212, No. PHY-1404569, and No. PHY-1708213. Computations were performed on Caltech cluster Wheeler, supported by the Sherman Fairchild Foundation and Caltech, on the University of Birmingham’s BlueBEAR cluster, and at the Maryland Advanced Research Computing Center (MARCC).
Group:TAPIR, Astronomy Department
Funders:
Funding AgencyGrant Number
NSF Graduate Research FellowshipDGE-1144469
Ford FoundationUNSPECIFIED
Bill and Melinda Gates FoundationUNSPECIFIED
NASA Einstein FellowshipPF6-170152
NASANAS8-03060
NSFPHY-1708212
NSFPHY-1404569
NSFPHY-1708213
Sherman Fairchild FoundationUNSPECIFIED
CaltechUNSPECIFIED
Issue or Number:12
Record Number:CaltechAUTHORS:20190625-111507915
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190625-111507915
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:96696
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:25 Jun 2019 18:23
Last Modified:09 Mar 2020 13:18

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