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Inference of the neutron star equation of state from cosmological distances

Haster, Carl-Johan and Chatziioannou, Katerina and Bauswein, Andreas and Clark, James Alexander (2020) Inference of the neutron star equation of state from cosmological distances. . (Unpublished) https://resolver.caltech.edu/CaltechAUTHORS:20200731-145542176

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Abstract

Finite-size effects on the gravitational wave signal from a neutron star merger typically manifest at high frequencies where detector sensitivity decreases. Proposed sensitivity improvements can give us access both to stronger signals and to a myriad of weak signals from cosmological distances. The latter will outnumber the former and the relevant part of signal will be redshifted towards the detector most sensitive band. We study the redshift dependence of information about neutron star matter and find that single-scale properties, such as the star radius or the post-merger frequency, are better measured from the distant weak sources from z∼1.


Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/2004.11334arXivDiscussion Paper
ORCID:
AuthorORCID
Chatziioannou, Katerina0000-0002-5833-413X
Bauswein, Andreas0000-0001-6798-3572
Additional Information:The authors would like to thank Tom Callister for useful discussions. We also thank Daniel Brown for providing the OzHF sensitivity curve, and Evan Hall for providing the CE 20km sensitivity curve. C.-J.H. acknowledge support of the National Science Foundation, and the LIGO Laboratory. A.B. acknowledges support by the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme under grant agreement No. 759253. A.B. and by Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) - Project-ID 279384907 - SFB 1245 and Project-ID 138713538 - SFB 881 (“The Milky Way System", subproject A10). J.A.C. acknowledge support of the National Science Foundation Grants PHY-1700765, OAC-1841530 and PHY-1809572. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative agreement PHY-1764464. The Flatiron Institute is supported by the Simons Foundation. The authors are grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grants PHY-0757058 and PHY-0823459. This analysis was made possible by the LALSuite [123], astropy [124, 125], numpy [126], SciPy [127] and matplotlib [128] software packages. This article carries LIGO Document Number LIGO-P2000143.
Group:LIGO
Funders:
Funding AgencyGrant Number
LIGO LaboratoryUNSPECIFIED
European Research Council (ERC)759253
Deutsche Forschungsgemeinschaft (DFG)279384907
Deutsche Forschungsgemeinschaft (DFG)SFB 1245
Deutsche Forschungsgemeinschaft (DFG)138713538
Deutsche Forschungsgemeinschaft (DFG)SFB 881
NSFPHY-1700765
NSFOAC-1841530
NSFPHY-1809572
NSFPHY-1764464
Simons FoundationUNSPECIFIED
NSFPHY-0757058
NSFPHY-0823459
Other Numbering System:
Other Numbering System NameOther Numbering System ID
LIGO DocumentP2000143
Record Number:CaltechAUTHORS:20200731-145542176
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200731-145542176
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:104686
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:31 Jul 2020 22:40
Last Modified:31 Jul 2020 22:40

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