Published December 31, 2020
| Published + Submitted
Journal Article
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Inference of the Neutron Star Equation of State from Cosmological Distances
Chicago
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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 the signal will be redshifted towards the detector's 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 postmerger frequency, are better measured from the distant weak sources from z∼1.
Additional Information
© 2020 American Physical Society. Received 27 April 2020; revised 23 August 2020; accepted 2 November 2020; published 21 December 2020. The authors would like to thank Tom Callister and Georgios Lioutas for useful discussions. We also thank Daniel Brown for providing the NEMO/OzHF sensitivity curve, and Evan Hall for providing the CE 20 km 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 program 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 No. PHY-1700765, No. OAC-1841475, and No. 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 No. PHY-0757058 and No. PHY-0823459. This analysis was made possible by the lalsuite [127], astropy [128,129], numpy [130], scipy [131], and matplotlib [132] software packages. This article carries LIGO Document Number LIGO-P2000143.Attached Files
Published - PhysRevLett.125.261101.pdf
Submitted - 2004.11334.pdf
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2004.11334.pdf
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Additional details
- Eprint ID
- 104686
- Resolver ID
- CaltechAUTHORS:20200731-145542176
- LIGO Laboratory
- European Research Council (ERC)
- 759253
- Deutsche Forschungsgemeinschaft (DFG)
- 279384907
- Deutsche Forschungsgemeinschaft (DFG)
- SFB 1245
- Deutsche Forschungsgemeinschaft (DFG)
- 138713538
- Deutsche Forschungsgemeinschaft (DFG)
- SFB 881
- NSF
- PHY-1700765
- NSF
- OAC-1841475
- NSF
- PHY-1809572
- NSF
- PHY-1764464
- Simons Foundation
- NSF
- PHY-0757058
- NSF
- PHY-0823459
- Created
-
2020-07-31Created from EPrint's datestamp field
- Updated
-
2021-09-02Created from EPrint's last_modified field
- Caltech groups
- LIGO
- Other Numbering System Name
- LIGO Document
- Other Numbering System Identifier
- P2000143