Systematic Parameter Errors in Inspiraling Neutron Star Binaries
- Creators
- Favata, Marc
Abstract
The coalescence of two neutron stars is an important gravitational wave source for LIGO and other detectors. Numerous studies have considered the precision with which binary parameters (masses, spins, Love numbers) can be measured. Here I consider the accuracy with which these parameters can be determined in the presence of systematic errors due to waveform approximations. These approximations include truncation of the post-Newtonian (PN) series and neglect of neutron star (NS) spin, tidal deformation, or orbital eccentricity. All of these effects can yield systematic errors that exceed statistical errors for plausible parameter values. In particular, neglecting spin, eccentricity, or high-order PN terms causes a significant bias in the NS Love number. Tidal effects will not be measurable with PN inspiral waveforms if these systematic errors are not controlled.
Additional Information
© 2014 American Physical Society. Published 10 March 2014; Received 30 October 2013. This work was supported by NSF Grants No. PHY- 0970074, No. PHY-1308527, and the UWM Research Growth Initiative. I thank Curt Cutler, Stephen Fairhurst, Jocelyn Read, Michele Vallisneri, and the referees for comments on this manuscript. I also thank Kent Yagi and Nicolás Yunes for helping me find a coding error that affected my results. Their complementary work [37] focuses on the systematic error in the tidal deformability using a modified version of the scheme discussed here.Attached Files
Published - PhysRevLett.112.101101.pdf
Submitted - 1310.8288v2.pdf
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Additional details
- Eprint ID
- 45120
- Resolver ID
- CaltechAUTHORS:20140422-143821253
- PHY-0970074
- NSF
- PHY-1308527
- NSF
- UWM Research Growth Initiative
- Created
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2014-04-25Created from EPrint's datestamp field
- Updated
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2021-11-10Created from EPrint's last_modified field