Gravitational wave spectroscopy of binary neutron star merger remnants with mode stacking
AffiliationUniv Arizona, Theoret Astrophys Program, Dept Astron
Univ Arizona, Theoret Astrophys Program, Dept Phys
MetadataShow full item record
PublisherAMER PHYSICAL SOC
CitationGravitational wave spectroscopy of binary neutron star merger remnants with mode stacking 2018, 97 (2) Physical Review D
JournalPhysical Review D
Rights© 2018 American Physical Society
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at email@example.com.
AbstractA binary neutron star coalescence event has recently been observed for the first time in gravitational waves, and many more detections are expected once current ground-based detectors begin operating at design sensitivity. As in the case of binary black holes, gravitational waves generated by binary neutron stars consist of inspiral, merger, and postmerger components. Detecting the latter is important because it encodes information about the nuclear equation of state in a regime that cannot be probed prior to merger. The postmerger signal, however, can only be expected to be measurable by current detectors for events closer than roughly ten megaparsecs, which given merger rate estimates implies a low probability of observation within the expected lifetime of these detectors. We carry out Monte Carlo simulations showing that the dominant postmerger signal (the l = m = 2 mode) from individual binary neutron star mergers may not have a good chance of observation even with the most sensitive future ground-based gravitational wave detectors proposed so far (the Einstein Telescope and Cosmic Explorer, for certain equations of state, assuming a full year of operation, the latest merger rates, and a detection threshold corresponding to a signal-to-noise ratio of 5). For this reason, we propose two methods that stack the postmerger signal from multiple binary neutron star observations to boost the postmerger detection probability. The first method follows a commonly used practice of multiplying the Bayes factors of individual events. The second method relies on an assumption that the mode phase can be determined from the inspiral waveform, so that coherent mode stacking of the data from different events becomes possible. We find that both methods significantly improve the chances of detecting the dominant postmerger signal, making a detection very likely after a year of observation with Cosmic Explorer for certain equations of state. We also show that in terms of detection, coherent stacking is more efficient in accumulating confidence for the presence of postmerger oscillations in a signal than the first method. Moreover, assuming the postmerger signal is detected with Cosmic Explorer via stacking, we estimate through a Fisher analysis that the peak frequency can be measured to a statistical error of similar to 4-20 Hz for certain equations of state. Such an error corresponds to a neutron star radius measurement to within similar to 15-56 m, a fractional relative error similar to 4%, suggesting that systematic errors from theoretical modeling greater than or similar to 100 m) may dominate the error budget.
VersionFinal published version
SponsorsNSF [PHY-1607449]; Simons Foundation; NASA [NNX16AR67G]; JSPS; NSF CAREER Grant [PHY-1250636]; NASA Grant [NNX16AB98G]; NSERC; CIFAR; Perimeter Institute through Industry Canada; Province of Ontario through the Ministry of Research Innovation