Gravitational Radiation, Inspiraling Binaries, and Cosmology

Details Gravitational Radiation, Inspiraling Binaries, and Cosmology Gravitational Radiation, Inspiraling Binaries, and Cosmology

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...183.6705f&link_type=abstract

American Astronomical Society, 183rd AAS Meeting, #67.05; Bulletin of the American Astronomical Society, Vol. 25, p.1395

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We show how to measure cosmological parameters using observations of inspiraling binary neutron star or black hole systems in one or more gravitational wave detectors. To illustrate, we focus on the case of fixed mass binary systems observed in a single Laser Interferometer Gravitational-wave Observatory (LIGO)-like detector. Using realistic detector noise estimates, we characterize the rate of detections as a function of a threshold signal-to-noise ratio rho_0 , the Hubble constant H_0, and the binary ``chirp'' mass. For rho_0 = 8, H_0 = 100km s(-1) Mpc(-1) , and 1.4 M_&sun; neutron star binaries, the anticipated sample has a median redshift of 0.22. Under the same assumptions but independent of H_0, a conservative rate density of coalescing binaries (8*E(-8) yr(-1) Mpc(-3) ) implies LIGO will observe ~ 50yr(-1) binary inspiral events. The precision with which H_0 and the deceleration parameter q_0 may be determined depends on the number of observed inspirals. For fixed mass binary systems, ~ 100 observations with rho_0 = 10 in the LIGO detector will give H_0 to 10% in an Einstein-DeSitter cosmology, and 3000 will give q_0 to 20%. For the conservative rate density of coalescing binaries, 100 detections with rho_0 = 10 will require about 4 yrs.

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