Stochastic Gravitational Wave Background: Upper Limits in the 10-6 to 10-3 Hz Band

Details Stochastic Gravitational Wave Background: Upper Limits in the 10-6 to 10-3 Hz Band Stochastic Gravitational Wave Background: Upper Limits in the 10-6 to 10-3 Hz Band

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003apj...599..806a&link_type=abstract

The Astrophysical Journal, Volume 599, Issue 2, pp. 806-813.

Astronomy and Astrophysics

Astronomy

34

Cosmology: Observations, Gravitational Waves, Relativity

Scientific paper

We have used precision Doppler tracking of the Cassini spacecraft during its 2001-2002 solar opposition to derive improved observational limits to an isotropic background of low-frequency gravitational waves. Using the Cassini multilink radio system and an advanced tropospheric calibration system, the effects of heretofore leading noises-plasma and tropospheric scintillation-were, respectively, removed and calibrated to levels lower than other noises. The resulting data were used to construct upper limits to the strength of an isotropic background in the 10-6 to 10-3 Hz band. Our results are summarized as limits on the strain spectrum Sh(f), the characteristic strain (hc = the square root of the product of the frequency and the one-sided spectrum of strain at that frequency), and the energy density (Ω = energy density in bandwidth equal to center frequency assuming a locally white energy density spectrum, divided by the critical density). Our best limits are Sh(f)<6×10-27 Hz-1 at several frequencies in the millihertz band, hc<2×10-15 at about 0.3 mHz, and Ω<0.025×h-275, where h75 is the Hubble constant in units of 75 km s-1 Mpc-1, at 1.2×10-6 Hz. These are the best observational limits in the low-frequency band, the bound on Ω, for example, being about 3 orders of magnitude better than previous constraints from Doppler tracking.

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