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Cosmological constraints on the very low frequency gravitational-wave background

Seto, Naoki and Cooray, Asantha (2006) Cosmological constraints on the very low frequency gravitational-wave background. Physical Review D, 73 (2). Art. No. 023005. ISSN 0556-2821. http://resolver.caltech.edu/CaltechAUTHORS:SETprd06a

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Abstract

The curl modes of cosmic microwave background polarization allow one to indirectly constrain the primordial background of gravitational waves with frequencies around 10^(-18) to 10^(-16) Hz. The proposed high precision timing observations of a large sample of millisecond pulsars with the pulsar timing array or with the square kilometer array can either detect or constrain the stochastic gravitational-wave background at frequencies greater than roughly 0.1 yr^(-1). While existing techniques are limited to either observe or constrain the gravitational-wave background across six or more orders of magnitude between 10^(-16) and 10^(-10) Hz, we suggest that the anisotropy pattern of time variation of the redshift related to a sample of high-redshift objects can be used to study the background around a frequency of 10^(-12) Hz. Useful observations to detect an anisotropy signal in the global redshift change include spectroscopic observations of the Ly-alpha forest in absorption towards a sample of quasars, redshifted 21 cm line observations either in absorption or emission towards a sample of neutral HI regions before or during reionization, and high-frequency (0.1 to 1 Hz) gravitational-wave analysis of a sample of neutron star-neutron star binaries detected with gravitational-wave instruments such as the Decihertz Interferometer Gravitational Wave Observatory (DECIGO). For reasonable observations expected in the future involving extragalactic sources, we find limits at the level of Omega(GW)< 10^(-6) at a frequency around 10^(-12) Hz while the ultimate limit is likely to be around Omega(GW)< 10^(-11). On the other hand, if there is a background of gravitational waves at 10^(-12) Hz with an amplitude larger than this limit, its presence will be visible as a measurable anisotropy in the time-evolving redshift of extragalactic sources.


Item Type:Article
Additional Information:©2006 The American Physical Society. Received 2 February 2005; published 20 January 2006. This work has been supported by NASA Grant No. NNG04GK98G and the Japan Society for the Promotion of Science.
Group:TAPIR
Subject Keywords:cosmology; gravitational waves; radiofrequency cosmic radiation; pulsars; red shift; circumstellar matter; infrared sources (astronomical); quasars; H I regions; neutron stars; binary stars
Record Number:CaltechAUTHORS:SETprd06a
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:SETprd06a
Alternative URL:http://dx.doi.org/10.1103/PhysRevD.73.023005
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:3685
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:29 Jun 2006
Last Modified:26 Dec 2012 08:55

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