Pulsar timing array observations of gravitational wave source timing parallax

Xihao Deng, Lee Samuel Finn

Research output: Contribution to journalArticle

16 Citations (Scopus)

Abstract

Pulsar timing arrays (PTAs) act to detect gravitational waves by observing the small, correlated effect the waves have on pulse arrival times at the Earth. This effect has conventionally been evaluated assuming the gravitational wave phase fronts are planar across the array, an assumption that is valid only for sources at distances R≫ 2πL2/λ, where L is physical extent of the array and λ is the radiation wavelength. In the case of PTAs, the array size is of the order of the pulsar-Earth distance (kpc) and λ is of the order of parsec. Correspondingly, for point gravitational wave sources closer than ~100Mpc, the PTA response is sensitive to the source parallax across the pulsar-Earth baseline. Here, we evaluate the PTA response to gravitational wave point sources including the important wavefront curvature effects. Taking the wavefront curvature into account, the relative amplitude and phase of the timing residuals associated with a collection of pulsars allow us to measure the distance to, and the sky position of, the source.

Original languageEnglish (US)
Pages (from-to)50-58
Number of pages9
JournalMonthly Notices of the Royal Astronomical Society
Volume414
Issue number1
DOIs
StatePublished - Jun 1 2011

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parallax
pulsars
gravitational waves
time measurement
curvature
arrival time
point sources
arrivals
point source
sky
wavelength
radiation
pulses
wavelengths
effect

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

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abstract = "Pulsar timing arrays (PTAs) act to detect gravitational waves by observing the small, correlated effect the waves have on pulse arrival times at the Earth. This effect has conventionally been evaluated assuming the gravitational wave phase fronts are planar across the array, an assumption that is valid only for sources at distances R≫ 2πL2/λ, where L is physical extent of the array and λ is the radiation wavelength. In the case of PTAs, the array size is of the order of the pulsar-Earth distance (kpc) and λ is of the order of parsec. Correspondingly, for point gravitational wave sources closer than ~100Mpc, the PTA response is sensitive to the source parallax across the pulsar-Earth baseline. Here, we evaluate the PTA response to gravitational wave point sources including the important wavefront curvature effects. Taking the wavefront curvature into account, the relative amplitude and phase of the timing residuals associated with a collection of pulsars allow us to measure the distance to, and the sky position of, the source.",
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Pulsar timing array observations of gravitational wave source timing parallax. / Deng, Xihao; Finn, Lee Samuel.

In: Monthly Notices of the Royal Astronomical Society, Vol. 414, No. 1, 01.06.2011, p. 50-58.

Research output: Contribution to journalArticle

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AU - Finn, Lee Samuel

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