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Detecting the Gravitational Wave background using Millisecond Pulsars

Detecting the Gravitational Wave background using Millisecond Pulsars. Fredrick A. Jenet Center for Gravitational Wave Astronomy University of Texas at Brownsville. Dick Manchester ATNF/CSIRO Australia. George Hobbs ATNF/CSIRO Australia. KJ Lee Peking U. China. Andrea Lommen

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Detecting the Gravitational Wave background using Millisecond Pulsars

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  1. Detecting the Gravitational Wave background using Millisecond Pulsars Fredrick A. Jenet Center for Gravitational Wave Astronomy University of Texas at Brownsville

  2. Dick Manchester ATNF/CSIRO Australia George Hobbs ATNF/CSIRO Australia KJ Lee Peking U. China Andrea Lommen Franklin & Marshall USA Shane L. Larson Penn State USA Linqing Wen AEI Germany Collaborators John Armstrong JPL USA Teviet Creighton Caltech USA

  3. What can we do with an array of pulsars and the G-wave background? Make a definitive detection of G-waves. Measure the polarization properties of G-waves. Place limits on the graviton mass. Study the properties of the G-wave source.

  4. The most likely source of G-waves will be a stochastic background generated by super-massive binary black holes distributed throughout the universe! • Jaffe & Backer (2002) • Wyithe & Lobe (2002) • Enoki, Inoue, Nagashima, Sugiyama (2004) Like the cosmic micro-wave background, the G-wave background is an incoherent sum of G-waves. hc = A f-  = 2/3 A = 10 -15 to 10 -14 yrs-2/3

  5. Detecting G-waves • The presence of G-waves will cause the rate of arrival a individual pulses to fluctuate.

  6. Pulsar Earth Photon Path km xm G-wave

  7. Important Points

  8. The timing residuals for a stochastic background This is the same for all pulsars. This depends on the pulsar. The induced residuals for different pulsars will be correlated.

  9. Two basic techniques Spherical Harmonic Decomposition Two-point correlation Hellings & Downs 1983 Jenet, Hobbs, Lee, & Manchester 2005 Hellings 1990 Jaffe & Backer 2002

  10. Single Pulsar Limit (1 ms, 7 years) Expected Regime For a background of SMBH binaries: hc = A f-2/3

  11. Single Pulsar Limit (1 ms, 7 years) Expected Regime 1 ms, 1 year (Current ability) For a background of SMBH binaries: hc = A f-2/3

  12. Single Pulsar Limit (1 ms, 7 years) Expected Regime 1 ms, 1 year (Current ability) For a background of SMBH binaries: hc = A f-2/3 .1 m s 5 years

  13. Single Pulsar Limit (1 ms, 7 years) Expected Regime 1 ms, 1 year (Current ability) For a background of SMBH binaries: hc = A f-2/3 .1  s 10 years .1 m s 5 years

  14. Single Pulsar Limit (1 ms, 7 years) Expected Regime 1 ms, 1 year (Current ability) For a background of SMBH binaries: hc = A f-2/3 SKA 10 ns 5 years 40 pulsars .1  s 10 years .1 m s 5 years

  15. Expected Regime 1 ms, 1 year (Current ability) For a background of SMBH binaries: hc = A f-2/3 Single Pulsar Limit (20 ns, 2 years) SKA 10 ns 5 years 40 pulsars .1  s 10 years .1 m s 5 years

  16. G-wave polarization properties

  17. Graviton Mass • Current solar system limits place mg < 4.4 10-22 eV • 2 = k2 + (2  mg/h)2 •  < 1/ (4 months) • Detecting 5 year period G-wave reduces the upper bound of the graviton mass by a factor of 15.

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