Upper limit map of a background of gravitational waves

B. Abbott; R. Abbott; R. Adhikari; J. Agresti; P. Ajith; B. Allen; R. Amin; S. B. Anderson; W. G. Anderson; M. Arain; M. Araya; H. Armandula; M. Ashley; S. Aston; P. Aufmuth; C. Aulbert; S. Babak; S. Ballmer; H. Bantilan; B. C. Barish; C. Barker; D. Barker; B. Barr; P. Barriga; M. A. Barton; K. Bayer; K. Belczynski; J. Betzwieser; P. T. Beyersdorf; B. Bhawal; I. A. Bilenko; G. Billingsley; R. Biswas; E. Black; K. Blackburn; L. Blackburn; D. Blair; B. Bland; J. Bogenstahl; L. Bogue; R. Bork; V. Boschi; S. Bose; P. R. Brady; V. B. Braginsky; J. E. Brau; M. Brinkmann; A. Brooks; D. A. Brown; A. Bullington

doi:10.1103/PhysRevD.76.082003

Upper limit map of a background of gravitational waves

B. Abbott^*, R. Abbott, R. Adhikari, J. Agresti, P. Ajith, B. Allen, R. Amin, S. B. Anderson, W. G. Anderson, M. Arain, M. Araya, H. Armandula, M. Ashley, S. Aston, P. Aufmuth, C. Aulbert, S. Babak, S. Ballmer, H. Bantilan, B. C. BarishC. Barker, D. Barker, B. Barr, P. Barriga, M. A. Barton, K. Bayer, K. Belczynski, J. Betzwieser, P. T. Beyersdorf, B. Bhawal, I. A. Bilenko, G. Billingsley, R. Biswas, E. Black, K. Blackburn, L. Blackburn, D. Blair, B. Bland, J. Bogenstahl, L. Bogue, R. Bork, V. Boschi, S. Bose, P. R. Brady, V. B. Braginsky, J. E. Brau, M. Brinkmann, A. Brooks, D. A. Brown, A. Bullington

^*Corresponding author for this work

Physics and Astronomy

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Abstract

We searched for an anisotropic background of gravitational waves using data from the LIGO S4 science run and a method that is optimized for point sources. This is appropriate if, for example, the gravitational wave background is dominated by a small number of distinct astrophysical sources. No signal was seen. Upper limit maps were produced assuming two different power laws for the source strain power spectrum. For an f-3 power law and using the 50 Hz to 1.8 kHz band the upper limits on the source strain power spectrum vary between 1.2×10-48Hz-1 (100Hz/f)3 and 1.2×10-47Hz-1 (100Hz/f)3, depending on the position in the sky. Similarly, in the case of constant strain power spectrum, the upper limits vary between 8.5×10-49Hz-1 and 6.1×10-48Hz-1. As a side product a limit on an isotropic background of gravitational waves was also obtained. All limits are at the 90% confidence level. Finally, as an application, we focused on the direction of Sco-X1, the brightest low-mass x-ray binary. We compare the upper limit on strain amplitude obtained by this method to expectations based on the x-ray flux from Sco-X1.

Original language	English (US)
Article number	082003
Journal	Physical Review D - Particles, Fields, Gravitation and Cosmology
Volume	76
Issue number	8
DOIs	https://doi.org/10.1103/PhysRevD.76.082003
State	Published - Oct 29 2007

ASJC Scopus subject areas

Nuclear and High Energy Physics
Physics and Astronomy (miscellaneous)

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10.1103/PhysRevD.76.082003

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Abbott, B., Abbott, R., Adhikari, R., Agresti, J., Ajith, P., Allen, B., Amin, R., Anderson, S. B., Anderson, W. G., Arain, M., Araya, M., Armandula, H., Ashley, M., Aston, S., Aufmuth, P., Aulbert, C., Babak, S., Ballmer, S., Bantilan, H., ... Bullington, A. (2007). Upper limit map of a background of gravitational waves. Physical Review D - Particles, Fields, Gravitation and Cosmology, 76(8), [082003]. https://doi.org/10.1103/PhysRevD.76.082003

@article{8ced88a8745e4203a45da13487a1ad70,

title = "Upper limit map of a background of gravitational waves",

abstract = "We searched for an anisotropic background of gravitational waves using data from the LIGO S4 science run and a method that is optimized for point sources. This is appropriate if, for example, the gravitational wave background is dominated by a small number of distinct astrophysical sources. No signal was seen. Upper limit maps were produced assuming two different power laws for the source strain power spectrum. For an f-3 power law and using the 50 Hz to 1.8 kHz band the upper limits on the source strain power spectrum vary between 1.2×10-48Hz-1 (100Hz/f)3 and 1.2×10-47Hz-1 (100Hz/f)3, depending on the position in the sky. Similarly, in the case of constant strain power spectrum, the upper limits vary between 8.5×10-49Hz-1 and 6.1×10-48Hz-1. As a side product a limit on an isotropic background of gravitational waves was also obtained. All limits are at the 90% confidence level. Finally, as an application, we focused on the direction of Sco-X1, the brightest low-mass x-ray binary. We compare the upper limit on strain amplitude obtained by this method to expectations based on the x-ray flux from Sco-X1.",

author = "B. Abbott and R. Abbott and R. Adhikari and J. Agresti and P. Ajith and B. Allen and R. Amin and Anderson, {S. B.} and Anderson, {W. G.} and M. Arain and M. Araya and H. Armandula and M. Ashley and S. Aston and P. Aufmuth and C. Aulbert and S. Babak and S. Ballmer and H. Bantilan and Barish, {B. C.} and C. Barker and D. Barker and B. Barr and P. Barriga and Barton, {M. A.} and K. Bayer and K. Belczynski and J. Betzwieser and Beyersdorf, {P. T.} and B. Bhawal and Bilenko, {I. A.} and G. Billingsley and R. Biswas and E. Black and K. Blackburn and L. Blackburn and D. Blair and B. Bland and J. Bogenstahl and L. Bogue and R. Bork and V. Boschi and S. Bose and Brady, {P. R.} and Braginsky, {V. B.} and Brau, {J. E.} and M. Brinkmann and A. Brooks and Brown, {D. A.} and A. Bullington",

year = "2007",

month = oct,

day = "29",

doi = "10.1103/PhysRevD.76.082003",

language = "English (US)",

volume = "76",

journal = "Physical Review D - Particles, Fields, Gravitation and Cosmology",

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Abbott, B, Abbott, R, Adhikari, R, Agresti, J, Ajith, P, Allen, B, Amin, R, Anderson, SB, Anderson, WG, Arain, M, Araya, M, Armandula, H, Ashley, M, Aston, S, Aufmuth, P, Aulbert, C, Babak, S, Ballmer, S, Bantilan, H, Barish, BC, Barker, C, Barker, D, Barr, B, Barriga, P, Barton, MA, Bayer, K, Belczynski, K, Betzwieser, J, Beyersdorf, PT, Bhawal, B, Bilenko, IA, Billingsley, G, Biswas, R, Black, E, Blackburn, K, Blackburn, L, Blair, D, Bland, B, Bogenstahl, J, Bogue, L, Bork, R, Boschi, V, Bose, S, Brady, PR, Braginsky, VB, Brau, JE, Brinkmann, M, Brooks, A, Brown, DA & Bullington, A 2007, 'Upper limit map of a background of gravitational waves', Physical Review D - Particles, Fields, Gravitation and Cosmology, vol. 76, no. 8, 082003. https://doi.org/10.1103/PhysRevD.76.082003

TY - JOUR

T1 - Upper limit map of a background of gravitational waves

AU - Abbott, B.

AU - Abbott, R.

AU - Adhikari, R.

AU - Agresti, J.

AU - Ajith, P.

AU - Allen, B.

AU - Amin, R.

AU - Anderson, S. B.

AU - Anderson, W. G.

AU - Arain, M.

AU - Araya, M.

AU - Armandula, H.

AU - Ashley, M.

AU - Aston, S.

AU - Aufmuth, P.

AU - Aulbert, C.

AU - Babak, S.

AU - Ballmer, S.

AU - Bantilan, H.

AU - Barish, B. C.

AU - Barker, C.

AU - Barker, D.

AU - Barr, B.

AU - Barriga, P.

AU - Barton, M. A.

AU - Bayer, K.

AU - Belczynski, K.

AU - Betzwieser, J.

AU - Beyersdorf, P. T.

AU - Bhawal, B.

AU - Bilenko, I. A.

AU - Billingsley, G.

AU - Biswas, R.

AU - Black, E.

AU - Blackburn, K.

AU - Blackburn, L.

AU - Blair, D.

AU - Bland, B.

AU - Bogenstahl, J.

AU - Bogue, L.

AU - Bork, R.

AU - Boschi, V.

AU - Bose, S.

AU - Brady, P. R.

AU - Braginsky, V. B.

AU - Brau, J. E.

AU - Brinkmann, M.

AU - Brooks, A.

AU - Brown, D. A.

AU - Bullington, A.

PY - 2007/10/29

Y1 - 2007/10/29

N2 - We searched for an anisotropic background of gravitational waves using data from the LIGO S4 science run and a method that is optimized for point sources. This is appropriate if, for example, the gravitational wave background is dominated by a small number of distinct astrophysical sources. No signal was seen. Upper limit maps were produced assuming two different power laws for the source strain power spectrum. For an f-3 power law and using the 50 Hz to 1.8 kHz band the upper limits on the source strain power spectrum vary between 1.2×10-48Hz-1 (100Hz/f)3 and 1.2×10-47Hz-1 (100Hz/f)3, depending on the position in the sky. Similarly, in the case of constant strain power spectrum, the upper limits vary between 8.5×10-49Hz-1 and 6.1×10-48Hz-1. As a side product a limit on an isotropic background of gravitational waves was also obtained. All limits are at the 90% confidence level. Finally, as an application, we focused on the direction of Sco-X1, the brightest low-mass x-ray binary. We compare the upper limit on strain amplitude obtained by this method to expectations based on the x-ray flux from Sco-X1.

AB - We searched for an anisotropic background of gravitational waves using data from the LIGO S4 science run and a method that is optimized for point sources. This is appropriate if, for example, the gravitational wave background is dominated by a small number of distinct astrophysical sources. No signal was seen. Upper limit maps were produced assuming two different power laws for the source strain power spectrum. For an f-3 power law and using the 50 Hz to 1.8 kHz band the upper limits on the source strain power spectrum vary between 1.2×10-48Hz-1 (100Hz/f)3 and 1.2×10-47Hz-1 (100Hz/f)3, depending on the position in the sky. Similarly, in the case of constant strain power spectrum, the upper limits vary between 8.5×10-49Hz-1 and 6.1×10-48Hz-1. As a side product a limit on an isotropic background of gravitational waves was also obtained. All limits are at the 90% confidence level. Finally, as an application, we focused on the direction of Sco-X1, the brightest low-mass x-ray binary. We compare the upper limit on strain amplitude obtained by this method to expectations based on the x-ray flux from Sco-X1.

UR - http://www.scopus.com/inward/record.url?scp=35649010892&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=35649010892&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.76.082003

DO - 10.1103/PhysRevD.76.082003

M3 - Article

AN - SCOPUS:35649010892

SN - 1550-7998

VL - 76

JO - Physical Review D - Particles, Fields, Gravitation and Cosmology

JF - Physical Review D - Particles, Fields, Gravitation and Cosmology

IS - 8

M1 - 082003

ER -

Upper limit map of a background of gravitational waves

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