Upper limit map of a background of gravitational waves

被引：86

作者：

Abbott, B.

Abbott, R.

Adhikari, R.

Agresti, J.

Ajith, P. ^{[2
]}

Allen, B. ^{[2
]}

Amin, R.

Anderson, S. B.

Anderson, W. G.

Arain, M.

Araya, M.

Armandula, H.

Ashley, M. ^{[4
]}

Aston, S.

Aufmuth, P.

Aulbert, C. ^{[1
]}

Babak, S. ^{[1
]}

Ballmer, S.

Bantilan, H. ^{[8
]}

Barish, B. C.

Barker, C.

Barker, D.

Barr, B.

Barriga, P.

Barton, M. A.

Bayer, K.

Belczynski, K.

Betzwieser, J.

Beyersdorf, P. T.

Bhawal, B.

Bilenko, I. A.

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, P. R.

Braginsky, V. B.

Brau, J. E.

Brinkmann, M. ^{[2
]}

Brooks, A.

Brown, D. A.

Bullington, A.

机构：

[1] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany

[2] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany

[3] Andrews Univ, Berrien Springs, MI 49104 USA

[4] Australian Natl Univ, Canberra, ACT 0200, Australia

[5] CALTECH, Pasadena, CA 91125 USA

[6] CALTECH, CaRT, Pasadena, CA 91125 USA

[7] Cardiff Univ, Cardiff CF23YB, Wales

[8] Carleton Coll, Northfield, MN 55057 USA

[9] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia

来源：

PHYSICAL REVIEW D | 2007年 / 76卷 / 08期

基金：

英国科学技术设施理事会;

关键词：

D O I：

10.1103/PhysRevD.76.082003

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 x 10(-48) Hz(-1) (100 Hz/f)(3) and 1.2 x 10(-47) Hz(-1) (100 Hz/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 x 10(-49) Hz(-1) and 6.1 x 10(-48) Hz(-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.

引用

页数：11

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