First cross-correlation analysis of interferometric and resonant-bar gravitational-wave data for stochastic backgrounds

被引：38

作者：

Abbott, B. ^{[1
]}

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.

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.

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 CF24 3AA, S Glam, Wales

[8] Carleton Coll, Northfield, MN 55057 USA

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

[10] Columbia Univ, New York, NY 10027 USA

[11] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA

[12] Hobart & William Smith Coll, Geneva, NY 14456 USA

[13] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India

[14] CALTECH, LIGO, Pasadena, CA 91125 USA

[15] LIGO Hanford Observ, Richland, WA 99352 USA

[16] LIGO Livingston Observ, Livingston, LA 70754 USA

[17] MIT, LIGO, Cambridge, MA 02139 USA

[18] Louisiana State Univ, Baton Rouge, LA 70803 USA

[19] Louisiana Tech Univ, Ruston, LA 71272 USA

[20] Loyola Univ, New Orleans, LA 70118 USA

[21] Moscow MV Lomonosov State Univ, Moscow 119992, Russia

[22] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[23] Natl Astron Observ, Tokyo 1818588, Japan

[24] Northwestern Univ, Evanston, IL 60208 USA

[25] Rochester Inst Technol, Rochester, NY 14623 USA

[26] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England

[27] San Jose State Univ, San Jose, CA 95192 USA

[28] SE Louisiana Univ, Hammond, LA 70402 USA

[29] So Univ, Baton Rouge, LA 70813 USA

[30] A&M Coll, Baton Rouge, LA 70813 USA

[31] Stanford Univ, Stanford, CA 94305 USA

[32] Syracuse Univ, Syracuse, NY 13244 USA

[33] Penn State Univ, University Pk, PA 16802 USA

[34] Univ Texas, Brownsville, TX 78520 USA

[35] Texas Southmost Coll, Brownsville, TX 78520 USA

[36] Trinity Univ, San Antonio, TX 78212 USA

[37] Univ Illes Balears, E-07122 Palma de Mallorca, Spain

[38] Leibniz Univ Hannover, D-30167 Hannover, Germany

[39] Univ Adelaide, Adelaide, SA 5005, Australia

[40] Univ Birmingham, Birmingham B15 2TT, W Midlands, England

[41] Univ Florida, Gainesville, FL 32611 USA

[42] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland

[43] Univ Maryland, College Pk, MD 20742 USA

[44] Univ Michigan, Ann Arbor, MI 48109 USA

[45] Univ Oregon, Eugene, OR 97403 USA

[46] Univ Rochester, Rochester, NY 14627 USA

[47] Univ Salerno, I-84084 Salerno, Italy

[48] Univ Sannio Benevento, I-82100 Benevento, Italy

[49] Univ Southampton, Southampton SO17 1BJ, Hants, England

[50] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland

来源：

PHYSICAL REVIEW D | 2007年 / 76卷 / 02期

基金：

英国科学技术设施理事会;

关键词：

D O I：

10.1103/PhysRevD.76.022001

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Data from the LIGO Livingston interferometer and the ALLEGRO resonant-bar detector, taken during LIGO's fourth science run, were examined for cross correlations indicative of a stochastic gravitational-wave background in the frequency range 850-950 Hz, with most of the sensitivity arising between 905 and 925 Hz. ALLEGRO was operated in three different orientations during the experiment to modulate the relative sign of gravitational-wave and environmental correlations. No statistically significant correlations were seen in any of the orientations, and the results were used to set a Bayesian 90% confidence level upper limit of Omega(gw)(f)<= 1.02, which corresponds to a gravitational-wave strain at 915 Hz of 1.5x10(-23) Hz(-1/2). In the traditional units of h(100)(2)Omega(gw)(f), this is a limit of 0.53, 2 orders of magnitude better than the previous direct limit at these frequencies. The method was also validated with successful extraction of simulated signals injected in hardware and software.

引用

页数：17

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