Upper limits from the LIGO and TAMA detectors on the rate of gravitational-wave bursts -: art. no. 122004

被引：44

作者：

Abbott, B ^{[1
]}

Abbott, R

Adhikari, R

Ageev, A

Agresti, J

Ajith, P

Allen, B

Allen, J

Amin, R

Anderson, SB

Anderson, WG

Araya, M

Armandula, H

Ashley, M

Asiri, F

Aufmuth, P

Aulbert, C

Babak, S

Balasubramanian, R

Ballmer, S

Barish, BC

Barker, C

Barker, D

Barnes, M

Barr, B

Barton, MA

Bayer, K

Beausoleil, R

Belczynski, K

Bennett, R

Berukoff, SJ

Betzwieser, J

Bhawal, B

Bilenko, IA

Billingsley, G

Black, E

Blackburn, K

Blackburn, L

Bland, B

Bochner, B

Bogue, L

Bork, R

Bose, S

Brady, PR

Braginsky, VB

Brau, JE

Brown, DA

Bullington, A

Bunkowski, A

Buonanno, A

机构：

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

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

[3] Syracuse Univ, Syracuse, NY 13244 USA

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

[5] Univ Wisconsin, Milwaukee, WI 53201 USA

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

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

[8] Univ Texas, Brownsville, TX 78520 USA

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

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

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

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

[13] Cardiff Univ, Cardiff CF2 3YB, Wales

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

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

[16] Stanford Univ, Stanford, CA 94305 USA

[17] Northwestern Univ, Evanston, IL 60208 USA

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

[19] Washington State Univ, Pullman, WA 99164 USA

[20] Univ Oregon, Eugene, OR 97403 USA

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

[22] Univ Rochester, Rochester, NY 14627 USA

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

[24] Univ Florida, Gainesville, FL 32611 USA

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

[26] Carleton Coll, Northfield, MN 55057 USA

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

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

[29] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India

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

[31] Calif State Univ Dominguez Hills, Carson, CA 90747 USA

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

[33] Max Planck Inst Quantum Opt, D-85748 Garching, Germany

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

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

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

[37] Vassar Coll, Poughkeepsie, NY 12604 USA

[38] Salish Kootenai Coll, Pablo, MT 59855 USA

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

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

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

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

[43] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan

[44] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan

[45] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan

[46] Natl Astron Observ, Tokyo 1818588, Japan

[47] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan

[48] Hirosaki Univ, Fac Sci & Technol, Hirosaki, Aomori 0368561, Japan

[49] Niigata Univ, Fac Sci, Niigata 9502102, Japan

[50] Osaka Univ, Grad Sch Sci, Toyonaka, Osaka 5600043, Japan

来源：

PHYSICAL REVIEW D | 2005年 / 72卷 / 12期

关键词：

D O I：

10.1103/PhysRevD.72.122004

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on the first joint search for gravitational waves by the TAMA and LIGO collaborations. We looked for millisecond-duration unmodeled gravitational-wave bursts in 473 hr of coincident data collected during early 2003. No candidate signals were found. We set an upper limit of 0.12 events per day on the rate of detectable gravitational-wave bursts, at 90% confidence level. From software simulations, we estimate that our detector network was sensitive to bursts with root-sum-square strain amplitude above approximately 1-3x10(-19) Hz(-1/2) in the frequency band 700-2000 Hz. We describe the details of this collaborative search, with particular emphasis on its advantages and disadvantages compared to searches by LIGO and TAMA separately using the same data. Benefits include a lower background and longer observation time, at some cost in sensitivity and bandwidth. We also demonstrate techniques for performing coincidence searches with a heterogeneous network of detectors with different noise spectra and orientations. These techniques include using coordinated software signal injections to estimate the network sensitivity, and tuning the analysis to maximize the sensitivity and the livetime, subject to constraints on the background.

引用

页数：16

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